| NAME | RA | DEC | LII | BII | ROLL_ANGLE | TIME | STOP_TIME | OBSID | EXPOSURE | TIME_AWARDED | XIS0_EXPO | XIS1_EXPO | XIS2_EXPO | XIS3_EXPO | XIS0_NUM_MODES | XIS1_NUM_MODES | XIS2_NUM_MODES | XIS3_NUM_MODES | HXD_NUM_MODES | HXD_EXPO_CO | HXD_EXPO_FI | HXD_EXPO_NO | HXD_EXPO | HXD_EXPO_WAM | HXD_BURSTS | PROCESSING_STATUS | PROCESSING_DATE | PUBLIC_DATE | DISTRIBUTION_DATE | PROCESSING_VERSION | NUM_PROCESSED | SOFTWARE_VERSION | PRNB | ABSTRACT | SUBJECT_CATEGORY | CATEGORY_CODE | PRIORITY | PI_LNAME | PI_FNAME | COPI_LNAME | COPI_FNAME | COUNTRY | CYCLE | OBS_TYPE | TITLE | AIMPOINT | INJECTION |
|---|
| E0102-72 | 16.139 | -72.1205 | 301.50933431 | -44.97149935 | 119.4064 | 53593.3086458333 | 53595.2485069444 | 100001010 | 2406.8 | 70000 | 2406.8 | 2406.8 | 2406.8 | 2406.8 | 1 | 1 | 1 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57520.6843287037 | 54247 | 54035.5925115741 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000001 | XIS door open with a SMC SNR E0102-72 | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | XIS door open | NULL | N |
| E0102-72 | 15.9884 | -72.0403 | 301.56673438 | -45.05476105 | 119.5512 | 53595.2489236111 | 53595.4618518518 | 100001020 | 4159.8 | 10000 | 4159.8 | 4159.8 | 4159.8 | 4159.8 | 1 | 1 | 1 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57520.6779861111 | 54247 | 54035.6312731482 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000001 | XIS door open with a SMC SNR E0102-72 | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | XIS door open | NULL | N |
| N132D | 81.2794 | -69.6524 | 280.31514531 | -32.77566051 | 53.3291 | 53595.4703125 | 53597.5313541667 | 100002010 | 7406.6 | 80000 | 7406.6 | 7406.6 | 7406.6 | 7406.6 | 2 | 2 | 2 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57520.7109606482 | 54247 | 54038.5875925926 | 3.0.22.43 | 6 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000002 | HXD HV ON WITH N132D, and 5 pointings with XIS | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | HXD HV ON WITH N132D | NULL | N |
| N132D | 81.1356 | -69.5861 | 280.24807804 | -32.83670135 | 53.4639 | 53597.5317361111 | 53597.6932291667 | 100002020 | 0 | 7000 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57520.6768865741 | 54247 | 54230.4131828704 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000002 | HXD HV ON WITH N132D, and 5 pointings with XIS | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | HXD HV ON WITH N132D | NULL | N |
| N132D | 81.4173 | -69.7177 | 280.38157857 | -32.71705874 | 53.198 | 53597.6939814815 | 53597.8369328704 | 100002030 | 0 | 7000 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57520.6825231482 | 54247 | 54230.4133449074 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000002 | HXD HV ON WITH N132D, and 5 pointings with XIS | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | HXD HV ON WITH N132D | NULL | N |
| N132D | 81.0865 | -69.7023 | 280.38777612 | -32.83268249 | 53.5118 | 53597.8375 | 53597.9865625 | 100002040 | 0 | 7000 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57520.6840277778 | 54247 | 54230.4148726852 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000002 | HXD HV ON WITH N132D, and 5 pointings with XIS | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | HXD HV ON WITH N132D | NULL | N |
| N132D | 81.4727 | -69.6025 | 280.24276086 | -32.71811202 | 53.1485 | 53597.9869444444 | 53598.2398958333 | 100002050 | 0 | 7000 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57520.6873263889 | 54247 | 54230.4157291667 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000002 | HXD HV ON WITH N132D, and 5 pointings with XIS | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | HXD HV ON WITH N132D | NULL | N |
| N132D | 81.2751 | -69.6506 | 280.31335191 | -32.77744994 | 53.3312 | 53598.2402777778 | 53598.5140046296 | 100002060 | 5963.5 | 7000 | 5963.5 | 5963.5 | 5963.5 | 5963.5 | 1 | 1 | 1 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57520.6925115741 | 54247 | 54038.4700810185 | 3.0.22.43 | 6 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000002 | HXD HV ON WITH N132D, and 5 pointings with XIS | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | HXD HV ON WITH N132D | NULL | N |
| DEM_L71/N23 | 76.4474 | -67.958 | 278.75859594 | -34.83581885 | 70.5849 | 53598.5206365741 | 53599.6042592593 | 100003010 | 5789.7 | 40000 | 5789.7 | 5789.7 | 5789.7 | 5789.7 | 2 | 2 | 2 | 2 | 0 | 0 | 0 | 0 | 0 | 93606.1 | 0 | PROCESSED | 57520.7098611111 | 54247 | 54035.7018171296 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000003 | LMC SNRs L71/N23 | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | LMC SNRs | NULL | N |
| MCG-6-30-15 | 203.9795 | -34.2919 | 313.29805273 | 27.68293005 | 295.971 | 53599.6735300926 | 53601.1459027778 | 100004010 | 46698.7 | 40000 | 46700.9 | 50916.9 | 46698.7 | 46725.4 | 3 | 3 | 3 | 3 | 1 | 0 | 0 | 46484.6 | 46484.6 | 127099.9 | 0 | PROCESSED | 57520.7326388889 | 54247 | 54035.7991782407 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000004 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | MCG-60-30-15 | NULL | N |
| Cen A | 201.3695 | -43.0177 | 309.51950829 | 19.41821819 | 303.9158 | 53601.1523032407 | 53602.4098148148 | 100005010 | 64675.9 | 40000 | 64694.2 | 64765.8 | 64675.9 | 64739.9 | 5 | 2 | 5 | 5 | 1 | 0 | 0 | 66258.2 | 66258.2 | 108611.9 | 0 | PROCESSED | 57520.7361921296 | 53705 | 53905.4597106482 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000005 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Cen A | NULL | N |
| A 2052 | 229.2779 | 6.8766 | 9.31339919 | 49.96215441 | 281.2328 | 53602.4238078704 | 53602.743287037 | 100006010 | 13902.1 | 20000 | 13902.1 | 13902.1 | 13902.1 | 13902.1 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 13416.3 | 13416.3 | 27583.9 | 0 | PROCESSED | 57520.7207407407 | 53705 | 53905.4607523148 | 3.0.22.43 | 11 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000006 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Outer region of A 2052 | NULL | N |
| A 2052 | 229.3237 | 7.1059 | 9.64711471 | 50.05514889 | 281.2373 | 53602.7440393518 | 53603.3406944445 | 100006020 | 25743.1 | 20000 | 25743.1 | 25743.1 | 25743.1 | 25743.1 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 21064.2 | 21064.2 | 51519.9 | 0 | PROCESSED | 57520.7246527778 | 53705 | 53905.4610300926 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000006 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Outer region of A 2052 | NULL | N |
| A 2052 | 229.0933 | 7.1516 | 9.50335527 | 50.26933049 | 281.2093 | 53603.3412615741 | 53603.6114351852 | 100006030 | 12969 | 20000 | 12969 | 12969 | 12969 | 12969 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 13141.3 | 13141.3 | 23327.9 | 0 | PROCESSED | 57520.7271527778 | 53705 | 53905.4613310185 | 3.0.22.43 | 9 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000006 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Outer region of A 2052 | NULL | N |
| A 2052 | 229.0471 | 6.9211 | 9.16646689 | 50.17566284 | 281.2031 | 53603.6121875 | 53603.9938425926 | 100006040 | 16744.3 | 20000 | 16744.3 | 16744.3 | 16744.3 | 16744.3 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 12839.5 | 12839.5 | 32951.9 | 0 | PROCESSED | 57520.7325810185 | 53705 | 53905.4634143518 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000006 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Outer region of A 2052 | NULL | N |
| A 2052 | 229.3311 | 7.2632 | 9.85579143 | 50.13807877 | 91.2371 | 53762.482650463 | 53762.9209953704 | 100006050 | 22366 | 20000 | 22366 | 22366 | 22366 | 22366 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 20388 | 20388 | 37865.9 | 0 | PROCESSED | 57532.800162037 | 54247 | 54040.5318634259 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000006 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Outer region of A 2052 | XIS | N |
| Crab Nebula | 83.6274 | 22.0192 | 184.55062413 | -5.78629385 | 86.8663 | 53604.1571412037 | 53604.2501273148 | 100007010 | 1722.9 | 5000 | 1722.9 | 1722.9 | 1722.9 | 1722.9 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 1808 | 1808 | 8034 | 0 | PROCESSED | 57520.7330324074 | 54247 | 54105.2758912037 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000007 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Crab Nebula | NULL | N |
| Crab nebula | 83.6201 | 22.1854 | 184.40591259 | -5.70300776 | 86.8631 | 53604.2507175926 | 53604.3889351852 | 100007020 | 3053.1 | 5000 | 3057.1 | 3053.1 | 3053.1 | 3053.1 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 3134.3 | 3134.3 | 11940 | 1 | PROCESSED | 57520.7416782407 | 54247 | 54105.2987268518 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000007 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Crab Nebula | NULL | N |
| Crab nebula | 83.6399 | 21.8519 | 184.69891686 | -5.86604099 | 86.8683 | 53604.3898263889 | 53604.4890972222 | 100007030 | 2786.1 | 5000 | 2786.1 | 2786.1 | 2790.1 | 2786.1 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2192.7 | 2192.7 | 8554.1 | 0 | PROCESSED | 57520.7416203704 | 54247 | 54105.2865393518 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000007 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Crab Nebula | NULL | N |
| Crab nebula | 83.4512 | 22.0082 | 184.47195778 | -5.93010486 | 86.7989 | 53604.489849537 | 53604.5835416667 | 100007040 | 4268.2 | 5000 | 4268.2 | 4268.2 | 4268.2 | 4268.2 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 4139.2 | 4139.2 | 8056 | 0 | PROCESSED | 57520.7454513889 | 54247 | 54105.3073726852 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000007 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Crab Nebula | NULL | N |
| Crab nebula | 83.8083 | 22.0272 | 184.63396429 | -5.64031243 | 86.9342 | 53604.5844791667 | 53604.6479861111 | 100007050 | 3262 | 5000 | 3262 | 3262 | 3262 | 3262 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 3179 | 3179 | 5448 | 0 | PROCESSED | 57520.7490509259 | 54247 | 54105.3334143518 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000007 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Crab Nebula | NULL | N |
| NGC 4945 | 196.3712 | -49.4666 | 305.27663793 | 13.34118784 | 313.9062 | 53604.7788310185 | 53605.1010763889 | 100008010 | 14338 | 15000 | 14338 | 14338 | 14338 | 14338 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 13806.7 | 13806.7 | 27841.9 | 1 | PROCESSED | 57526.8553819444 | 54247 | 54035.5212152778 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000008 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | NGC 4945 | NULL | N |
| NGC 4945 | 196.3733 | -49.4666 | 305.27803835 | 13.34111135 | 313.9078 | 53605.101087963 | 53605.1034490741 | 100008020 | 177.6 | 10000 | 181.5 | 181.5 | 179.6 | 177.6 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 200.1 | 200.1 | 202 | 0 | PROCESSED | 57526.8486574074 | 54247 | 54034.6891435185 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000008 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | NGC 4945 | NULL | N |
| NGC 4945 | 196.3681 | -49.4152 | 305.27752827 | 13.39262005 | 96.1296 | 53750.3365625 | 53752.9655092593 | 100008030 | 95066.3 | 10000 | 95081.7 | 95129.7 | 95066.3 | 95106.3 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 84981.3 | 84981.3 | 227115.7 | 2 | PROCESSED | 57532.7353240741 | 54247 | 54040.3587615741 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000008 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | NGC 4945 | HXD | N |
| PSR1509-58 | 228.4798 | -59.0943 | 320.34145971 | -1.12587132 | 287.6342 | 53605.36 | 53606.8597569444 | 100009010 | 65161.8 | 60000 | 65161.8 | 65322.7 | 65242.7 | 65242.7 | 3 | 3 | 3 | 3 | 1 | 0 | 0 | 49735.7 | 49735.7 | 129529.8 | 4 | PROCESSED | 57526.9045486111 | 53705 | 53905.4622337963 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000009 | HXD spectrum and timing check | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | PSR1509-58 | NULL | N |
| Crab Nebula | 83.6267 | 22.0751 | 184.50282132 | -5.75691305 | 86.8655 | 53607.0070833333 | 53607.1389814815 | 100010010 | 2937.9 | 5000 | 2937.9 | 2937.9 | 2937.9 | 2937.9 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 3438.7 | 3438.7 | 11381.9 | 0 | PROCESSED | 57526.8678703704 | 54247 | 54118.9886689815 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000010 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Crab Offset 1 | NULL | N |
| Crab nebula | 83.6336 | 21.9568 | 184.60669551 | -5.81484075 | 86.8687 | 53607.1394560185 | 53607.2779282407 | 100010020 | 3653.3 | 5000 | 3653.3 | 3653.3 | 3653.3 | 3653.3 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 3806.7 | 3806.7 | 11934 | 0 | PROCESSED | 57526.8772337963 | 54247 | 54118.9337615741 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000010 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Crab Offset 1 | NULL | N |
| Crab nebula | 83.6105 | 22.3483 | 184.26290563 | -5.62323625 | 86.8596 | 53607.2790509259 | 53607.5139583333 | 100010030 | 8112.9 | 5000 | 8112.9 | 8112.9 | 8112.9 | 8112.9 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 7835.9 | 7835.9 | 20264 | 1 | PROCESSED | 57526.8876388889 | 54247 | 54118.9698958333 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000010 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Crab Offset 1 | NULL | N |
| Crab nebula | 83.6511 | 21.6763 | 184.85366771 | -5.95118505 | 86.8795 | 53607.5153125 | 53607.7153472222 | 100010040 | 9580.6 | 5000 | 9580.6 | 9580.6 | 9580.6 | 9580.6 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 8178.3 | 8178.3 | 17248 | 0 | PROCESSED | 57526.8981828704 | 54247 | 54118.943125 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000010 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Crab Offset 1 | NULL | N |
| Crab nebula | 83.2708 | 21.9976 | 184.39063256 | -6.07689385 | 86.7331 | 53607.7165162037 | 53607.9167361111 | 100010050 | 9346.9 | 5000 | 9346.9 | 9346.9 | 9346.9 | 9346.9 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 6653 | 6653 | 17287.9 | 0 | PROCESSED | 57526.9 | 54247 | 54122.4223611111 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000010 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Crab Offset 1 | NULL | N |
| Crab nebula | 83.5677 | 22.0135 | 184.52566905 | -5.83608695 | 86.8444 | 53607.9175810185 | 53608.0695023148 | 100010060 | 4877.9 | 5000 | 4877.9 | 4877.9 | 4877.9 | 4877.9 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 5021.7 | 5021.7 | 13076 | 0 | PROCESSED | 57526.9066087963 | 54247 | 54122.4195486111 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000010 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Crab Offset 1 | NULL | N |
| Crab nebula | 83.6922 | 22.0221 | 184.58047361 | -5.73399538 | 86.8671 | 53608.0699768518 | 53608.2084027778 | 100010070 | 4089.9 | 5000 | 4089.9 | 4089.9 | 4089.9 | 4089.9 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 4228.3 | 4228.3 | 11925.9 | 0 | PROCESSED | 57526.9072222222 | 54247 | 54119.0149074074 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000010 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Crab Offset 1 | NULL | N |
| Crab nebula | 83.6222 | 22.1365 | 184.44846107 | -5.72755512 | 86.8666 | 53608.2089236111 | 53608.316087963 | 100010080 | 3382 | 5000 | 3382 | 3382 | 3382 | 3382 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 3700.3 | 3700.3 | 9253.9 | 0 | PROCESSED | 57526.9140856482 | 54247 | 54119.0056134259 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000010 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Crab Offset 1 | NULL | N |
| Crab nebula | 83.5807 | 22.8483 | 183.82410841 | -5.37832099 | 86.8677 | 53608.3175810185 | 53608.5139583333 | 100010090 | 6716 | 5000 | 6716 | 6716 | 6716 | 6716 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 6376.8 | 6376.8 | 16950.1 | 0 | PROCESSED | 57526.9164699074 | 54247 | 54119.0235648148 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000010 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Crab Offset 1 | NULL | N |
| Crab nebula | 83.9887 | 22.0345 | 184.71743044 | -5.49499441 | 86.8666 | 53608.5155902778 | 53608.7153472222 | 100010100 | 9694 | 5000 | 9694 | 9694 | 9694 | 9694 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 7581.2 | 7581.2 | 17247.9 | 0 | PROCESSED | 57526.9259606482 | 54247 | 54122.4242939815 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000010 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Crab Offset 1 | NULL | N |
| Crab nebula | 83.5122 | 24.0135 | 182.80375415 | -4.80497322 | 86.8675 | 53608.7179976852 | 53608.930625 | 100010110 | 9480.5 | 5000 | 9480.5 | 9480.5 | 9480.5 | 9480.5 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 7363 | 7363 | 18336 | 0 | PROCESSED | 57526.9265162037 | 54247 | 54118.98625 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000010 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Crab Offset 1 | NULL | N |
| Crab nebula | 83.6374 | 21.9009 | 184.65605757 | -5.84178049 | 86.8664 | 53608.9333217593 | 53609.069525463 | 100010120 | 4745.6 | 5000 | 4745.6 | 4745.6 | 4745.6 | 4745.6 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 5178.7 | 5178.7 | 11757.9 | 1 | PROCESSED | 57526.9343287037 | 54247 | 54118.9946180556 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000010 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Crab Offset 1 | NULL | N |
| Crab nebula | 83.5044 | 22.0116 | 184.49566519 | -5.88665136 | 86.8658 | 53609.0701388889 | 53609.2014583333 | 100010130 | 4222 | 5000 | 4222 | 4222 | 4222 | 4222 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 4372.4 | 4372.4 | 11335.9 | 0 | PROCESSED | 57526.9346180556 | 54247 | 54119.0454282407 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000010 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Crab Offset 1 | NULL | N |
| Crab nebula | 83.7552 | 22.0249 | 184.60948321 | -5.68314749 | 86.8656 | 53609.2022106482 | 53609.3125810185 | 100010140 | 3419 | 5000 | 3419 | 3419 | 3419 | 3419 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 3755.4 | 3755.4 | 9531.9 | 0 | PROCESSED | 57526.9383217593 | 54247 | 54118.9983796296 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000010 | Crab nebula multi pointings | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Crab Offset 1 | NULL | N |
| Galactic bulge | 236.4313 | -31.7013 | 340.99994533 | 17.99808229 | 283.5446 | 53609.4365856482 | 53611.060625 | 100011010 | 61133 | 70000 | 61133 | 61133 | 61133 | 61133 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 47983.4 | 47983.4 | 140282 | 2 | PROCESSED | 57526.962037037 | 54247 | 54034.8288310185 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000011 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Galactic bulge | NULL | N |
| Eta Carinae | 161.281 | -59.6845 | 287.6040589 | -0.62575348 | 343.8621 | 53611.0750347222 | 53612.0627546296 | 100012010 | 49782 | 40000 | 49790 | 49782 | 49782 | 49798 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 55960.7 | 55960.7 | 85252.9 | 0 | PROCESSED | 57526.9773032407 | 53705 | 53905.4648842593 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000012 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Eta Carinae | NULL | N |
| N103B | 77.2315 | -68.7507 | 279.61119012 | -34.36730962 | 73.8586 | 53612.0740162037 | 53613.0626273148 | 100013010 | 33064.6 | 40000 | 33064.6 | 33064.6 | 33064.6 | 33064.6 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 37281.4 | 37281.4 | 85405.9 | 1 | PROCESSED | 57526.9730324074 | 54247 | 54034.8733449074 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000013 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | N103B | NULL | N |
| E0102-72 | 15.9813 | -72.0378 | 301.56958331 | -45.05740554 | 140.1798 | 53613.0710648148 | 53613.7640509259 | 100014010 | 24333.9 | 20000 | 24333.9 | 24333.9 | 24333.9 | 24333.9 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 24514.4 | 24514.4 | 59863.9 | 2 | PROCESSED | 57511.5174884259 | 53705 | 53905.4615740741 | 3.0.22.43 | 13 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000014 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | XIS monitor with E0102-72 | NULL | N |
| Crab Nebula | 83.6372 | 22.097 | 184.48946706 | -5.73697 | 84.9994 | 53613.8323032407 | 53613.975787037 | 100015010 | 5658.7 | 5000 | 5658.7 | 5658.7 | 5658.7 | 5658.7 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 5790.7 | 5790.7 | 12387.9 | 0 | PROCESSED | 57527.2296412037 | 54247 | 54109.1053240741 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000015 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | HXD boresight check with Crab | NULL | N |
| Crab Nebula | 83.6296 | 22.1792 | 184.41590928 | -5.69889955 | 84.9998 | 53613.9762152778 | 53614.1077314815 | 100015020 | 4950 | 5000 | 4950 | 4950 | 4950 | 4950 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 5117.8 | 5117.8 | 11359.9 | 0 | PROCESSED | 57527.2276388889 | 54247 | 54109.1090972222 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000015 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | HXD boresight check with Crab | NULL | N |
| Crab Nebula | 83.6449 | 22.0152 | 184.56274906 | -5.77473152 | 84.9987 | 53614.1083449074 | 53614.1771759259 | 100015030 | 2100 | 5000 | 2100 | 2100 | 2100 | 2100 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2307.4 | 2307.4 | 5943.9 | 0 | PROCESSED | 57527.235150463 | 54247 | 54109.3966782407 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000015 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | HXD boresight check with Crab | NULL | N |
| Crab Nebula | 83.6442 | 22.0129 | 184.56435264 | -5.77651077 | 84.9978 | 53614.830775463 | 53614.9098263889 | 100015040 | 2978.6 | 5000 | 2978.6 | 2978.6 | 2978.6 | 2978.6 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 3049.3 | 3049.3 | 6807.9 | 0 | PROCESSED | 57527.2502430556 | 54247 | 54109.1815625 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000015 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | HXD boresight check with Crab | NULL | N |
| Crab Nebula | 83.5484 | 22.0881 | 184.45272098 | -5.81121698 | 85.0004 | 53614.9103009259 | 53615.0418518518 | 100015050 | 5344.7 | 5000 | 5344.7 | 5344.7 | 5344.7 | 5344.7 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 5485.9 | 5485.9 | 11356 | 0 | PROCESSED | 57527.2511342593 | 54247 | 54109.1357986111 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000015 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | HXD boresight check with Crab | NULL | N |
| Crab Nebula | 83.727 | 22.1071 | 184.52563634 | -5.6612791 | 84.9996 | 53615.0424652778 | 53615.2432175926 | 100015060 | 6525.6 | 5000 | 6525.6 | 6525.6 | 6525.6 | 6525.6 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 6759.9 | 6759.9 | 17340 | 0 | PROCESSED | 57527.2534490741 | 54247 | 54109.1715393518 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000015 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | HXD boresight check with Crab | NULL | N |
| Cas A | 350.8254 | 58.8156 | 111.72292809 | -2.12474901 | 12.9937 | 53614.2486458333 | 53614.7640509259 | 100016010 | 27965 | 20000 | 27973 | 27973 | 27973 | 27965 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 24130 | 24130 | 44495.9 | 2 | PROCESSED | 57527.2832175926 | 53705 | 53905.4659606482 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000016 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Cas A | NULL | N |
| Vega | 279.2264 | 38.7699 | 67.43212753 | 19.23869014 | 301.7896 | 53615.367349537 | 53615.603587963 | 100017010 | 11398.5 | 10000 | 11406.5 | 11406.5 | 11406.5 | 11398.5 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 11575.1 | 11575.1 | 20403.9 | 0 | PROCESSED | 57527.2607407407 | 54247 | 53906.0764814815 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000017 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | XIS OBF check with Vega | NULL | N |
| NEP | 272.7884 | 65.9814 | 95.75202722 | 28.67554678 | 290.9299 | 53615.6136921296 | 53617.625162037 | 100018010 | 106201.5 | 100000 | 106201.5 | 106217.5 | 106249.5 | 106225.5 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 106125 | 106125 | 173571.8 | 3 | PROCESSED | 57527.2880092593 | 53705 | 53905.4636921296 | 3.0.22.43 | 6 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000018 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | HXD background at North Ecliptic Pole | NULL | N |
| SN1006 NE BG | 226.7036 | -41.3998 | 328.51405135 | 14.65073262 | 293.6503 | 53617.7018865741 | 53622.1668287037 | 100019010 | 44750.3 | 50000 | 44754.3 | 44754.3 | 44754.3 | 44750.3 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 37388.3 | 37388.3 | 385601.8 | 5 | PROCESSED | 57527.2923148148 | 54247 | 54035.4224768518 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000019 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | SN1006 observation with XIS and HXD | NULL | N |
| SN1006 NE-Rim | 225.9645 | -41.7797 | 327.82254414 | 14.6038019 | 294.6606 | 53622.1683217593 | 53623.5835532407 | 100019020 | 42844.2 | 50000 | 42844.2 | 42852.6 | 42852.2 | 42848.2 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 37615.6 | 37615.6 | 122196 | 7 | PROCESSED | 57527.2923611111 | 54247 | 54034.9646875 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000019 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | SN1006 observation with XIS and HXD | NULL | N |
| SN1006 SW-Rim | 225.5051 | -42.0698 | 327.36692545 | 14.52303039 | 297.2712 | 53623.5862962963 | 53624.993287037 | 100019030 | 28524.5 | 50000 | 28532.5 | 28524.5 | 28540.9 | 28540.5 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 27008.2 | 27008.2 | 121551.9 | 5 | PROCESSED | 57527.3126967593 | 54247 | 54034.9697453704 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000019 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | SN1006 observation with XIS and HXD | NULL | N |
| SN1006 SW BG | 224.655 | -42.4005 | 326.632731 | 14.54333558 | 310.4886 | 53624.9999189815 | 53626.0071643518 | 100019040 | 32333.4 | 50000 | 32333.4 | 32349.4 | 32341.4 | 32341.4 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 24673.6 | 24673.6 | 87015.9 | 5 | PROCESSED | 57527.3647453704 | 54247 | 54035.4482638889 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000019 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | SN1006 observation with XIS and HXD | NULL | N |
| SN 1006 SW-Rim | 225.4961 | -42.0706 | 327.36052248 | 14.52564865 | 117.2713 | 53761.0914930556 | 53761.7155555556 | 100019050 | 28418.6 | 50000 | 28418.6 | 28418.6 | 28418.6 | 28418.6 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 24744.4 | 24744.4 | 53910 | 0 | PROCESSED | 57532.7834375 | 54247 | 54040.4586689815 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000019 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | SN1006 observation with XIS and HXD | XIS | N |
| SN1006 SW BG | 224.6468 | -42.4025 | 326.62625739 | 14.54451897 | 100.3489 | 53761.7199652778 | 53762.4752777778 | 100019060 | 27981.3 | 50000 | 27981.3 | 27989.3 | 27997.3 | 27997.3 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 29550.4 | 29550.4 | 65249.9 | 2 | PROCESSED | 57532.7989814815 | 54247 | 54040.5663541667 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000019 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | SN1006 observation with XIS and HXD | XIS | N |
| Fornax Cluster | 54.6395 | -35.4918 | 236.7850293 | -53.61976834 | 103.5002 | 53626.0756018518 | 53627.5002662037 | 100020010 | 76078.2 | 100000 | 76078.2 | 76078.2 | 76078.2 | 76078.2 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 71112.8 | 71112.8 | 123063.9 | 3 | PROCESSED | 57527.3377430556 | 54247 | 54035.4442013889 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000020 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Fornax Cluster | NULL | N |
| A0535+026 | 84.7243 | 26.3189 | 181.44092218 | -2.64422146 | 83.608 | 53627.5694907407 | 53628.0418865741 | 100021010 | 21761 | 20000 | 21761 | 21761 | 21761 | 21761 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 21257.2 | 21257.2 | 40783.9 | 1 | PROCESSED | 57527.3122337963 | 54247 | 54035.0644444444 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000021 | We propose to observe the X-ray binary pulsar A0535+26. The main objectives is measuring changes in the cyclotron resonance energy in an outburst decay.It is known from another X-ray pulsar 4U0115+63 that the cyclotron resonance energy increased from 11 keV to 16 keV, as the luminosity decreased across a threshold luminosity of 4x10^37 erg/s. The flare of A0535+26 is a chance to know whether this behavior is the RULE among binary pulsars or an EXCEPTION. A0535+26 is fading down and will reach 30mCrab (5-100keV) on September 17, which is 5x10^36 erg/s. It is better to be observed as soon as possible, before it fades out. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | TOO Observation of A0535+026 | NULL | N |
| Crab Nebula | 83.6622 | 21.1838 | 185.27784655 | -6.20565133 | 88.1125 | 53628.0468055556 | 53628.2988194444 | 100022010 | 12881 | 10000 | 12881 | 12881 | 12881 | 12881 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 12241 | 12241 | 21767.9 | 0 | PROCESSED | 57527.323275463 | 54247 | 54109.2599768518 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000022 | Crab at 50arcmin off from the XIS aimpoint to study stray light. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Crab at 50 arcmin off | NULL | N |
| Crab Nebula | 82.7325 | 21.9883 | 184.12771921 | -6.50224239 | 88.0978 | 53628.3006828704 | 53628.5835416667 | 100022020 | 10919.8 | 10000 | 10919.8 | 10919.8 | 10919.8 | 10919.8 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 6340.1 | 6340.1 | 24400 | 2 | PROCESSED | 57527.3262615741 | 54247 | 54109.1486342593 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000022 | Crab at 50arcmin off from the XIS aimpoint to study stray light. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Crab at 50 arcmin off | NULL | N |
| Crab Nebula | 84.5289 | 22.0469 | 184.974122 | -5.06424795 | 87.5879 | 53629.0921759259 | 53629.368275463 | 100022030 | 12824.4 | 10000 | 12840.4 | 12832.4 | 12824.4 | 12848.4 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 10351.8 | 10351.8 | 23824 | 1 | PROCESSED | 57527.3478009259 | 54247 | 54109.1621527778 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000022 | Crab at 50arcmin off from the XIS aimpoint to study stray light. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Crab at 50 arcmin off | NULL | N |
| Crab Nebula | 83.6282 | 22.0761 | 184.5027205 | -5.75520363 | 87.79 | 53628.5852199074 | 53628.8265393518 | 100023010 | 11997.8 | 10000 | 11997.8 | 11997.8 | 11997.8 | 11997.8 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 10513.2 | 10513.2 | 20823.9 | 0 | PROCESSED | 57527.3355902778 | 54247 | 54109.2268287037 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000023 | Calibration of detector response at both of XIS/HXD nominal positions, together with an absolute flux confirmation with differnt hit-pattern widths. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Crab at nominal positions | NULL | N |
| Crab Nebula | 83.6309 | 22.0151 | 184.55585082 | -5.78574816 | 87.8466 | 53628.8269212963 | 53629.0904976852 | 100023020 | 12527.1 | 10000 | 12531.1 | 12527.1 | 12536.4 | 12535.1 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 13352.9 | 13352.9 | 22764 | 1 | PROCESSED | 57527.3409143518 | 54247 | 54109.193599537 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000023 | Calibration of detector response at both of XIS/HXD nominal positions, together with an absolute flux confirmation with differnt hit-pattern widths. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Crab at nominal positions | NULL | N |
| NGC 2110 | 88.0444 | -7.458 | 212.92660512 | -16.54877043 | 103.4188 | 53629.3796296296 | 53631.8308333333 | 100024010 | 101748.7 | 100000 | 101926.5 | 103760.1 | 101748.7 | 102148.3 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 86043.3 | 86043.3 | 211755.8 | 4 | PROCESSED | 57527.4030324074 | 54247 | 54035.4624189815 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000024 | The Narrow Emission Line Galaxy NGC 2110 was the brightest AGN in the initial BAT survey release (BAT flux of 2.1E-10 erg/cm2/sec) visible to Suzaku during Sept./Oct., and is still currently bright in BAT. A 2003 RXTE observation yielded F_2-10 keV = 4E-11 erg/cm2/sec. The source is currently almost 3 times brighter than during the SAX observations. The main goals are to measure the high energy cutoff and to place a strong limit on the presence of reflection. The Compton reflection hump is weak in SAX data (suggesting that the Fe K line originates in Compton-thin material). Determining the strength of the reflection component is critical for constraining the geometry of the accreting material. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Narrow Emission Line Galaxy NGC 2110 | NULL | N |
| BD +30 3639 | 293.6887 | 30.5051 | 64.77556877 | 5.01383279 | 277.8713 | 53634.3814930556 | 53635.2473842593 | 100025010 | 35214.6 | 40000 | 35230.6 | 35230.6 | 35214.6 | 35222.6 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 33372.8 | 33372.8 | 74803.9 | 1 | PROCESSED | 57527.3931597222 | 54247 | 54035.4664583333 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000025 | The proposed target, BD +30 3639, is a prototypical planetary nebula which emit diffuse X-rays; planetary nebulae represent the final evolutionary stage of low mass stars, and contain very rich information on the stellar nucleosynthesis. The Chandra ACIS spectrum of BD +30 3639 bears an amazingly strong Ne-K line, most certainly because the X-ray emitting material directly reflect the "onion-like structure" of elements insied evolved stars. However, the ACIS was not able to resolve C, N, O lines, which are of vital importance. The XMM RGS and Chandra LETG could do, but we need very long exposure. Using the Suzaku XIS-BI with the excellent low-energy performance, we can for the first time measure the C/N/O/Mg abundance ratios of this important object in a short time. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Observation of planetary nebula BD +30 3639 | NULL | N |
| BD +30 3639 | 293.6993 | 30.5065 | 64.78119899 | 5.00649051 | 237.7342 | 53676.9934837963 | 53677.8230324074 | 100025020 | 31138.4 | 40000 | 31138.4 | 31162.4 | 31146.4 | 31154.4 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 27125.8 | 27125.8 | 71638 | 1 | PROCESSED | 57527.9315509259 | 54247 | 54037.1080902778 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000025 | The proposed target, BD +30 3639, is a prototypical planetary nebula which emit diffuse X-rays; planetary nebulae represent the final evolutionary stage of low mass stars, and contain very rich information on the stellar nucleosynthesis. The Chandra ACIS spectrum of BD +30 3639 bears an amazingly strong Ne-K line, most certainly because the X-ray emitting material directly reflect the "onion-like structure" of elements insied evolved stars. However, the ACIS was not able to resolve C, N, O lines, which are of vital importance. The XMM RGS and Chandra LETG could do, but we need very long exposure. Using the Suzaku XIS-BI with the excellent low-energy performance, we can for the first time measure the C/N/O/Mg abundance ratios of this important object in a short time. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Observation of planetary nebula BD +30 3639 | NULL | N |
| RXJ1713.7-3946 | 258.074 | -39.935 | 347.05133682 | -0.37925502 | 269.9977 | 53639.6563194444 | 53641.2960648148 | 100026010 | 68495.9 | 80000 | 68495.9 | 68565.3 | 68511.9 | 68525.3 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 56238.2 | 56238.2 | 141661.9 | 0 | PROCESSED | 57527.4561921296 | 54247 | 54037.0750694445 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000026 | RXJ1713 is very important sources in which we can study particle accelerator in the universe. X-ray synchrotron spectrum suggest the existence of distribution of high energy electron. Very similar TeV and ASCA morphologies show close connection between these energy bands. The interaction with molecular cloud suggests that proton accelerator resides in this object. The photon index of RXJ1713 seems to be difficult in the frame work of standard diffusive shock scenario. To obtain precise spectrum in the hard X-ray region is therefore very important to determine the energy cut off and to study the mechanism that produce such high energy electrons. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Observation of RXJ1713.7-3946 | NULL | N |
| RXJ1713-3946-BKGD1 | 257.3853 | -38.8228 | 347.63223985 | 0.70836337 | 270.0091 | 53638.7997685185 | 53639.6542708333 | 100026020 | 34928.4 | 40000 | 34928.4 | 34928.4 | 34928.4 | 34928.4 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 28371.3 | 28371.3 | 73819.9 | 0 | PROCESSED | 57527.432349537 | 54247 | 54035.5347453704 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000026 | RXJ1713 is very important sources in which we can study particle accelerator in the universe. X-ray synchrotron spectrum suggest the existence of distribution of high energy electron. Very similar TeV and ASCA morphologies show close connection between these energy bands. The interaction with molecular cloud suggests that proton accelerator resides in this object. The photon index of RXJ1713 seems to be difficult in the frame work of standard diffusive shock scenario. To obtain precise spectrum in the hard X-ray region is therefore very important to determine the energy cut off and to study the mechanism that produce such high energy electrons. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Observation of RXJ1713.7-3946 | NULL | N |
| RXJ1713-3946-BKGD2 | 257.2742 | -41.0338 | 345.80577047 | -0.54060643 | 270.0033 | 53641.2980671296 | 53642.1843055556 | 100026030 | 37513.2 | 40000 | 37537.2 | 37529.2 | 37513.2 | 37513.2 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 31898.2 | 31898.2 | 76565.9 | 0 | PROCESSED | 57527.4461574074 | 54247 | 54035.6187268518 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000026 | RXJ1713 is very important sources in which we can study particle accelerator in the universe. X-ray synchrotron spectrum suggest the existence of distribution of high energy electron. Very similar TeV and ASCA morphologies show close connection between these energy bands. The interaction with molecular cloud suggests that proton accelerator resides in this object. The photon index of RXJ1713 seems to be difficult in the frame work of standard diffusive shock scenario. To obtain precise spectrum in the hard X-ray region is therefore very important to determine the energy cut off and to study the mechanism that produce such high energy electrons. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Observation of RXJ1713.7-3946 | NULL | N |
| Sgr_A_East | 266.5146 | -28.9267 | 0.05802898 | -0.07696746 | 264.7152 | 53636.3044560185 | 53637.462025463 | 100027010 | 44785 | 50000 | 44801 | 44852.3 | 44785 | 44828.3 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 37854.3 | 37854.3 | 100013.9 | 1 | PROCESSED | 57527.4188657407 | 54247 | 54035.502662037 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000027 | We propose to obtain high quality spectra from 6 positions near the GC. The objective is to resolve 6.4 , 6.7 and 6.9 keV line and determine the high energy tail from each positions and/or from the sub-structures in each position. Combining all the results, we can see which sub-sub-structure is X-ray reflection from Sgr A* ( 6.4 keV line+ 7.1 keV edge + high energy tail), thermal plasma (6.7+6.9 keV lines, with no hard X-ray tail), non thermal emission (e.g. line but hard X-ray tail). Unexpected spectral feature could be also found, depending on the real origin. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Suzaku Observation of Galactic Center Region | NULL | N |
| Sgr_A_west | 266.3057 | -29.1697 | 359.75546849 | -0.04768885 | 264.9601 | 53637.5953356482 | 53638.7273032407 | 100027020 | 42814.8 | 50000 | 42814.8 | 42814.8 | 42814.8 | 42814.8 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 36091 | 36091 | 97800 | 0 | PROCESSED | 57527.4293865741 | 54247 | 54035.5135532407 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000027 | We propose to obtain high quality spectra from 6 positions near the GC. The objective is to resolve 6.4 , 6.7 and 6.9 keV line and determine the high energy tail from each positions and/or from the sub-structures in each position. Combining all the results, we can see which sub-sub-structure is X-ray reflection from Sgr A* ( 6.4 keV line+ 7.1 keV edge + high energy tail), thermal plasma (6.7+6.9 keV lines, with no hard X-ray tail), non thermal emission (e.g. line but hard X-ray tail). Unexpected spectral feature could be also found, depending on the real origin. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Suzaku Observation of Galactic Center Region | NULL | N |
| 1A1742-294(GC_BGD_1) | 266.5264 | -29.516 | 359.56008755 | -0.392308 | 264.8664 | 53637.463287037 | 53637.527962963 | 100027030 | 2066.3 | 5000 | 2066.3 | 2066.3 | 2066.3 | 2066.3 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 1887.7 | 1887.7 | 5584 | 0 | PROCESSED | 57527.4000462963 | 54247 | 54035.4639583333 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000027 | We propose to obtain high quality spectra from 6 positions near the GC. The objective is to resolve 6.4 , 6.7 and 6.9 keV line and determine the high energy tail from each positions and/or from the sub-structures in each position. Combining all the results, we can see which sub-sub-structure is X-ray reflection from Sgr A* ( 6.4 keV line+ 7.1 keV edge + high energy tail), thermal plasma (6.7+6.9 keV lines, with no hard X-ray tail), non thermal emission (e.g. line but hard X-ray tail). Unexpected spectral feature could be also found, depending on the real origin. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Suzaku Observation of Galactic Center Region | NULL | N |
| KS1741-293(GC_BGD_2) | 266.2069 | -29.3515 | 359.55541243 | -0.06909433 | 265.0174 | 53637.5288541667 | 53637.5946296296 | 100027040 | 1937 | 5000 | 1937 | 1937 | 1937 | 1937 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 1763.7 | 1763.7 | 5680 | 0 | PROCESSED | 57527.404525463 | 54247 | 53907.393275463 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000027 | We propose to obtain high quality spectra from 6 positions near the GC. The objective is to resolve 6.4 , 6.7 and 6.9 keV line and determine the high energy tail from each positions and/or from the sub-structures in each position. Combining all the results, we can see which sub-sub-structure is X-ray reflection from Sgr A* ( 6.4 keV line+ 7.1 keV edge + high energy tail), thermal plasma (6.7+6.9 keV lines, with no hard X-ray tail), non thermal emission (e.g. line but hard X-ray tail). Unexpected spectral feature could be also found, depending on the real origin. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Suzaku Observation of Galactic Center Region | NULL | N |
| 1E1743.1-2843(GC_BGD_3) | 266.592 | -28.6516 | 0.32828705 | 0.00813221 | 264.88 | 53638.7286111111 | 53638.793275463 | 100027050 | 1984.6 | 5000 | 1984.6 | 1984.6 | 1984.6 | 1984.6 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 1793.4 | 1793.4 | 5567.9 | 0 | PROCESSED | 57527.4093055556 | 54247 | 53905.6343055556 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000027 | We propose to obtain high quality spectra from 6 positions near the GC. The objective is to resolve 6.4 , 6.7 and 6.9 keV line and determine the high energy tail from each positions and/or from the sub-structures in each position. Combining all the results, we can see which sub-sub-structure is X-ray reflection from Sgr A* ( 6.4 keV line+ 7.1 keV edge + high energy tail), thermal plasma (6.7+6.9 keV lines, with no hard X-ray tail), non thermal emission (e.g. line but hard X-ray tail). Unexpected spectral feature could be also found, depending on the real origin. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Suzaku Observation of Galactic Center Region | NULL | N |
| HESS J1616-508 | 244.1248 | -50.8971 | 332.40352084 | -0.15000913 | 282.8476 | 53632.5000231482 | 53633.8183333333 | 100028010 | 41352 | 50000 | 41352 | 41376 | 41352 | 41368 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 35373.1 | 35373.1 | 113889.9 | 0 | PROCESSED | 57527.3838194444 | 54247 | 54035.4361111111 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000028 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | New HESS sources and the Galactic ridge Background | NULL | N |
| HESS J1616-508_BGD1 | 243.666 | -51.1742 | 332.00349288 | -0.15039556 | 283.0062 | 53631.9497222222 | 53632.4990856482 | 100028020 | 19327.7 | 25000 | 19327.7 | 20630 | 19360 | 19632.3 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 16642.6 | 16642.6 | 47447.9 | 0 | PROCESSED | 57527.3573148148 | 54247 | 54035.1692476852 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000028 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | New HESS sources and the Galactic ridge Background | NULL | N |
| HESS J1616-508_BGD2 | 244.4656 | -50.6883 | 332.70353325 | -0.14997577 | 283.1793 | 53633.8196412037 | 53634.3120833333 | 100028030 | 21873.5 | 25000 | 21889.5 | 21889.5 | 21881.5 | 21873.5 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 18206.3 | 18206.3 | 42535.9 | 0 | PROCESSED | 57527.3722800926 | 54247 | 54035.4698842593 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000028 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | New HESS sources and the Galactic ridge Background | NULL | N |
| GRO J1655-40 | 253.5027 | -39.8455 | 344.98315976 | 2.45489032 | 268.0237 | 53635.3140625 | 53636.2968055556 | 100029010 | 35222.8 | 40000 | 0 | 35233.6 | 35222.8 | 35230.8 | 0 | 1 | 2 | 2 | 1 | 0 | 0 | 28731.5 | 28731.5 | 84901.9 | 1 | PROCESSED | 57527.3997337963 | 54247 | 54035.4940625 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000029 | We propose to observe GRO J1655-40, a transient galactic black hole candidate. With M=~7 Msolar and distinct radio lobes, GRO J1655-40 has been classified as a microquasar. It was highly variable during the first few years after its discovery while showing irregular flaring and a wide range of continuum states. Discrete Fe K absorption structure was observed with ASCA. In the summer of 1997 it entered an extended quiescence that lasted for ~8 years. In March 2005 it became active again and XMM & Chandra have observed it since. Only Suzaku can provide the broadband sensitivity required to map the Fe K structure and the continuum as they change. GRO J1655-40 is rapidly declining and must be observed soon before it reenters quiescence. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | GRO J1655-40 | NULL | N |
| A 2218 | 249.0001 | 66.203 | 97.724401 | 38.11892096 | 242.3617 | 53644.3643402778 | 53645.3446643518 | 100030010 | 43362.9 | 50000 | 43362.9 | 44717.3 | 43425.3 | 43824.8 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 41491.8 | 41491.8 | 84678 | 1 | PROCESSED | 57527.4791898148 | 54247 | 54035.7677314815 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000030 | Search of redshifted (z=0.171) OVII emission line from warm-hot intergalactic matter around a cluster which shows a merger feature in the line of sight, with no central cool component. The depth of the structure can be ~20 Mpc, and the redshift allows a clear separation of the lines from the Galactic hot gas. The low background and the superior resolution of XIS in the soft X-ray energy range will allow the best measurement of the WHIM emission so far. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | A2218 and its offset observation | NULL | N |
| A2218_offset | 244.4769 | 65.4468 | 97.72059475 | 40.11912915 | 237.1965 | 53645.3474537037 | 53646.32375 | 100030020 | 44859.2 | 50000 | 44859.2 | 46190.7 | 44914.1 | 45374.7 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 42536.6 | 42536.6 | 84343.9 | 0 | PROCESSED | 57527.5203125 | 54247 | 54036.969224537 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000030 | Search of redshifted (z=0.171) OVII emission line from warm-hot intergalactic matter around a cluster which shows a merger feature in the line of sight, with no central cool component. The depth of the structure can be ~20 Mpc, and the redshift allows a clear separation of the lines from the Galactic hot gas. The low background and the superior resolution of XIS in the soft X-ray energy range will allow the best measurement of the WHIM emission so far. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | A2218 and its offset observation | NULL | N |
| NGC3516 | 166.7299 | 72.5779 | 133.2179652 | 42.40001774 | 148.9366 | 53655.5813541667 | 53658.3801388889 | 100031010 | 134469.6 | 150000 | 134509.6 | 134595.6 | 134509.6 | 134469.6 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 122818 | 122818 | 241684.8 | 0 | PROCESSED | 57527.6243634259 | 54247 | 54036.4704976852 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000031 | NGC 3516 is one of the brightest Seyfert 1s seen in BAT currently visible to Suzaku. Recent BAT and RXTE observations show that this source is ~2-3 mCrb in the 2-10 keV band and ~4-5 mCrb in 15-100 keV. NGC 3516 is currently much brighter than when XMM observed it in 2000 (e.g., it has since returned to "typical" flux). This source's Fe K line and Compton reflection hump are both quite strong (e.g., as seen with SAX; R is ~1.8 in SAX data). | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | NGC 3516 | NULL | N |
| ULXs in NGC 1313 | 49.5245 | -66.5352 | 283.41323765 | -44.63106544 | 172.6337 | 53658.556400463 | 53659.6252777778 | 100032010 | 32878 | 40000 | 32878 | 32878 | 32878 | 32878 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 30380 | 30380 | 92343.9 | 1 | PROCESSED | 57527.587349537 | 54247 | 54036.1929398148 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000032 | We propose Suzaku observation of a nearby (4.5 Mpc) galaxy NGC 1313 hosting two prototypical ULXs. These ASCA specta of many ULXs were described with a "high temperature diskbb" model, spectra obtained with XMM (and Chandra) prefer a "power-law plus low-temperature disk" modeling. The superior 5-10 keV sensitivity of Suzaku allows us to examine whether the spectra of luminous ULXs indeed exhibit a turn-over around 5 keV or extend up to 10 keV. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | ULXs in NGC 1313 | NULL | N |
| M82-Wind | 148.8893 | 69.7655 | 141.33880284 | 40.49464345 | 137.7608 | 53647.5072800926 | 53648.1418287037 | 100033010 | 32327.4 | 100000 | 32327.4 | 32327.4 | 32327.4 | 32327.4 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 30222.4 | 30222.4 | 54802.1 | 0 | PROCESSED | 57527.5155092593 | 54247 | 54037.0057175926 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000033 | We propose to observe the largely extened emission with the size of about 12kpc around M82 with Suzaku for 100ksec. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Largely Extended Emission (~12kpc) around M82 | NULL | N |
| M82-Wind | 148.894 | 69.7643 | 141.33883884 | 40.49666381 | 146.246 | 53662.0401273148 | 53662.9390393518 | 100033020 | 40358.6 | 100000 | 40358.6 | 40382.6 | 40358.6 | 40366.6 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 38353.3 | 38353.3 | 77658 | 0 | PROCESSED | 57527.6127546296 | 54247 | 54036.4196296296 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000033 | We propose to observe the largely extened emission with the size of about 12kpc around M82 with Suzaku for 100ksec. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Largely Extended Emission (~12kpc) around M82 | NULL | N |
| M82-Wind | 148.8885 | 69.7652 | 141.33933547 | 40.4945935 | 137.7608 | 53670.4681134259 | 53671.1002199074 | 100033030 | 28363.8 | 100000 | 28379.8 | 28379.8 | 28371.8 | 28363.8 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 25812.1 | 25812.1 | 54604 | 1 | PROCESSED | 57527.6784606482 | 54247 | 54036.8639467593 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000033 | We propose to observe the largely extened emission with the size of about 12kpc around M82 with Suzaku for 100ksec. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Largely Extended Emission (~12kpc) around M82 | NULL | N |
| A 3376 | 90.5561 | -39.9584 | 246.50686261 | -25.98989573 | 107.6124 | 53649.6153703704 | 53653.4495833333 | 100034010 | 118779.2 | 150000 | 118779.2 | 121737.3 | 118849.8 | 119335.7 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 100540.1 | 100540.1 | 331253.7 | 3 | PROCESSED | 57527.6218171296 | 54247 | 54109.6396990741 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000034 | Abell 3376 (z=0.046) is a merging cluster with a T=4 keV (*3) hosting a pair of strong radio halos (see figure). It is one of the few clusters from which BeppoSAX positively detected excess hard X-rays (Nevalainen et al. ApJ 608, 166, 2004). Because of the relatively low temperature, the HXD-PIN energy band is expected to be relatively free from thermal emission, making this object ideal to the search for non-thermal signals. We expect the non-thermal flux to be 4-5% of the PIN background at 20 keV, and a 150 ksec on-source exposure would be needed to securely detect this. To know the current background over the full COR range, an off-source exposure for one day or a ~40 ksec exposure onto a very soft source, would be required immediately before or after the on-source data acquisition. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Diffuse Hard X-rays from Clusters | NULL | N |
| Her X-1 | 254.465 | 35.3306 | 58.13562438 | 37.51514805 | 249.5714 | 53648.6450462963 | 53649.4341898148 | 100035010 | 36123.5 | 40000 | 36923.5 | 36123.5 | 36923.5 | 36923.5 | 2 | 1 | 2 | 2 | 1 | 0 | 0 | 33322.9 | 33322.9 | 68178 | 0 | PROCESSED | 57527.5593518518 | 54247 | 54036.0084375 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000035 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | HXD Performance Verification using Her X-1 | NULL | N |
| CYG X-1 | 299.5907 | 35.1892 | 71.32454904 | 3.06010347 | 276.9898 | 53648.2025347222 | 53648.6335532407 | 100036010 | 18213 | 20000 | 18213 | 18213 | 18213 | 18213 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 18145.7 | 18145.7 | 37229.9 | 0 | PROCESSED | 57527.5598726852 | 54247 | 54037.7278819444 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000036 | We propose to probe the geometry of optically-thick accretion disks which should exist around a BH even in the hard state and to verify the HXD performance to thermal cut-off in hard X-rays expected from AGN. The 1st may be done by measuring the cool disk emission with the XIS-BI, resolving the fluorescent Fe-K line with the XIS-FI and detecting the reflection continuum with the HXD. Since these features are thought to come from the optically-thick disk a simultaneous measurement will for the 1st time allow for self-consistent constraining of the disk geometry in the hard state. Cyg X-1 is the best & most secure object for this stufy and is now in the low/hard state. A 20 ks Suzaku obs. is sufficient to get a fine spectrum up to 300 keV & to determine the cutoff with a high significance. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Cyg X-1 in the low state | NULL | N |
| Sgr_A_west | 266.3063 | -29.1685 | 359.75676556 | -0.04750971 | 264.9604 | 53642.1914467593 | 53643.187025463 | 100037010 | 43741.2 | 50000 | 43741.2 | 43749.2 | 43749.2 | 43749.2 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 39394.1 | 39394.1 | 86013.9 | 0 | PROCESSED | 57527.4581828704 | 54247 | 54035.6663310185 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000037 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Suzaku Obseration of Galactic Center region 2 | NULL | N |
| 1A1742-294(GCBGD1) | 266.5239 | -29.5135 | 359.5610912 | -0.38914955 | 264.8673 | 53643.1880092593 | 53643.2536921296 | 100037020 | 3273 | 5000 | 3281 | 3273 | 3288.7 | 3281 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 3091.1 | 3091.1 | 5671.9 | 0 | PROCESSED | 57527.4425347222 | 54247 | 54035.5547453704 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000037 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Suzaku Obseration of Galactic Center region 2 | NULL | N |
| KS1741-293(GCBGD2) | 266.2067 | -29.3539 | 359.55327497 | -0.0701996 | 265.0162 | 53643.254537037 | 53643.3203703704 | 100037030 | 2970 | 5000 | 2994 | 2986 | 2978 | 2970 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 2824.4 | 2824.4 | 5679.9 | 0 | PROCESSED | 57527.4480439815 | 54247 | 54035.7774189815 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000037 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Suzaku Obseration of Galactic Center region 2 | NULL | N |
| Sgr_A_East | 266.5133 | -28.9266 | 0.05752244 | -0.07594372 | 264.7159 | 53643.3215393518 | 53644.2648611111 | 100037040 | 42917.6 | 50000 | 42957.6 | 42961.6 | 42917.6 | 42939.2 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 39453.3 | 39453.3 | 81494 | 1 | PROCESSED | 57527.4753356482 | 54247 | 54035.7619675926 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000037 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Suzaku Obseration of Galactic Center region 2 | NULL | N |
| 1E1743.1-2843 GCBGD3 | 266.5944 | -28.6526 | 0.32852719 | 0.00581314 | 264.8798 | 53644.2657523148 | 53644.3162268518 | 100037050 | 2400 | 5000 | 2400 | 2400 | 2400 | 2400 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 2232.9 | 2232.9 | 4353.9 | 0 | PROCESSED | 57527.4530902778 | 54247 | 54056.1970833333 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000037 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Suzaku Obseration of Galactic Center region 2 | NULL | N |
| Sgr_B2 | 266.8775 | -28.4435 | 0.63628385 | -0.09835114 | 265.3727 | 53653.5194560185 | 53655.2954050926 | 100037060 | 76596.6 | 100000 | 76628.6 | 76644.6 | 76596.6 | 76628.6 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 70819.2 | 70819.2 | 153431.9 | 0 | PROCESSED | 57527.5776041667 | 54247 | 54036.2262731482 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000037 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Suzaku Obseration of Galactic Center region 2 | NULL | N |
| Sgr_B2_BGD | 267.0943 | -28.1356 | 0.99854005 | -0.10262599 | 269.0208 | 53655.2988888889 | 53655.4620833333 | 100037070 | 9161.2 | 10000 | 9161.2 | 9164.3 | 9164.3 | 9163.2 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 9536.4 | 9536.4 | 14092 | 0 | PROCESSED | 57527.5688078704 | 54247 | 54036.0749884259 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000037 | NULL | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Suzaku Obseration of Galactic Center region 2 | NULL | N |
| NORTH POLAR SPUR | 260.5905 | 4.7489 | 26.83412197 | 21.95376599 | 264.1143 | 53646.4785763889 | 53647.4515277778 | 100038010 | 43068.9 | 50000 | 43148.9 | 44212.9 | 43068.9 | 43292.9 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 40771.5 | 40771.5 | 84001.9 | 0 | PROCESSED | 57527.5342824074 | 54247 | 54035.8928009259 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000038 | We propose to observe the North Polar Spur for 100 ksec. The main objectives are below (1) Search for emission lines of N and C that originates from low kT emission (2) Precisely determine the abundance of the NPS The measurement of N and C lines will be the first for XIS. This is also the first for extended sources. The first trial to measure the emission from the C-band (below 0.3keV) by using BI. This will be a guide line how to use the C-band data. Since the C-band intensity is already known, this will be the first calibration of the BI at low energy. The scientific objectives are already given in the mail distributed in the swg. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | North Polar Spur | NULL | N |
| GRS1915+105 | 288.8014 | 10.9368 | 45.35928754 | -0.22611181 | 260.5762 | 53659.6951967593 | 53661.9724305556 | 100039010 | 84777.7 | 80000 | 85063.1 | 86430.5 | 85071.1 | 84777.7 | 3 | 3 | 3 | 3 | 1 | 0 | 0 | 68862.3 | 68862.3 | 196733.8 | 2 | PROCESSED | 57527.9188541667 | 54247 | 54043.8117476852 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000039 | This observation will be performed as a part of the big multiwavelength campain including Suzaku, VLA, Integral, RXTE, and Spitzer. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | Campaign of coordinated observation of GRS 1915+105 | NULL | N |
| MKN 3 | 93.8839 | 71.0477 | 143.2836301 | 22.71631463 | 71.8326 | 53665.0848263889 | 53667.2682175926 | 100040010 | 95026.5 | 100000 | 95026.5 | 95077.2 | 95045.2 | 95034.5 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 91344.1 | 91344.1 | 188629.9 | 0 | PROCESSED | 57527.6643055556 | 54247 | 53906.4896759259 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000040 | Mkn 3 is the second brightest Compton-thick Sy 2 currently visible with Suzaku. The broadband spectrum of Mkn 3, as probed by previous SAX and Chandra observations, is dominated by a reflection component (Compton hump strength R is near 1), but there is also evidence for a strongly absorbed hard X-ray power law that may be direct emission from the obscured nucleus, filtering through Compton-thick material (such as the molecular torus). | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | MKN 3 | HXD | N |
| RXJ1856.5-3754 | 284.1498 | -37.9103 | 358.59888263 | -17.21635309 | 269.4259 | 53667.2829976852 | 53669.4793287037 | 100041010 | 76254.8 | 80000 | 0 | 76254.8 | 0 | 0 | 0 | 2 | 0 | 0 | 1 | 0 | 0 | 62621.7 | 62621.7 | 189720 | 3 | PROCESSED | 57527.6811111111 | 54247 | 54037.2294791667 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000041 | We propose Suzaku observation of a nearby isolated neuron star RXJ1856.5-3754 for the low energy QE calibration of the XIS. Our main purpose is, however, using this source as a soft X-ray QE calibrator on the sky. We hope this source will be observed again in future to check possible contamination on the filter surface etc. Note that the calibration is not only for the BI-CCD(XIS1), but also for FI-CCDs or relative QE among them. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | LOW ENERGY QE CALIBRATION OF XIS | XIS | N |
| RXJ1856.5-3754 | 284.1433 | -37.91 | 358.59722216 | -17.21146697 | 84.0127 | 53817.9388078704 | 53819.4433217593 | 100041020 | 79169 | 80000 | 79177 | 79169 | 79177 | 79177 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 53209.9 | 53209.9 | 129975.9 | 1 | PROCESSED | 57533.3325231482 | 54247 | 54042.2967824074 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000041 | We propose Suzaku observation of a nearby isolated neuron star RXJ1856.5-3754 for the low energy QE calibration of the XIS. Our main purpose is, however, using this source as a soft X-ray QE calibrator on the sky. We hope this source will be observed again in future to check possible contamination on the filter surface etc. Note that the calibration is not only for the BI-CCD(XIS1), but also for FI-CCDs or relative QE among them. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | LOW ENERGY QE CALIBRATION OF XIS | XIS | N |
| CAS A | 350.8729 | 58.8094 | 111.74406014 | -2.13880346 | 214.7372 | 53768.5363657407 | 53768.833599537 | 100043010 | 0 | 10000 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1 | 0 | 0 | 10326.8 | 10326.8 | 25673.9 | 1 | PROCESSED | 57532.8451736111 | 54247 | 54040.7488888889 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001097 | We propose the calibration observations for XIS: E0102-72 ... Gain and QE in the low energy band Cas A ... Gain and QE in the high energy band Eta Carinae ... Contamination of the BI chip | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 0 | SWG | XIS FLIGHT CAIBRATION PLAN | XIS | N |
| CAS A | 350.8761 | 58.8091 | 111.74552355 | -2.13963884 | 214.5537 | 53783.6003472222 | 53783.9218055556 | 100043020 | 14155 | 10000 | 14155 | 14155 | 14155 | 14155 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 17371.3 | 17371.3 | 27768 | 0 | PROCESSED | 57533.0311805556 | 54247 | 54041.4627893518 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001097 | We propose the calibration observations for XIS: E0102-72 ... Gain and QE in the low energy band Cas A ... Gain and QE in the high energy band Eta Carinae ... Contamination of the BI chip | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 0 | SWG | XIS FLIGHT CAIBRATION PLAN | XIS | N |
| E0102-72 | 15.9926 | -72.0236 | 301.56327722 | -45.07133229 | 226.8326 | 53720.0716203704 | 53723.4377199074 | 100044010 | 59731 | 20000 | 59735 | 125919.5 | 59731 | 59737 | 3 | 3 | 3 | 3 | 1 | 0 | 0 | 115330.2 | 115330.2 | 290803.7 | 1 | PROCESSED | 57532.5803935185 | 54247 | 54119.7612615741 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001097 | We propose the calibration observations for XIS: E0102-72 ... Gain and QE in the low energy band Cas A ... Gain and QE in the high energy band Eta Carinae ... Contamination of the BI chip | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 0 | SWG | XIS FLIGHT CAIBRATION PLAN | NULL | N |
| E0102-72 | 16.0206 | -72.0231 | 301.55102123 | -45.07123322 | 281.396 | 53752.9742708333 | 53755.3752199074 | 100044020 | 41260.5 | 20000 | 41268 | 41852.4 | 41260.5 | 41361 | 3 | 4 | 3 | 4 | 1 | 0 | 0 | 99793.5 | 99793.5 | 207429.8 | 3 | PROCESSED | 57532.7555555556 | 54247 | 54040.6979513889 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001097 | We propose the calibration observations for XIS: E0102-72 ... Gain and QE in the low energy band Cas A ... Gain and QE in the high energy band Eta Carinae ... Contamination of the BI chip | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 0 | SWG | XIS FLIGHT CAIBRATION PLAN | XIS | N |
| E0102-72 | 16.027 | -72.0223 | 301.54815221 | -45.07189388 | 294.0751 | 53768.8467592593 | 53769.4065393518 | 100044030 | 20827.7 | 20000 | 20835.7 | 20843.7 | 20843.7 | 20827.7 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 20268.8 | 20268.8 | 48360 | 1 | PROCESSED | 57532.8615740741 | 54247 | 53905.6764351852 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001097 | We propose the calibration observations for XIS: E0102-72 ... Gain and QE in the low energy band Cas A ... Gain and QE in the high energy band Eta Carinae ... Contamination of the BI chip | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 0 | SWG | XIS FLIGHT CAIBRATION PLAN | XIS | N |
| ETA CARINAE | 161.248 | -59.6859 | 287.58997588 | -0.63475906 | 156.124 | 53769.4163194444 | 53769.9481944444 | 100045010 | 21367.8 | 20000 | 21367.8 | 21367.8 | 21367.8 | 21367.8 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 18145.8 | 18145.8 | 45945.9 | 1 | PROCESSED | 57532.9369907407 | 54247 | 54040.9846643518 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001097 | We propose the calibration observations for XIS: E0102-72 ... Gain and QE in the low energy band Cas A ... Gain and QE in the high energy band Eta Carinae ... Contamination of the BI chip | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 0 | SWG | XIS FLIGHT CAIBRATION PLAN | XIS | N |
| LOCKMANHOLE | 163.4063 | 57.6108 | 148.98193179 | 53.14624927 | 119.611 | 53688.2372337963 | 53689.8300694444 | 100046010 | 76980.6 | 100000 | 76980.6 | 77044.6 | 77012.6 | 77020.6 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 94510.7 | 94510.7 | 137607.9 | 3 | PROCESSED | 57528.0048148148 | 54247 | 54037.5889814815 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001098 | We propose a 100 ks observation of LockmanHole with Suzaku. The main purpose is to obtain a template dataset of HXD background. | CALIBRATION | 1 | A | KOKUBUN | MOTOHIDE | NULL | NULL | JAP | 0 | SWG | BACKGROUND ESTABLISHMENT OF HXD | XIS | N |
| GALACTIC CENTER | 266.5135 | -28.9269 | 0.05735731 | -0.07624929 | 270.2495 | 53986.0995833333 | 53987.3793402778 | 100048010 | 63007.9 | 50000 | 63007.9 | 63007.9 | 63007.9 | 63007.9 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 60322.8 | 60322.8 | 110567.9 | 2 | PROCESSED | 57535.5201967593 | 54526 | 54056.4849189815 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | SWG | XIS FLIGHT CALIBRATION PLAN | XIS | N |
| CYGNUS LOOP | 314.0345 | 31.9311 | 75.67403832 | -8.61676541 | 64.2261 | 53884.1556018518 | 53884.3793865741 | 100049010 | 8380.5 | 10000 | 8380.5 | 8380.5 | 8380.5 | 8380.5 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 6021.1 | 6021.1 | 19304 | 0 | PROCESSED | 57534.4628240741 | 54258 | 54059.411099537 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | SWG | XIS FLIGHT CALIBRATION PLAN | SPE | N |
| CYGNUS LOOP | 314.0785 | 32.0438 | 75.78588033 | -8.57358243 | 64.2263 | 53884.3796759259 | 53884.6086342593 | 100049020 | 7892.8 | 10000 | 7892.8 | 7892.8 | 7892.8 | 7892.8 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 7452 | 7452 | 19769.9 | 0 | PROCESSED | 57534.4674884259 | 54258 | 54088.8429513889 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | SWG | XIS FLIGHT CALIBRATION PLAN | SPE | N |
| CYGNUS LOOP | 313.9494 | 32.0818 | 75.74490282 | -8.46508453 | 64.2292 | 53884.6089236111 | 53884.8377777778 | 100049030 | 11697.1 | 10000 | 11705.1 | 11697.1 | 11705.1 | 11705.1 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 12268.8 | 12268.8 | 19772 | 0 | PROCESSED | 57534.4722800926 | 54258 | 54052.4915046296 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | SWG | XIS FLIGHT CALIBRATION PLAN | SPE | N |
| CYGNUS LOOP | 313.9037 | 31.9696 | 75.63250703 | -8.50670526 | 64.2245 | 53884.8380671296 | 53885.0891666667 | 100049040 | 11765.6 | 10000 | 11781.6 | 11781.6 | 11773.6 | 11765.6 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 9788 | 9788 | 21687.9 | 0 | PROCESSED | 57534.4771296296 | 54258 | 54052.5201157407 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | SWG | XIS FLIGHT CALIBRATION PLAN | SPE | N |
| HER X-1 | 254.4224 | 35.4083 | 58.22535664 | 37.56185232 | 67.8783 | 53823.7669907407 | 53824.640462963 | 101001010 | 33062.1 | 40000 | 33062.1 | 38804.5 | 33062.1 | 33070.1 | 4 | 3 | 4 | 4 | 1 | 0 | 0 | 26222.8 | 26222.8 | 75437.9 | 0 | PROCESSED | 57526.8178703704 | 53826 | 53906.9875925926 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015002 | The main purpose of this observation is to calibrate the enery scale of HXD-GSO, which show a long-term decreasing trend. Another objective is to cross-calibrate the effective area between PIN and GSO. | CALIBRATION | 1 | A | KOKUBUN | MOTOHIDE | NULL | NULL | JAP | 1 | AO1 | SUZAKU OBSERVATION OF HER X-1 FOR HXD CALIBRATION | HXD | N |
| LOCKMAN HOLE | 162.9366 | 57.2557 | 149.70344314 | 53.20093146 | 281.8721 | 53872.7389583333 | 53874.7939583333 | 101002010 | 80398.2 | 80000 | 80398.2 | 80406.2 | 80406.2 | 80406.2 | 3 | 3 | 3 | 3 | 1 | 0 | 0 | 88854 | 88854 | 177513.8 | 4 | PROCESSED | 57534.3694212963 | 53826 | 53927.7689814815 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015003 | We propose an additional observation of the Lockman Hole for a purpose of the verification of the background (CXB+NXB) modeling of HXD. | CALIBRATION | 1 | A | KOKUBUN | MOTOHIDE | NULL | NULL | JAP | 1 | AO1 | SUZAKU OBSERVATION OF LOCKMANHOLE | XIS | N |
| CRAB | 83.6569 | 21.9577 | 184.61755594 | -5.79610428 | 250.9424 | 53830.5463425926 | 53831.5925115741 | 101003010 | 37832.3 | 40000 | 37832.3 | 37853.3 | 37832.3 | 37832.3 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 30989 | 30989 | 90379.9 | 1 | PROCESSED | 57533.4323726852 | 53826 | 53907.1306944445 | 3.0.22.43 | 6 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015004 | Crab cal at the XIS and HXD nominal positions. | CALIBRATION | 1 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 1 | AO1 | CRAB | HXD | N |
| CRAB | 83.6371 | 22.0108 | 184.56259415 | -5.78319491 | 253.3318 | 53824.652650463 | 53825.1668865741 | 101004010 | 16363.2 | 20000 | 16363.2 | 16372.8 | 16365 | 16365 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 9761.6 | 9761.6 | 44426 | 0 | PROCESSED | 57533.3378009259 | 53826 | 53906.0621875 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015004 | Crab cal at the XIS and HXD nominal positions. | CALIBRATION | 1 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 1 | AO1 | CRAB | XIS | N |
| CRAB | 83.6368 | 22.0131 | 184.56049184 | -5.78219867 | 250.943 | 53829.1296643518 | 53829.5974305556 | 101004020 | 19138.9 | 20000 | 19138.9 | 19145.8 | 19138.9 | 19138.9 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 13283.1 | 13283.1 | 40411.9 | 1 | PROCESSED | 57533.3778009259 | 53826 | 53906.6409375 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015004 | Crab cal at the XIS and HXD nominal positions. | CALIBRATION | 1 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 1 | AO1 | CRAB | XIS | N |
| E0102.2-7219 | 16.0331 | -72.0338 | 301.54662861 | -45.06029066 | 8.2024 | 53841.404212963 | 53841.9793865741 | 101005010 | 21324 | 40000 | 21340 | 21324 | 21332 | 21340 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 16683.1 | 16683.1 | 49663.9 | 0 | PROCESSED | 57533.4651273148 | 53826 | 53905.6938425926 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | AO1 | XIS FLIGHT CALIBRATION PLAN | XIS | N |
| E0102.2-7219 | 16.0278 | -72.0394 | 301.54948943 | -45.0548182 | 34.4136 | 53876.719525463 | 53877.1793287037 | 101005020 | 18161.9 | 20000 | 18161.9 | 18193.9 | 18161.9 | 18193.9 | 2 | 1 | 2 | 1 | 1 | 0 | 0 | 17763.3 | 17763.3 | 39719.9 | 0 | PROCESSED | 57534.3838425926 | 53826 | 53926.1422222222 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | AO1 | XIS FLIGHT CALIBRATION PLAN | XIS | N |
| E0102.2-7219 | 16.0175 | -72.0405 | 301.55408267 | -45.05394165 | 60.6353 | 53912.8662731482 | 53913.4245833333 | 101005030 | 21675.8 | 20000 | 21715.8 | 21683.8 | 21715.8 | 21675.8 | 2 | 4 | 2 | 4 | 1 | 0 | 0 | 35062.6 | 35062.6 | 48203.9 | 0 | PROCESSED | 57534.7584837963 | 53826 | 53928.4586458333 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | AO1 | XIS FLIGHT CALIBRATION PLAN | XIS | N |
| E0102.2-7219 | 15.9978 | -72.0424 | 301.56284618 | -45.05246644 | 92.9794 | 53933.2656597222 | 53933.9030439815 | 101005040 | 22063.4 | 20000 | 22063.4 | 22103.4 | 22063.4 | 22095.4 | 4 | 2 | 4 | 2 | 1 | 0 | 0 | 20982.3 | 20982.3 | 55047.9 | 1 | PROCESSED | 57534.9613888889 | 53826 | 53942.4630092593 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | AO1 | XIS FLIGHT CALIBRATION PLAN | XIS | N |
| E0102.2-7219 | 15.9824 | -72.0369 | 301.56901677 | -45.05828014 | 133.8232 | 53972.2052662037 | 53973.3933333333 | 101005050 | 68363.2 | 20000 | 68987.2 | 68363.2 | 68987.2 | 68971.2 | 5 | 5 | 5 | 6 | 1 | 0 | 0 | 68002.4 | 68002.4 | 102633.9 | 1 | PROCESSED | 57535.3618402778 | 53826 | 54020.9929050926 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | AO1 | XIS FLIGHT CALIBRATION PLAN | XIS | N |
| E0102.2-7219 | 15.9812 | -72.0315 | 301.5690149 | -45.06369281 | 159.2453 | 53997.2263425926 | 53997.562662037 | 101005060 | 10790.7 | 40000 | 10806.7 | 10806.7 | 10790.7 | 10798.7 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 10322.3 | 10322.3 | 29050 | 0 | PROCESSED | 57535.6263541667 | 53826 | 54021.1325115741 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | AO1 | XIS FLIGHT CALIBRATION PLAN | XIS | N |
| E0102.2-7219 | 15.9801 | -72.0277 | 301.56912514 | -45.06750714 | 192.8855 | 54029.650625 | 54030.2265625 | 101005070 | 37130.5 | 40000 | 37170.5 | 37130.5 | 37170.5 | 37162.5 | 3 | 3 | 3 | 3 | 1 | 0 | 0 | 36471.6 | 36471.6 | 49760 | 0 | PROCESSED | 57535.9063425926 | 53826 | 54055.5631828704 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | AO1 | XIS FLIGHT CALIBRATION PLAN | XIS | Y |
| E0102.2-7219 | 16.0029 | -72.0223 | 301.55865958 | -45.07240987 | 252.2709 | 54082.7869907407 | 54083.1279976852 | 101005090 | 28226 | 20000 | 28226 | 28226 | 0 | 28226 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 23054.6 | 23054.6 | 29455.9 | 0 | PROCESSED | 57536.3258101852 | 53826 | 54094.5930324074 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | AO1 | XIS FLIGHT CALIBRATION PLAN | XIS | Y |
| E0102.2-7219 | 16.0137 | -72.0201 | 301.5537348 | -45.07437383 | 265.9905 | 54115.1395023148 | 54115.6655555556 | 101005100 | 22614 | 20000 | 22614 | 22614 | 0 | 22614 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 19149.6 | 19149.6 | 45424 | 1 | PROCESSED | 57536.8323263889 | 53826 | 54132.8509490741 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | AO1 | XIS FLIGHT CALIBRATION PLAN | XIS | N |
| E0102.2-7219 | 16.0273 | -72.0256 | 301.54834682 | -45.06859544 | 302.8131 | 54141.9262384259 | 54142.812662037 | 101005110 | 36093.8 | 20000 | 36101.8 | 36093.8 | 0 | 36101.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 52703.8 | 52703.8 | 76575.9 | 1 | PROCESSED | 57537.3567592593 | 53826 | 54153.2227430556 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | AO1 | XIS FLIGHT CALIBRATION PLAN | XIS | Y |
| E0102.2-7219 | 16.0373 | -72.0314 | 301.54456169 | -45.06259438 | 341.0006 | 54177.8828587963 | 54178.2994675926 | 101005120 | 18242 | 20000 | 18242 | 18250 | 0 | 18258 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 14755.1 | 14755.1 | 35983.9 | 0 | PROCESSED | 57537.6970601852 | 53826 | 54185.4459027778 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | AO1 | XIS FLIGHT CALIBRATION PLAN | XIS | N |
| PKS2155-304 | 329.7138 | -30.2259 | 17.72949775 | -52.24318888 | 57.9013 | 53856.2600925926 | 53857.2501041667 | 101006010 | 38551.5 | 30000 | 38551.5 | 38551.5 | 38551.5 | 38551.5 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 23947.6 | 23947.6 | 85514.1 | 2 | PROCESSED | 57533.6080787037 | 53826 | 53913.2773842593 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | AO1 | XIS FLIGHT CALIBRATION PLAN | XIS | N |
| RXJ1856.5-3754 | 284.1489 | -37.9077 | 358.6011477 | -17.21474589 | 254.2953 | 54028.5128472222 | 54029.6405208333 | 101009010 | 40784.1 | 40000 | 40784.1 | 40784.1 | 40784.1 | 40784.1 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 35169.9 | 35169.9 | 97403.9 | 1 | PROCESSED | 57535.9219675926 | 53826 | 54055.4732523148 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015007 | Here is the list of the calibration sources in the AO-1 round: 1) E0102.2-7219 20ks x 2 2) PKS2155-304 30ks (simultaneous observation with CXO and XMM) 3) Galactic Center Plasma 50ks 4) Cygnus Loop 40ks (=10ks x 4), and 5) RXJ1856.5-3754 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | AO1 | XIS FLIGHT CALIBRATION PLAN | XIS | N |
| CRAB | 83.6301 | 22.0172 | 184.55366892 | -5.78525038 | 85.7026 | 53983.2227430556 | 53983.8196643518 | 101010010 | 20717.5 | 20000 | 20877.5 | 20717.5 | 20893.5 | 20885.5 | 3 | 2 | 3 | 3 | 1 | 0 | 0 | 19607.1 | 19607.1 | 51569.9 | 1 | PROCESSED | 57535.464224537 | 53826 | 54024.6695833333 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015014 | HXD cal. | CALIBRATION | 1 | A | NAKAZAWA | KAZUHIRO | NULL | NULL | JAP | 1 | AO1 | CRAB CAL FOR HXD ON 2006 AUTUMN | XIS | N |
| THE CRAB OFFSETS | 83.6209 | 22.1323 | 184.45137768 | -5.73082135 | 85.7132 | 53983.8199537037 | 53983.8891087963 | 101011010 | 3348 | 2000 | 3348 | 3348 | 3348 | 3348 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 3676 | 3676 | 5967.9 | 0 | PROCESSED | 57535.4548263889 | 53826 | 54104.4418287037 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015015 | We propose observing multiple offset pointings of the Crab nebula. | CALIBRATION | 1 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 1 | AO1 | CRAB OFFSET POINTINGS | SPE | N |
| THE CRAB OFFSETS | 83.6229 | 22.105 | 184.47554642 | -5.74387633 | 85.7146 | 53983.889212963 | 53983.9516087963 | 101011020 | 3350 | 2000 | 3350 | 3350 | 3350 | 3350 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 3004 | 3004 | 5383.9 | 0 | PROCESSED | 57535.4600694444 | 53826 | 54104.4374189815 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015015 | We propose observing multiple offset pointings of the Crab nebula. | CALIBRATION | 1 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 1 | AO1 | CRAB OFFSET POINTINGS | SPE | N |
| THE CRAB OFFSETS | 83.6254 | 22.076 | 184.50140903 | -5.75744861 | 85.7164 | 53983.951712963 | 53984.0904976852 | 101011030 | 6703 | 2000 | 6703 | 6703 | 6703 | 6703 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 5445.8 | 5445.8 | 11983.9 | 0 | PROCESSED | 57535.4650462963 | 53826 | 54104.972650463 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015015 | We propose observing multiple offset pointings of the Crab nebula. | CALIBRATION | 1 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 1 | AO1 | CRAB OFFSET POINTINGS | HXD | N |
| THE CRAB OFFSETS | 83.6274 | 22.0499 | 184.52456216 | -5.76985767 | 85.719 | 53984.0906018518 | 53984.1529976852 | 101011040 | 3353 | 2000 | 3353 | 3353 | 3353 | 3353 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2414 | 2414 | 5383.9 | 0 | PROCESSED | 57535.4661921296 | 53826 | 54104.4143518518 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015015 | We propose observing multiple offset pointings of the Crab nebula. | CALIBRATION | 1 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 1 | AO1 | CRAB OFFSET POINTINGS | SPE | N |
| THE CRAB OFFSETS | 83.6323 | 21.9916 | 184.57650041 | -5.79723168 | 85.7244 | 53984.1531944445 | 53984.2224421296 | 101011050 | 3355 | 2000 | 3355 | 3355 | 3355 | 3355 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2187 | 2187 | 5975.9 | 0 | PROCESSED | 57535.4744907407 | 53826 | 54104.4478587963 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015015 | We propose observing multiple offset pointings of the Crab nebula. | CALIBRATION | 1 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 1 | AO1 | CRAB OFFSET POINTINGS | SPE | N |
| THE CRAB OFFSETS | 83.6331 | 21.9589 | 184.60466298 | -5.81410844 | 87.5062 | 53996.8758680556 | 53996.9515509259 | 101011060 | 3368 | 2000 | 3368 | 3368 | 3368 | 3368 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2716 | 2716 | 6527.9 | 0 | PROCESSED | 57535.6113888889 | 53826 | 54104.4231481482 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015015 | We propose observing multiple offset pointings of the Crab nebula. | CALIBRATION | 1 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 1 | AO1 | CRAB OFFSET POINTINGS | SPE | N |
| THE CRAB OFFSETS | 83.6338 | 21.931 | 184.62870178 | -5.82849289 | 87.5103 | 53996.9516550926 | 53997.0140509259 | 101011070 | 2636 | 2000 | 2636 | 2636 | 2636 | 2636 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2157 | 2157 | 5383.9 | 0 | PROCESSED | 57535.6130092593 | 53826 | 54104.4160069444 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015015 | We propose observing multiple offset pointings of the Crab nebula. | CALIBRATION | 1 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 1 | AO1 | CRAB OFFSET POINTINGS | SPE | N |
| THE CRAB OFFSETS | 83.6343 | 21.9041 | 184.65179297 | -5.84249768 | 87.5094 | 53997.0141550926 | 53997.0834953704 | 101011080 | 2251 | 2000 | 2251 | 2251 | 2251 | 2251 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2275 | 2275 | 5983.9 | 1 | PROCESSED | 57535.6182407407 | 53826 | 54104.4469675926 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015015 | We propose observing multiple offset pointings of the Crab nebula. | CALIBRATION | 1 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 1 | AO1 | CRAB OFFSET POINTINGS | SPE | N |
| THE CRAB OFFSETS | 83.7555 | 22.0251 | 184.60946275 | -5.68280554 | 87.8963 | 53997.0840625 | 53997.1529282407 | 101011090 | 1895 | 2000 | 1895 | 1895 | 1895 | 1895 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 2081.5 | 2081.5 | 5945.9 | 0 | PROCESSED | 57535.6191435185 | 53826 | 54104.4517708333 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015015 | We propose observing multiple offset pointings of the Crab nebula. | CALIBRATION | 1 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 1 | AO1 | CRAB OFFSET POINTINGS | SPE | N |
| THE CRAB OFFSETS | 83.7241 | 22.023 | 184.59560566 | -5.70852703 | 87.5484 | 53997.1534490741 | 53997.2154513889 | 101011100 | 1545 | 2000 | 1545 | 1545 | 1545 | 1545 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 1806 | 1806 | 5356 | 0 | PROCESSED | 57535.619537037 | 53826 | 54104.4337731482 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015015 | We propose observing multiple offset pointings of the Crab nebula. | CALIBRATION | 1 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 1 | AO1 | CRAB OFFSET POINTINGS | SPE | N |
| THE CRAB OFFSETS | 83.6927 | 22.0229 | 184.58004352 | -5.7331758 | 85.756 | 53984.5680092593 | 53984.6252199074 | 101011110 | 2635.4 | 2000 | 2635.4 | 2635.4 | 2635.4 | 2635.4 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2457.3 | 2457.3 | 4942 | 0 | PROCESSED | 57535.4715046296 | 53826 | 54104.4321527778 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015015 | We propose observing multiple offset pointings of the Crab nebula. | CALIBRATION | 1 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 1 | AO1 | CRAB OFFSET POINTINGS | SPE | N |
| THE CRAB OFFSETS | 83.6616 | 22.0194 | 184.56751127 | -5.75940556 | 85.7473 | 53984.6253703704 | 53984.6876967593 | 101011120 | 2976.1 | 2000 | 2976.1 | 2976.1 | 2976.1 | 2976.1 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 2802 | 2802 | 5380 | 0 | PROCESSED | 57535.4738425926 | 53826 | 54104.4254513889 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015015 | We propose observing multiple offset pointings of the Crab nebula. | CALIBRATION | 1 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 1 | AO1 | CRAB OFFSET POINTINGS | SPE | N |
| THE CRAB OFFSETS | 83.5991 | 22.0137 | 184.54117278 | -5.81139714 | 85.7249 | 53984.6879398148 | 53984.7572222222 | 101011130 | 3366.1 | 2000 | 3366.1 | 3366.1 | 3366.1 | 3366.1 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 3190 | 3190 | 5983.9 | 0 | PROCESSED | 57535.4770486111 | 53826 | 54104.4575 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015015 | We propose observing multiple offset pointings of the Crab nebula. | CALIBRATION | 1 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 1 | AO1 | CRAB OFFSET POINTINGS | SPE | N |
| THE CRAB OFFSETS | 83.5675 | 22.0116 | 184.5271819 | -5.8372614 | 85.7131 | 53984.7573263889 | 53984.8197222222 | 101011140 | 3369 | 2000 | 3369 | 3369 | 3369 | 3369 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 3632 | 3632 | 5383.9 | 0 | PROCESSED | 57535.4802546296 | 53826 | 54104.4270601852 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015015 | We propose observing multiple offset pointings of the Crab nebula. | CALIBRATION | 1 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 1 | AO1 | CRAB OFFSET POINTINGS | SPE | N |
| THE CRAB OFFSETS | 83.536 | 22.0119 | 184.51119717 | -5.8617583 | 85.703 | 53984.8198263889 | 53984.8891666667 | 101011150 | 3370 | 2000 | 3370 | 3370 | 3370 | 3370 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 3347.2 | 3347.2 | 5983.9 | 0 | PROCESSED | 57535.4824189815 | 53826 | 54104.9730439815 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015015 | We propose observing multiple offset pointings of the Crab nebula. | CALIBRATION | 1 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 1 | AO1 | CRAB OFFSET POINTINGS | SPE | N |
| THE CRAB OFFSETS | 83.5056 | 22.0085 | 184.49889553 | -5.88737418 | 85.6939 | 53984.8892708333 | 53984.935 | 101011160 | 2765.1 | 2000 | 2765.1 | 2765.1 | 2765.1 | 2765.1 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2152 | 2152 | 3943.9 | 0 | PROCESSED | 57535.4827083333 | 53826 | 54104.4508449074 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015015 | We propose observing multiple offset pointings of the Crab nebula. | CALIBRATION | 1 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 1 | AO1 | CRAB OFFSET POINTINGS | SPE | N |
| PERSEUS CLUSTER | 49.9436 | 41.5175 | 150.56798595 | -13.25929387 | 66.0393 | 53976.788275463 | 53980.0793865741 | 101012010 | 150905.1 | 150000 | 150905.1 | 150921.1 | 150937.1 | 150921.1 | 6 | 6 | 6 | 6 | 1 | 0 | 0 | 142533.4 | 142533.4 | 284336 | 3 | PROCESSED | 57535.5159375 | 53826 | 54024.8648726852 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015016 | We propose the observation of Perseus cluster for 150ks. To recover the energy resolution of the XIS, we will try the periodic charge injection method. However, the charge injection will change calibrations such as gain, QE and so on dramatically. To study the change of the clibrations, Perseus cluster is one of the best targets, because it is extended over the whole XIS FOV and the iron K line from the cluster is extremely strong. For the first 50ks, the observation will be done with the normal mode without the charge injection. For the second and third 50ks, we will do the charge injections with every 54 and 108 rows, repectively. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | AO1 | PERSEUS OBSERVATION FOR CALIBRATIONS ON THE PERIODIC CHARGE INJECTION METHOD | XIS | Y |
| PERSEUS CLUSTER | 49.9542 | 41.5047 | 150.58204074 | -13.26559499 | 258.6515 | 54136.6651388889 | 54137.6043287037 | 101012020 | 43871.4 | 40000 | 43895.4 | 43879.4 | 0 | 43871.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41573.2 | 41573.2 | 81137.9 | 1 | PROCESSED | 57537.3356944444 | 53826 | 54151.6542361111 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015017 | we propose observations for the XIS flight calibrations during the left term of AO-1. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | AO1 | XIS CALIBRATIONS FOR AO1 | XIS | Y |
| CYGNUS LOOP | 314.0118 | 31.9912 | 75.70842949 | -8.56360013 | 217.4642 | 54090.3953935185 | 54090.6848842593 | 101013010 | 9102 | 10000 | 9102 | 9102 | 0 | 9102 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 9212.6 | 9212.6 | 25006 | 1 | PROCESSED | 57536.373275463 | 53826 | 54108.4571990741 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015017 | we propose observations for the XIS flight calibrations during the left term of AO-1. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | AO1 | XIS CALIBRATIONS FOR AO1 | XIS | Y |
| CYGNUS LOOP | 314.0133 | 31.992 | 75.70987313 | -8.56406979 | 213.2117 | 54090.6869791667 | 54091.1175231482 | 101013020 | 21004 | 20000 | 21004 | 21004 | 0 | 21004 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 18871.9 | 18871.9 | 37168 | 1 | PROCESSED | 57536.3885185185 | 53826 | 54132.7085763889 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015017 | we propose observations for the XIS flight calibrations during the left term of AO-1. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | AO1 | XIS CALIBRATIONS FOR AO1 | XIS | Y |
| CYGNUS LOOP | 314.0129 | 31.9925 | 75.71004378 | -8.56348961 | 212.8468 | 54091.1180439815 | 54091.6036342593 | 101013030 | 19729.5 | 20000 | 19729.5 | 19729.5 | 0 | 19729.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20100.5 | 20100.5 | 41927.9 | 1 | PROCESSED | 57536.3931134259 | 53826 | 54132.7375694444 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 015017 | we propose observations for the XIS flight calibrations during the left term of AO-1. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | AO1 | XIS CALIBRATIONS FOR AO1 | XIS | Y |
| E0102.2-7219 | 16.0421 | -72.0341 | 301.54273778 | -45.05979748 | 2.5391 | 54200.4410648148 | 54200.8127199074 | 102001010 | 18115 | 20000 | 18115 | 18115 | 0 | 18115 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 24523 | 24523 | 32103.9 | 0 | PROCESSED | 57538.1062384259 | 54191 | 54210.6037268518 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 025155 | The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 2 | AO2 | XIS FLIGHT CALIBRATION PLAN | XIS | Y |
| E0102.2-7219 | 16.0153 | -72.0406 | 301.55505042 | -45.05388895 | 60.6693 | 54264.42375 | 54265.1467476852 | 102002010 | 27871.7 | 20000 | 27871.7 | 27871.7 | 0 | 27871.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28315.5 | 28315.5 | 62463.9 | 1 | PROCESSED | 57538.9373726852 | 54191 | 54271.4505092593 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 025155 | The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 2 | AO2 | XIS FLIGHT CALIBRATION PLAN | XIS | Y |
| E0102.2-7219 | 15.9919 | -72.0394 | 301.56512259 | -45.05558467 | 110.1956 | 54324.2230208333 | 54325.1565277778 | 102003010 | 39482 | 20000 | 39490 | 39482 | 0 | 39490 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 37350.5 | 37350.5 | 80647.9 | 1 | PROCESSED | 57539.4810648148 | 54191 | 54347.4795717593 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 025155 | The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 2 | AO2 | XIS FLIGHT CALIBRATION PLAN | XIS | Y |
| E0102.2-7219 | 15.9812 | -72.0282 | 301.56869429 | -45.06698503 | 193.1812 | 54398.5171875 | 54399.375162037 | 102004010 | 26175.7 | 20000 | 26175.7 | 26175.7 | 0 | 26175.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25480.7 | 25480.7 | 74093.8 | 0 | PROCESSED | 57540.3610069444 | 54191 | 54407.5260416667 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 025155 | The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 2 | AO2 | XIS FLIGHT CALIBRATION PLAN | XIS | Y |
| E0102.2-7219 | 16.0039 | -72.0219 | 301.55818443 | -45.07278758 | 249.4582 | 54435.8094907407 | 54436.4099421296 | 102005010 | 24766.7 | 20000 | 24766.7 | 24790.7 | 0 | 24790.7 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 23722.3 | 23722.3 | 51871.9 | 1 | PROCESSED | 57540.7675810185 | 54191 | 54441.0108449074 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 025155 | The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 2 | AO2 | XIS FLIGHT CALIBRATION PLAN | XIS | Y |
| E0102.2-7219 | 16.0383 | -72.0304 | 301.54402708 | -45.06357038 | 338.1 | 54540.2385069444 | 54540.8648611111 | 102006010 | 28238.9 | 20000 | 28238.9 | 28238.9 | 0 | 28238.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38612.6 | 38612.6 | 54114 | 0 | PROCESSED | 57541.8710763889 | 54191 | 54550.2250347222 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 025155 | The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 2 | AO2 | XIS FLIGHT CALIBRATION PLAN | XIS | Y |
| CYGNUS LOOP | 313.9884 | 32.004 | 75.70560343 | -8.54015129 | 44.0016 | 54263.5520833333 | 54263.8668402778 | 102007010 | 13345.5 | 10000 | 13353.5 | 13345.5 | 0 | 13353.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12560.7 | 12560.7 | 27191.9 | 1 | PROCESSED | 57538.9070138889 | 54191 | 54269.4117013889 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 025155 | The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 2 | AO2 | XIS FLIGHT CALIBRATION PLAN | XIS | Y |
| CYGNUS LOOP | 314.0072 | 31.9862 | 75.70201861 | -8.56378367 | 248.0186 | 54437.219224537 | 54437.5627314815 | 102008010 | 13265.5 | 10000 | 13265.5 | 13265.5 | 0 | 13265.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13271.6 | 13271.6 | 29676 | 0 | PROCESSED | 57540.7827777778 | 54191 | 54445.1862731482 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 025155 | The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 2 | AO2 | XIS FLIGHT CALIBRATION PLAN | XIS | Y |
| CYGNUS LOOP | 313.9882 | 32.0035 | 75.70510458 | -8.54033943 | 43.7589 | 54263.8673148148 | 54264.412025463 | 102009010 | 22896.5 | 20000 | 22896.5 | 22900.5 | 0 | 22916.5 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 18570.8 | 18570.8 | 47060 | 0 | PROCESSED | 57538.9162847222 | 54191 | 54269.4275462963 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 025155 | The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 2 | AO2 | XIS FLIGHT CALIBRATION PLAN | XIS | Y |
| CYGNUS_LOOP_55FE | 314.0065 | 31.9862 | 75.70163572 | -8.56332634 | 247.7519 | 54437.5631597222 | 54438.1890740741 | 102010010 | 29585 | 20000 | 29585 | 29585 | 0 | 29585 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 27780.4 | 27780.4 | 54075.9 | 0 | PROCESSED | 57540.7912268518 | 54191 | 54451.4647916667 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 025155 | The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 2 | AO2 | XIS FLIGHT CALIBRATION PLAN | XIS | Y |
| PERSEUS CLUSTER | 49.9461 | 41.5179 | 150.56936377 | -13.25792808 | 83.376 | 54327.5283449074 | 54328.477337963 | 102011010 | 42281.7 | 40000 | 42281.7 | 42281.7 | 0 | 42281.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36206.3 | 36206.3 | 81983.9 | 1 | PROCESSED | 57539.6215046296 | 54191 | 54347.6070833333 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 025155 | The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 2 | AO2 | XIS FLIGHT CALIBRATION PLAN | XIS | Y |
| PERSEUS_CLUSTER_Normal | 49.9565 | 41.505 | 150.58334697 | -13.26439478 | 255.1861 | 54503.0900694444 | 54504.4377199074 | 102012010 | 61742.6 | 40000 | 61742.6 | 61742.6 | 0 | 61742.6 | 4 | 4 | 0 | 4 | 1 | 0 | 0 | 62315.7 | 62315.7 | 116399.9 | 0 | PROCESSED | 57541.5492824074 | 54191 | 54515.8301736111 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 025155 | The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 2 | AO2 | XIS FLIGHT CALIBRATION PLAN | XIS | Y |
| GALACTIC CENTER | 266.5129 | -28.9278 | 0.05631549 | -0.07626904 | 265.2972 | 54346.7924768518 | 54348.2224537037 | 102013010 | 51396 | 50000 | 51396 | 51420 | 0 | 51404 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44477.8 | 44477.8 | 123535.8 | 0 | PROCESSED | 57539.9440162037 | 54191 | 54356.3951388889 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 025155 | The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 2 | AO2 | XIS FLIGHT CALIBRATION PLAN | XIS | Y |
| RXJ1856.5-3754 | 284.1483 | -37.9083 | 358.60038232 | -17.21452318 | 271.9345 | 54388.7289930556 | 54389.587025463 | 102014010 | 41318 | 40000 | 41318 | 41318 | 0 | 41318 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40654.5 | 40654.5 | 74129.9 | 1 | PROCESSED | 57540.2918518518 | 54191 | 54403.060462963 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 025155 | The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 2 | AO2 | XIS FLIGHT CALIBRATION PLAN | XIS | Y |
| RXJ1856.5-3754 | 284.1438 | -37.9098 | 358.59756743 | -17.21176167 | 89.7041 | 54547.2693402778 | 54548.4723842593 | 102015010 | 50652.3 | 40000 | 50652.3 | 50668.3 | 0 | 50652.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38365.4 | 38365.4 | 103923.8 | 2 | PROCESSED | 57541.945625 | 54191 | 54566.3157523148 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 025155 | The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 2 | AO2 | XIS FLIGHT CALIBRATION PLAN | XIS | Y |
| PSR 1509-58 AT NOM. | 228.4878 | -59.1337 | 320.32453924 | -1.16169081 | 289.2119 | 54333.5632060185 | 54334.1044444444 | 102016010 | 41213.8 | 40000 | 41221.8 | 41221.8 | 0 | 41213.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 32908.4 | 32908.4 | 46759.9 | 1 | PROCESSED | 57539.6434375 | 54191 | 54350.4146875 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 025156 | PSR 1509-58 | CALIBRATION | 1 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 2 | AO2 | PSR 1509-58 | XIS | Y |
| PSR 1509-58 AT FIXEA | 228.4815 | -59.094 | 320.34236207 | -1.12606748 | 287.6329 | 54334.1057060185 | 54334.7690277778 | 102017010 | 43803.8 | 40000 | 43843.8 | 43827.8 | 0 | 43803.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37119.9 | 37119.9 | 57303.9 | 3 | PROCESSED | 57539.6453125 | 54191 | 54350.6658449074 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 025156 | PSR 1509-58 | CALIBRATION | 1 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 2 | AO2 | PSR 1509-58 | XIS | Y |
| LOCKMANHOLE | 162.9257 | 57.2581 | 149.70707974 | 53.19495056 | 319.512 | 54223.9667592593 | 54226.0835532407 | 102018010 | 96071.6 | 80000 | 96079.6 | 96079.6 | 0 | 96071.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 92778 | 92778 | 182824.8 | 3 | PROCESSED | 57538.6101273148 | 54191 | 54230.4555902778 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 025157 | The purpose of this observation is to verify the energy response of HXD-PIN/GSO. | CALIBRATION | 1 | A | KOKUBUN | MOTOHIDE | NULL | NULL | JAP | 2 | AO2 | CALIBRATION OBSERVATION OF HXD WITH CRAB | XIS | Y |
| CRAB | 83.6357 | 21.9546 | 184.60961134 | -5.81437304 | 269.3898 | 54179.4457407407 | 54180.6008912037 | 102019010 | 47633.1 | 40000 | 47633.1 | 47633.1 | 0 | 47633.1 | 3 | 2 | 0 | 3 | 1 | 0 | 0 | 43407.5 | 43407.5 | 99773.9 | 1 | PROCESSED | 57537.8123958333 | 54191 | 54314.6631597222 | 3.0.22.43 | 6 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 025158 | The purpose of this observation is to verify the energy response of HXD-PIN/GSO. | CALIBRATION | 1 | A | KOKUBUN | MOTOHIDE | NULL | NULL | JAP | 2 | AO2 | CALIBRATION OBSERVATION OF HXD WITH CRAB | HXD | Y |
| PKS2155-304 | 329.716 | -30.2268 | 17.72837689 | -52.24517694 | 58.2058 | 54212.5208796296 | 54212.8488310185 | 102020010 | 12036.6 | 15000 | 12036.6 | 12036.6 | 0 | 12036.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10572 | 10572 | 28327.9 | 1 | PROCESSED | 57538.4461226852 | 54191 | 54217.2257523148 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 025160 | This is a coordinated observation of PKS2155-304 with Chandra and XMM-Newton for spectral calibration. The observation also aims at evaluating the amount of contaminant on the XIS OBF. | CALIBRATION | 1 | A | ISHIDA | MANABU | NULL | NULL | JAP | 2 | AO2 | PKS2155-304 COORDINATED WITH CHANDRA AND XMM-NEWTON | XIS | Y |
| E0102.2-7219 | 15.976 | -72.0294 | 301.57107704 | -45.06589786 | 179.7828 | 54371.2595833333 | 54371.6390509259 | 102021010 | 25314.6 | 12000 | 25314.6 | 25314.6 | 0 | 25314.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20225 | 20225 | 32781.9 | 0 | PROCESSED | 57540.1292361111 | 54191 | 54402.2749421296 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 025155 | The XIS team plans to observe these targets for the calibrations: E0102, Cygnus Loop, Perseus cluster, Galactic Center, and RXJ1856. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 2 | AO2 | XIS FLIGHT CALIBRATION PLAN | XIS | N |
| E0102.2-7219 | 16.0349 | -72.0243 | 301.54490568 | -45.06972875 | 306.7237 | 54510.7065740741 | 54512.1322222222 | 102022010 | 48424.5 | 40000 | 48424.5 | 48437.3 | 0 | 48432.5 | 3 | 2 | 0 | 3 | 1 | 0 | 0 | 46842.1 | 46842.1 | 123151.8 | 0 | PROCESSED | 57526.8876967593 | 54191 | 54553.2132523148 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 025161 | 4 Calibration in Ao-2 phase. E0102-72 with PSUM mode and HXD lower gain operation. Her X-1 with XIS Timing mode. PSR B0545-69 for cross calibration of the absolute effective area. Perseus[cluster for gain calibration of 1/4 window mode. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 2 | AO2 | SUZAKU ADDITIONAL CALIBRATION | XIS | Y |
| PSR B0540-69 | 85.0333 | -69.3191 | 279.70305196 | -31.5216772 | 241.3303 | 54512.1372337963 | 54513.444537037 | 102023010 | 52168.9 | 40000 | 52168.9 | 52168.9 | 0 | 52168.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46459 | 46459 | 112937.8 | 1 | PROCESSED | 57541.5891782407 | 54191 | 54522.2283217593 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 025161 | 4 Calibration in Ao-2 phase. E0102-72 with PSUM mode and HXD lower gain operation. Her X-1 with XIS Timing mode. PSR B0545-69 for cross calibration of the absolute effective area. Perseus[cluster for gain calibration of 1/4 window mode. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 2 | AO2 | SUZAKU ADDITIONAL CALIBRATION | XIS | Y |
| HER X-1 | 254.4589 | 35.3557 | 58.16585628 | 37.52408174 | 104.6168 | 54517.6276736111 | 54518.4863888889 | 102024010 | 38931 | 40000 | 38939 | 38931 | 0 | 38939 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34312.1 | 34312.1 | 74190 | 2 | PROCESSED | 57541.7036574074 | 54191 | 54525.4895138889 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 025161 | 4 Calibration in Ao-2 phase. E0102-72 with PSUM mode and HXD lower gain operation. Her X-1 with XIS Timing mode. PSR B0545-69 for cross calibration of the absolute effective area. Perseus[cluster for gain calibration of 1/4 window mode. | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 2 | AO2 | SUZAKU ADDITIONAL CALIBRATION | XIS | Y |
| E0102.2-7219 | 16.0298 | -72.0236 | 301.54705976 | -45.07053683 | 295.9817 | 54501.0571990741 | 54501.5245833333 | 102026010 | 0 | 15000 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1 | 0 | 0 | 19059.4 | 19059.4 | 40380 | 0 | PROCESSED | 57541.5004166667 | 54191 | 54515.8508912037 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 025162 | Recovery operation of XIS CPU HALT | CALIBRATION | 1 | A | SWG | NULL | NULL | NULL | JAP | 2 | AO2 | XIS RECOVERY AND VERIFICATION | XIS | Y |
| E0102.2-7219 | 16.0427 | -72.0346 | 301.54252595 | -45.05928576 | 1.5429 | 54564.6063888889 | 54565.2190277778 | 103001010 | 22361.5 | 20000 | 22377.5 | 22361.5 | 0 | 22377.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22318.5 | 22318.5 | 52926 | 1 | PROCESSED | 57542.2691782407 | 54557 | 54580.9409722222 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 035001 | Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 3 | AO3 | AO-3 XIS FLIGHT CALIBRATION PLAN | XIS | Y |
| E0102.2-7219 | 16.0204 | -72.038 | 301.5525741 | -45.05637352 | 46.6005 | 54622.1603356482 | 54622.8557175926 | 103001020 | 21313 | 20000 | 21329 | 21313 | 0 | 21329 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19486.9 | 19486.9 | 60069.9 | 0 | PROCESSED | 57542.7328472222 | 54557 | 54636.3245833333 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 035001 | Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 3 | AO3 | AO-3 XIS FLIGHT CALIBRATION PLAN | XIS | Y |
| E0102.2-7219 | 15.987 | -72.0401 | 301.56732456 | -45.05499026 | 122.9265 | 54690.9315740741 | 54691.5905555556 | 103001030 | 21301.8 | 20000 | 21309.8 | 21309.8 | 0 | 21301.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17083.1 | 17083.1 | 56929.9 | 0 | PROCESSED | 57543.2733680556 | 54557 | 54710.2804166667 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 035001 | Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 3 | AO3 | AO-3 XIS FLIGHT CALIBRATION PLAN | XIS | Y |
| E0102.2-7219 | 15.9798 | -72.0267 | 301.56915878 | -45.06851113 | 190.5435 | 54761.1055092593 | 54761.6265277778 | 103001040 | 25405.2 | 20000 | 25405.2 | 25405.2 | 0 | 25405.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22263.6 | 22263.6 | 45005.9 | 1 | PROCESSED | 57544.2317013889 | 54557 | 54780.7231134259 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 035001 | Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 3 | AO3 | AO-3 XIS FLIGHT CALIBRATION PLAN | XIS | Y |
| E0102.2-7219 | 16.0024 | -72.0211 | 301.55876018 | -45.07361767 | 248.5277 | 54813.5648263889 | 54814.3092476852 | 103001050 | 29618 | 20000 | 29633.6 | 29634 | 0 | 29618 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27676.9 | 27676.9 | 64293.9 | 0 | PROCESSED | 57544.9487847222 | 54557 | 54839.9906481482 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 035001 | Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 3 | AO3 | AO-3 XIS FLIGHT CALIBRATION PLAN | XIS | Y |
| E0102.2-7219 | 16.0385 | -72.0294 | 301.54384101 | -45.06456362 | 331.5978 | 54899.1304861111 | 54899.6454282407 | 103001060 | 23843.9 | 20000 | 23859.9 | 23843.9 | 0 | 23867.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 21711.2 | 21711.2 | 44463.9 | 0 | PROCESSED | 57545.7459722222 | 54557 | 54916.3664814815 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 035001 | Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 3 | AO3 | AO-3 XIS FLIGHT CALIBRATION PLAN | XIS | Y |
| CYGNUS LOOP | 313.9898 | 32.0072 | 75.70886169 | -8.53902556 | 62.1393 | 54628.6164814815 | 54629.4703125 | 103002010 | 33166.9 | 10000 | 33166.9 | 33166.9 | 0 | 33166.9 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 29636.1 | 29636.1 | 73763.9 | 0 | PROCESSED | 57542.8019097222 | 54557 | 54655.4782523148 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 035001 | Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 3 | AO3 | AO-3 XIS FLIGHT CALIBRATION PLAN | XIS | Y |
| CYGNUS LOOP | 313.9023 | 31.8775 | 75.55993186 | -8.5644348 | 221.2652 | 54811.2228587963 | 54811.8571064815 | 103002020 | 21920.2 | 10000 | 21920.2 | 21920.2 | 0 | 21920.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19489.9 | 19489.9 | 54770 | 0 | PROCESSED | 57544.7157060185 | 54557 | 54826.3522569444 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 035001 | Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 3 | AO3 | AO-3 XIS FLIGHT CALIBRATION PLAN | XIS | Y |
| CYGNUS LOOP (WIN FE) | 313.9898 | 32.0072 | 75.70886169 | -8.53902556 | 62.1393 | 54628.6164814815 | 54629.4703125 | 103003010 | 33166.9 | 20000 | 33166.9 | 33166.9 | 0 | 33166.9 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 29636.1 | 29636.1 | 73763.9 | 0 | PROCESSED | 57542.8161458333 | 54557 | 54655.483287037 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 035001 | Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 3 | AO3 | AO-3 XIS FLIGHT CALIBRATION PLAN | XIS | Y |
| CYGNUS LOOP (WIN FE) | 313.902 | 31.8775 | 75.55976783 | -8.56423835 | 221.2647 | 54811.8571180556 | 54812.4321064815 | 103003020 | 26673.2 | 20000 | 26673.2 | 26673.2 | 0 | 26673.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22795.9 | 22795.9 | 49663.9 | 1 | PROCESSED | 57544.9441550926 | 54557 | 54828.3679166667 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 035001 | Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 3 | AO3 | AO-3 XIS FLIGHT CALIBRATION PLAN | XIS | Y |
| PERSEUS | 49.9468 | 41.518 | 150.56975635 | -13.25755566 | 86.8161 | 54691.602974537 | 54692.6204166667 | 103004010 | 40568.5 | 40000 | 40584.5 | 40568.5 | 0 | 40584.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 31597.9 | 31597.9 | 87897.9 | 1 | PROCESSED | 57543.3051967593 | 54557 | 54710.2764467593 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 035001 | Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 3 | AO3 | AO-3 XIS FLIGHT CALIBRATION PLAN | XIS | Y |
| PERSEUS | 49.9546 | 41.5055 | 150.58184418 | -13.26476244 | 256.0759 | 54873.7298611111 | 54874.8141087963 | 103004020 | 50006.6 | 40000 | 50014.6 | 50014.6 | 0 | 50006.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44840.4 | 44840.4 | 93669.9 | 0 | PROCESSED | 57545.5546875 | 54557 | 54893.3133680556 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 035001 | Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 3 | AO3 | AO-3 XIS FLIGHT CALIBRATION PLAN | XIS | Y |
| PERSEUS (1/4WIN) | 49.9475 | 41.518 | 150.57020557 | -13.25726666 | 86.8158 | 54692.6204282407 | 54693.1071643518 | 103005010 | 21478 | 20000 | 21478 | 21501 | 0 | 21486 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 16992.2 | 16992.2 | 42049.9 | 0 | PROCESSED | 57543.2932175926 | 54557 | 54780.5282291667 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 035001 | Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 3 | AO3 | AO-3 XIS FLIGHT CALIBRATION PLAN | XIS | Y |
| PERSEUS (1/4WIN) | 49.9551 | 41.5057 | 150.58205177 | -13.2643891 | 255.655 | 54874.8146759259 | 54875.4398032407 | 103005020 | 28816.2 | 20000 | 28816.2 | 28840.2 | 0 | 28824.2 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 26779.3 | 26779.3 | 53986 | 0 | PROCESSED | 57545.5219791667 | 54557 | 54893.0113888889 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 035001 | Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 3 | AO3 | AO-3 XIS FLIGHT CALIBRATION PLAN | XIS | Y |
| RXJ1856.5-3754 | 284.1503 | -37.908 | 358.6012758 | -17.21588394 | 280.5087 | 54759.7973148148 | 54761.0974421296 | 103006010 | 43040.2 | 40000 | 43048.2 | 43048.2 | 0 | 43040.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37677.4 | 37677.4 | 112322 | 0 | PROCESSED | 57544.2416550926 | 54557 | 54780.5234837963 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 035001 | Here are the calbiration targets for the XIS: E0102-72 ... 20ks x 6 Cygnus Loop ... 10ks X 2 Cygnus Loop (1/4win 55Fe) ... 20ks x 2 Perseus ... 40ks x 2 Perseus (1/4win) ... 20ks x 2 RXJ1856.5-3754 ... 40ks | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 3 | AO3 | AO-3 XIS FLIGHT CALIBRATION PLAN | XIS | Y |
| CRAB | 83.6308 | 22.0168 | 184.5543577 | -5.78491639 | 87.005 | 54705.3561458333 | 54706.218912037 | 103007010 | 39822 | 40000 | 39822 | 39822 | 0 | 39822 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32782.3 | 32782.3 | 74527.8 | 1 | PROCESSED | 57543.4440277778 | 54557 | 54780.5351851852 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 035002 | We are the HXD team. We propose Crab XIS nominal and HXD nominal observation, each with 40ks exposure for response calibration, a Lockman hole observation with 80 ks exposure for NXB+CXB long term stability study, and a 20ks Cyg X-1 observation for cross-check of Crab calibration. | CALIBRATION | 1 | A | NAKAZAWA | KAZUHIRO | NULL | NULL | JAP | 3 | AO3 | HXD CALIBRATIONS ON AO-3 | XIS | Y |
| CRAB | 83.6295 | 22.0815 | 184.49878495 | -5.75129488 | 87.125 | 54710.3844560185 | 54711.412662037 | 103008010 | 45090 | 40000 | 45090 | 45090 | 0 | 45090 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 33916.7 | 33916.7 | 88827.8 | 0 | PROCESSED | 57545.6288078704 | 54557 | 54780.4386458333 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 035002 | We are the HXD team. We propose Crab XIS nominal and HXD nominal observation, each with 40ks exposure for response calibration, a Lockman hole observation with 80 ks exposure for NXB+CXB long term stability study, and a 20ks Cyg X-1 observation for cross-check of Crab calibration. | CALIBRATION | 1 | A | NAKAZAWA | KAZUHIRO | NULL | NULL | JAP | 3 | AO3 | HXD CALIBRATIONS ON AO-3 | HXD | Y |
| LOCKMANHOLE | 162.9369 | 57.2546 | 149.70462232 | 53.2017902 | 281.5296 | 54604.4635300926 | 54606.0529398148 | 103009010 | 83419.7 | 80000 | 83419.7 | 83419.7 | 0 | 83419.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 87485.2 | 87485.2 | 137300 | 3 | PROCESSED | 57542.5921412037 | 54557 | 54616.4206597222 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 035002 | We are the HXD team. We propose Crab XIS nominal and HXD nominal observation, each with 40ks exposure for response calibration, a Lockman hole observation with 80 ks exposure for NXB+CXB long term stability study, and a 20ks Cyg X-1 observation for cross-check of Crab calibration. | CALIBRATION | 1 | A | NAKAZAWA | KAZUHIRO | NULL | NULL | JAP | 3 | AO3 | HXD CALIBRATIONS ON AO-3 | XIS | Y |
| PKS2155-304 | 329.7153 | -30.2277 | 17.72680762 | -52.24467434 | 58.2307 | 54598.5708912037 | 54599.1120138889 | 103011010 | 23119 | 20000 | 23119 | 23119 | 0 | 23119 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17813.1 | 17813.1 | 46745.9 | 0 | PROCESSED | 57542.5125810185 | 54557 | 54608.9900115741 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 035003 | XMM/Chandra/Suzaku cross calibration by an coordinated observation of PKS215-304. | CALIBRATION | 1 | A | ISHIDA | MANABU | NULL | NULL | JAP | 3 | AO3 | COORDINATED OBSERVATION FOR CROSS-CALIBRATION WITH PKS2155-304 | XIS | Y |
| CRAB | 83.6356 | 21.9544 | 184.60973125 | -5.81455843 | 269.3968 | 54923.0747337963 | 54924.0418287037 | 104001010 | 42105.2 | 40000 | 42808.5 | 42105.2 | 0 | 42808.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 33587.7 | 33587.7 | 83539.8 | 0 | PROCESSED | 57546.0901273148 | 54922 | 54949.4458680556 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 045003 | N/A | CALIBRATION | 1 | A | NAKAZAWA | KAZUHIRO | NULL | NULL | JAP | 4 | AO4 | CRAB CAL 2009 | HXD | Y |
| CRAB | 83.6363 | 22.0087 | 184.56397797 | -5.78494551 | 270.0021 | 55250.0427199074 | 55251.1904976852 | 104001070 | 45830.9 | 40000 | 45830.9 | 45830.9 | 0 | 45830.9 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 16318 | 16318 | 99157.9 | 1 | PROCESSED | 57550.7280555556 | 54922 | 55267.2846643518 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 045003 | N/A | CALIBRATION | 1 | A | NAKAZAWA | KAZUHIRO | NULL | NULL | JAP | 4 | AO4 | CRAB CAL 2009 | XIS | Y |
| LOCKMAN HOLE | 162.9377 | 57.2549 | 149.70376614 | 53.20190951 | 281.53 | 54994.3039351852 | 54996.0634375 | 104002010 | 92848.4 | 80000 | 92848.4 | 92848.4 | 0 | 92848.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 79880 | 79880 | 152000 | 0 | PROCESSED | 57547.574537037 | 54922 | 55005.1389814815 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 045004 | HXD / XIS NXB/ CXB cal | CALIBRATION | 1 | A | NAKAZAWA | KAZUHIRO | NULL | NULL | JAP | 4 | AO4 | LOCKMAN HOLE 2009 | XIS | Y |
| LOCKMAN HOLE | 162.9419 | 57.2782 | 149.67240249 | 53.18794557 | 110.367 | 55161.4316319444 | 55161.7502199074 | 104002020 | 2359.1 | 12000 | 2383.1 | 2359.1 | 0 | 2375.1 | 5 | 2 | 0 | 3 | 1 | 0 | 0 | 10017.4 | 10017.4 | 27515.9 | 0 | PROCESSED | 57549.5740972222 | 54922 | 55182.6514467593 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 045004 | HXD / XIS NXB/ CXB cal | CALIBRATION | 1 | A | NAKAZAWA | KAZUHIRO | NULL | NULL | JAP | 4 | AO4 | LOCKMAN HOLE 2009 | XIS | Y |
| PKS2155-304 | 329.7145 | -30.2263 | 17.72895666 | -52.2438339 | 83.4423 | 54978.6583217593 | 54980.486400463 | 104004010 | 62440.1 | 60000 | 62440.1 | 62440.1 | 0 | 62440.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 53071.7 | 53071.7 | 157931.8 | 2 | PROCESSED | 57546.7456828704 | 54922 | 54994.3621296296 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 045006 | This is a cross calibration observation with PKD2155-304 among Suzaku, XMM-Newton and Chandra. | CALIBRATION | 1 | A | ISHIDA | MANABU | NULL | NULL | JAP | 4 | AO4 | CROSS CALIBRATION OF SUZAKU/XMM/CHANDRA WITH PKS2155-304 | XIS | Y |
| E0102-72 | 16.0343 | -72.0367 | 301.54639234 | -45.05737191 | 19.8885 | 54944.6369560185 | 54945.6225 | 104005010 | 45028.7 | 20000 | 45654.5 | 45028.7 | 0 | 45654.5 | 3 | 2 | 0 | 3 | 1 | 0 | 0 | 49726.9 | 49726.9 | 85135.8 | 1 | PROCESSED | 57546.255 | 54922 | 54966.3543518518 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 045007 | We propose some observations for the calibtaions of XIS. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 4 | AO4 | XIS FLIGHT CALIBRATION IN AO4 | XIS | Y |
| E0102-72 | 16.0181 | -72.0439 | 301.55415549 | -45.05053701 | 69.1611 | 55008.1544097222 | 55008.571087963 | 104006010 | 22061.5 | 20000 | 22061.5 | 22061.5 | 0 | 22061.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16326.3 | 16326.3 | 35991.9 | 1 | PROCESSED | 57547.682662037 | 54922 | 55022.2400694445 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 045007 | We propose some observations for the calibtaions of XIS. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 4 | AO4 | XIS FLIGHT CALIBRATION IN AO4 | XIS | Y |
| E0102-72 | 15.9824 | -72.0274 | 301.56809353 | -45.06775773 | 194.7588 | 55130.7598148148 | 55131.4169444444 | 104007010 | 20375.6 | 20000 | 20383.6 | 20383.6 | 0 | 20375.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18037.9 | 18037.9 | 56761.8 | 1 | PROCESSED | 57549.0115277778 | 54922 | 55141.2502777778 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 045007 | We propose some observations for the calibtaions of XIS. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 4 | AO4 | XIS FLIGHT CALIBRATION IN AO4 | XIS | Y |
| E0102-72 | 15.9813 | -72.0285 | 301.56867985 | -45.06668362 | 180.8386 | 55115.6048032407 | 55116.6237615741 | 104008010 | 31449.9 | 20000 | 31449.9 | 49641.1 | 0 | 49935.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43716.7 | 43716.7 | 88013.9 | 1 | PROCESSED | 57548.8638541667 | 54922 | 55134.4398842593 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 045007 | We propose some observations for the calibtaions of XIS. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 4 | AO4 | XIS FLIGHT CALIBRATION IN AO4 | XIS | Y |
| E0102-72 | 16.0091 | -72.0251 | 301.55623091 | -45.06948422 | 251.7193 | 55190.9159837963 | 55191.5411921296 | 104009010 | 21985.2 | 20000 | 21993.2 | 21985.2 | 0 | 21993.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21639.6 | 21639.6 | 54016 | 0 | PROCESSED | 57549.9296180556 | 54922 | 55225.1469328704 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 045007 | We propose some observations for the calibtaions of XIS. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 4 | AO4 | XIS FLIGHT CALIBRATION IN AO4 | XIS | Y |
| E0102-72 | 16.0186 | -72.0293 | 301.55250278 | -45.06509107 | 296.1745 | 55231.7435069444 | 55232.4343055556 | 104010010 | 20500.6 | 20000 | 20508.6 | 20500.6 | 0 | 20508.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 24497.1 | 24497.1 | 59675.9 | 2 | PROCESSED | 57550.4799652778 | 54922 | 55249.7236111111 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 045007 | We propose some observations for the calibtaions of XIS. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 4 | AO4 | XIS FLIGHT CALIBRATION IN AO4 | XIS | Y |
| E0102-72 1/4 WIN | 15.9806 | -72.0277 | 301.56890722 | -45.06749655 | 189.3214 | 55124.8016203704 | 55125.3654282407 | 104011010 | 19091.3 | 20000 | 19091.3 | 20038.1 | 0 | 20038.1 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 16209 | 16209 | 48711.9 | 1 | PROCESSED | 57548.9278472222 | 54922 | 55134.1777777778 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 045007 | We propose some observations for the calibtaions of XIS. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 4 | AO4 | XIS FLIGHT CALIBRATION IN AO4 | XIS | Y |
| E0102-72 1/4 WIN | 16.0261 | -72.0284 | 301.54914583 | -45.06582801 | 296.9556 | 55232.435150463 | 55233.0002777778 | 104012010 | 23553.7 | 20000 | 23553.7 | 23553.7 | 0 | 23560 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25339.4 | 25339.4 | 48815.9 | 0 | PROCESSED | 57550.4981481482 | 54922 | 55266.2358449074 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 045007 | We propose some observations for the calibtaions of XIS. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 4 | AO4 | XIS FLIGHT CALIBRATION IN AO4 | XIS | Y |
| E0102-72 PSUM | 15.9904 | -72.0242 | 301.56429483 | -45.07078046 | 218.0047 | 55166.9023032407 | 55167.9336111111 | 104014010 | 62658.9 | 20000 | 63019.2 | 62658.9 | 0 | 63011.2 | 1 | 2 | 0 | 1 | 1 | 0 | 0 | 54915.1 | 54915.1 | 89091.8 | 1 | PROCESSED | 57549.6857060185 | 54922 | 55181.4406365741 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 045007 | We propose some observations for the calibtaions of XIS. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 4 | AO4 | XIS FLIGHT CALIBRATION IN AO4 | XIS | N |
| CYGNUS LOOP NE2 | 313.9438 | 31.9667 | 75.6521583 | -8.53477618 | 43.0005 | 54998.5732407407 | 54998.7883449074 | 104015010 | 10889.7 | 10000 | 10889.7 | 10889.7 | 0 | 10889.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 9923 | 9923 | 18577.9 | 0 | PROCESSED | 57547.5743518518 | 54922 | 55008.1053356482 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 045007 | We propose some observations for the calibtaions of XIS. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 4 | AO4 | XIS FLIGHT CALIBRATION IN AO4 | XIS | Y |
| CYGNUS LOOP NE2 | 313.9634 | 31.9567 | 75.65508045 | -8.55396375 | 223.0007 | 55175.7922106482 | 55176.0640509259 | 104016010 | 12573.5 | 10000 | 12573.5 | 12573.5 | 0 | 12573.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10077.6 | 10077.6 | 23479.9 | 0 | PROCESSED | 57549.7463541667 | 54922 | 55189.115625 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 045007 | We propose some observations for the calibtaions of XIS. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 4 | AO4 | XIS FLIGHT CALIBRATION IN AO4 | XIS | Y |
| CYGNUS LOOP P8 | 313.9958 | 31.4752 | 75.29735897 | -8.88195371 | 62.5173 | 54998.7930787037 | 54999.0668865741 | 104017010 | 9708.7 | 10000 | 9708.7 | 9708.7 | 0 | 9708.7 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 6711.9 | 6711.9 | 23652 | 1 | PROCESSED | 57547.5808101852 | 54922 | 55008.151087963 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 045007 | We propose some observations for the calibtaions of XIS. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 4 | AO4 | XIS FLIGHT CALIBRATION IN AO4 | XIS | Y |
| PERSEUS | 49.9444 | 41.5171 | 150.56872595 | -13.25929731 | 66.998 | 55069.1669907407 | 55070.1453009259 | 104018010 | 41279.8 | 40000 | 41279.8 | 41279.8 | 0 | 41295.8 | 4 | 3 | 0 | 3 | 1 | 0 | 0 | 37348.8 | 37348.8 | 84499.8 | 1 | PROCESSED | 57548.366412037 | 54922 | 55088.1261458333 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 045007 | We propose some observations for the calibtaions of XIS. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 4 | AO4 | XIS FLIGHT CALIBRATION IN AO4 | XIS | Y |
| PERSEUS | 49.9512 | 41.4934 | 150.58651783 | -13.27626038 | 277.3248 | 55228.3356944444 | 55229.2502199074 | 104019010 | 38615.1 | 40000 | 38615.1 | 38615.1 | 0 | 38615.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35781.4 | 35781.4 | 78997.9 | 0 | PROCESSED | 57550.4707523148 | 54922 | 55249.7985069444 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 045007 | We propose some observations for the calibtaions of XIS. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 4 | AO4 | XIS FLIGHT CALIBRATION IN AO4 | XIS | Y |
| PERSEUS 1/4 WIN | 49.9444 | 41.516 | 150.56934906 | -13.260215 | 66.9976 | 55070.1453125 | 55071.500162037 | 104020010 | 55044.9 | 20000 | 55067.7 | 55052.9 | 0 | 55044.9 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 51280.2 | 51280.2 | 117049.8 | 2 | PROCESSED | 57548.3782986111 | 54922 | 55109.4175115741 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 045007 | We propose some observations for the calibtaions of XIS. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 4 | AO4 | XIS FLIGHT CALIBRATION IN AO4 | XIS | Y |
| PERSEUS 1/4 WIN | 49.9506 | 41.4949 | 150.58528271 | -13.27525693 | 276.9447 | 55229.250787037 | 55229.7078587963 | 104021010 | 21641.5 | 20000 | 21649.1 | 21646.9 | 0 | 21641.5 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 21574.3 | 21574.3 | 39482 | 0 | PROCESSED | 57550.454212963 | 54922 | 55249.7129513889 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 045007 | We propose some observations for the calibtaions of XIS. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 4 | AO4 | XIS FLIGHT CALIBRATION IN AO4 | XIS | Y |
| RXJ1856.5 | 284.1483 | -37.909 | 358.59969969 | -17.21477781 | 277.829 | 55127.9550115741 | 55128.8363425926 | 104022010 | 43484.5 | 40000 | 43484.5 | 43492.5 | 0 | 43492.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39424.6 | 39424.6 | 76101.8 | 0 | PROCESSED | 57548.9638657407 | 54922 | 55141.2812384259 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 045007 | We propose some observations for the calibtaions of XIS. | CALIBRATION | 1 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 4 | AO4 | XIS FLIGHT CALIBRATION IN AO4 | XIS | Y |
| RXJ1856.5 | 284.0709 | -37.7784 | 358.70367738 | -17.11026819 | 79.4744 | 55269.4572569444 | 55270.6856944444 | 104022020 | 40415.2 | 40000 | 40426.9 | 40415.2 | 0 | 40415.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34577.2 | 34577.2 | 106107.9 | 0 | PROCESSED | 57550.9002199074 | 54922 | 55285.0858564815 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 045007 | We propose some observations for the calibtaions of XIS. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 4 | AO4 | XIS FLIGHT CALIBRATION IN AO4 | XIS | Y |
| RXJ1856.5 | 284.1421 | -37.9072 | 358.59959193 | -17.20956639 | 77.5864 | 55281.1527083333 | 55282.3710069444 | 104022030 | 42450.9 | 40000 | 42450.9 | 42450.9 | 0 | 42450.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11139.6 | 11139.6 | 105252 | 2 | PROCESSED | 57551.0588773148 | 54922 | 55301.2941203704 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 045007 | We propose some observations for the calibtaions of XIS. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 4 | AO4 | XIS FLIGHT CALIBRATION IN AO4 | XIS | Y |
| G21.5-0.9 | 278.3939 | -10.5728 | 21.49883061 | -0.89086145 | 264.65 | 55114.5957986111 | 55115.5953009259 | 104023010 | 40156.1 | 40000 | 40156.1 | 40156.1 | 0 | 40156.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30452.1 | 30452.1 | 86354 | 0 | PROCESSED | 57548.8377662037 | 54922 | 55131.2519675926 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 045008 | We propose G21.5-0.9 observation for the cross-calibtaions of XIS. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 4 | AO4 | CROSS CALIBRATION OF G21.5-0.9 | XIS | Y |
| PKS2155-304 | 329.7122 | -30.2251 | 17.73054892 | -52.24172704 | 58.9372 | 55313.9868171296 | 55315.8536458333 | 105001010 | 63457.2 | 60000 | 63465.2 | 63471 | 0 | 63457.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 54701.5 | 54701.5 | 161277.8 | 2 | PROCESSED | 57551.3529513889 | 55287 | 55327.3816087963 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 055001 | This observation of PKS2155-304 is coordinated with XMM-Newton and Chandra. | CALIBRATION | 1 | A | ISHIDA | MANABU | NULL | NULL | JAP | 5 | AO5 | COORDINATED OBSERVATION OF PKS2155-304 WITH CHANDRA AND XMM-NEWTON | XIS | Y |
| CRAB | 83.6381 | 22.0079 | 184.56555504 | -5.78396412 | 269.4791 | 55291.5258680556 | 55292.5001273148 | 105002010 | 481.5 | 40000 | 481.5 | 481.6 | 0 | 481.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 33897.4 | 33897.4 | 84133.8 | 1 | PROCESSED | 57551.1472800926 | 55287 | 55350.3368981482 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 055002 | We propose an annual calibration of Crab, as a standard candle from 1 kev upto 500 keV. | CALIBRATION | 1 | A | NAKAZAWA | KAZUHIRO | NULL | NULL | JAP | 5 | AO5 | AO-5 CRAB CALIBRATION | XIS | Y |
| LOCKMAN_HOLE | 162.9382 | 57.2507 | 149.70866001 | 53.20492954 | 279.8869 | 55358.311875 | 55360.0828935185 | 105003010 | 77997.6 | 80000 | 78013.6 | 77997.6 | 0 | 78258.3 | 2 | 2 | 0 | 1 | 1 | 0 | 0 | 73083.2 | 73083.2 | 152981.8 | 1 | PROCESSED | 57552.0549074074 | 55287 | 55370.3379861111 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 055003 | 2010 Annual observation of Lockman hole, with XIS in the Psum mode. | CALIBRATION | 1 | A | NAKAZAWA | KAZUHIRO | NULL | NULL | JAP | 5 | AO5 | LOCKMAN HOLE | XIS | N |
| E0102-72 | 16.0161 | -72.0335 | 301.55400478 | -45.06095473 | 357.7405 | 55291.0014699074 | 55291.5147453704 | 105004010 | 21592.8 | 20000 | 21592.8 | 21592.8 | 0 | 21592.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17139 | 17139 | 44311.9 | 0 | PROCESSED | 57551.0826388889 | 55287 | 55306.2144328704 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 055004 | We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF X-RAY IMAGING SPECTROMETER | XIS | Y |
| E0102-72 | 16.0035 | -72.0383 | 301.55996349 | -45.05643533 | 65.2308 | 55366.1296412037 | 55366.7869791667 | 105004020 | 19230.2 | 20000 | 19238.2 | 19238.2 | 0 | 19230.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16589.5 | 16589.5 | 56783.9 | 2 | PROCESSED | 57552.3804861111 | 55287 | 55413.4019097222 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 055004 | We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF X-RAY IMAGING SPECTROMETER | XIS | Y |
| E0102-72 | 16.0129 | -72.0282 | 301.55487873 | -45.06631044 | 194.5389 | 55495.8125694444 | 55496.3217939815 | 105004040 | 20018.9 | 20000 | 20619.9 | 20018.9 | 0 | 20643.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19219.3 | 19219.3 | 43988 | 0 | PROCESSED | 57553.8484143518 | 55287 | 55505.2302893518 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 055004 | We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF X-RAY IMAGING SPECTROMETER | XIS | Y |
| E0102-72 | 16.0026 | -72.0263 | 301.55918173 | -45.06842583 | 227.0923 | 55539.0256481482 | 55539.487662037 | 105004050 | 20046.8 | 20000 | 20070.8 | 20070.8 | 0 | 20046.8 | 1 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 39913.9 | 0 | PROCESSED | 57554.3461921296 | 55287 | 55552.4359953704 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 055004 | We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF X-RAY IMAGING SPECTROMETER | XIS | Y |
| E0102-72 | 16.0173 | -72.0347 | 301.55359992 | -45.05973194 | 299.5457 | 55600.0152430556 | 55600.4516319444 | 105004060 | 17242.6 | 20000 | 17258.6 | 17242.6 | 0 | 17258.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13743.2 | 13743.2 | 37695.9 | 0 | PROCESSED | 57600.8649305556 | 55287 | 55617.4086805556 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 055004 | We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF X-RAY IMAGING SPECTROMETER | XIS | Y |
| E0102-72_1_4_WIN | 16.0018 | -72.0347 | 301.56035188 | -45.06006295 | 65.8655 | 55366.7877314815 | 55367.3098842593 | 105005010 | 20345.6 | 20000 | 20353.6 | 20345.6 | 0 | 20361.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17482.3 | 17482.3 | 45080 | 2 | PROCESSED | 57552.3703356482 | 55287 | 55400.4271412037 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 055004 | We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF X-RAY IMAGING SPECTROMETER | XIS | Y |
| E0102-72_1_4_WIN | 16.0156 | -72.0284 | 301.55372169 | -45.06605315 | 226.5285 | 55539.4883680556 | 55540.2502546296 | 105005020 | 22538.8 | 20000 | 22546.8 | 22538.8 | 0 | 22554.8 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 5796.9 | 5796.9 | 65821.9 | 2 | PROCESSED | 57554.3662731482 | 55287 | 55550.9436689815 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 055004 | We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF X-RAY IMAGING SPECTROMETER | XIS | Y |
| E0102-72_PSUM | 15.883 | -72.0319 | 301.61184542 | -45.06533979 | 66.3881 | 55367.3105439815 | 55368.5202314815 | 105006010 | 356.5 | 40000 | 356.5 | 356.5 | 0 | 356.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 303 | 303 | 36191.9 | 0 | PROCESSED | 57552.3753356482 | 55287 | 55400.4299537037 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 055004 | We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF X-RAY IMAGING SPECTROMETER | XIS | N |
| E0102-72_PSUM | 16.0136 | -72.0296 | 301.55471109 | -45.06489883 | 226.8844 | 55537.8034375 | 55539.0252199074 | 105006020 | 40871.5 | 40000 | 40936.3 | 40871.5 | 0 | 41120.5 | 4 | 3 | 0 | 1 | 1 | 0 | 0 | 157.4 | 157.4 | 105549.9 | 0 | PROCESSED | 57554.3595717593 | 55287 | 55778.433275463 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 055004 | We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF X-RAY IMAGING SPECTROMETER | XIS | N |
| E0102-72_PSUM | 16.0081 | -72.0302 | 301.5571666 | -45.06441782 | 138.5223 | 55437.769525463 | 55438.8884606482 | 105006030 | 37067.5 | 40000 | 37083.1 | 37067.5 | 0 | 37636.5 | 2 | 2 | 0 | 1 | 1 | 0 | 0 | 33043.8 | 33043.8 | 96641.9 | 1 | PROCESSED | 57553.21875 | 55287 | 55449.0261574074 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 055004 | We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF X-RAY IMAGING SPECTROMETER | XIS | N |
| CYGNUS LOOP P8 | 313.9885 | 31.4813 | 75.29810685 | -8.87326903 | 62.5188 | 55358.0139583333 | 55358.3015393518 | 105007010 | 12093.9 | 10000 | 12881.6 | 12093.9 | 0 | 12889.6 | 2 | 3 | 0 | 2 | 1 | 0 | 0 | 9985.5 | 9985.5 | 24839.9 | 0 | PROCESSED | 57551.995474537 | 55287 | 55376.4220717593 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 055004 | We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF X-RAY IMAGING SPECTROMETER | XIS | Y |
| CYGNUS LOOP P8 CI 6 | 314.021 | 31.4644 | 75.3027873 | -8.90540252 | 222.2994 | 55552.9622569444 | 55553.0467824074 | 105007020 | 2740 | 10000 | 2755.6 | 2740 | 0 | 2755.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 2487.4 | 2487.4 | 7295.9 | 0 | PROCESSED | 57554.4917361111 | 55287 | 55593.2584722222 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 055004 | We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF X-RAY IMAGING SPECTROMETER | XIS | Y |
| CYGNUS LOOP P8 CI 2 | 314.0088 | 31.4691 | 75.29974588 | -8.89438689 | 222.2165 | 55553.0469791667 | 55553.1446990741 | 105007030 | 4963.1 | 10000 | 4987 | 4979 | 0 | 4963.1 | 1 | 2 | 0 | 1 | 1 | 0 | 0 | 3566.5 | 3566.5 | 8431.9 | 0 | PROCESSED | 57554.4921875 | 55287 | 55593.2653587963 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 055004 | We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF X-RAY IMAGING SPECTROMETER | XIS | Y |
| RXJ1856.5-3754 | 284.1491 | -37.9166 | 358.59252855 | -17.21813017 | 271.239 | 55496.329537037 | 55497.4509722222 | 105008010 | 40091.7 | 40000 | 40091.7 | 40099.7 | 0 | 40107.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32908.1 | 32908.1 | 96875.8 | 0 | PROCESSED | 57553.8765740741 | 55287 | 55509.0637731482 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 055004 | We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF X-RAY IMAGING SPECTROMETER | XIS | Y |
| PERSEUS | 49.9406 | 41.5199 | 150.56470121 | -13.25852998 | 66.581 | 55417.3825925926 | 55418.010625 | 105009010 | 33624.2 | 40000 | 33624.2 | 33624.2 | 0 | 33624.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37659.6 | 37659.6 | 54254 | 0 | PROCESSED | 57552.9264351852 | 55287 | 55428.0593171296 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 055004 | We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF X-RAY IMAGING SPECTROMETER | XIS | Y |
| PERSEUS | 49.9557 | 41.5028 | 150.58408011 | -13.26656036 | 259.7325 | 55595.0249421296 | 55595.9578472222 | 105009020 | 40461.1 | 40000 | 40469.1 | 40461.1 | 0 | 40477.1 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 29594.3 | 29594.3 | 80593.9 | 1 | PROCESSED | 57600.8453472222 | 55287 | 55610.273587963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 055004 | We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF X-RAY IMAGING SPECTROMETER | XIS | Y |
| PERSEUS_1_4_WIN | 49.9403 | 41.521 | 150.56388564 | -13.25773608 | 66.5805 | 55418.0106365741 | 55418.6467476852 | 105010010 | 27372.7 | 20000 | 27372.7 | 27380.4 | 0 | 27386.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 33712.7 | 33712.7 | 54955.9 | 1 | PROCESSED | 57552.9240509259 | 55287 | 55428.0721759259 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 055004 | We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF X-RAY IMAGING SPECTROMETER | XIS | Y |
| PERSEUS_1_4_WIN | 49.9552 | 41.5037 | 150.58324921 | -13.26601613 | 259.969 | 55594.4623958333 | 55595.0245138889 | 105010020 | 21092.6 | 20000 | 21096.3 | 21096.3 | 0 | 21092.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16573 | 16573 | 48559.9 | 0 | PROCESSED | 57600.8212847222 | 55287 | 55610.2645717593 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 055004 | We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF X-RAY IMAGING SPECTROMETER | XIS | Y |
| N132D | 81.279 | -69.6505 | 280.31295018 | -32.77613267 | 32.9954 | 55404.1821296296 | 55405.1411226852 | 105011010 | 35849.5 | 30000 | 35849.5 | 35849.5 | 0 | 35849.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32540.9 | 32540.9 | 82839.8 | 1 | PROCESSED | 57552.7373842593 | 55287 | 55414.1006828704 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 055005 | We propose a observation of N132D for the calibration of the XIS in the AO5 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF X-RAY IMAGING SPECTROMETER | XIS | Y |
| CRAB_80OFF_0DEG | 83.6952 | 20.686 | 185.71797799 | -6.44521522 | 87.4149 | 55452.6214467593 | 55453.046712963 | 105012010 | 19241.5 | 20000 | 19241.5 | 19241.5 | 0 | 19241.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17364.4 | 17364.4 | 36736 | 0 | PROCESSED | 57553.4108796296 | 55287 | 55463.4094212963 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 055006 | For better understanding of stray light levels we propose Crab offset observations for 180 ks in total. | CALIBRATION | 1 | A | TAKEI | YOH | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF STRAY LIGHT | SPE | Y |
| CRAB_80OFF_22.5DEG | 83.1525 | 20.7619 | 185.38009186 | -6.83349718 | 86.9209 | 55453.0474189815 | 55453.4918518518 | 105013010 | 18989.1 | 20000 | 18989.1 | 18989.1 | 0 | 18989.1 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13723 | 13723 | 38376 | 0 | PROCESSED | 57553.4129166667 | 55287 | 55463.4117013889 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 055006 | For better understanding of stray light levels we propose Crab offset observations for 180 ks in total. | CALIBRATION | 1 | A | TAKEI | YOH | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF STRAY LIGHT | SPE | Y |
| CRAB_80OFF_45DEG | 82.6663 | 21.0307 | 184.90557346 | -7.07161845 | 87.0482 | 55453.4925578704 | 55453.9550115741 | 105014010 | 20599.2 | 20000 | 20607.2 | 20607.2 | 0 | 20599.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19812.1 | 19812.1 | 39937.9 | 2 | PROCESSED | 57553.4202662037 | 55287 | 55463.4144675926 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 055006 | For better understanding of stray light levels we propose Crab offset observations for 180 ks in total. | CALIBRATION | 1 | A | TAKEI | YOH | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF STRAY LIGHT | SPE | Y |
| CRAB_50OFF_45DEG | 83.0202 | 21.413 | 184.76043538 | -6.58765564 | 87.6753 | 55431.8338194445 | 55432.0682291667 | 105015010 | 10549.2 | 10000 | 11277.2 | 10549.2 | 0 | 11277.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10191.7 | 10191.7 | 20245.9 | 1 | PROCESSED | 57553.1744444444 | 55287 | 55446.446875 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 055006 | For better understanding of stray light levels we propose Crab offset observations for 180 ks in total. | CALIBRATION | 1 | A | TAKEI | YOH | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF STRAY LIGHT | SPE | Y |
| CRAB_50OFF_135DEG | 82.9576 | 22.5813 | 183.73915584 | -6.0064164 | 86.6565 | 55432.0694907407 | 55432.3105555556 | 105016010 | 6489.4 | 10000 | 6489.4 | 6497.4 | 0 | 6497.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 3638.1 | 3638.1 | 20822 | 0 | PROCESSED | 57553.1780439815 | 55287 | 55446.4488425926 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 055006 | For better understanding of stray light levels we propose Crab offset observations for 180 ks in total. | CALIBRATION | 1 | A | TAKEI | YOH | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF STRAY LIGHT | SPE | Y |
| CRAB_50OFF_225DEG | 84.2344 | 22.6444 | 184.32067652 | -4.97776831 | 87.1427 | 55432.3115856482 | 55432.5827777778 | 105017010 | 12345.6 | 10000 | 12353.6 | 12345.6 | 0 | 12361.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12151 | 12151 | 23423.9 | 0 | PROCESSED | 57553.1875347222 | 55287 | 55447.4086921296 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 055006 | For better understanding of stray light levels we propose Crab offset observations for 180 ks in total. | CALIBRATION | 1 | A | TAKEI | YOH | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF STRAY LIGHT | SPE | Y |
| CRAB_50OFF_315DEG | 84.2968 | 21.4693 | 185.35120349 | -5.55324373 | 87.1743 | 55432.5838078704 | 55432.8980555556 | 105018010 | 14432.3 | 10000 | 14432.3 | 14456.3 | 0 | 14440.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12415.6 | 12415.6 | 27143.9 | 1 | PROCESSED | 57553.1893865741 | 55287 | 55447.4099884259 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 055006 | For better understanding of stray light levels we propose Crab offset observations for 180 ks in total. | CALIBRATION | 1 | A | TAKEI | YOH | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF STRAY LIGHT | SPE | Y |
| CRAB_65OFF_0DEG | 83.6859 | 20.9369 | 185.49975653 | -6.31874712 | 87.2696 | 55446.25 | 55446.4605439815 | 105019010 | 9657.5 | 10000 | 9657.5 | 9657.5 | 0 | 9657.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7899.5 | 7899.5 | 18183.9 | 0 | PROCESSED | 57553.3143634259 | 55287 | 55461.3910763889 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 055006 | For better understanding of stray light levels we propose Crab offset observations for 180 ks in total. | CALIBRATION | 1 | A | TAKEI | YOH | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF STRAY LIGHT | SPE | Y |
| CRAB_65OFF_45DEG | 82.8482 | 21.2156 | 184.84096902 | -6.82899548 | 86.9607 | 55446.4614351852 | 55446.6875694444 | 105020010 | 9450.4 | 10000 | 9458.4 | 9450.4 | 0 | 9458.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 7906.9 | 7906.9 | 19533.9 | 0 | PROCESSED | 57553.3146643518 | 55287 | 55461.3925231482 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 055006 | For better understanding of stray light levels we propose Crab offset observations for 180 ks in total. | CALIBRATION | 1 | A | TAKEI | YOH | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF STRAY LIGHT | SPE | Y |
| CRAB_65OFF_90DEG | 82.4629 | 21.9742 | 184.00329077 | -6.72000946 | 87.3211 | 55446.6885532407 | 55446.9076967593 | 105021010 | 10912 | 10000 | 10921.9 | 10920 | 0 | 10912 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10033.9 | 10033.9 | 18930 | 0 | PROCESSED | 57553.3193634259 | 55287 | 55461.3931944444 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 055006 | For better understanding of stray light levels we propose Crab offset observations for 180 ks in total. | CALIBRATION | 1 | A | TAKEI | YOH | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF STRAY LIGHT | SPE | Y |
| CRAB_65OFF_135DEG | 82.7613 | 22.7517 | 183.49649927 | -6.06655162 | 87.038 | 55446.9086805556 | 55447.1314236111 | 105022010 | 9248.2 | 10000 | 9248.2 | 9248.2 | 0 | 9248.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 7939.3 | 7939.3 | 19237.9 | 0 | PROCESSED | 57553.3269791667 | 55287 | 55466.4006365741 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 055006 | For better understanding of stray light levels we propose Crab offset observations for 180 ks in total. | CALIBRATION | 1 | A | TAKEI | YOH | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF STRAY LIGHT | SPE | Y |
| CRAB_65OFF_180DEG | 83.5739 | 23.1022 | 183.60559643 | -5.24730073 | 87.2466 | 55447.1322685185 | 55447.3557291667 | 105023010 | 11470.6 | 10000 | 11470.6 | 11478.6 | 0 | 11478.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10091.3 | 10091.3 | 19295.9 | 0 | PROCESSED | 57553.3272222222 | 55287 | 55461.3950810185 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 055006 | For better understanding of stray light levels we propose Crab offset observations for 180 ks in total. | CALIBRATION | 1 | A | TAKEI | YOH | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF STRAY LIGHT | SPE | Y |
| CRAB_65OFF_225DEG | 84.3921 | 22.8458 | 184.22714627 | -4.7474889 | 85.6608 | 55447.3571296296 | 55447.5793402778 | 105024010 | 9404.2 | 10000 | 9412.2 | 9404.2 | 0 | 9420.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7822.5 | 7822.5 | 19191.9 | 0 | PROCESSED | 57553.3290277778 | 55287 | 55461.3963541667 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 055006 | For better understanding of stray light levels we propose Crab offset observations for 180 ks in total. | CALIBRATION | 1 | A | TAKEI | YOH | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF STRAY LIGHT | SPE | Y |
| CRAB_65OFF_270DEG | 84.7966 | 22.0949 | 185.06495422 | -4.82832438 | 86.3168 | 55447.5802777778 | 55447.7918287037 | 105025010 | 8891 | 10000 | 8891 | 8891 | 0 | 8891 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8535 | 8535 | 18273.9 | 0 | PROCESSED | 57553.3358680556 | 55287 | 55461.3998032407 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 055006 | For better understanding of stray light levels we propose Crab offset observations for 180 ks in total. | CALIBRATION | 1 | A | TAKEI | YOH | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF STRAY LIGHT | SPE | Y |
| CRAB_65OFF_315DEG | 84.4913 | 21.2878 | 185.60226135 | -5.4958009 | 87.6059 | 55447.7930902778 | 55448.0217824074 | 105026010 | 11382 | 10000 | 11390 | 11390 | 0 | 11382 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 9884.1 | 9884.1 | 19750 | 0 | PROCESSED | 57553.3379398148 | 55287 | 55461.4004050926 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 055006 | For better understanding of stray light levels we propose Crab offset observations for 180 ks in total. | CALIBRATION | 1 | A | TAKEI | YOH | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF STRAY LIGHT | SPE | Y |
| PERSEUS_CI_6 | 49.9577 | 41.5001 | 150.58689381 | -13.26798644 | 252.2456 | 55614.2081365741 | 55615.187662037 | 105027010 | 45272.2 | 40000 | 45905.5 | 45272.2 | 0 | 45905.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41885.9 | 41885.9 | 84609.8 | 0 | PROCESSED | 57601.0380092593 | 55287 | 55624.2249421296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 055004 | We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF X-RAY IMAGING SPECTROMETER | XIS | Y |
| PERSEUS_1_4_WIN_CI_6 | 49.9565 | 41.5014 | 150.58538691 | -13.26739774 | 252.427 | 55613.7422106482 | 55614.2078009259 | 105028010 | 20636.3 | 20000 | 20636.3 | 20636.3 | 0 | 20636.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17845 | 17845 | 40215.9 | 0 | PROCESSED | 57600.9969328704 | 55287 | 55624.1639814815 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 055004 | We propose a set of observations for the calibration of the XIS in the AO5 cycle. This is for routine calibration, and additional telescope times may be requested for discontinuous changes of the instrumental performance. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 5 | AO5 | CALIBRATION OF X-RAY IMAGING SPECTROMETER | XIS | Y |
| CRAB | 83.6359 | 22.0094 | 184.56318415 | -5.78488405 | 269.6199 | 55641.8131828704 | 55643.1459490741 | 105029010 | 614.6 | 40000 | 614.6 | 614.6 | 0 | 614.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36940.8 | 36940.8 | 115139.9 | 0 | PROCESSED | 57601.3233333333 | 55287 | 55652.1669097222 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 055002 | We propose an annual calibration of Crab, as a standard candle from 1 kev upto 500 keV. | CALIBRATION | 1 | A | NAKAZAWA | KAZUHIRO | NULL | NULL | JAP | 5 | AO5 | AO-5 CRAB CALIBRATION | XIS | Y |
| LOCKMAN HOLE | 162.9265 | 57.2528 | 149.71315343 | 53.19882847 | 305.9894 | 55685.7406712963 | 55686.7675925926 | 106001010 | 42278 | 40000 | 42278 | 43590.5 | 0 | 44442.7 | 2 | 2 | 0 | 1 | 1 | 0 | 0 | 57821.4 | 57821.4 | 88709.8 | 0 | PROCESSED | 57601.9586574074 | 55652 | 55768.8116898148 | 3.0.22.44 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 065001 | This is the proposal for the XIS calibration observations in the AO6 term. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 6 | AO6-CAL | XIS CALIBRATION OBSERVATIONS | XIS | N |
| E0102-72 CI 6 | 15.9973 | -72.0342 | 301.56226334 | -45.06065755 | 3.8307 | 55662.8284490741 | 55663.3522569444 | 106002010 | 20386.2 | 30000 | 20386.2 | 20386.2 | 0 | 20386.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17842 | 17842 | 45247.9 | 0 | PROCESSED | 57601.469837963 | 55652 | 55690.5690625 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 065001 | This is the proposal for the XIS calibration observations in the AO6 term. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 6 | AO6-CAL | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| E0102-72 | 16.0024 | -72.0368 | 301.56029587 | -45.05795518 | 69.5441 | 55741.0977314815 | 55741.5828009259 | 106002020 | 28782 | 30000 | 28790 | 28798 | 0 | 28782 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 24611.5 | 24611.5 | 41903.9 | 1 | PROCESSED | 57602.4336574074 | 55652 | 55775.250150463 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 065001 | This is the proposal for the XIS calibration observations in the AO6 term. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 6 | AO6-CAL | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| E0102-72 | 16.001 | -72.0295 | 301.56019202 | -45.06526758 | 183.1599 | 55848.6463310185 | 55849.0905092593 | 106002030 | 32817.5 | 30000 | 32825.5 | 32817.5 | 0 | 32825.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 29913.7 | 29913.7 | 38361.9 | 0 | PROCESSED | 57603.4194791667 | 55652 | 55873.0106597222 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 065001 | This is the proposal for the XIS calibration observations in the AO6 term. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 6 | AO6-CAL | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| E0102-72 | 16.0145 | -72.0334 | 301.55469199 | -45.06108873 | 340.2388 | 56003.3836574074 | 56004.1619444445 | 106002040 | 32378 | 30000 | 32394 | 32378 | 0 | 32394 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30718 | 30718 | 67244 | 0 | PROCESSED | 57604.9525231482 | 55652 | 56019.2768518518 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 065001 | This is the proposal for the XIS calibration observations in the AO6 term. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 6 | AO6-CAL | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| E0102-72 CI 2 | 15.9944 | -72.0366 | 301.5637608 | -45.05832492 | 4.3228 | 55663.352962963 | 55663.8890740741 | 106002050 | 20814.3 | 20000 | 20825.2 | 20822.2 | 0 | 20814.3 | 2 | 3 | 0 | 2 | 1 | 0 | 0 | 19623.9 | 19623.9 | 46318 | 0 | PROCESSED | 57601.4738773148 | 55652 | 55690.5705439815 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 065001 | This is the proposal for the XIS calibration observations in the AO6 term. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 6 | AO6-CAL | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| E0102-72_1_4_WIN | 16.0104 | -72.0348 | 301.55661541 | -45.05977973 | 4.7976 | 55663.8897337963 | 55664.4098726852 | 106003010 | 16829.5 | 30000 | 16829.5 | 18277.5 | 0 | 18277.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16956.4 | 16956.4 | 44931.9 | 0 | PROCESSED | 57601.4861921296 | 55652 | 55690.5713310185 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 065001 | This is the proposal for the XIS calibration observations in the AO6 term. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 6 | AO6-CAL | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| E0102-72_1_4_WIN | 16.0013 | -72.0289 | 301.56000261 | -45.06585975 | 183.5797 | 55849.0910763889 | 55849.5446643518 | 106003020 | 31657.1 | 30000 | 31657.1 | 31753.1 | 0 | 31769.1 | 4 | 3 | 0 | 3 | 1 | 0 | 0 | 24464.3 | 24464.3 | 39183.9 | 0 | PROCESSED | 57603.4278125 | 55652 | 55873.0426736111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 065001 | This is the proposal for the XIS calibration observations in the AO6 term. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 6 | AO6-CAL | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| CYGNUS_LOOP_P8 | 313.9841 | 31.4885 | 75.30130763 | -8.86579122 | 62.5162 | 55721.2910763889 | 55721.5835532407 | 106004010 | 11551.1 | 10000 | 11559.1 | 11567.1 | 0 | 11551.1 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10646.2 | 10646.2 | 25255.9 | 0 | PROCESSED | 57602.2328009259 | 55652 | 55757.6943287037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 065001 | This is the proposal for the XIS calibration observations in the AO6 term. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 6 | AO6-CAL | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| CYGNUS_LOOP_P8 | 314.0101 | 31.4557 | 75.29000417 | -8.90377623 | 240.0029 | 55915.0575231482 | 55915.3196527778 | 106004020 | 11990 | 10000 | 11990 | 11990 | 0 | 11990 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12321.2 | 12321.2 | 22643.9 | 0 | PROCESSED | 57604.1579976852 | 55652 | 55932.095162037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 065001 | This is the proposal for the XIS calibration observations in the AO6 term. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 6 | AO6-CAL | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| PERSEUS | 49.9433 | 41.526 | 150.56297877 | -13.25232631 | 83.8173 | 55769.5188888889 | 55770.5467939815 | 106005010 | 40838.2 | 40000 | 40854.2 | 40838.2 | 0 | 40963.1 | 2 | 3 | 0 | 2 | 1 | 0 | 0 | 36688.5 | 36688.5 | 88801.9 | 1 | PROCESSED | 57602.7044097222 | 55652 | 55792.3246990741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 065001 | This is the proposal for the XIS calibration observations in the AO6 term. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 6 | AO6-CAL | XIS CALIBRATION OBSERVATIONS | XIS | N |
| PERSEUS | 49.9531 | 41.5016 | 150.58309121 | -13.26863527 | 261.9986 | 55964.8470138889 | 55965.9169328704 | 106005020 | 46813.8 | 40000 | 46813.8 | 46813.8 | 0 | 46821.8 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 45202.5 | 45202.5 | 92427.8 | 0 | PROCESSED | 57604.6007291667 | 55652 | 56019.2664583333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 065001 | This is the proposal for the XIS calibration observations in the AO6 term. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 6 | AO6-CAL | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| PERSEUS_CI_2 | 49.9439 | 41.5251 | 150.56387356 | -13.25282951 | 84.2575 | 55768.5049768518 | 55769.518275463 | 106006010 | 40145.3 | 40000 | 40153.3 | 40161.3 | 0 | 40145.3 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 35470.3 | 35470.3 | 87505.9 | 0 | PROCESSED | 57602.6941898148 | 55652 | 55792.2315740741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 065001 | This is the proposal for the XIS calibration observations in the AO6 term. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 6 | AO6-CAL | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| PERSEUS_1_4_WIN | 49.9438 | 41.5162 | 150.5688507 | -13.26029585 | 67.7327 | 55796.234849537 | 55796.7167824074 | 106007010 | 20971.3 | 20000 | 20971.3 | 21003.2 | 0 | 20985.5 | 2 | 3 | 0 | 2 | 1 | 0 | 0 | 18760.7 | 18760.7 | 41633.9 | 2 | PROCESSED | 57602.9109143518 | 55652 | 55809.1967013889 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 065001 | This is the proposal for the XIS calibration observations in the AO6 term. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 6 | AO6-CAL | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| PERSEUS_1_4_WIN | 49.954 | 41.5015 | 150.58372556 | -13.26834695 | 262.0009 | 55965.9169444444 | 55966.4167824074 | 106007020 | 20856.9 | 20000 | 20880.9 | 20872.9 | 0 | 20856.9 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 21425.5 | 21425.5 | 43173.9 | 1 | PROCESSED | 57604.5908796296 | 55652 | 55991.4500810185 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 065001 | This is the proposal for the XIS calibration observations in the AO6 term. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 6 | AO6-CAL | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| PERSEUS_1_4_WIN_CI_2 | 49.9427 | 41.5184 | 150.56689856 | -13.25891455 | 67.7307 | 55795.7574305556 | 55796.234837963 | 106008010 | 23202.3 | 20000 | 23210.3 | 23202.3 | 0 | 23218.3 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 22067.8 | 22067.8 | 41244 | 0 | PROCESSED | 57602.9046643518 | 55652 | 55806.3485069445 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 065001 | This is the proposal for the XIS calibration observations in the AO6 term. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 6 | AO6-CAL | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| RXJ1856.5-3754 | 284.1491 | -37.9147 | 358.59438145 | -17.21743909 | 269.0594 | 55856.467037037 | 55857.327962963 | 106009010 | 39312.3 | 40000 | 39312.3 | 39320.3 | 0 | 39312.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35512.7 | 35512.7 | 74370.1 | 1 | PROCESSED | 57603.5093287037 | 55652 | 55873.9976041667 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 065001 | This is the proposal for the XIS calibration observations in the AO6 term. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 6 | AO6-CAL | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| N132D | 81.27 | -69.6453 | 280.30751952 | -32.78013136 | 312.914 | 55676.4828935185 | 55677.0820138889 | 106010010 | 26045.3 | 25000 | 26045.3 | 26045.3 | 0 | 26045.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 23421 | 23421 | 51753.9 | 0 | PROCESSED | 57601.585150463 | 55652 | 55697.1447685185 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 065001 | This is the proposal for the XIS calibration observations in the AO6 term. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 6 | AO6-CAL | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| N132D | 81.2448 | -69.6458 | 280.30994764 | -32.78867022 | 111.8253 | 55841.4446759259 | 55841.8703935185 | 106010020 | 23903 | 25000 | 23903 | 23903 | 0 | 23903 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22252.9 | 22252.9 | 36763.9 | 0 | PROCESSED | 57603.3429166667 | 55652 | 55858.3789814815 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 065001 | This is the proposal for the XIS calibration observations in the AO6 term. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 6 | AO6-CAL | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| PKS2155-304 | 329.71 | -30.2187 | 17.74059687 | -52.23913549 | 58.7962 | 55677.0907291667 | 55678.5925925926 | 106011010 | 60569.3 | 60000 | 60577.3 | 60583 | 0 | 60569.3 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 49583.6 | 49583.6 | 129709.8 | 1 | PROCESSED | 57601.6363657407 | 55652 | 55697.2337152778 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 065002 | This observation is a coordinated observation with Chandra and XMM carried out regularly once per year. The purpose is to calibrate relative effective areas among the three observatories. | CALIBRATION | 1 | A | ISHIDA | MANABU | NULL | NULL | JAP | 6 | AO6-CAL | COORDINATED OBSERVATION OF PKS2155-304 WITH CHANDRA AND XMM-NEWTON | XIS | Y |
| CRAB | 83.6298 | 22.0234 | 184.54825576 | -5.78216614 | 87.1025 | 55805.2472916667 | 55806.2585532407 | 106012010 | 509.9 | 40000 | 509.9 | 509.9 | 0 | 509.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36558.9 | 36558.9 | 87353.9 | 1 | PROCESSED | 57603.0659143518 | 55652 | 55851.4353356482 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 065003 | We propose to observe the Crab in order to calibrate the HXD response functions. | CALIBRATION | 1 | A | FUKAZAWA | YASUSHI | NULL | NULL | JAP | 6 | AO6-CAL | CALIBRATION OF HXD RESPONSE FUNCTIONS | XIS | Y |
| CRAB | 83.6357 | 22.0122 | 184.56070723 | -5.78354183 | 269.6254 | 55985.4765740741 | 55986.5585532407 | 106013010 | 521.7 | 40000 | 521.7 | 521.7 | 0 | 521.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36421.7 | 36421.7 | 93465.8 | 1 | PROCESSED | 57604.7881828704 | 55652 | 55995.2489699074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 065004 | We observe the Crab in order to calibrate the HXD response functions after PIN-LD is raised up. | CALIBRATION | 1 | A | FUKAZAWA | YASUSHI | NULL | NULL | JAP | 6 | AO6-CAL | CALIBRATION OF THE HXD RESPONSE FUNCTIONS | XIS | Y |
| CRAB | 83.6352 | 22.0094 | 184.56283497 | -5.78543222 | 269.6994 | 56000.0051967593 | 56001.1391435185 | 106014010 | 607 | 40000 | 607 | 607 | 0 | 607 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44787.9 | 44787.9 | 97955.8 | 1 | PROCESSED | 57604.9368981482 | 55652 | 56019.3369907407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 065004 | We observe the Crab in order to calibrate the HXD response functions after PIN-LD is raised up. | CALIBRATION | 1 | A | FUKAZAWA | YASUSHI | NULL | NULL | JAP | 6 | AO6-CAL | CALIBRATION OF THE HXD RESPONSE FUNCTIONS | XIS | Y |
| CRAB | 83.6348 | 22.004 | 184.56721998 | -5.78863608 | 269.6984 | 56012.5465393518 | 56013.5182407407 | 106015010 | 533.6 | 40000 | 533.6 | 533.6 | 0 | 533.6 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 24545 | 24545 | 83940.9 | 1 | PROCESSED | 57605.0600925926 | 55652 | 56023.2694212963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 065004 | We observe the Crab in order to calibrate the HXD response functions after PIN-LD is raised up. | CALIBRATION | 1 | A | FUKAZAWA | YASUSHI | NULL | NULL | JAP | 6 | AO6-CAL | CALIBRATION OF THE HXD RESPONSE FUNCTIONS | XIS | Y |
| LOCKMAN HOLE | 162.9197 | 57.2548 | 149.71479874 | 53.19475932 | 318.6945 | 56052.8901851852 | 56053.6759143518 | 107001010 | 35913.1 | 40000 | 35933.7 | 35933.7 | 0 | 35913.1 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 34153.6 | 34153.6 | 67871.9 | 2 | PROCESSED | 57605.3488888889 | 56018 | 56103.1997800926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 075001 | This is the proposal for the XIS calibration observations in the AO7 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 7 | AO7 | XIS CALIBRATION OBSERVATIONS | XIS | N |
| E0102-72 | 16.0127 | -72.0346 | 301.55559389 | -45.0599301 | 14.0258 | 56039.926099537 | 56040.7294212963 | 107002010 | 30438.2 | 30000 | 30470.2 | 30438.2 | 0 | 30462.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28052.8 | 28052.8 | 69401.9 | 0 | PROCESSED | 57605.2474305556 | 56018 | 56054.2693634259 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 075001 | This is the proposal for the XIS calibration observations in the AO7 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 7 | AO7 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| E0102-72 | 16.0126 | -72.0415 | 301.55631435 | -45.05304883 | 69.1459 | 56103.3768287037 | 56104.1668055556 | 107002020 | 30726.9 | 30000 | 30728.1 | 30726.9 | 0 | 30728.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27423.6 | 27423.6 | 68248 | 0 | PROCESSED | 57606.4992939815 | 56018 | 56114.2101967593 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 075001 | This is the proposal for the XIS calibration observations in the AO7 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 7 | AO7 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| E0102-72 | 15.9776 | -72.0269 | 301.57013713 | -45.06835815 | 193.0032 | 56229.1207175926 | 56229.9446412037 | 107002030 | 32102.6 | 30000 | 32110 | 32107.6 | 0 | 32102.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 29822.7 | 29822.7 | 71181.9 | 1 | PROCESSED | 57607.8912268518 | 56018 | 56240.4750810185 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 075001 | This is the proposal for the XIS calibration observations in the AO7 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 7 | AO7 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| E0102-72 | 16.0369 | -72.03 | 301.54459754 | -45.06399958 | 336.4364 | 56364.8870717593 | 56365.6383449074 | 107002040 | 32601.3 | 30000 | 32601.3 | 32609.3 | 0 | 32609.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35668.7 | 35668.7 | 64895.9 | 0 | PROCESSED | 57610.7968634259 | 56018 | 56377.5104861111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 075001 | This is the proposal for the XIS calibration observations in the AO7 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 7 | AO7 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| E0102-72_1_4_WIN | 16.0207 | -72.0344 | 301.55208936 | -45.05995839 | 14.0185 | 56040.7294328704 | 56041.5522453704 | 107003010 | 32127.6 | 30000 | 32127.6 | 32127.6 | 0 | 32127.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 29577.6 | 29577.6 | 71086 | 1 | PROCESSED | 57605.277974537 | 56018 | 56068.6207407407 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 075001 | This is the proposal for the XIS calibration observations in the AO7 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 7 | AO7 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| E0102-72_1_4_WIN | 15.9774 | -72.0274 | 301.57027283 | -45.06786356 | 193.004 | 56229.9446527778 | 56230.6634259259 | 107003020 | 31357.1 | 30000 | 31357.1 | 31357.1 | 0 | 31357.1 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 28574.3 | 28574.3 | 62100 | 0 | PROCESSED | 57607.9083333333 | 56018 | 56240.4835648148 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 075001 | This is the proposal for the XIS calibration observations in the AO7 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 7 | AO7 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| CYGNUS_LOOP_P8 | 313.9853 | 31.4884 | 75.30188904 | -8.86664393 | 62.4975 | 56089.3554282407 | 56089.5523032407 | 107004010 | 8222.1 | 10000 | 8222.1 | 8222.1 | 0 | 8222.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 7339.4 | 7339.4 | 17007.9 | 1 | PROCESSED | 57605.6387615741 | 56018 | 56106.1733912037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 075001 | This is the proposal for the XIS calibration observations in the AO7 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 7 | AO7 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| CYGNUS_LOOP_P8 | 314.0092 | 31.4675 | 75.29871729 | -8.89566896 | 227.4007 | 56278.9212731482 | 56279.1764930556 | 107004020 | 10045.6 | 10000 | 10053.6 | 10061.6 | 0 | 10045.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11682 | 11682 | 22013.9 | 0 | PROCESSED | 57608.3005902778 | 56018 | 56316.536412037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 075001 | This is the proposal for the XIS calibration observations in the AO7 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 7 | AO7 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| PERSEUS | 49.9448 | 41.5174 | 150.56881272 | -13.2588819 | 72.6103 | 56159.9797569444 | 56160.9820601852 | 107005010 | 41131.5 | 40000 | 41131.5 | 41131.5 | 0 | 41131.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38984.1 | 38984.1 | 86583.8 | 0 | PROCESSED | 57606.9408680556 | 56018 | 56212.8025115741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 075001 | This is the proposal for the XIS calibration observations in the AO7 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 7 | AO7 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| PERSEUS | 49.9562 | 41.5103 | 150.58015129 | -13.26009762 | 256.2876 | 56334.208275463 | 56335.2007523148 | 107005020 | 37690.1 | 40000 | 41272.7 | 37690.1 | 0 | 41522.1 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 36431.4 | 36431.4 | 85733.8 | 0 | PROCESSED | 57610.5866203704 | 56018 | 56349.5875694444 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 075001 | This is the proposal for the XIS calibration observations in the AO7 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 7 | AO7 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| PERSEUS_1_4_WIN | 49.9443 | 41.5178 | 150.56826526 | -13.25875461 | 72.777 | 56159.5393518518 | 56159.9794212963 | 107006010 | 23678.6 | 20000 | 23678.6 | 23678.6 | 0 | 23678.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 20255 | 20255 | 38015.9 | 0 | PROCESSED | 57606.9012731482 | 56018 | 56214.981087963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 075001 | This is the proposal for the XIS calibration observations in the AO7 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 7 | AO7 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| PERSEUS_1_4_WIN | 49.9556 | 41.5052 | 150.582656 | -13.26459967 | 255.9019 | 56335.2013657407 | 56335.6875694444 | 107006020 | 22024.7 | 20000 | 22032.7 | 22024.7 | 0 | 22040.7 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 17799 | 17799 | 41999.9 | 1 | PROCESSED | 57610.5863078704 | 56018 | 56349.5725810185 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 075001 | This is the proposal for the XIS calibration observations in the AO7 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 7 | AO7 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| RXJ1856.5-3754 | 284.1441 | -37.9006 | 358.60662879 | -17.20863504 | 88.5024 | 56019.1209143518 | 56020.3237384259 | 107007010 | 42087.7 | 40000 | 42095.7 | 42087.7 | 0 | 42095.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37740.3 | 37740.3 | 103914 | 1 | PROCESSED | 57605.1078009259 | 56018 | 56034.3014699074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 075001 | This is the proposal for the XIS calibration observations in the AO7 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 7 | AO7 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| RXJ1856.5-3754 | 284.1491 | -37.909 | 358.59994006 | -17.21536576 | 268.9999 | 56220.5826388889 | 56221.7570486111 | 107007020 | 44047 | 40000 | 44047 | 44047 | 0 | 44047 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37256.8 | 37256.8 | 101465.9 | 1 | PROCESSED | 57607.8037384259 | 56018 | 56236.5089583333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 075001 | This is the proposal for the XIS calibration observations in the AO7 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 7 | AO7 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| N132D | 81.2348 | -69.654 | 280.32028023 | -32.79064068 | 125.4993 | 56219.7585532407 | 56220.5737384259 | 107008010 | 24141.6 | 25000 | 24141.6 | 24141.6 | 0 | 24141.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28382 | 28382 | 70419.9 | 0 | PROCESSED | 57607.7927546296 | 56018 | 56324.4719097222 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 075001 | This is the proposal for the XIS calibration observations in the AO7 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 7 | AO7 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| N132D | 81.2721 | -69.634 | 280.29413666 | -32.78140611 | 283.9121 | 56377.4215393518 | 56378.1669560185 | 107008020 | 23118.2 | 25000 | 23134.2 | 23118.2 | 0 | 23134.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22472.5 | 22472.5 | 64397.9 | 1 | PROCESSED | 57610.9240856482 | 56018 | 56387.4974189815 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 075001 | This is the proposal for the XIS calibration observations in the AO7 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 7 | AO7 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| PKS2155-304 | 329.7182 | -30.2228 | 17.73521081 | -52.24662805 | 244.9394 | 56230.6707986111 | 56231.3327777778 | 107009010 | 21377.1 | 20000 | 21377.1 | 21377.1 | 0 | 21377.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19998.3 | 19998.3 | 57188 | 0 | PROCESSED | 57607.9053819444 | 56018 | 56327.5484953704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 075001 | This is the proposal for the XIS calibration observations in the AO7 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 7 | AO7 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| PKS2155-304 | 329.7129 | -30.2255 | 17.73000788 | -52.24237208 | 57.9628 | 56044.5907175926 | 56046.250162037 | 107010010 | 61887.2 | 60000 | 61887.2 | 68199.2 | 0 | 68199.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 59298.6 | 59298.6 | 143362 | 1 | PROCESSED | 57605.3036805556 | 56018 | 56068.6218055556 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 075002 | This observation is a coordinated observation with Chandra and XMM carried out regularly once per year. The purpose is to calibrate relative effective areas among the three observatories. | CALIBRATION | 1 | A | ISHIDA | MANABU | NULL | NULL | JAP | 7 | AO7 | COORDINATED OBSERVATION OF PKS2155-304 WITH CHANDRA AND XMM-NEWTON | XIS | Y |
| CRAB | 83.6307 | 22.0167 | 184.55439271 | -5.78504823 | 87.6815 | 56196.2328125 | 56197.2258217593 | 107011010 | 520.2 | 40000 | 520.2 | 520.2 | 0 | 520.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35748 | 35748 | 85768 | 2 | PROCESSED | 57607.2286689815 | 56018 | 56225.5467939815 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 075003 | We propose to observe the Crab in order to calibrate the HXD response functions. | CALIBRATION | 1 | A | FUKAZAWA | YASUSHI | NULL | NULL | JAP | 7 | AO7 | CALIBRATION OF HXD RESPONSE FUNCTIONS | XIS | Y |
| CRAB | 83.6342 | 22.0129 | 184.55936471 | -5.78434175 | 269.312 | 56350.008599537 | 56350.9133564815 | 107012010 | 515 | 40000 | 515 | 515 | 0 | 515 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 39843.5 | 39843.5 | 78161.9 | 1 | PROCESSED | 57610.6875347222 | 56018 | 56372.548900463 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 075004 | We observe the Crab in order to calibrate the HXD response functions after PIN-LD is raised up. | CALIBRATION | 1 | A | FUKAZAWA | YASUSHI | NULL | NULL | JAP | 7 | AO7 | CALIBRATION OF THE HXD RESPONSE FUNCTIONS | XIS | Y |
| 3C273 | 187.2808 | 2.0495 | 289.95874213 | 64.35772193 | 291.7637 | 56124.3395138889 | 56125.3752083333 | 107013010 | 39755.3 | 40000 | 39755.3 | 40363.3 | 0 | 40359.6 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 35778.3 | 35778.3 | 89475.8 | 2 | PROCESSED | 57606.6472800926 | 56018 | 56141.181400463 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 075005 | This observation is a coordinated observation with NuStar, Chandra and XMM. | CALIBRATION | 1 | A | ISHIDA | MANABU | NULL | NULL | JAP | 7 | AO7 | COORDINATED OBSERVATION OF 3C 273 | XIS | Y |
| LOCKMAN HOLE | 162.9444 | 57.2754 | 149.67434926 | 53.19082755 | 122.9996 | 56602.9618634259 | 56603.8751157407 | 108001010 | 38846.3 | 40000 | 38851.9 | 38846.3 | 0 | 39095.2 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 39473.6 | 39473.6 | 78901.9 | 1 | PROCESSED | 57613.2451388889 | 56383 | 56652.6887731482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 085001 | This is the proposal for the XIS calibration observations in the AO8 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 8 | AO8 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| E0102-72 | 16.037 | -72.0354 | 301.54508789 | -45.05861061 | 18.1989 | 56409.4608217593 | 56410.2349768518 | 108002010 | 29322.8 | 30000 | 29344.8 | 29322.8 | 0 | 29336.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 46113.1 | 46113.1 | 66879.9 | 0 | PROCESSED | 57611.1766087963 | 56383 | 56429.5862384259 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 085001 | This is the proposal for the XIS calibration observations in the AO8 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 8 | AO8 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| E0102-72 | 16.0133 | -72.0418 | 301.556039 | -45.05273459 | 69.0007 | 56469.5902430556 | 56470.3662037037 | 108002020 | 33138.3 | 30000 | 33143.9 | 33141.4 | 0 | 33138.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47278 | 47278 | 67037.9 | 0 | PROCESSED | 57611.643900463 | 56383 | 56491.6117476852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 085001 | This is the proposal for the XIS calibration observations in the AO8 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 8 | AO8 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| E0102-72 | 15.986 | -72.0312 | 301.5668942 | -45.06389041 | 160.5274 | 56563.587025463 | 56564.4820949074 | 108002030 | 31959.5 | 30000 | 31959.5 | 31959.5 | 0 | 31961.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30139.4 | 30139.4 | 77317.9 | 0 | PROCESSED | 57612.7569328704 | 56383 | 56625.6360763889 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 085001 | This is the proposal for the XIS calibration observations in the AO8 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 8 | AO8 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| E0102-72 | 16.0359 | -72.0296 | 301.54499373 | -45.06442014 | 337.9663 | 56731.6566782407 | 56732.3821759259 | 108002040 | 29279.3 | 30000 | 29279.3 | 29279.3 | 0 | 29287.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 26418.8 | 26418.8 | 62678 | 0 | PROCESSED | 57614.023599537 | 56383 | 56747.6579166667 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 085001 | This is the proposal for the XIS calibration observations in the AO8 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 8 | AO8 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| E0102-72_1_4_WIN | 16.0332 | -72.0356 | 301.5467628 | -45.0584929 | 18.2026 | 56410.2349884259 | 56411.0058101852 | 108003010 | 27568.9 | 30000 | 27568.9 | 30932.2 | 0 | 30918.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47013.9 | 47013.9 | 66591.9 | 0 | PROCESSED | 57611.1975231482 | 56383 | 56429.6067361111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 085001 | This is the proposal for the XIS calibration observations in the AO8 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 8 | AO8 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| E0102-72_1_4_WIN | 15.9825 | -72.0303 | 301.56833182 | -45.06486245 | 171.8498 | 56564.4855787037 | 56565.406400463 | 108003020 | 33612.9 | 30000 | 33612.9 | 33612.9 | 0 | 33612.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 31660.9 | 31660.9 | 79536 | 0 | PROCESSED | 57612.7799537037 | 56383 | 56628.7726157407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 085001 | This is the proposal for the XIS calibration observations in the AO8 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 8 | AO8 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| CYGNUS_LOOP_P8 | 313.983 | 31.4894 | 75.30140551 | -8.86449487 | 62.2962 | 56450.9733333333 | 56451.3675115741 | 108004010 | 11883.7 | 10000 | 11892.7 | 11886 | 0 | 11883.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12927 | 12927 | 34055.9 | 1 | PROCESSED | 57611.480625 | 56383 | 56461.6706944444 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 085001 | This is the proposal for the XIS calibration observations in the AO8 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 8 | AO8 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| CYGNUS_LOOP_P8 | 314.0082 | 31.4652 | 75.29637267 | -8.89647626 | 240.0001 | 56631.1784259259 | 56631.4008680556 | 108004020 | 11768.3 | 10000 | 11776.3 | 11768.3 | 0 | 11784.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8229.7 | 8229.7 | 19215.9 | 0 | PROCESSED | 57613.5167476852 | 56383 | 56664.6555671296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 085001 | This is the proposal for the XIS calibration observations in the AO8 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 8 | AO8 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| PERSEUS | 49.9459 | 41.5178 | 150.56929207 | -13.25809407 | 76.2419 | 56519.4411342593 | 56520.3558333333 | 108005010 | 41256.9 | 40000 | 41257 | 41256.9 | 0 | 41256.9 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 40686.7 | 40686.7 | 79006 | 1 | PROCESSED | 57612.2773958333 | 56383 | 56587.736712963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 085001 | This is the proposal for the XIS calibration observations in the AO8 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 8 | AO8 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| PERSEUS | 49.9546 | 41.5052 | 150.58201417 | -13.26501269 | 255.9996 | 56693.5266550926 | 56694.382025463 | 108005020 | 37999.6 | 40000 | 37999.6 | 37999.6 | 0 | 37999.6 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57613.7941898148 | 56383 | 56709.7097685185 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 085001 | This is the proposal for the XIS calibration observations in the AO8 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 8 | AO8 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| PERSEUS_1_4_WIN | 49.9469 | 41.5176 | 150.57004712 | -13.25784807 | 75.8995 | 56520.3563541667 | 56520.8092939815 | 108006010 | 21623.9 | 20000 | 21623.9 | 21623.9 | 0 | 21628.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18833.6 | 18833.6 | 39131.9 | 1 | PROCESSED | 57612.3280092593 | 56383 | 56587.6592708333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 085001 | This is the proposal for the XIS calibration observations in the AO8 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 8 | AO8 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| PERSEUS_1_4_WIN | 49.9545 | 41.505 | 150.58206331 | -13.26522083 | 255.9996 | 56694.382037037 | 56694.7883449074 | 108006020 | 18956.5 | 20000 | 18974.3 | 18956.5 | 0 | 18972.5 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57613.7966782407 | 56383 | 56709.7151851852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 085001 | This is the proposal for the XIS calibration observations in the AO8 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 8 | AO8 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| RXJ1856.5-3754 | 284.1435 | -37.9087 | 358.59854994 | -17.21114101 | 89.8164 | 56397.1347916667 | 56398.4009490741 | 108007010 | 40747.3 | 40000 | 40755.3 | 40747.3 | 0 | 40755.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36272 | 36272 | 109385.8 | 1 | PROCESSED | 57611.0803587963 | 56383 | 56421.704837963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 085001 | This is the proposal for the XIS calibration observations in the AO8 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 8 | AO8 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| RXJ1856.5-3754 | 284.1497 | -37.9108 | 358.59836499 | -17.21646147 | 268.9972 | 56570.3889930556 | 56571.6043865741 | 108007020 | 40783.9 | 40000 | 40831.9 | 40783.9 | 0 | 40831.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35392.6 | 35392.6 | 104997.8 | 0 | PROCESSED | 57612.8589814815 | 56383 | 56628.7985648148 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 085001 | This is the proposal for the XIS calibration observations in the AO8 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 8 | AO8 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| N132D | 81.2389 | -69.6575 | 280.32407725 | -32.78861762 | 111.496 | 56571.6132407407 | 56572.1738310185 | 108008020 | 5127.2 | 25000 | 5127.2 | 5127.2 | 0 | 5127.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 34963.1 | 34963.1 | 48423.9 | 1 | PROCESSED | 57612.8405092593 | 56383 | 56628.7620601852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 085001 | This is the proposal for the XIS calibration observations in the AO8 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 8 | AO8 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| N132D | 81.2957 | -69.6416 | 280.30131329 | -32.77198365 | 339.1924 | 56434.2591550926 | 56435.1334606482 | 108008030 | 29839.4 | 25000 | 29839.4 | 29859.4 | 0 | 29847.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28335 | 28335 | 75531.9 | 1 | PROCESSED | 57611.3464699074 | 56383 | 56474.7165972222 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 085001 | This is the proposal for the XIS calibration observations in the AO8 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 8 | AO8 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| N132D | 81.229 | -69.6452 | 280.31040291 | -32.79418529 | 157.2884 | 56621.0686805556 | 56621.5834953704 | 108008040 | 27046.8 | 25000 | 27102.8 | 27046.8 | 0 | 27110 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 24430 | 24430 | 44471.9 | 0 | PROCESSED | 57613.4168402778 | 56383 | 56664.6637615741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 085001 | This is the proposal for the XIS calibration observations in the AO8 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 8 | AO8 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| N132D | 81.2306 | -69.6358 | 280.2992802 | -32.7953027 | 210.9996 | 56668.9114236111 | 56670.9794328704 | 108008050 | 7520.3 | 25000 | 7520.3 | 7528.3 | 0 | 7528.3 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 12471 | 0 | PROCESSED | 57613.7671296296 | 56383 | 56687.7807291667 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 085001 | This is the proposal for the XIS calibration observations in the AO8 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 8 | AO8 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| PKS2155-304 | 329.7186 | -30.2268 | 17.72877882 | -52.24740992 | 244.697 | 56595.1408101852 | 56595.6765625 | 108009010 | 23765.1 | 20000 | 23765.1 | 23765.1 | 0 | 23765.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25583.6 | 25583.6 | 46283.9 | 0 | PROCESSED | 57613.198599537 | 56383 | 56608.6163425926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 085001 | This is the proposal for the XIS calibration observations in the AO8 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 8 | AO8 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| PKS2155-304 | 329.7149 | -30.2268 | 17.72820682 | -52.24423222 | 58.7562 | 56405.8401388889 | 56407.3786342593 | 108010010 | 53352.6 | 60000 | 53352.6 | 53352.6 | 0 | 53352.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48511.8 | 48511.8 | 132923.8 | 2 | PROCESSED | 57611.2064351852 | 56383 | 56608.6270949074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 085002 | This observation is a coordinated observation with Chandra and XMM carried out regularly once per year. The purpose is to calibrate relative effective areas among the three observatories. | CALIBRATION | 1 | A | ISHIDA | MANABU | NULL | NULL | JAP | 8 | AO8 | COORDINATED OBSERVATION OF PKS2155-304 WITH CHANDRA AND XMM-NEWTON | XIS | Y |
| CRAB | 83.6307 | 22.0165 | 184.5545625 | -5.7851553 | 87.2995 | 56565.4174768518 | 56566.4176273148 | 108011010 | 522.6 | 40000 | 522.6 | 522.6 | 0 | 522.6 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 40141 | 40141 | 86405.9 | 0 | PROCESSED | 57612.824212963 | 56383 | 56588.5681481482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 085003 | We propose to observe the Crab in order to calibrate the HXD response functions. | CALIBRATION | 1 | A | FUKAZAWA | YASUSHI | NULL | NULL | JAP | 8 | AO8 | CALIBRATION OF HXD RESPONSE FUNCTIONS | XIS | Y |
| CRAB | 83.6349 | 22.0126 | 184.55996858 | -5.78395418 | 269.5698 | 56722.0566087963 | 56723.0417939815 | 108012010 | 474.1 | 40000 | 474.1 | 474.1 | 0 | 474.1 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 32514.9 | 32514.9 | 85091.9 | 1 | PROCESSED | 57613.9898263889 | 56383 | 56734.706099537 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 085004 | We observe the Crab in order to calibrate the HXD response functions after PIN-LD is raised up. | CALIBRATION | 1 | A | FUKAZAWA | YASUSHI | NULL | NULL | JAP | 8 | AO8 | CALIBRATION OF THE HXD RESPONSE FUNCTIONS | XIS | Y |
| RX J1712.6-2414 | 258.1492 | -24.2452 | 359.86576841 | 8.74169228 | 94.3118 | 56709.5823958333 | 56710.4883333333 | 108014010 | 39713.3 | 40000 | 39729.3 | 39713.3 | 0 | 39729.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40442.7 | 40442.7 | 78255.8 | 1 | PROCESSED | 57613.8970601852 | 56383 | 56754.6772569445 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 085006 | Check the change of PSF due to XRT heatter setting | CALIBRATION | 1 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 8 | AO8 | CONFIRMATION OF PSF | XIS | Y |
| E0102-72 | 16.0411 | -72.0372 | 301.54348026 | -45.05672664 | 12.49 | 56768.2360069444 | 56769.1376967593 | 109001010 | 30737.5 | 30000 | 30737.5 | 30745.5 | 0 | 30745.5 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57614.9712731482 | 56748 | 56825.6177314815 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 095001 | This is the proposal for the XIS calibration observations in the AO9 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 9 | AO9 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| E0102-72 | 15.984 | -72.028 | 301.5674545 | -45.06712525 | 192.4976 | 56958.3214930556 | 56959.2327777778 | 109001020 | 28916.3 | 30000 | 28916.3 | 32217.3 | 0 | 32217.3 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7003819445 | 56748 | 56986.3994560185 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 095001 | This is the proposal for the XIS calibration observations in the AO9 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 9 | AO9 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| E0102-72 | 16.035 | -72.0314 | 301.54556378 | -45.06264392 | 356.2112 | 57115.6737962963 | 57116.4591435185 | 109001030 | 29730.3 | 30000 | 29730.3 | 29730.3 | 0 | 29730.3 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.9196990741 | 56748 | 57183.662662037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 095001 | This is the proposal for the XIS calibration observations in the AO9 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 9 | AO9 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| E0102-72_1_4_WIN | 16.0383 | -72.0354 | 301.54452166 | -45.0585826 | 13.3075 | 56769.1385416667 | 56770.0181828704 | 109002010 | 31670.8 | 30000 | 31684.6 | 31670.8 | 0 | 31684.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 7299 | 7299 | 18287.9 | 0 | PROCESSED | 57614.9815625 | 56748 | 56821.7266550926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 095001 | This is the proposal for the XIS calibration observations in the AO9 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 9 | AO9 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| E0102-72_1_4_WIN | 15.9793 | -72.0266 | 301.56936701 | -45.06862148 | 192.5036 | 56959.2327893518 | 56960.0938888889 | 109002020 | 23834.5 | 30000 | 23834.5 | 31343.2 | 0 | 31343.2 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7092939815 | 56748 | 56979.4305671296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 095001 | This is the proposal for the XIS calibration observations in the AO9 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 9 | AO9 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| E0102-72_PSUM | 16.041 | -72.0333 | 301.54313775 | -45.06061925 | 359.8441 | 57119.5810763889 | 57120.4917361111 | 109003010 | 33311.3 | 30000 | 33389.5 | 33397.5 | 0 | 33311.3 | 2 | 2 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.9503472222 | 56748 | 57129.4064699074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 095001 | This is the proposal for the XIS calibration observations in the AO9 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 9 | AO9 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| CYGNUS_LOOP_P8 | 313.9843 | 31.4837 | 75.29767156 | -8.86897904 | 46.7112 | 56824.8687615741 | 56825.0675 | 109004010 | 9340 | 10000 | 9340 | 9348 | 0 | 9348 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9797.1 | 9797.1 | 17167.9 | 0 | PROCESSED | 57615.2541435185 | 56748 | 56835.7101388889 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 095001 | This is the proposal for the XIS calibration observations in the AO9 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 9 | AO9 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| CYGNUS_LOOP_P8 | 314.0058 | 31.4646 | 75.29458482 | -8.89528015 | 238.4683 | 56996.9847453704 | 56997.2154398148 | 109004020 | 8889.3 | 10000 | 8889.3 | 8889.3 | 0 | 8889.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9303 | 9303 | 19928 | 1 | PROCESSED | 57617.4549074074 | 56748 | 57092.1997685185 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 095001 | This is the proposal for the XIS calibration observations in the AO9 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 9 | AO9 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| PERSEUS | 49.9434 | 41.5178 | 150.56768766 | -13.25912615 | 67.3431 | 56896.6728703704 | 56897.185462963 | 109005010 | 19977.3 | 40000 | 19977.3 | 20073.3 | 0 | 20073.3 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.5268402778 | 56748 | 56910.6477893518 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 095001 | This is the proposal for the XIS calibration observations in the AO9 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 9 | AO9 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| PERSEUS | 49.956 | 41.5054 | 150.5827994 | -13.26426763 | 248.5273 | 57084.7367476852 | 57085.5849537037 | 109005020 | 37204.6 | 40000 | 37204.6 | 37204.6 | 0 | 37204.6 | 3 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.7130902778 | 56748 | 57097.4044212963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 095001 | This is the proposal for the XIS calibration observations in the AO9 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 9 | AO9 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| PERSEUS_1_4_WIN | 49.9556 | 41.5053 | 150.58259934 | -13.26451625 | 248.5264 | 57085.5849652778 | 57086.1141203704 | 109006010 | 23649.2 | 20000 | 23649.2 | 23649.2 | 0 | 23649.2 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.7465393518 | 56748 | 57098.4141435185 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 095001 | This is the proposal for the XIS calibration observations in the AO9 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 9 | AO9 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| PERSEUS_PSUM | 49.9564 | 41.5056 | 150.5829428 | -13.26393558 | 248.5274 | 57086.1141319445 | 57086.7752662037 | 109007010 | 30680.2 | 30000 | 30680.2 | 30682.6 | 0 | 30925.2 | 4 | 4 | 0 | 2 | 1 | 0 | 0 | 390 | 390 | 539 | 0 | PROCESSED | 57617.7395717593 | 56748 | 57098.0128240741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 095001 | This is the proposal for the XIS calibration observations in the AO9 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 9 | AO9 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| RXJ1856.5-3754 | 284.1438 | -37.9107 | 358.59668979 | -17.21208909 | 88.7001 | 56755.512974537 | 56756.5002546296 | 109008010 | 38969 | 40000 | 38969 | 38969 | 0 | 38969 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34621 | 34621 | 85287.9 | 1 | PROCESSED | 57614.225787037 | 56748 | 56769.6997106482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 095001 | This is the proposal for the XIS calibration observations in the AO9 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 9 | AO9 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| RXJ1856.5-3754 | 284.1489 | -37.9089 | 358.59997749 | -17.2151824 | 269.1688 | 56953.6878240741 | 56954.8155324074 | 109008020 | 39563.8 | 40000 | 39563.8 | 39563.8 | 0 | 39571.8 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.6894328704 | 56748 | 56979.4129861111 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 095001 | This is the proposal for the XIS calibration observations in the AO9 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 9 | AO9 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| N132D | 81.2854 | -69.6352 | 280.29457121 | -32.77663858 | 305.0548 | 56764.2015625 | 56764.8543055556 | 109009010 | 24922 | 25000 | 24922 | 24922 | 0 | 24922 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57614.960625 | 56748 | 56782.4936111111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 095001 | This is the proposal for the XIS calibration observations in the AO9 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 9 | AO9 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| N132D | 81.226 | -69.6524 | 280.31905235 | -32.79393564 | 136.0055 | 56960.0986689815 | 56960.5570833333 | 109009020 | 13529.3 | 25000 | 13529.3 | 24753.9 | 0 | 24753.9 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7134606482 | 56748 | 56979.4327430556 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 095001 | This is the proposal for the XIS calibration observations in the AO9 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 9 | AO9 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| PKS2155-304 | 329.721 | -30.2253 | 17.73158513 | -52.24930684 | 244.7507 | 56960.5657523148 | 56961.2918981482 | 109010010 | 20370.6 | 20000 | 20370.6 | 21473.6 | 0 | 21473.6 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7328819444 | 56748 | 56979.4450694444 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 095001 | This is the proposal for the XIS calibration observations in the AO9 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 9 | AO9 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| PKS2155-304 | 329.7146 | -30.2278 | 17.72653709 | -52.24408412 | 59.175 | 56771.816724537 | 56773.2710069445 | 109011010 | 63991.6 | 60000 | 63991.6 | 63999.6 | 0 | 64009.4 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.0047106482 | 56748 | 56825.6212037037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 095002 | This observation is a coordinated observation with Chandra and XMM carried out regularly once per year. The purpose is to calibrate relative effective areas among the three observatories. | CALIBRATION | 1 | A | ISHIDA | MANABU | NULL | NULL | JAP | 9 | AO9 | COORDINATED OBSERVATION OF PKS2155-304 WITH CHANDRA AND XMM-NEWTON | XIS | Y |
| LOCKMAN HOLE | 162.9402 | 57.278 | 149.67367992 | 53.18739913 | 107.8721 | 56991.0124884259 | 56991.9933101852 | 109014010 | 37057.1 | 40000 | 37057.1 | 37065.1 | 0 | 37065.1 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 39200 | 39200 | 84548 | 0 | PROCESSED | 57617.4540740741 | 56748 | 57006.9648263889 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 095005 | We observe the Locaman hole in order to calibrate the HXD background level. | CALIBRATION | 1 | A | FUKAZAWA | YASUSHI | NULL | NULL | JAP | 9 | AO9 | CALIBRATION OF THE HXD RESPONSE FUNCTIONS | XIS | Y |
| SS CYG | 325.6907 | 43.5765 | 90.55960302 | -7.12368552 | 237.9822 | 57010.2666319444 | 57010.9974305556 | 109015010 | 43187.4 | 20000 | 43187.4 | 43203.4 | 0 | 43187.4 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.5432407407 | 56748 | 57049.4521296296 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 095006 | ADDITIONAL CALIBRATION OF XRT WITH SS CYG | CALIBRATION | 1 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 9 | AO9 | XRT CHECK WITH SS CYG | XIS | Y |
| NEP | 270.0344 | 66.574 | 96.39928472 | 29.79775756 | 142.5162 | 57052.9388078704 | 57056.250162037 | 109016010 | 154011.4 | 200000 | 0 | 0 | 0 | 154011.4 | 0 | 0 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.5675462963 | 56748 | 57066.4217708333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 095007 | MAINTENANCE OF SUZAKU | CALIBRATION | 1 | A | DOTANI | TADAYASU | NULL | NULL | JAP | 9 | AO9 | NEP | XIS | Y |
| NEP | 270.0357 | 66.574 | 96.39928473 | 29.79724073 | 142.5167 | 57056.2501736111 | 57056.7258564815 | 109016020 | 21676.4 | 200000 | 0 | 0 | 0 | 21676.4 | 0 | 0 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.5715740741 | 56748 | 57066.4225231482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 095007 | MAINTENANCE OF SUZAKU | CALIBRATION | 1 | A | DOTANI | TADAYASU | NULL | NULL | JAP | 9 | AO9 | NEP | XIS | Y |
| N132D | 81.2911 | -69.6367 | 280.29591185 | -32.77442189 | 319.8518 | 57144.6915972222 | 57145.5405092593 | 110007010 | 31487.8 | 25000 | 31487.8 | 31487.8 | 0 | 31487.8 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57618.064837963 | 57113 | 57164.52875 | 3.0.22.44 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 105001 | This is the proposal for the XIS calibration observations in the AO10 cycle. | CALIBRATION | 1 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 10 | AO10 | XIS CALIBRATION OBSERVATIONS | XIS | Y |
| AE AQUARII | 310.0457 | -0.9355 | 45.22275468 | -24.45710482 | 264.8759 | 53673.9022685185 | 53676.043275463 | 400001010 | 70528.9 | 100000 | 70528.9 | 70616.9 | 70568.9 | 70544.9 | 3 | 3 | 3 | 3 | 1 | 0 | 0 | 59453.8 | 59453.8 | 184956.9 | 2 | PROCESSED | 57527.7308217593 | 54247 | 54036.9851388889 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001004 | We have a new idea that a magnetized white dwarf can be a particle-acceleration cite to emit non thermal emission. In order to understand the particle acceleration process in rotation-powered objects, it is important to measure the hard X-ray emission from magnetized white dwarfs, in addition to that from well-known neutron stars. Here, we propose a 100ksec observation of a magnetic cataclysmic valiable, AE Aqurii. It is difficult for INTEGRAL mission, and is challenging even for the HXD, but it will be a ``first detection'' of the non-thermal emission in the hard X-ray band from a white dwarf with Suzaku. | GALACTIC POINT SOURCES | 4 | A | TERADA | YUKIKATSU | NULL | NULL | JAP | 0 | SWG | SEARCH FOR THE NON-THERMAL EMISSION FROM MAGNETIZED WHITE DWARF WITH SUZAKU | NULL | N |
| AE AQUARII | 310.0612 | -0.931 | 45.23545862 | -24.46836188 | 250.6241 | 54033.2319907407 | 54034.3829282407 | 400001020 | 47974.3 | 50000 | 47974.3 | 48595.6 | 48131.6 | 48310.3 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 45538.4 | 45538.4 | 99423.9 | 1 | PROCESSED | 57526.8238773148 | 54526 | 54109.7083449074 | 3.0.22.43 | 9 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001004 | We have a new idea that a magnetized white dwarf can be a particle-acceleration cite to emit non thermal emission. In order to understand the particle acceleration process in rotation-powered objects, it is important to measure the hard X-ray emission from magnetized white dwarfs, in addition to that from well-known neutron stars. Here, we propose a 100ksec observation of a magnetic cataclysmic valiable, AE Aqurii. It is difficult for INTEGRAL mission, and is challenging even for the HXD, but it will be a ``first detection'' of the non-thermal emission in the hard X-ray band from a white dwarf with Suzaku. | GALACTIC POINT SOURCES | 4 | A | TERADA | YUKIKATSU | NULL | NULL | JAP | 0 | SWG | SEARCH FOR THE NON-THERMAL EMISSION FROM MAGNETIZED WHITE DWARF WITH SUZAKU | HXD | N |
| GX 349+2 | 256.427 | -36.366 | 349.14511841 | 2.78820606 | 85.6584 | 53808.5453240741 | 53809.2216782407 | 400003010 | 25230.8 | 50000 | 25230.8 | 25233.2 | 25230.8 | 25230.8 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 20050.7 | 20050.7 | 58434 | 2 | PROCESSED | 57533.2006365741 | 54247 | 54041.9132060185 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001026 | We propose Suzaku observations of two luminous low-mass X-ray binaries (Z sources), GX 349+2 and Cyg X-2, to investigate the origin of the hard tails of Z sources, of which the spectral photon indices are reported to become occasionally less than unity. With the high sensitivity of the HXD, we detect the spectral shape up to several 100 keV and reveal existence of particle acceleration caused by high radiation pressure. | GALACTIC POINT SOURCES | 4 | A | TAKAHASHI | HIROMITSU | NULL | NULL | JAP | 0 | SWG | SUZAKU OBSERVATIONS OF THE HARD TAILS OF LUMINOUS LOW-MASS X-RAY BINARIES (Z SOURCES) | HXD | N |
| GX 349+2 | 256.4194 | -36.3657 | 349.14166441 | 2.79326977 | 78.9359 | 53813.9267708333 | 53814.6043402778 | 400003020 | 28117.7 | 50000 | 28117.7 | 28131.7 | 28120.4 | 28120.4 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 25657.3 | 25657.3 | 58538 | 0 | PROCESSED | 57533.2767939815 | 54247 | 54042.1657407407 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001026 | We propose Suzaku observations of two luminous low-mass X-ray binaries (Z sources), GX 349+2 and Cyg X-2, to investigate the origin of the hard tails of Z sources, of which the spectral photon indices are reported to become occasionally less than unity. With the high sensitivity of the HXD, we detect the spectral shape up to several 100 keV and reveal existence of particle acceleration caused by high radiation pressure. | GALACTIC POINT SOURCES | 4 | A | TAKAHASHI | HIROMITSU | NULL | NULL | JAP | 0 | SWG | SUZAKU OBSERVATIONS OF THE HARD TAILS OF LUMINOUS LOW-MASS X-RAY BINARIES (Z SOURCES) | HXD | N |
| SS CYG | 325.6789 | 43.5736 | 90.55119171 | -7.12024619 | 276.5788 | 53676.0503703704 | 53676.9856944444 | 400006010 | 39451.2 | 40000 | 39451.2 | 39451.2 | 39451.2 | 39451.2 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 32047.2 | 32047.2 | 80810 | 1 | PROCESSED | 57527.7175925926 | 54247 | 54036.9898148148 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001043 | Although the boundary layer that is formed between the rapidly rotating inner accretion disk and the white dwarf surface has been known as a hard-X-ray emitter, its geometry and structure has not been well understood yet. We aim to investigate the boundary layer structure with SS Cyg, the brightest dwarf nova, by means of a soft X-ray component with the BI CCD, a fluorescent Fe K-alpha line with the FI CCDs, and a continuum reflection by the white dwarf surface with the HXD PIN. It is of great use to observe states of a different mass accretion rate, and hence we propose to observe both in quiescence and in outburst. | GALACTIC POINT SOURCES | 4 | A | ISHIDA | MANABU | NULL | NULL | JAP | 0 | SWG | SS CYG OBSERVATION IN QUIESCENCE | NULL | N |
| SS CYG | 325.6842 | 43.5739 | 90.55430501 | -7.12254626 | 256.8767 | 53692.6066203704 | 53693.8646759259 | 400007010 | 56043 | 60000 | 56059 | 56179 | 56043 | 56059 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 54357.2 | 54357.2 | 108665.8 | 2 | PROCESSED | 57528.0435763889 | 54247 | 54037.9128472222 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001044 | Although the boundary layer that is formed between the rapidly rotating inner accretion disk and the white dwarf surface has been known as a hard-X-ray emitter, its geometry and structure has not been well understood yet. We aim to investigate the boundary layer structure with SS Cyg, the brightest dwarf nova, by means of a soft X-ray component with the BI CCD, a fluorescent Fe K-alpha line with the FI CCDs, and a continuum reflection by the white dwarf surface with the HXD PIN. It is of great use to observe states of a different mass accretion rate, and hence we propose to observe both in quiescence and in outburst. | GALACTIC POINT SOURCES | 4 | A | ISHIDA | MANABU | NULL | NULL | JAP | 0 | SWG-TOO | SS CYG OBSERVATION IN OUTBURST | XIS | N |
| X1630-472 | 248.4828 | -47.3401 | 336.93914719 | 0.29801709 | 78.3341 | 53774.6318981482 | 53775.1390972222 | 400010010 | 22190.2 | 200000 | 22190.2 | 22190.2 | 22190.2 | 22190.2 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 22247 | 22247 | 43816 | 0 | PROCESSED | 57532.9380787037 | 54247 | 54040.9540856482 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001058 | We propose to monitor a transient black hole binary in outburst through a series of 20 ks observations. Our goal is to map the physical conditions in the accretion disk as the source evolves through the various continuum states using the spectral diagnostics available in the Fe K fluorescence emission. Measurements of the Fe K emission will allow us to quantify the thermal, kinematic, and geometric conditions in both the disk and the surrounding material. Correlating the Fe K diagnostics with sensitive measurements of the direct and reprocessed continuum emission will allow us to map the evolving conditions and constrain models of the dynamic accretion processes in black hole binaries. We will monitor 7 targets with the RXTE. This observation will be triggered when one becomes active. | GALACTIC POINT SOURCES | 4 | A | COTTAM | JEAN | NULL | NULL | JAP | 0 | SWG-TOO | FE K SPECTROSCOPY OF TRANSIENT BLACK HOLE BINARIES | HXD | N |
| X1630-472 | 248.4706 | -47.343 | 336.93140696 | 0.30212129 | 69.0657 | 53781.9791087963 | 53782.5474305556 | 400010020 | 21429 | 200000 | 21429 | 21485 | 21429 | 21429 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 17022.3 | 17022.3 | 49101.9 | 0 | PROCESSED | 57533.0117592593 | 54247 | 54041.4892013889 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001058 | We propose to monitor a transient black hole binary in outburst through a series of 20 ks observations. Our goal is to map the physical conditions in the accretion disk as the source evolves through the various continuum states using the spectral diagnostics available in the Fe K fluorescence emission. Measurements of the Fe K emission will allow us to quantify the thermal, kinematic, and geometric conditions in both the disk and the surrounding material. Correlating the Fe K diagnostics with sensitive measurements of the direct and reprocessed continuum emission will allow us to map the evolving conditions and constrain models of the dynamic accretion processes in black hole binaries. We will monitor 7 targets with the RXTE. This observation will be triggered when one becomes active. | GALACTIC POINT SOURCES | 4 | A | COTTAM | JEAN | NULL | NULL | JAP | 0 | SWG-TOO | FE K SPECTROSCOPY OF TRANSIENT BLACK HOLE BINARIES | HXD | N |
| X1630-472 | 248.4772 | -47.3405 | 336.93627828 | 0.30053306 | 75.5959 | 53794.9708333333 | 53795.6968055556 | 400010030 | 21521.6 | 200000 | 21521.6 | 21521.6 | 21521.6 | 21521.6 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 19032.8 | 19032.8 | 62718 | 0 | PROCESSED | 57533.1079050926 | 54247 | 54041.5956018518 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001058 | We propose to monitor a transient black hole binary in outburst through a series of 20 ks observations. Our goal is to map the physical conditions in the accretion disk as the source evolves through the various continuum states using the spectral diagnostics available in the Fe K fluorescence emission. Measurements of the Fe K emission will allow us to quantify the thermal, kinematic, and geometric conditions in both the disk and the surrounding material. Correlating the Fe K diagnostics with sensitive measurements of the direct and reprocessed continuum emission will allow us to map the evolving conditions and constrain models of the dynamic accretion processes in black hole binaries. We will monitor 7 targets with the RXTE. This observation will be triggered when one becomes active. | GALACTIC POINT SOURCES | 4 | A | COTTAM | JEAN | NULL | NULL | JAP | 0 | SWG-TOO | FE K SPECTROSCOPY OF TRANSIENT BLACK HOLE BINARIES | HXD | N |
| X1630-472 | 248.5414 | -47.3441 | 336.96314137 | 0.26612574 | 120.5775 | 53802.0758796296 | 53802.7300231482 | 400010040 | 21248.1 | 200000 | 21248.1 | 21249.9 | 21249.9 | 21249.9 | 3 | 3 | 3 | 3 | 1 | 0 | 0 | 20477.8 | 20477.8 | 56512 | 0 | PROCESSED | 57533.1620486111 | 54247 | 54041.7698726852 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001058 | We propose to monitor a transient black hole binary in outburst through a series of 20 ks observations. Our goal is to map the physical conditions in the accretion disk as the source evolves through the various continuum states using the spectral diagnostics available in the Fe K fluorescence emission. Measurements of the Fe K emission will allow us to quantify the thermal, kinematic, and geometric conditions in both the disk and the surrounding material. Correlating the Fe K diagnostics with sensitive measurements of the direct and reprocessed continuum emission will allow us to map the evolving conditions and constrain models of the dynamic accretion processes in black hole binaries. We will monitor 7 targets with the RXTE. This observation will be triggered when one becomes active. | GALACTIC POINT SOURCES | 4 | A | COTTAM | JEAN | NULL | NULL | JAP | 0 | SWG-TOO | FE K SPECTROSCOPY OF TRANSIENT BLACK HOLE BINARIES | HXD | N |
| X1630-472 | 248.5239 | -47.3401 | 336.95804041 | 0.27755382 | 107.6616 | 53809.226412037 | 53809.743912037 | 400010050 | 23167.1 | 200000 | 23175.1 | 23176.9 | 23176.8 | 23167.1 | 2 | 1 | 2 | 2 | 1 | 0 | 0 | 18860.5 | 18860.5 | 44706 | 0 | PROCESSED | 57533.2189930556 | 54247 | 54041.9302662037 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001058 | We propose to monitor a transient black hole binary in outburst through a series of 20 ks observations. Our goal is to map the physical conditions in the accretion disk as the source evolves through the various continuum states using the spectral diagnostics available in the Fe K fluorescence emission. Measurements of the Fe K emission will allow us to quantify the thermal, kinematic, and geometric conditions in both the disk and the surrounding material. Correlating the Fe K diagnostics with sensitive measurements of the direct and reprocessed continuum emission will allow us to map the evolving conditions and constrain models of the dynamic accretion processes in black hole binaries. We will monitor 7 targets with the RXTE. This observation will be triggered when one becomes active. | GALACTIC POINT SOURCES | 4 | A | COTTAM | JEAN | NULL | NULL | JAP | 0 | SWG-TOO | FE K SPECTROSCOPY OF TRANSIENT BLACK HOLE BINARIES | HXD | N |
| X1630-472 | 248.5405 | -47.3458 | 336.96147829 | 0.2654214 | 120.3 | 53817.4260300926 | 53817.9313425926 | 400010060 | 21654.1 | 200000 | 21662.1 | 21654.1 | 21654.1 | 21654.1 | 2 | 1 | 2 | 2 | 1 | 0 | 0 | 22761.9 | 22761.9 | 43655.9 | 1 | PROCESSED | 57533.3033796296 | 54247 | 54042.1043287037 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001058 | We propose to monitor a transient black hole binary in outburst through a series of 20 ks observations. Our goal is to map the physical conditions in the accretion disk as the source evolves through the various continuum states using the spectral diagnostics available in the Fe K fluorescence emission. Measurements of the Fe K emission will allow us to quantify the thermal, kinematic, and geometric conditions in both the disk and the surrounding material. Correlating the Fe K diagnostics with sensitive measurements of the direct and reprocessed continuum emission will allow us to map the evolving conditions and constrain models of the dynamic accretion processes in black hole binaries. We will monitor 7 targets with the RXTE. This observation will be triggered when one becomes active. | GALACTIC POINT SOURCES | 4 | A | COTTAM | JEAN | NULL | NULL | JAP | 0 | SWG-TOO | FE K SPECTROSCOPY OF TRANSIENT BLACK HOLE BINARIES | HXD | N |
| 4U1626-67 | 248.0601 | -67.4675 | 321.78071552 | -13.09322804 | 103.0359 | 53803.0543518518 | 53805.818275463 | 400015010 | 102639.2 | 100000 | 102654 | 102639.2 | 102647.2 | 102654 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 93393.2 | 93393.2 | 238781.9 | 3 | PROCESSED | 57533.2349652778 | 54247 | 54042.4663657407 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001081 | The X-ray spectrum of the 7 second LMXRB pulsar 4U1626-67 is dominated by low energy line emission with little evedence of iron K line in the pulse phase resolved spectra. It showd also cyclotron line at 37 keV that departs from the correlation of energy cutoff cyclotron energy observed in many other X-ray pulsars. This Suzaku observation allow to characterize the overall continuum, the low energy, the iron K alpha and cyclotron lines as function of the pulse phase, | GALACTIC POINT SOURCES | 4 | A | ANGELINI | LORELLA | NULL | NULL | JAP | 0 | SWG | 4U1626-67: PHASE RESOLVED SPECTRA AND CYCLOTRON LINE | XIS | N |
| CH CYG | 291.1621 | 50.2424 | 81.86550652 | 15.56609243 | 185.7481 | 53739.5736458333 | 53740.2919560185 | 400016020 | 33305.8 | 25000 | 33307.5 | 33337.8 | 33315.5 | 33305.8 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 28461.5 | 28461.5 | 62056 | 1 | PROCESSED | 57532.6355902778 | 54247 | 54039.6712268518 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001082 | CH Cygni is a symbiotic star in which a white dwarf is believed to be accreting the wind of the red giant. ASCA observation revealed a complex X-ray spectrum consisting of a heavily absorbed hard component and a relatively unabsorbed soft component. We propose to obtain the spectrum of CH Cyg above 10 keV for the first time using Suzaku HXD (PIN), while simultaneously obtaining high quality spectrum below 10 keV with the XIS. | GALACTIC POINT SOURCES | 4 | A | MUKAI | KOJI | NULL | NULL | JAP | 0 | SWG | SUZAKU OBSERVATION OF THE SYMBIOTIC SYSTEM CH CYGNI | XIS | N |
| CH CYG | 291.1168 | 50.2494 | 81.85997028 | 15.59541424 | 38.1861 | 53883.3112962963 | 53884.1502199074 | 400016030 | 35144 | 35000 | 35152 | 35160 | 35160 | 35144 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 37459 | 37459 | 72447.9 | 1 | PROCESSED | 57534.4573726852 | 54258 | 54109.7043981482 | 3.0.22.43 | 9 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001082 | CH Cygni is a symbiotic star in which a white dwarf is believed to be accreting the wind of the red giant. ASCA observation revealed a complex X-ray spectrum consisting of a heavily absorbed hard component and a relatively unabsorbed soft component. We propose to obtain the spectrum of CH Cyg above 10 keV for the first time using Suzaku HXD (PIN), while simultaneously obtaining high quality spectrum below 10 keV with the XIS. | GALACTIC POINT SOURCES | 4 | A | MUKAI | KOJI | NULL | NULL | JAP | 0 | SWG | SUZAKU OBSERVATION OF THE SYMBIOTIC SYSTEM CH CYGNI | XIS | N |
| JUPITER | 226.5694 | -16.1887 | 343.96536778 | 35.7224308 | 118.4901 | 53790.7643402778 | 53791.7940277778 | 401001010 | 37759.4 | 36000 | 37767.4 | 37759.4 | 37767.4 | 37767.4 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 32836.1 | 32836.1 | 88936.1 | 1 | PROCESSED | 57533.0781597222 | 54401 | 53905.533900463 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011003 | We propose XIS observations of Jupiter with an exposure time of 144 ks (4 planetary rotations). Our goals are: 1) to obtain and study the highest resolution x-ray CCD spectra of Jupiter's planetary x-ray emission, including separation into auroral and low-latitude components; and 2) to fully characterize the high energy (>1 keV) auroral component recently discovered in 2003 XMM-Newton data. These spectral studies will provide greater understanding of the physical properties of, and physical processes occurring in, the planet's magnetosphere. This research supports the National and NASA objectives of exploring the Solar System, in particular the Jupiter system, and the universe, and of understanding their structure, in particular Jupiter's magnetospheric and atmospheric structure. | GALACTIC POINT SOURCES | 4 | C | ELSNER | RONALD | NULL | NULL | USA | 1 | AO1 | JUPITER OBSERVATIONS WITH THE XIS: THE X-RAY SPECTRUM | XIS | N |
| JUPITER | 226.5948 | -16.1928 | 343.98613419 | 35.70433361 | 118.4906 | 53791.7941319445 | 53792.7940277778 | 401001020 | 37704 | 36000 | 37704 | 37704 | 37704 | 37704 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 32778.1 | 32778.1 | 86360 | 1 | PROCESSED | 57533.0943981482 | 54401 | 53905.5035416667 | 3.0.22.43 | 6 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011003 | We propose XIS observations of Jupiter with an exposure time of 144 ks (4 planetary rotations). Our goals are: 1) to obtain and study the highest resolution x-ray CCD spectra of Jupiter's planetary x-ray emission, including separation into auroral and low-latitude components; and 2) to fully characterize the high energy (>1 keV) auroral component recently discovered in 2003 XMM-Newton data. These spectral studies will provide greater understanding of the physical properties of, and physical processes occurring in, the planet's magnetosphere. This research supports the National and NASA objectives of exploring the Solar System, in particular the Jupiter system, and the universe, and of understanding their structure, in particular Jupiter's magnetospheric and atmospheric structure. | GALACTIC POINT SOURCES | 4 | C | ELSNER | RONALD | NULL | NULL | USA | 1 | AO1 | JUPITER OBSERVATIONS WITH THE XIS: THE X-RAY SPECTRUM | XIS | N |
| JUPITER | 226.6157 | -16.1957 | 344.00356707 | 35.68981432 | 118.4907 | 53792.7940856482 | 53793.8599421296 | 401001030 | 40791.2 | 36000 | 40799.2 | 40791.2 | 40799.2 | 40799.2 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 35536.3 | 35536.3 | 92073.9 | 0 | PROCESSED | 57533.1063078704 | 54401 | 53905.5868055556 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011003 | We propose XIS observations of Jupiter with an exposure time of 144 ks (4 planetary rotations). Our goals are: 1) to obtain and study the highest resolution x-ray CCD spectra of Jupiter's planetary x-ray emission, including separation into auroral and low-latitude components; and 2) to fully characterize the high energy (>1 keV) auroral component recently discovered in 2003 XMM-Newton data. These spectral studies will provide greater understanding of the physical properties of, and physical processes occurring in, the planet's magnetosphere. This research supports the National and NASA objectives of exploring the Solar System, in particular the Jupiter system, and the universe, and of understanding their structure, in particular Jupiter's magnetospheric and atmospheric structure. | GALACTIC POINT SOURCES | 4 | C | ELSNER | RONALD | NULL | NULL | USA | 1 | AO1 | JUPITER OBSERVATIONS WITH THE XIS: THE X-RAY SPECTRUM | XIS | N |
| JUPITER | 226.6349 | -16.1983 | 344.01962259 | 35.67652355 | 118.4908 | 53793.86 | 53794.9585532407 | 401001040 | 42255.8 | 36000 | 42263.8 | 42263.8 | 42263.8 | 42255.8 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 35706.7 | 35706.7 | 94905.9 | 2 | PROCESSED | 57533.1103819444 | 54401 | 53906.5712615741 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011003 | We propose XIS observations of Jupiter with an exposure time of 144 ks (4 planetary rotations). Our goals are: 1) to obtain and study the highest resolution x-ray CCD spectra of Jupiter's planetary x-ray emission, including separation into auroral and low-latitude components; and 2) to fully characterize the high energy (>1 keV) auroral component recently discovered in 2003 XMM-Newton data. These spectral studies will provide greater understanding of the physical properties of, and physical processes occurring in, the planet's magnetosphere. This research supports the National and NASA objectives of exploring the Solar System, in particular the Jupiter system, and the universe, and of understanding their structure, in particular Jupiter's magnetospheric and atmospheric structure. | GALACTIC POINT SOURCES | 4 | C | ELSNER | RONALD | NULL | NULL | USA | 1 | AO1 | JUPITER OBSERVATIONS WITH THE XIS: THE X-RAY SPECTRUM | XIS | N |
| XB1323-619 | 201.6454 | -62.1418 | 307.02498182 | 0.45033402 | 99.5731 | 54109.4794907407 | 54110.9168402778 | 401002010 | 55936.8 | 50000 | 55936.8 | 55936.8 | 0 | 55936.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 81817.3 | 81817.3 | 124176.9 | 1 | PROCESSED | 57536.8666087963 | 54735 | 54133.0271759259 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010002 | XB 1323-619 is a non-transient dipping LMXB and one of the few LMXB with spectrum extending to high energies. Our XMM-Newton observation revealed many lines including Fe XXV and XXVI absorption. Uniquely, the rate of bursting has increased systematically over 18 years by 15 times to every 20 min in 2006/07 making it the best source for study of absorption in bursts. Suzaku allows measurement of ADC temperature via the high energy cut-off and can give the first detection of cooling by soft photons from the neutron star from the change of cut-off energy during bursts. Curve-of-growth analysis gives the absorber temperature and tests our suggestion that absorption lines are formed in the ADC. Detailed comparison with burst theory is possible because of the regular bursting. | GALACTIC POINT SOURCES | 4 | C | DOTANI | TADAYASU | NULL | NULL | JAP | 1 | AO1 | BORADBAND INVESTIGATIONS OF THE DIPPING, BURSTGING LOW MASS X-RAY BINARY XB1323-619 | XIS | Y |
| SS 433 | 287.9531 | 4.9906 | 39.69950989 | -2.2379409 | 78.6445 | 53829.6109606482 | 53830.5327662037 | 401003010 | 38676.7 | 40000 | 38676.7 | 38676.7 | 38676.7 | 38676.7 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 28241.1 | 28241.1 | 79634 | 1 | PROCESSED | 57533.395162037 | 54394 | 53906.1478125 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010031 | SS433 is the most intensively studied jet source, however the nature of the object and the jet-formation mechanism remain unknown. We propose to examine the fundamental system parameters; the jet's mass-outflow rate and the total X-ray luminosity. The ionized or blue-shifted iron absorption edge recently discovered with XMM-Newton indicates either the absorber is photo-ionized by a hidden X-ray as luminous as 1E39 erg/s, or is moving along with the jet. SS433 may be an ultra-luminous source if seen face-on, or an unobserved cool component may coexist in the X-ray jet. The spectral continuum over 10 keV to be obtained with the HXD and the absorption edge by the XIS will reveal the nature of the absorber. | GALACTIC POINT SOURCES | 4 | A | KAWAI | NOBUYUKI | NULL | NULL | JAP | 1 | AO1 | SS 433 OBSERVATIONS OF THE HARD X-RAY CONTINUUM AND THE IRON ABSORPTION EDGE | XIS | N |
| SS 433 | 287.9527 | 4.99 | 39.69879316 | -2.23786427 | 78.6446 | 53833.4611458333 | 53834.4579166667 | 401004010 | 40197.6 | 40000 | 40221.6 | 40197.6 | 40229.6 | 40213.6 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 30474.9 | 30474.9 | 86110 | 2 | PROCESSED | 57533.4357638889 | 54400 | 53906.5501736111 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010031 | SS433 is the most intensively studied jet source, however the nature of the object and the jet-formation mechanism remain unknown. We propose to examine the fundamental system parameters; the jet's mass-outflow rate and the total X-ray luminosity. The ionized or blue-shifted iron absorption edge recently discovered with XMM-Newton indicates either the absorber is photo-ionized by a hidden X-ray as luminous as 1E39 erg/s, or is moving along with the jet. SS433 may be an ultra-luminous source if seen face-on, or an unobserved cool component may coexist in the X-ray jet. The spectral continuum over 10 keV to be obtained with the HXD and the absorption edge by the XIS will reveal the nature of the absorber. | GALACTIC POINT SOURCES | 4 | A | KAWAI | NOBUYUKI | NULL | NULL | JAP | 1 | AO1 | SS 433 OBSERVATIONS OF THE HARD X-RAY CONTINUUM AND THE IRON ABSORPTION EDGE | XIS | N |
| G11.2-0.3 | 272.8676 | 19.433 | 46.34586116 | 17.29738119 | 77.6432 | 53834.4626041667 | 53835.6634143518 | 401010010 | 43984.6 | 50000 | 43992.6 | 43984.6 | 43992.6 | 43992.6 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 37387.9 | 37387.9 | 83679.9 | 1 | PROCESSED | 57533.4279166667 | 54397 | 53905.4671875 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010049 | The PSR 1811-1925 in a historical supernova remnant G11.2-0.3 has its characteristic age as 10 times longer than the age of the remnant. The pulsar has its period 64 ms and the hard spectrum. We suggest that the pulsar shows the signs of having the small magnetic field. The SUZAKU observation must give the answer for this hypothesis. First, HXD allows us to observe the spectrum in the high energy range, and if the cut-off would be observed, the magnetic fields of pulsar will be estimate. Seconds, XIS has the great energy resolution to determine the abundance of the shell. This would let us estimate the mass of the progenitor. Third, HXD provides the new spin down rate observation. Then, we can make sure the constancy of the spin down rate. The pulsar age mystery must be solved by SUZAKU. | GALACTIC POINT SOURCES | 4 | C | HAYATO | ASAMI | NULL | NULL | JAP | 1 | AO1 | CLEARING UP THE MECHANISM OF THE PSR J1811-1925 IN SNR G11.2-0.3 | XIS | N |
| CYGNUS X-3 | 308.2593 | 40.981 | 79.93230299 | 0.62160244 | 252.424 | 54052.0902893518 | 54054.3676388889 | 401011010 | 99744.5 | 100000 | 99746.2 | 99746.2 | 0 | 99744.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 95389.3 | 95389.3 | 196745 | 1 | PROCESSED | 57536.1520717593 | 54456 | 54088.9545023148 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010058 | We propose an observation of the unusual X-ray binary Cygnus X-3. Cyg X-3 is a final stage of the massive binary stars consisting of a WR(N) star and a compact star. However the nature of the compact star is not well understood. We have fore scientific objective. (A)Determine the Doppler modulation of iron K lines and discuss the binary nature. (2) Determine the iron abundance in the WR wind. (3) Search for the high energy cut off about 100keV of the power law component. (4) Search for the X-ray emission from radio knots. For these four sciences, we propose 100ksec observation of Cyg X-3. | GALACTIC POINT SOURCES | 4 | C | KITAMOTO | SHUNJI | NULL | NULL | JAP | 1 | AO1 | WIDE BAND OBSERVATION OF CYGNUS X-3 WITH SUZAKU | SPE | Y |
| LMC X-2 | 80.025 | -71.9941 | 283.14092563 | -32.7117801 | 313.3022 | 53849.381712963 | 53850.7731365741 | 401012010 | 56152 | 60000 | 56165.7 | 56165.7 | 56152 | 56160 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 73408 | 73408 | 120193.8 | 1 | PROCESSED | 57533.5735300926 | 54394 | 53907.6288078704 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010090 | We propose the Suzaku observation of LMC X-2, to detect the slim disk structure in its flaring branch. The luminosity of LMC X-2 is always as luminous as the Eddington limit, and the absorption is so low that the energy spectrum can be observed over the 0.2-30 keV energy range. Then, LMC X-2 is the best target to study whether the disk structure becomes the slim disk or not. | GALACTIC POINT SOURCES | 4 | B | TAKAHASHI | HIROMITSU | NULL | NULL | JAP | 1 | AO1 | DETECTION OF SLIM-DISK STRUCTURE FROM LOW-MASS X-RAY BINARY LMC X-2 | HXD | N |
| SGR1806-20 | 272.1595 | -20.349 | 10.0481975 | -0.20823053 | 88.7483 | 54189.6305555556 | 54190.0627199074 | 401021010 | 19288.9 | 20000 | 19288.9 | 19595 | 0 | 19356.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16507.1 | 16507.1 | 37327.9 | 1 | PROCESSED | 57538.0253587963 | 54561 | 54209.5169212963 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010124 | We propose a study of proton cyclotron structures and broadband burst spectra of SGRs, magnetar candidate, which are believed to have very strong magnetic field of the order of 10^15 G. Although many observations have been made by different instruments in the space, their spectra and magnetic field are yet to be well understood. The first scientific goal is the detection of proton cyclotron structures. It allows us a direct measurement of a magnetic field intensity. The second scientific goal is to reveal the burst spectral shape in a wide-band and to find out common properties to magnetars, i.e., SGRs and AXPs. We will trigger the Suzaku observation when one of the following two criteria is satisfied; 1) the burst activity becomes high state, or 2) the giant flare occurs. | GALACTIC POINT SOURCES | 4 | A | NAKAGAWA | YUJIN | NULL | NULL | JAP | 1 | AO1-TOO | PROTON CYCLOTRON STRUCTURE AND BROADBAND SPECTRA OF "SGR" | HXD | N |
| SGR1900+14 | 286.803 | 9.3875 | 43.07594962 | 0.80149907 | 86.5533 | 53826.3631597222 | 53826.9113310185 | 401022010 | 17056.2 | 20000 | 17704.6 | 21707.4 | 21655.5 | 17056.2 | 1 | 2 | 1 | 1 | 1 | 0 | 0 | 14360.4 | 14360.4 | 47336 | 1 | PROCESSED | 57533.34875 | 54394 | 53906.0977893518 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010124 | We propose a study of proton cyclotron structures and broadband burst spectra of SGRs, magnetar candidate, which are believed to have very strong magnetic field of the order of 10^15 G. Although many observations have been made by different instruments in the space, their spectra and magnetic field are yet to be well understood. The first scientific goal is the detection of proton cyclotron structures. It allows us a direct measurement of a magnetic field intensity. The second scientific goal is to reveal the burst spectral shape in a wide-band and to find out common properties to magnetars, i.e., SGRs and AXPs. We will trigger the Suzaku observation when one of the following two criteria is satisfied; 1) the burst activity becomes high state, or 2) the giant flare occurs. | GALACTIC POINT SOURCES | 4 | A | NAKAGAWA | YUJIN | NULL | NULL | JAP | 1 | AO1-TOO | PROTON CYCLOTRON STRUCTURE AND BROADBAND SPECTRA OF "SGR" | HXD | N |
| HESS J1837-069 | 279.4395 | -6.8651 | 25.2664546 | -0.10276403 | 102.6144 | 54164.5341898148 | 54165.4286342593 | 401026010 | 42191.1 | 40000 | 42191.1 | 42199.1 | 0 | 42207.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37702.1 | 37702.1 | 77259.9 | 1 | PROCESSED | 57537.6010185185 | 54750 | 54171.2613425926 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010131 | The HESS (High Energy Stereoscopic System) collaboration has recently reported the TeV survey of the inner-part of the Galaxy, which revealed the existence of a new population of gamma-ray objects. Most of which are unknown, but at least two of them, HESS J1813-178 and HESS J1837-069 are point-like, and the ASCA Galactic survey and the INTEGRAL survey detected the counterparts in 0.5-10 keV and 20-100 keV, respectively. Making full use of Suzaku's wide-band spectral capability, we will study spectral characteristics of HESS J1813-178 and HESS J1837-069 in 0.5 keV to ~200 keV, and investigate for their origins. We will also carry out pulse-search to evaluate the pulsar-wind hypothesis. | GALACTIC POINT SOURCES | 4 | B | EBISAWA | KEN | NULL | NULL | JAP | 1 | AO1 | INVESTIGATION OF TWO HESS SOURCES DETECTED WITH INTEGRAL | HXD | Y |
| 1E1207.4-5209 | 182.5062 | -52.436 | 296.5458403 | 9.92149786 | 302.4939 | 53946.5682060185 | 53948.2603587963 | 401030010 | 96351.9 | 120000 | 96351.9 | 102278.4 | 96367.9 | 96351.9 | 3 | 2 | 3 | 3 | 1 | 0 | 0 | 94049.8 | 94049.8 | 135379.9 | 1 | PROCESSED | 57535.1230787037 | 54750 | 54132.8187268518 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010152 | 1E1207.4-5209 may be the most exotic astronomical object. We propose a temporal and spectroscopic study of this peculiar X-ray source that was regarded as a "cooling" isolated NS. The previous Chandra/Newton observations reported "harmonic absorption" lines at 0.7, 1.4 and 2.1keV. Possible interpretations are electron cyclotron lines at B = 10^{10} G, ionic transition lines at 10^{12-13} G, and proton cyclotron lines at 10^{14} G. These are inconsistent each other. The highest B-field could suggest that the source is a member of "magnetars". Alternative explanation is the source might be a "strange" star with a lower mass. Suzaku observation of these line features should be the most powerful tool to investigate B field of this very peculiar object. | GALACTIC POINT SOURCES | 4 | B | YOSHIDA | ATSUMASA | NULL | NULL | JAP | 1 | AO1 | A STUDY OF A PECULIAR X-RAY SOURCE 1E1207.4-5209 | XIS | N |
| 1E1207.4-5209 | 182.4916 | -52.442 | 296.53791481 | 9.91413144 | 148.6893 | 54146.2087384259 | 54147.6390509259 | 401030020 | 49826.6 | 50000 | 50073.4 | 49826.6 | 0 | 50089.4 | 1 | 2 | 0 | 1 | 1 | 0 | 0 | 44446.8 | 44446.8 | 123576 | 2 | PROCESSED | 57537.4372337963 | 54750 | 54153.9886458333 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010152 | 1E1207.4-5209 may be the most exotic astronomical object. We propose a temporal and spectroscopic study of this peculiar X-ray source that was regarded as a "cooling" isolated NS. The previous Chandra/Newton observations reported "harmonic absorption" lines at 0.7, 1.4 and 2.1keV. Possible interpretations are electron cyclotron lines at B = 10^{10} G, ionic transition lines at 10^{12-13} G, and proton cyclotron lines at 10^{14} G. These are inconsistent each other. The highest B-field could suggest that the source is a member of "magnetars". Alternative explanation is the source might be a "strange" star with a lower mass. Suzaku observation of these line features should be the most powerful tool to investigate B field of this very peculiar object. | GALACTIC POINT SOURCES | 4 | B | YOSHIDA | ATSUMASA | NULL | NULL | JAP | 1 | AO1 | A STUDY OF A PECULIAR X-RAY SOURCE 1E1207.4-5209 | XIS | Y |
| AB DOR | 82.2835 | -65.427 | 275.26967334 | -33.00819219 | 154.6774 | 54060.0265277778 | 54061.4586111111 | 401031010 | 53451.7 | 80000 | 53451.7 | 53459.7 | 0 | 53461.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48033.4 | 48033.4 | 123708 | 1 | PROCESSED | 57536.170462963 | 54502 | 54133.0222916667 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011021 | We propose to observe the rapidly rotating star AB Doradus for 80 ks with Suzaku Our main goals are to detect non-thermal hard X-rays and fluorescent Fe at 6.4 keV with the HXD and the XIS during a stellar flare. Such a spectral feature can be induced by non-thermal electrons in the impulsive flare phase, or by X-rays of the very hot flare plasma. The hard X-ray detectors will be used to detect non-thermal bremsstrahlung expected when a beam of non-thermal electrons (typically observed in the radio) impacts the dense chromosphere. We will also study the coronal element composition and its temporal evolution during the flare. Finally, we will attempt coordination with the Australian Telescope to monitor the non-thermal electron population, without any timing constraint for Suzaku. | GALACTIC POINT SOURCES | 4 | B | AUDARD | MARC | NULL | NULL | USA | 1 | AO1 | NON-THERMAL HARD X-RAYS AND FLUORESCENT FE IN STELLAR FLARES | HXD | N |
| AB DOR | 82.2881 | -65.4658 | 275.31538375 | -33.00189818 | 204.2849 | 54108.0647569444 | 54109.4724421296 | 401031020 | 49096.5 | 45000 | 49096.5 | 49096.5 | 0 | 49096.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44961.1 | 44961.1 | 121619.9 | 2 | PROCESSED | 57536.5000578704 | 54502 | 54133.0127083333 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011021 | We propose to observe the rapidly rotating star AB Doradus for 80 ks with Suzaku Our main goals are to detect non-thermal hard X-rays and fluorescent Fe at 6.4 keV with the HXD and the XIS during a stellar flare. Such a spectral feature can be induced by non-thermal electrons in the impulsive flare phase, or by X-rays of the very hot flare plasma. The hard X-ray detectors will be used to detect non-thermal bremsstrahlung expected when a beam of non-thermal electrons (typically observed in the radio) impacts the dense chromosphere. We will also study the coronal element composition and its temporal evolution during the flare. Finally, we will attempt coordination with the Australian Telescope to monitor the non-thermal electron population, without any timing constraint for Suzaku. | GALACTIC POINT SOURCES | 4 | B | AUDARD | MARC | NULL | NULL | USA | 1 | AO1 | NON-THERMAL HARD X-RAYS AND FLUORESCENT FE IN STELLAR FLARES | HXD | N |
| HR 9024 | 357.4125 | 36.4308 | 109.27773456 | -24.79729068 | 49.8624 | 53939.0616782407 | 53940.6016087963 | 401032010 | 58775.7 | 60000 | 58799.7 | 58775.7 | 58783.7 | 58791.7 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 56011.6 | 56011.6 | 133039.8 | 1 | PROCESSED | 57535.042025463 | 54401 | 53950.2624074074 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011022 | Suzaku-XIS is the best available instrument to study the Fe fluorescence emission from late-type evolved stars. Fe fluorescence is produced by illumination of the photosphere by ionizing coronal X-rays and its intensity depends on the height of the X-ray source. We propose to observe Fe fluorescence in the single G-type giant HR 9024 and in the active RS CVn system II Peg to obtain a direct geometrical constraint on the scale height of their coronal structures. These two stars have the brightest Fe fluorescence features of all the late-type stars observed by the Chandra-HETGS and their different stellar parameters (stellar radius, gravity, multiplicity,..) and evolutionary stage will allow us to probe the typical coronal scale for significantly different conditions. | GALACTIC POINT SOURCES | 4 | B | TESTA | PAOLA | NULL | NULL | USA | 1 | AO1 | GEOMETRY DIAGNOSTICS FROM FE FLUORESCENT EMISSION IN LATE-TYPE EVOLVED STARS | XIS | N |
| SIGMA^2 CRB | 243.6552 | 33.7881 | 54.56402364 | 46.14689859 | 281.1207 | 53969.4764467593 | 53972.1925231482 | 401034010 | 109160.4 | 110000 | 109190.4 | 109160.4 | 109168.4 | 109176.4 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 98837.6 | 98837.6 | 234653.9 | 3 | PROCESSED | 57535.3877777778 | 54526 | 54021.2578587963 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011025 | Suzaku is a powerful instrument for studying the hot (>100 MK) coronal quiescent and flare emission from RS CVn binaries. We propose to obtain 110 ksec (3 day elapsed time) observations of the RS CVn systems Sigma^2 CrB (F6V + G0V) and Sigma Gem (K0III +?). Our goals are i) to better characterize their hard (> 10 keV) emission, ii) to understand the origin of coronal thermal and nonthermal plasma by studying the evolution of the coronal thermal structure, and iii) to investigate the persistent and flaring nonthermal electron population using a combination of X-ray and radio cm+mm continuum data. Such studies require the long duty cycle of Suzaku observations and its high sensitivity, particularly the greatly enhanced capability in the 10-25 keV region provided by HXD. | GALACTIC POINT SOURCES | 4 | B | BROWN | ALEXANDER | NULL | NULL | USA | 1 | AO1 | SUZAKU OBSERVATIONS OF THERMAL AND NONTHERMAL CORONAL EMISSION ON THE RS CVN BINARIES SIGMA^2 CRB AND SIGMA GEM | HXD | N |
| BETA LYR | 282.5094 | 33.3738 | 63.19462876 | 14.79594569 | 59.4704 | 53862.545474537 | 53862.9952083333 | 401036010 | 20251.5 | 20000 | 20267.5 | 20251.5 | 20267.5 | 20267.5 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 9894.7 | 9894.7 | 38851.9 | 1 | PROCESSED | 57533.7394212963 | 54401 | 53913.8191550926 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011031 | The goal of our project is to determine the location and properties of the hard X-ray emitting gas in the massive B7II+B0V interacting binary Beta Lyr. Our experiment is designed to distinguish between X-rays originating in the mass transfer stream and those originating in the extended circumbinary envelope. Modeling of XIS spectra will allow us to constrain the plasma temperature and emission measure, while the light curve with three exposures and high count rates will probe variability at around the 1% level over both the orbital timescale (13 days) and dynamical flow timescales (hours). Our request is for 20 ksec exposures at 3 different orbital phases to catch the system in and out of eclipse. | GALACTIC POINT SOURCES | 4 | A | IGNACE | RICHARD | NULL | NULL | USA | 1 | AO1 | AN X-RAY STUDY OF HOT PLASMA IN THE INTERACTING BINARY BETA LYRAE | XIS | N |
| BETA LYR | 282.5098 | 33.3716 | 63.19266924 | 14.79477853 | 53.4974 | 53867.1260185185 | 53867.6252199074 | 401036020 | 21496.2 | 20000 | 21496.2 | 21496.2 | 21496.2 | 21496.2 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 19164.2 | 19164.2 | 43119.9 | 2 | PROCESSED | 57534.2764814815 | 54401 | 53914.2784143518 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011031 | The goal of our project is to determine the location and properties of the hard X-ray emitting gas in the massive B7II+B0V interacting binary Beta Lyr. Our experiment is designed to distinguish between X-rays originating in the mass transfer stream and those originating in the extended circumbinary envelope. Modeling of XIS spectra will allow us to constrain the plasma temperature and emission measure, while the light curve with three exposures and high count rates will probe variability at around the 1% level over both the orbital timescale (13 days) and dynamical flow timescales (hours). Our request is for 20 ksec exposures at 3 different orbital phases to catch the system in and out of eclipse. | GALACTIC POINT SOURCES | 4 | A | IGNACE | RICHARD | NULL | NULL | USA | 1 | AO1 | AN X-RAY STUDY OF HOT PLASMA IN THE INTERACTING BINARY BETA LYRAE | XIS | N |
| BETA LYR | 282.5093 | 33.3719 | 63.19278609 | 14.79528012 | 53.4973 | 53871.4311226852 | 53871.8571875 | 401036030 | 18195.4 | 20000 | 18195.4 | 18195.4 | 18195.4 | 18195.4 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 19842.1 | 19842.1 | 36807.9 | 0 | PROCESSED | 57534.3160532407 | 54401 | 53920.4164351852 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011031 | The goal of our project is to determine the location and properties of the hard X-ray emitting gas in the massive B7II+B0V interacting binary Beta Lyr. Our experiment is designed to distinguish between X-rays originating in the mass transfer stream and those originating in the extended circumbinary envelope. Modeling of XIS spectra will allow us to constrain the plasma temperature and emission measure, while the light curve with three exposures and high count rates will probe variability at around the 1% level over both the orbital timescale (13 days) and dynamical flow timescales (hours). Our request is for 20 ksec exposures at 3 different orbital phases to catch the system in and out of eclipse. | GALACTIC POINT SOURCES | 4 | A | IGNACE | RICHARD | NULL | NULL | USA | 1 | AO1 | AN X-RAY STUDY OF HOT PLASMA IN THE INTERACTING BINARY BETA LYRAE | XIS | N |
| 1RX J154814.5-452845 | 237.0511 | -45.4226 | 332.46961393 | 7.07040697 | 85.7358 | 54132.6368518518 | 54135.3543865741 | 401037010 | 99454.1 | 100000 | 99454.1 | 99462.1 | 0 | 99470.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 86855.2 | 86855.2 | 234783.8 | 3 | PROCESSED | 57537.0252777778 | 54702 | 54139.4767939815 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011102 | Intermediate Polars (IPs) are strong soft and hard X-ray sources and Suzaku is therefore ideally suited to their study. We have selected three IPs that are of particularly high priority. They have all been detected as hard (E>10 keV) X-ray sources; they all have a hot (kT~100 eV), blackbody-like component; none have been studied simultaneously over a wide band-pass. We therefore propose 80 ksec observations each of V2400 Oph, 1RXS J154814.5-452845, and 1RXS J213344.1+510725, with an additional 40 ksec background observation for V2400 Oph. We plan to analyze the average and phase-resolved spectra to determine the strength of the reflection continuum; the highest temperature present in the plasma; and the details of the complex absorber. | GALACTIC POINT SOURCES | 4 | A | MUKAI | KOJI | NULL | NULL | USA | 1 | AO1 | BROAD-BAND SPECTROSCOPY OF INTERMEDIATE POLARS: FROM THE SOFT COMPONENT TO REFLECTION | HXD | Y |
| 1RXS J213344.1+51072 | 323.4354 | 51.1973 | 94.50909334 | -0.42447705 | 94.0452 | 53854.2853009259 | 53856.2501736111 | 401038010 | 81924.1 | 80000 | 81924.1 | 81924.1 | 81924.1 | 81924.1 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 62888.1 | 62888.1 | 169726.1 | 3 | PROCESSED | 57533.6330671296 | 54391 | 53908.1887962963 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011102 | Intermediate Polars (IPs) are strong soft and hard X-ray sources and Suzaku is therefore ideally suited to their study. We have selected three IPs that are of particularly high priority. They have all been detected as hard (E>10 keV) X-ray sources; they all have a hot (kT~100 eV), blackbody-like component; none have been studied simultaneously over a wide band-pass. We therefore propose 80 ksec observations each of V2400 Oph, 1RXS J154814.5-452845, and 1RXS J213344.1+510725, with an additional 40 ksec background observation for V2400 Oph. We plan to analyze the average and phase-resolved spectra to determine the strength of the reflection continuum; the highest temperature present in the plasma; and the details of the complex absorber. | GALACTIC POINT SOURCES | 4 | A | MUKAI | KOJI | NULL | NULL | USA | 1 | AO1 | BROAD-BAND SPECTROSCOPY OF INTERMEDIATE POLARS: FROM THE SOFT COMPONENT TO REFLECTION | HXD | N |
| V893 SCO | 243.8144 | -28.6275 | 348.06577336 | 15.88028883 | 274.6746 | 53973.4024189815 | 53974.056412037 | 401041010 | 18497.8 | 20000 | 18497.8 | 18497.8 | 18497.8 | 18497.8 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 16140.3 | 16140.3 | 56482 | 0 | PROCESSED | 57535.3695601852 | 54526 | 54053.4763888889 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011103 | The RXTE All-Sky Slew Survey (XSS) catalog, containing 294 objects detected in the 3-20 keV sky, is of great potential use for a variety of purposes. Included in this catalog are two sources identified with lesser known dwarf novae, V893 Sco and SS Aur. Although these are known to be soft X-ray sources from the ROSAT All-sky Survey, there has never been a pointed observation with an imaging X-ray telescope of either object. Here I propose short Suzaku observations of V893 Sco and SS Aur to check the reliability of XSS fluxes, hence that of the luminosity functions derived from the XSS catalog. In addition, such observations serve as a pilot study to determine if these individual dwarf novae may merit further in-depth X-ray studies. | GALACTIC POINT SOURCES | 4 | B | MUKAI | KOJI | NULL | NULL | USA | 1 | AO1 | CONFIRMING THE IDENTIFICATION OF RXTE ALL-SKY SLEW SURVEY SOURCES WITH DWARF NOVAE | XIS | N |
| T CRB | 239.8773 | 25.9106 | 42.36027985 | 48.16117824 | 268.9321 | 53984.9474652778 | 53986.0911921296 | 401043010 | 46303.3 | 50000 | 46311.3 | 46311.3 | 46319.3 | 46303.3 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 45431.4 | 45431.4 | 98815.9 | 1 | PROCESSED | 57535.5107175926 | 54526 | 54053.4340856482 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011106 | Hard X-ray emission up to ~100 keV has recently been detected with INTEGRAL and Swift from 3 exceptional symbiotic stars. These 3 objects are members of a subclass of symbiotics characterized by rapid optical flickering, and in some cases jets, recurrent nova eruptions, and high-mass white dwarfs possibly headed toward supernova Type Ia explosion. The origin of the hard X-ray emission from these accreting white dwarfs is a mystery. Broad-band X-ray observations, which only Suzaku can provide, are needed to bridge the gap between existing soft and hard X-ray spectra. We propose to perform such Suzaku observations of RT Cru, T CrB, and RS Oph to distinguish among thermal emission from a magnetic accretion column, non-thermal emission from a jet, or some unforeseen emission mechanism. | GALACTIC POINT SOURCES | 4 | A | SOKOLOSKI | JENNIFER | NULL | NULL | USA | 1 | AO1 | THE NATURE OF HARD X-RAY SYMBIOTIC BINARIES | XIS | N |
| 4U 1705-44 | 257.2295 | -44.1004 | 343.32321952 | -2.34240238 | 264.0794 | 53976.2429166667 | 53976.7731712963 | 401046010 | 18315.5 | 20000 | 18315.5 | 18315.5 | 18315.5 | 18315.5 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 15371.5 | 15371.5 | 45809.9 | 0 | PROCESSED | 57535.3889236111 | 54526 | 54021.306087963 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011112 | We propose 3x20 ks observations of the neutron star binary 4U 1705-44. The primary science goals are: 1) Accurately characterize the profile of the iron K line using the XIS, and determine whether the iron line is produced in a Comptonizing corona or is a fluorescence line produced in an accretion disk. 2) Measure the hard X-ray spectral shape up to 30 keV with the HXD, and determine the relative importance of thermal Comptonization vs. synchrotron or inverse-Compton emission from a jet. 3) Determine how the iron line and hard X-ray spectrum change with spectral state, and hence how the corona and/or disk change with spectral state (e.g. variations in corona size or disk inner radius), and the role of the jet in the low/hard state. | GALACTIC POINT SOURCES | 4 | A | YOUNG | ANDREW | NULL | NULL | USA | 1 | AO1 | REVEALING THE SPECTRAL COMPONENTS OF 4U 1705-44 | XIS | N |
| 4U 1705-44 | 257.2281 | -44.1019 | 343.32141433 | -2.34248879 | 264.0666 | 53996.5173611111 | 53996.8619675926 | 401046020 | 17134 | 20000 | 17342 | 17134 | 17334 | 17334 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 15447.7 | 15447.7 | 29767.9 | 0 | PROCESSED | 57535.6082175926 | 54526 | 54020.9055555556 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011112 | We propose 3x20 ks observations of the neutron star binary 4U 1705-44. The primary science goals are: 1) Accurately characterize the profile of the iron K line using the XIS, and determine whether the iron line is produced in a Comptonizing corona or is a fluorescence line produced in an accretion disk. 2) Measure the hard X-ray spectral shape up to 30 keV with the HXD, and determine the relative importance of thermal Comptonization vs. synchrotron or inverse-Compton emission from a jet. 3) Determine how the iron line and hard X-ray spectrum change with spectral state, and hence how the corona and/or disk change with spectral state (e.g. variations in corona size or disk inner radius), and the role of the jet in the low/hard state. | GALACTIC POINT SOURCES | 4 | A | YOUNG | ANDREW | NULL | NULL | USA | 1 | AO1 | REVEALING THE SPECTRAL COMPONENTS OF 4U 1705-44 | XIS | N |
| 4U 1705-44 | 257.2313 | -44.1028 | 343.32206131 | -2.34487049 | 297.0793 | 54014.4242708333 | 54015.0891087963 | 401046030 | 20065 | 20000 | 20065 | 20065 | 20065 | 20065 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 17919.6 | 17919.6 | 57423.9 | 2 | PROCESSED | 57535.7945138889 | 54526 | 54021.6765162037 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011112 | We propose 3x20 ks observations of the neutron star binary 4U 1705-44. The primary science goals are: 1) Accurately characterize the profile of the iron K line using the XIS, and determine whether the iron line is produced in a Comptonizing corona or is a fluorescence line produced in an accretion disk. 2) Measure the hard X-ray spectral shape up to 30 keV with the HXD, and determine the relative importance of thermal Comptonization vs. synchrotron or inverse-Compton emission from a jet. 3) Determine how the iron line and hard X-ray spectrum change with spectral state, and hence how the corona and/or disk change with spectral state (e.g. variations in corona size or disk inner radius), and the role of the jet in the low/hard state. | GALACTIC POINT SOURCES | 4 | A | YOUNG | ANDREW | NULL | NULL | USA | 1 | AO1 | REVEALING THE SPECTRAL COMPONENTS OF 4U 1705-44 | XIS | N |
| 4U 1820-30 | 275.9207 | -30.3623 | 2.78792233 | -7.91550172 | 265.9754 | 53992.9234606482 | 53993.6605902778 | 401047010 | 25700.8 | 37000 | 25700.8 | 25810.9 | 25723.9 | 25714.8 | 2 | 1 | 2 | 2 | 1 | 0 | 0 | 31878.2 | 31878.2 | 63633.9 | 1 | PROCESSED | 57535.6012962963 | 54526 | 54021.2227083333 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011113 | The potential well around low-magnetic field neutron stars is very similar to that around Schwarzschild black holes. Doppler shifts expected at the inner disk around such neutron stars should be very similar, and should produce relativistic FeK-alpha emission lines like those observed in some black hole systems. To date, however, relativistically broadened FeK-alpha emission lines have not been clearly detected in neutron star systems, in part because their lines are generally weaker than those found in black hole systems. We propose to observe the neutron star binaries 4U 1820-30, Cygnus X-2, and Serpens X-1 for 37 ksec each in Suzaku Cycle 1, to confirm possible evidence of relativistic broadening. Relativistic phenomena and accretion studies are central to NASA's ``SEU'' theme. | GALACTIC POINT SOURCES | 4 | B | MILLER | JON | NULL | NULL | USA | 1 | AO1 | A SUZAKU STUDY OF BROAD IRON LINES IN NEUTRON STAR BINARIES | XIS | N |
| SERPENS X-1 | 279.9934 | 5.0285 | 36.11311789 | 4.83561165 | 256.1423 | 54032.2853819444 | 54033.2259143518 | 401048010 | 37157.8 | 37000 | 37157.8 | 37269.8 | 37205.8 | 37165.8 | 2 | 1 | 2 | 2 | 1 | 0 | 0 | 31069.5 | 31069.5 | 81239.9 | 2 | PROCESSED | 57535.9734722222 | 54526 | 54056.4719328704 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011113 | The potential well around low-magnetic field neutron stars is very similar to that around Schwarzschild black holes. Doppler shifts expected at the inner disk around such neutron stars should be very similar, and should produce relativistic FeK-alpha emission lines like those observed in some black hole systems. To date, however, relativistically broadened FeK-alpha emission lines have not been clearly detected in neutron star systems, in part because their lines are generally weaker than those found in black hole systems. We propose to observe the neutron star binaries 4U 1820-30, Cygnus X-2, and Serpens X-1 for 37 ksec each in Suzaku Cycle 1, to confirm possible evidence of relativistic broadening. Relativistic phenomena and accretion studies are central to NASA's ``SEU'' theme. | GALACTIC POINT SOURCES | 4 | B | MILLER | JON | NULL | NULL | USA | 1 | AO1 | A SUZAKU STUDY OF BROAD IRON LINES IN NEUTRON STAR BINARIES | XIS | N |
| CYGNUS X-2 | 326.1653 | 38.3323 | 87.3318132 | -11.3049847 | 76.3142 | 53871.8636805556 | 53872.7293171296 | 401049010 | 39390.3 | 37000 | 39390.3 | 39406.3 | 39390.3 | 39390.3 | 2 | 1 | 2 | 2 | 1 | 0 | 0 | 36880.4 | 36880.4 | 74786 | 1 | PROCESSED | 57534.3858217593 | 54401 | 53927.6429166667 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011113 | The potential well around low-magnetic field neutron stars is very similar to that around Schwarzschild black holes. Doppler shifts expected at the inner disk around such neutron stars should be very similar, and should produce relativistic FeK-alpha emission lines like those observed in some black hole systems. To date, however, relativistically broadened FeK-alpha emission lines have not been clearly detected in neutron star systems, in part because their lines are generally weaker than those found in black hole systems. We propose to observe the neutron star binaries 4U 1820-30, Cygnus X-2, and Serpens X-1 for 37 ksec each in Suzaku Cycle 1, to confirm possible evidence of relativistic broadening. Relativistic phenomena and accretion studies are central to NASA's ``SEU'' theme. | GALACTIC POINT SOURCES | 4 | B | MILLER | JON | NULL | NULL | USA | 1 | AO1 | A SUZAKU STUDY OF BROAD IRON LINES IN NEUTRON STAR BINARIES | XIS | N |
| 4U 1636-536 | 250.2262 | -53.7541 | 332.91086545 | -4.81751491 | 91.2457 | 54140.3877546296 | 54140.99125 | 401050010 | 24232 | 19000 | 24232 | 24232 | 0 | 24232 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 21689.5 | 21689.5 | 52136 | 0 | PROCESSED | 57537.3410069445 | 54525 | 54151.5052893518 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011117 | Transitions between soft and hard spectral states in LMXBs involve significant reconfigurations of the accretion flow, which are poorly understood. In neutron star LMXBs, the boundary layer may hold additional key information for distinguishing between various proposed models for the hard state spectrum. With the aim to improve our understanding of the evolution of the boundary layer, we propose to observe the neutron star LMXB 4U 1636-536 with Suzaku in different spectral states. The high-sensitivity broadband coverage provided by Suzaku will be used to follow the evolution of the boundary layer and study other phenomena that might constrain the accretion flow properties. We request four 15 ks Suzaku observations of 4U 1636-536 spaced throughout one state transition cycle. | GALACTIC POINT SOURCES | 4 | A | HOMAN | JEROEN | NULL | NULL | USA | 1 | AO1 | THE VARIABLE BOUNDARY LAYER IN THE NEUTRON-STAR LMXB 4U 1636-536 | XIS | Y |
| 4U 1636-536 | 250.2273 | -53.7542 | 332.91122007 | -4.81806999 | 91.2447 | 54153.2955787037 | 54154.3544560185 | 401050020 | 40096 | 38000 | 40096 | 40104 | 0 | 40096 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 35550 | 35550 | 91477.9 | 0 | PROCESSED | 57537.4821990741 | 54525 | 54158.392037037 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011117 | Transitions between soft and hard spectral states in LMXBs involve significant reconfigurations of the accretion flow, which are poorly understood. In neutron star LMXBs, the boundary layer may hold additional key information for distinguishing between various proposed models for the hard state spectrum. With the aim to improve our understanding of the evolution of the boundary layer, we propose to observe the neutron star LMXB 4U 1636-536 with Suzaku in different spectral states. The high-sensitivity broadband coverage provided by Suzaku will be used to follow the evolution of the boundary layer and study other phenomena that might constrain the accretion flow properties. We request four 15 ks Suzaku observations of 4U 1636-536 spaced throughout one state transition cycle. | GALACTIC POINT SOURCES | 4 | A | HOMAN | JEROEN | NULL | NULL | USA | 1 | AO1 | THE VARIABLE BOUNDARY LAYER IN THE NEUTRON-STAR LMXB 4U 1636-536 | XIS | Y |
| 4U 1636-536 | 250.2272 | -53.754 | 332.91133194 | -4.81789372 | 91.2454 | 54160.0424421296 | 54160.8931597222 | 401050030 | 38719.3 | 38000 | 38727.4 | 38719.3 | 0 | 38719.4 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 48145.9 | 48145.9 | 73498 | 1 | PROCESSED | 57537.5161111111 | 54695 | 54167.6400462963 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011117 | Transitions between soft and hard spectral states in LMXBs involve significant reconfigurations of the accretion flow, which are poorly understood. In neutron star LMXBs, the boundary layer may hold additional key information for distinguishing between various proposed models for the hard state spectrum. With the aim to improve our understanding of the evolution of the boundary layer, we propose to observe the neutron star LMXB 4U 1636-536 with Suzaku in different spectral states. The high-sensitivity broadband coverage provided by Suzaku will be used to follow the evolution of the boundary layer and study other phenomena that might constrain the accretion flow properties. We request four 15 ks Suzaku observations of 4U 1636-536 spaced throughout one state transition cycle. | GALACTIC POINT SOURCES | 4 | A | HOMAN | JEROEN | NULL | NULL | USA | 1 | AO1 | THE VARIABLE BOUNDARY LAYER IN THE NEUTRON-STAR LMXB 4U 1636-536 | XIS | Y |
| 4U 1636-536 | 250.2277 | -53.7538 | 332.91167841 | -4.81798429 | 93.2445 | 54186.4802777778 | 54187.3043287037 | 401050040 | 32130.4 | 38000 | 32130.4 | 32138.4 | 0 | 32130.4 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 27784.2 | 27784.2 | 71177.9 | 1 | PROCESSED | 57538.0141782407 | 54695 | 54209.541412037 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011117 | Transitions between soft and hard spectral states in LMXBs involve significant reconfigurations of the accretion flow, which are poorly understood. In neutron star LMXBs, the boundary layer may hold additional key information for distinguishing between various proposed models for the hard state spectrum. With the aim to improve our understanding of the evolution of the boundary layer, we propose to observe the neutron star LMXB 4U 1636-536 with Suzaku in different spectral states. The high-sensitivity broadband coverage provided by Suzaku will be used to follow the evolution of the boundary layer and study other phenomena that might constrain the accretion flow properties. We request four 15 ks Suzaku observations of 4U 1636-536 spaced throughout one state transition cycle. | GALACTIC POINT SOURCES | 4 | A | HOMAN | JEROEN | NULL | NULL | USA | 1 | AO1 | THE VARIABLE BOUNDARY LAYER IN THE NEUTRON-STAR LMXB 4U 1636-536 | XIS | Y |
| 4U 1636-536 | 250.2259 | -53.7533 | 332.911352 | -4.8168543 | 100.7755 | 54188.4720717593 | 54188.7856944445 | 401050050 | 12241.8 | 38000 | 12249.8 | 12241.8 | 0 | 12249.8 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 11804 | 11804 | 27088 | 0 | PROCESSED | 57537.9973148148 | 54695 | 54200.4687731482 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011117 | Transitions between soft and hard spectral states in LMXBs involve significant reconfigurations of the accretion flow, which are poorly understood. In neutron star LMXBs, the boundary layer may hold additional key information for distinguishing between various proposed models for the hard state spectrum. With the aim to improve our understanding of the evolution of the boundary layer, we propose to observe the neutron star LMXB 4U 1636-536 with Suzaku in different spectral states. The high-sensitivity broadband coverage provided by Suzaku will be used to follow the evolution of the boundary layer and study other phenomena that might constrain the accretion flow properties. We request four 15 ks Suzaku observations of 4U 1636-536 spaced throughout one state transition cycle. | GALACTIC POINT SOURCES | 4 | A | HOMAN | JEROEN | NULL | NULL | USA | 1 | AO1 | THE VARIABLE BOUNDARY LAYER IN THE NEUTRON-STAR LMXB 4U 1636-536 | XIS | Y |
| 4U 1822-37 | 276.4461 | -37.1042 | 356.85149319 | -11.29112534 | 258.4537 | 54010.4563888889 | 54011.5189699074 | 401051010 | 37743.4 | 40000 | 37768.2 | 37768.2 | 37743.4 | 37743.4 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 33178.5 | 33178.5 | 91805.9 | 0 | PROCESSED | 57535.7615393518 | 54695 | 54024.6539814815 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011121 | We propose a 40 ks observation of the accretion disk corona source 4U 1822-37. Despite repeated observations over the years and even excellent high-resolution data from the Chandra Observatory, the nature and origin of the corona and even the source of the Fe K fluorescence emission remains controversial. The spectral resolution of the XIS and the broad-band coverage provided by the combined XIS and HXD instruments make Suzaku uniquely suited to a definitive measurement. Determining the physical conditions in this source is particularly interesting. Because of its geometry 4U 1822-37 is a link between x-ray binaries and AGN, and an therefore serve as a laboratory for studying accretion processes throughout the universe. | GALACTIC POINT SOURCES | 4 | B | COTTAM | JEAN | NULL | NULL | USA | 1 | AO1 | ACCRETION PHYSICS IN THE ADC SOURCE 4U 1822-37 | XIS | Y |
| IGRJ16465-4507 | 251.6303 | -45.1738 | 340.00343338 | 0.10772124 | 284.9562 | 53987.3839814815 | 53987.9203009259 | 401052010 | 22527.9 | 20000 | 22535.9 | 22527.9 | 22535.9 | 22535.9 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 24645.4 | 24645.4 | 46332 | 0 | PROCESSED | 57535.4975925926 | 54526 | 54021.113287037 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011132 | INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources. | GALACTIC POINT SOURCES | 4 | A | SMITH | RANDALL | NULL | NULL | USA | 1 | AO1 | HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYS | HXD | N |
| SWIFTJ2000.6+3210 | 300.0869 | 32.2033 | 68.99570836 | 1.1443147 | 87.4233 | 53837.6619212963 | 53837.9139351852 | 401053010 | 12438.4 | 20000 | 12444 | 12451.2 | 12451.2 | 12438.4 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 9876.7 | 9876.7 | 21767.9 | 0 | PROCESSED | 57533.4456134259 | 54775 | 53927.3549189815 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011132 | INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources. | GALACTIC POINT SOURCES | 4 | A | SMITH | RANDALL | NULL | NULL | USA | 1 | AO1 | HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYS | HXD | N |
| SWIFTJ2000.6+3210 | 300.1137 | 32.1218 | 68.93835501 | 1.08211502 | 255.6072 | 54039.0205671296 | 54039.3029976852 | 401053020 | 12748.4 | 10000 | 12756.4 | 12748.4 | 12756.4 | 12756.4 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 11727 | 11727 | 24393.9 | 0 | PROCESSED | 57535.9859490741 | 54775 | 54056.1959953704 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011132 | INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources. | GALACTIC POINT SOURCES | 4 | A | SMITH | RANDALL | NULL | NULL | USA | 1 | AO1 | HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYS | HXD | Y |
| IGRJ16493-4348 | 252.3173 | -43.8652 | 341.31911758 | 0.57823277 | 287.444 | 54013.8822916667 | 54014.4204166667 | 401054010 | 21199.8 | 20000 | 21215.8 | 21215.8 | 21199.8 | 21207.8 | 3 | 3 | 3 | 3 | 1 | 0 | 0 | 20219.7 | 20219.7 | 46463.9 | 1 | PROCESSED | 57535.7818634259 | 54695 | 54025.4796412037 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011132 | INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources. | GALACTIC POINT SOURCES | 4 | A | SMITH | RANDALL | NULL | NULL | USA | 1 | AO1 | HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYS | HXD | Y |
| SWIFTJ1010.1-5747 | 152.7309 | -57.8539 | 282.8705066 | -1.37559689 | 290.7012 | 53891.2175 | 53891.5544560185 | 401055010 | 19171.7 | 20000 | 19171.7 | 19171.7 | 19171.7 | 19171.7 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 17877.8 | 17877.8 | 29087.9 | 0 | PROCESSED | 57534.4906944444 | 54401 | 53926.1075347222 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011132 | INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources. | GALACTIC POINT SOURCES | 4 | A | SMITH | RANDALL | NULL | NULL | USA | 1 | AO1 | HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYS | HXD | N |
| IGRJ16195-4945 | 244.8541 | -49.816 | 333.49117084 | 0.29973526 | 284.0301 | 53998.8508333333 | 53999.7231481482 | 401056010 | 39148.6 | 40000 | 39148.6 | 39148.6 | 39148.6 | 39148.6 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 42265.2 | 42265.2 | 75357.9 | 1 | PROCESSED | 57535.652662037 | 54526 | 54020.9227199074 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011132 | INTEGRAL has discovered a new type of highly absorbed Galactic X-ray sources with column densities of 1e23 cm^-2 or more. This is larger than Galactic interstellar column density and much larger than the optical extinction would imply, so the absorbing material must be concentrated on X-ray source. These may form an entirely new class with a common origin, or may simply be the highly obscured tail of the distribution of High and Low Mass X-ray Binaries. We propose to observe three these sources along with two new possibilities from the Swift BAT survey. Our goal is to observe the hard X-rays with the HXD and Fe K lines with the XIS to simultaneously measure the total flux, column density, and line strengths, in order to better understand the physics behind these intriguing new sources. | GALACTIC POINT SOURCES | 4 | A | SMITH | RANDALL | NULL | NULL | USA | 1 | AO1 | HIGHLY ABSORBED GALACTIC X-RAY SOURCES IN SOFT AND HARD X-RAYS | HXD | N |
| 4U1907+09 | 287.4013 | 9.8378 | 43.74739314 | 0.48531727 | 60.2599 | 53857.2580324074 | 53858.7322222222 | 401057010 | 58440.3 | 60000 | 58440.3 | 58456.3 | 58448.3 | 58456.3 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 38821.5 | 38821.5 | 127353.9 | 1 | PROCESSED | 57533.6690509259 | 54401 | 53913.4367476852 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011133 | We propose 60ksec of Suzaku observations of the high mass X-ray binary 4U1907+09, to study the little known spectrum of the source below 2keV and to measure its behavior during its frequent dips, where matter ceases to accrete onto the magnetic poles of the neutron star. Making use of Suzaku's unique broad band capabilities, we will also perform pulse phase spectroscopy of the cyclotron line and study the parameters of the fundamental and first harmonic cyclotron lines, as 4U1907+09 is one of the few accreting neutron stars where two cyclotron lines lie within the energy range of the XIS and HXD-PIN detectors. The scientific aims of this proposal address questions within NASA's Goals and Research Focus Area ``Structure and Evolution of the Universe''. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 1 | AO1 | THE BROAD BAND SPECTRUM OF 4U1907+09 | XIS | N |
| 4U1700-37 | 255.9894 | -37.8441 | 347.75582102 | 2.17172645 | 269.6945 | 53991.447662037 | 53992.918912037 | 401058010 | 81442.5 | 80000 | 81456.9 | 81470.4 | 81442.5 | 81454.4 | 3 | 3 | 3 | 3 | 1 | 0 | 0 | 82109.3 | 82109.3 | 127109 | 1 | PROCESSED | 57535.6097916667 | 54526 | 54053.5428240741 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011135 | The compact object in the massive X-ray binary 4U1700-37/HD153919 has been inferred to be a neutron star based on its spectral shape, but no pulsations have been observed. One possible explanation for the absence of observed pulsations is that the pulsed signal is beamed in directions other than our line of sight. This can be tested using Suzaku by searching for pulsations in the iron K line. This line is formed efficiently under almost all conditions of ionization and temperature, and so represents an X-ray bolometer which should respond to pulsed X-rays no matter where they are pointed. We plan to make such a search, and to probe the other properties of the wind and compact object in this system by observing with Suzaku for 80 ks away from eclipse. | GALACTIC POINT SOURCES | 4 | A | KALLMAN | TIMOTHY | NULL | NULL | USA | 1 | AO1 | IRON LINE VARIABILITY IN 4U1700-37 | XIS | N |
| CYGNUS X-1 | 299.6124 | 35.133 | 71.28577556 | 3.01567368 | 256.2202 | 54038.1501273148 | 54038.8225 | 401059010 | 27706.8 | 30000 | 27706.8 | 27737.8 | 27706.8 | 27706.8 | 2 | 1 | 2 | 2 | 1 | 0 | 0 | 27689.2 | 27689.2 | 58083.9 | 0 | PROCESSED | 57535.9949768518 | 54526 | 54063.4924884259 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011141 | We request three, 30 ksec observations of Cyg X-1, to be coordinated with our ongoing RXTE and Ryle radio telescope monitoring campaign. Suzaku will bring three unique attributes to this campaign: the ability to describe the 0.5-3 keV spectrum (crucial for describing the disk spectrum), high spectral resolution in the Fe line region (crucial for resolving narrow from relativistically broadened features), and the 200-600 keV spectrum (crucial for distinguishing among thermal corona, non-thermal corona, and jet models). By coordinating with our ongoing monitoring program, we not only obtain useful cross-calibration information, we will be able to place current and future Suzaku observations of Cyg X-1 in the context of the source's global history. | GALACTIC POINT SOURCES | 4 | B | NOWAK | MICHAEL | NULL | NULL | USA | 1 | AO1 | ENHANCING THE LONG TERM MONITORING CAMPAIGN OF CYGNUS X-1 IN THE SUZAKU ERA | HXD | N |
| GX 339-4 | 255.7025 | -48.7916 | 338.93635594 | -4.32587966 | 86.7489 | 54143.2316087963 | 54146.2003009259 | 401068010 | 77205.3 | 100000 | 83893.5 | 77205.3 | 0 | 82113.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 94026 | 94026 | 256484 | 4 | PROCESSED | 57537.4905208333 | 54535 | 54167.7751851852 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011146 | Skewed iron emission lines from the inner accretion disk and broad-band disk reflection spectra are incisive diagnostics of relativistic effects and the inner accretion flow geometry in black hole binaries. With its high effective area, efficient instrument modes, and sensitivity in hard X-rays, Suzaku is ideally suited to fully exploit these diagnostics. We request a total of 154 ksec in up to four observations to observe a black hole transient in outburst, using a scheme tailored to accommodate different source fluxes and Suzaku's observing windows. We will support these observations with a global multi-wavelength network of observatories. Understanding accretion onto black holes is central to NASA's ``SEU'' research theme. | GALACTIC POINT SOURCES | 4 | A | MILLER | JON | NULL | NULL | USA | 1 | AO1-TOO | SUZAKU OBSERVATIONS OF A BLACK HOLE TRANSIENT IN OUTBURST | XIS | N |
| SGR 1806-20 | 272.166 | -20.4729 | 9.94279657 | -0.27364584 | 269.9473 | 53987.9261921296 | 53989.1668287037 | 401092010 | 48915.5 | 50000 | 48915.5 | 48923.5 | 48931.5 | 48931.5 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 55408.5 | 55408.5 | 107175.9 | 1 | PROCESSED | 57535.5272453704 | 54526 | 54021.1112615741 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012017 | The soft gamma-ray repeater SGR 1806-20 has recently emitted the most powerful giant flare ever observed from these sources. This probably involved a large scale restructuring of the magnetosphere, leading to observable variations in the properties of its persistent emission, from IR to hard X-rays. We propose to observe SGR 1806-20 with Suzaku considering the unique opportunity offered by this satellite to study the spectrum of this source simultaneously both in the soft and hard X-ray bands. We also suggest to coordinate this observation with a simultaneous XMM-Newton one, in order to obtain a significantly better determination of the broad band spectral parameters. | GALACTIC POINT SOURCES | 4 | B | MEREGHETTI | SANDRO | NULL | NULL | EUR | 1 | AO1 | COORDINATED SUZAKU AND XMM-NEWTON OBSERVATIONS OF SGR 1806-20 AFTER THE GIANT FLARE | HXD | N |
| ALGOL | 47.0831 | 40.8965 | 149.0355551 | -14.93487401 | 244.4771 | 54167.6197222222 | 54169.6132986111 | 401093010 | 102164.2 | 105000 | 102164.2 | 102164.2 | 0 | 102164.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 102472.9 | 102472.9 | 172192.8 | 1 | PROCESSED | 57537.6825810185 | 54736 | 54186.3983564815 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012024 | Stellar and solar coronae reveal high-energy phenomena including the presence of accelerated electrons, explosive dissipation of magnetic energy, and heating to extreme temperatures. Many of these processes are likely to be physically related. We propose to use Suzaku's suite of instruments to observe the interplay between thermal and non-thermal high-energy processes in the active, eclipsing binary Algol. Our prime objective is the observation of hard X-rays above 10 keV, but also the appearance of an Fe fluorescence line that could be induced either by irradiation from flaring plasma or by electron beams. These models can be distinguished by correlating the emission with nonthermal hard X-rays as possibly detected by the HXD. | GALACTIC POINT SOURCES | 4 | C | GUEDEL | MANUEL | NULL | NULL | EUR | 1 | AO1 | A SYNOPTIC VIEW OF HIGH-ENERGY PHENOMENA IN THE CORONA OF ALGOL | HXD | Y |
| IGR J16318-4848 | 247.9691 | -48.8061 | 335.63186461 | -0.44896472 | 266.5948 | 53961.4825 | 53964.3488310185 | 401094010 | 97253.8 | 100000 | 97269.8 | 97253.8 | 97269.8 | 97269.8 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 87112.8 | 87112.8 | 247605.9 | 5 | PROCESSED | 57535.3483564815 | 54526 | 54020.9181597222 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012034 | We propose a detailed study of Compton thick X-ray absorption in neutral or weakly ionized material by using 100ksec of Suzaku observations of the strongly absorbed (N_H~2E24cm2) Galactic X-ray binary IGR J16318-4848. Measuring a high signal to noise ratio broad band spectrum will allow us to determine the curvature in the >10keV continuum caused by Compton downscattering in the absorber, to deduce its ionization state from observations of the Fe Kalpha line, and to study the variability of the source and the absorber. These observations will also shed more light onto the nature of the compact object in IGR J16318-4848. | GALACTIC POINT SOURCES | 4 | B | WILMS | JOERN | NULL | NULL | EUR | 1 | AO1 | OBSERVING IGR J16318-4848: PROBING COMPTON-THICK ABSORPTION | XIS | N |
| XB 1916-053 | 289.7027 | -5.2415 | 31.35614078 | -8.46800846 | 250.2538 | 54047.242974537 | 54048.1119791667 | 401095010 | 38464.7 | 40000 | 39096.7 | 39088.7 | 38464.7 | 39096.7 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 37485.7 | 37485.7 | 75082 | 2 | PROCESSED | 57536.0684259259 | 54735 | 54088.866087963 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012038 | We propose Suzaku observations of the dipping low mass X-ray binaries XB1916-053, XB1323-619, EXO0748-676 and X 1624-490. The changes in both the continuum and the He- and H- like Fe K absorption features during dips have been recently demonstrated to be consistent with a change in the properties of the photoionized absorbers present in these systems. We will use the XIS to characterise the photoionised absorbers and reliably determine the values of the ionization parameter for each source, and the simultaneous spectra of HXD to uniquely determine the underlying continuum shapes including any contributions due to reflection components and to extend the photoionized absorber fits to higher energies. This will test the validity of the ionized absorber model also >10 keV. | GALACTIC POINT SOURCES | 4 | A | DIAZ TRIGO | MARIA | NULL | NULL | EUR | 1 | AO1 | BROAD-BAND OBSERVATIONS OF HIGHLY-IONIZED ABSORBERS IN DIPPING LMXBS | XIS | Y |
| HESS J1731-347 | 263.0179 | -34.7706 | 353.53173388 | -0.68198005 | 79.8005 | 54154.7807060185 | 54155.7432291667 | 401099010 | 40618.9 | 38000 | 40626.9 | 40618.9 | 0 | 40626.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34647.9 | 34647.9 | 83155.9 | 0 | PROCESSED | 57537.4739351852 | 54528 | 54160.3931944444 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012042 | The hard (Gamma=2.0) TeV source HESS J1731-347 discovered in the H.E.S.S. Galactic plane survey has an intriguing possible counterpart seen in ROSAT survey data. The X-ray data show an unidentified, extended nebular structure with a hard spectrum, in close coincidence to the TeV source. It is plausible to assume that the same energetic particle population is responsible for the emission in both bands. Suzaku is optimally suited to establish the likely non-thermal nature of the X-ray spectrum and to search for the high-energy end of the emitting particle spectrum, which is likely visible in the HXD domain. The observations will help to clarify the nature of HESS J1731-347, which may be a new type of Galactic particle accelerator. | GALACTIC POINT SOURCES | 4 | A | PUEHLHOFER | GERD | NULL | NULL | EUR | 1 | AO1 | THE HIGH ENERGY PARTICLE SPECTRUM OF THE TEV/X-RAY NEBULA HESS J1731-347 | XIS | N |
| 1E 1841-045 | 280.3141 | -4.8735 | 27.4352849 | 0.03686802 | 77.3227 | 53844.4525462963 | 53847.1328009259 | 401100010 | 97962.2 | 100000 | 97962.2 | 97970.2 | 97970.9 | 97970.9 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 63474 | 63474 | 231539.9 | 2 | PROCESSED | 57533.5748032407 | 54401 | 53907.2806597222 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 014204 | Anomalous X-ray Pulsars are young radio-quiet pulsars with unconventional properties challenging conventional wisdom on neutron star formation and evolution. Their slow rotation periods, unprecedented for their apparent youth, point to enormous surface magnetic fields, a thousand times stronger than the typical inferred radio-pulsar field. The origin of the X-ray emission from these pulsars is still being debated. The recent discovery of a hard nonthermal pulsed X-ray emission from 1E 1841-045 with RXTE well beyond 10keV, can probably be explain by a magnetospheric origin and should extend above 100keV. The HXD onboard Suzaku gives us a unique opportunity to characterize the high-energy part of the emission with the added advantage to use the XIS to characterize the lower energy data. | GALACTIC POINT SOURCES | 4 | A | HARRUS | ILANA | NORII | MIKIO | USJ | 1 | AO1 | SUZAKU OBSERVATIONS OF THE ANOMALOUS X-RAY PULSAR 1E~1841-045 IN THE SNR KES 73 | HXD | N |
| HESSJ1813-178 | 273.3946 | -17.7704 | 12.87014503 | 0.01155473 | 90.9367 | 54160.8999768518 | 54162.2814699074 | 401101010 | 63839.1 | 65000 | 63847.1 | 63839.1 | 0 | 63847.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 57756.1 | 57756.1 | 119351.9 | 1 | PROCESSED | 57537.5358449074 | 54736 | 54167.6346990741 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 014214 | Radio and X-ray observations towards the VHE gamma-ray source HESS J1813-178, initially dubbed being a dark accelerator , suggested its association with a SNR. However, a recent XMM observation confirmed earlier ASCA findings of an extended, center-filled X-ray source, not resembling the contours of the radio-detected SNR. We propose hard X-ray observations to investigate the alternatively plerionic origin of HESS J1813-178, given the wide spectral coverage possible by XIS/HXD. This will clarify the discrepancy between ASCA and recent INTEGRAL data. Constructing a valid spectral energy distribution will enable us to constrain the age and field strength of the particle accelerator powering the synchrotron emission and accurately model the radiation processes up to VHE energies. | GALACTIC POINT SOURCES | 4 | B | REIMER | OLAF | EBISAWA | KEN | USJ | 1 | AO1 | IS THE ASSOCIATION OF HESS J1813-178/SNR G12.8-0.0 CONCEALING ITS TRUE PLERIONIC NATURE? | HXD | Y |
| EX HYA | 193.0706 | -29.2994 | 303.15288952 | 33.57198642 | 300.0004 | 54299.8912152778 | 54302.4377199074 | 402001010 | 100515.7 | 100000 | 100523.7 | 100515.7 | 0 | 100523.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 91113.5 | 91113.5 | 219959.9 | 1 | PROCESSED | 57539.3319097222 | 54707 | 54339.5139467593 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020008 | The standard theory of the post-shock plasma in intermediate polars predicts that the shock height is negligibly small compared with the radius of the white dwarf under normal accretion state. Some recent observational results, however, seem to contradict this prediction, and suggest that the shock height may be of the same order as the white dwarf radius. The shock height is an important quantity for the post-shock plasma in that it is deeply related to the mass accretion rate, heating and cooling mechanism of the post-shock plasma and so on. We therefore propose to observe two of the brightest intermediate polars EX Hya and V1223 Sgr to measure their shock height directly in terms of the reflection spectrum from the HXD-PIN and the iron K-shell structure from the XIS. | GALACTIC POINT SOURCES | 4 | A | ISHIDA | MANABU | NULL | NULL | JAP | 2 | AO2 | MEASUREMENT OF THE SHOCK HEIGHT IN INTERMEDIATE POLARS | HXD | Y |
| V1223 SGR | 283.7445 | -31.105 | 5.0082738 | -14.31987205 | 79.9528 | 54203.4803240741 | 54204.9418055556 | 402002010 | 60706 | 60000 | 60706 | 60706 | 0 | 60706 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46286.1 | 46286.1 | 126271.9 | 2 | PROCESSED | 57538.1822800926 | 54744 | 54210.6596875 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020008 | The standard theory of the post-shock plasma in intermediate polars predicts that the shock height is negligibly small compared with the radius of the white dwarf under normal accretion state. Some recent observational results, however, seem to contradict this prediction, and suggest that the shock height may be of the same order as the white dwarf radius. The shock height is an important quantity for the post-shock plasma in that it is deeply related to the mass accretion rate, heating and cooling mechanism of the post-shock plasma and so on. We therefore propose to observe two of the brightest intermediate polars EX Hya and V1223 Sgr to measure their shock height directly in terms of the reflection spectrum from the HXD-PIN and the iron K-shell structure from the XIS. | GALACTIC POINT SOURCES | 4 | A | ISHIDA | MANABU | NULL | NULL | JAP | 2 | AO2 | MEASUREMENT OF THE SHOCK HEIGHT IN INTERMEDIATE POLARS | HXD | Y |
| 1RXSJ174459.5-172640 | 266.2467 | -17.4406 | 9.76958181 | 6.08973572 | 101.0461 | 54555.6304050926 | 54556.5834953704 | 402003010 | 43579.3 | 40000 | 43595.3 | 43579.3 | 0 | 43603.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 29591.6 | 29591.6 | 82343.9 | 1 | PROCESSED | 57541.9975462963 | 54937 | 54570.1529282407 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020015 | We propose to study wide-band X-ray properties of 5 unidentified sources with luminosities of ~10^35 erg/s, which were detected in the ROSAT All Sky Survey. These sources are a part of the complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge constructed by Mori (2005). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the Suzaku fine spectra together with optical identifications. This is a new step toward understanding the formation history of the bulge. Furthermore, because the luminosity range we observe corresponds to a "missing link" region ever studied for a neutron star or black-hole X-ray binary, our results are also unique to test acrretion disk theories at intermediate mass accretion rates. | GALACTIC POINT SOURCES | 4 | C | MORI | HIDEYUKI | NULL | NULL | JAP | 2 | AO2 | SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE | XIS | Y |
| 1RXSJ165256.3-264503 | 253.236 | -26.7533 | 355.1420085 | 10.81079439 | 277.5876 | 54337.0024421296 | 54338.0419444444 | 402004010 | 49582.2 | 40000 | 49582.2 | 49582.2 | 0 | 49582.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46658.1 | 46658.1 | 89777.9 | 2 | PROCESSED | 57539.6777083333 | 54723 | 54350.4155092593 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020015 | We propose to study wide-band X-ray properties of 5 unidentified sources with luminosities of ~10^35 erg/s, which were detected in the ROSAT All Sky Survey. These sources are a part of the complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge constructed by Mori (2005). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the Suzaku fine spectra together with optical identifications. This is a new step toward understanding the formation history of the bulge. Furthermore, because the luminosity range we observe corresponds to a "missing link" region ever studied for a neutron star or black-hole X-ray binary, our results are also unique to test acrretion disk theories at intermediate mass accretion rates. | GALACTIC POINT SOURCES | 4 | C | MORI | HIDEYUKI | NULL | NULL | JAP | 2 | AO2 | SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE | XIS | Y |
| 1RXS J070407.9+26250 | 106.0341 | 26.4126 | 190.27497025 | 14.29877104 | 282.0717 | 54548.4868865741 | 54549.9862384259 | 402008010 | 58315.7 | 50000 | 58323.7 | 58315.7 | 0 | 58323.7 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 49476.6 | 49476.6 | 129527.8 | 0 | PROCESSED | 57541.9808912037 | 54933 | 54566.326712963 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020029 | Soft Intermediate Polar (IP) is a small group of IPs whose X-ray spectrum is extremely soft compared with general IPs. Recent observations reveal that some soft IPs harbor a soft blackbody component like polars, yet its nature is not fully understood. Systematic study of the soft IP blackbody emission is important in the sense that it may provide a clue to understand possible evolutionary link from IPs to polars, the origin of the soft excess in polars, etc. We propose to observe five soft IPs, each for 50ksec, in order to search for the blackbody component and to measure their temperature and flux systematically. | GALACTIC POINT SOURCES | 4 | C | ISHIDA | MANABU | NULL | NULL | JAP | 2 | AO2 | OBSERVATIONS OF SOFT INTERMEDIATE POLARS | XIS | Y |
| 1RXS J180340.0+40121 | 270.932 | 40.2098 | 66.8583442 | 25.77561005 | 157.538 | 54478.0290972222 | 54479.1877777778 | 402009010 | 53090.7 | 50000 | 53090.7 | 53090.7 | 0 | 53090.7 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 44348.9 | 44348.9 | 100095.9 | 3 | PROCESSED | 57541.2965625 | 54864 | 54490.0707291667 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020029 | Soft Intermediate Polar (IP) is a small group of IPs whose X-ray spectrum is extremely soft compared with general IPs. Recent observations reveal that some soft IPs harbor a soft blackbody component like polars, yet its nature is not fully understood. Systematic study of the soft IP blackbody emission is important in the sense that it may provide a clue to understand possible evolutionary link from IPs to polars, the origin of the soft excess in polars, etc. We propose to observe five soft IPs, each for 50ksec, in order to search for the blackbody component and to measure their temperature and flux systematically. | GALACTIC POINT SOURCES | 4 | C | ISHIDA | MANABU | NULL | NULL | JAP | 2 | AO2 | OBSERVATIONS OF SOFT INTERMEDIATE POLARS | XIS | Y |
| 4U 0142+61 | 26.4803 | 61.7944 | 129.32255084 | -0.39946076 | 40.959 | 54325.1695949074 | 54327.5209259259 | 402013010 | 99674.4 | 100000 | 99674.4 | 99674.4 | 0 | 99674.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 101609.6 | 101609.6 | 203129.7 | 4 | PROCESSED | 57549.823900463 | 54730 | 54347.6221296296 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020058 | Recently, high energy pulsed x-ray emissions from anomalous x-ay pulsears have been founded. This emissions extend to neary 100 keV with photon index ~1, and the emission mechanism is unknown. In order to trace this enigmatic component, we propose the observation of the anomalous x-ray pulsar 4u 0142+61 with 100 ksec exposures. The main aim of this observation is to examine how high energy this emission extend to. Because the these emissions are almost 100% pulsed component, so using the pulse on-off method, we can achive the ultimate sensitivity not depending on the reproducibility of the background but depending only on the photon statistics. If the spectrum have the strong break neary ~250 keV, this emissions have originated as the compton scatterd photons in the star surface. | GALACTIC POINT SOURCES | 4 | A | ENOTO | TERUAKI | NULL | NULL | JAP | 2 | AO2 | THE PULSED HARD X-RAY EMISSION FROM ANOMALOUS X-RAY PULSAR 4U 0142+61 | HXD | Y |
| PSR B1259-63 | 195.6821 | -63.8856 | 304.1741357 | -1.04108664 | 280.935 | 54288.622025463 | 54289.062662037 | 402014010 | 21863.4 | 20000 | 21871.4 | 21863.4 | 0 | 21871.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 26860 | 26860 | 38063.9 | 1 | PROCESSED | 57539.1256481482 | 54696 | 54328.4884722222 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020059 | We propose to monitor the flux and spectral evolutions in both X-rays and TeV gamma-rays of the gamma-ray binary PSR B1259-63 around its periastron passage in July 2007. Combined with planned TeV gamma-ray observations with HESS, Suzaku XIS+HXD measurements of the hard continuum allow us to investigate particle acceleration in a highly variable environment as a result of collisions of the pulsar wind with the Be star wind. We request 12 observations with Suzaku, each with 20 ks, covering from the first disk passage to the second disk passage. Our X-ray and TeV campaign will aid in understanding the physical structure of interacting pulsar winds in a very unique way. | GALACTIC POINT SOURCES | 4 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63 | HXD | Y |
| PSR B1259-63 | 195.6782 | -63.8867 | 304.17237227 | -1.04211039 | 282.6534 | 54290.6852083333 | 54291.1876041667 | 402014020 | 19481.7 | 20000 | 19481.7 | 19481.7 | 0 | 19481.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26911.1 | 26911.1 | 43378 | 1 | PROCESSED | 57539.1396759259 | 54696 | 54328.5032060185 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020059 | We propose to monitor the flux and spectral evolutions in both X-rays and TeV gamma-rays of the gamma-ray binary PSR B1259-63 around its periastron passage in July 2007. Combined with planned TeV gamma-ray observations with HESS, Suzaku XIS+HXD measurements of the hard continuum allow us to investigate particle acceleration in a highly variable environment as a result of collisions of the pulsar wind with the Be star wind. We request 12 observations with Suzaku, each with 20 ks, covering from the first disk passage to the second disk passage. Our X-ray and TeV campaign will aid in understanding the physical structure of interacting pulsar winds in a very unique way. | GALACTIC POINT SOURCES | 4 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63 | HXD | Y |
| PSR B1259-63 | 195.6777 | -63.8873 | 304.1721261 | -1.04270018 | 282.6527 | 54292.6291319444 | 54293.1910763889 | 402014030 | 22721.7 | 20000 | 22721.7 | 22721.7 | 0 | 22721.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 24280.8 | 24280.8 | 48545.9 | 0 | PROCESSED | 57539.1606712963 | 54707 | 54339.0273842593 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020059 | We propose to monitor the flux and spectral evolutions in both X-rays and TeV gamma-rays of the gamma-ray binary PSR B1259-63 around its periastron passage in July 2007. Combined with planned TeV gamma-ray observations with HESS, Suzaku XIS+HXD measurements of the hard continuum allow us to investigate particle acceleration in a highly variable environment as a result of collisions of the pulsar wind with the Be star wind. We request 12 observations with Suzaku, each with 20 ks, covering from the first disk passage to the second disk passage. Our X-ray and TeV campaign will aid in understanding the physical structure of interacting pulsar winds in a very unique way. | GALACTIC POINT SOURCES | 4 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63 | HXD | Y |
| PSR B1259-63 | 195.6732 | -63.8823 | 304.17036556 | -1.03761834 | 285.8945 | 54294.6568865741 | 54295.3459953704 | 402014040 | 22914.9 | 20000 | 22914.9 | 22914.9 | 0 | 22914.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21070.6 | 21070.6 | 59495.9 | 1 | PROCESSED | 57539.2651273148 | 54709 | 54339.4142592593 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020059 | We propose to monitor the flux and spectral evolutions in both X-rays and TeV gamma-rays of the gamma-ray binary PSR B1259-63 around its periastron passage in July 2007. Combined with planned TeV gamma-ray observations with HESS, Suzaku XIS+HXD measurements of the hard continuum allow us to investigate particle acceleration in a highly variable environment as a result of collisions of the pulsar wind with the Be star wind. We request 12 observations with Suzaku, each with 20 ks, covering from the first disk passage to the second disk passage. Our X-ray and TeV campaign will aid in understanding the physical structure of interacting pulsar winds in a very unique way. | GALACTIC POINT SOURCES | 4 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63 | HXD | Y |
| PSR B1259-63 | 195.6556 | -63.8839 | 304.16255435 | -1.03887935 | 293.4832 | 54304.2811226852 | 54304.6877777778 | 402014050 | 19702.3 | 20000 | 19702.3 | 19702.3 | 0 | 19702.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17754.9 | 17754.9 | 35127.9 | 0 | PROCESSED | 57539.3024768518 | 54707 | 54339.2175347222 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020059 | We propose to monitor the flux and spectral evolutions in both X-rays and TeV gamma-rays of the gamma-ray binary PSR B1259-63 around its periastron passage in July 2007. Combined with planned TeV gamma-ray observations with HESS, Suzaku XIS+HXD measurements of the hard continuum allow us to investigate particle acceleration in a highly variable environment as a result of collisions of the pulsar wind with the Be star wind. We request 12 observations with Suzaku, each with 20 ks, covering from the first disk passage to the second disk passage. Our X-ray and TeV campaign will aid in understanding the physical structure of interacting pulsar winds in a very unique way. | GALACTIC POINT SOURCES | 4 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63 | HXD | Y |
| PSR B1259-63 | 195.6402 | -63.8787 | 304.15600524 | -1.03339065 | 289.9992 | 54315.2640856482 | 54316.0419444444 | 402014060 | 24038.8 | 20000 | 24038.8 | 24038.8 | 0 | 24038.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21580.8 | 21580.8 | 67195.9 | 1 | PROCESSED | 57539.3969675926 | 54722 | 54347.6946527778 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020059 | We propose to monitor the flux and spectral evolutions in both X-rays and TeV gamma-rays of the gamma-ray binary PSR B1259-63 around its periastron passage in July 2007. Combined with planned TeV gamma-ray observations with HESS, Suzaku XIS+HXD measurements of the hard continuum allow us to investigate particle acceleration in a highly variable environment as a result of collisions of the pulsar wind with the Be star wind. We request 12 observations with Suzaku, each with 20 ks, covering from the first disk passage to the second disk passage. Our X-ray and TeV campaign will aid in understanding the physical structure of interacting pulsar winds in a very unique way. | GALACTIC POINT SOURCES | 4 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63 | HXD | Y |
| PSR B1259-63 | 195.6594 | -63.8834 | 304.16424752 | -1.0384525 | 292.9998 | 54330.0581481482 | 54330.6877777778 | 402014070 | 20481.2 | 20000 | 20481.2 | 20481.2 | 0 | 20482.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19470.3 | 19470.3 | 54364 | 0 | PROCESSED | 57539.6 | 54724 | 54356.2228472222 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020059 | We propose to monitor the flux and spectral evolutions in both X-rays and TeV gamma-rays of the gamma-ray binary PSR B1259-63 around its periastron passage in July 2007. Combined with planned TeV gamma-ray observations with HESS, Suzaku XIS+HXD measurements of the hard continuum allow us to investigate particle acceleration in a highly variable environment as a result of collisions of the pulsar wind with the Be star wind. We request 12 observations with Suzaku, each with 20 ks, covering from the first disk passage to the second disk passage. Our X-ray and TeV campaign will aid in understanding the physical structure of interacting pulsar winds in a very unique way. | GALACTIC POINT SOURCES | 4 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63 | HXD | Y |
| PSR B1259-63 | 195.6089 | -63.8685 | 304.14267075 | -1.0226082 | 321.9333 | 54348.2308449074 | 54348.6043287037 | 402014080 | 18332.7 | 20000 | 18340.7 | 18348.7 | 0 | 18332.7 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 22351.3 | 22351.3 | 32260 | 0 | PROCESSED | 57539.9271412037 | 54724 | 54356.1999537037 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020059 | We propose to monitor the flux and spectral evolutions in both X-rays and TeV gamma-rays of the gamma-ray binary PSR B1259-63 around its periastron passage in July 2007. Combined with planned TeV gamma-ray observations with HESS, Suzaku XIS+HXD measurements of the hard continuum allow us to investigate particle acceleration in a highly variable environment as a result of collisions of the pulsar wind with the Be star wind. We request 12 observations with Suzaku, each with 20 ks, covering from the first disk passage to the second disk passage. Our X-ray and TeV campaign will aid in understanding the physical structure of interacting pulsar winds in a very unique way. | GALACTIC POINT SOURCES | 4 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | THE 2007 PERIASTRON PASSAGE OF THE GAMMA-RAY BINARY PSR B1259-63 | HXD | Y |
| LS 5039 | 276.5633 | -14.9109 | 16.82651822 | -1.31880921 | 270.412 | 54352.6780555556 | 54358.4725 | 402015010 | 203239.9 | 200000 | 203239.9 | 203239.9 | 0 | 203239.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 181095 | 181095 | 442087.9 | 4 | PROCESSED | 57540.0947685185 | 54745 | 54384.7259027778 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020062 | The periodicity of TeV gamma-rays from the Galactic microquasar LS 5039 has recently been detected by the HESS Cherenkov telescope. We propose to conduct a simultaneous X-ray/VHE gamma-ray observations for a total of 200 ks of the microquasar with Suzaku XIS and HXD in conjuction with the HESS telescope. A full orbital period of 3.9 days is planned to be covered with Suzaku and HESS. The goal of this program is to study a possible correlation of X-TeV fluxes and spectral changes as a function of orbital phase, thereby shedding a new light on the origin of high-energy radiation from the microquasar system. | GALACTIC POINT SOURCES | 4 | A | TAKAHASHI | TADAYUKI | NULL | NULL | JAP | 2 | AO2 | SIMULTANEOUS SUZAKU AND HESS OBSERVATIONS OF THE TEV GAMMA-RAY MICROQUASAR LS 5039 | HXD | Y |
| HETEJ1900.1-2455 | 285.0506 | -24.9802 | 11.25454685 | -12.90928139 | 259.4192 | 54389.5913425926 | 54390.5071064815 | 402016010 | 41759.1 | 40000 | 41778.8 | 41759.1 | 0 | 41775.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39906.3 | 39906.3 | 79105.8 | 1 | PROCESSED | 57540.3158564815 | 54771 | 54403.1292708333 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020068 | We propose a 40 ks observation of the accreting millisecond pulsar HETE J1900.1-2455, which was discovered by HETE-2 only recently. Good sensitivity in 10-100keV and enough timing resolution of HXD on Suzaku allow us to measure the light curve and the phase resolved spectra of its hard X-ray pulsation, with which we study the physical parameters of the Comptonizing plasma that is considered as the source of the hard X-ray emission of accreting millisecond pulsars. With XIS, we study the radiation from the accretion disk and the neutron star surface, and search for spectral features such as emission lines or absorption edges, which will provide information on the binary environment. | GALACTIC POINT SOURCES | 4 | B | SUZUKI | MOTOKO | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY PULSATION OF ACCRETION-DRIVEN MILLISECOND PULSAR HETE J1900.1-2455 | HXD | Y |
| 4U 1700+24 | 256.6316 | 23.9071 | 45.07419011 | 32.98144858 | 280.149 | 54334.7787615741 | 54335.875162037 | 402023010 | 50244.5 | 50000 | 50252.5 | 50260.5 | 0 | 50244.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45326.8 | 45326.8 | 94715.8 | 2 | PROCESSED | 57539.6636226852 | 54723 | 54350.4606481482 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020105 | We propose the observation of Neutron Star Low Mass X-ray Binary (LMXB) system 4U 1700+24.This system would be Advection Dominant Accretion Flow (ADAF) and we research the hard-tail in hard X-ray region. Though the X-ray intensity in a Low Hard state is very faint, $sim$10$^{33}$ erg/s we can obtain the energy spectrum of 10-100keV for the first time using Suzaku 50ksec observation because it is the nearest LMXB. If we know the extension of hard-tail in low luminosity state, we can understand the physical state of electron in the accretion disk and/or compact object. Suzaku is the best satellite to research the faint emission around 100keV. | GALACTIC POINT SOURCES | 4 | B | NAGAE | OSAMU | NULL | NULL | JAP | 2 | AO2 | STUDY OF MASS ACCRETION FLOW IN ADAF FOR LOW LUMINOUS X-RAY BINARY 4U 1700+24 | HXD | Y |
| CYG OB2 ASSOCIATION | 308.2175 | 41.2935 | 80.16491027 | 0.83267098 | 220.3949 | 54452.9185532407 | 54453.843912037 | 402030010 | 41114.7 | 40000 | 41114.7 | 41114.7 | 0 | 41114.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37918.1 | 37918.1 | 79943.9 | 0 | PROCESSED | 57540.9006597222 | 54828 | 54460.6521643518 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020150 | Cygnus OB2 Association (hereafter Cyg OB2) is a candidate of a counterpart of a TeV gamma-ray source; TeV J 2032+4130 discovered by HEGRA. Cyg OB2 is a peculiar cluster of early type stars including extremely high mass stars (>100 solar mass). Some stars in the cluster are bright in an X-ray range, and their spectra show unusually high temperature and also their winds are violently strong. TeV J 2032+4130 lies about 20 f apart from the stars and no obvious X-ray counterpart has been detected in its error circle. We propose to reveal a hidden link between the stars and TeV J2032+4130 by looking for a non-thermal diffuse X-ray emission between them with Suzaku. Also we search for possible non-thermal properties of the stars in high quality spectra obtained with Suzaku. | GALACTIC POINT SOURCES | 4 | C | KITAMOTO | SHUNJI | NULL | NULL | JAP | 2 | AO2 | STUDY OF THE RELATION BETWEEN CYGNUS OB2 ASSOCIATION AND TEV J 2032+4130 | XIS | Y |
| TEVJ2032+4130 | 308.0461 | 41.5016 | 80.25613164 | 1.05964615 | 221.0839 | 54451.984212963 | 54452.9176157407 | 402031010 | 40043.9 | 40000 | 40043.9 | 40043.9 | 0 | 40043.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37309.1 | 37309.1 | 80641.9 | 1 | PROCESSED | 57540.8865625 | 54828 | 54460.6569675926 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020150 | Cygnus OB2 Association (hereafter Cyg OB2) is a candidate of a counterpart of a TeV gamma-ray source; TeV J 2032+4130 discovered by HEGRA. Cyg OB2 is a peculiar cluster of early type stars including extremely high mass stars (>100 solar mass). Some stars in the cluster are bright in an X-ray range, and their spectra show unusually high temperature and also their winds are violently strong. TeV J 2032+4130 lies about 20 f apart from the stars and no obvious X-ray counterpart has been detected in its error circle. We propose to reveal a hidden link between the stars and TeV J2032+4130 by looking for a non-thermal diffuse X-ray emission between them with Suzaku. Also we search for possible non-thermal properties of the stars in high quality spectra obtained with Suzaku. | GALACTIC POINT SOURCES | 4 | C | KITAMOTO | SHUNJI | NULL | NULL | JAP | 2 | AO2 | STUDY OF THE RELATION BETWEEN CYGNUS OB2 ASSOCIATION AND TEV J 2032+4130 | XIS | Y |
| EV LAC | 341.7127 | 44.3232 | 100.60502245 | -13.08073089 | 256.1601 | 54432.9692013889 | 54434.4655208333 | 402032010 | 68949.3 | 100000 | 68949.3 | 69133.3 | 0 | 69127.5 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 65011.3 | 65011.3 | 129232.8 | 2 | PROCESSED | 57540.7939236111 | 54808 | 54441.0876851852 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021013 | We propose a 100 ks Suzaku XIS observation of the dMe flare star EV Lac to measure coronal element abundances during quiescence and flares of different sizes. EV Lac undergoes frequent small flares, and is known to have undergone a very large flare at ~300 times the quiescent count rate in 2000. Coronal abundance changes shed light on the process of chromospheric evaporation under conditions different to those on the Sun. Depending on the size and spectrum of the flare, we may also be able to detect a hard burst of emission that would serve as a time marker for particle acceleration during the flare. | GALACTIC POINT SOURCES | 4 | C | HWANG | UNA | NULL | NULL | USA | 2 | AO2 | FLARE AND QUIESENT CONORAL ELEMENT ABUNDANCES IN EV LAC | XIS | Y |
| SIGMA GEM | 115.843 | 28.9438 | 191.13214337 | 23.30670736 | 104.4403 | 54394.4090162037 | 54397.9690162037 | 402033010 | 142889.7 | 125000 | 142889.7 | 142993.6 | 0 | 142985.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 124447.1 | 124447.1 | 307541.6 | 1 | PROCESSED | 57540.4020138889 | 54776 | 54407.830474537 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021014 | Suzaku is a powerful instrument for studying the hot (>100 MK) coronal quiescent and flare emission on RS CVn binaries. We propose a 125 ksec (3-4 day elapsed time) observation of the RS CVn binary Sigma Gem. Our goals are i) to better characterize its hard (>10 keV) emission, ii) to understand the origin of coronal thermal and nonthermal plasma by studying the evolution of the coronal thermal structure, iii) to investigate the persistent and flaring nonthermal electron population using a combination of X-ray and radio cm+mm continuum data, and iv) compare long duration flares on Sigma Gem with the 6 hour flares of Sigma2 CrB. Such studies require the long duty cycle of Suzaku observations and its high sensitivity, particularly the greatly enhanced capability at 10-25 keV provided by HXD. | GALACTIC POINT SOURCES | 4 | C | BROWN | ALEXANDER | NULL | NULL | USA | 2 | AO2 | SUZAKU OBSERVATIONS OF THERMAL AND NONTHERMAL CORONAL STRUCTURE ON THE RS CVN BINARY SIGMA GEM (K0III +?) | HXD | Y |
| HD432 | 2.3072 | 59.1394 | 117.5327944 | -3.28915956 | 247.7181 | 54469.7038310185 | 54470.5154513889 | 402034010 | 38240.6 | 40000 | 38248.6 | 38240.6 | 0 | 38248.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35050.3 | 35050.3 | 70120 | 1 | PROCESSED | 57540.9911574074 | 54908 | 54483.4635532407 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021016 | Suzaku XIS spectra of three "X-ray deficient" Hertzsprung gap giants will explore why they display anomalous coronal behavior compared with cooler giants only slightly further advanced in their evolution. The apparent sharp transition in coronal properties on the way to helium flash might be caused by disruption of a "fossil" magnetosphere by a newly born solar-like dynamo. A key discriminator is the coronal energy distribution, especially enhanced and sporadic hard emission associated with flaring. The proposed targets are the brightest not previously observed in X-rays at CCD resolution; all three have supporting high resolution UV spectra. Expanding the sample of high quality, high energy information on this key class of objects is essential for probing their odd behavior. | GALACTIC POINT SOURCES | 4 | C | AYRES | THOMAS | NULL | NULL | USA | 2 | AO2 | ANOMALOUS CORONAE OF HERTZSPRUNG GAP GIANTS | XIS | Y |
| HD432 | 2.3079 | 59.1397 | 117.53319828 | -3.2889222 | 246.0535 | 54471.6956944444 | 54472.297349537 | 402034020 | 26984.4 | 27000 | 26984.4 | 26984.4 | 0 | 26984.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 24601 | 24601 | 51975.9 | 0 | PROCESSED | 57541.2823958333 | 54871 | 54483.3863773148 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021016 | Suzaku XIS spectra of three "X-ray deficient" Hertzsprung gap giants will explore why they display anomalous coronal behavior compared with cooler giants only slightly further advanced in their evolution. The apparent sharp transition in coronal properties on the way to helium flash might be caused by disruption of a "fossil" magnetosphere by a newly born solar-like dynamo. A key discriminator is the coronal energy distribution, especially enhanced and sporadic hard emission associated with flaring. The proposed targets are the brightest not previously observed in X-rays at CCD resolution; all three have supporting high resolution UV spectra. Expanding the sample of high quality, high energy information on this key class of objects is essential for probing their odd behavior. | GALACTIC POINT SOURCES | 4 | C | AYRES | THOMAS | NULL | NULL | USA | 2 | AO2 | ANOMALOUS CORONAE OF HERTZSPRUNG GAP GIANTS | XIS | Y |
| ZETA OPH | 249.2878 | -10.5628 | 6.28378927 | 23.59180747 | 94.9452 | 54540.8758912037 | 54543.8543287037 | 402038010 | 105583.7 | 100000 | 105591.7 | 105591.7 | 0 | 105583.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 79981.3 | 79981.3 | 257317.8 | 2 | PROCESSED | 57541.9592708333 | 54922 | 54553.3785300926 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021022 | Zeta Oph is a well known optical and UV variable star and is now known to displays both short (hours) and long (years) term X-ray variability. The short term variability has different periods for the soft and hard X-ray bands. The soft period being identical with the UV DAC reoccurrence period. The hard period is 40 percent smaller than the soft period and the source of it's variability is thus far unclear. Zeta Oph has been observed by several X-ray telescopes over a 22 year time span and the observations show significant variations in the total observed X-ray flux. We are requesting an XIS observation of this star to develop: 1) a greater understanding of the hard X-ray emission; 2) confirm the hard and soft periodicities, and; 3) provide further monitoring of the long term variability. | GALACTIC POINT SOURCES | 4 | C | WALDRON | WAYNE | NULL | NULL | USA | 2 | AO2 | MULTIPLE X-RAY EMISSION PERIODICITY IN THE RAPIDLY ROTATING O-STAR, ZETA OPH | XIS | Y |
| ETA CARINAE | 161.2181 | -59.7282 | 287.59637986 | -0.67920855 | 289.0006 | 54274.2459259259 | 54275.9015509259 | 402039010 | 58396.1 | 50000 | 58404.1 | 58396.1 | 0 | 58404.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51552 | 51552 | 143009.9 | 1 | PROCESSED | 57539.0368981482 | 54695 | 54322.5140856482 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021026 | XMM-Newton observations in 2003 suggest that X-ray emission from Eta Carinae has a hard X-ray component above 10 keV in addition to the thermal emission with kT ~3-5 keV. The excess is apparently strongest near the 2-10 keV X-ray maximum, and possibly produced by very hot plasma or 1st-order Fermi acceleration of particles which then inverse Compton-upscatter UV seed photons from the stellar photospheres. We propose a 50 ksec observation of Eta Carinae with the Suzaku telescope during AO2, compare the X-ray spectrum with earlier observations and determine the level of emission at E >9 keV. | GALACTIC POINT SOURCES | 4 | B | HAMAGUCHI | KENJI | NULL | NULL | USA | 2 | AO2 | HARD X-RAY EMISSION FROM ETA CARINAE | HXD | Y |
| RT CRU | 188.7055 | -64.6161 | 301.15157727 | -1.80180428 | 281.609 | 54283.5270023148 | 54284.2433333333 | 402040010 | 50880.6 | 50000 | 50880.6 | 50880.6 | 0 | 50880.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42850.6 | 42850.6 | 61887.9 | 0 | PROCESSED | 57539.0744328704 | 54695 | 54328.4668055556 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021102 | Symbiotic stars are interacting binaries in which a white dwarf (WD) accretes from the wind of a red giant. Their X-ray emission is typically very soft. Recently, however, 4 symbiotics have been detected out to almost 100 keV. Suzaku observations of two of these sources revealed that the hard X-rays emanated from an extremely hot thermal plasma. One means of producing such hot gas is accretion onto a near Chandrasekhar-mass WD. We propose to use the unique capabilities of Suzaku to test this hypothesis. We will use broad-band X-ray spectral fitting to determine the temperature of the hot plasma, hard X-ray timing studies to search for or constrain rapid variations due to either magnetic or non-magnetic accretion, and Fe line diagnostics to investigate the role of scattering. | GALACTIC POINT SOURCES | 4 | B | SOKOLOSKI | JENNIFER | NULL | NULL | USA | 2 | AO2 | ARE HARD X-RAY SYMBIOTICS PROGENITORS OF TYPE IA SUPERNOVAE? | HXD | Y |
| VY AQR | 318.0426 | -8.8307 | 41.59091784 | -35.22055705 | 252.6652 | 54414.6528587963 | 54415.3855787037 | 402043010 | 25447.3 | 20000 | 25447.3 | 25447.3 | 0 | 25447.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22360.5 | 22360.5 | 63299.9 | 2 | PROCESSED | 57540.476712963 | 54790 | 54423.1702314815 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021105 | Dwarf Novae, the most numerous subclass of cataclysmic variables, are important contributors to the unresolved X-ray emissions from the Galactic disk and the bulge. However, current estimates of the integrated X-ray luminosity of dwarf novae are highly uncertain and are based on samples that may contain significant biases. We need to obtain an unbiased X-ray luminosity function of dwarf novae to estimate the true contribution of dwarf novae to the unresolved Galactic X-ray emission. Here we propose short Suzaku observations of dwarf novae with secure, parallax-based distance estimates that have not been the subject of pointed, imaging, X-ray observations in the 0.5-10 keV band. This will be an important check of potential biases in earlier studies. | GALACTIC POINT SOURCES | 4 | C | MUKAI | KOJI | NULL | NULL | USA | 2 | AO2 | BUILDING UP AN UNBIASED X-RAY LUMINOSITY FUNCTION OF DWARF NOVAE: A PARALLAX SELECTED SAMPLE | XIS | Y |
| SW UMA | 129.1769 | 53.4845 | 164.80593722 | 36.96002764 | 98.2716 | 54410.2367708333 | 54410.6252199074 | 402044010 | 16899.1 | 20000 | 16907.1 | 16899.1 | 0 | 16907.1 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13896.9 | 13896.9 | 33551.9 | 1 | PROCESSED | 57540.4388194444 | 54784 | 54417.2697569444 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021105 | Dwarf Novae, the most numerous subclass of cataclysmic variables, are important contributors to the unresolved X-ray emissions from the Galactic disk and the bulge. However, current estimates of the integrated X-ray luminosity of dwarf novae are highly uncertain and are based on samples that may contain significant biases. We need to obtain an unbiased X-ray luminosity function of dwarf novae to estimate the true contribution of dwarf novae to the unresolved Galactic X-ray emission. Here we propose short Suzaku observations of dwarf novae with secure, parallax-based distance estimates that have not been the subject of pointed, imaging, X-ray observations in the 0.5-10 keV band. This will be an important check of potential biases in earlier studies. | GALACTIC POINT SOURCES | 4 | C | MUKAI | KOJI | NULL | NULL | USA | 2 | AO2 | BUILDING UP AN UNBIASED X-RAY LUMINOSITY FUNCTION OF DWARF NOVAE: A PARALLAX SELECTED SAMPLE | XIS | Y |
| SS AUR | 93.3423 | 47.7333 | 166.0127795 | 13.79596984 | 289.1089 | 54529.7508796296 | 54530.180775463 | 402045010 | 19471.4 | 20000 | 19471.4 | 19471.4 | 0 | 19471.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17378 | 17378 | 37135.9 | 0 | PROCESSED | 57541.7699074074 | 54905 | 54539.2223726852 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021105 | Dwarf Novae, the most numerous subclass of cataclysmic variables, are important contributors to the unresolved X-ray emissions from the Galactic disk and the bulge. However, current estimates of the integrated X-ray luminosity of dwarf novae are highly uncertain and are based on samples that may contain significant biases. We need to obtain an unbiased X-ray luminosity function of dwarf novae to estimate the true contribution of dwarf novae to the unresolved Galactic X-ray emission. Here we propose short Suzaku observations of dwarf novae with secure, parallax-based distance estimates that have not been the subject of pointed, imaging, X-ray observations in the 0.5-10 keV band. This will be an important check of potential biases in earlier studies. | GALACTIC POINT SOURCES | 4 | C | MUKAI | KOJI | NULL | NULL | USA | 2 | AO2 | BUILDING UP AN UNBIASED X-RAY LUMINOSITY FUNCTION OF DWARF NOVAE: A PARALLAX SELECTED SAMPLE | XIS | Y |
| BZ UMA | 133.4243 | 57.801 | 159.01672768 | 38.83001001 | 307.4767 | 54549.9926388889 | 54550.4446064815 | 402046010 | 29746.6 | 20000 | 29754.6 | 29754.6 | 0 | 29746.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 24921.2 | 24921.2 | 39045.9 | 0 | PROCESSED | 57541.9622106482 | 54933 | 54566.2225231482 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021105 | Dwarf Novae, the most numerous subclass of cataclysmic variables, are important contributors to the unresolved X-ray emissions from the Galactic disk and the bulge. However, current estimates of the integrated X-ray luminosity of dwarf novae are highly uncertain and are based on samples that may contain significant biases. We need to obtain an unbiased X-ray luminosity function of dwarf novae to estimate the true contribution of dwarf novae to the unresolved Galactic X-ray emission. Here we propose short Suzaku observations of dwarf novae with secure, parallax-based distance estimates that have not been the subject of pointed, imaging, X-ray observations in the 0.5-10 keV band. This will be an important check of potential biases in earlier studies. | GALACTIC POINT SOURCES | 4 | C | MUKAI | KOJI | NULL | NULL | USA | 2 | AO2 | BUILDING UP AN UNBIASED X-RAY LUMINOSITY FUNCTION OF DWARF NOVAE: A PARALLAX SELECTED SAMPLE | XIS | Y |
| GX17+2 | 274.0087 | -14.1006 | 16.37694194 | 1.24456043 | 269.7113 | 54362.2773032407 | 54362.8543402778 | 402050010 | 19095.9 | 20000 | 19095.9 | 19104.4 | 0 | 19095.9 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 16044.5 | 16044.5 | 49849.9 | 0 | PROCESSED | 57540.0136458333 | 54751 | 54384.4487037037 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021111 | Z sources are bright low-mass X-ray binaries with variable spectra that describe a characteristic "Z" shape in an X-ray color-color plot. The forces driving the spectral shape and variability of the Z sources are not well understood, as there are few detectors with the necessary capabilities. GX17+2 is a Sco-type Z sources with an unusual time-varying hard X-ray tail whose origin is uncertain. Bright X-ray sources also illuminate the interstellar medium. Highly absorbed X-ray sources show halos due to dust scattering as well as absorption features. These will allow us to place constraints on interstellar dust and gas models. Suzaku can address all of these issues with simultaneous observations of the hard X-ray continuum and the dust-scattered X-ray halo. | GALACTIC POINT SOURCES | 4 | A | SMITH | RANDALL | NULL | NULL | USA | 2 | AO2 | OBSERVING THE SPECTRUM AND HALO OF GX17+2 | HXD | Y |
| GX17+2 | 274.0098 | -14.0991 | 16.37876929 | 1.24433559 | 268.3778 | 54370.5988078704 | 54371.2502199074 | 402050020 | 23011.7 | 20000 | 23019.7 | 23025.8 | 0 | 23011.7 | 3 | 2 | 0 | 3 | 1 | 0 | 0 | 19048.8 | 19048.8 | 56276 | 0 | PROCESSED | 57540.1139351852 | 54769 | 54402.3511921296 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021111 | Z sources are bright low-mass X-ray binaries with variable spectra that describe a characteristic "Z" shape in an X-ray color-color plot. The forces driving the spectral shape and variability of the Z sources are not well understood, as there are few detectors with the necessary capabilities. GX17+2 is a Sco-type Z sources with an unusual time-varying hard X-ray tail whose origin is uncertain. Bright X-ray sources also illuminate the interstellar medium. Highly absorbed X-ray sources show halos due to dust scattering as well as absorption features. These will allow us to place constraints on interstellar dust and gas models. Suzaku can address all of these issues with simultaneous observations of the hard X-ray continuum and the dust-scattered X-ray halo. | GALACTIC POINT SOURCES | 4 | A | SMITH | RANDALL | NULL | NULL | USA | 2 | AO2 | OBSERVING THE SPECTRUM AND HALO OF GX17+2 | HXD | Y |
| 4U1705-44 | 257.2319 | -44.0961 | 343.32770356 | -2.34122442 | 265.637 | 54348.6112847222 | 54349.0140509259 | 402051010 | 13343.6 | 15000 | 13343.6 | 13343.6 | 0 | 13343.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9370.6 | 9370.6 | 34791.9 | 1 | PROCESSED | 57539.9453472222 | 54773 | 54356.2627430556 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021113 | We recently proposed a solution to the problem of model ambiguity for the spectra of atoll-type neutron stars. This work was performed on X-ray transient, and we need to test the model on the main population of persistent atolls. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. We propose to supplement the Suzaku monitoring archive begun in AO-1 by targeting the two persistent atolls with the greatest X-ray variability. | GALACTIC POINT SOURCES | 4 | A | REMILLARD | RONALD | NULL | NULL | USA | 2 | AO2 | X-RAY SPECTRA OF ATOLL-TYPE NEUTRON STARS | XIS | Y |
| 4U1705-44 | 257.2347 | -44.0965 | 343.32858118 | -2.34307771 | 294.8341 | 54381.763275463 | 54382.2015509259 | 402051020 | 21971.3 | 15000 | 21979.3 | 21981 | 0 | 21971.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15688 | 15688 | 37856 | 1 | PROCESSED | 57540.198125 | 54770 | 54402.6586226852 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021113 | We recently proposed a solution to the problem of model ambiguity for the spectra of atoll-type neutron stars. This work was performed on X-ray transient, and we need to test the model on the main population of persistent atolls. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. We propose to supplement the Suzaku monitoring archive begun in AO-1 by targeting the two persistent atolls with the greatest X-ray variability. | GALACTIC POINT SOURCES | 4 | A | REMILLARD | RONALD | NULL | NULL | USA | 2 | AO2 | X-RAY SPECTRA OF ATOLL-TYPE NEUTRON STARS | XIS | Y |
| 4U1705-44 | 257.2244 | -44.1021 | 343.31966899 | -2.34047423 | 86.9924 | 54516.9847569444 | 54517.6182175926 | 402051030 | 25995.6 | 15000 | 26051.6 | 25995.6 | 0 | 26051.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20820.5 | 20820.5 | 54723.9 | 1 | PROCESSED | 57541.7148611111 | 54901 | 54535.2030439815 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021113 | We recently proposed a solution to the problem of model ambiguity for the spectra of atoll-type neutron stars. This work was performed on X-ray transient, and we need to test the model on the main population of persistent atolls. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. We propose to supplement the Suzaku monitoring archive begun in AO-1 by targeting the two persistent atolls with the greatest X-ray variability. | GALACTIC POINT SOURCES | 4 | A | REMILLARD | RONALD | NULL | NULL | USA | 2 | AO2 | X-RAY SPECTRA OF ATOLL-TYPE NEUTRON STARS | XIS | Y |
| 4U1705-44 | 257.2229 | -44.1035 | 343.31790137 | -2.34044351 | 107.4157 | 54543.8610532407 | 54544.5210532407 | 402051040 | 20074.4 | 15000 | 20074.4 | 20074.4 | 0 | 20082.4 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 13411.3 | 13411.3 | 57017.9 | 1 | PROCESSED | 57541.899525463 | 54922 | 54553.1912268518 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021113 | We recently proposed a solution to the problem of model ambiguity for the spectra of atoll-type neutron stars. This work was performed on X-ray transient, and we need to test the model on the main population of persistent atolls. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. We propose to supplement the Suzaku monitoring archive begun in AO-1 by targeting the two persistent atolls with the greatest X-ray variability. | GALACTIC POINT SOURCES | 4 | A | REMILLARD | RONALD | NULL | NULL | USA | 2 | AO2 | X-RAY SPECTRA OF ATOLL-TYPE NEUTRON STARS | XIS | Y |
| AQL X-1 | 287.816 | 0.5784 | 35.71219982 | -4.14539755 | 284.0925 | 54371.6493402778 | 54372.062662037 | 402053010 | 13825.2 | 15000 | 13825.2 | 13825.2 | 0 | 13825.2 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 13745 | 13745 | 35704 | 0 | PROCESSED | 57540.1327199074 | 54769 | 54402.3541550926 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021114 | We recently proposed a solution to the problem of model ambiguity for the X-ray spectra of atoll-type neutron stars. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. This proposal requests a TOO program for monitoring observations of one of the two atoll-type transients that were used to develop our spectral model with RXTE data. | GALACTIC POINT SOURCES | 4 | A | REMILLARD | RONALD | NULL | NULL | USA | 2 | AO2-TOO | X-RAY SPECTRA OF NEUTRON-STAR X-RAY TRANSIENTS | XIS | Y |
| AQL X-1 | 287.8179 | 0.5789 | 35.71351779 | -4.14685757 | 277.9777 | 54376.9927777778 | 54377.3516087963 | 402053020 | 15132.6 | 15000 | 15140.6 | 15142.3 | 0 | 15132.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11890.8 | 11890.8 | 30999.9 | 1 | PROCESSED | 57540.1490277778 | 54771 | 54403.9157175926 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021114 | We recently proposed a solution to the problem of model ambiguity for the X-ray spectra of atoll-type neutron stars. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. This proposal requests a TOO program for monitoring observations of one of the two atoll-type transients that were used to develop our spectral model with RXTE data. | GALACTIC POINT SOURCES | 4 | A | REMILLARD | RONALD | NULL | NULL | USA | 2 | AO2-TOO | X-RAY SPECTRA OF NEUTRON-STAR X-RAY TRANSIENTS | XIS | Y |
| AQL X-1 | 287.8182 | 0.5791 | 35.71383379 | -4.14703266 | 264.9589 | 54382.2112384259 | 54382.6877893518 | 402053030 | 19711.7 | 15000 | 19719.7 | 19727.7 | 0 | 19711.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17552.2 | 17552.2 | 41162 | 0 | PROCESSED | 57540.2157291667 | 54770 | 54402.5719328704 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021114 | We recently proposed a solution to the problem of model ambiguity for the X-ray spectra of atoll-type neutron stars. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. This proposal requests a TOO program for monitoring observations of one of the two atoll-type transients that were used to develop our spectral model with RXTE data. | GALACTIC POINT SOURCES | 4 | A | REMILLARD | RONALD | NULL | NULL | USA | 2 | AO2-TOO | X-RAY SPECTRA OF NEUTRON-STAR X-RAY TRANSIENTS | XIS | Y |
| AQL X-1 | 287.8171 | 0.5794 | 35.71359616 | -4.14591745 | 272.6027 | 54388.3395833333 | 54388.7225 | 402053040 | 17915.7 | 15000 | 17915.7 | 17915.7 | 0 | 17915.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17668.2 | 17668.2 | 33080 | 0 | PROCESSED | 57540.2752893518 | 54769 | 54402.4060648148 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021114 | We recently proposed a solution to the problem of model ambiguity for the X-ray spectra of atoll-type neutron stars. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. This proposal requests a TOO program for monitoring observations of one of the two atoll-type transients that were used to develop our spectral model with RXTE data. | GALACTIC POINT SOURCES | 4 | A | REMILLARD | RONALD | NULL | NULL | USA | 2 | AO2-TOO | X-RAY SPECTRA OF NEUTRON-STAR X-RAY TRANSIENTS | XIS | Y |
| AQL X-1 | 287.8181 | 0.5776 | 35.7124509 | -4.14763067 | 265.5384 | 54392.3838310185 | 54392.7918287037 | 402053050 | 17889.9 | 15000 | 17889.9 | 17889.9 | 0 | 17889.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16927.8 | 16927.8 | 35231.9 | 1 | PROCESSED | 57540.3079513889 | 54769 | 54402.4178935185 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021114 | We recently proposed a solution to the problem of model ambiguity for the X-ray spectra of atoll-type neutron stars. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. This proposal requests a TOO program for monitoring observations of one of the two atoll-type transients that were used to develop our spectral model with RXTE data. | GALACTIC POINT SOURCES | 4 | A | REMILLARD | RONALD | NULL | NULL | USA | 2 | AO2-TOO | X-RAY SPECTRA OF NEUTRON-STAR X-RAY TRANSIENTS | XIS | Y |
| AQL X-1 | 287.8172 | 0.5775 | 35.71194856 | -4.14687642 | 265.833 | 54397.9824074074 | 54398.5072222222 | 402053060 | 21364.8 | 15000 | 21460.8 | 21460.8 | 0 | 21364.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21402.2 | 21402.2 | 45343.9 | 0 | PROCESSED | 57540.3340509259 | 54776 | 54407.3747222222 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021114 | We recently proposed a solution to the problem of model ambiguity for the X-ray spectra of atoll-type neutron stars. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. This proposal requests a TOO program for monitoring observations of one of the two atoll-type transients that were used to develop our spectral model with RXTE data. | GALACTIC POINT SOURCES | 4 | A | REMILLARD | RONALD | NULL | NULL | USA | 2 | AO2-TOO | X-RAY SPECTRA OF NEUTRON-STAR X-RAY TRANSIENTS | XIS | Y |
| AQL X-1 | 287.8217 | 0.5796 | 35.71588636 | -4.14991498 | 243.6715 | 54403.2743171296 | 54403.66 | 402053070 | 17536.2 | 15000 | 17584.2 | 17604 | 0 | 17536.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 14332.2 | 14332.2 | 33319.9 | 0 | PROCESSED | 57540.3767824074 | 54776 | 54409.1320138889 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021114 | We recently proposed a solution to the problem of model ambiguity for the X-ray spectra of atoll-type neutron stars. Our preferred model involves a resurrection of the double-thermal model for the soft state. The results have ramifications for such issues as neutron star ISCOs, the structure of the accretion boundary layer, and the radiative efficiency of the hard state (jets). Suzaku instruments can test and refine the model directly, with a focus on spectral fits rather than a reliance on model performance arguments. This proposal requests a TOO program for monitoring observations of one of the two atoll-type transients that were used to develop our spectral model with RXTE data. | GALACTIC POINT SOURCES | 4 | A | REMILLARD | RONALD | NULL | NULL | USA | 2 | AO2-TOO | X-RAY SPECTRA OF NEUTRON-STAR X-RAY TRANSIENTS | XIS | Y |
| 2S 0921-630 | 140.6632 | -63.3 | 281.84517925 | -9.33739383 | 20.5636 | 54340.7614351852 | 54341.8335532407 | 402057010 | 43213.1 | 40000 | 43213.1 | 43221.1 | 0 | 43221.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15856.8 | 15856.8 | 92615.8 | 0 | PROCESSED | 57539.9304976852 | 54721 | 54353.4365625 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021118 | 2S 0921-630 is a bright, long-period LMXB that is thought to contain an accretion disk corona. Observations with both the Chandra HETGS and XMM-Newton spectrometers revealed line emission from a photoionized plasma. The spectral features are consistent with the predictions for emission from an accretion disk corona. However, with the present data it is impossible to determine whether the emission originates in the corona or in a localized region of the disk. We propose to observer 2S 0921-630 with Suzaku at four orbital phases in order to localize and identify the emitting plasma. The simultaneous HXD coverage will also allow us to constrain the underlying continuum and allow more sensitive study of the high energy region of the spectrum. | GALACTIC POINT SOURCES | 4 | A | COTTAM | JEAN | NULL | NULL | USA | 2 | AO2 | PHASE-RESOLVED SPECTROSCOPY OF 2S 0921-630 | XIS | Y |
| 2S 0921-630 | 140.6643 | -63.2995 | 281.84516955 | -9.33669084 | 18.1705 | 54342.4079166667 | 54343.5134722222 | 402058010 | 45693.7 | 40000 | 45693.7 | 45693.7 | 0 | 45693.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43346.3 | 43346.3 | 95499.8 | 2 | PROCESSED | 57539.9018981482 | 54724 | 54356.2760763889 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021118 | 2S 0921-630 is a bright, long-period LMXB that is thought to contain an accretion disk corona. Observations with both the Chandra HETGS and XMM-Newton spectrometers revealed line emission from a photoionized plasma. The spectral features are consistent with the predictions for emission from an accretion disk corona. However, with the present data it is impossible to determine whether the emission originates in the corona or in a localized region of the disk. We propose to observer 2S 0921-630 with Suzaku at four orbital phases in order to localize and identify the emitting plasma. The simultaneous HXD coverage will also allow us to constrain the underlying continuum and allow more sensitive study of the high energy region of the spectrum. | GALACTIC POINT SOURCES | 4 | A | COTTAM | JEAN | NULL | NULL | USA | 2 | AO2 | PHASE-RESOLVED SPECTROSCOPY OF 2S 0921-630 | XIS | Y |
| 2S 0921-630 | 140.6655 | -63.298 | 281.84446964 | -9.33525426 | 8.3442 | 54335.887025463 | 54336.9932175926 | 402059010 | 43131 | 40000 | 43131 | 43131 | 0 | 43131 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37162.2 | 37162.2 | 95559.8 | 0 | PROCESSED | 57539.6661805556 | 54721 | 54350.5504861111 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021118 | 2S 0921-630 is a bright, long-period LMXB that is thought to contain an accretion disk corona. Observations with both the Chandra HETGS and XMM-Newton spectrometers revealed line emission from a photoionized plasma. The spectral features are consistent with the predictions for emission from an accretion disk corona. However, with the present data it is impossible to determine whether the emission originates in the corona or in a localized region of the disk. We propose to observer 2S 0921-630 with Suzaku at four orbital phases in order to localize and identify the emitting plasma. The simultaneous HXD coverage will also allow us to constrain the underlying continuum and allow more sensitive study of the high energy region of the spectrum. | GALACTIC POINT SOURCES | 4 | A | COTTAM | JEAN | NULL | NULL | USA | 2 | AO2 | PHASE-RESOLVED SPECTROSCOPY OF 2S 0921-630 | XIS | Y |
| 2S 0921-630 | 140.666 | -63.2982 | 281.84477381 | -9.33523447 | 8.344 | 54338.0511226852 | 54339.16 | 402060010 | 40342.3 | 40000 | 40350.3 | 40342.3 | 0 | 40350.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 35646.4 | 35646.4 | 95799.9 | 2 | PROCESSED | 57539.6728703704 | 54721 | 54350.5629398148 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021118 | 2S 0921-630 is a bright, long-period LMXB that is thought to contain an accretion disk corona. Observations with both the Chandra HETGS and XMM-Newton spectrometers revealed line emission from a photoionized plasma. The spectral features are consistent with the predictions for emission from an accretion disk corona. However, with the present data it is impossible to determine whether the emission originates in the corona or in a localized region of the disk. We propose to observer 2S 0921-630 with Suzaku at four orbital phases in order to localize and identify the emitting plasma. The simultaneous HXD coverage will also allow us to constrain the underlying continuum and allow more sensitive study of the high energy region of the spectrum. | GALACTIC POINT SOURCES | 4 | A | COTTAM | JEAN | NULL | NULL | USA | 2 | AO2 | PHASE-RESOLVED SPECTROSCOPY OF 2S 0921-630 | XIS | Y |
| IGR J17544-2619 | 268.6038 | -26.3314 | 3.23518966 | -0.33446224 | 84.5765 | 54544.5263425926 | 54547.2640509259 | 402061010 | 103417.3 | 72000 | 103811.5 | 103827.5 | 0 | 103417.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 65565.6 | 65565.6 | 236505.9 | 3 | PROCESSED | 57541.9752314815 | 54933 | 54566.6106134259 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021121 | Supergiant Fast X-ray Transients are a newly-discovered class of x-ray binary with short outbursts and late O to early B supergiant companions. They are not persistently bright, but the nature of their low-level variability is not well known. Similarly short outbursts are also seen in bright HMXBs with supergiant companions such as Cyg X-1 and Vel X-1. The mechanism of these outbursts is unknown in all cases. We propose long pointings to the two best-studied SFXTs and a third object, XTE J1743-363, which seems to be transitional between SFXTs and persistent supergiant HMXBs. We will characterize their variability at low flux levels, both to understand the accretion mechanism and to enable surveys of archival data for new SFXTs. | GALACTIC POINT SOURCES | 4 | C | SMITH | DAVID | NULL | NULL | USA | 2 | AO2 | CHARACTERIZING THE SPECTRUM AND VARIABILITY OF THE SUPERGIANT FAST X-RAY TRANSIENTS | XIS | Y |
| IGR J00370+6122 | 9.2836 | 61.3722 | 121.21895683 | -1.4519667 | 87.6081 | 54273.499849537 | 54274.230775463 | 402064010 | 34908.9 | 30000 | 35384.4 | 35400.4 | 0 | 34908.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 33792.6 | 33792.6 | 63141.9 | 2 | PROCESSED | 57637.5249652778 | 54695 | 54322.4714236111 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021122 | We propose to observe 3 INTEGRAL-discovered High Mass X-ray Binaries (IGR HMXBs) to search for X-ray pulsations and to study their broadband spectra. Over the past few years, INTEGRAL has found a surprising number of HMXBs, and the large number of new, locally absorbed supergiant HMXBs indicate that these wind-accretors are more common than previously thought. In addition to high column densities, some of these systems have other extreme properties such as slowly rotating neutron stars (NSs) or rapid X-ray flares. For the systems we propose to observe, detection of pulsations is important for establishing the presence of a NS and for constraining the spin period distribution for HMXB NSs. As these are strong hard X-ray emitters, we will take advantage of Suzaku's broadband capabilities. | GALACTIC POINT SOURCES | 4 | B | TOMSICK | JOHN | NULL | NULL | USA | 2 | AO2 | LOOKING FOR SIGNATURES OF HIGH MAGNETIC FIELD NEUTRON STARS IN INTEGRAL HMXBS | XIS | Y |
| IGR J16207-5129 | 245.1895 | -51.5038 | 332.45599844 | -1.05021687 | 88.1855 | 54499.8231365741 | 54500.7841898148 | 402065010 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1 | 0 | 0 | 49595.5 | 49595.5 | 83031.9 | 1 | PROCESSED | 57541.498587963 | 54883 | 54515.6347800926 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021122 | We propose to observe 3 INTEGRAL-discovered High Mass X-ray Binaries (IGR HMXBs) to search for X-ray pulsations and to study their broadband spectra. Over the past few years, INTEGRAL has found a surprising number of HMXBs, and the large number of new, locally absorbed supergiant HMXBs indicate that these wind-accretors are more common than previously thought. In addition to high column densities, some of these systems have other extreme properties such as slowly rotating neutron stars (NSs) or rapid X-ray flares. For the systems we propose to observe, detection of pulsations is important for establishing the presence of a NS and for constraining the spin period distribution for HMXB NSs. As these are strong hard X-ray emitters, we will take advantage of Suzaku's broadband capabilities. | GALACTIC POINT SOURCES | 4 | B | TOMSICK | JOHN | NULL | NULL | USA | 2 | AO2 | LOOKING FOR SIGNATURES OF HIGH MAGNETIC FIELD NEUTRON STARS IN INTEGRAL HMXBS | XIS | Y |
| IGR J16207-5129 | 245.1891 | -51.5041 | 332.45561032 | -1.05025433 | 89.5006 | 54526.8661111111 | 54527.7502199074 | 402065020 | 32612.7 | 30000 | 32709.5 | 32713.3 | 0 | 32612.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28331.2 | 28331.2 | 76375.9 | 0 | PROCESSED | 57541.7496180556 | 54901 | 54535.208599537 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021122 | We propose to observe 3 INTEGRAL-discovered High Mass X-ray Binaries (IGR HMXBs) to search for X-ray pulsations and to study their broadband spectra. Over the past few years, INTEGRAL has found a surprising number of HMXBs, and the large number of new, locally absorbed supergiant HMXBs indicate that these wind-accretors are more common than previously thought. In addition to high column densities, some of these systems have other extreme properties such as slowly rotating neutron stars (NSs) or rapid X-ray flares. For the systems we propose to observe, detection of pulsations is important for establishing the presence of a NS and for constraining the spin period distribution for HMXB NSs. As these are strong hard X-ray emitters, we will take advantage of Suzaku's broadband capabilities. | GALACTIC POINT SOURCES | 4 | B | TOMSICK | JOHN | NULL | NULL | USA | 2 | AO2 | LOOKING FOR SIGNATURES OF HIGH MAGNETIC FIELD NEUTRON STARS IN INTEGRAL HMXBS | XIS | Y |
| IGR J17391-3021 | 264.795 | -30.3419 | 358.06793122 | 0.44854091 | 89.216 | 54518.4950115741 | 54519.3961226852 | 402066010 | 36465.7 | 30000 | 36545.7 | 36593.7 | 0 | 36465.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 31259.1 | 31259.1 | 77819.8 | 1 | PROCESSED | 57541.7105671296 | 54892 | 54525.5064699074 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021122 | We propose to observe 3 INTEGRAL-discovered High Mass X-ray Binaries (IGR HMXBs) to search for X-ray pulsations and to study their broadband spectra. Over the past few years, INTEGRAL has found a surprising number of HMXBs, and the large number of new, locally absorbed supergiant HMXBs indicate that these wind-accretors are more common than previously thought. In addition to high column densities, some of these systems have other extreme properties such as slowly rotating neutron stars (NSs) or rapid X-ray flares. For the systems we propose to observe, detection of pulsations is important for establishing the presence of a NS and for constraining the spin period distribution for HMXB NSs. As these are strong hard X-ray emitters, we will take advantage of Suzaku's broadband capabilities. | GALACTIC POINT SOURCES | 4 | B | TOMSICK | JOHN | NULL | NULL | USA | 2 | AO2 | LOOKING FOR SIGNATURES OF HIGH MAGNETIC FIELD NEUTRON STARS IN INTEGRAL HMXBS | XIS | Y |
| 4U 1907+09 | 287.4001 | 9.8965 | 43.79892996 | 0.51344636 | 85.3836 | 54209.4191666667 | 54211.2612731482 | 402067010 | 80628.3 | 65000 | 80628.3 | 80636.3 | 0 | 80636.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 73268.5 | 73268.5 | 159147.9 | 2 | PROCESSED | 57538.4515393518 | 54702 | 54216.2674189815 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021123 | The HMXB 4U 1907+09 shows a rich phenomenology: two cyclotron lines, an uncommonly weak iron line, intermittent X-ray fading, and a recent torque reversal. Compared to other persistent supergiant X-ray pulsars it has been less well observed, although it is a prime target to study the interaction of the neutron star's X-rays with the stellar wind and the accretion column. The latter has been confirmed by our 60ks AO1 observation which allowed for the first detection of a soft excess below 2keV as well as the determination of the paramters of the fundamental cyclotron line with unprecedented accuracy. Due to an unusually low source state during the AO1 exposure, however, an additional observation of 65ks is needed to perform the first phase resolved analysis of this interesting source. | GALACTIC POINT SOURCES | 4 | B | POTTSCHMIDT | KATJA | NULL | NULL | USA | 2 | AO2 | THE BROAD BAND SPECTRUM OF 4U 1907+09 | HXD | N |
| EXO 2030+375 | 308.0118 | 37.6951 | 77.17399477 | -1.17458429 | 56.3502 | 54234.8591666667 | 54236.1565277778 | 402068010 | 57607.1 | 40000 | 57607.1 | 57607.1 | 0 | 57607.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 53395.4 | 53395.4 | 112067.8 | 2 | PROCESSED | 57538.7243055556 | 54702 | 54242.497962963 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021124 | We propose a 40 ks Suzaku observation to confirm EXO 2030+375's recently discovered ~10 keV cyclotron feature and constrain its second harmonic at ~20 keV. EXO 2030+375 is a 42-second Be/X-ray pulsar in an eccentric 46-day orbit. If confirmed the ~10 keV cyclotron feature will be the lowest in energy known for an accreting pulsar and will provide the missing piece to make EXO 2030+375 an ideal candidate to observationally test accretion theory. In addition, we will measure EXO 2030+375's spin frequency, study its pulse shape versus energy, and perform phase resolved spectroscopy. Suzaku will allow these studies to reach lower energies and provide high quality spectra at lower luminosities than in any previous observations. | GALACTIC POINT SOURCES | 4 | A | WILSON | COLLEEN | NULL | NULL | USA | 2 | AO2 | CONSTRAINING CYCLOTRON FEATURES IN A NORMAL OUTBURST OF EXO 2030+375 | HXD | Y |
| 4U2206+54 | 331.9811 | 54.5897 | 100.6432606 | -1.04691755 | 90.2357 | 54236.1620949074 | 54237.812662037 | 402069010 | 103976.8 | 100000 | 103984.8 | 103990.6 | 0 | 103976.8 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 99784.2 | 99784.2 | 142581.9 | 1 | PROCESSED | 57538.7118402778 | 54695 | 54242.76625 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021125 | 4U 2206+54 is a high mass X-ray binary which is suspected to contain a neutron star accreting from the wind of its companion BD +53 2790. However, there has been no confirmed detection of X-ray pulsations, and while several authors have reported hints of a cyclotron line in the energy spectra near 30 keV, none have reported significant detections. We propose Suzaku observations to search for long-period pulsations with the XIS, and possible confirmation of the cyclotron line using HXD/PIN. | GALACTIC POINT SOURCES | 4 | A | FINGER | MARK | NULL | NULL | USA | 2 | AO2 | SUZAKU OBSERVATIONS OF THE PECULIAR HMXB 4U 2206+54 | HXD | Y |
| CIRCINUS X-1 | 230.1633 | -57.1695 | 322.11384942 | 0.03740334 | 115.206 | 54530.1953240741 | 54531.5523032407 | 402070010 | 46411.3 | 43000 | 46411.3 | 46411.3 | 0 | 46411.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41821.3 | 41821.3 | 117196 | 0 | PROCESSED | 57541.8053125 | 54916 | 54550.2459953704 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021128 | We propose a 100ks Suzaku observation of Circinus X-1 through the zero (dipping) phase to facilitate 2 important and independent science goals. (1) For the binary, we wish to better understand the viewing geometry, and investigate physical changes in the binary behavior as it relates to observed spectral changes through periastron passage. (2) Conduct a large angle scattering study of the X-ray halo surrounding Circinus X-1 to diagnose ISM grain properties (the line-of-sight position, size distribution, and grain density) near us, in complement with our Chandra halo studies at small angles on grain properties near the source. | GALACTIC POINT SOURCES | 4 | A | LEE | JULIA | NULL | NULL | USA | 2 | AO2 | CIRCINUS X-1 NEAR PERIASTRON: PROBING BINARY PHYSICS AND ISM GRAINS ALONG THE LINE OF SIGHT | XIS | Y |
| GRS 1915+105 | 288.7933 | 10.9535 | 45.37037141 | -0.21130356 | 67.354 | 54227.6113657407 | 54229.0717476852 | 402071010 | 65656.8 | 37000 | 65656.8 | 65803.9 | 0 | 65672.8 | 1 | 2 | 0 | 1 | 1 | 0 | 0 | 56897.3 | 56897.3 | 126168 | 1 | PROCESSED | 57538.6640972222 | 54702 | 54235.5321759259 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021132 | We have discovered a connection between Fe line strength and QPO phase in RXTE observations of GRS 1915+105. This connection independently ties Fe lines to radii less than 100 R_Schw. QPO-phase-resolved Suzaku spectra will enable us to detect changes in the relativistic line profile (inner radius, equivalent width), to extend the connection to the broadband disk reflection spectrum, and to test models for the Fe line - QPO connection. Moreover, at CCD resolution, the connection can be used to over-constrain disk radii - a first step toward mapping the inner disk. We therefore request a 37 ksec TOO observation of GRS 1915+105. Understanding black hole accretion is fundamental to NASA's "SEU" theme. | GALACTIC POINT SOURCES | 4 | A | MILLER | JON | NULL | NULL | USA | 2 | AO2-TOO | THE RELATIVISTIC IRON LINE - QPO CONNECTION IN GRS 1915+105 | XIS | Y |
| CYG X-1 | 299.5792 | 35.2719 | 71.39034122 | 3.11120593 | 84.3565 | 54220.8163657407 | 54221.783587963 | 402072010 | 45320.4 | 30000 | 45320.4 | 45328.4 | 0 | 45320.4 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 40187.3 | 40187.3 | 83566 | 2 | PROCESSED | 57538.518275463 | 54773 | 54228.1718518518 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021133 | We request two additional 30 ksec observations of Cyg X-1, to be coordinated with our ongoing RXTE and Ryle radio telescope monitoring campaign. Suzaku will bring three unique attributes to this campaign: the ability to describe the 0.5-3 keV spectrum (crucial for describing the disk spectrum), high spectral resolution in the Fe line region (crucial for resolving narrow from relativistically broadened features), and the 200-600 keV spectrum (crucial for distinguishing among thermal corona, non-thermal corona, and jet models). By coordinating with our ongoing monitoring program, we not only obtain useful cross-calibration information, we will be able to place current and future Suzaku observations of Cyg X-1 in the context of the source's global history. | GALACTIC POINT SOURCES | 4 | A | NOWAK | MICHAEL | NULL | NULL | USA | 2 | AO2 | CONTINUING TO ENHANCE THE LONG TERM MONITORING CAMPAIGN OF CYGNUS X-1 IN THE SUZAKU ERA | HXD | Y |
| CYG X-1 | 299.5451 | 35.2618 | 71.3671857 | 3.12971485 | 59.9371 | 54237.8204050926 | 54238.6480787037 | 402072020 | 33356.8 | 30000 | 33356.8 | 33364.9 | 0 | 33356.8 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 32563.7 | 32563.7 | 71503.9 | 1 | PROCESSED | 57538.696724537 | 54695 | 54245.0149884259 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021133 | We request two additional 30 ksec observations of Cyg X-1, to be coordinated with our ongoing RXTE and Ryle radio telescope monitoring campaign. Suzaku will bring three unique attributes to this campaign: the ability to describe the 0.5-3 keV spectrum (crucial for describing the disk spectrum), high spectral resolution in the Fe line region (crucial for resolving narrow from relativistically broadened features), and the 200-600 keV spectrum (crucial for distinguishing among thermal corona, non-thermal corona, and jet models). By coordinating with our ongoing monitoring program, we not only obtain useful cross-calibration information, we will be able to place current and future Suzaku observations of Cyg X-1 in the context of the source's global history. | GALACTIC POINT SOURCES | 4 | A | NOWAK | MICHAEL | NULL | NULL | USA | 2 | AO2 | CONTINUING TO ENHANCE THE LONG TERM MONITORING CAMPAIGN OF CYGNUS X-1 IN THE SUZAKU ERA | HXD | Y |
| SWIFT J1753.5-0127 | 268.3714 | -1.4588 | 24.89300861 | 12.1795145 | 261.3846 | 54362.8585185185 | 54365.4377777778 | 402088010 | 94600.5 | 93000 | 94608.5 | 94616.5 | 0 | 94600.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 81739 | 81739 | 222836 | 3 | PROCESSED | 57540.1123842593 | 54743 | 54371.6366319444 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021147 | While the spectrally hard state represents the most common mode of accretion in black hole X-ray binaries, the nature of its accretion flow is poorly understood. We recently discovered cool accretion disks extending close to the innermost stable circular orbit in the hard states of two black hole transients. Such disks could give rise to strong reflection features, but instead these are weak or not detected. We propose a 70 ks Suzaku observation of Swift J1753.5-0127 (one of the two transients), which is currently in a prolonged hard state. Our goal is to put tight constraints on the strength of the reflection features and increase our understanding of the geometry of the spectrally hard component. Understanding accretion onto compact objects is fundamental to NASA's "SEU" theme. | GALACTIC POINT SOURCES | 4 | A | HOMAN | JEROEN | NULL | NULL | USA | 2 | AO2 | CONSTRAINING REFLECTION FEATURES IN THE HARD STATE OF BLACK HOLE X-RAY BINARIES | XIS | Y |
| TW HYA | 165.4619 | -34.7081 | 278.67685486 | 22.95004903 | 99.3673 | 54429.0615625 | 54429.6946064815 | 402089020 | 20009.6 | 11000 | 20009.6 | 20017.6 | 0 | 20025.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17550 | 17550 | 54687.9 | 2 | PROCESSED | 57540.5900115741 | 54804 | 54434.1387268518 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 022007 | We propose to observe the cTTS TW~Hya, SU~Aur and XZ~Tau with the Suzaku XIS in order to search for soft X-ray "excesses", indicating the presence of accretion induced X-rays in cTTS. We plan to utilize the sensitivity and capability of the Suzaku XIS to resolve the OVIII/OVII lines.With grating observations the absence of the forbidden line in the latter was found to provide strong evidence for the presence of accretion in the X-ray spectra of a few cTTS. With the increased sensitivity of Suzaku the presence of soft X-ray excesses can be demonstrated in a far larger sample of stars, and we want to demonstrate the existence of a soft X-ray, probably accretion induced component in cTTS with extremely hot coronae exhibiting the presence of the 6.7 keV iron line complex in their spectra. | GALACTIC POINT SOURCES | 4 | B | SCHMITT | JURGEN | NULL | NULL | EUR | 2 | AO2 | ACCRETION RELATED SOFT X-RAY EMISSION IN CLASSICAL T TAURI STARS | XIS | Y |
| SU AUR | 73.9934 | 30.5715 | 172.51103259 | -7.93275707 | 85.9197 | 54339.1713541667 | 54340.7502199074 | 402090010 | 57303.4 | 55000 | 57311.4 | 57303.4 | 0 | 57311.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 54384.8 | 54384.8 | 136401.8 | 1 | PROCESSED | 57539.9114699074 | 54723 | 54350.6381597222 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 022007 | We propose to observe the cTTS TW~Hya, SU~Aur and XZ~Tau with the Suzaku XIS in order to search for soft X-ray "excesses", indicating the presence of accretion induced X-rays in cTTS. We plan to utilize the sensitivity and capability of the Suzaku XIS to resolve the OVIII/OVII lines.With grating observations the absence of the forbidden line in the latter was found to provide strong evidence for the presence of accretion in the X-ray spectra of a few cTTS. With the increased sensitivity of Suzaku the presence of soft X-ray excesses can be demonstrated in a far larger sample of stars, and we want to demonstrate the existence of a soft X-ray, probably accretion induced component in cTTS with extremely hot coronae exhibiting the presence of the 6.7 keV iron line complex in their spectra. | GALACTIC POINT SOURCES | 4 | A | SCHMITT | JURGEN | NULL | NULL | EUR | 2 | AO2 | ACCRETION RELATED SOFT X-RAY EMISSION IN CLASSICAL T TAURI STARS | XIS | Y |
| EXO 0748-676 | 117.1051 | -67.7525 | 279.97237585 | -19.82332654 | 158.0884 | 54459.2369560185 | 54460.2919444444 | 402092010 | 45898.8 | 40000 | 45912.6 | 45898.8 | 0 | 45904.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43574.7 | 43574.7 | 91135.8 | 1 | PROCESSED | 57540.9732175926 | 54854 | 54483.1839351852 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 022014 | We propose Suzaku observations of the dipping Low Mass X-ray Binaries (LMXBs) EXO 0748-676 and X 1624-490. The changes in both the continuum and the He- and H- like Fe K absorption features during dips have been demonstrated to be consistent with a change in the properties of the photoionized absorbers present in these systems. We will use the XIS to characterise the absorbers and the HXD to uniquely determine the underlying continuum shapes including any contributions due to reflection components. This will allow to reliably determine the absolute values of the ionization parameters for each of the sources, which was not possible with XMM due to the lack of contemporaneous high energy spectra, providing for a detailed comparison of the absorbers with source properties such as luminosity. | GALACTIC POINT SOURCES | 4 | C | DIAZ TRIGO | MARIA | NULL | NULL | EUR | 2 | AO2 | BROAD-BAND OBSERVATIONS OF HIGHLY-IONIZED ABSORBERS IN DIPPING LMXBS | XIS | Y |
| SGR 1806-20 | 272.1687 | -20.4711 | 9.94559743 | -0.27498509 | 268.1397 | 54387.2332060185 | 54388.333599537 | 402094010 | 52247.7 | 50000 | 52247.7 | 52271.7 | 0 | 52263.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 50089.5 | 50089.5 | 95059.9 | 1 | PROCESSED | 57540.2839583333 | 54771 | 54403.9548611111 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 022016 | Among magnetars, SGR 1806-20 is particularly interesting since it emitted two years ago the most powerful giant flare ever observed. We are performing a long term monitoring in the soft X-rays with XMM-Newton and hard X-rays with INTEGRAL to study how the source evolves back to quiescence. We obtained in AO-1 a Suzaku observation that was carried out simultaneously with XMM-Newton and provided for the first time a broad band spectrum of SGR 1806-20 on a short timescale. A new observation is required to study the spectral variability in the hard X-ray range and possibly the properties of bursts. | GALACTIC POINT SOURCES | 4 | C | MEREGHETTI | SANDRO | NULL | NULL | EUR | 2 | AO2 | CONTINUED MONITORING OF SGR 1806-20 AFTER THE GIANT FLARE WITH SUZAKU AND XMM-NEWTON | HXD | Y |
| GT MUS | 174.8799 | -65.348 | 295.52044001 | -3.51633969 | 94.8564 | 54446.4736689815 | 54449.187662037 | 402095010 | 93308.7 | 80000 | 93308.7 | 93308.7 | 0 | 93308.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 94696.5 | 94696.5 | 234469.9 | 3 | PROCESSED | 57540.9318287037 | 54828 | 54460.7707060185 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 022020 | We propose to perform broad-band X-ray spectroscopy of the RS CVn-like system GT Muscae, with the aim to study the thermal and non-thermal components of its X-ray emitting plasma. Our target is a known hard X-ray source, detected with Uhuru and recently with Integral/IBIS in the 20-40 keV band, but lacking a dedicated observation with modern X-ray spectrometers. The proposed observation will allow us to investigate both the quiescent and flaring states of this complex (possibly interacting) binary system, by means of a variability study and a time-resolved spectral analysis of its X-ray emission. We aim to detect and constrain the non-thermal hard X-ray emission component, and to search for a possible Fe Kalpha line emission, thanks to the superb broad-band spectral capabilities of Suzaku. | GALACTIC POINT SOURCES | 4 | B | MAGGIO | ANTONIO | NULL | NULL | EUR | 2 | AO2 | BROAD-BAND X-RAY SPECTROSCOPY OF AN EXTREMELY ACTIVE CORONAL SOURCE | HXD | Y |
| HD161103 | 266.1888 | -27.2272 | 1.35850162 | 1.05434609 | 105.2351 | 54884.7946643518 | 54886.7057175926 | 403001010 | 71524.9 | 60000 | 71532.9 | 71524.9 | 0 | 71540.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 59664.7 | 59664.7 | 165085.8 | 1 | PROCESSED | 57545.6533217593 | 55330 | 54903.6732523148 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030005 | We propose Suzaku observations of gamma Cas analogues. The sources in this class are characterized by extremely high thermal temperature and iron fluorescent line. We aim to identify the hard X-ray production site using the XIS's spectral capability at the iron K complex and the wide-band sensitivity combining XIS and HXD PIN. | GALACTIC POINT SOURCES | 4 | B | MIURA | JUNICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU INVESTIGATION OF GAMMA CAS ANALOGUES | XIS | Y |
| HD110432 | 190.599 | -63.0744 | 301.908501 | -0.22062002 | 344.9423 | 54718.9065740741 | 54719.7050231482 | 403002010 | 25333.2 | 25000 | 25333.2 | 25333.2 | 0 | 25333.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21343.6 | 21343.6 | 68977.9 | 0 | PROCESSED | 57543.8037615741 | 55148 | 54780.4451736111 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030005 | We propose Suzaku observations of gamma Cas analogues. The sources in this class are characterized by extremely high thermal temperature and iron fluorescent line. We aim to identify the hard X-ray production site using the XIS's spectral capability at the iron K complex and the wide-band sensitivity combining XIS and HXD PIN. | GALACTIC POINT SOURCES | 4 | B | MIURA | JUNICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU INVESTIGATION OF GAMMA CAS ANALOGUES | HXD | Y |
| 1RXS J070407.9+26250 | 106.0316 | 26.4199 | 190.26714041 | 14.29962915 | 96.1437 | 54749.1266319444 | 54750.3682175926 | 403003010 | 53551.9 | 50000 | 53551.9 | 53551.9 | 0 | 53551.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41140.5 | 41140.5 | 107231.9 | 0 | PROCESSED | 57544.1456944445 | 55148 | 54780.5445949074 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030009 | Soft Intermediate Polar (IP) is a group of IPs whose X-ray spectra are extremely soft compared with general IPs. Recent observations reveal that some soft IPs have a soft blackbody emission component like polars, yet its nature is not fully understood. Systematic study of the soft IP blackbody emission is important in the sense that it may provide a clue to understand comprehensively the emission characteristics of polars and IPs in the soft X-ray band, and to follow possible evolutionary link from IPs to polars, etc. We propose to observe five soft IPs, each for 50ksec, in order to search for the blackbody component and to measure its temperature and flux systematically. | GALACTIC POINT SOURCES | 4 | B | ISHIDA | MANABU | NULL | NULL | JAP | 3 | AO3 | OBSERVATIONS OF SOFT INTERMEDIATE POLARS | XIS | Y |
| 1RXS J062518.2+73343 | 96.3307 | 73.5671 | 140.86801575 | 24.12512545 | 262.0383 | 54570.0388310185 | 54571.1252777778 | 403004010 | 50326.7 | 50000 | 50326.7 | 50326.7 | 0 | 50326.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 50125.3 | 50125.3 | 93848.8 | 0 | PROCESSED | 57542.3202430556 | 54953 | 54581.2328472222 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030009 | Soft Intermediate Polar (IP) is a group of IPs whose X-ray spectra are extremely soft compared with general IPs. Recent observations reveal that some soft IPs have a soft blackbody emission component like polars, yet its nature is not fully understood. Systematic study of the soft IP blackbody emission is important in the sense that it may provide a clue to understand comprehensively the emission characteristics of polars and IPs in the soft X-ray band, and to follow possible evolutionary link from IPs to polars, etc. We propose to observe five soft IPs, each for 50ksec, in order to search for the blackbody component and to measure its temperature and flux systematically. | GALACTIC POINT SOURCES | 4 | B | ISHIDA | MANABU | NULL | NULL | JAP | 3 | AO3 | OBSERVATIONS OF SOFT INTERMEDIATE POLARS | XIS | Y |
| 1E 1048.1-5937 | 162.5452 | -59.8394 | 288.24102095 | -0.47209541 | 101.4368 | 54800.9597337963 | 54802.5927083333 | 403005010 | 100423.1 | 100000 | 100443 | 100423.1 | 0 | 100423.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 68104.9 | 68104.9 | 141081.9 | 0 | PROCESSED | 57544.6078472222 | 55178 | 54812.0471875 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030013 | Observations in soft X-ray through hard X-ray bands are key to understand the emission processes in the magnetosphere of Anomalous X-ray Pulsars (AXPs). We propose to observe the two AXPs, 1E 2259+586 and 1E 1048.1-5937, with SUZAKU. Although no detections of the hard X-ray emissions have been reported, the results of the simulation using XSPEC for HXD indicate that SUZAKU detects the hard X-ray emissions above 20~keV from both AXPs for the first time with a quite high probability. The time resolution of HXD is able to provide the pulse profiles and the phase-resolved spectra in hard X-rays emissions. With these results of the observations, SUZAKU will provide a crucial information to study the emission processes in the magnetosphere of AXPs. | GALACTIC POINT SOURCES | 4 | C | TAKATA | JUMPEI | NULL | NULL | JAP | 3 | AO3 | X-RAY OBSERVATIONS OF ANOMALOUS X-RAY PULSARS WITH SUZAKU | HXD | Y |
| MARS-P1 | 102.8773 | 25.1625 | 190.24974394 | 11.19384085 | 298.0037 | 54559.3414814815 | 54559.4099421296 | 403006010 | 2904.8 | 100000 | 2904.8 | 2912.8 | 0 | 2912.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 2909.6 | 2909.6 | 5911.9 | 0 | PROCESSED | 57542.0343981482 | 54953 | 54577.0446875 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y |
| MARS-P2 | 102.9198 | 25.1641 | 190.26475308 | 11.2294146 | 298.0203 | 54559.4100925926 | 54559.493275463 | 403006020 | 4854.6 | 100000 | 4854.6 | 4886.6 | 0 | 4870.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3612.1 | 3612.1 | 7183.9 | 0 | PROCESSED | 57542.0367939815 | 54953 | 54577.0304976852 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y |
| MARS-P3 | 102.9612 | 25.1565 | 190.28784034 | 11.26022306 | 298.032 | 54559.4933796296 | 54559.5766087963 | 403006030 | 3886 | 100000 | 3886 | 3910 | 0 | 3894 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3113.4 | 3113.4 | 7183.9 | 0 | PROCESSED | 57542.0373148148 | 54953 | 54577.0484259259 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y |
| MARS-P4 | 103.0016 | 25.1536 | 190.30618657 | 11.29219101 | 298.0476 | 54559.5767592593 | 54559.6599421296 | 403006040 | 2288.2 | 100000 | 2288.2 | 2288.2 | 0 | 2288.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 2010 | 2010 | 7183.9 | 0 | PROCESSED | 57542.0411226852 | 54953 | 54577.0528935185 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y |
| MARS-P5 | 103.045 | 25.1496 | 190.32670814 | 11.32616716 | 298.0638 | 54559.6600462963 | 54559.7432407407 | 403006050 | 1956.2 | 100000 | 1956.2 | 1956.2 | 0 | 1956.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 1992.6 | 1992.6 | 7167.9 | 0 | PROCESSED | 57542.0421527778 | 54953 | 54577.1345486111 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y |
| MARS-P6 | 103.0844 | 25.143 | 190.34808199 | 11.3557719 | 298.0743 | 54559.7434375 | 54559.8265972222 | 403006060 | 1939 | 100000 | 1939 | 1939 | 0 | 1939 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 1804.6 | 1804.6 | 7181.9 | 0 | PROCESSED | 57542.0435416667 | 54953 | 54577.1376388889 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y |
| MARS-P7 | 103.127 | 25.1401 | 190.36726484 | 11.38956433 | 298.0907 | 54559.8267476852 | 54559.9029861111 | 403006070 | 2502.8 | 100000 | 2513.9 | 2510.8 | 0 | 2502.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 1650.6 | 1650.6 | 6584 | 0 | PROCESSED | 57542.0488310185 | 54953 | 54577.1486342593 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y |
| MARS-P8 | 103.1682 | 25.1356 | 190.38738197 | 11.42154102 | 298.1062 | 54559.9031365741 | 54560.0072222222 | 403006080 | 2748.9 | 100000 | 2753.8 | 2757.8 | 0 | 2748.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 2286.4 | 2286.4 | 8984 | 0 | PROCESSED | 57542.0500578704 | 54953 | 54577.1637615741 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y |
| MARS-P9 | 103.2195 | 25.1275 | 190.41473742 | 11.46031922 | 298.1247 | 54560.0073726852 | 54560.0766666667 | 403006090 | 2150.6 | 100000 | 2150.6 | 2174.6 | 0 | 2150.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 1891.9 | 1891.9 | 5975.9 | 0 | PROCESSED | 57542.0488888889 | 54953 | 54577.1428009259 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y |
| MARS-P10 | 103.2518 | 25.125 | 190.42954859 | 11.48582895 | 298.135 | 54560.0767708333 | 54560.16 | 403006100 | 3771.6 | 100000 | 3795.6 | 3771.6 | 0 | 3796 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 4001.4 | 4001.4 | 7183.9 | 0 | PROCESSED | 57542.0546527778 | 54953 | 54577.1537847222 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y |
| MARS-P11 | 103.2936 | 25.1207 | 190.44969799 | 11.5184009 | 298.1493 | 54560.1601041667 | 54560.2433333333 | 403006110 | 4619.8 | 100000 | 4627.8 | 4619.8 | 0 | 4635.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 4074.9 | 4074.9 | 7183.9 | 0 | PROCESSED | 57542.0559490741 | 54953 | 54577.1745023148 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y |
| MARS-P12 | 103.3358 | 25.1148 | 190.47148034 | 11.55063865 | 298.1645 | 54560.2434837963 | 54560.3266666667 | 403006120 | 3455 | 100000 | 3455 | 3455 | 0 | 3455 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 2678 | 2678 | 7175.9 | 0 | PROCESSED | 57542.0566782407 | 54953 | 54577.1789467593 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y |
| MARS-P13 | 103.3779 | 25.1101 | 190.49210676 | 11.58330245 | 298.1799 | 54560.3267708333 | 54560.41 | 403006130 | 4251.8 | 100000 | 4267.8 | 4251.8 | 0 | 4267.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3529 | 3529 | 7183.9 | 0 | PROCESSED | 57542.0605671296 | 54953 | 54577.9292939815 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y |
| MARS-P14 | 103.4188 | 25.1057 | 190.5119865 | 11.61511049 | 298.1941 | 54560.410150463 | 54560.4933333333 | 403006140 | 4825.2 | 100000 | 4849.2 | 4825.2 | 0 | 4857.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3721.4 | 3721.4 | 7175.9 | 0 | PROCESSED | 57542.063125 | 54953 | 54577.9434722222 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y |
| MARS-P15 | 103.4611 | 25.1019 | 190.53184536 | 11.64832678 | 298.2083 | 54560.4934375 | 54560.5766666667 | 403006150 | 3831 | 100000 | 3839 | 3831 | 0 | 3847 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3192.8 | 3192.8 | 7183.9 | 1 | PROCESSED | 57542.0622222222 | 54953 | 54580.5809837963 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y |
| MARS-P16 | 103.503 | 25.0968 | 190.55275085 | 11.68067717 | 298.2223 | 54560.5768171296 | 54560.66 | 403006160 | 2326.2 | 100000 | 2326.2 | 2326.2 | 0 | 2326.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 2134 | 2134 | 7179.9 | 0 | PROCESSED | 57542.0664236111 | 54953 | 54577.9478935185 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y |
| MARS-P17 | 103.5439 | 25.0908 | 190.5741012 | 11.71183533 | 298.237 | 54560.6601041667 | 54560.743287037 | 403006170 | 1978.2 | 100000 | 1978.2 | 1978.2 | 0 | 1978.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 1959.6 | 1959.6 | 7182 | 0 | PROCESSED | 57542.0674074074 | 54953 | 54578.0406597222 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y |
| MARS-P18 | 103.5869 | 25.0943 | 190.58743765 | 11.74868918 | 298.2592 | 54560.7434837963 | 54560.8264351852 | 403006180 | 1861.8 | 100000 | 1861.8 | 1861.8 | 0 | 1861.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 1939.6 | 1939.6 | 7153.9 | 0 | PROCESSED | 57542.0705555556 | 54953 | 54578.0530555556 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y |
| MARS-P19 | 103.6272 | 25.0809 | 190.61541806 | 11.77628093 | 298.2673 | 54560.8266319444 | 54560.9098842593 | 403006190 | 2839.8 | 100000 | 2839.8 | 2848.2 | 0 | 2843.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 1844.1 | 1844.1 | 7190 | 0 | PROCESSED | 57542.0723958333 | 54953 | 54578.0465625 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y |
| MARS-P20 | 103.6685 | 25.0732 | 190.63848879 | 11.80707935 | 298.2779 | 54560.9100347222 | 54560.9932175926 | 403006200 | 1849 | 100000 | 1849 | 1849 | 0 | 1849 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 1222 | 1222 | 7183.9 | 0 | PROCESSED | 57542.0733101852 | 54953 | 54578.0575231482 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y |
| MARS-P21 | 103.7101 | 25.0688 | 190.65860601 | 11.8395058 | 298.2947 | 54560.9933217593 | 54561.0765509259 | 403006210 | 2880.8 | 100000 | 2880.8 | 2880.8 | 0 | 2880.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3451.6 | 3451.6 | 7183.9 | 0 | PROCESSED | 57542.0774884259 | 54953 | 54578.0612847222 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y |
| MARS-P22 | 103.7541 | 25.0677 | 190.67657625 | 11.87528798 | 298.3117 | 54561.0767013889 | 54561.1598842593 | 403006220 | 4024.6 | 100000 | 4040.6 | 4024.6 | 0 | 4047.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 4102 | 4102 | 7183.9 | 0 | PROCESSED | 57542.0781712963 | 54953 | 54578.0665625 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y |
| MARS-P23 | 103.7955 | 25.0599 | 190.69976585 | 11.90614711 | 298.325 | 54561.1600347222 | 54561.2432175926 | 403006230 | 4518.8 | 100000 | 4526.8 | 4518.8 | 0 | 4534.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3686.8 | 3686.8 | 7183.9 | 0 | PROCESSED | 57542.0791898148 | 54953 | 54578.1176157407 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y |
| MARS-P24 | 103.8389 | 25.0556 | 190.72046804 | 11.94011608 | 298.3401 | 54561.2433680556 | 54561.3265509259 | 403006240 | 3423 | 100000 | 3423 | 3423 | 0 | 3423 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 2511 | 2511 | 7183.9 | 0 | PROCESSED | 57542.0844328704 | 54953 | 54578.1234375 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y |
| MARS-P25 | 103.8803 | 25.0503 | 190.74132534 | 11.97202775 | 298.3546 | 54561.3266550926 | 54561.4098842593 | 403006250 | 4261.2 | 100000 | 4269.2 | 4261.2 | 0 | 4269.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3251.1 | 3251.1 | 7183.9 | 0 | PROCESSED | 57542.2336458333 | 54953 | 54578.1323032407 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y |
| MARS-P26 | 103.921 | 25.0474 | 190.75967691 | 12.00436516 | 298.3671 | 54561.4100347222 | 54561.4932175926 | 403006260 | 4797.6 | 100000 | 4813.6 | 4797.6 | 0 | 4821.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3762.2 | 3762.2 | 7183.9 | 0 | PROCESSED | 57542.2337962963 | 54953 | 54578.1374074074 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y |
| MARS-P27 | 103.964 | 25.0399 | 190.78318678 | 12.0366945 | 298.3836 | 54561.4933217593 | 54561.5418171296 | 403006270 | 1099.8 | 100000 | 1107.8 | 1099.8 | 0 | 1115.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 1093.5 | 1093.5 | 4183.9 | 0 | PROCESSED | 57542.2332175926 | 54953 | 54578.1251273148 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030015 | We propose Suzaku XIS observation of Mars. With XMM-Newton RGS, X-rays from Mars are suggested to have two components: one due to fluorescent scattering of solar X-rays in its atmosphere and the other due to the solar wind charge exchange in its exosphere. X-rays thus can be a new probe to study the puzzling Martian exosphere that holds key information about how the Martian air has been lost. With XIS, we can detect the emission lines with the highest photon statistics ever. For the first time, we will observe the solar wind near the Mars simultaneously with Mars Express and extract information about the exosphere. This will be the first X-ray observation of Mars at solar minimum when the exosphere is expected to be dense and X-rays from the exosphere will largely increase. | GALACTIC POINT SOURCES | 4 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF X-RAY EMISSION LINES FROM THE MARTIAN EXOSPHERE INDUCED BY THE SOLAR WIND CHARGE EXCHANGE | XIS | Y |
| AM HERCULES | 274.126 | 49.8084 | 77.81082077 | 25.81903319 | 234.8814 | 54768.8590162037 | 54771.3043287037 | 403007010 | 108496.5 | 100000 | 108504.5 | 108504.5 | 0 | 108496.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 94467.1 | 94467.1 | 211257.7 | 3 | PROCESSED | 57544.3392476852 | 55156 | 54788.4722222222 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030021 | We propose the observation of the proto-type magnetic catacrysmic variables, AM Hercules, to search for possible hard X-ray tail on the thermal emission with Suzaku. To reduce the systematics of the estimation of the GSO background in the analyses, we propose the additional observation of blank sky near the object. | GALACTIC POINT SOURCES | 4 | C | TERADA | YUKIKATSU | NULL | NULL | JAP | 3 | AO3 | NON THERMAL EMISSION FROM THE POLAR AM HERCULES | HXD | Y |
| AM HERCULES BGD | 282.0964 | 47.9785 | 77.40285415 | 20.2844947 | 234.9986 | 54771.3072106482 | 54772.3438310185 | 403008010 | 44360.1 | 40000 | 44368.1 | 44360.1 | 0 | 44392.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40411.5 | 40411.5 | 89551.9 | 1 | PROCESSED | 57544.3170833333 | 55154 | 54788.4288541667 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030021 | We propose the observation of the proto-type magnetic catacrysmic variables, AM Hercules, to search for possible hard X-ray tail on the thermal emission with Suzaku. To reduce the systematics of the estimation of the GSO background in the analyses, we propose the additional observation of blank sky near the object. | GALACTIC POINT SOURCES | 4 | C | TERADA | YUKIKATSU | NULL | NULL | JAP | 3 | AO3 | NON THERMAL EMISSION FROM THE POLAR AM HERCULES | XIS | Y |
| ARCHES CLUSTER | 266.4808 | -28.778 | 0.16960578 | 0.02569084 | 109.9998 | 54911.0857407407 | 54913.7681712963 | 403009010 | 110793.3 | 100000 | 110793.3 | 110793.3 | 0 | 110793.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 91657.8 | 91657.8 | 231741.7 | 3 | PROCESSED | 57545.9555787037 | 55330 | 54924.3822106482 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030029 | We propose to observe a hard X-ray ring which has an emission line around 6.4 keV, located at the north of the Arches cluster. The ring is probably produced by an energetic jet or a supernova explosion. We aim to determine the continuum shape, the center energy of the emission line, and the absorption column to figure out the origin of the ring. | GALACTIC POINT SOURCES | 4 | B | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 3 | AO3 | A 6.4 KEV RING AT THE NORTH OF THE ARCHES CLUSTER | XIS | Y |
| GX 339-4 | 255.6944 | -48.7333 | 338.97952784 | -4.28620483 | 84.7264 | 54908.0786226852 | 54908.9613310185 | 403011010 | 43040.8 | 40000 | 43055.4 | 43040.8 | 0 | 43061.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 35391.4 | 35391.4 | 76257.9 | 1 | PROCESSED | 57545.8736458333 | 55330 | 54917.4333796296 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030046 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 3 | AO3-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | HXD | Y |
| GX 339-4 | 255.7293 | -48.7348 | 338.99236079 | -4.30539701 | 107.9544 | 54915.3430555556 | 54916.2711111111 | 403011020 | 39079.2 | 40000 | 39116.5 | 39079.2 | 0 | 39116.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 34785.2 | 34785.2 | 80165.8 | 0 | PROCESSED | 57545.909849537 | 55330 | 54930.1609490741 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030046 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 3 | AO3-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | HXD | Y |
| GX 339-4 | 255.7297 | -48.7352 | 338.99220289 | -4.30584956 | 108.3513 | 54920.4773958333 | 54921.5216435185 | 403011030 | 39638.4 | 40000 | 39663.3 | 39638.4 | 0 | 39663.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35068.6 | 35068.6 | 90186 | 0 | PROCESSED | 57545.9795601852 | 55330 | 54931.0610416667 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030046 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon the RXTE ASM. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 3 | AO3-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | HXD | Y |
| LS I+61 303_1 | 40.1455 | 61.188 | 135.69810374 | 1.0510579 | 270.0003 | 54853.9515856482 | 54854.8648032407 | 403015010 | 40551.4 | 40000 | 40551.4 | 40551.4 | 0 | 40551.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25731.2 | 25731.2 | 78868 | 0 | PROCESSED | 57545.3022916667 | 55329 | 54880.5343865741 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030077 | We propose to observe a gamma-ray binary LS I+61 303 simultaneously with the GeV/TeV gamma-ray (GLAST/VERITAS), radio, and optical, in order to ob tain the orbital-phase dependent multi-wavelength spectra (SED) in the early 2009. This observation will give us information of the relation between the binary geometry and the emission to understand the gamma-ray emissio n mechanism. Suzaku data also will enable us to probe the material distribution in the binary system by searching the Fe-K emission or absorption line, edge, an d so on. This observation will open a new window to study gamma-ray binaries, which are expected to be found with GLAST. | GALACTIC POINT SOURCES | 4 | A | FUKAZAWA | YASUSHI | NULL | NULL | JAP | 3 | AO3 | X-RAY SPECTRAL VARIABILITY OF THE GAMMA-RAY BINARY LS I+61 303 | HXD | Y |
| LS I+61 303_2 | 40.1457 | 61.1877 | 135.69831419 | 1.05082335 | 270.0006 | 54856.6966087963 | 54858.1766666667 | 403016010 | 61066.7 | 60000 | 61078.4 | 61066.7 | 0 | 61078.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26659.1 | 26659.1 | 127839.8 | 1 | PROCESSED | 57545.3828819444 | 55329 | 54880.5522106482 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030077 | We propose to observe a gamma-ray binary LS I+61 303 simultaneously with the GeV/TeV gamma-ray (GLAST/VERITAS), radio, and optical, in order to ob tain the orbital-phase dependent multi-wavelength spectra (SED) in the early 2009. This observation will give us information of the relation between the binary geometry and the emission to understand the gamma-ray emissio n mechanism. Suzaku data also will enable us to probe the material distribution in the binary system by searching the Fe-K emission or absorption line, edge, an d so on. This observation will open a new window to study gamma-ray binaries, which are expected to be found with GLAST. | GALACTIC POINT SOURCES | 4 | A | FUKAZAWA | YASUSHI | NULL | NULL | JAP | 3 | AO3 | X-RAY SPECTRAL VARIABILITY OF THE GAMMA-RAY BINARY LS I+61 303 | HXD | Y |
| LS I+61 303_3 | 40.2018 | 61.1949 | 135.72005286 | 1.06843757 | 246.2753 | 54872.1842592593 | 54873.7252199074 | 403017010 | 68627.3 | 60000 | 68627.3 | 68627.3 | 0 | 68627.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 65068.5 | 65068.5 | 133121.8 | 1 | PROCESSED | 57545.5290856482 | 55330 | 54893.4210300926 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030077 | We propose to observe a gamma-ray binary LS I+61 303 simultaneously with the GeV/TeV gamma-ray (GLAST/VERITAS), radio, and optical, in order to ob tain the orbital-phase dependent multi-wavelength spectra (SED) in the early 2009. This observation will give us information of the relation between the binary geometry and the emission to understand the gamma-ray emissio n mechanism. Suzaku data also will enable us to probe the material distribution in the binary system by searching the Fe-K emission or absorption line, edge, an d so on. This observation will open a new window to study gamma-ray binaries, which are expected to be found with GLAST. | GALACTIC POINT SOURCES | 4 | A | FUKAZAWA | YASUSHI | NULL | NULL | JAP | 3 | AO3 | X-RAY SPECTRAL VARIABILITY OF THE GAMMA-RAY BINARY LS I+61 303 | HXD | Y |
| HESS J0632+057 | 98.2456 | 5.8062 | 205.66072349 | -1.43796588 | 289.8173 | 54579.6856828704 | 54580.6877199074 | 403018010 | 44076 | 40000 | 44076 | 44076 | 0 | 44076 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41475.8 | 41475.8 | 86565.8 | 0 | PROCESSED | 57542.3746643518 | 54961 | 54594.1596990741 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030080 | We propose a 40 ks observation on HESS J0632+057, the newly discovered TeV gamma-ray source in the interacting region of Monoceros SNR and Rosette Nebula. Although this point-like source is found inside the error circle of an unidentified EGRET source 3EG J0634+0521, it has no clear counterpart at other wavelengths. Two sources, a weak X-ray source 1RXS J063258.3+05487 and a Be-star MCW 148, are found inside the error circle of HESS. The aim of the Suzaku observation is to obtain a clue to solve the yet feasible three scenarios of the TeV gamma-ray source. | GALACTIC POINT SOURCES | 4 | A | KOKUBUN | MOTOHIDE | NULL | NULL | JAP | 3 | AO3 | INVESTIGATION ON HESS J0632+057 IN MONOCEROS/ROSETTE REGION | XIS | Y |
| LMC X -3 | 84.7048 | -64.0785 | 273.57060216 | -32.09537201 | 185.5067 | 54822.3015856482 | 54823.8675694444 | 403020010 | 73973.8 | 60000 | 73973.8 | 73981.8 | 0 | 73987.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70050.5 | 70050.5 | 135283.8 | 1 | PROCESSED | 57545.0347800926 | 55206 | 54840.5013310185 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030102 | Ionized iron K absorption lines are commonly observed from high state black hole binaries. Thus the highly ionized plasma are thought to be generally associated with optically thick accretion disks. Huge outflow by the plasma has been confirmed by some of these objects, and thus such plasma is thought to have an important role on accretion flow. In order to establish generality of the plasma by detecting the absorption lines, and to distinguish whether creation mechanism of the plasma is determined by X-ray luminosity or there is another key parameter, we propose Suzaku observation of luminous persistent black hole binary LMC X-3, with exposure of 60ks. This observation will enable us to find critical parameters which determine the creation of the accretion disk wind. | GALACTIC POINT SOURCES | 4 | C | KUBOTA | AYA | NULL | NULL | JAP | 3 | AO3 | SEARCH FOR IRON K ABSORPTION LINES FROM LMC X-3 | XIS | Y |
| RX J1712.6-2414 | 258.1492 | -24.2444 | 359.8664305 | 8.74215246 | 94.4586 | 54889.4875925926 | 54892.2710532407 | 403021010 | 110481.3 | 100000 | 110489.3 | 110481.3 | 0 | 110489.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 89458.4 | 89458.4 | 240441.8 | 4 | PROCESSED | 57545.7503587963 | 55330 | 54908.5588310185 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030106 | We propose to observe a peculiar Intermediate Polar, RX J1712.6-2414, which has no accretion disk around the white dwarf. This source shows the X-ray modulation only at the beat period and broad Fe-K emission lines in the phase-averaged spectrum. Our goal is to obtain a clear picture about the accretion flow geometry, which can explain the timing and spectral properties, utilizing the fine phase-resolved spectra. Furthermore, we examine the non-thermal emission from the source, since the magnetized white dwarf is a promising candidate of particle acceleration sites. | GALACTIC POINT SOURCES | 4 | B | MORI | HIDEYUKI | NULL | NULL | JAP | 3 | AO3 | ACCRETION FLOW AND EMISSION MECHANISM OF A DISKLESS INTERMEDIATE POLAR, RX J1712.6-2414 | XIS | Y |
| YY DRA | 175.8686 | 71.6187 | 130.35712902 | 44.51671754 | 282.0676 | 54632.7758217593 | 54633.4098842593 | 403022010 | 29185.1 | 30000 | 29185.1 | 29185.1 | 0 | 29185.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27474.3 | 27474.3 | 54777.9 | 1 | PROCESSED | 57542.8240509259 | 55013 | 54644.1517592593 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030107 | We propose observations of 5 Intermediate Polars, a subcategory of magnetic CVs, as the first step toward establishment of an averaged hard X-ray spectrum of IPs that exist near the Solar system.The averaged spectrum should be compared with that of the Galactic Diffese X-ray Emssion (GDXE), to investigate the claimed spectral resemblance between them in energies above 10 keV. If the averaged IP spectrum shows any discrepancy with that of the GDXE, the "point-source origin" explanation for the GDXE would face a lack of appropriate hard X-ray source populations. This in turn is expected to strengthen the competing "truly diffuse origin"explanation, which attributes the GDXE hard X-rays to non thermal emission from electrons being accelerated in the interstellar space. | GALACTIC POINT SOURCES | 4 | C | YUASA | TAKAYUKI | NULL | NULL | JAP | 3 | AO3 | SURVEY OBSERVATION OF INTERMEDIATE POLARS | HXD | Y |
| TV COL | 82.3326 | -32.8641 | 236.83580562 | -30.63495041 | 295.9146 | 54573.7555555556 | 54574.6668634259 | 403023010 | 35836.7 | 40000 | 35836.7 | 35836.7 | 0 | 35836.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30102.3 | 30102.3 | 78729.9 | 0 | PROCESSED | 57542.3393055556 | 54953 | 54587.0666550926 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030107 | We propose observations of 5 Intermediate Polars, a subcategory of magnetic CVs, as the first step toward establishment of an averaged hard X-ray spectrum of IPs that exist near the Solar system.The averaged spectrum should be compared with that of the Galactic Diffese X-ray Emssion (GDXE), to investigate the claimed spectral resemblance between them in energies above 10 keV. If the averaged IP spectrum shows any discrepancy with that of the GDXE, the "point-source origin" explanation for the GDXE would face a lack of appropriate hard X-ray source populations. This in turn is expected to strengthen the competing "truly diffuse origin"explanation, which attributes the GDXE hard X-rays to non thermal emission from electrons being accelerated in the interstellar space. | GALACTIC POINT SOURCES | 4 | C | YUASA | TAKAYUKI | NULL | NULL | JAP | 3 | AO3 | SURVEY OBSERVATION OF INTERMEDIATE POLARS | HXD | Y |
| IGR J16194-2810 | 244.8908 | -28.0663 | 349.1669856 | 15.58223604 | 95.1879 | 54867.1762152778 | 54868.4314236111 | 403024010 | 45568.7 | 50000 | 45568.7 | 45573.8 | 0 | 45568.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38785.9 | 38785.9 | 108435.8 | 1 | PROCESSED | 57545.4895023148 | 55329 | 54880.5743518518 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030121 | We propose to observe the weakly magnetized neutron star X-ray binary, IGR J16194-2810. This target object has almost constant luminosity and is expected to be state of ADAF. Assuming that we observe the object using HXD and XIS of the Suzaku for 50ks, we can investigate the soft X-ray emission from the NS and/or the accretion disk and hard X-ray tail. Comparing Black Body and Disk Black Body parameters of this object with that of fainter source, 4U 1700+24, we obtain a picture of accretion disk and accretion flow. If we measure the photon index and cutoff energy of the hard tail, we can reveal the physical condition of corona surrounding the NS or the disk. Only Suzaku can carry out this observation which observe soft-thermal and hard-nonthermal X-ray emission from faint source. | GALACTIC POINT SOURCES | 4 | C | NAGAE | OSAMU | NULL | NULL | JAP | 3 | AO3 | ELUCIDATION OF THE ADAF OBSERVING LOW LUMINOUS NEUTRON STAR X-RAY BINARY IGR J16194-2810 | HXD | Y |
| V709 CAS | 7.1951 | 59.3013 | 120.03837674 | -3.44309479 | 84.0816 | 54637.4334837963 | 54638.1542824074 | 403025010 | 35898.2 | 30000 | 35898.2 | 35898.2 | 0 | 35898.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 33382.3 | 33382.3 | 62267.9 | 0 | PROCESSED | 57542.8811921296 | 55014 | 54648.3358101852 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030140 | Origin of the Galactic Ridge X-ray Emission (GRXE) has been a significant problem in X-ray astronomy for over 20 years. The GRXE has a hard-tail above ~15 keV, which was considered to be an evidence of non-thermal cosmic-ray interaction. On the other hand, Suzaku recently revealed that the GRXE iron line feature is composed of three narrow emission lines, whose origin is unknown yet. Recently, INTEGRAL discovered dozens of previously unknown cataclysmic variables (CVs) which are bright above ~15 keV, while their spectral characteristics below 10 keV are hardly known. If there are a large number of such hard CVs, they may account for ~100 % of the GRXE above ~15 keV. If so, these sources should have similar iron line feature as the GRXE, which we are proposing to investigate. | GALACTIC POINT SOURCES | 4 | B | EBISAWA | KEN | NULL | NULL | JAP | 3 | AO3 | IRON LINE SPECTROSCOPY OF THE HARD CATACLYSMIC VARIABLES DISCOVERED BY INTEGRAL | XIS | Y |
| IGR J17303-0601 | 262.5864 | -5.9814 | 17.93788623 | 15.02149808 | 100.7922 | 54878.4233217593 | 54879.3355787037 | 403026010 | 32963.5 | 30000 | 32963.5 | 32963.5 | 0 | 32963.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27755.9 | 27755.9 | 78818 | 2 | PROCESSED | 57545.5746990741 | 55325 | 54893.4381018518 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030140 | Origin of the Galactic Ridge X-ray Emission (GRXE) has been a significant problem in X-ray astronomy for over 20 years. The GRXE has a hard-tail above ~15 keV, which was considered to be an evidence of non-thermal cosmic-ray interaction. On the other hand, Suzaku recently revealed that the GRXE iron line feature is composed of three narrow emission lines, whose origin is unknown yet. Recently, INTEGRAL discovered dozens of previously unknown cataclysmic variables (CVs) which are bright above ~15 keV, while their spectral characteristics below 10 keV are hardly known. If there are a large number of such hard CVs, they may account for ~100 % of the GRXE above ~15 keV. If so, these sources should have similar iron line feature as the GRXE, which we are proposing to investigate. | GALACTIC POINT SOURCES | 4 | B | EBISAWA | KEN | NULL | NULL | JAP | 3 | AO3 | IRON LINE SPECTROSCOPY OF THE HARD CATACLYSMIC VARIABLES DISCOVERED BY INTEGRAL | XIS | Y |
| RX J1940.1-1025 | 295.0445 | -10.4193 | 28.98688715 | -15.49869645 | 79.7405 | 54572.8979976852 | 54573.743275463 | 403027010 | 32453.6 | 30000 | 32453.6 | 32453.6 | 0 | 32453.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26465.7 | 26465.7 | 73021.9 | 2 | PROCESSED | 57542.3241087963 | 54953 | 54587.0481481482 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030140 | Origin of the Galactic Ridge X-ray Emission (GRXE) has been a significant problem in X-ray astronomy for over 20 years. The GRXE has a hard-tail above ~15 keV, which was considered to be an evidence of non-thermal cosmic-ray interaction. On the other hand, Suzaku recently revealed that the GRXE iron line feature is composed of three narrow emission lines, whose origin is unknown yet. Recently, INTEGRAL discovered dozens of previously unknown cataclysmic variables (CVs) which are bright above ~15 keV, while their spectral characteristics below 10 keV are hardly known. If there are a large number of such hard CVs, they may account for ~100 % of the GRXE above ~15 keV. If so, these sources should have similar iron line feature as the GRXE, which we are proposing to investigate. | GALACTIC POINT SOURCES | 4 | B | EBISAWA | KEN | NULL | NULL | JAP | 3 | AO3 | IRON LINE SPECTROSCOPY OF THE HARD CATACLYSMIC VARIABLES DISCOVERED BY INTEGRAL | XIS | Y |
| IGR J17195-4100 | 259.8947 | -41.0152 | 346.97641748 | -2.13400756 | 97.0631 | 54880.4607175926 | 54881.3106481482 | 403028010 | 31645.6 | 30000 | 31645.6 | 31645.6 | 0 | 31645.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26917.8 | 26917.8 | 73428 | 0 | PROCESSED | 57545.5868981482 | 55330 | 54895.5494328704 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030140 | Origin of the Galactic Ridge X-ray Emission (GRXE) has been a significant problem in X-ray astronomy for over 20 years. The GRXE has a hard-tail above ~15 keV, which was considered to be an evidence of non-thermal cosmic-ray interaction. On the other hand, Suzaku recently revealed that the GRXE iron line feature is composed of three narrow emission lines, whose origin is unknown yet. Recently, INTEGRAL discovered dozens of previously unknown cataclysmic variables (CVs) which are bright above ~15 keV, while their spectral characteristics below 10 keV are hardly known. If there are a large number of such hard CVs, they may account for ~100 % of the GRXE above ~15 keV. If so, these sources should have similar iron line feature as the GRXE, which we are proposing to investigate. | GALACTIC POINT SOURCES | 4 | B | EBISAWA | KEN | NULL | NULL | JAP | 3 | AO3 | IRON LINE SPECTROSCOPY OF THE HARD CATACLYSMIC VARIABLES DISCOVERED BY INTEGRAL | XIS | Y |
| XSS J12270-4859 | 187.002 | -48.8936 | 298.97017898 | 13.79783482 | 315.9792 | 54686.9674421296 | 54687.6480787037 | 403029010 | 29623.2 | 30000 | 29623.2 | 29623.2 | 0 | 29623.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34580 | 34580 | 58791.9 | 0 | PROCESSED | 57543.2069907407 | 55073 | 54707.1730208333 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030140 | Origin of the Galactic Ridge X-ray Emission (GRXE) has been a significant problem in X-ray astronomy for over 20 years. The GRXE has a hard-tail above ~15 keV, which was considered to be an evidence of non-thermal cosmic-ray interaction. On the other hand, Suzaku recently revealed that the GRXE iron line feature is composed of three narrow emission lines, whose origin is unknown yet. Recently, INTEGRAL discovered dozens of previously unknown cataclysmic variables (CVs) which are bright above ~15 keV, while their spectral characteristics below 10 keV are hardly known. If there are a large number of such hard CVs, they may account for ~100 % of the GRXE above ~15 keV. If so, these sources should have similar iron line feature as the GRXE, which we are proposing to investigate. | GALACTIC POINT SOURCES | 4 | B | EBISAWA | KEN | NULL | NULL | JAP | 3 | AO3 | IRON LINE SPECTROSCOPY OF THE HARD CATACLYSMIC VARIABLES DISCOVERED BY INTEGRAL | XIS | Y |
| WR140 | 305.2159 | 43.8446 | 80.96257668 | 4.11237193 | 190.1825 | 54844.5415162037 | 54846.500162037 | 403030010 | 89406.8 | 80000 | 89406.8 | 89406.8 | 0 | 89406.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 78055.7 | 78055.7 | 169196.9 | 1 | PROCESSED | 57545.2609606482 | 55328 | 54861.8550115741 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030157 | WR 140 (WC7+O4I) is a long-period (P=7.94 yrs), extremely eccentric (e=0.88) massive binary. Winds from each star collide and produce strong changes in the X-ray spectrum and the production of thick dust shells. All the orbital and stellar parameters are measured, so WR 140 is the best shock-physics laboratory known. X-ray observations are crucial to understand the hot shocked gas and the mass loss phenomena. WR140's next periastron passage is in Jan. 2009. We propose a series of Suzaku observations to precisely determine the change in the X-ray emitting plasma and in the cool absorbing wind from the WC7 star, and the amount of hard X-ray emission (E>20 keV) from particle acceleration in the shock. This may be the only opportunity to observe a periastron passage of WR 140 with Suzaku. | GALACTIC POINT SOURCES | 4 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 3 | AO3 | X-RAYING THE PERIASTRON PASSAGE OF THE CANONICAL, LONG PERIOD COLLIDING WIND LABORATORY, WR140 | HXD | Y |
| WR140 | 305.211 | 43.8318 | 80.94998516 | 4.10805919 | 199.7371 | 54835.3583449074 | 54836.4252199074 | 403031010 | 47266.4 | 40000 | 47266.4 | 47266.4 | 0 | 47282.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45303 | 45303 | 92161.8 | 0 | PROCESSED | 57545.1036921296 | 55328 | 54850.2164583333 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030157 | WR 140 (WC7+O4I) is a long-period (P=7.94 yrs), extremely eccentric (e=0.88) massive binary. Winds from each star collide and produce strong changes in the X-ray spectrum and the production of thick dust shells. All the orbital and stellar parameters are measured, so WR 140 is the best shock-physics laboratory known. X-ray observations are crucial to understand the hot shocked gas and the mass loss phenomena. WR140's next periastron passage is in Jan. 2009. We propose a series of Suzaku observations to precisely determine the change in the X-ray emitting plasma and in the cool absorbing wind from the WC7 star, and the amount of hard X-ray emission (E>20 keV) from particle acceleration in the shock. This may be the only opportunity to observe a periastron passage of WR 140 with Suzaku. | GALACTIC POINT SOURCES | 4 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 3 | AO3 | X-RAYING THE PERIASTRON PASSAGE OF THE CANONICAL, LONG PERIOD COLLIDING WIND LABORATORY, WR140 | HXD | Y |
| WR140 | 305.1942 | 43.809 | 80.92425741 | 4.10518752 | 220.5408 | 54812.4360069444 | 54813.5523148148 | 403032010 | 52910.6 | 40000 | 52910.6 | 52910.6 | 0 | 52910.6 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 48260.9 | 48260.9 | 96431.8 | 0 | PROCESSED | 57544.9612847222 | 55192 | 54826.2481365741 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030157 | WR 140 (WC7+O4I) is a long-period (P=7.94 yrs), extremely eccentric (e=0.88) massive binary. Winds from each star collide and produce strong changes in the X-ray spectrum and the production of thick dust shells. All the orbital and stellar parameters are measured, so WR 140 is the best shock-physics laboratory known. X-ray observations are crucial to understand the hot shocked gas and the mass loss phenomena. WR140's next periastron passage is in Jan. 2009. We propose a series of Suzaku observations to precisely determine the change in the X-ray emitting plasma and in the cool absorbing wind from the WC7 star, and the amount of hard X-ray emission (E>20 keV) from particle acceleration in the shock. This may be the only opportunity to observe a periastron passage of WR 140 with Suzaku. | GALACTIC POINT SOURCES | 4 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 3 | AO3 | X-RAYING THE PERIASTRON PASSAGE OF THE CANONICAL, LONG PERIOD COLLIDING WIND LABORATORY, WR140 | HXD | Y |
| WR140 | 305.1135 | 43.9272 | 80.98919394 | 4.21991141 | 90.2945 | 54565.231400463 | 54565.7224305556 | 403033010 | 21625.3 | 20000 | 21625.3 | 21625.3 | 0 | 21625.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18605.5 | 18605.5 | 42415.9 | 2 | PROCESSED | 57542.2656828704 | 54953 | 54580.4185648148 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030157 | WR 140 (WC7+O4I) is a long-period (P=7.94 yrs), extremely eccentric (e=0.88) massive binary. Winds from each star collide and produce strong changes in the X-ray spectrum and the production of thick dust shells. All the orbital and stellar parameters are measured, so WR 140 is the best shock-physics laboratory known. X-ray observations are crucial to understand the hot shocked gas and the mass loss phenomena. WR140's next periastron passage is in Jan. 2009. We propose a series of Suzaku observations to precisely determine the change in the X-ray emitting plasma and in the cool absorbing wind from the WC7 star, and the amount of hard X-ray emission (E>20 keV) from particle acceleration in the shock. This may be the only opportunity to observe a periastron passage of WR 140 with Suzaku. | GALACTIC POINT SOURCES | 4 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 3 | AO3 | X-RAYING THE PERIASTRON PASSAGE OF THE CANONICAL, LONG PERIOD COLLIDING WIND LABORATORY, WR140 | HXD | Y |
| TAU SCO | 248.9714 | -28.2185 | 351.53328031 | 12.80600635 | 277.9748 | 54710.0436689815 | 54710.3697222222 | 403034010 | 14617.1 | 10000 | 14617.1 | 14617.1 | 0 | 14617.1 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12085.5 | 12085.5 | 28135.9 | 0 | PROCESSED | 57543.4427777778 | 55148 | 54780.4170138889 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031121 | We are proposing to observe the magnetic hot star tau Sco (B0.2V) with six Suzaku pointings of 10 ksec each. This star has a highly structured surface magnetic field at around 500 G, and its unusually hard emission has been associated with wind confinement in closed magnetic loops. Our proposal is to test this claim. The surface field sports a torus-like structure of closed loops with a magnetic axis that is tilted by nearly 90 degrees from the stellar rotation axis. We selected six phases to optimize the detection of hard X-ray variability from occultation of hot plasma confined in the torus field arrangement as it rotates about the star. The Suzaku data will be important for confronting models of interactions between line-driven winds and magnetic fields in massive stars. | GALACTIC POINT SOURCES | 4 | A | IGNACE | RICHARD | NULL | NULL | USA | 3 | AO3 | X-RAYS FROM MAGNETICALLY CONFINED HOT PLASMA IN TAU SCO | XIS | Y |
| TAU SCO | 248.9731 | -28.2173 | 351.53521528 | 12.80565459 | 288.7028 | 54717.0750115741 | 54717.3752777778 | 403034020 | 14521.5 | 10000 | 14529.5 | 14521.5 | 0 | 14537.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9652.4 | 9652.4 | 25935.9 | 1 | PROCESSED | 57543.7784606482 | 55148 | 54780.6118171296 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031121 | We are proposing to observe the magnetic hot star tau Sco (B0.2V) with six Suzaku pointings of 10 ksec each. This star has a highly structured surface magnetic field at around 500 G, and its unusually hard emission has been associated with wind confinement in closed magnetic loops. Our proposal is to test this claim. The surface field sports a torus-like structure of closed loops with a magnetic axis that is tilted by nearly 90 degrees from the stellar rotation axis. We selected six phases to optimize the detection of hard X-ray variability from occultation of hot plasma confined in the torus field arrangement as it rotates about the star. The Suzaku data will be important for confronting models of interactions between line-driven winds and magnetic fields in massive stars. | GALACTIC POINT SOURCES | 4 | A | IGNACE | RICHARD | NULL | NULL | USA | 3 | AO3 | X-RAYS FROM MAGNETICALLY CONFINED HOT PLASMA IN TAU SCO | XIS | Y |
| TAU SCO | 248.9736 | -28.2151 | 351.53721955 | 12.80675658 | 279.3712 | 54723.4207291667 | 54723.8119675926 | 403034030 | 12290.2 | 10000 | 12298.2 | 12298.2 | 0 | 12290.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11028.2 | 11028.2 | 33799.9 | 0 | PROCESSED | 57543.8133564815 | 55148 | 54780.4631597222 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031121 | We are proposing to observe the magnetic hot star tau Sco (B0.2V) with six Suzaku pointings of 10 ksec each. This star has a highly structured surface magnetic field at around 500 G, and its unusually hard emission has been associated with wind confinement in closed magnetic loops. Our proposal is to test this claim. The surface field sports a torus-like structure of closed loops with a magnetic axis that is tilted by nearly 90 degrees from the stellar rotation axis. We selected six phases to optimize the detection of hard X-ray variability from occultation of hot plasma confined in the torus field arrangement as it rotates about the star. The Suzaku data will be important for confronting models of interactions between line-driven winds and magnetic fields in massive stars. | GALACTIC POINT SOURCES | 4 | A | IGNACE | RICHARD | NULL | NULL | USA | 3 | AO3 | X-RAYS FROM MAGNETICALLY CONFINED HOT PLASMA IN TAU SCO | XIS | Y |
| TAU SCO | 248.9733 | -28.218 | 351.53478934 | 12.80506422 | 280.0312 | 54729.4179398148 | 54729.7578009259 | 403034040 | 13971.1 | 10000 | 13971.1 | 13971.1 | 0 | 13971.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12891.2 | 12891.2 | 29350 | 0 | PROCESSED | 57543.857974537 | 55148 | 54780.4954050926 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031121 | We are proposing to observe the magnetic hot star tau Sco (B0.2V) with six Suzaku pointings of 10 ksec each. This star has a highly structured surface magnetic field at around 500 G, and its unusually hard emission has been associated with wind confinement in closed magnetic loops. Our proposal is to test this claim. The surface field sports a torus-like structure of closed loops with a magnetic axis that is tilted by nearly 90 degrees from the stellar rotation axis. We selected six phases to optimize the detection of hard X-ray variability from occultation of hot plasma confined in the torus field arrangement as it rotates about the star. The Suzaku data will be important for confronting models of interactions between line-driven winds and magnetic fields in massive stars. | GALACTIC POINT SOURCES | 4 | A | IGNACE | RICHARD | NULL | NULL | USA | 3 | AO3 | X-RAYS FROM MAGNETICALLY CONFINED HOT PLASMA IN TAU SCO | XIS | Y |
| TAU SCO | 248.9722 | -28.2177 | 351.53437371 | 12.80599439 | 271.5181 | 54696.3145833333 | 54696.6675810185 | 403034050 | 16313.6 | 10000 | 16350.4 | 16313.6 | 0 | 16358.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13967 | 13967 | 30472 | 0 | PROCESSED | 57543.3225694444 | 55084 | 54713.1924189815 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031121 | We are proposing to observe the magnetic hot star tau Sco (B0.2V) with six Suzaku pointings of 10 ksec each. This star has a highly structured surface magnetic field at around 500 G, and its unusually hard emission has been associated with wind confinement in closed magnetic loops. Our proposal is to test this claim. The surface field sports a torus-like structure of closed loops with a magnetic axis that is tilted by nearly 90 degrees from the stellar rotation axis. We selected six phases to optimize the detection of hard X-ray variability from occultation of hot plasma confined in the torus field arrangement as it rotates about the star. The Suzaku data will be important for confronting models of interactions between line-driven winds and magnetic fields in massive stars. | GALACTIC POINT SOURCES | 4 | A | IGNACE | RICHARD | NULL | NULL | USA | 3 | AO3 | X-RAYS FROM MAGNETICALLY CONFINED HOT PLASMA IN TAU SCO | XIS | Y |
| TAU SCO | 248.9729 | -28.218 | 351.53455344 | 12.80533126 | 274.2608 | 54703.1981597222 | 54703.5447222222 | 403034060 | 15018.3 | 10000 | 15026.3 | 15034.3 | 0 | 15018.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12904.9 | 12904.9 | 29911.9 | 0 | PROCESSED | 57543.3841898148 | 55084 | 54713.2754976852 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031121 | We are proposing to observe the magnetic hot star tau Sco (B0.2V) with six Suzaku pointings of 10 ksec each. This star has a highly structured surface magnetic field at around 500 G, and its unusually hard emission has been associated with wind confinement in closed magnetic loops. Our proposal is to test this claim. The surface field sports a torus-like structure of closed loops with a magnetic axis that is tilted by nearly 90 degrees from the stellar rotation axis. We selected six phases to optimize the detection of hard X-ray variability from occultation of hot plasma confined in the torus field arrangement as it rotates about the star. The Suzaku data will be important for confronting models of interactions between line-driven winds and magnetic fields in massive stars. | GALACTIC POINT SOURCES | 4 | A | IGNACE | RICHARD | NULL | NULL | USA | 3 | AO3 | X-RAYS FROM MAGNETICALLY CONFINED HOT PLASMA IN TAU SCO | XIS | Y |
| ETA CARINAE | 161.2297 | -59.7314 | 287.60304523 | -0.67930865 | 294 | 54627.0775 | 54627.649525463 | 403035010 | 35447.9 | 30000 | 35463.9 | 35447.9 | 0 | 35463.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27210.2 | 27210.2 | 49415.9 | 1 | PROCESSED | 57542.7628819445 | 55003 | 54637.2680092593 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031124 | X-ray observations of Eta Carinae near the 2003 periastron passage confirmed that the X-ray emission primarily arises from collision of winds in a binary system, but raised fundamental questions about the cause of the 3 month-long X-ray minimum and an excess above ~10 keV (possibly up to 50 keV) in addition to the thermal emission with kT ~3-5 keV. These features would originate from plasma extremely embedded in the primary winds and acceleration of high energy particles at the wind colliding region. To resolve these features clearly, broad band Suzaku observations around the periastron passage are crucial. We propose four 30 ksec Suzaku observations of Eta Carinae during AO3, which will cover the next X-ray maximum (in late 2008) and minimum (in early 2009). | GALACTIC POINT SOURCES | 4 | A | HAMAGUCHI | KENJI | NULL | NULL | USA | 3 | AO3 | X-RAY EMISSION FROM ETA CARINAE DURING THE X-RAY MAXIMUM AND MINIMUM | HXD | Y |
| ETA CARINAE | 161.2769 | -59.635 | 287.57915278 | -0.58292483 | 99.9027 | 54810.21125 | 54811.2084953704 | 403036010 | 48501.6 | 30000 | 48501.6 | 48501.6 | 0 | 48501.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42425.9 | 42425.9 | 86151.8 | 2 | PROCESSED | 57544.6853125 | 55198 | 54828.3640972222 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031124 | X-ray observations of Eta Carinae near the 2003 periastron passage confirmed that the X-ray emission primarily arises from collision of winds in a binary system, but raised fundamental questions about the cause of the 3 month-long X-ray minimum and an excess above ~10 keV (possibly up to 50 keV) in addition to the thermal emission with kT ~3-5 keV. These features would originate from plasma extremely embedded in the primary winds and acceleration of high energy particles at the wind colliding region. To resolve these features clearly, broad band Suzaku observations around the periastron passage are crucial. We propose four 30 ksec Suzaku observations of Eta Carinae during AO3, which will cover the next X-ray maximum (in late 2008) and minimum (in early 2009). | GALACTIC POINT SOURCES | 4 | A | HAMAGUCHI | KENJI | NULL | NULL | USA | 3 | AO3 | X-RAY EMISSION FROM ETA CARINAE DURING THE X-RAY MAXIMUM AND MINIMUM | HXD | Y |
| ETA CARINAE | 161.3407 | -59.6518 | 287.61551185 | -0.58277566 | 142.0006 | 54856.1332291667 | 54856.6821064815 | 403037010 | 28805.3 | 30000 | 28805.3 | 28805.3 | 0 | 28805.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17453.9 | 17453.9 | 47407.9 | 0 | PROCESSED | 57545.3235185185 | 55328 | 54880.533587963 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031124 | X-ray observations of Eta Carinae near the 2003 periastron passage confirmed that the X-ray emission primarily arises from collision of winds in a binary system, but raised fundamental questions about the cause of the 3 month-long X-ray minimum and an excess above ~10 keV (possibly up to 50 keV) in addition to the thermal emission with kT ~3-5 keV. These features would originate from plasma extremely embedded in the primary winds and acceleration of high energy particles at the wind colliding region. To resolve these features clearly, broad band Suzaku observations around the periastron passage are crucial. We propose four 30 ksec Suzaku observations of Eta Carinae during AO3, which will cover the next X-ray maximum (in late 2008) and minimum (in early 2009). | GALACTIC POINT SOURCES | 4 | A | HAMAGUCHI | KENJI | NULL | NULL | USA | 3 | AO3 | X-RAY EMISSION FROM ETA CARINAE DURING THE X-RAY MAXIMUM AND MINIMUM | HXD | Y |
| ETA CARINAE | 161.3639 | -59.6742 | 287.63630523 | -0.59715454 | 170.6228 | 54877.528287037 | 54878.4119675926 | 403038010 | 35552.5 | 30000 | 35568.5 | 35552.5 | 0 | 35560.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 31119.3 | 31119.3 | 76323.9 | 1 | PROCESSED | 57545.5564814815 | 55328 | 54893.4307407407 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031124 | X-ray observations of Eta Carinae near the 2003 periastron passage confirmed that the X-ray emission primarily arises from collision of winds in a binary system, but raised fundamental questions about the cause of the 3 month-long X-ray minimum and an excess above ~10 keV (possibly up to 50 keV) in addition to the thermal emission with kT ~3-5 keV. These features would originate from plasma extremely embedded in the primary winds and acceleration of high energy particles at the wind colliding region. To resolve these features clearly, broad band Suzaku observations around the periastron passage are crucial. We propose four 30 ksec Suzaku observations of Eta Carinae during AO3, which will cover the next X-ray maximum (in late 2008) and minimum (in early 2009). | GALACTIC POINT SOURCES | 4 | A | HAMAGUCHI | KENJI | NULL | NULL | USA | 3 | AO3 | X-RAY EMISSION FROM ETA CARINAE DURING THE X-RAY MAXIMUM AND MINIMUM | HXD | Y |
| ASAS J002511+1217.2 | 6.2997 | 12.2847 | 112.91544003 | -50.07604687 | 234.9156 | 54841.6813773148 | 54842.5468055556 | 403039010 | 33256 | 30000 | 33256 | 33256 | 0 | 33256 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 29873 | 29873 | 74752 | 1 | PROCESSED | 57545.1348726852 | 55328 | 54851.4143055556 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031144 | Dwarf Novae, the most numerous subclass of cataclysmic variables, are important contributors to the unresolved X-ray emissions from the Galactic disk and the bulge. However, current estimates of the integrated X-ray luminosity of dwarf novae are highly uncertain and are based on samples that may contain significant biases. We need to obtain an unbiased X-ray luminosity function of dwarf novae to estimate the true contribution of dwarf novae to the unresolved Galactic X-ray emission. Here we propose to continue our ongoing program to observe dwarf novae with secure, parallax-based distance estimates. | GALACTIC POINT SOURCES | 4 | C | MUKAI | KOJI | NULL | NULL | USA | 3 | AO3 | BUILDING UP AND UNBIASED X-RAY LUMINOSITY FUNCTION OF DWARF NOVAE: A CONTINUATION IN SUZAKU CYCLE 3 | XIS | Y |
| KT PER | 24.2933 | 50.9468 | 130.24865907 | -11.27406186 | 260.9001 | 54843.8957060185 | 54844.5334953704 | 403041010 | 29195.7 | 20000 | 29195.7 | 29195.7 | 0 | 29195.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28165.8 | 28165.8 | 55089.9 | 0 | PROCESSED | 57545.1649537037 | 55328 | 54854.0547916667 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031144 | Dwarf Novae, the most numerous subclass of cataclysmic variables, are important contributors to the unresolved X-ray emissions from the Galactic disk and the bulge. However, current estimates of the integrated X-ray luminosity of dwarf novae are highly uncertain and are based on samples that may contain significant biases. We need to obtain an unbiased X-ray luminosity function of dwarf novae to estimate the true contribution of dwarf novae to the unresolved Galactic X-ray emission. Here we propose to continue our ongoing program to observe dwarf novae with secure, parallax-based distance estimates. | GALACTIC POINT SOURCES | 4 | C | MUKAI | KOJI | NULL | NULL | USA | 3 | AO3 | BUILDING UP AND UNBIASED X-RAY LUMINOSITY FUNCTION OF DWARF NOVAE: A CONTINUATION IN SUZAKU CYCLE 3 | XIS | Y |
| SS73 17 | 152.7399 | -57.7545 | 282.81739372 | -1.29143094 | 80.1552 | 54775.6877430556 | 54776.3072453704 | 403043010 | 24907 | 20000 | 24907 | 24907 | 0 | 24907 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20809.1 | 20809.1 | 53519.9 | 0 | PROCESSED | 57544.3629282407 | 55157 | 54791.6362847222 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031145 | SS73 17 was an innocuous Mira-type symbiotic star until INTEGRAL and Swift discovered its bright hard X-ray emission. Suzaku observations showed it emits three bright iron lines, with almost no emission in the 0.5-2 keV bandpass. The PI has an approved 100 ksec Chandra HETG observation in 2008 to determine the origin of the iron lines and measure any weak emission lines. With simultaneous Suzaku observations we will also measure the hard X-ray emission from the source, both to constrain the continuum and detect any non-thermal component. The effective areas of the XIS and HXD will constrain the broadband emission process much better than the HETG data. Combined with simultaneous optical observations of the Mira-type star we will determine the origin of this star's unusual emission. | GALACTIC POINT SOURCES | 4 | A | SMITH | RANDALL | NULL | NULL | USA | 3 | AO3 | SIMULTANEOUS MULTIWAVELENGTH OBSERVATIONS OF THE SYMBIOTIC STAR SS73 17 | HXD | Y |
| GX 301-2 | 186.5611 | -62.8021 | 300.05773343 | -0.07103063 | 326.712 | 54703.5522800926 | 54704.0036689815 | 403044010 | 11427.5 | 60000 | 11429.2 | 11430.6 | 0 | 11427.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10714.8 | 10714.8 | 38993.9 | 0 | PROCESSED | 57543.3977546296 | 55218 | 54720.435462963 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031152 | We propose the first observation of the bright neutron star GX 301-2 with Suzaku. The aim of the proposed 60 ks observation is a study of the broadband spectrum of the source in unprecedented detail and quality. This will allow us to analyze the structure (including density and clumpiness) of the intense wind of the optical companion and the gas stream flowing from Wray 977 to the neutron star. Spectral data will be used to study the evolution of nH and the iron line with very high time resolution. Furthermore, we will perform phase resolved spectroscopy to study the spectral variation of the cyclotron line with pulse phase. | GALACTIC POINT SOURCES | 4 | A | ROTHSCHILD | RICHARD | NULL | NULL | USA | 3 | AO3 | BROAD-BAND STUDY OF GX 301-2 | HXD | Y |
| GX 301-2 | 186.689 | -62.7212 | 300.10817936 | 0.01514837 | 109.0098 | 54836.4396296296 | 54838.0419328704 | 403044020 | 61813.6 | 50000 | 61813.6 | 61813.6 | 0 | 61813.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 54992.2 | 54992.2 | 138398.1 | 2 | PROCESSED | 57545.1371064815 | 55328 | 54851.4303125 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031152 | We propose the first observation of the bright neutron star GX 301-2 with Suzaku. The aim of the proposed 60 ks observation is a study of the broadband spectrum of the source in unprecedented detail and quality. This will allow us to analyze the structure (including density and clumpiness) of the intense wind of the optical companion and the gas stream flowing from Wray 977 to the neutron star. Spectral data will be used to study the evolution of nH and the iron line with very high time resolution. Furthermore, we will perform phase resolved spectroscopy to study the spectral variation of the cyclotron line with pulse phase. | GALACTIC POINT SOURCES | 4 | A | ROTHSCHILD | RICHARD | NULL | NULL | USA | 3 | AO3 | BROAD-BAND STUDY OF GX 301-2 | HXD | Y |
| VELA X-1 | 135.5377 | -40.5514 | 263.06039339 | 3.93722667 | 314.5441 | 54634.1981134259 | 54635.9043287037 | 403045010 | 104709.6 | 100000 | 104723.4 | 104709.6 | 0 | 104715.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 96008.9 | 96008.9 | 147389.9 | 1 | PROCESSED | 57542.8859375 | 55010 | 54644.4687847222 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031153 | We propose to observe the well-known X-ray pulsar Vela X-1 (4U0900-40) using Suzaku in order to test models for the circumstellar environment by measuring teh spectrum and searching for variability in the iron line. The line is expected to exhibit changes in intensity and centroid energy as the X-ray beam sweeps around the wind an illuminates material with varying column density, ionization state, and vleocity. In addition we will study the variability in the cyclotron feature. We will compare our observations with detailed hydrodynamical simulations of the stellar wind and its interaction with the compact object. | GALACTIC POINT SOURCES | 4 | A | KALLMAN | TIMOTHY | NULL | NULL | USA | 3 | AO3 | SPECTROSCOPY OF VELA X-1 (4U0900-40) AND SEARCHES FOR PULSE PHASE VARIABILITY | XIS | Y |
| CENTAURUS X-3 | 170.3244 | -60.5721 | 292.07802241 | 0.38603209 | 97.3521 | 54808.2886111111 | 54810.2085532407 | 403046010 | 97587.1 | 90000 | 97587.1 | 97587.1 | 0 | 97587.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 79656.2 | 79656.2 | 165853.7 | 0 | PROCESSED | 57544.7036805556 | 55188 | 54822.6243634259 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031154 | We ask for a 90 ks observation (which will be performed within typically 180 ks taking Suzaku's duty cycle into account) of the accreting HMXB Centaurus X-3 to conduct the most sensitive study to date of the wide range of changes of its broad band spectrum over one 2.1 binary orbit and with pulse phase. Especially we will determine the evolution of the hydrogen absorption column over the orbit and test whether signatures of the tidal wake observed with RXTE can be confirmed. The variable Fe line complex will be studied. The cyclotron resonance scattering feature of Cen X-3 at ~30 keV is especially well suited to test new physical models describing phase-resolved line profiles, since it is very variable over the pulse, with the line centroid spanning an energy range from 28 to 39 keV. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 3 | AO3 | THE BROAD BAND SPECTRUM OF CEN X-3 OVER ORBIT AND PULSE PHASE | HXD | Y |
| 1A1118-61 | 170.3073 | -61.878 | 292.515895 | -0.84430143 | 131.7127 | 54846.5144328704 | 54847.9029976852 | 403049010 | 49667.4 | 45000 | 49667.4 | 49667.4 | 0 | 49667.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46815.9 | 46815.9 | 119953.8 | 0 | PROCESSED | 57545.2346296296 | 55328 | 54858.6603125 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031155 | We propose to perform Target of Opportunity Observations of one accreting neutron star in outburst during Suzaku AO3. The aim of the observations is to observe the source at a level of 40 and 200mCrab, to determine the properties of the cyclotron line in this system and to determine its broad band spectrum. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 3 | AO3-TOO | SEARCHING FOR CYCLOTRON RESONANCE SCATTERING FEATURES IN TRANSIENT ACCRETING X-RAY PULSARS WITH SUZAKU | HXD | Y |
| 1A1118-61 | 170.3215 | -61.8847 | 292.5244731 | -0.84831529 | 142.606 | 54859.2344328704 | 54859.8925810185 | 403050010 | 44212.5 | 45000 | 44212.5 | 44212.5 | 0 | 44212.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30915.4 | 30915.4 | 56859.9 | 0 | PROCESSED | 57545.3633680556 | 55328 | 54880.5326273148 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031155 | We propose to perform Target of Opportunity Observations of one accreting neutron star in outburst during Suzaku AO3. The aim of the observations is to observe the source at a level of 40 and 200mCrab, to determine the properties of the cyclotron line in this system and to determine its broad band spectrum. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 3 | AO3-TOO | SEARCHING FOR CYCLOTRON RESONANCE SCATTERING FEATURES IN TRANSIENT ACCRETING X-RAY PULSARS WITH SUZAKU | HXD | Y |
| CEN X-4 | 224.5893 | -31.6684 | 332.24097668 | 23.88258751 | 104.6233 | 54847.9102314815 | 54850.9717939815 | 403057010 | 146670.4 | 150000 | 146687.6 | 146670.4 | 0 | 146691.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 133618.5 | 133618.5 | 264453.9 | 2 | PROCESSED | 57545.3354513889 | 55328 | 54880.5460069444 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031161 | Observations of thermal emission from the surface of quiescent neutron star low-mass X-ray binaries (LMXBs) can be used to measure neutron star radii. However, their quiescent spectra are complicated due to the presence of an additional power-law, and because variability has been seen on timescales as short as 100s. The nearest known neutron star LMXB Cen X-4 gives us the clearest view of these objects. But, the best observation so far lacked the sensitivity to determine the cause of the variability. Yet, the cause has important ramifications for measuring neutron star radii - if it is the thermal (rather than power-law) component that is varying our picture of quiescent emission may be wrong. To solve this critical problem we propose a 150 ksec observation of Cen X-4 with Suzaku. | GALACTIC POINT SOURCES | 4 | A | CACKETT | EDWARD | NULL | NULL | USA | 3 | AO3 | UNCOVERING VARIABLE QUIESCENT EMISSION IN THE NEUTRON STAR CEN X-4 | XIS | Y |
| GX 340+0 | 251.4463 | -45.6133 | 339.58535361 | -0.07953483 | 81.21 | 54892.2765740741 | 54894.8168287037 | 403060010 | 107312.7 | 100000 | 107314.5 | 107312.7 | 0 | 107314.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 86104 | 86104 | 219446.7 | 1 | PROCESSED | 57545.7913541667 | 55329 | 54908.7293055556 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031164 | In this proposal we request to observe accreting neutron stars sources GX 340+0, GX 3+1 and GX 13+1. The observational goal of the observations is to collect high-spectral resolution data in the region of K$_alpha$ iron line. Our scientific motivation is to put the origin of the line emission under additional theoretical scrutiny. We wish to compare the performance of the wind-reprocessing model to relativistic model in as many sources as possible. This proposal is a part of our broader effort to investigate the origin of iron emission line in Galactic X-ray binaries, which includes a parallel proposal to observe WD binaries. | GALACTIC POINT SOURCES | 4 | B | SHAPOSHNIKOV | NIKOLAI | NULL | NULL | USA | 3 | AO3 | IRON KALPHA EMISSION LINE DIAGNOSTICS IN ACCRETING NEUTRON STARS | XIS | Y |
| CYG X-2 | 326.1609 | 38.3293 | 87.3271497 | -11.30495752 | 51.1203 | 54648.0669097222 | 54650.6154398148 | 403063010 | 72430.8 | 100000 | 102692.2 | 72430.8 | 0 | 89814.4 | 1 | 1 | 0 | 2 | 1 | 0 | 0 | 88133.1 | 88133.1 | 220167.8 | 0 | PROCESSED | 57527.0641319444 | 55031 | 54665.3170601852 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031165 | The nature of ultra-dense matter in neutron stars remains enigmatic. To probe this requires accurate neutron star radii and masses. We recently showed that broad iron lines in neutron star low-mass X-ray binaries (LMXBs) constrain the neutron star radius. LMXBs also provide us with another tool, kHz quasi-periodic oscillations (QPOs). Combining the inner disk velocity (from modeling the iron line) and the frequency of the kHz QPOs gives a method to measure the neutron star mass. We propose a 100 ks observation of Cyg X-2 with Suzaku to provide a detailed iron line profile. Combined with simultaneous observations with RXTE to determine the kHz QPO frequency, we will measure the neutron star mass. Cyg X-2 is the perfect test case as it already has a known mass from optical observations. | GALACTIC POINT SOURCES | 4 | B | CACKETT | EDWARD | NULL | NULL | USA | 3 | AO3 | MEASURING NEUTRON STAR MASSES USING BROAD IRON LINES AND KHZ QPOS | XIS | Y |
| CYG X-1 | 299.5797 | 35.2714 | 71.39012673 | 3.11059703 | 84.4565 | 54574.6816898148 | 54575.4238425926 | 403065010 | 33943.5 | 30000 | 33943.5 | 33978.2 | 0 | 33970.3 | 1 | 1 | 0 | 2 | 1 | 0 | 0 | 28955.6 | 28955.6 | 64118 | 0 | PROCESSED | 57542.3725231482 | 54957 | 54587.2117476852 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031172 | We request two 30 ksec observations of Cyg X-1, to be coordinated with our ongoing RXTE and Ryle radio telescope monitoring campaign. Suzaku brings three unique attributes to this campaign: the ability to describe the 0.5-3 keV spectrum (crucial for describing the disk spectrum), high spectral resolution in the Fe line region (crucial for resolving narrow from relativistically broadened features), and the 100-600 keV spectrum (crucial for distinguishing among thermal corona, non-thermal corona, and jet models). By coordinating with our ongoing monitoring program, we not only obtain useful cross-calibration information, we will be able to place current and future Suzaku observations of Cyg X-1 in the context of the source's global history. | GALACTIC POINT SOURCES | 4 | A | NOWAK | MICHAEL | NULL | NULL | USA | 3 | AO3 | CONTINUING TO ENHANCE THE LONG TERM MONITORING CAMPAIGN IN THE SUZAKU ERA | HXD | Y |
| GX 339-4 | 255.7095 | -48.7885 | 338.94163546 | -4.32765826 | 281.8009 | 54733.942650463 | 54736.0968055556 | 403067010 | 104994 | 100000 | 105018 | 104994 | 0 | 104994 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 114775.9 | 114775.9 | 186091.7 | 2 | PROCESSED | 57544.0505092593 | 55148 | 54780.5803935185 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031174 | Understanding black hole systems in their canonical hard state is a major goal of high energy astrophysics. This state features a hard X-ray spectrum, a high level of timing noise, and emission from a steady jet at radio, IR, and perhaps higher frequencies. Along with our multi-wavelength, radio to X-ray, program, Suzaku observations can constrain theoretical models by answering the following questions: Does the inner edge of the accretion disk recede in the hard state? How is the location of the disk's inner edge related to the presence of a jet? Here, we propose to extend X-ray and radio studies of the hard state to low flux levels in order to answer these questions. | GALACTIC POINT SOURCES | 4 | A | TOMSICK | JOHN | NULL | NULL | USA | 3 | AO3-TOO | CONSTRAINING MODELS FOR BLACK HOLE ACCRETION IN THE HARD STATE | XIS | Y |
| XTE J1759-220 | 269.9393 | -22.0118 | 7.5831003 | 0.77858469 | 86.479 | 54566.5188773148 | 54567.6460532407 | 403072010 | 48961 | 50000 | 49361 | 49425 | 0 | 48961 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43912.9 | 43912.9 | 97363.9 | 1 | PROCESSED | 57542.2983912037 | 54953 | 54580.4766550926 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 032012 | Dipping low-mass X-ray binaries (LMXBs), a subclass of LMXBs that are viewed close to the disk plane, provide us with a rare opportunity to probe the structure of accretion disks. This was nicely illustrated with the discovery of Fe XXV and Fe XXVI absorption lines in all the dipping LMXBs observed with XMM and Chandra. It revealed the existence of a highly-ionized atmosphere above the disk which is likely present in any LMXB but only detectable in the ones seen close to edge-on. We propose to observe two recently discovered dipping binaries with Suzaku, to constrain the basic astrophysical properties (orbital period, distance, variability, high energy cutoff, etc) of these yet poorly observed sources, and to further investigate the ionized atmosphere in X-ray binaries in general. | GALACTIC POINT SOURCES | 4 | B | BOIRIN | LAURENCE | NULL | NULL | EUR | 3 | AO3 | NEW DIPPING X-RAY BINARIES TO PROBE ACCRETION DISKS AND THEIR IONIZED ATMOSPHER | XIS | Y |
| V2129 OPH | 246.9149 | -24.3651 | 353.29078542 | 16.72506486 | 88.3342 | 54866.0202430556 | 54866.5821296296 | 403074010 | 21033.5 | 20000 | 21033.5 | 21033.5 | 0 | 21033.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16533.1 | 16533.1 | 48533.9 | 0 | PROCESSED | 57545.4470833333 | 55329 | 54880.5317708333 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 032022 | We propose to observe the classical T Tauri stars CS Cha, MN Lup, V2129 Oph and XZ Tau with the Suzaku XIS to investigate accretion induced X-ray emission in CTTS as evidenced by the presence of excess emission in the soft X-ray regime. Specifically we intend to utilize Suzaku's sensitivity, low background and the capability of the XIS to resolve the OVIII Ly-alpha line from the OVII triplet. XMM-Newton and Chandra grating spectra provide strong evidence for the presence of accretion induced X-ray emission in CTTS, however, due to low SNR and the presence of absorption an accretion scenario often cannot be probed within reasonable exposure times. With the proposed observations we want to investigate a sample of these CTTS showing additional exceptional properties. | GALACTIC POINT SOURCES | 4 | B | ROBRADE | JAN | NULL | NULL | EUR | 3 | AO3 | ACCRETION RELATED SOFT X-RAY EMISSION IN CLASSICAL T TAURI STARS | XIS | Y |
| ESO 137-G034 | 248.7664 | -58.1298 | 329.07669192 | -7.11373135 | 296.1293 | 54744.462650463 | 54746.6745833333 | 403075010 | 92052.5 | 90000 | 92061.3 | 92058.7 | 0 | 92052.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 83661.5 | 83661.5 | 191089.7 | 1 | PROCESSED | 57544.095775463 | 55148 | 54780.6031828704 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 032025 | Suzaku observations of hard X-ray (> 15 keV) selected, bright AGN discovered by INTEGRAL and Swift have revealed several examples of previously unknown Compton Thick (NH > 1e24 cm-2) AGN in the nearby Universe. Their broad band X-ray spectra show a high degree of complexity and a wide range of the relative intensities of the various components (i.e. scattered/reflected fraction; iron line intensity, etc.). We propose a medium/deep Suzaku observation of a bright source detected by INTEGRAL above 15 keV and optically identified with a nearby Seyfert 2 galaxy. Besides the various soft X-ray components, the flat 2-10 keV spectrum and the strong (EW ~ 1 keV) iron line present in an archival XMM-Newton observation strongly suggest that the nucleus is obscured by Compton-Thick gas. | GALACTIC POINT SOURCES | 4 | B | GILLI | ROBERTO | NULL | NULL | EUR | 3 | AO3 | ANOTHER COMPTON-THICK AGN JUST AROUND THE CORNER | HXD | Y |
| GK PER | 52.8202 | 43.8404 | 151.00566373 | -10.1477205 | 257.5144 | 54875.4415277778 | 54876.0899884259 | 403081010 | 30388.8 | 30000 | 30388.8 | 30388.8 | 0 | 30388.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27399.9 | 27399.9 | 55997.9 | 2 | PROCESSED | 57545.5260648148 | 55330 | 54893.4257407407 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 033107 | We propose observations of 5 Intermediate Polars, a subcategory of magnetic CVs, as the first step toward establishment of an averaged hard X-ray spectrum of IPs that exist near the Solar system.The averaged spectrum should be compared with that of the Galactic Diffese X-ray Emssion (GDXE), to investigate the claimed spectral resemblance between them in energies above 10 keV. If the averaged IP spectrum shows any discrepancy with that of the GDXE, the "point-source origin" explanation for the GDXE would face a lack of appropriate hard X-ray source populations. This in turn is expected to strengthen the competing "truly diffuse origin"explanation, which attributes the GDXE hard X-rays to non thermal emission from electrons being accelerated in the interstellar space. | GALACTIC POINT SOURCES | 4 | C | YUASA | TAKAYUKI | HARRISON | THOMAS | JUS | 3 | AO3 | SURVEY OBSERVATION OF INTERMEDIATE POLARS | HXD | Y |
| AE AQUARII | 310.0451 | -0.9346 | 45.22328928 | -24.45613885 | 265.1622 | 55120.7618518518 | 55124.2265393518 | 404001010 | 160454.6 | 160000 | 161451.9 | 161720.9 | 0 | 160454.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 136071.5 | 136071.5 | 299327.7 | 3 | PROCESSED | 57548.9948958333 | 55503 | 55134.5588194444 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040032 | As picked up in the NASA press release in 2008, one of the most important results with Suzaku in three years was the first discovery of a possible non-thermal pulsation from a white dwarf AE Aquarii. This job was performed by our group. "Can magnetized white dwarfs accelerate particles like neutron stars?" This is the basic question of this study as a long standing mystery of Cosmic-ray origin for near 100 years. To ensure our result with Suzaku, we triggered the guest observation of AE Aquarii in TeV gamma-ray band with the recent powerful telescope, H.E.S.S., in their first GO program on 2009. Here, we propose the simultaneous observation with Suzaku and H.E.S.S, to distinguish the acceleration site in and/or outer of the binary system using X-ray and TeV gamma-ray flux informations. | GALACTIC POINT SOURCES | 4 | A | TERADA | YUKIKATSU | NULL | NULL | JAP | 4 | AO4 | SUZAKU, H.E.S.S., OPTICAL SIMULTANEOUS OBSERVATION OF THE WHITE DWARF PULSAR, AE AQUARII | HXD | Y |
| GS 1826-238 | 277.3735 | -23.8572 | 9.22092987 | -6.12003001 | 267.2862 | 55125.8488310185 | 55127.9502777778 | 404007010 | 102515.4 | 100000 | 102515.4 | 102531.4 | 0 | 102537.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 87999.6 | 87999.6 | 181541.8 | 2 | PROCESSED | 57549.0104976852 | 55534 | 55166.4220833333 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040035 | We propose a 100 ksec Suzaku observation of the neutron star (NS) binary GS 1826-238. It is already known that there is a high energy cutoff at around 150 keV in the hard state of black hole candidates (BNCs). Additional non-thermal spectrum above 300 keV has sometimes been verified by gamma-ray observatories. Some NS binaries exhibit a 'hard state' which shows X-ray properties similar to those observed in hard state BHCs. Their cutoff energies (~50 keV) are systematically lower than those of BHCs, but firm detections of non-thermal emissions are not reported so far. This proposal is aimed at the first detection of the non-thermal hard tail from this source in the steady 'hard state', and verification of its possible jet origin via simultaneous radio, near-IR, and optical observations. | GALACTIC POINT SOURCES | 4 | B | YAMAOKA | KAZUTAKA | NULL | NULL | JAP | 4 | AO4 | SEARCH FOR A NON-THERMAL HARD TAIL FROM THE NEUTRON STAR BINARY GS 1826-238 | HXD | Y |
| UX ARIETIS | 51.6466 | 28.6421 | 159.59610539 | -22.97107378 | 272.6966 | 55229.7116666667 | 55231.7321064815 | 404008010 | 87799.3 | 90000 | 87799.3 | 87799.3 | 0 | 87799.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 79742.9 | 79742.9 | 174539.9 | 0 | PROCESSED | 57550.5166203704 | 55616 | 55249.830150463 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040036 | We propose a hard X-ray observation of RS CVn-type active binary UX Arietis. Detection of nonthermal hard X-ray radiation is essentially important to solve the generation mechanism of stellar flares. UX Ari has a high coronal activity with a high temperature of ~2keV, and large stellar flares were frequently observed in the radio, UV, and X-ray band. Therefore, UX Ari is very suitable for hard X-ray observation of stellar flares. Large X-ray flares were observed by BeppoSAX, ASCA and Ginga sattellite, and hard X-ray emission upto ~50keV is detected by BeppoSAX. If a flare is large such as the events of former X-ray observations, we can detect the nonthermal hard X-ray emssion by Suzaku HXD. | GALACTIC POINT SOURCES | 4 | C | ISHIKAWA | SHIN-NOSUKE | NULL | NULL | JAP | 4 | AO4 | STUDY ON GENERATION MECHANISM OF STELLAR FLARES BY HARD X-RAY OBSERVATION OF ACTIVE BINARY UX ARIETIS | HXD | Y |
| RXJ0007.0+7302 | 1.8916 | 72.9843 | 119.68700382 | 10.38954096 | 241.7328 | 55204.6112847222 | 55207.0675231482 | 404011010 | 105373.9 | 100000 | 105373.9 | 105373.9 | 0 | 106971.4 | 2 | 2 | 0 | 1 | 1 | 0 | 0 | 58564.4 | 58564.4 | 212205.9 | 2 | PROCESSED | 57550.1958564815 | 55587 | 55768.9633333333 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040054 | We propose to observe the gamma-ray pulsar and itswind nebula (PWN) in the supernova remnant CTA1 with SUZAKU. Observations in X-ray wavebands are crucial to study non-thermal processes of PWNe. Its flux and spectral shape provide us important information about the energy distribution of the accelerated particles and the strength of the magnetic field. Observations made by Suzaku-HXD will constrain the X-ray spectrum above 20keV from the PWN for the first time. The high spectral resolution of XIS will allow us to search for metal lines, which tell us circumstance of the emission region. In addition, we will probably able to detect X-ray pulsation, which has notbeen detected yet, using XIS timing mode. | GALACTIC POINT SOURCES | 4 | C | TAKATA | JUMPEI | NULL | NULL | JAP | 4 | AO4 | X-RAY OBSERVATIONS OF GAMMA-RAY PULSAR AND ITS WIND NEBULA IN CTA1 | HXD | N |
| U SCO | 245.6288 | -17.8156 | 357.72079613 | 21.90901194 | 93.2747 | 55233.0102430556 | 55234.2918865741 | 404018010 | 46076.4 | 20000 | 46076.4 | 46076.4 | 0 | 46076.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37611.7 | 37611.7 | 110719.9 | 1 | PROCESSED | 57550.518599537 | 55617 | 55250.1559375 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040057 | We propose a 100ks TOO observation of a recurrent novae burst in our Galaxy. Using Suzaku's wide-energy coverage and excellent spectral performance at the iron K complex, we aim to derive the amount of mass loss at a classical nova burst. We plan to visit a nova withinin a few days and take spectra at five epochs spanning 10 days with 20ks each. | GALACTIC POINT SOURCES | 4 | A | TAKEI | DAI | NULL | NULL | JAP | 4 | AO4-TOO | TOO OBSERVATION OF A RECURRENT NOVA EXPLOSION | HXD | Y |
| U SCO | 245.629 | -17.8143 | 357.72199881 | 21.90970563 | 93.274 | 55236.514375 | 55237.1668865741 | 404018020 | 28936.9 | 20000 | 28936.9 | 28936.9 | 0 | 28936.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18328.8 | 18328.8 | 56369.9 | 0 | PROCESSED | 57550.5565393518 | 55619 | 55251.1498611111 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040057 | We propose a 100ks TOO observation of a recurrent novae burst in our Galaxy. Using Suzaku's wide-energy coverage and excellent spectral performance at the iron K complex, we aim to derive the amount of mass loss at a classical nova burst. We plan to visit a nova withinin a few days and take spectra at five epochs spanning 10 days with 20ks each. | GALACTIC POINT SOURCES | 4 | A | TAKEI | DAI | NULL | NULL | JAP | 4 | AO4-TOO | TOO OBSERVATION OF A RECURRENT NOVA EXPLOSION | HXD | Y |
| U SCO | 245.6292 | -17.8133 | 357.72295453 | 21.91020567 | 93.2753 | 55239.299224537 | 55239.8259027778 | 404018030 | 26826 | 20000 | 26826 | 26826 | 0 | 26826 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 24903.7 | 24903.7 | 45472 | 1 | PROCESSED | 57550.5610763889 | 55619 | 55253.1155671296 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040057 | We propose a 100ks TOO observation of a recurrent novae burst in our Galaxy. Using Suzaku's wide-energy coverage and excellent spectral performance at the iron K complex, we aim to derive the amount of mass loss at a classical nova burst. We plan to visit a nova withinin a few days and take spectra at five epochs spanning 10 days with 20ks each. | GALACTIC POINT SOURCES | 4 | A | TAKEI | DAI | NULL | NULL | JAP | 4 | AO4-TOO | TOO OBSERVATION OF A RECURRENT NOVA EXPLOSION | HXD | Y |
| EUVE J0317-85.5 | 48.9864 | -85.5003 | 299.84736337 | -30.72881529 | 65.46 | 55028.6017476852 | 55030.1460185185 | 404019010 | 63084.3 | 60000 | 63084.3 | 63084.3 | 0 | 63084.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 56896.5 | 56896.5 | 133413.8 | 1 | PROCESSED | 57547.8712847222 | 55406 | 55040.2674305556 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040083 | Where is the particle acceleration site in the universe? The Cosmic-ray origin is the long standing mystery for near 100 years. The first discovery of "the white dwarf pulsar" in the AE Aquarii system with Suzaku is one of the most important step in this study, because Suzaku demonstrated the possibility of particle acceleration in white dwarfs. The next important step is to search for the sign of non-thermal emission from a NORMAL white dwarf. Here, we propose the Suzaku observation of an isolated white dwarf EUVE J0317-85.5, which has very high magnetic field strength of 450 MG and very fast rotation period 725 sec among this type of objects. | GALACTIC POINT SOURCES | 4 | B | HARAYAMA | ATSUSHI | NULL | NULL | JAP | 4 | AO4 | FIRST SEARCH FOR NON THERMAL EMISSION FROM AN ISOLATED MAGNETIZED WHITE DWARF | HXD | Y |
| V603 AQL | 282.2246 | 0.5976 | 33.17431822 | 0.83751501 | 93.9529 | 55267.0156597222 | 55267.9773032407 | 404020010 | 34917.3 | 30000 | 34930.9 | 34917.3 | 0 | 34930.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30204.5 | 30204.5 | 83077.8 | 1 | PROCESSED | 57550.8656018518 | 55645 | 55279.4471296296 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040095 | The origin of the Galactic Ridge X-ray Emission (GRXE) is one of the unresolved issues in the X-ray astronomy for over 20 years. GRXE has a hard tail above ~10 keV and three iron emission lines from different ionization states. Recently, INTEGRAL discovered dozens of magnetic Cataclysmic Variables (mCVs), which are considered to contribute the GRXE hard tail. This year, we studied mCVs with Suzaku for the hard tail and the iron lines, and found that mCVs cannot explain the structure of iron lines of GRXE. If GRXE is a superposition of numerous point sources, other contributors which have strong He-like iron line are needed. Non-mCVs have generally a strong He-like iron line, and some non-mCVs have hard tail emission. We propose to investigate non-mCVs which are expected to have hard tail. | GALACTIC POINT SOURCES | 4 | B | SAITOU | KEI | NULL | NULL | JAP | 4 | AO4 | IRON LINE SPECTROSCOPY AND HARD TAIL DETECTION OF NON-MAGNETIC CATACLYSMIC VARIABLES | XIS | Y |
| TT ARI | 31.7181 | 15.2972 | 148.52228749 | -43.79443 | 71.0668 | 55018.4424652778 | 55019.3023611111 | 404021010 | 35742.1 | 35000 | 35742.1 | 35779.6 | 0 | 35787.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 31794 | 31794 | 74257.8 | 1 | PROCESSED | 57547.7822453704 | 55399 | 55029.236712963 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040095 | The origin of the Galactic Ridge X-ray Emission (GRXE) is one of the unresolved issues in the X-ray astronomy for over 20 years. GRXE has a hard tail above ~10 keV and three iron emission lines from different ionization states. Recently, INTEGRAL discovered dozens of magnetic Cataclysmic Variables (mCVs), which are considered to contribute the GRXE hard tail. This year, we studied mCVs with Suzaku for the hard tail and the iron lines, and found that mCVs cannot explain the structure of iron lines of GRXE. If GRXE is a superposition of numerous point sources, other contributors which have strong He-like iron line are needed. Non-mCVs have generally a strong He-like iron line, and some non-mCVs have hard tail emission. We propose to investigate non-mCVs which are expected to have hard tail. | GALACTIC POINT SOURCES | 4 | B | SAITOU | KEI | NULL | NULL | JAP | 4 | AO4 | IRON LINE SPECTROSCOPY AND HARD TAIL DETECTION OF NON-MAGNETIC CATACLYSMIC VARIABLES | XIS | Y |
| Z CAM | 126.2993 | 73.0997 | 141.39550179 | 32.62975748 | 289.0998 | 54931.1187152778 | 54931.9092476852 | 404022010 | 37663 | 35000 | 37663 | 37663 | 0 | 37663 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36532.9 | 36532.9 | 68289.9 | 0 | PROCESSED | 57546.1159722222 | 55324 | 54949.4517824074 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040095 | The origin of the Galactic Ridge X-ray Emission (GRXE) is one of the unresolved issues in the X-ray astronomy for over 20 years. GRXE has a hard tail above ~10 keV and three iron emission lines from different ionization states. Recently, INTEGRAL discovered dozens of magnetic Cataclysmic Variables (mCVs), which are considered to contribute the GRXE hard tail. This year, we studied mCVs with Suzaku for the hard tail and the iron lines, and found that mCVs cannot explain the structure of iron lines of GRXE. If GRXE is a superposition of numerous point sources, other contributors which have strong He-like iron line are needed. Non-mCVs have generally a strong He-like iron line, and some non-mCVs have hard tail emission. We propose to investigate non-mCVs which are expected to have hard tail. | GALACTIC POINT SOURCES | 4 | B | SAITOU | KEI | NULL | NULL | JAP | 4 | AO4 | IRON LINE SPECTROSCOPY AND HARD TAIL DETECTION OF NON-MAGNETIC CATACLYSMIC VARIABLES | XIS | Y |
| HESS J0632+057 | 98.2448 | 5.8057 | 205.66080027 | -1.43890266 | 289.9631 | 54941.5631944444 | 54944.1542708333 | 404027010 | 100034.3 | 100000 | 100034.3 | 100034.3 | 0 | 100034.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 82391.8 | 82391.8 | 223841.9 | 6 | PROCESSED | 57546.2406481482 | 55336 | 54966.5323958333 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040102 | We propose a coordinate observation of HESS J0632+057 with Suzaku and VLA. This source is recently discovered as a fourth gamma-ray binary with HESS and XMM-Newton, and our results obtained in Suzaku AO-3 also confirmed a gradual variety of X-ray intensity, possibly associated with the binary period. With a combined observation with VLA, we will for the first time obtain a "real-time" variety from both of image and spectrum of this interesting source. | GALACTIC POINT SOURCES | 4 | A | KOKUBUN | MOTOHIDE | NULL | NULL | JAP | 4 | AO4 | SIMULTANEOUS OBSERVATION OF HESS J0632+057 WITH SUZAKU AND VLA | XIS | Y |
| BG CMI | 112.8488 | 9.8847 | 208.51997296 | 13.31865509 | 292.793 | 54932.5078703704 | 54933.5710532407 | 404029010 | 47079.1 | 40000 | 47087.1 | 47079.1 | 0 | 47087.1 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 45034.6 | 45034.6 | 91808 | 2 | PROCESSED | 57546.1223958333 | 55324 | 54949.5279050926 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040113 | We propose observations of 5 Intermediate Polars, a subcategory of magnetic CVs, as the first step toward establishment of an averaged hard X-ray spectrum of IPs that exist near the Solar system.The averaged spectrum should be compared with that of the Galactic Diffese X-ray Emssion (GDXE), to investigate the claimed spectral resemblance between them in energies above 10 keV. If the averaged IP spectrum shows any discrepancy with that of the GDXE, the "point-source origin" explanation for the GDXE would face a lack of appropriate hard X-ray source populations. This in turn is expected to strengthen the competing "truly diffuse origin"explanation, which attributes the GDXE hard X-rays to non thermal emission from electrons being accelerated in the interstellar space. | GALACTIC POINT SOURCES | 4 | A | YUASA | TAKAYUKI | NULL | NULL | JAP | 4 | AO4 | SURVEY OBSERVATION OF INTERMEDIATE POLARS | HXD | Y |
| PQ GEM | 117.7967 | 14.685 | 206.10344887 | 19.72488518 | 295.2889 | 54933.5737037037 | 54934.6329166667 | 404030010 | 46738.7 | 40000 | 46738.7 | 46738.7 | 0 | 46738.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43247.9 | 43247.9 | 91507.9 | 0 | PROCESSED | 57546.1405787037 | 55324 | 54949.5317939815 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040113 | We propose observations of 5 Intermediate Polars, a subcategory of magnetic CVs, as the first step toward establishment of an averaged hard X-ray spectrum of IPs that exist near the Solar system.The averaged spectrum should be compared with that of the Galactic Diffese X-ray Emssion (GDXE), to investigate the claimed spectral resemblance between them in energies above 10 keV. If the averaged IP spectrum shows any discrepancy with that of the GDXE, the "point-source origin" explanation for the GDXE would face a lack of appropriate hard X-ray source populations. This in turn is expected to strengthen the competing "truly diffuse origin"explanation, which attributes the GDXE hard X-rays to non thermal emission from electrons being accelerated in the interstellar space. | GALACTIC POINT SOURCES | 4 | A | YUASA | TAKAYUKI | NULL | NULL | JAP | 4 | AO4 | SURVEY OBSERVATION OF INTERMEDIATE POLARS | HXD | Y |
| TX COL | 85.7822 | -41.0648 | 246.79781267 | -29.77494364 | 322.4827 | 54963.6800578704 | 54965.2502199074 | 404031010 | 59781.8 | 40000 | 59789.8 | 59789.8 | 0 | 59781.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51123 | 51123 | 135654 | 0 | PROCESSED | 57546.5734143518 | 55345 | 54978.2105439815 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040113 | We propose observations of 5 Intermediate Polars, a subcategory of magnetic CVs, as the first step toward establishment of an averaged hard X-ray spectrum of IPs that exist near the Solar system.The averaged spectrum should be compared with that of the Galactic Diffese X-ray Emssion (GDXE), to investigate the claimed spectral resemblance between them in energies above 10 keV. If the averaged IP spectrum shows any discrepancy with that of the GDXE, the "point-source origin" explanation for the GDXE would face a lack of appropriate hard X-ray source populations. This in turn is expected to strengthen the competing "truly diffuse origin"explanation, which attributes the GDXE hard X-rays to non thermal emission from electrons being accelerated in the interstellar space. | GALACTIC POINT SOURCES | 4 | A | YUASA | TAKAYUKI | NULL | NULL | JAP | 4 | AO4 | SURVEY OBSERVATION OF INTERMEDIATE POLARS | HXD | Y |
| FO AQR | 334.4646 | -8.2931 | 53.06192299 | -49.11309098 | 76.4186 | 54987.3437152778 | 54988.5536921296 | 404032010 | 46084.6 | 40000 | 46084.6 | 46084.6 | 0 | 46084.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 33499.3 | 33499.3 | 104529.9 | 0 | PROCESSED | 57547.5153356482 | 55366 | 54998.3271064815 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040113 | We propose observations of 5 Intermediate Polars, a subcategory of magnetic CVs, as the first step toward establishment of an averaged hard X-ray spectrum of IPs that exist near the Solar system.The averaged spectrum should be compared with that of the Galactic Diffese X-ray Emssion (GDXE), to investigate the claimed spectral resemblance between them in energies above 10 keV. If the averaged IP spectrum shows any discrepancy with that of the GDXE, the "point-source origin" explanation for the GDXE would face a lack of appropriate hard X-ray source populations. This in turn is expected to strengthen the competing "truly diffuse origin"explanation, which attributes the GDXE hard X-rays to non thermal emission from electrons being accelerated in the interstellar space. | GALACTIC POINT SOURCES | 4 | A | YUASA | TAKAYUKI | NULL | NULL | JAP | 4 | AO4 | SURVEY OBSERVATION OF INTERMEDIATE POLARS | HXD | Y |
| AO PSC | 343.7945 | -3.1271 | 68.69841137 | -53.28578539 | 60.9461 | 55004.4934143518 | 55005.3328587963 | 404033010 | 39654.4 | 40000 | 39654.4 | 39662.4 | 0 | 39662.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35683.4 | 35683.4 | 72517.9 | 0 | PROCESSED | 57547.6306481482 | 55385 | 55018.165474537 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040113 | We propose observations of 5 Intermediate Polars, a subcategory of magnetic CVs, as the first step toward establishment of an averaged hard X-ray spectrum of IPs that exist near the Solar system.The averaged spectrum should be compared with that of the Galactic Diffese X-ray Emssion (GDXE), to investigate the claimed spectral resemblance between them in energies above 10 keV. If the averaged IP spectrum shows any discrepancy with that of the GDXE, the "point-source origin" explanation for the GDXE would face a lack of appropriate hard X-ray source populations. This in turn is expected to strengthen the competing "truly diffuse origin"explanation, which attributes the GDXE hard X-rays to non thermal emission from electrons being accelerated in the interstellar space. | GALACTIC POINT SOURCES | 4 | A | YUASA | TAKAYUKI | NULL | NULL | JAP | 4 | AO4 | SURVEY OBSERVATION OF INTERMEDIATE POLARS | HXD | Y |
| HD6903 | 17.4507 | 19.662 | 128.84764567 | -42.9987034 | 70.0004 | 55031.3824305556 | 55032.3578703704 | 404034010 | 36813.5 | 35000 | 36829.5 | 36813.5 | 0 | 36821.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 29672.7 | 29672.7 | 84263.9 | 0 | PROCESSED | 57547.8823958333 | 55419 | 55048.3029976852 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041201 | Suzaku XIS spectra of two G0 III Hertzsprung gap giants will complete a multi-observatory survey of the anomalous coronal behavior of this "X-ray deficient" class. The abrupt rise in coronal luminosities from the warmer giants to their cooler cousins, only slightly further advanced in evolution, might signal disruption of a "fossil" magnetosphere by a newly born solar-like dynamo. Key discriminators are the coronal energy distribution, composition (FIP bias), and sporadic hard emission associated with flaring. The proposed targets are the brightest not previously observed in X-rays at CCD resolution, and both have supporting HST UV spectra. Expanding the high energy sample of this key class of objects is essential for probing their contrary, but perhaps deeply significant, behavior. | GALACTIC POINT SOURCES | 4 | B | AYRES | THOMAS | NULL | NULL | USA | 4 | AO4 | ANOMALOUS CORONAE IN THE MIDST OF THE HERTZSPRUNG GAP | XIS | Y |
| HD72779 | 128.8308 | 19.5933 | 205.51018209 | 31.33811175 | 104.3214 | 55141.3245949074 | 55142.9515277778 | 404035010 | 71033.5 | 70000 | 71033.5 | 71033.5 | 0 | 71033.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47461 | 47461 | 140555.9 | 0 | PROCESSED | 57549.2155902778 | 55532 | 55166.2074189815 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041201 | Suzaku XIS spectra of two G0 III Hertzsprung gap giants will complete a multi-observatory survey of the anomalous coronal behavior of this "X-ray deficient" class. The abrupt rise in coronal luminosities from the warmer giants to their cooler cousins, only slightly further advanced in evolution, might signal disruption of a "fossil" magnetosphere by a newly born solar-like dynamo. Key discriminators are the coronal energy distribution, composition (FIP bias), and sporadic hard emission associated with flaring. The proposed targets are the brightest not previously observed in X-rays at CCD resolution, and both have supporting HST UV spectra. Expanding the high energy sample of this key class of objects is essential for probing their contrary, but perhaps deeply significant, behavior. | GALACTIC POINT SOURCES | 4 | B | AYRES | THOMAS | NULL | NULL | USA | 4 | AO4 | ANOMALOUS CORONAE IN THE MIDST OF THE HERTZSPRUNG GAP | XIS | Y |
| YY MEN | 74.6207 | -75.281 | 287.41045099 | -33.23069192 | 7.2587 | 54996.0772916667 | 54998.5606365741 | 404036010 | 106949.8 | 100000 | 106957.8 | 106957.8 | 0 | 106949.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 104090.2 | 104090.2 | 214539.8 | 0 | PROCESSED | 57547.6240393518 | 55378 | 55008.2997106482 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041202 | The single K giant YY Men is one of the most active stars within 300 pc of the Sun, having produced 2 of the most powerful radio flares and 1 of the most powerful and long-duration optical flares ever detected. Its corona is one of the hottest and brightest known, with a *typical* X-ray luminosity of 32.0-32.5 (log erg/s) which most other cool stars only reach during major flares. We propose to obtain a 100-ksec observation of this hyperactive star to get a high S/N XIS exposure of its spectrum, particularly in the 5-10 keV region in which the XIS excels. We will study the He- and H-like Fe lines, search for 6.4 keV fluorescent emission, search for the presence of ultrahigh temperature and nonthermal spectral components, and look for correlations with simultaneous ATCA radio observations. | GALACTIC POINT SOURCES | 4 | B | DRAKE | STEPHEN | NULL | NULL | USA | 4 | AO4 | THE EXTREME CORONAL PROPERTIES OF THE HYPERACTIVE K GIANT YY MEN | XIS | Y |
| V773 TAU | 63.5591 | 28.1916 | 168.22897578 | -16.34488481 | 264.3183 | 55255.9666550926 | 55258.750162037 | 404037010 | 115405.7 | 120000 | 115405.7 | 115405.7 | 0 | 115405.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 95563 | 95563 | 240466.7 | 1 | PROCESSED | 57550.8499189815 | 55637 | 55271.499537037 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041203 | Young stars display magnetic activity at the extreme of that produced in nearby active stars and the Sun, making them useful tools to probe the dominant physical processes controlling such activity. The unique features of V773 Tau's X-ray and radio properties (frequent X-ray flaring of highly energetic flares, extreme nonthermal radio emission) mark it as one of the most active young stars. We seek coordinated Suzaku and mm wavelength observations to probe the interplay between the hot plasma and the stellar environment. We focus on utilizing the unique capabilities of Suzaku, namely the spectral resolution and sensitivity at 5--10 keV, to elucidate the properties of its hot plasma and its potential effects on the stellar environment such as detecting Fe fluorescence. | GALACTIC POINT SOURCES | 4 | C | OSTEN | RACHEL | NULL | NULL | USA | 4 | AO4 | X-RAY EMISSION AND THE STELLAR ENVIRONMENT AROUND THE PRE-MAIN SEQUENCE BINARY V773 TAU | XIS | Y |
| ETA CARINAE | 161.2306 | -59.7313 | 287.60339978 | -0.67900846 | 291.9998 | 54992.8234143518 | 54994.2918865741 | 404038010 | 51225.9 | 45000 | 51225.9 | 51233.9 | 0 | 51233.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 49118.6 | 49118.6 | 126839.8 | 0 | PROCESSED | 57547.5667361111 | 55378 | 55006.2447569444 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041204 | The collision of winds in the supermassive binary Eta Car produces hot plasma detectable by Suzaku to 40 keV. This emission provides key clues to the way extremely massive stars lose mass. We propose to observe this hard X-ray emission with Suzaku after the periastron passage in order to measure the intrinsic luminosity of the wind-wind shock to determine the density of the wind near the shock boundary, and to measure the absorbing column to indicate the density profile in the distorted wind of the primary star. In addition HXD observations will measure any excess emission up to energies of 40 keV to constrain the amount of particle acceleration in the shock by the first order Fermi process and to help resolve the discrepancy between published BeppoSAX and INTEGRAL measurements. | GALACTIC POINT SOURCES | 4 | A | HAMAGUCHI | KENJI | NULL | NULL | USA | 4 | AO4 | HARD X-RAY EMISSION, PARTICLE ACCELERATION AND MASS LOSS FROM ETA CAR | HXD | Y |
| ETA CARINAE | 161.2575 | -59.6351 | 287.57052339 | -0.58758586 | 87.8919 | 55156.1883449074 | 55157.3196643518 | 404039010 | 49388.7 | 45000 | 49388.7 | 49388.7 | 0 | 49388.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34255.3 | 34255.3 | 97720.1 | 0 | PROCESSED | 57549.5287152778 | 55542 | 55176.3651388889 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041204 | The collision of winds in the supermassive binary Eta Car produces hot plasma detectable by Suzaku to 40 keV. This emission provides key clues to the way extremely massive stars lose mass. We propose to observe this hard X-ray emission with Suzaku after the periastron passage in order to measure the intrinsic luminosity of the wind-wind shock to determine the density of the wind near the shock boundary, and to measure the absorbing column to indicate the density profile in the distorted wind of the primary star. In addition HXD observations will measure any excess emission up to energies of 40 keV to constrain the amount of particle acceleration in the shock by the first order Fermi process and to help resolve the discrepancy between published BeppoSAX and INTEGRAL measurements. | GALACTIC POINT SOURCES | 4 | A | HAMAGUCHI | KENJI | NULL | NULL | USA | 4 | AO4 | HARD X-RAY EMISSION, PARTICLE ACCELERATION AND MASS LOSS FROM ETA CAR | HXD | Y |
| SKY(270, +25) | 270.2558 | 25.1504 | 50.99920401 | 21.68976417 | 70.6538 | 55284.5620023148 | 55285.2994791667 | 404041010 | 1701.9 | 25000 | 1926.6 | 2094.4 | 0 | 1701.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 5621.1 | 5621.1 | 63713.9 | 1 | PROCESSED | 57551.0540277778 | 55284 | 55301.2652314815 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041222 | Suzaku has recently revealed relativistically broadened Fe Kalpha emission lines in the spectra of neutron star low-mass X-ray binaries (LMXBs). We have now seen these lines in 10 neutron star LMXBs that we have examined, allowing measurements of the inner accretion disk radius, and hence an upper limit on the neutron star radius in all these objects. Only with the sensitivity of Suzaku, its high effective area in the Fe K band, and its broad bandpass has it been possible to robustly determine the shape of the lines. With a longer-term aim of completing a census of iron lines in neutron star LMXBs, we request a total of 200 ks to observe 5 neutron star low-mass X-ray binaries to study the relativistic broadening in the Fe Kalpha emission line profiles. | GALACTIC POINT SOURCES | 4 | C | CACKETT | EDWARD | NULL | NULL | USA | 4 | AO4 | AN FE KALPHA EMISSION LINE SURVEY OF NEUTRON STAR LMXBS | HXD | Y |
| 4U 1608-52 | 243.1847 | -52.3651 | 330.96850701 | -0.81056533 | 96.6085 | 55266.077650463 | 55267.0072222222 | 404044010 | 34010.1 | 30000 | 34010.1 | 34010.1 | 0 | 34010.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30194 | 30194 | 80297.8 | 0 | PROCESSED | 57550.8305902778 | 55647 | 55279.4591666667 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041223 | The true nature of X-ray emission from neutron star X-ray binaries (NSXRBs) has not been clear for sometime and there are many possibilities for the spectral model. Recent progress has been made, but relies on RXTE data which lacks the low energy sensitivity where disk emission is most prominent. Using Suzaku we propose four 30 ksec observations of the transient 4U 1608-52 throughout an outburst. We will test how spectral parameters change with luminosity, allowing us to untangle the correct model. An essential part of this proposal is the unique ability of Suzaku to detect asymmetric broad iron emission lines in NSXRBs. We will study how the iron line varies throughout the outburst, which combined with the spectral fits will test the interaction between the accretion disk and corona. | GALACTIC POINT SOURCES | 4 | A | CACKETT | EDWARD | NULL | NULL | USA | 4 | AO4-TOO | ACCRETION DISK EVOLUTION THROUGHOUT A NEUTRON STAR LMXB OUTBURST | HXD | Y |
| 4U 1608-52 | 243.1805 | -52.3646 | 330.96698106 | -0.80844416 | 94.0316 | 55270.6937615741 | 55271.6668287037 | 404044020 | 32718.1 | 30000 | 32718.1 | 32726.1 | 0 | 32718.1 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 26988 | 26988 | 84055.8 | 1 | PROCESSED | 57550.9065277778 | 55651 | 55285.1175462963 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041223 | The true nature of X-ray emission from neutron star X-ray binaries (NSXRBs) has not been clear for sometime and there are many possibilities for the spectral model. Recent progress has been made, but relies on RXTE data which lacks the low energy sensitivity where disk emission is most prominent. Using Suzaku we propose four 30 ksec observations of the transient 4U 1608-52 throughout an outburst. We will test how spectral parameters change with luminosity, allowing us to untangle the correct model. An essential part of this proposal is the unique ability of Suzaku to detect asymmetric broad iron emission lines in NSXRBs. We will study how the iron line varies throughout the outburst, which combined with the spectral fits will test the interaction between the accretion disk and corona. | GALACTIC POINT SOURCES | 4 | A | CACKETT | EDWARD | NULL | NULL | USA | 4 | AO4-TOO | ACCRETION DISK EVOLUTION THROUGHOUT A NEUTRON STAR LMXB OUTBURST | HXD | Y |
| 4U 1608-52 | 243.2309 | -52.3757 | 330.98178647 | -0.83761569 | 125.7606 | 55273.9986689815 | 55274.9154166667 | 404044030 | 31756.8 | 30000 | 31756.8 | 31756.8 | 0 | 31756.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15309.4 | 15309.4 | 79193.8 | 0 | PROCESSED | 57550.9191898148 | 55652 | 55286.259849537 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041223 | The true nature of X-ray emission from neutron star X-ray binaries (NSXRBs) has not been clear for sometime and there are many possibilities for the spectral model. Recent progress has been made, but relies on RXTE data which lacks the low energy sensitivity where disk emission is most prominent. Using Suzaku we propose four 30 ksec observations of the transient 4U 1608-52 throughout an outburst. We will test how spectral parameters change with luminosity, allowing us to untangle the correct model. An essential part of this proposal is the unique ability of Suzaku to detect asymmetric broad iron emission lines in NSXRBs. We will study how the iron line varies throughout the outburst, which combined with the spectral fits will test the interaction between the accretion disk and corona. | GALACTIC POINT SOURCES | 4 | A | CACKETT | EDWARD | NULL | NULL | USA | 4 | AO4-TOO | ACCRETION DISK EVOLUTION THROUGHOUT A NEUTRON STAR LMXB OUTBURST | HXD | Y |
| 4U 1608-52 | 243.1735 | -52.4241 | 330.92310685 | -0.84886634 | 127.9983 | 55277.989849537 | 55278.9140393518 | 404044040 | 16072.8 | 30000 | 16072.8 | 16072.8 | 0 | 16072.8 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 15655.7 | 15655.7 | 79843.9 | 2 | PROCESSED | 57550.9805439815 | 55665 | 55299.4128819444 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041223 | The true nature of X-ray emission from neutron star X-ray binaries (NSXRBs) has not been clear for sometime and there are many possibilities for the spectral model. Recent progress has been made, but relies on RXTE data which lacks the low energy sensitivity where disk emission is most prominent. Using Suzaku we propose four 30 ksec observations of the transient 4U 1608-52 throughout an outburst. We will test how spectral parameters change with luminosity, allowing us to untangle the correct model. An essential part of this proposal is the unique ability of Suzaku to detect asymmetric broad iron emission lines in NSXRBs. We will study how the iron line varies throughout the outburst, which combined with the spectral fits will test the interaction between the accretion disk and corona. | GALACTIC POINT SOURCES | 4 | A | CACKETT | EDWARD | NULL | NULL | USA | 4 | AO4-TOO | ACCRETION DISK EVOLUTION THROUGHOUT A NEUTRON STAR LMXB OUTBURST | HXD | Y |
| A 0535+26 | 84.7195 | 26.3786 | 181.38803208 | -2.61609461 | 86.1856 | 55067.9626273148 | 55069.1599421296 | 404054010 | 51866.8 | 45000 | 51870.6 | 51870.6 | 0 | 51866.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42078 | 42078 | 103429.8 | 1 | PROCESSED | 57548.3667708333 | 55448 | 55078.219837963 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041232 | We propose to perform Target of Opportunity Observations of one accreting neutron star in outburst during Suzaku's AO-4. The aim of the observations is to observe the source at a level of 40 and 200mCrab, to determine the properties of the cyclotron line(s) in this system and to constrain its broad band spectrum. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 4 | AO4-TOO | CYCLOTRON RESONANCE SCATTERING FEATURES IN TRANSIENT ACCRETING X-RAY PULSARS WITH SUZAKU | HXD | Y |
| A 0535+26 | 84.7291 | 26.2457 | 181.50526016 | -2.67952465 | 272.2555 | 55292.5024074074 | 55293.7029282407 | 404055010 | 3177.9 | 45000 | 3177.9 | 3460.4 | 0 | 3177.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34392.8 | 34392.8 | 103715.8 | 1 | PROCESSED | 57553.0049074074 | 55689 | 55323.4435532407 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041232 | We propose to perform Target of Opportunity Observations of one accreting neutron star in outburst during Suzaku's AO-4. The aim of the observations is to observe the source at a level of 40 and 200mCrab, to determine the properties of the cyclotron line(s) in this system and to constrain its broad band spectrum. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 4 | AO4-TOO | CYCLOTRON RESONANCE SCATTERING FEATURES IN TRANSIENT ACCRETING X-RAY PULSARS WITH SUZAKU | HXD | Y |
| IGRJ16393-4643 | 249.7688 | -46.7009 | 338.00177501 | 0.07896045 | 111.6627 | 55267.9865740741 | 55269.4508564815 | 404056010 | 50540 | 50000 | 50564 | 50540 | 0 | 50564 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42256.5 | 42256.5 | 126467.8 | 1 | PROCESSED | 57550.8754166667 | 55647 | 55279.4686689815 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041234 | Stellar winds play a critical role in several as yet poorly understood astrophysical processes. One of the best laboratories for studying winds is in wind fed Supergiant High Mass X-ray binaries. Using the neutron star (NS) as a backlight, variable absorption in X-rays measures column density variations in the secondary star wind. A recent explosion in the number of known HMXBs has defined two additional subclasses of HMXBs, potentially related through geometry and wind properties: 1) heavily obscured sources and 2) so-called Supergiant Fast X-ray Transients (SFXTs). We propose observations of 2 obscured sgHMXBs and 2 SFXTs to monitor the column density. This will test wind models and probe whether these subclasses are related to one another and to classical HMXBs through wind parameters. | GALACTIC POINT SOURCES | 4 | C | MORRIS | DAVID | NULL | NULL | USA | 4 | AO4 | PROBING DONOR STAR WIND STRUCTURE IN HMXBS THROUGH VARIABLE ABSORPTION | XIS | Y |
| GS 2023+338 | 306.0444 | 33.8015 | 73.0785131 | -2.14854563 | 252.4521 | 55142.9636805556 | 55144.0550810185 | 404059010 | 42324.6 | 40000 | 42348.6 | 42324.6 | 0 | 42356.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 29140.4 | 29140.4 | 94283.9 | 1 | PROCESSED | 57549.1887384259 | 55531 | 55155.1065625 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041243 | The quiescent state is the dominant accretion mode for black holes on all mass scales. Our knowledge of the X-ray spectrum is limited due to the characteristic low luminosity in this state. Here, we propose a 40 ks observation of the most luminous quiescent stellar mass black hole GS 2023+338 (V404 Cyg). These observations will allow us to detect hard X-ray emission from a quiescent stellar mass black hole for the first time, providing unique contraints on the nature of the accretion flow in this low luminosity state. | GALACTIC POINT SOURCES | 4 | B | REYNOLDS | MARK | NULL | NULL | USA | 4 | AO4 | CONSTRAINING THE QUIESCENT ACCRETION FLOW AROUND A BLACK HOLE WITH SUZAKU | HXD | Y |
| GRS 1758-258 | 270.2971 | -25.679 | 4.56169204 | -1.32563061 | 89.3817 | 55263.8983333333 | 55266.0711111111 | 404060010 | 82682.7 | 80000 | 82682.7 | 82682.7 | 0 | 82682.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 71178.9 | 71178.9 | 187709.7 | 1 | PROCESSED | 57550.8664583333 | 55647 | 55279.5468402778 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041244 | We propose an 80 ks observation to obtain a broadband spectrum of the Galactic microquasar GRS 1758-258 while in the low-hard state with Suzaku. Here we aim to constrain the nature and geometry of the accretion flow via measurements of the various disc reflection features, which are detectable for the first time due to the unique capabilities of Suzaku. As this system is known to power large radio jets, its study will also aid our understanding of the conditions necessary for the formation of relativistic outflows and how these relate to the accretion geometry in the low-hard state. | GALACTIC POINT SOURCES | 4 | B | REYNOLDS | MARK | NULL | NULL | USA | 4 | AO4 | CONSTRAINING DISC REFLECTION IN THE MICROQUASAR GRS 1758-258 | HXD | Y |
| LMC X-1 | 84.947 | -69.7479 | 280.20680376 | -31.50316575 | 10.0004 | 55033.776724537 | 55036.8953587963 | 404061010 | 129867.9 | 120000 | 129867.9 | 129867.9 | 0 | 129867.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 132597.6 | 132597.6 | 269395.6 | 4 | PROCESSED | 57548.0199537037 | 55419 | 55048.6509143518 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041245 | We propose to measure the spins of two black holes, LMC X-1 and LMC X-3, using two independent methods concurrently: modeling the thermal spectrum of the accretion disk and modeling the profile of the Fe K line. Suzaku is the only mission capable of achieving both of our main objectives: (1) to make the first Fe K spin measurements of these LMC sources, and (2) to explore whether the two methods deliver consistent results. The XIS will provide full coverage of the continuum spectrum and handily resolve the broad Fe line, while the HXD PIN will strongly constrain the Compton power-law component, which is important to both methods. For both of these LMC sources, we confidently argue that the spins obtained by modeling the continuum spectrum will be of exceptional precision and reliability. | GALACTIC POINT SOURCES | 4 | A | MCCLINTOCK | JEFFREY | NULL | NULL | USA | 4 | AO4 | MEASURING BLACK-HOLE SPINS IN THE LMC USING BOTH THE THERMAL X-RAY CONTINUUM AND FE K LINE | XIS | Y |
| LMC X-3 | 84.7128 | -64.0821 | 273.5746003 | -32.09166858 | 184.4521 | 55186.5265162037 | 55190.9105555556 | 404062010 | 154424.2 | 150000 | 154434 | 154434 | 0 | 154424.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 101172.1 | 101172.1 | 352145.8 | 2 | PROCESSED | 57550.1364930556 | 55587 | 55218.7384375 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041245 | We propose to measure the spins of two black holes, LMC X-1 and LMC X-3, using two independent methods concurrently: modeling the thermal spectrum of the accretion disk and modeling the profile of the Fe K line. Suzaku is the only mission capable of achieving both of our main objectives: (1) to make the first Fe K spin measurements of these LMC sources, and (2) to explore whether the two methods deliver consistent results. The XIS will provide full coverage of the continuum spectrum and handily resolve the broad Fe line, while the HXD PIN will strongly constrain the Compton power-law component, which is important to both methods. For both of these LMC sources, we confidently argue that the spins obtained by modeling the continuum spectrum will be of exceptional precision and reliability. | GALACTIC POINT SOURCES | 4 | C | MCCLINTOCK | JEFFREY | NULL | NULL | USA | 4 | AO4 | MEASURING BLACK-HOLE SPINS IN THE LMC USING BOTH THE THERMAL X-RAY CONTINUUM AND FE K LINE | XIS | Y |
| XTE J1710-281 | 257.5483 | -28.1282 | 356.35839186 | 6.92613447 | 86.2275 | 55278.9207638889 | 55281.1460300926 | 404068010 | 76138.5 | 75000 | 76138.5 | 76146.5 | 0 | 76146.5 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 23656.5 | 23656.5 | 192239.7 | 3 | PROCESSED | 57551.0466435185 | 55668 | 55301.5227662037 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 042003 | We propose to observe XTE J1710-281, a low-mass X-ray binary showing bursts, eclipses and dips. We want to determine the nature of the X-ray emission in this yet poorly-studied system and exploit the fact it is viewed close to edge-on to probe the structure of the disk and of the ionized plasma located above it. The broad-band coverage of Suzaku XIS and HXD will allow us to determine the overall shape of the ionizing continuum, which is a key parameter to infer the properties of the warm absorber whose narrow spectral signatures will be simultaneously detected thanks to the good spectral resolution of XIS near 6 keV. | GALACTIC POINT SOURCES | 4 | C | BOIRIN | LAURENCE | NULL | NULL | EUR | 4 | AO4 | SUZAKU TO INVESTIGATE A LOW-MASS X-RAY BINARY SHOWING BURSTS, ECLIPSES, AND DIPS | XIS | Y |
| 4U 1820-30 | 275.9267 | -30.4234 | 2.73525617 | -7.94773658 | 265.1815 | 55083.1120023148 | 55083.2015740741 | 404069010 | 3517.5 | 20000 | 3525.5 | 3517.5 | 0 | 3525.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3712.4 | 3712.4 | 7738 | 0 | PROCESSED | 57548.5052546296 | 55475 | 55109.4203125 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 042004 | Fe K-alpha lines have now been detected in about half a dozen of neutron-star X-ray binaries. These lines can be used to set tight constrains on the accretion disk geometry and the radius of the neutron star. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kilohertz quasi-periodic oscillations (kHz QPOs). However, contemporaneous measurements in one of these systems appear to contradict this picture. We propose to observe 4U 1820-30 with Suzaku, simultaneously with RXTE. Our program will sample a wide range of inner disk radii and thereby explore the combined use of Fe K-alpha lines and kHz QPOs to probe strong gravity in X-ray binaries. | GALACTIC POINT SOURCES | 4 | A | LINARES | MANUEL | NULL | NULL | EUR | 4 | AO4 | ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES. | HXD | Y |
| 4U 1820-30 | 275.9248 | -30.4209 | 2.73676025 | -7.94514519 | 265.9319 | 55088.3645833333 | 55088.8141087963 | 404069020 | 21037.3 | 20000 | 21037.3 | 21037.3 | 0 | 21037.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17170 | 17170 | 38831.9 | 0 | PROCESSED | 57548.569837963 | 55469 | 55103.4457407407 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 042004 | Fe K-alpha lines have now been detected in about half a dozen of neutron-star X-ray binaries. These lines can be used to set tight constrains on the accretion disk geometry and the radius of the neutron star. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kilohertz quasi-periodic oscillations (kHz QPOs). However, contemporaneous measurements in one of these systems appear to contradict this picture. We propose to observe 4U 1820-30 with Suzaku, simultaneously with RXTE. Our program will sample a wide range of inner disk radii and thereby explore the combined use of Fe K-alpha lines and kHz QPOs to probe strong gravity in X-ray binaries. | GALACTIC POINT SOURCES | 4 | A | LINARES | MANUEL | NULL | NULL | EUR | 4 | AO4 | ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES. | HXD | Y |
| 4U 1820-30 | 275.9316 | -30.4206 | 2.73970623 | -7.95024046 | 261.8755 | 55096.0447453704 | 55096.8335416667 | 404069030 | 29225.4 | 20000 | 29225.4 | 29225.4 | 0 | 29225.4 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 25940.5 | 25940.5 | 68148 | 1 | PROCESSED | 57548.6598726852 | 55477 | 55110.3989699074 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 042004 | Fe K-alpha lines have now been detected in about half a dozen of neutron-star X-ray binaries. These lines can be used to set tight constrains on the accretion disk geometry and the radius of the neutron star. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kilohertz quasi-periodic oscillations (kHz QPOs). However, contemporaneous measurements in one of these systems appear to contradict this picture. We propose to observe 4U 1820-30 with Suzaku, simultaneously with RXTE. Our program will sample a wide range of inner disk radii and thereby explore the combined use of Fe K-alpha lines and kHz QPOs to probe strong gravity in X-ray binaries. | GALACTIC POINT SOURCES | 4 | A | LINARES | MANUEL | NULL | NULL | EUR | 4 | AO4 | ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES. | HXD | Y |
| 4U 1820-30 | 275.9314 | -30.4193 | 2.74079847 | -7.94949913 | 261.8762 | 55102.6696759259 | 55103.5002662037 | 404069040 | 28699.4 | 20000 | 28699.4 | 28699.4 | 0 | 28699.4 | 3 | 2 | 0 | 3 | 1 | 0 | 0 | 24926.1 | 24926.1 | 71751.9 | 2 | PROCESSED | 57548.6752546296 | 55499 | 55133.2273263889 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 042004 | Fe K-alpha lines have now been detected in about half a dozen of neutron-star X-ray binaries. These lines can be used to set tight constrains on the accretion disk geometry and the radius of the neutron star. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kilohertz quasi-periodic oscillations (kHz QPOs). However, contemporaneous measurements in one of these systems appear to contradict this picture. We propose to observe 4U 1820-30 with Suzaku, simultaneously with RXTE. Our program will sample a wide range of inner disk radii and thereby explore the combined use of Fe K-alpha lines and kHz QPOs to probe strong gravity in X-ray binaries. | GALACTIC POINT SOURCES | 4 | A | LINARES | MANUEL | NULL | NULL | EUR | 4 | AO4 | ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES. | HXD | Y |
| 4U 1820-30 | 275.9251 | -30.4172 | 2.74021083 | -7.94370371 | 265.2009 | 55111.1096643518 | 55111.700162037 | 404069050 | 21767.4 | 20000 | 21767.4 | 21767.4 | 0 | 21767.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15674.3 | 15674.3 | 51003.9 | 0 | PROCESSED | 57548.7799884259 | 55496 | 55127.2938194445 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 042004 | Fe K-alpha lines have now been detected in about half a dozen of neutron-star X-ray binaries. These lines can be used to set tight constrains on the accretion disk geometry and the radius of the neutron star. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kilohertz quasi-periodic oscillations (kHz QPOs). However, contemporaneous measurements in one of these systems appear to contradict this picture. We propose to observe 4U 1820-30 with Suzaku, simultaneously with RXTE. Our program will sample a wide range of inner disk radii and thereby explore the combined use of Fe K-alpha lines and kHz QPOs to probe strong gravity in X-ray binaries. | GALACTIC POINT SOURCES | 4 | A | LINARES | MANUEL | NULL | NULL | EUR | 4 | AO4 | ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES. | HXD | Y |
| 4U 1820-30 | 275.9218 | -30.4206 | 2.73584989 | -7.94270191 | 269.3964 | 55116.6321064815 | 55117.1759143518 | 404069060 | 24668.7 | 100000 | 0 | 24668.7 | 0 | 24668.7 | 0 | 1 | 0 | 2 | 1 | 0 | 0 | 16950.5 | 16950.5 | 46978 | 0 | PROCESSED | 57548.8754861111 | 55507 | 55131.3693518518 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 042004 | Fe K-alpha lines have now been detected in about half a dozen of neutron-star X-ray binaries. These lines can be used to set tight constrains on the accretion disk geometry and the radius of the neutron star. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kilohertz quasi-periodic oscillations (kHz QPOs). However, contemporaneous measurements in one of these systems appear to contradict this picture. We propose to observe 4U 1820-30 with Suzaku, simultaneously with RXTE. Our program will sample a wide range of inner disk radii and thereby explore the combined use of Fe K-alpha lines and kHz QPOs to probe strong gravity in X-ray binaries. | GALACTIC POINT SOURCES | 4 | A | LINARES | MANUEL | NULL | NULL | EUR | 4 | AO4 | ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES. | HXD | Y |
| 4U 1820-30 | 275.9205 | -30.4212 | 2.7347979 | -7.94197311 | 270.4164 | 55124.2356134259 | 55124.7925810185 | 404069070 | 24056.6 | 100000 | 24056.7 | 24072.6 | 0 | 24056.6 | 3 | 1 | 0 | 2 | 1 | 0 | 0 | 18903.5 | 18903.5 | 48107.9 | 0 | PROCESSED | 57548.9193981482 | 55503 | 55134.2427314815 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 042004 | Fe K-alpha lines have now been detected in about half a dozen of neutron-star X-ray binaries. These lines can be used to set tight constrains on the accretion disk geometry and the radius of the neutron star. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kilohertz quasi-periodic oscillations (kHz QPOs). However, contemporaneous measurements in one of these systems appear to contradict this picture. We propose to observe 4U 1820-30 with Suzaku, simultaneously with RXTE. Our program will sample a wide range of inner disk radii and thereby explore the combined use of Fe K-alpha lines and kHz QPOs to probe strong gravity in X-ray binaries. | GALACTIC POINT SOURCES | 4 | A | LINARES | MANUEL | NULL | NULL | EUR | 4 | AO4 | ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES. | HXD | Y |
| IGR J08408-4503 | 130.2449 | -45.0216 | 264.03123634 | -1.90203871 | 133.4432 | 55176.7452199074 | 55179.5002199074 | 404070010 | 92566 | 100000 | 92646 | 92566 | 0 | 92630 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 69434.4 | 69434.4 | 237989.8 | 2 | PROCESSED | 57549.8697222222 | 55567 | 55200.3941550926 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 042007 | We propose a 100 ks Suzaku observation of a Supergiant Fast X-ray Transient (SFXT) displaying periodic outbursts, IGRJ08408-4503, with the main aim of searching for cyclotron lines in its spectrum.This would be the first direct measurement of the neutron star magnetic field in this recently discovered class of HMXBs, and would be crucial in discriminating between different models for the outburst mechanisms, involving highly magnetized neutron stars (1E14 G) versus more typical magnetic fields of 1E12 G.The source is a SFXT displaying recurrent outbursts on short timescales (flaring every about 11 and 24 days).Because in most SFXTs the outbursts are not predictable, fast and difficult to observe,the SFXT we are proposing is a key system to understand the physical properties of this class. | GALACTIC POINT SOURCES | 4 | C | SIDOLI | LARA | NULL | NULL | EUR | 4 | AO4 | SEARCH FOR CYCLOTRON LINES IN THE X-RAY SPECTRUM OF THE SUPERGIANT FAST X-RAY TRANSIENT IGRJ08408-4503 | HXD | Y |
| GX 9+9 | 262.9404 | -16.8929 | 8.57505694 | 9.06920034 | 97.5329 | 55271.6738773148 | 55273.9918981482 | 404071010 | 85187.1 | 75000 | 85208.7 | 85203.1 | 0 | 85187.1 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 61694.2 | 61694.2 | 200263.9 | 0 | PROCESSED | 57550.9767476852 | 55652 | 55285.4179513889 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 042011 | We propose two 75 ks Suzaku observations of the bright neutron star low mass X-ray binary (LMXB) GX9+9, spread over six months. We will investigate the presence of X-ray narrow absorption features in the Suzaku spectra, which are a signature of a disk wind. Such features, identified with ions such as Fe XXV and Fe XXVI, have been observed in a number of LMXBs and give us information about the mass outflow rate and the launching mechanism of the wind. We will study the connection of the disk wind to the presence of radio jet emission with simultaneous radio observations. Finally, we will determine if the broad Fe emission line indicated by the XMM-Newton spectrum is relativistically broadened. Variability will be studied as a function of accretion rate in the two proposed observations. | GALACTIC POINT SOURCES | 4 | B | DIAZ TRIGO | MARIA | NULL | NULL | EUR | 4 | AO4 | A STUDY OF THE DISK WIND-JET CONNECTION IN GX9+9 WITH MULTIWAVELENGTH OBSERVATIONS | HXD | Y |
| CYGNUS X-1 | 299.5964 | 35.2723 | 71.39800953 | 3.09942804 | 95.8123 | 54924.0537384259 | 54924.5654282407 | 404075010 | 15309.1 | 300000 | 15309.1 | 15318.8 | 0 | 15310.8 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 15537.4 | 15537.4 | 44203.9 | 1 | PROCESSED | 57546.0113425926 | 54922 | 54949.4917824074 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 044131 | In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. | GALACTIC POINT SOURCES | 4 | A | MILLER | JON | YAMADA | SHIN | USJ | 4 | AO4 | A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE | HXD | Y |
| CYGNUS X-1 | 299.5895 | 35.2721 | 71.39489928 | 3.10413213 | 91.3103 | 54929.2562847222 | 54929.8224421296 | 404075020 | 21336.1 | 300000 | 21336.1 | 21336.1 | 0 | 21336.1 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 13125.8 | 13125.8 | 48914 | 0 | PROCESSED | 57546.0782638889 | 54922 | 54949.4903125 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 044131 | In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. | GALACTIC POINT SOURCES | 4 | A | MILLER | JON | YAMADA | SHIN | USJ | 4 | AO4 | A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE | HXD | Y |
| CYGNUS X-1 | 299.5891 | 35.272 | 71.39464341 | 3.10435878 | 91.3113 | 54935.7650462963 | 54936.1473958333 | 404075030 | 17108.8 | 300000 | 17108.8 | 17116.8 | 0 | 17108.8 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 12986 | 12986 | 33027.9 | 1 | PROCESSED | 57546.1452662037 | 54922 | 54949.5303240741 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 044131 | In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. | GALACTIC POINT SOURCES | 4 | A | MILLER | JON | YAMADA | SHIN | USJ | 4 | AO4 | A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE | HXD | Y |
| CYGNUS X-1 | 299.5791 | 35.2719 | 71.39029863 | 3.11127562 | 84.0536 | 54944.1674768518 | 54944.6252777778 | 404075040 | 18014 | 300000 | 18016.6 | 18014 | 0 | 18016.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16327.7 | 16327.7 | 39550 | 0 | PROCESSED | 57546.2094097222 | 54922 | 54966.3125 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 044131 | In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. | GALACTIC POINT SOURCES | 4 | A | MILLER | JON | YAMADA | SHIN | USJ | 4 | AO4 | A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE | HXD | Y |
| CYGNUS X-1 | 299.5814 | 35.2712 | 71.39067981 | 3.10930809 | 85.1433 | 54949.7099884259 | 54950.2175925926 | 404075050 | 20521.2 | 300000 | 20529.2 | 20535.4 | 0 | 20521.2 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 12401.3 | 12401.3 | 43845.9 | 0 | PROCESSED | 57546.4475462963 | 54922 | 54976.2030671296 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 044131 | In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. | GALACTIC POINT SOURCES | 4 | A | MILLER | JON | YAMADA | SHIN | USJ | 4 | AO4 | A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE | HXD | Y |
| CYGNUS X-1 | 299.5392 | 35.2589 | 71.36219421 | 3.13231837 | 55.3254 | 54957.7006828704 | 54958.1356365741 | 404075060 | 19434.5 | 300000 | 19434.5 | 19450.5 | 0 | 19434.5 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 15279.5 | 15279.5 | 37557.9 | 0 | PROCESSED | 57546.5121412037 | 54922 | 54976.0885300926 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 044131 | In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. | GALACTIC POINT SOURCES | 4 | A | MILLER | JON | YAMADA | SHIN | USJ | 4 | AO4 | A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE | HXD | Y |
| CYGNUS X-1 | 299.6653 | 35.165 | 71.33570459 | 2.99545336 | 212.8004 | 55182.0619328704 | 55182.5508564815 | 404075070 | 22101.9 | 300000 | 22101.9 | 22109.9 | 0 | 23664 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3460.7 | 3460.7 | 42236 | 0 | PROCESSED | 57549.8755671296 | 54922 | 55200.4490046296 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 044131 | In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. | GALACTIC POINT SOURCES | 4 | A | MILLER | JON | YAMADA | SHIN | USJ | 4 | AO4 | A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE | HXD | N |
| CYGNUS X-1 | 299.5434 | 35.2592 | 71.36423878 | 3.12954641 | 57.7977 | 54971.0242592593 | 54971.6043865741 | 404075080 | 21340.4 | 300000 | 21340.4 | 21348.4 | 0 | 21340.4 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 17495.4 | 17495.4 | 50119.9 | 1 | PROCESSED | 57546.6088888889 | 54922 | 54992.6546875 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 044131 | In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. | GALACTIC POINT SOURCES | 4 | A | MILLER | JON | YAMADA | SHIN | USJ | 4 | AO4 | A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE | HXD | Y |
| CYGNUS X-1 | 299.5373 | 35.2573 | 71.3600172 | 3.13281014 | 53.4895 | 54976.3582060185 | 54976.8259722222 | 404075090 | 20925.2 | 300000 | 20925.2 | 20933.2 | 0 | 20925.2 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 16116.4 | 16116.4 | 40412 | 1 | PROCESSED | 57546.6796296296 | 54922 | 54992.6651736111 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 044131 | In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. | GALACTIC POINT SOURCES | 4 | A | MILLER | JON | YAMADA | SHIN | USJ | 4 | AO4 | A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE | HXD | Y |
| CYGNUS X-1 | 299.5337 | 35.2545 | 71.35609035 | 3.13386262 | 50.0944 | 54980.4956712963 | 54981.0586226852 | 404075100 | 28784.5 | 300000 | 28784.5 | 28784.5 | 0 | 28784.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 25738.9 | 25738.9 | 48631.9 | 1 | PROCESSED | 57546.7292476852 | 54922 | 54994.3872800926 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 044131 | In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. | GALACTIC POINT SOURCES | 4 | A | MILLER | JON | YAMADA | SHIN | USJ | 4 | AO4 | A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE | HXD | Y |
| CYGNUS X-1 | 299.5294 | 35.2515 | 71.35169447 | 3.13529932 | 46.7675 | 54984.481400463 | 54984.9870833333 | 404075110 | 17450.2 | 300000 | 19037 | 17778.2 | 0 | 17450.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15040.9 | 15040.9 | 43687.9 | 1 | PROCESSED | 57547.4475462963 | 54922 | 54994.4091087963 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 044131 | In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. | GALACTIC POINT SOURCES | 4 | A | MILLER | JON | YAMADA | SHIN | USJ | 4 | AO4 | A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE | HXD | Y |
| CYGNUS X-1 | 299.5272 | 35.2497 | 71.34921869 | 3.1358965 | 44.7834 | 54986.8208333333 | 54987.3356944444 | 404075120 | 16873.3 | 300000 | 16881.3 | 16889.4 | 0 | 16873.3 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 6764.7 | 6764.7 | 44477.9 | 1 | PROCESSED | 57547.4806018518 | 54922 | 55001.0163078704 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 044131 | In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. | GALACTIC POINT SOURCES | 4 | A | MILLER | JON | YAMADA | SHIN | USJ | 4 | AO4 | A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE | HXD | Y |
| CYGNUS X-1 | 299.6021 | 35.1308 | 71.27949874 | 3.02171591 | 263.2299 | 55125.3772106482 | 55125.8404398148 | 404075130 | 20498.5 | 300000 | 20498.5 | 20506.5 | 0 | 20498.5 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 15163 | 15163 | 40015.9 | 0 | PROCESSED | 57548.9405208333 | 54922 | 55134.2701967593 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 044131 | In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. | GALACTIC POINT SOURCES | 4 | A | MILLER | JON | YAMADA | SHIN | USJ | 4 | AO4 | A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE | HXD | Y |
| CYGNUS X-1 | 299.6086 | 35.1319 | 71.28321336 | 3.01775246 | 259.2069 | 55130.2652314815 | 55130.7481365741 | 404075140 | 23104.2 | 300000 | 23104.2 | 23128.2 | 0 | 23120.2 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 20011 | 20011 | 41716 | 0 | PROCESSED | 57548.9943171296 | 54922 | 55141.3539467593 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 044131 | In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. | GALACTIC POINT SOURCES | 4 | A | MILLER | JON | YAMADA | SHIN | USJ | 4 | AO4 | A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE | HXD | Y |
| CYGNUS X-1 | 299.6206 | 35.1339 | 71.29004535 | 3.01042005 | 252.1788 | 55138.8946180556 | 55139.4106365741 | 404075150 | 22616.8 | 300000 | 22616.8 | 22624.8 | 0 | 22616.8 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 14061 | 14061 | 44575.9 | 1 | PROCESSED | 57549.0593981482 | 54922 | 55149.4202199074 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 044131 | In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. | GALACTIC POINT SOURCES | 4 | A | MILLER | JON | YAMADA | SHIN | USJ | 4 | AO4 | A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE | HXD | Y |
| CYGNUS X-1 | 299.6277 | 35.1371 | 71.29581116 | 3.00713364 | 246.5433 | 55145.8193981482 | 55146.4377199074 | 404075160 | 26022.2 | 300000 | 26022.2 | 26038.2 | 0 | 26026.5 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 18250.5 | 18250.5 | 53416 | 0 | PROCESSED | 57549.2577199074 | 54922 | 55176.2027430556 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 044131 | In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. | GALACTIC POINT SOURCES | 4 | A | MILLER | JON | YAMADA | SHIN | USJ | 4 | AO4 | A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE | HXD | Y |
| CYGNUS X-1 | 299.6355 | 35.1397 | 71.30136328 | 3.00304649 | 241.2259 | 55152.2855092593 | 55152.9418287037 | 404075170 | 23448.5 | 300000 | 23448.5 | 23888.5 | 0 | 23880.5 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 18707.1 | 18707.1 | 56691.8 | 3 | PROCESSED | 57549.4356597222 | 54922 | 55162.2019212963 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 044131 | In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. | GALACTIC POINT SOURCES | 4 | A | MILLER | JON | YAMADA | SHIN | USJ | 4 | AO4 | A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE | HXD | Y |
| CYGNUS X-1 | 299.6354 | 35.1397 | 71.30132058 | 3.00311627 | 241.1557 | 55159.514224537 | 55160.1328587963 | 404075180 | 21768.5 | 300000 | 21768.5 | 22480.5 | 0 | 22472.5 | 5 | 2 | 0 | 3 | 1 | 0 | 0 | 11406.4 | 11406.4 | 53435.8 | 0 | PROCESSED | 57549.5783680556 | 54922 | 55176.294849537 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 044131 | In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. | GALACTIC POINT SOURCES | 4 | A | MILLER | JON | YAMADA | SHIN | USJ | 4 | AO4 | A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE | HXD | Y |
| CYGNUS X-1 | 299.6537 | 35.1518 | 71.31947353 | 2.99665901 | 225.8159 | 55166.2922453704 | 55166.8904398148 | 404075190 | 22415.5 | 300000 | 22415.5 | 22431.5 | 0 | 22423.5 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 13157.8 | 13157.8 | 51673.9 | 0 | PROCESSED | 57549.6647222222 | 54922 | 55181.288912037 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 044131 | In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. | GALACTIC POINT SOURCES | 4 | A | MILLER | JON | YAMADA | SHIN | USJ | 4 | AO4 | A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE | HXD | Y |
| CYGNUS X-1 | 299.6549 | 35.1555 | 71.32314713 | 2.99775182 | 222.7295 | 55173.647349537 | 55174.1043287037 | 404075200 | 20016.6 | 300000 | 20016.6 | 21752.6 | 0 | 21859.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17442.6 | 17442.6 | 39471.9 | 0 | PROCESSED | 57549.7233912037 | 54922 | 55189.2752430556 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 044131 | In both stellar-mass and supermassive black holes, connections between X-ray flux and radio flux hint at disk-jet connections expected theoretically. The next step in this work is to move beyond fluxes, and tie the physical parameters of the disk to radio jet emission. Cygnus X-1 is bright and highly variable in both X-rays and radio bands; moreover, it is the only black hole that always permits two measurements of the disk (through disk continuum and broad Fe K disk line/reflection). We propose to observe Cygnus X-1 on 20 occasions for 15 ksec (each) during AO-4, simultaneously with the updated Ryle radio telescope. This will form a modest Large Program with public data access, and an important legacy dataset for Suzaku. This project addresses NASA Beyond Einstein science goals. | GALACTIC POINT SOURCES | 4 | A | MILLER | JON | YAMADA | SHIN | USJ | 4 | AO4 | A STRONG TEST OF DISK-JET CONNECTIONS IN AN ACCRETING BLACK HOLE | HXD | N |
| 1E 2259+586 | 345.2716 | 58.9493 | 109.11022544 | -0.92895504 | 86.3239 | 54976.8335300926 | 54978.6446064815 | 404076010 | 122579.1 | 120000 | 122580.9 | 122580.9 | 0 | 122579.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 103446.2 | 103446.2 | 156463.8 | 1 | PROCESSED | 57546.7298726852 | 54922 | 54992.6935069444 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 046002 | We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics". | GALACTIC POINT SOURCES | 4 | A | MAKISHIMA | KAZUO | NULL | NULL | JAP | 4 | AO4 | A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM | HXD | Y |
| SGR 1900+14 | 286.7986 | 9.3873 | 43.07377535 | 0.80526184 | 82.6704 | 54947.7664814815 | 54949.0807175926 | 404077010 | 53137.4 | 50000 | 53393.4 | 53393.4 | 0 | 53137.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42101.1 | 42101.1 | 113547.9 | 1 | PROCESSED | 57546.4694444444 | 54922 | 54973.4547222222 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 046002 | We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics". | GALACTIC POINT SOURCES | 4 | A | MAKISHIMA | KAZUO | NULL | NULL | JAP | 4 | AO4 | A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM | HXD | Y |
| SGR 0501+4516 | 75.2795 | 45.3414 | 161.49568149 | 1.98976538 | 93.3341 | 55060.8485069445 | 55061.8348842593 | 404078010 | 42675.3 | 40000 | 42675.3 | 42955.3 | 0 | 42891.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27487.8 | 27487.8 | 85185.8 | 0 | PROCESSED | 57548.1780092593 | 54922 | 55071.2594328704 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 046002 | We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics". | GALACTIC POINT SOURCES | 4 | A | MAKISHIMA | KAZUO | NULL | NULL | JAP | 4 | AO4 | A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM | HXD | Y |
| 4U0142+61 | 26.5176 | 61.8112 | 129.33625727 | -0.37933599 | 61.041 | 55055.0703125 | 55057.3654976852 | 404079010 | 107412.9 | 100000 | 107412.9 | 107420.9 | 0 | 107422.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 99757.6 | 99757.6 | 198283.8 | 2 | PROCESSED | 57548.2012152778 | 54922 | 55068.3037268518 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 046002 | We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics". | GALACTIC POINT SOURCES | 4 | A | MAKISHIMA | KAZUO | NULL | NULL | JAP | 4 | AO4 | A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM | HXD | Y |
| 1RXS J1708-4009 | 257.2032 | -40.2034 | 346.44001394 | -0.00188973 | 266.4021 | 55066.6841203704 | 55067.9466898148 | 404080010 | 60886.9 | 60000 | 60886.9 | 60894.9 | 0 | 60904.6 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 51531.3 | 51531.3 | 109075.8 | 1 | PROCESSED | 57548.350150463 | 54922 | 55078.1751851852 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 046002 | We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics". | GALACTIC POINT SOURCES | 4 | A | MAKISHIMA | KAZUO | NULL | NULL | JAP | 4 | AO4 | A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM | HXD | Y |
| PSR J1846-0258 | 281.5972 | -2.9106 | 29.7662115 | -0.20474108 | 86.0001 | 54936.8175578704 | 54939.6779398148 | 404081010 | 104345.1 | 100000 | 104345.1 | 104367.5 | 0 | 104353.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 76006.5 | 76006.5 | 247101.8 | 1 | PROCESSED | 57546.2746990741 | 54922 | 54959.5006018518 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 046002 | We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics". | GALACTIC POINT SOURCES | 4 | A | MAKISHIMA | KAZUO | NULL | NULL | JAP | 4 | AO4 | A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM | HXD | Y |
| IGR J15094-6649 | 227.3484 | -66.8278 | 315.91945149 | -7.50109233 | 90.4626 | 55588.7031365741 | 55589.5557638889 | 405007010 | 49461.2 | 50000 | 49483.2 | 49475.2 | 0 | 49461.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48018.5 | 48018.5 | 73659.9 | 0 | PROCESSED | 57600.7830092593 | 55990 | 55621.2282291667 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050025 | The all-sky survey in hard X-rays with INTEGRAL has been finding new magnetic Cataclysmic Variables. Among them, we propose Suzaku observations of five Intermediate Polars (IPs) which have no detailed follow-up spectroscopy in the hard X-ray band up to now. The wide-band energy coverage of Suzaku, therefore, is definitely useful to extract physical information from their spectra since, generally, the vFv spectrum of an IP peaks at E=20-50 keV and strong intrinsic absorption (nH=1E22-23 cm-2). By fitting the spectrum with our numerical model, we estimate a plasma temperature and an Fe abundance, and furthermore, a white dwarf mass which is one of the most basic and important parameter of a binary system. | GALACTIC POINT SOURCES | 4 | C | YUASA | TAKAYUKI | NULL | NULL | JAP | 5 | AO5 | ESTIMATE MASSES OF NEWLY-FOUND MAGNETIC WHITE DWARFS BASED ON HARD X-RAY CONTINUUM AND FE EMISSION LINES | XIS | Y |
| V773TAU | 63.5571 | 28.1952 | 168.22500409 | -16.34364304 | 260.6557 | 55610.1581712963 | 55611.9815277778 | 405011010 | 82246.3 | 80000 | 82254.3 | 82246.3 | 0 | 82254.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 72828.7 | 72828.7 | 157525.8 | 2 | PROCESSED | 57601.0256134259 | 55990 | 55621.2978703704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050033 | We propose a Suzaku observation of the pre-main sequence binary system V773 Tau with the high sensitivity of HXD. The empirical Lx-Lr relation (Benz-G"udel relation) and radio flux variation predict that this source can have a flare with a peak luminosity Lx=10^34 ergs s-1, seven orders of magnitude larger than that of the Sun, when it is just before the periastron passage. We will observe this target simultaneously with radio band using VLBI network. Our goal is (1) to test whether the gigantic flare is still on the empirical relation (2) to detect inpulsive non-thermal emission at the most powerful stellar flare (3) to establish unified view of stellar flare mechanism via the wide radio-X-ray band. | GALACTIC POINT SOURCES | 4 | B | TSUBOI | YOHKO | NULL | NULL | JAP | 5 | AO5 | NON-THERMAL EMISSION AT THE MOST POWERFUL STELLAR FLARE | XIS | Y |
| PSR J1429-5911 | 217.5051 | -59.1899 | 315.26780851 | 1.30018252 | 101.124 | 55588.2265625 | 55588.7001157407 | 405012010 | 30382.4 | 30000 | 30390.4 | 30398.4 | 0 | 30382.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 28792.3 | 28792.3 | 40903.9 | 0 | PROCESSED | 57600.7562384259 | 55968 | 55602.1404513889 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050047 | Fermi Gamma-Ray Space Telescope has detected more than 50 gamma-ray pulsars in its first year of operation. We propose Suzaku observation of 7 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. | GALACTIC POINT SOURCES | 4 | C | KAWAI | NOBUYUKI | NULL | NULL | JAP | 5 | AO5 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y |
| PSR J1044-5737 | 161.1338 | -57.616 | 286.57019106 | 1.16750605 | 109.1973 | 55542.2984259259 | 55542.7292939815 | 405013010 | 22630 | 30000 | 22630 | 22630 | 0 | 22635.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 21960.3 | 21960.3 | 37200 | 0 | PROCESSED | 57554.3753125 | 55917 | 55550.9648148148 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050047 | Fermi Gamma-Ray Space Telescope has detected more than 50 gamma-ray pulsars in its first year of operation. We propose Suzaku observation of 7 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. | GALACTIC POINT SOURCES | 4 | C | KAWAI | NOBUYUKI | NULL | NULL | JAP | 5 | AO5 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y |
| PSR J0614-33 | 93.5386 | -33.5015 | 240.50300829 | -21.83180137 | 119.1484 | 55498.9719675926 | 55499.6140740741 | 405014010 | 31210.9 | 30000 | 31210.9 | 31210.9 | 0 | 31210.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27331.4 | 27331.4 | 55449.9 | 0 | PROCESSED | 57553.8985763889 | 55875 | 55509.0359722222 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050047 | Fermi Gamma-Ray Space Telescope has detected more than 50 gamma-ray pulsars in its first year of operation. We propose Suzaku observation of 7 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. | GALACTIC POINT SOURCES | 4 | C | KAWAI | NOBUYUKI | NULL | NULL | JAP | 5 | AO5 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y |
| PSR J2055+2539 | 313.957 | 25.6505 | 70.67687842 | -12.53222207 | 262.3229 | 55498.1479398148 | 55498.9578356482 | 405015010 | 31106.9 | 30000 | 31106.9 | 31106.9 | 0 | 31106.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 21458.1 | 21458.1 | 69967.9 | 0 | PROCESSED | 57553.8967592593 | 55890 | 55523.9927314815 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050047 | Fermi Gamma-Ray Space Telescope has detected more than 50 gamma-ray pulsars in its first year of operation. We propose Suzaku observation of 7 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. | GALACTIC POINT SOURCES | 4 | C | KAWAI | NOBUYUKI | NULL | NULL | JAP | 5 | AO5 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y |
| PSR J1957+5036 | 299.4354 | 50.5474 | 84.58480161 | 10.99652902 | 216.5649 | 55543.4586689815 | 55544.0842939815 | 405016010 | 32469 | 30000 | 32485 | 32469 | 0 | 32485 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25313.9 | 25313.9 | 54033.9 | 2 | PROCESSED | 57554.3965393518 | 55959 | 55592.9341782407 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050047 | Fermi Gamma-Ray Space Telescope has detected more than 50 gamma-ray pulsars in its first year of operation. We propose Suzaku observation of 7 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. | GALACTIC POINT SOURCES | 4 | C | KAWAI | NOBUYUKI | NULL | NULL | JAP | 5 | AO5 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y |
| V2487 OPH | 262.9946 | -19.3061 | 6.53905762 | 7.73892052 | 274.1277 | 55478.2880439815 | 55479.5827893518 | 405021010 | 56307.6 | 50000 | 56315.6 | 56307.6 | 0 | 56323.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51358 | 51358 | 111832 | 2 | PROCESSED | 57553.6771875 | 55854 | 55488.179224537 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050059 | Suzaku discovery of the first white dwarf pulsar, AE Aqr (Terada et.al 2008) had a great impact on the studies of the cosmic-ray origin, since white dwarfs were not recognized as a particle accelerator. The next step is to check whether this phenomenon is common or not. In order to search for the second white dwarf pulsar, we picked up hard objects among the INTEGRAL and Swift sample, and propose the Suzaku observation of the best two objects, V2487 Oph and IGRJ00234+6141. | GALACTIC POINT SOURCES | 4 | A | TERADA | YUKIKATSU | NULL | NULL | JAP | 5 | AO5 | SEARCH FOR NON-THERMAL EMISSION FROM HARD WHITE DWARFS WITH SUZAKU | HXD | Y |
| IGR J00234+6141 | 5.7092 | 61.7549 | 119.55446517 | -0.92914674 | 80.286 | 55372.004375 | 55373.2397569445 | 405022010 | 81880 | 80000 | 81880 | 81880 | 0 | 81880 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70036.4 | 70036.4 | 106697.9 | 1 | PROCESSED | 57552.4371759259 | 55780 | 55414.1791666667 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050059 | Suzaku discovery of the first white dwarf pulsar, AE Aqr (Terada et.al 2008) had a great impact on the studies of the cosmic-ray origin, since white dwarfs were not recognized as a particle accelerator. The next step is to check whether this phenomenon is common or not. In order to search for the second white dwarf pulsar, we picked up hard objects among the INTEGRAL and Swift sample, and propose the Suzaku observation of the best two objects, V2487 Oph and IGRJ00234+6141. | GALACTIC POINT SOURCES | 4 | A | TERADA | YUKIKATSU | NULL | NULL | JAP | 5 | AO5 | SEARCH FOR NON-THERMAL EMISSION FROM HARD WHITE DWARFS WITH SUZAKU | HXD | Y |
| 1E 1547.0-5408 | 237.7284 | -54.3676 | 327.20000551 | -0.18012949 | 271.1663 | 55415.1611921296 | 55415.9633796296 | 405024010 | 51672.8 | 50000 | 51672.8 | 51792.8 | 0 | 52152.9 | 2 | 2 | 0 | 1 | 1 | 0 | 0 | 42781.2 | 42781.2 | 69299.9 | 0 | PROCESSED | 57552.8870949074 | 55793 | 55427.247025463 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050099 | Recently, hard X-ray tails have been detected by INTEGRAL at least up to 150 keV from ~5 magnetars. Suzaku has observed some magnetars during Key Project (AO-4) and ToO observations. As a result, soft X-ray emissions and hard X-ray tails have been detected from ~10 magnetars. This peculiar spectrum is seem to be common in all the magnetars, and we discovered the spectral evolution of magnetars. The remaining problem is to study the spectral difference between the active and quiescent states. Transient magnetar 1E 1547.0-540 was observed with Suzaku in 2009 January, and the extremely hard X-ray tail was detected up to 110 keV with photon index of 1.5, and it is appropriate to study the spectral change. Thus, we propose the observation of 1E 1547.0-5408 with 50 ks. | GALACTIC POINT SOURCES | 4 | B | NISHIOKA | HIROYUKI | NULL | NULL | JAP | 5 | AO5 | OBSERVATION OF THE HARD X-RAY TAIL AND SOFT X-RAY EMISSION OF AXP 1E 1547.0-5408 IN QUIESCENT STATE | HXD | N |
| EMS0918 | 211.2948 | -61.3938 | 311.64055354 | 0.22486043 | 106.822 | 55589.5588310185 | 55590.0834837963 | 405025010 | 24542.5 | 20000 | 24550.5 | 24542.5 | 0 | 24558.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 23281.1 | 23281.1 | 45309.9 | 1 | PROCESSED | 57600.7734606482 | 55972 | 55602.2015046296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050104 | Fermi discovered a lot of unidentified GeV sources in the Galactic plane. Among them, some of the low-latitude unIDs show "pulsar-like" cutoff power-law spectra with the cutoff energy of 1-5 GeV. We propose to search for X-ray counterparts of these unIDs. Using an X-ray spectral shape and a time variability, we would be able to identify these objects as pulsars. In addition, we search for diffuse X-ray emission around the targets. Finally, we investigate acceleration mechanisms which work in pulsars based on a broadband spectrum from X-ray to GeV. | GALACTIC POINT SOURCES | 4 | A | TANAKA | YASUYUKI | NULL | NULL | JAP | 5 | AO5 | SEARCH FOR X-RAY COUNTERPARTS OF FERMI "PULSAR-LIKE" LOW-LATITUDE UNIDENTIFIED GEV SOURCES | XIS | Y |
| EMS1150 | 263.083 | -32.7212 | 355.27740066 | 0.39306698 | 91.2452 | 55611.9964930556 | 55612.6968055556 | 405026010 | 20918.6 | 20000 | 20918.6 | 20918.6 | 0 | 20918.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17263.9 | 17263.9 | 60503.9 | 0 | PROCESSED | 57600.9777893518 | 55988 | 55621.1440740741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050104 | Fermi discovered a lot of unidentified GeV sources in the Galactic plane. Among them, some of the low-latitude unIDs show "pulsar-like" cutoff power-law spectra with the cutoff energy of 1-5 GeV. We propose to search for X-ray counterparts of these unIDs. Using an X-ray spectral shape and a time variability, we would be able to identify these objects as pulsars. In addition, we search for diffuse X-ray emission around the targets. Finally, we investigate acceleration mechanisms which work in pulsars based on a broadband spectrum from X-ray to GeV. | GALACTIC POINT SOURCES | 4 | A | TANAKA | YASUYUKI | NULL | NULL | JAP | 5 | AO5 | SEARCH FOR X-RAY COUNTERPARTS OF FERMI "PULSAR-LIKE" LOW-LATITUDE UNIDENTIFIED GEV SOURCES | XIS | Y |
| EMS01095 | 252.3381 | -45.0256 | 340.43907916 | -0.17827348 | 87.5534 | 55603.1544328704 | 55603.7613310185 | 405027010 | 20933.2 | 20000 | 20934.4 | 20934.4 | 0 | 20933.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16976.2 | 16976.2 | 52431.9 | 0 | PROCESSED | 57600.9093055556 | 55983 | 55617.4127430556 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050104 | Fermi discovered a lot of unidentified GeV sources in the Galactic plane. Among them, some of the low-latitude unIDs show "pulsar-like" cutoff power-law spectra with the cutoff energy of 1-5 GeV. We propose to search for X-ray counterparts of these unIDs. Using an X-ray spectral shape and a time variability, we would be able to identify these objects as pulsars. In addition, we search for diffuse X-ray emission around the targets. Finally, we investigate acceleration mechanisms which work in pulsars based on a broadband spectrum from X-ray to GeV. | GALACTIC POINT SOURCES | 4 | A | TANAKA | YASUYUKI | NULL | NULL | JAP | 5 | AO5 | SEARCH FOR X-RAY COUNTERPARTS OF FERMI "PULSAR-LIKE" LOW-LATITUDE UNIDENTIFIED GEV SOURCES | XIS | Y |
| EMS1308 | 293.0393 | 19.2567 | 54.62289289 | 0.10827332 | 90.0001 | 55313.4365740741 | 55313.9766203704 | 405028010 | 23898.7 | 20000 | 23906.7 | 23906.7 | 0 | 23898.7 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 23209 | 23209 | 46652 | 1 | PROCESSED | 57551.306400463 | 55693 | 55327.1789930556 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050104 | Fermi discovered a lot of unidentified GeV sources in the Galactic plane. Among them, some of the low-latitude unIDs show "pulsar-like" cutoff power-law spectra with the cutoff energy of 1-5 GeV. We propose to search for X-ray counterparts of these unIDs. Using an X-ray spectral shape and a time variability, we would be able to identify these objects as pulsars. In addition, we search for diffuse X-ray emission around the targets. Finally, we investigate acceleration mechanisms which work in pulsars based on a broadband spectrum from X-ray to GeV. | GALACTIC POINT SOURCES | 4 | A | TANAKA | YASUYUKI | NULL | NULL | JAP | 5 | AO5 | SEARCH FOR X-RAY COUNTERPARTS OF FERMI "PULSAR-LIKE" LOW-LATITUDE UNIDENTIFIED GEV SOURCES | XIS | Y |
| V1280 SCO | 254.4172 | -32.3368 | 351.33470039 | 6.5596985 | 97.7451 | 55605.3662615741 | 55608.0501851852 | 405029010 | 99683 | 100000 | 99699 | 99683 | 0 | 99699 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 86930.6 | 86930.6 | 231873.9 | 2 | PROCESSED | 57600.9978472222 | 55983 | 55617.4142361111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050110 | We propose a 100 ks observation of the C-rich classical nova V1280 Sco. Using Suzaku's excellent spectral performance in the soft X-ray energy band, we aim to detect and to resolve emission lines from C, N, and O. | GALACTIC POINT SOURCES | 4 | A | TAKEI | DAI | NULL | NULL | JAP | 5 | AO5 | X-RAY SPECTROSCOPY OF THE C-RICH CLASSICAL NOVA V1280 SCO | XIS | Y |
| HD125599 | 215.4515 | -48.0762 | 318.15137849 | 12.10713587 | 289.1653 | 55414.6760069444 | 55415.1571990741 | 405030010 | 31048 | 30000 | 31056 | 31056 | 0 | 31048 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 24859.9 | 24859.9 | 41567.9 | 0 | PROCESSED | 57552.8615277778 | 55793 | 55427.1753819444 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050116 | Recently, an ultra-deep Chandra observation was conducted to resolve the Galactic Ridge X-ray Emission (GRXE), and more than 80 percent of the GRXE was resolved into point sources in the iron energy band. However, we do not know what these point sources are, that have strong iron line emission. We have compared the GRXE iron line structure and those of cataclysmic variables (CVs) using Suzaku, and found that the CVs tend to emit stronger H-like line at 6.97 keV compared to the GRXE. We need another kind of sources which preferentially emit 6.7 keV line to explain the GRXE. We propose to study iron line structures of four active binary candidates from the XTE Slew Survey catalog, which are candidates of the 6.7 keV line sources. | GALACTIC POINT SOURCES | 4 | B | EBISAWA | KEN | NULL | NULL | JAP | 5 | AO5 | QUEST FOR THE 6.7 KEV LINE SOURCES TO EXPLAIN THE GALACTIC RIDGE EMISSION | XIS | Y |
| HD130693 | 222.5749 | -24.4173 | 334.71293898 | 31.01917553 | 104.6337 | 55580.6525925926 | 55581.2384375 | 405031010 | 21314.5 | 20000 | 21314.5 | 21314.5 | 0 | 21314.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17462.5 | 17462.5 | 50605.9 | 2 | PROCESSED | 57600.6648842593 | 55965 | 55598.9831597222 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050116 | Recently, an ultra-deep Chandra observation was conducted to resolve the Galactic Ridge X-ray Emission (GRXE), and more than 80 percent of the GRXE was resolved into point sources in the iron energy band. However, we do not know what these point sources are, that have strong iron line emission. We have compared the GRXE iron line structure and those of cataclysmic variables (CVs) using Suzaku, and found that the CVs tend to emit stronger H-like line at 6.97 keV compared to the GRXE. We need another kind of sources which preferentially emit 6.7 keV line to explain the GRXE. We propose to study iron line structures of four active binary candidates from the XTE Slew Survey catalog, which are candidates of the 6.7 keV line sources. | GALACTIC POINT SOURCES | 4 | B | EBISAWA | KEN | NULL | NULL | JAP | 5 | AO5 | QUEST FOR THE 6.7 KEV LINE SOURCES TO EXPLAIN THE GALACTIC RIDGE EMISSION | XIS | Y |
| XSS J16537-1905 | 253.8855 | -18.1447 | 2.56699105 | 15.52634316 | 96.7569 | 55602.7046412037 | 55603.1488657407 | 405032010 | 20024.3 | 20000 | 20032.3 | 20040.3 | 0 | 20024.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18152.8 | 18152.8 | 38343.9 | 0 | PROCESSED | 57600.887337963 | 55983 | 55617.4104282407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050116 | Recently, an ultra-deep Chandra observation was conducted to resolve the Galactic Ridge X-ray Emission (GRXE), and more than 80 percent of the GRXE was resolved into point sources in the iron energy band. However, we do not know what these point sources are, that have strong iron line emission. We have compared the GRXE iron line structure and those of cataclysmic variables (CVs) using Suzaku, and found that the CVs tend to emit stronger H-like line at 6.97 keV compared to the GRXE. We need another kind of sources which preferentially emit 6.7 keV line to explain the GRXE. We propose to study iron line structures of four active binary candidates from the XTE Slew Survey catalog, which are candidates of the 6.7 keV line sources. | GALACTIC POINT SOURCES | 4 | B | EBISAWA | KEN | NULL | NULL | JAP | 5 | AO5 | QUEST FOR THE 6.7 KEV LINE SOURCES TO EXPLAIN THE GALACTIC RIDGE EMISSION | XIS | Y |
| XSS J17223-7301 | 259.6949 | -73.4263 | 319.10640118 | -19.70481928 | 106.6643 | 55302.152650463 | 55302.5939467593 | 405033010 | 33386.1 | 30000 | 33386.1 | 33386.1 | 0 | 33386.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25588.9 | 25588.9 | 38127.9 | 0 | PROCESSED | 57551.2373726852 | 55692 | 55326.1437731482 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050116 | Recently, an ultra-deep Chandra observation was conducted to resolve the Galactic Ridge X-ray Emission (GRXE), and more than 80 percent of the GRXE was resolved into point sources in the iron energy band. However, we do not know what these point sources are, that have strong iron line emission. We have compared the GRXE iron line structure and those of cataclysmic variables (CVs) using Suzaku, and found that the CVs tend to emit stronger H-like line at 6.97 keV compared to the GRXE. We need another kind of sources which preferentially emit 6.7 keV line to explain the GRXE. We propose to study iron line structures of four active binary candidates from the XTE Slew Survey catalog, which are candidates of the 6.7 keV line sources. | GALACTIC POINT SOURCES | 4 | B | EBISAWA | KEN | NULL | NULL | JAP | 5 | AO5 | QUEST FOR THE 6.7 KEV LINE SOURCES TO EXPLAIN THE GALACTIC RIDGE EMISSION | XIS | Y |
| EG AND | 11.168 | 40.673 | 121.54657283 | -22.18054863 | 225.2111 | 55597.6281018518 | 55600.0030092593 | 405034010 | 100533.3 | 100000 | 100533.3 | 100541.3 | 0 | 100549.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 84658.9 | 84658.9 | 205171.9 | 3 | PROCESSED | 57600.9241666667 | 55983 | 55614.2972106482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051211 | The goals of this proposal are to use Suzaku XIS observations to : 1) determine whether EG And, BX Mon, and BF Cyg are members of the recently recognized class of hard X-ray emitting symbiotic stars; and 2) if they are, compare the nature of any absorption, the optical depth of the boundary layer, and the accretion rate to those of the well established hard X-ray symbiotics. Understanding the accretion processes in symbiotic stars is a crucial step in determining the role they play as progenitors of type Ia supernovae. | GALACTIC POINT SOURCES | 4 | C | NELSON | THOMAS | NULL | NULL | USA | 5 | AO5 | EXPLORING THE ACCRETION DISK BOUNDARY LAYERS OF SYMBIOTIC STARS | XIS | Y |
| 4 DRA | 187.4841 | 69.1938 | 125.77229084 | 47.81569563 | 339.9969 | 55304.8913773148 | 55305.8557291667 | 405035010 | 42260.2 | 40000 | 42268.2 | 42268.2 | 0 | 42260.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43792 | 43792 | 83277.8 | 1 | PROCESSED | 57551.2555439815 | 55693 | 55327.2173958333 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051212 | The symbiotic star, 4 Dra, has been poorly studied in X-rays. Based on the ROSAT data, we argue that it is a nearby, lower accretion rate analogue of the hard X-ray bright symibiotic stars that have been detected above 10 keV. We propose the first pointed observation of 4 Dra that covers the entire 0.4-10 keV band to test our interpretation: we expect it to be bright above 2 keV, with an optically thin thermal spectrum, likely with a strong and complex intrinsic absorber. If confirmed, 4 Dra may turn out to be a key object in the study of hard X-ray emitting symbiotic stars. | GALACTIC POINT SOURCES | 4 | B | MUKAI | KOJI | NULL | NULL | USA | 5 | AO5 | THE FIRST LOOK AT THE SYMBIOTIC STAR 4 DRA ABOVE 2 KEV | XIS | Y |
| V2491 CYG | 295.7679 | 32.3068 | 67.2208484 | 4.33923679 | 253.6206 | 55503.4390162037 | 55505.2709837963 | 405036010 | 74400.4 | 70000 | 74400.4 | 74400.4 | 0 | 74400.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 57206.5 | 57206.5 | 158251.9 | 2 | PROCESSED | 57553.9866087963 | 55885 | 55518.4178356482 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051213 | We propose to observe again one of the most luminous and intriguing classical novae of the last two years, after it has returned to quiescence. The goala are to understand how accretion is re-estabilished, investigate the claim that the white dwarf an intermediate polar (IP), estimate mass accretion are and white dwarf mass. IP are a class of X-ray sources that Suzaku is ideally suited to study, and we want to study the influence of the magnetic field on the nova evolution. | GALACTIC POINT SOURCES | 4 | C | ORIO | MARINA | NULL | NULL | USA | 5 | AO5 | REVISITING AN X-RAY LUMINOUS NOVA NOVA AFTER THE ERUPTION | XIS | Y |
| PSR B1259-63 | 195.6931 | -63.8349 | 304.18120501 | -0.9906484 | 99.8696 | 55566.8369212963 | 55569.3959722222 | 405037010 | 90040.7 | 80000 | 90040.7 | 90040.7 | 0 | 90040.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 74450.6 | 74450.6 | 221061.8 | 1 | PROCESSED | 57600.639375 | 55961 | 55595.2642939815 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051221 | We propose to observe a gamma-ray binary PSR B1259-63 during the pulsar's second disk crossing after periastron passage. PSR B1259-63 is a young radio pulsar orbiting around a B2e star with a highly eccentric 3.4 yr orbit. Suzaku XIS+HXD measurements of the hard continuum emission from the binary system allow us to investigate particle acceleration in a highly variable environment as a result of interactions between the relativistic wind of the pulsar and the circumstellar disk of the Be star. With the advent of the Fermi Gamma-ray Space Telescope, we will be able to simultaneously observe X-rays and GeV gamma-rays during the disk transit for the first time. The observations of PSR B1259-63 will give us a unique opportunity to study the physics of pulsar winds on AU-scale. | GALACTIC POINT SOURCES | 4 | A | UCHIYAMA | YASUNOBU | NULL | NULL | USA | 5 | AO5 | SUZAKU BROADBAND OBSERVATIONS OF A GAMMA-RAY BINARY PSRB1259-63 DURING THE POST-PERIASTRON FLARE IN 2011 | XIS | Y |
| PSR B1259-63 | 195.6913 | -63.8356 | 304.18038114 | -0.9913128 | 117.5773 | 55594.1927662037 | 55594.4487731482 | 405038010 | 21478.1 | 20000 | 21494.1 | 21478.1 | 0 | 21494.1 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15677.4 | 15677.4 | 22111.9 | 0 | PROCESSED | 57600.7966435185 | 55974 | 55607.1295601852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051221 | We propose to observe a gamma-ray binary PSR B1259-63 during the pulsar's second disk crossing after periastron passage. PSR B1259-63 is a young radio pulsar orbiting around a B2e star with a highly eccentric 3.4 yr orbit. Suzaku XIS+HXD measurements of the hard continuum emission from the binary system allow us to investigate particle acceleration in a highly variable environment as a result of interactions between the relativistic wind of the pulsar and the circumstellar disk of the Be star. With the advent of the Fermi Gamma-ray Space Telescope, we will be able to simultaneously observe X-rays and GeV gamma-rays during the disk transit for the first time. The observations of PSR B1259-63 will give us a unique opportunity to study the physics of pulsar winds on AU-scale. | GALACTIC POINT SOURCES | 4 | A | UCHIYAMA | YASUNOBU | NULL | NULL | USA | 5 | AO5 | SUZAKU BROADBAND OBSERVATIONS OF A GAMMA-RAY BINARY PSRB1259-63 DURING THE POST-PERIASTRON FLARE IN 2011 | XIS | Y |
| XTE J1946+274 | 296.4201 | 27.2906 | 63.14511565 | 1.35338176 | 267.925 | 55480.9086805556 | 55482.2446064815 | 405041010 | 50731.7 | 45000 | 50731.7 | 50731.7 | 0 | 50731.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46557.1 | 46557.1 | 115373.9 | 1 | PROCESSED | 57553.7260185185 | 55867 | 55491.1017476852 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051231 | We propose to perform Target of Opportunity Observations of one accreting neutron star out of a sample of five in outburst during Suzaku's AO-5. The aim is to observe the source for 45 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) in this system and to constrain the broad band spectrum. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 5 | AO5-TOO | CYCLOTRON RESONANCE SCATTERING FEATURES IN TRANSIENT ACCRETING X-RAY PULSARS WITH SUZAKU | HXD | Y |
| 4U 1626-67 | 248.0734 | -67.4643 | 321.7866399 | -13.09493758 | 285.8172 | 55445.5409259259 | 55446.2376273148 | 405044010 | 20033.5 | 20000 | 20033.5 | 20057.5 | 0 | 20045.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19537.2 | 19537.2 | 60179.9 | 0 | PROCESSED | 57553.3082175926 | 55822 | 55456.2336574074 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051234 | Recent X-ray observations by Fermi/GBM and Swift/BAT of 4U 1626-67 discovered a new torque reversal of this source after 18 years of steady spinning down. Centered on Feb 4 2008, a dramatic increase in the X-ray flux was also observed. The lack of correlation between the X-ray flux and the torque applied to the neutron star before the transition, challenges our understanding of the physical mechanisms operating in this system. The main goal of this proposal is to look for changes in the long term flux behavior, energy spectra, pulse profile, line features and power spectra with the current evolution in 4U1626-67 s spin-up rate. In addition, we wish to determine whether the absence of the QPO observed just after the torque reversal persist. | GALACTIC POINT SOURCES | 4 | A | FINGER | MARK | NULL | NULL | USA | 5 | AO5 | THE ACCRETING X-RAY PULSAR 4U 1626-67 AFTER A NEW TORQUE REVERSAL | XIS | Y |
| 4U 1210-64 | 183.3036 | -64.8719 | 298.88624165 | -2.30082607 | 98.4956 | 55553.1591550926 | 55555.1488194444 | 405045010 | 79347.6 | 80000 | 79347.6 | 79347.6 | 0 | 79356.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70751.2 | 70751.2 | 171879.9 | 0 | PROCESSED | 57554.5554398148 | 55961 | 55595.085474537 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051236 | 4U 1210-64 is a high mass X-ray binary with a stable 6.7 day period when the long-term (RXTE ASM) light curve is analyzed. However, we observed strong aperiodic variability in a series of pointed observations with the RXTE PCA, to the point of masking this 6.7 day period. Moreover, we have not detected a spin period, even though the accretor is most likely a neutron star. The strong variability is suggestive of accretion from a clumpy wind. We propose a 2-day Suzaku observation of this object (1) to search for unequivocal evidence for a neutron star, such as the spin period and cyclotron features; and (2) to measure the spectral shapes at different flux levels, to investigate the cause of the strong aperiodic variability. | GALACTIC POINT SOURCES | 4 | C | MUKAI | KOJI | NULL | NULL | USA | 5 | AO5 | 4U 1210-64: A HIGHLY VARIABLE X-RAY BINARY | XIS | Y |
| 4U 1728-34 | 262.9799 | -33.9051 | 354.23908298 | -0.18221646 | 278.0266 | 55473.517349537 | 55475.6876967593 | 405048010 | 50547.2 | 100000 | 50652.2 | 50547.2 | 0 | 50652.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 95360.6 | 95360.6 | 187467.8 | 3 | PROCESSED | 57553.6884490741 | 55867 | 55487.4662615741 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051244 | Fe K-alpha lines have been detected in ten NS-LMXBs. Under the commonly accepted interpretation, they can be used to set tight constrains on the accretion disk geometry. In two of these systems, the inner radius of the accretion disk as inferred from the line profile appears to be consistent with the radius inferred from the frequency of the kHz QPOs. We have recently shown that simultaneous measurements of Fe lines and kHz QPOs in a NS-LMXB appear to contradict this picture. We propose to observe 4U 1728-34 with Suzaku five times for 20 ks, simultaneously with RXTE and ATCA. This program will allow us to study and compare the dynamics of the inner edge of the disk as inferred from the Fe line and the kHz QPOs, as well as the relation of both observables with the jet radio emission. | GALACTIC POINT SOURCES | 4 | A | LINARES | MANUEL | NULL | NULL | USA | 5 | AO5 | ACCRETION DISKS IN STRONG GRAVITY: FE LINES VS. KHZ QPOS AND SPECTRAL STATES. | HXD | Y |
| 4U 1630-47 | 248.5034 | -47.402 | 336.90313759 | 0.24577164 | 279.8256 | 55432.911724537 | 55435.6134259259 | 405051010 | 99937.3 | 100000 | 99937.3 | 99937.3 | 0 | 99937.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 90451.2 | 90451.2 | 233397.6 | 2 | PROCESSED | 57553.2849652778 | 55815 | 55449.4369560185 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051252 | Understanding black hole systems in their canonical hard state is a major goal of high energy astrophysics. This state features a hard X-ray spectrum, a high level of timing noise, and emission from a steady jet at radio, IR, and perhaps higher frequencies. Along with radio observations, Suzaku is constraining theoretical models by answering the following questions: Does the inner edge of the accretion disk recede in the hard state? How is the location of the disk's inner edge related to the presence of a jet? Here, we propose to extend X-ray and radio studies of the hard state to low flux levels in order to answer these questions. | GALACTIC POINT SOURCES | 4 | A | TOMSICK | JOHN | NULL | NULL | USA | 5 | AO5-TOO | CONSTRAINING THE HARD STATE ACCRETION GEOMETRY FOR BLACK HOLE BINARIES | XIS | Y |
| 4U 1957+11 | 299.8426 | 11.72 | 51.31417386 | -9.31797438 | 71.6227 | 55320.4377777778 | 55321.4168055556 | 405057010 | 35796 | 35000 | 35804 | 35804 | 0 | 35796 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30869.2 | 30869.2 | 84580 | 0 | PROCESSED | 57551.4086226852 | 55741 | 55375.7567013889 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051254 | We propose three observations of the black hole candidate 4U 1957+11. It is one of only two persistently soft state BHC, and has the highest fitted temperature, and highest fitted spin parameter, of any observed BHC. The question arises of whether this high spin is a good estimate of the true spin, or whether this high temperature is evidence of a low level or corona or wind. The multiple Suzaku observations will allow us to track how the disk parameters change, and offer us a 40% chance of observing a state with a large coronal component. The latter might be indicative of launching of a disk wind. | GALACTIC POINT SOURCES | 4 | B | NOWAK | MICHAEL | NULL | NULL | USA | 5 | AO5 | 4U1957+11: THE MOST RAPIDLY SPINNING BLACK HOLE? | XIS | Y |
| 4U 1957+11 | 299.8418 | 11.7197 | 51.31351001 | -9.31745051 | 63.9325 | 55333.5190277778 | 55334.4675 | 405057020 | 34935.3 | 35000 | 34943.3 | 34951.3 | 0 | 34935.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28262.5 | 28262.5 | 81911.8 | 0 | PROCESSED | 57551.562650463 | 55714 | 55347.2466898148 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051254 | We propose three observations of the black hole candidate 4U 1957+11. It is one of only two persistently soft state BHC, and has the highest fitted temperature, and highest fitted spin parameter, of any observed BHC. The question arises of whether this high spin is a good estimate of the true spin, or whether this high temperature is evidence of a low level or corona or wind. The multiple Suzaku observations will allow us to track how the disk parameters change, and offer us a 40% chance of observing a state with a large coronal component. The latter might be indicative of launching of a disk wind. | GALACTIC POINT SOURCES | 4 | B | NOWAK | MICHAEL | NULL | NULL | USA | 5 | AO5 | 4U1957+11: THE MOST RAPIDLY SPINNING BLACK HOLE? | XIS | Y |
| 4U 1957+11 | 299.8589 | 11.6979 | 51.30303986 | -9.34292333 | 251.3459 | 55501.8275462963 | 55502.7001157407 | 405057030 | 35349.1 | 35000 | 35357.1 | 35349.1 | 0 | 35357.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27169.7 | 27169.7 | 75362 | 0 | PROCESSED | 57553.9520601852 | 55881 | 55515.3015046296 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051254 | We propose three observations of the black hole candidate 4U 1957+11. It is one of only two persistently soft state BHC, and has the highest fitted temperature, and highest fitted spin parameter, of any observed BHC. The question arises of whether this high spin is a good estimate of the true spin, or whether this high temperature is evidence of a low level or corona or wind. The multiple Suzaku observations will allow us to track how the disk parameters change, and offer us a 40% chance of observing a state with a large coronal component. The latter might be indicative of launching of a disk wind. | GALACTIC POINT SOURCES | 4 | B | NOWAK | MICHAEL | NULL | NULL | USA | 5 | AO5 | 4U1957+11: THE MOST RAPIDLY SPINNING BLACK HOLE? | XIS | Y |
| HER X-1 | 254.4936 | 35.2712 | 58.06646448 | 37.48255114 | 250.0637 | 55467.7830208333 | 55468.2362962963 | 405058010 | 21356.7 | 20000 | 21356.7 | 21356.7 | 0 | 21503.4 | 2 | 2 | 0 | 1 | 1 | 0 | 0 | 18932.3 | 18932.3 | 39159.9 | 0 | PROCESSED | 57553.5804050926 | 55843 | 55477.2237152778 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 052001 | We propose to observe Her X-1 during Suzaku s AO-5 for a total observing time of 80 ksec, covering one Main-On with four observations of 20 ks each: the first two during the flux maximum and the remaining two during the decay of the Main-On. Our prime objective is to systematically study the centroid energy of the fundamental cyclotron line Ecyc as a function of time, X-ray flux, 35 day phase and 1.24 s phase. These observations will contribute to answering the following questions: Is there a slow secular decrease in the value of Ecyc with time? Does Ecyc depend on 35 day phase? How stable is the positive correlation of the value of Ecyc with the X-ray luminosity? | GALACTIC POINT SOURCES | 4 | B | STAUBERT | R DIGER | NULL | NULL | EUR | 5 | AO5 | VARIABILITY OF THE CYCLOTRON LINE ENERGY E_CYC IN HERCULES X-1 | HXD | N |
| HER X-1 | 254.4925 | 35.2707 | 58.06565994 | 37.48335671 | 250.2455 | 55468.7003356482 | 55469.2258912037 | 405058020 | 24303 | 20000 | 24303 | 24322.3 | 0 | 24467.7 | 2 | 2 | 0 | 1 | 1 | 0 | 0 | 22483.7 | 22483.7 | 45405.9 | 0 | PROCESSED | 57553.5917476852 | 55848 | 55482.4726967593 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 052001 | We propose to observe Her X-1 during Suzaku s AO-5 for a total observing time of 80 ksec, covering one Main-On with four observations of 20 ks each: the first two during the flux maximum and the remaining two during the decay of the Main-On. Our prime objective is to systematically study the centroid energy of the fundamental cyclotron line Ecyc as a function of time, X-ray flux, 35 day phase and 1.24 s phase. These observations will contribute to answering the following questions: Is there a slow secular decrease in the value of Ecyc with time? Does Ecyc depend on 35 day phase? How stable is the positive correlation of the value of Ecyc with the X-ray luminosity? | GALACTIC POINT SOURCES | 4 | B | STAUBERT | R DIGER | NULL | NULL | EUR | 5 | AO5 | VARIABILITY OF THE CYCLOTRON LINE ENERGY E_CYC IN HERCULES X-1 | HXD | N |
| HER X-1 | 254.4632 | 35.2657 | 58.05457552 | 37.50615868 | 268.4858 | 55461.0002083333 | 55461.4494675926 | 405058030 | 19924 | 20000 | 19924 | 19924 | 0 | 20243.8 | 2 | 2 | 0 | 1 | 1 | 0 | 0 | 17507.3 | 17507.3 | 38811.9 | 0 | PROCESSED | 57553.4994560185 | 55836 | 55470.1508796296 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 052001 | We propose to observe Her X-1 during Suzaku s AO-5 for a total observing time of 80 ksec, covering one Main-On with four observations of 20 ks each: the first two during the flux maximum and the remaining two during the decay of the Main-On. Our prime objective is to systematically study the centroid energy of the fundamental cyclotron line Ecyc as a function of time, X-ray flux, 35 day phase and 1.24 s phase. These observations will contribute to answering the following questions: Is there a slow secular decrease in the value of Ecyc with time? Does Ecyc depend on 35 day phase? How stable is the positive correlation of the value of Ecyc with the X-ray luminosity? | GALACTIC POINT SOURCES | 4 | B | STAUBERT | R DIGER | NULL | NULL | EUR | 5 | AO5 | VARIABILITY OF THE CYCLOTRON LINE ENERGY E_CYC IN HERCULES X-1 | HXD | N |
| HER X-1 | 254.4619 | 35.2659 | 58.05460857 | 37.50723847 | 268.3041 | 55461.7937037037 | 55462.2467476852 | 405058040 | 21740 | 20000 | 21740 | 21796 | 0 | 21870.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 19803 | 19803 | 39135.9 | 0 | PROCESSED | 57553.5121180556 | 55840 | 55474.0995486111 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 052001 | We propose to observe Her X-1 during Suzaku s AO-5 for a total observing time of 80 ksec, covering one Main-On with four observations of 20 ks each: the first two during the flux maximum and the remaining two during the decay of the Main-On. Our prime objective is to systematically study the centroid energy of the fundamental cyclotron line Ecyc as a function of time, X-ray flux, 35 day phase and 1.24 s phase. These observations will contribute to answering the following questions: Is there a slow secular decrease in the value of Ecyc with time? Does Ecyc depend on 35 day phase? How stable is the positive correlation of the value of Ecyc with the X-ray luminosity? | GALACTIC POINT SOURCES | 4 | B | STAUBERT | R DIGER | NULL | NULL | EUR | 5 | AO5 | VARIABILITY OF THE CYCLOTRON LINE ENERGY E_CYC IN HERCULES X-1 | HXD | N |
| MU COL | 86.4962 | -32.3107 | 237.28985275 | -27.10600903 | 93.5874 | 55455.752337963 | 55456.3113541667 | 405059010 | 25961 | 20000 | 25961 | 25961 | 0 | 25961 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 21873.4 | 21873.4 | 48287.9 | 0 | PROCESSED | 57553.4381018518 | 55836 | 55469.2452314815 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 052005 | We propose to obtain XIS spectra of two O stars with weak winds. They belong to a class of O stars which show significantly weaker mass loss than predicted by the theory of radiation-driven winds. In this respect they resemble the first generation of stars in the early universe, which presumably had only weak winds due to their low metallicity. As explanation for the weak-wind phenomenon it has been suggested that X-rays affect the ionization balance and thus lead to a reduction of the wind-driving force. To check this hypothesis the proposed Suzaku observations are needed. The new data will allow us to discriminate between possible mechanisms for the generation of X-rays, such as magnetic wind confinement or dynamical friction, and serve as input parameters in numerical models. | GALACTIC POINT SOURCES | 4 | A | OSKINOVA | LIDIA | NULL | NULL | EUR | 5 | AO5 | STRONG EXPLORATION OF WEAK STELLAR WINDS WITH SUZAKU | XIS | Y |
| 10 LAC | 339.8111 | 39.0619 | 96.65409432 | -16.97165842 | 81.7456 | 55344.5001967593 | 55345.0690162037 | 405060010 | 25028.4 | 25000 | 25028.4 | 25028.4 | 0 | 25028.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21743.1 | 21743.1 | 49135.9 | 2 | PROCESSED | 57551.6393287037 | 55731 | 55365.1824305556 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 052005 | We propose to obtain XIS spectra of two O stars with weak winds. They belong to a class of O stars which show significantly weaker mass loss than predicted by the theory of radiation-driven winds. In this respect they resemble the first generation of stars in the early universe, which presumably had only weak winds due to their low metallicity. As explanation for the weak-wind phenomenon it has been suggested that X-rays affect the ionization balance and thus lead to a reduction of the wind-driving force. To check this hypothesis the proposed Suzaku observations are needed. The new data will allow us to discriminate between possible mechanisms for the generation of X-rays, such as magnetic wind confinement or dynamical friction, and serve as input parameters in numerical models. | GALACTIC POINT SOURCES | 4 | A | OSKINOVA | LIDIA | NULL | NULL | EUR | 5 | AO5 | STRONG EXPLORATION OF WEAK STELLAR WINDS WITH SUZAKU | XIS | Y |
| GX 339-4 | 255.7015 | -48.7852 | 338.94105133 | -4.32146688 | 83.6944 | 55603.7634722222 | 55604.2349421296 | 405063010 | 22459.4 | 100000 | 22459.4 | 22459.4 | 0 | 22483.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19328.7 | 19328.7 | 40727.9 | 0 | PROCESSED | 57600.9244675926 | 55983 | 55617.4120601852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 052015 | We propose to perform a series of 5 short (20 ks) Suzaku observations of a microquasar during its outburst decline phase with the purpose of following for the first time its broad band X-ray spectral evolution during a soft-to-hard state transition. Such observations will allow 1) to correctly disentangle the different spectral components (accretion disc vs corona) generally present in X-rays; this will permit 2) to precisely investigate the changes in the corona and the disc component through the transition, insuring an accurate study of the variation (if any) of the inner accretion disc radius as such variation was largely debated recently. We will perform simultaneous radio observations to catch the reappearance of the jet. This is a resubmission of an accepted proposal for AO4 | GALACTIC POINT SOURCES | 4 | A | CABANAC | CLEMENT | NULL | NULL | EUR | 5 | AO5-TOO | PROBING THE BROAD BAND X-RAY SPECTRAL EVOLUTION OF MICROQUASARS DURING SOFT-TO-HARD STATE TRANSITIONS | XIS | Y |
| GX 339-4 | 255.7013 | -48.7848 | 338.94128957 | -4.32111913 | 86.3597 | 55608.9686111111 | 55609.6501967593 | 405063020 | 21015.7 | 20000 | 21015.7 | 21015.7 | 0 | 21015.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17595.8 | 17595.8 | 58883.9 | 0 | PROCESSED | 57600.9613773148 | 55988 | 55621.1561342593 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 052015 | We propose to perform a series of 5 short (20 ks) Suzaku observations of a microquasar during its outburst decline phase with the purpose of following for the first time its broad band X-ray spectral evolution during a soft-to-hard state transition. Such observations will allow 1) to correctly disentangle the different spectral components (accretion disc vs corona) generally present in X-rays; this will permit 2) to precisely investigate the changes in the corona and the disc component through the transition, insuring an accurate study of the variation (if any) of the inner accretion disc radius as such variation was largely debated recently. We will perform simultaneous radio observations to catch the reappearance of the jet. This is a resubmission of an accepted proposal for AO4 | GALACTIC POINT SOURCES | 4 | A | CABANAC | CLEMENT | NULL | NULL | EUR | 5 | AO5-TOO | PROBING THE BROAD BAND X-RAY SPECTRAL EVOLUTION OF MICROQUASARS DURING SOFT-TO-HARD STATE TRANSITIONS | XIS | Y |
| GX 339-4 | 255.7016 | -48.7831 | 338.94276391 | -4.32024293 | 90.1024 | 55616.8233680556 | 55617.4487268518 | 405063030 | 19182 | 20000 | 19190 | 19198 | 0 | 19182 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15684 | 15684 | 54025.9 | 1 | PROCESSED | 57601.0471180556 | 55996 | 55628.1679976852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 052015 | We propose to perform a series of 5 short (20 ks) Suzaku observations of a microquasar during its outburst decline phase with the purpose of following for the first time its broad band X-ray spectral evolution during a soft-to-hard state transition. Such observations will allow 1) to correctly disentangle the different spectral components (accretion disc vs corona) generally present in X-rays; this will permit 2) to precisely investigate the changes in the corona and the disc component through the transition, insuring an accurate study of the variation (if any) of the inner accretion disc radius as such variation was largely debated recently. We will perform simultaneous radio observations to catch the reappearance of the jet. This is a resubmission of an accepted proposal for AO4 | GALACTIC POINT SOURCES | 4 | A | CABANAC | CLEMENT | NULL | NULL | EUR | 5 | AO5-TOO | PROBING THE BROAD BAND X-RAY SPECTRAL EVOLUTION OF MICROQUASARS DURING SOFT-TO-HARD STATE TRANSITIONS | XIS | Y |
| GX 339-4 | 255.7013 | -48.7851 | 338.94105066 | -4.32130146 | 91.6296 | 55620.1778703704 | 55620.8022569445 | 405063040 | 21799 | 20000 | 21799 | 21807 | 0 | 21816.8 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 18850.2 | 18850.2 | 53923.9 | 0 | PROCESSED | 57601.0624074074 | 56009 | 55642.1310300926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 052015 | We propose to perform a series of 5 short (20 ks) Suzaku observations of a microquasar during its outburst decline phase with the purpose of following for the first time its broad band X-ray spectral evolution during a soft-to-hard state transition. Such observations will allow 1) to correctly disentangle the different spectral components (accretion disc vs corona) generally present in X-rays; this will permit 2) to precisely investigate the changes in the corona and the disc component through the transition, insuring an accurate study of the variation (if any) of the inner accretion disc radius as such variation was largely debated recently. We will perform simultaneous radio observations to catch the reappearance of the jet. This is a resubmission of an accepted proposal for AO4 | GALACTIC POINT SOURCES | 4 | A | CABANAC | CLEMENT | NULL | NULL | EUR | 5 | AO5-TOO | PROBING THE BROAD BAND X-RAY SPECTRAL EVOLUTION OF MICROQUASARS DURING SOFT-TO-HARD STATE TRANSITIONS | XIS | Y |
| GX 339-4 | 255.7041 | -48.783 | 338.94384752 | -4.32149031 | 92.8952 | 55627.5468518518 | 55628.0320138889 | 405063050 | 16992.5 | 20000 | 16992.5 | 20269.3 | 0 | 20269.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15985.1 | 15985.1 | 41874.1 | 2 | PROCESSED | 57601.1142476852 | 56015 | 55645.2088078704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 052015 | We propose to perform a series of 5 short (20 ks) Suzaku observations of a microquasar during its outburst decline phase with the purpose of following for the first time its broad band X-ray spectral evolution during a soft-to-hard state transition. Such observations will allow 1) to correctly disentangle the different spectral components (accretion disc vs corona) generally present in X-rays; this will permit 2) to precisely investigate the changes in the corona and the disc component through the transition, insuring an accurate study of the variation (if any) of the inner accretion disc radius as such variation was largely debated recently. We will perform simultaneous radio observations to catch the reappearance of the jet. This is a resubmission of an accepted proposal for AO4 | GALACTIC POINT SOURCES | 4 | A | CABANAC | CLEMENT | NULL | NULL | EUR | 5 | AO5-TOO | PROBING THE BROAD BAND X-RAY SPECTRAL EVOLUTION OF MICROQUASARS DURING SOFT-TO-HARD STATE TRANSITIONS | XIS | Y |
| 4U 1909+07 | 287.7097 | 7.5883 | 41.89273161 | -0.82371888 | 247.9131 | 55502.7037847222 | 55503.4337731482 | 405073010 | 29298.2 | 25000 | 29298.2 | 29298.2 | 0 | 29298.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21391.1 | 21391.1 | 63051.9 | 0 | PROCESSED | 57553.9348958333 | 55882 | 55515.2869328704 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 052024 | We propose the first observation of the neutron star HMXB 4U 1909+07 with Suzaku. The aim of the proposed 25 ksec observation is to study the broadband spectrum of the source. The data will provide information about the structure and ionization state of the accreted medium, as well as of the geometry of the accretion column and the strength of the magnetic field. No high-resolution CCD spectra of this source have been published so far. The source shows flaring behavior, so the wind is expected to be strongly clumped, which could be probed by studying the evolution of N_H and the iron line with high time resolution. Furthermore we will perform phase resolved spectroscopy to study the spectral variation with pulse phase and perform a detailed search for a CRSF. | GALACTIC POINT SOURCES | 4 | A | FUERST | FELIX | NULL | NULL | EUR | 5 | AO5 | STUDYING ACCRETION IN THE UNCELEBRATED HMXB 4U 1909+07 | XIS | Y |
| SGR 0501+4516 | 75.2625 | 45.3425 | 161.48747118 | 1.98100999 | 82.3996 | 55459.7272569444 | 55460.9897337963 | 405075010 | 59720.5 | 50000 | 59808.5 | 59812.3 | 0 | 59720.5 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 52935.7 | 52935.7 | 109065.8 | 0 | PROCESSED | 57553.4903935185 | 55287 | 55470.1458449074 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056002 | We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics". | GALACTIC POINT SOURCES | 4 | A | MAKISHIMA | KAZUO | NULL | NULL | JAP | 5 | AO5 | A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM | HXD | Y |
| 1RXS J1708-4009 | 257.2038 | -40.2142 | 346.43162325 | -0.00870489 | 267.1357 | 55466.6124074074 | 55467.7738425926 | 405076010 | 62810.9 | 60000 | 62818.9 | 62822.6 | 0 | 62810.9 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 59511.4 | 59511.4 | 100323.9 | 1 | PROCESSED | 57553.5661342593 | 55287 | 55477.2762268518 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056002 | We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics". | GALACTIC POINT SOURCES | 4 | A | MAKISHIMA | KAZUO | NULL | NULL | JAP | 5 | AO5 | A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM | HXD | Y |
| GX 1+4 | 263.0071 | -24.816 | 1.87675865 | 4.75818757 | 273.1727 | 55471.2801273148 | 55473.5140509259 | 405077010 | 99670 | 100000 | 99670.4 | 99670 | 0 | 99670.4 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 96525.9 | 96525.9 | 192609.1 | 0 | PROCESSED | 57553.6626967593 | 55287 | 55487.4199537037 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056002 | We propose a comprehensive study of magnetars and associated objects in order to resolve strong magnetism of neutron stars. Magnetars are estimated to have an ultra strong magnetic filed as 1E+15 Gauss, and have been attracted growing wide attention recent years. These classes are extreme case of magnetars and have excellent clues to complete our scientific goal, including magnetism and ultrahigh magnetic-field physics. This proposal carries a sense of future potential to become "Suzaku Legacy" Key Project and to break the new ground of "Magnetar Physics". | GALACTIC POINT SOURCES | 4 | A | MAKISHIMA | KAZUO | NULL | NULL | JAP | 5 | AO5 | A SUZAKU STUDY OF MAGNETARS AND THE NEUTRON-STAR MAGNETISM | HXD | Y |
| 1FGL J2339.7-0531 | 354.9077 | -5.5469 | 81.34836456 | -62.4702773 | 67.4026 | 55741.5915625 | 55743.8092361111 | 406007010 | 104091.4 | 100000 | 104091.4 | 104091.4 | 0 | 104099.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 92902.2 | 92902.2 | 191583.7 | 2 | PROCESSED | 57602.4861805556 | 56144 | 55775.4025925926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060007 | We propose to observe an unidentified Fermi source (1FGL J2339.7-0531) in the first-year Fermi catalog to search for the first ``radio-quiet'' Gamma-ray emitting millisecond pulsar. The Fermi source has a candidate X-ray counterpart from Chandra data and its X-ray and Gamma-ray properties are consistent with known Gamma-ray pulsars. This system is likely in a low-mass X-ray binary system based on optical observations. Both X-ray and optical observations show clear variability. We propose to observe the Chandra source with Suzaku to search for the possible orbital period and to study its X-ray spectrum in detail. The results will provide a better insight into the high-energy emission processes in the magnetosphere of millisecond pulsars. | GALACTIC POINT SOURCES | 4 | A | KONG | ALBERT | KATAOKA | JUN | JAP | 6 | AO6 | REVEALING THE NATURE OF AN UNIDENTIFIED FERMI SOURCE | XIS | Y |
| 4U1812-12 | 273.8053 | -12.0935 | 18.04900466 | 2.37362039 | 267.159 | 55838.1400347222 | 55839.9168981482 | 406008010 | 62014.3 | 60000 | 62014.3 | 62014.3 | 0 | 62014.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 53544.1 | 53544.1 | 153509.9 | 1 | PROCESSED | 57603.3255902778 | 56226 | 55858.3124768518 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060012 | Low-Mass X-ray binaries (LMXBs) are known to have soft and hard states, like black hole binaries. Through an analysis of archival Suzaku data of the LMXB Aql X-1 in the hard state, we obtained a clear picture of its accretion geometry; a truncated accretion disk, and a hot corona that Comptonize blackbody photons from the neutron star surface. In order to investigate whether this picture also applies to other LMXBs in the low/hard state, and to better constrain the accretion geometry in comparison with those of black hole binaries, we propose a 60 ksec Suzaku observation of the LMXB 4U 1812-12. This is a valuable object,which is known to reside almost always in the low/hard state. | GALACTIC POINT SOURCES | 4 | A | SAKURAI | SOKI | NULL | NULL | JAP | 6 | AO6 | REVEALING THE ACCRETION GEOMETRY OF THE LOW/HARD STATE LMXB 4U 1812-12 WITH SUZAKU | XIS | Y |
| VW HYI | 62.2833 | -71.2901 | 284.88594452 | -38.13999051 | 181.9815 | 55894.1004513889 | 55895.1821759259 | 406009010 | 70083.4 | 60000 | 70091.4 | 70083.4 | 0 | 70091.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 64970.1 | 64970.1 | 93446.8 | 1 | PROCESSED | 57604.0242939815 | 56274 | 55907.1562615741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060023 | SU UMa type dwarf novae, which are a subclass of cataclysmic variables, sometimes exhibit outburst and superoutburst. It is supposed that the superoutburst is caused by a tidal instability when a disk reachs 3:1 resonance radius. This is related with a mass accretion rate onto white dwarf. Recently, Suzaku observed dwarf nova SS Cyg in its quiescence and outburst, and reveals a plasma structure of a boundary layer in these states, while a plasma structure in superoutburst has been unknown yet. We propose ToO observations of SU UMa star VW Hyi in one superoutburst and three quiescence states proceeded by normal outburst to investigate plasma geometry in superoutburst and a temporal growth of mass accretion rate. | GALACTIC POINT SOURCES | 4 | B | SAITOU | KEI | NULL | NULL | JAP | 6 | AO6-TOO | TOO OBSERVATIONS OF SU UMA TYPE DWARF NOVA VW HYI IN SUPEROUTBURST AND QUIESCENCE | XIS | Y |
| VW HYI | 62.3036 | -71.2936 | 284.88553906 | -38.13260514 | 212.7427 | 55924.6383796296 | 55925.1806828704 | 406009020 | 16159.3 | 20000 | 16159.3 | 16159.3 | 0 | 16159.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13758.7 | 13758.7 | 46851.9 | 0 | PROCESSED | 57604.2667939815 | 56313 | 55945.9133912037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060023 | SU UMa type dwarf novae, which are a subclass of cataclysmic variables, sometimes exhibit outburst and superoutburst. It is supposed that the superoutburst is caused by a tidal instability when a disk reachs 3:1 resonance radius. This is related with a mass accretion rate onto white dwarf. Recently, Suzaku observed dwarf nova SS Cyg in its quiescence and outburst, and reveals a plasma structure of a boundary layer in these states, while a plasma structure in superoutburst has been unknown yet. We propose ToO observations of SU UMa star VW Hyi in one superoutburst and three quiescence states proceeded by normal outburst to investigate plasma geometry in superoutburst and a temporal growth of mass accretion rate. | GALACTIC POINT SOURCES | 4 | B | SAITOU | KEI | NULL | NULL | JAP | 6 | AO6-TOO | TOO OBSERVATIONS OF SU UMA TYPE DWARF NOVA VW HYI IN SUPEROUTBURST AND QUIESCENCE | XIS | Y |
| VW HYI | 62.3086 | -71.2914 | 284.88209314 | -38.1323503 | 276.4367 | 55986.5687962963 | 55987.2501273148 | 406009030 | 20109.7 | 20000 | 20109.7 | 20109.7 | 0 | 20109.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20571.2 | 20571.2 | 58857.9 | 1 | PROCESSED | 57604.7590972222 | 56385 | 56018.9417824074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060023 | SU UMa type dwarf novae, which are a subclass of cataclysmic variables, sometimes exhibit outburst and superoutburst. It is supposed that the superoutburst is caused by a tidal instability when a disk reachs 3:1 resonance radius. This is related with a mass accretion rate onto white dwarf. Recently, Suzaku observed dwarf nova SS Cyg in its quiescence and outburst, and reveals a plasma structure of a boundary layer in these states, while a plasma structure in superoutburst has been unknown yet. We propose ToO observations of SU UMa star VW Hyi in one superoutburst and three quiescence states proceeded by normal outburst to investigate plasma geometry in superoutburst and a temporal growth of mass accretion rate. | GALACTIC POINT SOURCES | 4 | B | SAITOU | KEI | NULL | NULL | JAP | 6 | AO6-TOO | TOO OBSERVATIONS OF SU UMA TYPE DWARF NOVA VW HYI IN SUPEROUTBURST AND QUIESCENCE | XIS | Y |
| VW HYI | 62.3084 | -71.2978 | 284.88912946 | -38.12913625 | 338.7313 | 56049.8124305556 | 56050.1668171296 | 406009040 | 16817.7 | 20000 | 16825.7 | 16825.7 | 0 | 16817.7 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 13947.8 | 13947.8 | 30615.9 | 0 | PROCESSED | 57605.3312847222 | 56449 | 56083.0857060185 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060023 | SU UMa type dwarf novae, which are a subclass of cataclysmic variables, sometimes exhibit outburst and superoutburst. It is supposed that the superoutburst is caused by a tidal instability when a disk reachs 3:1 resonance radius. This is related with a mass accretion rate onto white dwarf. Recently, Suzaku observed dwarf nova SS Cyg in its quiescence and outburst, and reveals a plasma structure of a boundary layer in these states, while a plasma structure in superoutburst has been unknown yet. We propose ToO observations of SU UMa star VW Hyi in one superoutburst and three quiescence states proceeded by normal outburst to investigate plasma geometry in superoutburst and a temporal growth of mass accretion rate. | GALACTIC POINT SOURCES | 4 | B | SAITOU | KEI | NULL | NULL | JAP | 6 | AO6-TOO | TOO OBSERVATIONS OF SU UMA TYPE DWARF NOVA VW HYI IN SUPEROUTBURST AND QUIESCENCE | XIS | Y |
| AQL X-1 | 287.8271 | 0.5745 | 35.71381986 | -4.15705073 | 244.5264 | 55852.1545486111 | 55853.110625 | 406010010 | 9494.8 | 40000 | 9596.8 | 9494.8 | 0 | 9596.8 | 2 | 1 | 0 | 1 | 1 | 0 | 0 | 35325 | 35325 | 82587.8 | 1 | PROCESSED | 57603.4610763889 | 56240 | 55873.1222337963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060036 | We propose to observe the neutron star binary Aql X-1 during the initial outburst phase with Suzaku ToO. The initial outburst phase is very important for studying the spectral state transition and jet ejections in the accretion physics. However, a detailed study of this phase has not been done much yet due to the insufficient sky coverage and sensitivity of the all-sky monitors. The current MAXI/GSC, Swift/BAT and RXTE/ASM+PCA survey has a very good sensitivity and sky coverage, which can promptly trigger the pointed X-ray observations. Suzaku high-sensitive broadband observations and possible radio coordinated observations will reveals us to establish the unified picture in accretion disks and jets in X-ray binaries, which are independent of the central object. | GALACTIC POINT SOURCES | 4 | A | YAMAOKA | KAZUTAKA | NULL | NULL | JAP | 6 | AO6-TOO | SUZAKU TOO OBSERVATIONS OF THE NEUTRON STAR BINARY AQL X-1 DURING THE INITIAL OUTBURST PHASE | XIS | Y |
| AQL X-1 | 287.8264 | 0.5741 | 35.71314195 | -4.15661165 | 244.5268 | 55855.5357986111 | 55856.4599884259 | 406010020 | 9940.6 | 40000 | 10041 | 9940.6 | 0 | 10041 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 37845.1 | 37845.1 | 79846 | 1 | PROCESSED | 57603.5073958333 | 56241 | 55873.3025578704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060036 | We propose to observe the neutron star binary Aql X-1 during the initial outburst phase with Suzaku ToO. The initial outburst phase is very important for studying the spectral state transition and jet ejections in the accretion physics. However, a detailed study of this phase has not been done much yet due to the insufficient sky coverage and sensitivity of the all-sky monitors. The current MAXI/GSC, Swift/BAT and RXTE/ASM+PCA survey has a very good sensitivity and sky coverage, which can promptly trigger the pointed X-ray observations. Suzaku high-sensitive broadband observations and possible radio coordinated observations will reveals us to establish the unified picture in accretion disks and jets in X-ray binaries, which are independent of the central object. | GALACTIC POINT SOURCES | 4 | A | YAMAOKA | KAZUTAKA | NULL | NULL | JAP | 6 | AO6-TOO | SUZAKU TOO OBSERVATIONS OF THE NEUTRON STAR BINARY AQL X-1 DURING THE INITIAL OUTBURST PHASE | XIS | Y |
| AQL X-1 | 287.8278 | 0.5718 | 35.71173466 | -4.15890942 | 243.2618 | 55858.7269328704 | 55859.5786921296 | 406010030 | 8495 | 40000 | 8495 | 9538.3 | 0 | 9556.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 36476.8 | 36476.8 | 73581.9 | 2 | PROCESSED | 57603.6460416667 | 56241 | 55874.1380555556 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060036 | We propose to observe the neutron star binary Aql X-1 during the initial outburst phase with Suzaku ToO. The initial outburst phase is very important for studying the spectral state transition and jet ejections in the accretion physics. However, a detailed study of this phase has not been done much yet due to the insufficient sky coverage and sensitivity of the all-sky monitors. The current MAXI/GSC, Swift/BAT and RXTE/ASM+PCA survey has a very good sensitivity and sky coverage, which can promptly trigger the pointed X-ray observations. Suzaku high-sensitive broadband observations and possible radio coordinated observations will reveals us to establish the unified picture in accretion disks and jets in X-ray binaries, which are independent of the central object. | GALACTIC POINT SOURCES | 4 | A | YAMAOKA | KAZUTAKA | NULL | NULL | JAP | 6 | AO6-TOO | SUZAKU TOO OBSERVATIONS OF THE NEUTRON STAR BINARY AQL X-1 DURING THE INITIAL OUTBURST PHASE | XIS | Y |
| OAO1657-415 | 255.2026 | -41.6667 | 344.36019061 | 0.31327103 | 285.9012 | 55830.3988425926 | 55832.6667939815 | 406011010 | 84729.9 | 80000 | 84733.7 | 84729.9 | 0 | 84741.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 74588.5 | 74588.5 | 195929.7 | 2 | PROCESSED | 57603.3220023148 | 56226 | 55858.2768518518 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060037 | We propose Suzaku observation of accretion-powered pulsar OAO 1657-415 to study matter accretion onto the neutron star. This object is a unique high mass X-ray binary (HMXB) that shows intermediate characteristics between wind-fed accretion pulsars and disk-fed accretion pulsars. High S/N spectra obtained by XIS, HXD-PIN/GSO with short exposure time (1 ks) allow us to investigate short-time variability of physical states of the accretion column, which is close to the neutron star surface. The proposed observation also reveals the matter distribution in the HMXB by using a 6.4-keV iron fluorescence line and hard X-rays. The data at the phase of eclipse egress provide essential information about the stellar wind and atmosphere of the companion star to constrain its stellar type in question. | GALACTIC POINT SOURCES | 4 | B | ODAKA | HIROKAZU | NULL | NULL | JAP | 6 | AO6 | WIDE-BAND X-RAY OBSERVATION OF HIGH MASS X-RAY BINARY PULSAR OAO 1657-415 | XIS | Y |
| PSR J0726-2612 | 111.531 | -26.2114 | 240.07877209 | -4.64696128 | 117.9984 | 55881.5691782407 | 55882.6252546296 | 406012010 | 43757 | 100000 | 43757 | 43792 | 0 | 43792 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39728.8 | 39728.8 | 91227.8 | 0 | PROCESSED | 57603.8172685185 | 56264 | 55895.2388078704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060041 | To study the origin of magnetars, a unique opportunity is provided by detecting an excess of thermal radiation in the radio pulsars which has dipolar magnetic fields as high as magnetars. The excess is caused by field decay as seen in magnetars. A question is raised whether the rotation powered pulsars can have active magnetic flux similar to magnetars. PSR J0726-2612 is a nearby (3kpc) radio pulsar with magnetic field as high as 10^13.5 G, and therefore is an ideal target. We propose 100ksec observation of this pulsar to discover magnetar-like thermal radiation, and determine the structure of the active magnetic flux tubes by phase alignment of rotational modulation of the X-ray radiation with radio pulses. | GALACTIC POINT SOURCES | 4 | C | SHIBATA | SHINPEI | NULL | NULL | JAP | 6 | AO6 | CAN HIGH MAGNETIC FIELD RADIO PULSARS BE THE MAGNETAR ? | XIS | Y |
| CYG X-1 | 299.5916 | 35.1745 | 71.31236822 | 3.05181611 | 279.5001 | 55839.9245023148 | 55840.9169328704 | 406013010 | 3702.7 | 40000 | 3832 | 3702.7 | 0 | 40271.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 32962.5 | 32962.5 | 85733.9 | 1 | PROCESSED | 57603.3954166667 | 56582 | 56212.7247916667 | 3.0.22.44 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060057 | We achieved 0.1 s time resolution with enough statistics on accumulating profiles of source brightening and made clear that electron temperature decreases and optical depth increases at the peak of brightness by using the XIS data of Psum mode. Progress to understanding the nature of fast time variability, which has been a mystery for 40 years since its discovery, connected with spectral properties is being made now. However, this property is not confirmed yet in other observations having different time scales of variability and spectral shapes, lacking the XIS data in Psum mode. We propose here another observation of Cyg X-1 with XIS0 1/8 window no burst, XIS1 1/4 window 0.5 s burst,and XIS3 Psum mode for a exposure of 40 ks. | GALACTIC POINT SOURCES | 4 | A | YAMADA | SHIN'YA | NULL | NULL | JAP | 6 | AO6 | REVEALING THE NATURE OF FAST TIME VARIABILITY OF CYG X-1 WITH SHOT ANALYSIS | XIS | Y |
| RXJ2056.6+4940 | 314.1926 | 49.6559 | 89.31769097 | 2.74712249 | 241.0011 | 55887.7886805556 | 55888.5355208333 | 406014010 | 42373.1 | 40000 | 42381.1 | 42373.1 | 0 | 42373.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44666.5 | 44666.5 | 64524 | 1 | PROCESSED | 57603.9503356482 | 56264 | 55897.0994791667 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060065 | There are a total 1451 gamma-ray emitting objects in the Fermi 11-month survey catalogue. About 60% of sources were identified with counterparts in other wavelengths, most of which are extragalactic sources. Among them, XSS J12270-4859 stands out as a very peculiar Galactic source with unusual timing and spectral behaviours in the X-ray band. We aim to search for similar sources among the Fermi sources. | GALACTIC POINT SOURCES | 4 | C | ISO | NAOKI | NULL | NULL | JAP | 6 | AO6 | SEARCH FOR GAMMA-RAY BINARIES WITH A LOW-MASS COUNTERPART | XIS | Y |
| 4U0114+65 | 19.4873 | 65.3067 | 125.69846298 | 2.57745686 | 71.642 | 55763.4307291667 | 55764.9453472222 | 406017010 | 106492.5 | 100000 | 106550.8 | 106558.8 | 0 | 106492.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 88506.1 | 88506.1 | 130821.9 | 1 | PROCESSED | 57602.6518402778 | 56152 | 55785.0443981482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060071 | We propose to observe an X-ray pulsar, 4U 0114+65 for 100 ks. This object is known to be a neutron star binary with an orbital period of 12 days and a long pulse priod of 10 ks. Our goals are to obtain time-averaged spectra of the XIS and HXD, and to quantify spectral changes between flare and quiescense phases, and to search for a cyclotron absorption line around ~ 60 keV. We also study pulse-phase resolved spectra. With these pieces of information, we aim at clarifying whether this source is a magnetar descendent or a neutron star with ordinary magnetic fields. | GALACTIC POINT SOURCES | 4 | A | SASANO | MAKOTO | NULL | NULL | JAP | 6 | AO6 | SEARCH FOR HIGH MAGNETIC NEUTRON STARS IN HIGH-MASS X-RAY BINARIES | XIS | Y |
| 1RXSJ175911.0-344921 | 269.7922 | -34.8194 | 356.38251758 | -5.46102238 | 72.1205 | 55993.9029513889 | 55994.912650463 | 406019010 | 40181.3 | 40000 | 40181.3 | 40181.3 | 0 | 40181.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34751 | 34751 | 87233.9 | 1 | PROCESSED | 57604.8358564815 | 56385 | 56016.6680787037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060085 | We propose to study wide-band X-ray properties of 5 unidentified sources with luminosities of ~10^35 erg/s, detected in the ROSAT All Sky Survey. These sources are a part of the complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge constructed by Mori (2005). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with optical identifications. This is a new step toward understanding the formation history of the bulge. Furthermore, because the luminosity range we observe corresponds to a "missing link" region ever studied for a neutron star or black-hole X-ray binary, our results are also unique to test accretion disk theories at intermediate mass accretion rates. | GALACTIC POINT SOURCES | 4 | C | MORI | HIDEYUKI | NULL | NULL | JAP | 6 | AO6 | SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE | XIS | Y |
| 24M2791 | 334.9577 | 63.2629 | 106.81877019 | 5.23758822 | 230.0008 | 55947.3704513889 | 55948.0926388889 | 406023010 | 34601.7 | 30000 | 34617.7 | 34601.7 | 0 | 34609.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35059.5 | 35059.5 | 62391.9 | 0 | PROCESSED | 57604.5087847222 | 56340 | 55973.1102893518 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060087 | We propose to observe 5 Fermi unidentified gamma-ray sources which are selected by possible association with extremely bright infrared source. The infrared-selected Fermi unIDs in low-latitude plane are potentially very interesting because they could be a new class of gamma-ray emitter such as starburst galaxy, Seyfert, or X-ray binary. To investigate X-ray counterpart and identify what they are, we propose 30 ks observation for each object. | GALACTIC POINT SOURCES | 4 | C | OHNO | MASANORI | NULL | NULL | JAP | 6 | AO6 | SEARCH FOR NEW CLASS OF GAMMA-RAY EMITTER BY X-RAY IDENTIFICATION OF BRIGHT INFRARED-SELECTED FERMI UNID SOURCES | XIS | Y |
| 1FGL J1715.2-3319 | 258.713 | -33.4282 | 352.62684601 | 3.01774525 | 99.0737 | 56002.5629166667 | 56003.3750810185 | 406024010 | 32165 | 30000 | 32165 | 32165 | 0 | 32165 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27984.8 | 27984.8 | 70166 | 0 | PROCESSED | 57604.9296064815 | 56386 | 56019.2516435185 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060087 | We propose to observe 5 Fermi unidentified gamma-ray sources which are selected by possible association with extremely bright infrared source. The infrared-selected Fermi unIDs in low-latitude plane are potentially very interesting because they could be a new class of gamma-ray emitter such as starburst galaxy, Seyfert, or X-ray binary. To investigate X-ray counterpart and identify what they are, we propose 30 ks observation for each object. | GALACTIC POINT SOURCES | 4 | C | OHNO | MASANORI | NULL | NULL | JAP | 6 | AO6 | SEARCH FOR NEW CLASS OF GAMMA-RAY EMITTER BY X-RAY IDENTIFICATION OF BRIGHT INFRARED-SELECTED FERMI UNID SOURCES | XIS | Y |
| AXP 4U 0142+614 | 26.5682 | 61.7591 | 129.37061357 | -0.42523158 | 40.384 | 55811.6552314815 | 55812.5731134259 | 406031010 | 38649.7 | 60000 | 38649.7 | 38649.7 | 0 | 38682.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42196.4 | 42196.4 | 79292 | 0 | PROCESSED | 57603.1220138889 | 56218 | 55851.4406828704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060092 | We propose a broad-band spectral study of magnetars in active phases in order to derive a unified interpretation of burst and persistent emissions. Magnetars are known for their unusually strong surface magnetic fields, up to 10^15 G. This proposal has two main observational goals. The first objective is to detect hard X-ray emission in magnetar burst spectra as seen in a previous SGR 0501+4516 burst spectrum. The second goal is to detect persistent emission in active phases. It is important to compare spectral characteristics in active phases with those in non-active phases. We will trigger ToO observations when one of the five magnetars exhibit high bursting activity and/or brightening of their persistent emission as observed by very sensitive monitoring observations with MAXI. | GALACTIC POINT SOURCES | 4 | A | NAKAGAWA | YUJIN | NULL | NULL | JAP | 6 | AO6-TOO | A SYSTEMATIC STUDY TO SUPPORT A UNIFIED INTERPRETATION OF MAGNETAR EMISSIONS | XIS | Y |
| RS OPH | 267.5535 | -6.6951 | 19.81011082 | 10.37967032 | 94.9072 | 55987.2608796296 | 55988.855 | 406033010 | 69386 | 100000 | 69386 | 69386 | 0 | 69386 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 60089.9 | 60089.9 | 137719.8 | 0 | PROCESSED | 57604.8300810185 | 56375 | 56008.324224537 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060096 | We propose a 100 ks observation of a recurrent novae remnant RS Ophiuchi. Using Suzaku's wide-energy coverage and excellent spectral performance, we aim to diagnose plasma and to discover non-thermal emission at a recurrent novae remnant. | GALACTIC POINT SOURCES | 4 | C | TAKEI | DAI | NULL | NULL | JAP | 6 | AO6 | OBSERVATION OF A RECURRENT NOVA REMNANT RS OPHIUCHI | XIS | Y |
| 1RXSJ013106.4+612035 | 22.7619 | 61.3591 | 127.66105316 | -1.14841945 | 76.8129 | 55765.7032175926 | 55766.0182060185 | 406034010 | 13296.3 | 20000 | 13296.3 | 13296.3 | 0 | 13296.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15882.9 | 15882.9 | 27199.9 | 0 | PROCESSED | 57602.6424884259 | 56374 | 55784.9886458333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060097 | We propose to observe 3 X-ray unidentified sources by Suzaku. Their positions are consistent with those detected in radio, optical and gamma-ray. | GALACTIC POINT SOURCES | 4 | B | TAKAHASHI | HIROMITSU | NULL | NULL | JAP | 6 | AO6 | SUZAKU OBSERVATIONS OF GAMMA-RAY BINARY CANDIDATES | XIS | Y |
| 1RXSJ013106.4+612035 | 22.8032 | 61.3371 | 127.68400105 | -1.16712133 | 215.0025 | 55993.5664930556 | 55993.889837963 | 406034020 | 12173.7 | 8000 | 12173.7 | 12173.7 | 0 | 12173.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17897 | 17897 | 27921.9 | 0 | PROCESSED | 57604.8011574074 | 56374 | 56008.1191782407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060097 | We propose to observe 3 X-ray unidentified sources by Suzaku. Their positions are consistent with those detected in radio, optical and gamma-ray. | GALACTIC POINT SOURCES | 4 | B | TAKAHASHI | HIROMITSU | NULL | NULL | JAP | 6 | AO6 | SUZAKU OBSERVATIONS OF GAMMA-RAY BINARY CANDIDATES | XIS | Y |
| 1RXSJ194246.3+103339 | 295.6976 | 10.5399 | 48.24168916 | -6.37340779 | 280.0002 | 55848.1433564815 | 55848.635625 | 406035010 | 20488.9 | 20000 | 20488.9 | 20488.9 | 0 | 20488.9 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 17142 | 17142 | 42508 | 0 | PROCESSED | 57603.4189583333 | 56240 | 55873.0004861111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060097 | We propose to observe 3 X-ray unidentified sources by Suzaku. Their positions are consistent with those detected in radio, optical and gamma-ray. | GALACTIC POINT SOURCES | 4 | B | TAKAHASHI | HIROMITSU | NULL | NULL | JAP | 6 | AO6 | SUZAKU OBSERVATIONS OF GAMMA-RAY BINARY CANDIDATES | XIS | Y |
| 1RXSJ135341.1-664002 | 208.4233 | -66.67 | 309.05087215 | -4.54070575 | 288.5314 | 55774.1593055556 | 55774.6939236111 | 406036010 | 23267.9 | 20000 | 23275.9 | 23267.9 | 0 | 23275.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 22424.1 | 22424.1 | 46183.9 | 0 | PROCESSED | 57602.7124189815 | 56166 | 55802.4628472222 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060097 | We propose to observe 3 X-ray unidentified sources by Suzaku. Their positions are consistent with those detected in radio, optical and gamma-ray. | GALACTIC POINT SOURCES | 4 | B | TAKAHASHI | HIROMITSU | NULL | NULL | JAP | 6 | AO6 | SUZAKU OBSERVATIONS OF GAMMA-RAY BINARY CANDIDATES | XIS | Y |
| HD162020 | 267.6611 | -40.3282 | 350.73095661 | -6.73195128 | 265.867 | 55808.0919560185 | 55808.4078703704 | 406037010 | 15922.9 | 15000 | 15922.9 | 15922.9 | 0 | 15922.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15940.6 | 15940.6 | 27287.9 | 2 | PROCESSED | 57603.0570949074 | 56232 | 55865.1159953704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061202 | Star-planet interaction (SPI) in X-rays is predicted by models of interacting magnetospheres of stars and their hot-Jupiter class planets. We propose to explore the realm of X-ray SPI in the case of a system with a high eccentricity hot Jupiter like in HD162020. This is a system formed by a K2V star plus a massive hot-Jupiter class planet with a minimum-maximum separation of 0.026-0.046 AU, respectively (e = 0.28, P = 8.42 days). We request a series of observations, four of 15 ks at the periastron and three of 10 ks at the apoastron in order to compare the flux and the spectrum at the extreme phases and discover SPI effects due to magnetospheric interaction. | GALACTIC POINT SOURCES | 4 | A | PILLITTERI | IGNAZIO | NULL | NULL | USA | 6 | AO6 | STAR-PLANET INTERACTION IN X-RAYS BAND IN HIGH ECCENTRICITY EXO-PLANETS. | XIS | Y |
| HD162020 | 267.6612 | -40.3294 | 350.72995016 | -6.73261971 | 268.3343 | 55816.4132291667 | 55816.727962963 | 406037020 | 15036.2 | 15000 | 15044.2 | 15044.2 | 0 | 15036.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15582.9 | 15582.9 | 27183.9 | 0 | PROCESSED | 57603.1194328704 | 56218 | 55851.4394444444 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061202 | Star-planet interaction (SPI) in X-rays is predicted by models of interacting magnetospheres of stars and their hot-Jupiter class planets. We propose to explore the realm of X-ray SPI in the case of a system with a high eccentricity hot Jupiter like in HD162020. This is a system formed by a K2V star plus a massive hot-Jupiter class planet with a minimum-maximum separation of 0.026-0.046 AU, respectively (e = 0.28, P = 8.42 days). We request a series of observations, four of 15 ks at the periastron and three of 10 ks at the apoastron in order to compare the flux and the spectrum at the extreme phases and discover SPI effects due to magnetospheric interaction. | GALACTIC POINT SOURCES | 4 | A | PILLITTERI | IGNAZIO | NULL | NULL | USA | 6 | AO6 | STAR-PLANET INTERACTION IN X-RAYS BAND IN HIGH ECCENTRICITY EXO-PLANETS. | XIS | Y |
| HD162020 | 267.6618 | -40.3275 | 350.73183598 | -6.73206134 | 259.9987 | 55824.6498958333 | 55825.1632407407 | 406037030 | 16230 | 15000 | 16238 | 16238 | 0 | 16230 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13378.4 | 13378.4 | 44345.9 | 1 | PROCESSED | 57603.1988078704 | 56218 | 55851.4474884259 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061202 | Star-planet interaction (SPI) in X-rays is predicted by models of interacting magnetospheres of stars and their hot-Jupiter class planets. We propose to explore the realm of X-ray SPI in the case of a system with a high eccentricity hot Jupiter like in HD162020. This is a system formed by a K2V star plus a massive hot-Jupiter class planet with a minimum-maximum separation of 0.026-0.046 AU, respectively (e = 0.28, P = 8.42 days). We request a series of observations, four of 15 ks at the periastron and three of 10 ks at the apoastron in order to compare the flux and the spectrum at the extreme phases and discover SPI effects due to magnetospheric interaction. | GALACTIC POINT SOURCES | 4 | A | PILLITTERI | IGNAZIO | NULL | NULL | USA | 6 | AO6 | STAR-PLANET INTERACTION IN X-RAYS BAND IN HIGH ECCENTRICITY EXO-PLANETS. | XIS | Y |
| HD162020 | 267.6661 | -40.3245 | 350.73610578 | -6.73339029 | 259.9986 | 55833.0255208333 | 55833.4279513889 | 406037040 | 16729.7 | 15000 | 16737.7 | 16737.7 | 0 | 16729.7 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15728.6 | 15728.6 | 34749.9 | 0 | PROCESSED | 57603.2728356482 | 56225 | 55858.1397453704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061202 | Star-planet interaction (SPI) in X-rays is predicted by models of interacting magnetospheres of stars and their hot-Jupiter class planets. We propose to explore the realm of X-ray SPI in the case of a system with a high eccentricity hot Jupiter like in HD162020. This is a system formed by a K2V star plus a massive hot-Jupiter class planet with a minimum-maximum separation of 0.026-0.046 AU, respectively (e = 0.28, P = 8.42 days). We request a series of observations, four of 15 ks at the periastron and three of 10 ks at the apoastron in order to compare the flux and the spectrum at the extreme phases and discover SPI effects due to magnetospheric interaction. | GALACTIC POINT SOURCES | 4 | A | PILLITTERI | IGNAZIO | NULL | NULL | USA | 6 | AO6 | STAR-PLANET INTERACTION IN X-RAYS BAND IN HIGH ECCENTRICITY EXO-PLANETS. | XIS | Y |
| HD162020 | 267.6578 | -40.3138 | 350.74222411 | -6.72254511 | 106.352 | 56005.8535069444 | 56006.0626157407 | 406038010 | 10428.6 | 10000 | 10437.3 | 10437.3 | 0 | 10428.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7673 | 7673 | 18055.9 | 0 | PROCESSED | 57604.9610185185 | 56435 | 56068.625474537 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061202 | Star-planet interaction (SPI) in X-rays is predicted by models of interacting magnetospheres of stars and their hot-Jupiter class planets. We propose to explore the realm of X-ray SPI in the case of a system with a high eccentricity hot Jupiter like in HD162020. This is a system formed by a K2V star plus a massive hot-Jupiter class planet with a minimum-maximum separation of 0.026-0.046 AU, respectively (e = 0.28, P = 8.42 days). We request a series of observations, four of 15 ks at the periastron and three of 10 ks at the apoastron in order to compare the flux and the spectrum at the extreme phases and discover SPI effects due to magnetospheric interaction. | GALACTIC POINT SOURCES | 4 | A | PILLITTERI | IGNAZIO | NULL | NULL | USA | 6 | AO6 | STAR-PLANET INTERACTION IN X-RAYS BAND IN HIGH ECCENTRICITY EXO-PLANETS. | XIS | Y |
| HD162020 | 267.6599 | -40.3316 | 350.72753331 | -6.73286722 | 269.5018 | 55820.4672453704 | 55820.6918634259 | 406038020 | 8896 | 10000 | 8896 | 8896 | 0 | 8896 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7851.9 | 7851.9 | 19399.9 | 0 | PROCESSED | 57603.1676851852 | 56218 | 55851.4444097222 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061202 | Star-planet interaction (SPI) in X-rays is predicted by models of interacting magnetospheres of stars and their hot-Jupiter class planets. We propose to explore the realm of X-ray SPI in the case of a system with a high eccentricity hot Jupiter like in HD162020. This is a system formed by a K2V star plus a massive hot-Jupiter class planet with a minimum-maximum separation of 0.026-0.046 AU, respectively (e = 0.28, P = 8.42 days). We request a series of observations, four of 15 ks at the periastron and three of 10 ks at the apoastron in order to compare the flux and the spectrum at the extreme phases and discover SPI effects due to magnetospheric interaction. | GALACTIC POINT SOURCES | 4 | A | PILLITTERI | IGNAZIO | NULL | NULL | USA | 6 | AO6 | STAR-PLANET INTERACTION IN X-RAYS BAND IN HIGH ECCENTRICITY EXO-PLANETS. | XIS | Y |
| HD162020 | 267.6631 | -40.3218 | 350.73730077 | -6.73005667 | 259.9987 | 55829.424212963 | 55829.6543865741 | 406038030 | 11481 | 10000 | 11481 | 11481 | 0 | 11481 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8540.2 | 8540.2 | 19879.9 | 0 | PROCESSED | 57603.2407638889 | 56225 | 55858.0790162037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061202 | Star-planet interaction (SPI) in X-rays is predicted by models of interacting magnetospheres of stars and their hot-Jupiter class planets. We propose to explore the realm of X-ray SPI in the case of a system with a high eccentricity hot Jupiter like in HD162020. This is a system formed by a K2V star plus a massive hot-Jupiter class planet with a minimum-maximum separation of 0.026-0.046 AU, respectively (e = 0.28, P = 8.42 days). We request a series of observations, four of 15 ks at the periastron and three of 10 ks at the apoastron in order to compare the flux and the spectrum at the extreme phases and discover SPI effects due to magnetospheric interaction. | GALACTIC POINT SOURCES | 4 | A | PILLITTERI | IGNAZIO | NULL | NULL | USA | 6 | AO6 | STAR-PLANET INTERACTION IN X-RAYS BAND IN HIGH ECCENTRICITY EXO-PLANETS. | XIS | Y |
| ETA CARINAE | 161.2639 | -59.6881 | 287.59810122 | -0.63296206 | 310.0122 | 55766.0329398148 | 55766.9286226852 | 406039010 | 42030.2 | 50000 | 42030.2 | 42030.2 | 0 | 42030.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 49093.7 | 49093.7 | 77383.9 | 0 | PROCESSED | 57602.6625462963 | 56163 | 55785.0281712963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061205 | Eta Car is the nearest highly unstable extremely massive star and a key object for understanding how mass and angular momentum change as an extremely massive star heads towards hypernova. Periodic minima in X-rays and other wavebands show it as an extremely eccentric binary with a massive companion. A surprising change in the X-ray emission during the January 2009 X-ray minimum probably indicates a large-scale variation in the LBV primary's mass loss rate. We propose a Suzaku observation in AO6 to monitor the change of the absorption column in the line of sight and the non-thermal emission above 10 keV. The observation will help to study geometry of the binary orbit of Eta Car and the mechanism of the non-thermal emission. | GALACTIC POINT SOURCES | 4 | B | HAMAGUCHI | KENJI | NULL | NULL | USA | 6 | AO6 | MONITORING DYNAMICAL MASS LOSS FROM ETA CAR WITH SUZAKU: APASTRON | XIS | Y |
| GAMMA CASSIOPEIAE | 14.1598 | 60.7356 | 123.56796459 | -2.12972511 | 72.5084 | 55755.0038888889 | 55756.333587963 | 406040010 | 55394 | 50000 | 55394 | 55394 | 0 | 55394 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 56216.4 | 56216.4 | 114877.8 | 0 | PROCESSED | 57602.6019791667 | 56183 | 55816.6655208333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061207 | We propose a 50 ks Suzaku observation to obtain for the first time the hard X-ray spectrum of the classical Be star Gamma Cas. This star is a prototype of the "Gamma Cas stars" class, whose nature is not yet understood. Earlier XMM-Newton and Swift BAT observations gave a hint of the presence of the hard X-ray emission above 10 keV. The broadband Suzaku spectrum will allow to establish its X-ray emission mechanism - non-thermal emission or reflection of thermal emission from a neutral surface. On this basis, we will be able to discriminate the mechanisms between the magnetic disk dynamo and the accretion on a compact star. These new data will be pivotal in solving the enigma of Gamma Cas and revealing the true nature of this astrophysically important object. | GALACTIC POINT SOURCES | 4 | C | HAMAGUCHI | KENJI | NULL | NULL | USA | 6 | AO6 | SUZAKU'S HARD LOOK AT GAMMA CASSIOPEIAE | XIS | Y |
| 4 DRA | 187.5655 | 69.216 | 125.72551845 | 47.79722512 | 145.5318 | 55874.1707291667 | 55875.0619328704 | 406041010 | 42258 | 40000 | 42258 | 42258 | 0 | 42258 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39792.5 | 39792.5 | 76998 | 2 | PROCESSED | 57603.7210532407 | 56260 | 55890.6961458333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061212 | 4 Dra is a weakly symbiotic star that exhibited strong variability in ROSAT observations. Our Suzaku Cycle 5 observation confirms it to be an absorbed hard X-ray source, powered by accretion. It is thus a nearby, lower accretion rate analogue of the hard X-ray bright symbiotic stars such as T CrB and CH Cyg. During Suzaku Cycle 6, 4 Dra is near apastron and near the inferior conjunction of the accreting white dwarf: both these should reduce the absorption due to the M giant, while absorption by the accretion flow near the white dwarf should remain roughly comparable. We therefore propose a second Suzaku observation of 4 Dra to constrain the relative contributions of these two X-ray absorbers, and to obtain a high signal-to-noise spectrum of a symbiotic star boundary layer near 1 keV. | GALACTIC POINT SOURCES | 4 | C | MUKAI | KOJI | NULL | NULL | USA | 6 | AO6 | A SUZAKU OBSERVATION OF 4 DRA NEAR INFERIOR CONJUNCTION | XIS | Y |
| V1082 SGR | 286.8363 | -20.7721 | 15.88147607 | -12.67535412 | 81.3818 | 56009.1848148148 | 56010.4459375 | 406042010 | 39460.5 | 40000 | 39460.5 | 39460.5 | 0 | 39460.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36017.1 | 36017.1 | 108924 | 2 | PROCESSED | 57605.0088541667 | 56399 | 56023.1564236111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061217 | V1082 Sgr is a BAT-detected cataclysmic variable with a 20 hr orbital period that exhibits high and low states. The high X-ray luminosity and the presence of the HeII 4686 lines in its optical spectrum have led to the suggestion that this is an intermediate polar (IP). We propose an exploratory 40 ks Suzaku observation with the aim of establishing if it is indeed an IP. If it is, then this system may provide a unique opportunity to study an IP in a low state, which has not been possible with other IPs. | GALACTIC POINT SOURCES | 4 | C | MUKAI | KOJI | NULL | NULL | USA | 6 | AO6 | AN UNUSUAL BAT-DETECTED CATACLYSMIC VARIABLE, V1082 SGR | XIS | Y |
| 4U 1954+31 | 298.9334 | 32.0803 | 68.38077131 | 1.91321277 | 261.2562 | 55857.3373263889 | 55858.7203009259 | 406046010 | 60216 | 60000 | 60224 | 60232 | 0 | 60216 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 57900.8 | 57900.8 | 119467.9 | 0 | PROCESSED | 57603.6159953704 | 56241 | 55874.1069328704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061226 | We propose the first Suzaku observation of a symbiotic X-ray binary 4U 1954+31. This object has an extraordinarily long spin period, ~5 hour, attributed to the neutron star (NS) rotation, making 4U 1954+31 the slowest-rotating accreting NS binary. It raises a question about its binary evolution, since a slowly rotating NS orbiting an M-type giant is quite unique. As to its large variability, the popular clumpy wind model has not yet become a smoking-gun, and we propose an alternative hypothesis that the NS is a magnetar descendent captured by an M-type giant in their closer encounter. Known X-ray properties of 4U~1954+31 will be revisited in a view of gated accretion onto the strongly magnetized NS. A 60 ks Suzaku observation can examine these scenarios. | GALACTIC POINT SOURCES | 4 | B | ENOTO | TERUAKI | NULL | NULL | USA | 6 | AO6 | THE SLOWEST ROTATING PULSAR 4U 1954+31 | XIS | Y |
| 4U 0115+63 | 19.6209 | 63.7559 | 125.91670035 | 1.04099954 | 84.7167 | 55747.0027430556 | 55748.0529976852 | 406048010 | 24279 | 50000 | 24280 | 24279 | 0 | 24283.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45127.2 | 45127.2 | 90727.9 | 1 | PROCESSED | 57602.5201157407 | 56163 | 55778.4298611111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061234 | We propose to perform Target of Opportunity observations of one accreting neutron star that is a known cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 6 | AO6-TOO | CYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELD | XIS | Y |
| 4U 0115+63 | 19.6139 | 63.7554 | 125.91367385 | 1.04017806 | 82.1235 | 55750.053587963 | 55751.0210763889 | 406049010 | 42274.8 | 45000 | 42274.8 | 42354.8 | 0 | 42354.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42143.2 | 42143.2 | 83577.9 | 1 | PROCESSED | 57602.5577662037 | 56163 | 55778.4311226852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061234 | We propose to perform Target of Opportunity observations of one accreting neutron star that is a known cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 6 | AO6-TOO | CYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELD | XIS | Y |
| GX 304-1 | 195.3153 | -61.5986 | 304.10001953 | 1.25086712 | 115.9338 | 55957.437037037 | 55959.1669444444 | 406060010 | 16524.3 | 65000 | 16691.2 | 16524.3 | 0 | 16691.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 58712.4 | 58712.4 | 149432.1 | 3 | PROCESSED | 57604.5523148148 | 56399 | 56033.2695023148 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061235 | We propose to perform Target of Opportunity observations of one accreting neutron star that is not yet a known or clearly confirmed cyclotron line source, out of a sample of five, in outburst. The aim is to observe the source for 65 ks at a level of >~100 mCrab, in order search for cyclotron line(s) and constrain the broad band spectrum. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 6 | AO6-TOO | CYCLOTRON LINES IN TRANSIENT PULSARS II: NEW LINES | XIS | Y |
| SGR 1806-20 | 272.1607 | -20.4008 | 10.00344249 | -0.23433657 | 89.0334 | 56010.449837963 | 56012.5314814815 | 406069010 | 70596.4 | 70000 | 70596.4 | 70596.4 | 0 | 70596.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 63957.1 | 63957.1 | 179827.9 | 2 | PROCESSED | 57605.0500462963 | 56399 | 56023.2387384259 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061301 | Recent Suzaku investigations revealed that a broad-band (0.8-70 keV) spectra of known magnetars systematically change depending on their characteristic ages. The hard X-rays of magnetars become weaker but harder for older objects. In order to accomplish this picture, we have to verify that this correlation is rather free from selection effects, and holds even when the sources vary on long time scales. Here we propose a 70 ks observation of SGR 1806-20. If we detect the hard X-rays from this source at a rather intensity, the above correlation will be much reinforced. | GALACTIC POINT SOURCES | 4 | C | ENOTO | TERUAKI | NULL | NULL | USA | 6 | AO6 | VARIABILITY OF HARD X-RAYS FROM MAGNETARS | XIS | Y |
| GX 17+2 | 274.0108 | -14.0482 | 16.42401351 | 1.2676957 | 264.7715 | 55853.116099537 | 55855.5287037037 | 406070010 | 6506.9 | 100000 | 6757.2 | 6506.9 | 0 | 6757.2 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 87359.9 | 87359.9 | 208429.7 | 3 | PROCESSED | 57603.5270023148 | 56241 | 55873.2944444445 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 062003 | The behaviour of dense matter in neutron stars remains enigmatic. To probe this requires accurate measurements of neutron star radii and masses. We have recently shown that broad relativistic Fe emission lines in neutron star low-mass X-ray binaries can be used to constrain the neutron star radius. These sources also provide another tool, kHz quasi-periodic oscillations (QPOs). Combining a measurement of the velocity of the gas in the inner disk (from the Fe line) and the frequency of the kHz QPOs provides a method to measure the neutron star mass if kHz QPOs originate at the inner disk. We propose 100 ksec observations of GX 349+2 and GX 17+2 to provide a detailed Fe line profile. Simultaneously, we will also observe with RXTE to detect the kHz QPOs, allowing us to test this technique. | GALACTIC POINT SOURCES | 4 | A | CACKETT | EDWARD | NULL | NULL | EUR | 6 | AO6 | EXPLORING THE IRON LINE - KHZ QPO CONNECTION | XIS | Y |
| 4U 1543-624 | 236.9719 | -62.5774 | 321.74901084 | -6.34183385 | 299.1939 | 55826.4056828704 | 55827.6217592593 | 406072010 | 49185.1 | 50000 | 49193.1 | 49185.1 | 0 | 49201.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45309.4 | 45309.4 | 105059.9 | 1 | PROCESSED | 57603.2564699074 | 56222 | 55851.4556134259 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 062010 | We propose to observe the ultra-compact X-ray binaries 4U 0614+091 and 4U 1543-624 for 50 ksec each. The aim of these observations is to constrain the inner radius of the accretion disc for both sources using the recently discovered in both sources relativistialy broadened OVIII Ly alpha line at ~0.7 keV. This constrains the radius of the neutron star. The second goal is to constrain the continuum using more physical model than was used in the literature so far. The unique, large energy coverage of Suzaku will enable us to break possible degeneracies between the properties of the broadened lines and the continuum, providing more convidence on the results. | GALACTIC POINT SOURCES | 4 | A | MADEJ | OLIWIA | NULL | NULL | EUR | 6 | AO6 | INVESTIGATING THE ORIGIN OF THE CONTINUUM AND LINE EMISSION IN THE UCXBS 4U 0614+091 AND 4U 1543-624 | XIS | Y |
| AX J1818.8-1559 | 274.7184 | -16.0002 | 15.02984997 | -0.2600064 | 265.8517 | 55849.5538888889 | 55852.1474537037 | 406074010 | 95191.2 | 100000 | 99385.9 | 99385.9 | 0 | 95191.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 83874.6 | 83874.6 | 224069.9 | 1 | PROCESSED | 57603.4900347222 | 56241 | 55873.993599537 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 062016 | The Galactic X-ray source AX J1818.8-1559 is a possible new member of the small class of magnetar candidates since a short and soft burst was detected in the 15--100 keV range from this source in 2007 with INTEGRAL. We request a Suzaku pointing of 100 ks in order to carry out a sensitive search for pulsations. This, together with the good quality spectrum, possibly extending in the hard X-ray range, that can be obtained with the Suzaku instruments, will allow us to reveal the nature of AX J1818.8-1559, most likely adding a new member to the small but rapidly increasing family of magnetar candidates | GALACTIC POINT SOURCES | 4 | B | MEREGHETTI | SANDRO | NULL | NULL | EUR | 6 | AO6 | A NEW GALACTIC MAGNETAR CANDIDATE | XIS | Y |
| 4U 1705-44 | 257.2257 | -44.096 | 343.32512852 | -2.33758895 | 104.9955 | 56013.5320486111 | 56016.4231134259 | 406076010 | 100811.2 | 100000 | 100811.2 | 100819.2 | 0 | 100820.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 90075.9 | 90075.9 | 249767.7 | 2 | PROCESSED | 57605.1022453704 | 56393 | 56027.2013657407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 062019 | We propose a ToO Suzaku 100-ks observation of the neutron star X-ray binary 4U 1705-44, to perform a detailed study of its broad-band (0.4-200 keV) X-ray spectrum during a hard state. XIS data will provide important information on the iron K-shell features, and the broad-band spectral capabilities of the HXD will allow to study the hard X-ray spectrum and in particular the Compton reflection bump at 20-50 keV. We plan to fit both the iron features and the reflection bump with a self-consistent model, which will allow to prove (or disprove) a disk origin of the iron line. Moreover the proposed observation will allow to study the correlation between the spectral index of the primary spectrum and the reflection amplitude, which gives important constraints on the geometry of the system. | GALACTIC POINT SOURCES | 4 | A | DI SALVO | TIZIANA | NULL | NULL | EUR | 6 | AO6-TOO | SUZAKU BROAD-BAND OBSERVATION OF 4U 1705-44: PROBING THE DISK ORIGIN OF THE IRON LINE IN THE HARD STATE | XIS | Y |
| IGRJ16479-4514 | 252.0242 | -45.1934 | 340.16807688 | -0.11668459 | 91.5317 | 55980.9438194444 | 55983.5363541667 | 406078010 | 149778.5 | 150000 | 149786.5 | 149778.5 | 0 | 149786.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 154729.5 | 154729.5 | 223981.9 | 0 | PROCESSED | 57604.8063888889 | 56429 | 56062.2788425926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 068014 | We propose a 100 ks observation of the Supergiant Fast X-ray Transient (SFXT) with the shortest orbital period, the eclipsing IGRJ16479-4514 (3.3 d), with the main aim of probing its X-ray properties along one entire orbital phase with unprecedented sensitivity. The requested net exposure time indeed translates into an observation almost continuously spanning the whole binary system orbit, allowing for the first time an orbital phase resolved investigation of the X-ray emission properties, which will allow us to study the structure of the supergiant companion (its density and ionization state) and to cast light on the outburst mechanism at work in this new class of transients. | GALACTIC POINT SOURCES | 4 | A | SIDOLI | LARA | BODAGHEE | ARASH | EUS | 6 | AO6 | UNVEILING THE MYSTERY OF THE SUPERGIANT FAST X-RAY TRANSIENT WITH THE SHORTEST ORBITAL PERIOD | XIS | Y |
| H1743-322 | 266.5676 | -32.2352 | 357.25483145 | -1.83570092 | 273.6877 | 56204.7822800926 | 56205.6078240741 | 407005010 | 20811 | 40000 | 20811 | 20811 | 0 | 20811 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42433.7 | 42433.7 | 71321.9 | 0 | PROCESSED | 57607.2960300926 | 56595 | 56226.5596296296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070002 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 7 | AO7-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | XIS | Y |
| H1743-322 | 266.5662 | -32.2338 | 357.25541352 | -1.83396197 | 273.6881 | 56210.6462268518 | 56211.5862731482 | 407005020 | 21192.2 | 40000 | 21192.2 | 21192.2 | 0 | 21192.2 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 41517 | 41517 | 81215.9 | 2 | PROCESSED | 57607.7447337963 | 56595 | 56226.5882291667 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070002 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 7 | AO7-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | XIS | Y |
| H1743-322 | 266.5672 | -32.235 | 357.25482673 | -1.83530791 | 277.9713 | 56212.4049884259 | 56213.3744560185 | 407005030 | 21361 | 40000 | 21370.6 | 21372.2 | 0 | 21361 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 40615 | 40615 | 83736 | 1 | PROCESSED | 57607.7385416667 | 56598 | 56232.473275463 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070002 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 7 | AO7-TOO | MULTIWAVELENGH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | XIS | Y |
| HEN 3-461 | 159.7779 | -51.4088 | 282.90269516 | 6.2428626 | 116.1715 | 56278.1336342593 | 56278.906400463 | 407007010 | 45734.8 | 40000 | 45734.8 | 45734.8 | 0 | 45734.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46677.4 | 46677.4 | 66761.9 | 0 | PROCESSED | 57608.3071990741 | 56018 | 56303.5505902778 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070021 | Hard X-ray emitting symbiotic stars have been identified to emit 6.4 keV iron line with similar equivalent width of the 6.4 keV line of the Galactic Ridge X-ray Emission (GRXE). Only four of such hard X-ray emitting symbiotic stars have been observed with Suzaku. We propose to use Suzaku observations of all the eight newly discovered hard X-ray emitting symbiotic stars to ascertain if they have similar equivalent width of the 6.4 keV line of the GRXE. We will also confirm the emission of hard X-rays above 10 keV using the HXD PIN and use this feature to test for non-thermal emission in these objects. | GALACTIC POINT SOURCES | 4 | C | EZE | ROMANUS | NULL | NULL | JAP | 7 | AO7 | SEARCH FOR 6.4 KEV IRON EMISSION LINE IN THE NEWLY DISCOVERED HARD X-RAY EMITTING SYMBIOTIC STARS | XIS | Y |
| MRK 520 | 330.1768 | 10.545 | 69.38972894 | -34.038497 | 250.5002 | 56258.8186458333 | 56260.6571412037 | 407014010 | 79779.5 | 80000 | 79779.5 | 79787.5 | 0 | 79795.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 77641 | 77641 | 158825.8 | 1 | PROCESSED | 57608.1523263889 | 56644 | 56275.7255555556 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070028 | Compton-thick AGNs contribute to the hard X-ray background and are key objects for investigating the cosmological evolution of AGNs. But heavy obscuration under 10 keV, and source misidentification mean that very few sources have been studied in detail. We have developed new infrared and hard X-ray diagnostics of AGN identification, based on which we select one candidate, Mrk 520, which must be very highly obscured and likely Compton-thick. With Suzaku, we will characterize all emission components, not only thermal and scattering components under 10 keV, but also the heavily obscured continuum over 10 keV, and reflection components. | GALACTIC POINT SOURCES | 4 | C | MATSUTA | KEIKO | NULL | NULL | JAP | 7 | AO7 | MRK 520 : A NEW COMPTON-THICK AGN? | XIS | Y |
| CYG X-1 | 299.5875 | 35.2031 | 71.33506579 | 3.06957776 | 88.7802 | 56390.0953472222 | 56391.9585532407 | 407015010 | 4149.9 | 85000 | 8503 | 4149.9 | 0 | 66475.1 | 2 | 1 | 0 | 1 | 1 | 0 | 0 | 71712.8 | 71712.8 | 160965.8 | 3 | PROCESSED | 57611.2046875 | 56808 | 56402.1391087963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070030 | We propose to observe Cyg X-1 for 85 ks, utilizing P-sum mode for XIS3. Our aim is to perform shot analysis, which is originally invented by Negoro et al. 1995 with Ginga, and obtain high-quality wide-band spectra for several phases in less than 1 sec; for example, 0.1 sec before the peak, +/- 0.05 sec at the peak, and after the peak. With these spectra, we will quantify changes in five spectral components: hard Comptonization, soft Comptonization, disk emission, Fe-K lines, and reflection. This will be a clue to know long-standing mystery on rapid variability in black holes. | GALACTIC POINT SOURCES | 4 | A | YAMADA | SHINYA | NULL | NULL | JAP | 7 | AO7 | INVESTIGATION OF DYNAMICAL SPECTRAL CHANGE IN CYG X-1 | XIS | Y |
| CYG X-1 | 299.5787 | 35.2024 | 71.3307159 | 3.0753508 | 59.5691 | 56419.0925578704 | 56419.6071643518 | 407015020 | 1512.4 | 20000 | 3244.2 | 1512.4 | 0 | 21480 | 2 | 2 | 0 | 1 | 1 | 0 | 0 | 20925.8 | 20925.8 | 44458 | 0 | PROCESSED | 57611.2625347222 | 56808 | 56442.9715509259 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070030 | We propose to observe Cyg X-1 for 85 ks, utilizing P-sum mode for XIS3. Our aim is to perform shot analysis, which is originally invented by Negoro et al. 1995 with Ginga, and obtain high-quality wide-band spectra for several phases in less than 1 sec; for example, 0.1 sec before the peak, +/- 0.05 sec at the peak, and after the peak. With these spectra, we will quantify changes in five spectral components: hard Comptonization, soft Comptonization, disk emission, Fe-K lines, and reflection. This will be a clue to know long-standing mystery on rapid variability in black holes. | GALACTIC POINT SOURCES | 4 | A | YAMADA | SHINYA | NULL | NULL | JAP | 7 | AO7 | INVESTIGATION OF DYNAMICAL SPECTRAL CHANGE IN CYG X-1 | XIS | Y |
| Z CAM | 126.3 | 73.123 | 141.36861973 | 32.62424745 | 91.2043 | 56239.0368981482 | 56239.7800347222 | 407016010 | 35852 | 35000 | 35852 | 35852 | 0 | 35852 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 33896.8 | 33896.8 | 64193.9 | 1 | PROCESSED | 57607.9797337963 | 56631 | 56264.602349537 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070038 | Dwarf novae are a subclass of cataclysmic variables, which sometimes show outbursts. In the outbursts, they are considered to emanate disk winds, but observational evidence had been lacking. Recently, our Suzaku observation of Z Cam during a very transition from quiescence to an outburst revealed clear evidence of the disk wind for the first time, and we were able to study characteristics of the disk wind in detail. Z Cam in quiescence, however, has never been observed with high quality instruments. We, therefore, propose an observation of Z Cam in quiescence in order to study entire behavior of the disk wind throughout different phases, combining the existent Suzaku transition phase data and ASCA archival data taken in other phases. | GALACTIC POINT SOURCES | 4 | C | SAITOU | KEI | NULL | NULL | JAP | 7 | AO7 | COMPREHENSIVE STUDY FOR THE DISK WIND OF THE DWARF NOVA Z CAM THROUGH OUTBURST CYCLES WITH AN OBSERVATION IN QUIESCENCE | XIS | Y |
| AX J1622.1-5005 | 245.5334 | -50.0932 | 333.60606211 | -0.20489946 | 274.3812 | 56160.9968402778 | 56161.9398148148 | 407018010 | 39126.3 | 40000 | 40536.6 | 40536.6 | 0 | 39126.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37476 | 37476 | 81461.9 | 0 | PROCESSED | 57606.9317824074 | 56667 | 56300.5637731482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070043 | Through studies of magnetars and supernova remnants associated to them, we have arrived at a possibility that magnetars are in fact much younger than their characteristic ages, and hence are born with a much higher rate than was considered previously. This predicts a large population of aged magnetars to lurk in the Galactic plane as slowly rotating soft X-ray sources. From the X-ray source catalog with the ASCA Galactic plane survey, we have selected four candidates for such aged magnetars, and propose to observe them for 40 ksec each. We expect them to appear as faint soft X-ray sources with blackbody temperatures of 0.5 keV or so, possibly pulsating at periods of about 10 seconds. One FI CCD of the XIS is set in the 1/8-window option to achieve a sufficient time resolution. | GALACTIC POINT SOURCES | 4 | A | MAKISHIMA | KAZUO | NULL | NULL | JAP | 7 | AO7 | ARE A LARGE FRACTION OF NEUTRON STARS BORN AS MAGNETARS? | XIS | Y |
| AX J1846.8-0240 | 281.7182 | -2.6613 | 30.04319345 | -0.19850989 | 89.4057 | 56018.0125115741 | 56019.1146990741 | 407019010 | 37620.9 | 40000 | 37620.9 | 41612.7 | 0 | 39220.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37250 | 37250 | 95219.9 | 0 | PROCESSED | 57605.0756944445 | 56400 | 56033.2323032407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070043 | Through studies of magnetars and supernova remnants associated to them, we have arrived at a possibility that magnetars are in fact much younger than their characteristic ages, and hence are born with a much higher rate than was considered previously. This predicts a large population of aged magnetars to lurk in the Galactic plane as slowly rotating soft X-ray sources. From the X-ray source catalog with the ASCA Galactic plane survey, we have selected four candidates for such aged magnetars, and propose to observe them for 40 ksec each. We expect them to appear as faint soft X-ray sources with blackbody temperatures of 0.5 keV or so, possibly pulsating at periods of about 10 seconds. One FI CCD of the XIS is set in the 1/8-window option to achieve a sufficient time resolution. | GALACTIC POINT SOURCES | 4 | A | MAKISHIMA | KAZUO | NULL | NULL | JAP | 7 | AO7 | ARE A LARGE FRACTION OF NEUTRON STARS BORN AS MAGNETARS? | XIS | Y |
| AX J1620.7-4942 | 245.1985 | -49.7112 | 333.72306976 | 0.21790295 | 274.6004 | 56158.5209027778 | 56159.5245717593 | 407020010 | 42206.2 | 40000 | 44271.3 | 44274.4 | 0 | 42206.2 | 3 | 2 | 0 | 3 | 1 | 0 | 0 | 44805.2 | 44805.2 | 86711.9 | 0 | PROCESSED | 57606.89875 | 56582 | 56212.7789930556 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070043 | Through studies of magnetars and supernova remnants associated to them, we have arrived at a possibility that magnetars are in fact much younger than their characteristic ages, and hence are born with a much higher rate than was considered previously. This predicts a large population of aged magnetars to lurk in the Galactic plane as slowly rotating soft X-ray sources. From the X-ray source catalog with the ASCA Galactic plane survey, we have selected four candidates for such aged magnetars, and propose to observe them for 40 ksec each. We expect them to appear as faint soft X-ray sources with blackbody temperatures of 0.5 keV or so, possibly pulsating at periods of about 10 seconds. One FI CCD of the XIS is set in the 1/8-window option to achieve a sufficient time resolution. | GALACTIC POINT SOURCES | 4 | A | MAKISHIMA | KAZUO | NULL | NULL | JAP | 7 | AO7 | ARE A LARGE FRACTION OF NEUTRON STARS BORN AS MAGNETARS? | XIS | Y |
| AX J1445.7-5931 | 221.4519 | -59.5275 | 316.97780419 | 0.18867801 | 281.526 | 56143.2829513889 | 56144.2918865741 | 407021010 | 40052.5 | 40000 | 41068.2 | 41060.2 | 0 | 40052.5 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 36808.9 | 36808.9 | 87157.9 | 1 | PROCESSED | 57606.7459722222 | 56533 | 56167.2116319444 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070043 | Through studies of magnetars and supernova remnants associated to them, we have arrived at a possibility that magnetars are in fact much younger than their characteristic ages, and hence are born with a much higher rate than was considered previously. This predicts a large population of aged magnetars to lurk in the Galactic plane as slowly rotating soft X-ray sources. From the X-ray source catalog with the ASCA Galactic plane survey, we have selected four candidates for such aged magnetars, and propose to observe them for 40 ksec each. We expect them to appear as faint soft X-ray sources with blackbody temperatures of 0.5 keV or so, possibly pulsating at periods of about 10 seconds. One FI CCD of the XIS is set in the 1/8-window option to achieve a sufficient time resolution. | GALACTIC POINT SOURCES | 4 | A | MAKISHIMA | KAZUO | NULL | NULL | JAP | 7 | AO7 | ARE A LARGE FRACTION OF NEUTRON STARS BORN AS MAGNETARS? | XIS | Y |
| 1RXSJ170047.8-314442 | 255.196 | -31.7452 | 352.21229356 | 6.40020757 | 90.7944 | 56341.4932060185 | 56341.7501273148 | 407027010 | 8926.2 | 12000 | 8926.2 | 8926.2 | 0 | 8926.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 8232 | 8232 | 22186 | 0 | PROCESSED | 57610.6225810185 | 56718 | 56352.4986458333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070052 | We propose to study wide-band X-ray properties of 9 unidentified sources with luminosities of ~10^35 erg/s. These sources are a part of the first complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge, that is constructed from the detected sources in the ROSAT All Sky Survey (Mori 2005, PhD. thesis). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with follow-up optical identifications. This is a new step toward understanding the formation history of the bulge, and hence that of galaxies with various Hubble sequences in the universe. | GALACTIC POINT SOURCES | 4 | C | MORI | HIDEYUKI | NULL | NULL | JAP | 7 | AO7 | SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE | XIS | Y |
| 1RXSJ173905.2-392615 | 264.7748 | -39.4365 | 350.35081336 | -4.37467046 | 271.2006 | 56188.8237384259 | 56189.3446990741 | 407029010 | 22063.8 | 15000 | 22071.8 | 22063.8 | 0 | 22071.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 18251.5 | 18251.5 | 44999.9 | 0 | PROCESSED | 57607.0891898148 | 56584 | 56218.4994212963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070052 | We propose to study wide-band X-ray properties of 9 unidentified sources with luminosities of ~10^35 erg/s. These sources are a part of the first complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge, that is constructed from the detected sources in the ROSAT All Sky Survey (Mori 2005, PhD. thesis). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with follow-up optical identifications. This is a new step toward understanding the formation history of the bulge, and hence that of galaxies with various Hubble sequences in the universe. | GALACTIC POINT SOURCES | 4 | C | MORI | HIDEYUKI | NULL | NULL | JAP | 7 | AO7 | SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE | XIS | Y |
| U GEM IN QUIECSECNCE | 118.777 | 21.9977 | 199.22882002 | 23.39765052 | 280.879 | 56041.5636921296 | 56044.5765856482 | 407034010 | 119113.6 | 120000 | 119113.6 | 119113.6 | 0 | 119113.6 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 102835.4 | 102835.4 | 260306 | 1 | PROCESSED | 57605.3496064815 | 56434 | 56068.6228356482 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070065 | It has been believed that the optically thin boundary layer in dwarf novae (DNe) turns into optically thick state in outburst, and, as a result, hard optically thin X-ray emission becomes weaker than in quiescence. This theory was verified in multi-waveband observations of SS Cyg. The DN U Gem, however, does not follow this scenario, and the hard X-ray intensity increases in outburst as well as soft X-ray emission. We propose ToO observations of U Gem both in quiescence and in outburst in order to understand behavior of DNe in X-rays in general, by means of detailed spectroscopy of the soft disk blackbody component, the hard component reflected off the white dwarf, and a 6.4 keV iron line. This study eventually enables us to understand the origin of the Galactic Ridge X-ray Emission. | GALACTIC POINT SOURCES | 4 | B | HAYASHI | TAKAYUKI | NULL | NULL | JAP | 7 | AO7-TOO | OBSERVATION OF THE DWARF NOVA U GEM IN QUIESCENCE AND OUTBURST | XIS | Y |
| U GEM IN OUTBURST | 118.7732 | 21.9928 | 199.23241259 | 23.39259554 | 281.117 | 56029.4105324074 | 56030.750162037 | 407035010 | 50254.7 | 50000 | 50254.7 | 50254.7 | 0 | 50254.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47296.7 | 47296.7 | 115707.9 | 1 | PROCESSED | 57605.2002199074 | 56415 | 56044.3887731482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070065 | It has been believed that the optically thin boundary layer in dwarf novae (DNe) turns into optically thick state in outburst, and, as a result, hard optically thin X-ray emission becomes weaker than in quiescence. This theory was verified in multi-waveband observations of SS Cyg. The DN U Gem, however, does not follow this scenario, and the hard X-ray intensity increases in outburst as well as soft X-ray emission. We propose ToO observations of U Gem both in quiescence and in outburst in order to understand behavior of DNe in X-rays in general, by means of detailed spectroscopy of the soft disk blackbody component, the hard component reflected off the white dwarf, and a 6.4 keV iron line. This study eventually enables us to understand the origin of the Galactic Ridge X-ray Emission. | GALACTIC POINT SOURCES | 4 | B | HAYASHI | TAKAYUKI | NULL | NULL | JAP | 7 | AO7-TOO | OBSERVATION OF THE DWARF NOVA U GEM IN QUIESCENCE AND OUTBURST | XIS | Y |
| IGR J17091-3624 | 257.2866 | -36.4073 | 349.52701092 | 2.20940495 | 283.8915 | 56202.8636689815 | 56203.7202662037 | 407037010 | 42075.9 | 120000 | 42075.9 | 42083.7 | 0 | 42079.7 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 40392 | 40392 | 74007.9 | 0 | PROCESSED | 57607.2660069444 | 56728 | 56226.6701388889 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070097 | We propose a Suzaku observation of "the second GRS 1915+105" IGR J17091-3624 with a high energy resolution and broadband capability. GRS 1915+105 has been considered to be the unique black hole binary that stays at a high mass accretion rate and shows limit-cycle oscillations, but it was recently discovered that the BHC IGR J17091-3624 has exactly the same X-ray variability patterns as GRS 1915+105. This fact suggests an evidence for common physical mechanism in both system. The Suzaku observation will reveal both similarity and difference with GRS 1915+105 from a point of view of broad-band spectral properties and disk wind, and help us understanding of the accretion flow onto a black hole under a high mass accretion rate. | GALACTIC POINT SOURCES | 4 | B | YAMAOKA | KAZUTAKA | NULL | NULL | JAP | 7 | AO7 | SUZAKU BROADBAND OBSERVATION OF "THE SECOND GRS 1915+105" IGR J17091-3624 | XIS | Y |
| IGR J17091-3624 | 257.2807 | -36.4071 | 349.52434208 | 2.21333885 | 90.7245 | 56342.7065162037 | 56344.8856828704 | 407037020 | 81946.7 | 80000 | 81946.7 | 81946.7 | 0 | 81946.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 72871 | 72871 | 188260 | 1 | PROCESSED | 57610.6944212963 | 56728 | 56363.6146990741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070097 | We propose a Suzaku observation of "the second GRS 1915+105" IGR J17091-3624 with a high energy resolution and broadband capability. GRS 1915+105 has been considered to be the unique black hole binary that stays at a high mass accretion rate and shows limit-cycle oscillations, but it was recently discovered that the BHC IGR J17091-3624 has exactly the same X-ray variability patterns as GRS 1915+105. This fact suggests an evidence for common physical mechanism in both system. The Suzaku observation will reveal both similarity and difference with GRS 1915+105 from a point of view of broad-band spectral properties and disk wind, and help us understanding of the accretion flow onto a black hole under a high mass accretion rate. | GALACTIC POINT SOURCES | 4 | B | YAMAOKA | KAZUTAKA | NULL | NULL | JAP | 7 | AO7 | SUZAKU BROADBAND OBSERVATION OF "THE SECOND GRS 1915+105" IGR J17091-3624 | XIS | Y |
| II PEG | 358.7744 | 28.6284 | 108.23861581 | -32.63076231 | 231.1411 | 56301.1877314815 | 56303.6487962963 | 407038010 | 17017.6 | 100000 | 111506.5 | 111514.5 | 0 | 17017.6 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 107905.8 | 107905.8 | 212619.8 | 2 | PROCESSED | 57608.5074305556 | 56724 | 56363.602037037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070102 | We propose a Suzaku observation of the powerful flare star II Peg with the high sensitivity of HXD. MAXI/GSC results from 2009 to 2011 show that this source exhibits the highest flaring activity with the largest luminosities and the largest fluxes. Then detection of the non-thermal emission is the most expected from this source at the on-set of a flare. We are to observe this target simultaneously with radio, infrared, optical, and X-ray bands for the first time. Our goal is (1) to detect impulsive non-thermal emission at the powerful II Peg flare (2) to obtain wide-band SED variability from radio to hard X-ray band, and (3) to establish unified view of stellar flare mechanism via the wide radio-X-ray band. | GALACTIC POINT SOURCES | 4 | C | TSUBOI | YOHKO | NULL | NULL | JAP | 7 | AO7 | NON-THERMAL EMISSION ON THE POWERFUL STELLAR FLARE FROM II PEG | XIS | Y |
| EUVE J1439 +75.0 | 219.9459 | 75.0823 | 114.11249059 | 40.13551871 | 340.4897 | 56067.2884722222 | 56067.8599421296 | 407039010 | 29961.3 | 40000 | 29969.3 | 29969.3 | 0 | 29961.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 32393.2 | 32393.2 | 49343.9 | 0 | PROCESSED | 57605.4757523148 | 56442 | 56076.028912037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070112 | The main purpose of the proposal is to search for possible non-thermal emission from isolated white dwarfs (WDs) with Suzaku. The origins of cosmic-rays are a long standing mystery for just 100 years in AO-7 phase from a discovery by Hess. One of the most important milestones recently is the discovery of a hint of "a WD pulsar" in the AE Aquarii system with Suzaku, because number density of this class is much larger than those of famous acceleration sites like SNRs, NS pulsars, etc. The next step is to detect non thermal emissions from isolated WDs. We search for promising objects from a large sample of white dwarfs by SDDS survey, and finally found three isolated magnetized WDs; EUVE J1439+75.0, PG 1658+440 and EUVE J0823-25.4. Here, we propose Suzaku observations of these objects. | GALACTIC POINT SOURCES | 4 | B | HARAYAMA | ATSUSHI | NULL | NULL | JAP | 7 | AO7 | SEARCH FOR NON THERMAL EMISSION FROM ISOLATED MAGNETIZED WHITE WDARFS | XIS | Y |
| PG 1658 +440 | 254.9348 | 44.0094 | 69.11167171 | 38.06633743 | 330.9998 | 56115.6740972222 | 56116.8301041667 | 407040010 | 51032.9 | 50000 | 51032.9 | 51032.9 | 0 | 51032.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 46674.6 | 46674.6 | 99871.8 | 1 | PROCESSED | 57606.5897222222 | 56508 | 56142.1447337963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070112 | The main purpose of the proposal is to search for possible non-thermal emission from isolated white dwarfs (WDs) with Suzaku. The origins of cosmic-rays are a long standing mystery for just 100 years in AO-7 phase from a discovery by Hess. One of the most important milestones recently is the discovery of a hint of "a WD pulsar" in the AE Aquarii system with Suzaku, because number density of this class is much larger than those of famous acceleration sites like SNRs, NS pulsars, etc. The next step is to detect non thermal emissions from isolated WDs. We search for promising objects from a large sample of white dwarfs by SDDS survey, and finally found three isolated magnetized WDs; EUVE J1439+75.0, PG 1658+440 and EUVE J0823-25.4. Here, we propose Suzaku observations of these objects. | GALACTIC POINT SOURCES | 4 | B | HARAYAMA | ATSUSHI | NULL | NULL | JAP | 7 | AO7 | SEARCH FOR NON THERMAL EMISSION FROM ISOLATED MAGNETIZED WHITE WDARFS | XIS | Y |
| WR140 | 305.1374 | 43.8475 | 80.93293792 | 4.16074264 | 212.5272 | 56283.3528356482 | 56284.2085300926 | 407041010 | 54780.2 | 50000 | 54796.2 | 54780.2 | 0 | 54804.2 | 3 | 2 | 0 | 3 | 1 | 0 | 0 | 52381.1 | 52381.1 | 73920 | 0 | PROCESSED | 57608.3396990741 | 56710 | 56344.6961689815 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071203 | In the campaign observations of the prototypical colliding wind binary system WR 140 at its last periastron passage in 2009, Suzaku discovered an extremely hard and variable X-ray component. The current best explanation of its origin is inverse-Compton cooling of particles accelerated in the wind-wind collision shock, and if so this would be the first detection of non-thermal X-ray emission from any Wolf-Rayet system. However, other mechanisms cannot be excluded because the observed intensity was stronger than expected from the observed radio luminosity. We propose to re-observe WR 140 near apastron in 2012 with Suzaku to identify the emission mechanism which produces the hard component. | GALACTIC POINT SOURCES | 4 | C | HAMAGUCHI | KENJI | NULL | NULL | USA | 7 | AO7 | MEASURING EXTREMELY HARD X-RAY EMISSION FROM WR140 AT APASTRON | XIS | Y |
| HEN 3-1591 | 271.8863 | -25.8981 | 5.07192211 | -2.68044312 | 269.6421 | 56203.7249537037 | 56204.7793981482 | 407042010 | 51387.6 | 50000 | 51387.7 | 51387.6 | 0 | 51403.6 | 4 | 3 | 0 | 3 | 1 | 0 | 0 | 52368.1 | 52368.1 | 91095.9 | 1 | PROCESSED | 57607.2899884259 | 56592 | 56226.5545601852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071211 | The number of symbiotic stars known to be medium energy (2-10 keV) X-ray emitters has increased markedly in the last several years. These are white dwarfs accreting from a giant mass donor, unlike the less common class of symbiotic X-ray binaries in which the accretor is a neutron star. The X-ray spectra of the white dwarf symbiotics can be used to constrain the white dwarf mass and accretion rate. Here we focus on one object, Hen 3-1591, which belongs to a rare subclass of d'-type yellow symbiotic, commonly thought to harbor a young white dwarf. Hen 3-1591 is the first of this subclass to show medium energy X-ray emission, and hence we propose a moderately deep Suzaku observation to characterize its white dwarf and the circum-binary environment. | GALACTIC POINT SOURCES | 4 | B | MUKAI | KOJI | NULL | NULL | USA | 7 | AO7 | THE X-RAY EMISSION OF THE YELLOW SYMBIOTIC STAR, HEN 3-1591 | XIS | Y |
| CH UMA | 151.7457 | 67.5324 | 142.91256562 | 42.65793237 | 289.9979 | 56048.5009490741 | 56049.4815046296 | 407043010 | 45204.5 | 40000 | 45204.5 | 45204.5 | 0 | 45204.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43375.1 | 43375.1 | 84698.1 | 0 | PROCESSED | 57605.3249652778 | 56435 | 56068.6246180556 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071212 | The mass of an accreting white dwarf is a key parameter governing its X-ray emission. We expect that the higher the mass, the higher the temperature and luminosity. Existing data appear consistent with this expectation, given the considerable uncertainties usually associated with the white dwarf masses of individual systems. Here we propose Suzaku observations of 5 dwarf novae for which very high or very low white dwarf mass estimates have been published. These targets provide the best opportunity of further establishing the mass-temperature correlation. Moreover, if the mass estimates are reliable, these targets are of interest from evolutionary considerations - how did these systems form with such high/low mass white dwarfs, and what are their ultimate fates? | GALACTIC POINT SOURCES | 4 | A | MUKAI | KOJI | NULL | NULL | USA | 7 | AO7 | DWARF NOVAE WITH EXTREME WHITE DWARF MASSES | XIS | Y |
| EK TRA | 228.5098 | -65.0893 | 317.22984637 | -6.25468419 | 278.6002 | 56149.7387152778 | 56150.8473611111 | 407044010 | 77834.4 | 70000 | 77850.4 | 77834.4 | 0 | 77850.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 69897.3 | 69897.3 | 95777.9 | 2 | PROCESSED | 57606.8494907407 | 56540 | 56170.0360532407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071212 | The mass of an accreting white dwarf is a key parameter governing its X-ray emission. We expect that the higher the mass, the higher the temperature and luminosity. Existing data appear consistent with this expectation, given the considerable uncertainties usually associated with the white dwarf masses of individual systems. Here we propose Suzaku observations of 5 dwarf novae for which very high or very low white dwarf mass estimates have been published. These targets provide the best opportunity of further establishing the mass-temperature correlation. Moreover, if the mass estimates are reliable, these targets are of interest from evolutionary considerations - how did these systems form with such high/low mass white dwarfs, and what are their ultimate fates? | GALACTIC POINT SOURCES | 4 | A | MUKAI | KOJI | NULL | NULL | USA | 7 | AO7 | DWARF NOVAE WITH EXTREME WHITE DWARF MASSES | XIS | Y |
| BF ERI | 69.8754 | -4.5962 | 201.0367912 | -31.29845078 | 262.0133 | 56350.9190625 | 56351.6253009259 | 407045010 | 32817.7 | 30000 | 32817.7 | 32817.7 | 0 | 32817.8 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 32016.1 | 32016.1 | 61009.9 | 1 | PROCESSED | 57610.6930092593 | 56738 | 56372.5138773148 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071212 | The mass of an accreting white dwarf is a key parameter governing its X-ray emission. We expect that the higher the mass, the higher the temperature and luminosity. Existing data appear consistent with this expectation, given the considerable uncertainties usually associated with the white dwarf masses of individual systems. Here we propose Suzaku observations of 5 dwarf novae for which very high or very low white dwarf mass estimates have been published. These targets provide the best opportunity of further establishing the mass-temperature correlation. Moreover, if the mass estimates are reliable, these targets are of interest from evolutionary considerations - how did these systems form with such high/low mass white dwarfs, and what are their ultimate fates? | GALACTIC POINT SOURCES | 4 | C | MUKAI | KOJI | NULL | NULL | USA | 7 | AO7 | DWARF NOVAE WITH EXTREME WHITE DWARF MASSES | XIS | Y |
| BV CEN | 202.8234 | -54.9803 | 308.67903183 | 7.44609562 | 120.7167 | 56329.0246875 | 56329.4856018518 | 407047010 | 33380 | 30000 | 33388 | 33388 | 0 | 33380 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 30869.2 | 30869.2 | 39815.9 | 0 | PROCESSED | 57610.5262268518 | 56715 | 56349.4846990741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071212 | The mass of an accreting white dwarf is a key parameter governing its X-ray emission. We expect that the higher the mass, the higher the temperature and luminosity. Existing data appear consistent with this expectation, given the considerable uncertainties usually associated with the white dwarf masses of individual systems. Here we propose Suzaku observations of 5 dwarf novae for which very high or very low white dwarf mass estimates have been published. These targets provide the best opportunity of further establishing the mass-temperature correlation. Moreover, if the mass estimates are reliable, these targets are of interest from evolutionary considerations - how did these systems form with such high/low mass white dwarfs, and what are their ultimate fates? | GALACTIC POINT SOURCES | 4 | C | MUKAI | KOJI | NULL | NULL | USA | 7 | AO7 | DWARF NOVAE WITH EXTREME WHITE DWARF MASSES | XIS | Y |
| T PYXIDIS | 136.1704 | -32.3688 | 257.19727302 | 9.71237496 | 121.9943 | 56266.272662037 | 56268.8695486111 | 407048010 | 86676 | 100000 | 86676 | 86676 | 0 | 86676 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 73611.8 | 73611.8 | 224357.9 | 4 | PROCESSED | 57608.249525463 | 56660 | 56291.8230787037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071213 | We propose a 100 ks observation of the classical nova remnant in the accreting binary system T Pyxidis using Suzaku. T Pyxidis is a system which causes a cycle of classical nova outbursts in a decade time scale. Shocks might occur in the ejecta, and X-rays were detected from its spatially-resolved expanding shell like a miniature supernova remnant. The immediate purposes of this program are (1) to derive the X-ray flux and luminosity after its last outburst in 2011, (2) to diagnose plasma temperature deeply, and (3) to obtain the second sample of non-thermal X-ray emission from classical nova remnants. The target is a remarkable newly discovered candidate of cosmic-ray acceleration sites, and a successful detection of non-thermal X-rays provides a new view of cosmic-ray origins. | GALACTIC POINT SOURCES | 4 | C | TAKEI | DAI | NULL | NULL | USA | 7 | AO7 | COSMIC-RAYS FROM MINIATURE SUPERNOVA REMNANTS | XIS | Y |
| HERCULES X-1 | 254.4605 | 35.3288 | 58.13264186 | 37.51848299 | 268.7999 | 56189.3538310185 | 56190.0300231482 | 407051010 | 25535.6 | 20000 | 25543.6 | 25549.4 | 0 | 25535.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25087.9 | 25087.9 | 58421.9 | 0 | PROCESSED | 57607.1017013889 | 56590 | 56218.5228472222 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071224 | This proposal is for the continuation of successful Suzaku observations of Her X-1. The proposal is led by the NuSTAR team, extended with experts on X-ray binary pulsars with cyclotron lines. We propose three 20 ks simultaneous Suzaku and NuSTAR observations of Her X-1. Joint observations will substantial increase the science that can be addressed, allowing a systematic study of the fundamental cyclotron line (~40 keV) as a function of time, X-ray flux, 35 day phase, and 1.24 s pulse phase. The combined data will probe fundamental physics in this system, including the structure of the magnetic field in the polar caps, the physics of sub-Eddington accretion, and physical processes inside the neutron star. | GALACTIC POINT SOURCES | 4 | B | GREFENSTETTE | BRIAN | NULL | NULL | USA | 7 | AO7 | STUDY OF THE CYCLOTRON LINE FEATURE IN HERCULES X-1: THE PROFILE AND THE SHORT- AND LONG-TERM VARIABILITY | XIS | Y |
| HERCULES X-1 | 254.4605 | 35.3288 | 58.13264186 | 37.51848299 | 268.3999 | 56192.1811342593 | 56192.781412037 | 407051020 | 22609.4 | 20000 | 22609.4 | 22609.4 | 0 | 22609.4 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 20178.7 | 20178.7 | 51836 | 1 | PROCESSED | 57607.16 | 56590 | 56218.5726967593 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071224 | This proposal is for the continuation of successful Suzaku observations of Her X-1. The proposal is led by the NuSTAR team, extended with experts on X-ray binary pulsars with cyclotron lines. We propose three 20 ks simultaneous Suzaku and NuSTAR observations of Her X-1. Joint observations will substantial increase the science that can be addressed, allowing a systematic study of the fundamental cyclotron line (~40 keV) as a function of time, X-ray flux, 35 day phase, and 1.24 s pulse phase. The combined data will probe fundamental physics in this system, including the structure of the magnetic field in the polar caps, the physics of sub-Eddington accretion, and physical processes inside the neutron star. | GALACTIC POINT SOURCES | 4 | B | GREFENSTETTE | BRIAN | NULL | NULL | USA | 7 | AO7 | STUDY OF THE CYCLOTRON LINE FEATURE IN HERCULES X-1: THE PROFILE AND THE SHORT- AND LONG-TERM VARIABILITY | XIS | Y |
| HERCULES X-1 | 254.4612 | 35.329 | 58.13300626 | 37.51795138 | 268.1998 | 56194.4317708333 | 56195.0641087963 | 407051030 | 23589.4 | 20000 | 23593.1 | 23593.1 | 0 | 23589.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 23476.9 | 23476.9 | 54634 | 0 | PROCESSED | 57607.1945601852 | 56689 | 56323.5148726852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071224 | This proposal is for the continuation of successful Suzaku observations of Her X-1. The proposal is led by the NuSTAR team, extended with experts on X-ray binary pulsars with cyclotron lines. We propose three 20 ks simultaneous Suzaku and NuSTAR observations of Her X-1. Joint observations will substantial increase the science that can be addressed, allowing a systematic study of the fundamental cyclotron line (~40 keV) as a function of time, X-ray flux, 35 day phase, and 1.24 s pulse phase. The combined data will probe fundamental physics in this system, including the structure of the magnetic field in the polar caps, the physics of sub-Eddington accretion, and physical processes inside the neutron star. | GALACTIC POINT SOURCES | 4 | B | GREFENSTETTE | BRIAN | NULL | NULL | USA | 7 | AO7 | STUDY OF THE CYCLOTRON LINE FEATURE IN HERCULES X-1: THE PROFILE AND THE SHORT- AND LONG-TERM VARIABILITY | XIS | Y |
| 4U1538-522 | 235.6015 | -52.3857 | 327.42188954 | 2.16239803 | 275.2972 | 56149.0031134259 | 56149.7349537037 | 407068010 | 45955.4 | 40000 | 45955.4 | 45955.4 | 0 | 45955.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40050 | 40050 | 63212 | 0 | PROCESSED | 57606.8269444444 | 56640 | 56272.688900463 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071233 | Observations of accreting pulsars in High Mass X-ray Binaries (HMXBs) provide us with important information about the physical processes in the stellar wind of the high mass donor star, the coupling between the accreting material and the neutron star's magnetic field, and the physics of the strongly magnetized accretion column above the neutron star. In this proposal we ask for a 40 ks observation of the accreting HMXB 4U1538-522 to conduct the most sensitive study to date of the wide range of characteristics of the broad band (0.1-100 keV) spectrum over a quarter of a binary orbit and with pulse phase. When one considers the ~50% duty cycle of Suzaku observations, the proposed observation will yield coverage of a quarter of the binary orbit. | GALACTIC POINT SOURCES | 4 | A | ROTHSCHILD | RICHARD | NULL | NULL | USA | 7 | AO7 | THE FIRST SUZAKU OBSERVATION OF 4U1538-522 | XIS | Y |
| 1FGL J1018.6-5856 | 154.7397 | -58.9449 | 284.35462729 | -1.68677577 | 302.8974 | 56098.9298611111 | 56100.4612384259 | 407069010 | 72841.2 | 70000 | 72841.2 | 72841.2 | 0 | 72841.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 57677.3 | 57677.3 | 132250 | 0 | PROCESSED | 57605.7791087963 | 56479 | 56113.258900463 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071234 | We propose Suzaku observations of a newly discovered gamma-ray binary 1FGL J1018.6-5856. Recent observations by the Fermi Gamma-ray Space Telescope and follow-up observations in other wavelengths revealed that the gamma-ray source is a new member of the rare gamma-ray binary class with an orbital period of 16 days. We propose two types of observations with Suzaku. One is a continuous observation of a sharp X-ray peak found in the lightcurve by the Swift XRT. Another is a series of snap shot observations in orbital phase between the peaks. We aim to perform phase-resolved spectral analysis which is not possible with the Swift XRT data. We also compare the Swift XRT lightcurve with new lightcurves taken by Suzaku in order to test the repeatability of the X-ray orbital modulation. | GALACTIC POINT SOURCES | 4 | B | TANAKA | TAKAAKI | NULL | NULL | USA | 7 | AO7 | SUZAKU OBSERVATIONS OF A NEWLY DISCOVERED GAMMA-RAY BINARY: 1FGL J1018.6-5856 | XIS | Y |
| 1FGL J1018.6-5856 | 154.7377 | -58.9433 | 284.35288518 | -1.68600623 | 306.342 | 56102.9882407407 | 56103.3696875 | 407070010 | 17447.3 | 20000 | 17464.5 | 17463.3 | 0 | 17447.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14447.4 | 14447.4 | 32949.9 | 2 | PROCESSED | 57606.4834722222 | 56480 | 56114.1719328704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071234 | We propose Suzaku observations of a newly discovered gamma-ray binary 1FGL J1018.6-5856. Recent observations by the Fermi Gamma-ray Space Telescope and follow-up observations in other wavelengths revealed that the gamma-ray source is a new member of the rare gamma-ray binary class with an orbital period of 16 days. We propose two types of observations with Suzaku. One is a continuous observation of a sharp X-ray peak found in the lightcurve by the Swift XRT. Another is a series of snap shot observations in orbital phase between the peaks. We aim to perform phase-resolved spectral analysis which is not possible with the Swift XRT data. We also compare the Swift XRT lightcurve with new lightcurves taken by Suzaku in order to test the repeatability of the X-ray orbital modulation. | GALACTIC POINT SOURCES | 4 | B | TANAKA | TAKAAKI | NULL | NULL | USA | 7 | AO7 | SUZAKU OBSERVATIONS OF A NEWLY DISCOVERED GAMMA-RAY BINARY: 1FGL J1018.6-5856 | XIS | Y |
| 1FGL J1018.6-5856 | 154.7369 | -58.9465 | 284.35429996 | -1.68890631 | 297.8367 | 56093.0246875 | 56093.5348032407 | 407071010 | 20820.3 | 20000 | 20820.3 | 20820.3 | 0 | 20820.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16813 | 16813 | 44063.9 | 0 | PROCESSED | 57605.6779282407 | 56542 | 56176.237025463 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071234 | We propose Suzaku observations of a newly discovered gamma-ray binary 1FGL J1018.6-5856. Recent observations by the Fermi Gamma-ray Space Telescope and follow-up observations in other wavelengths revealed that the gamma-ray source is a new member of the rare gamma-ray binary class with an orbital period of 16 days. We propose two types of observations with Suzaku. One is a continuous observation of a sharp X-ray peak found in the lightcurve by the Swift XRT. Another is a series of snap shot observations in orbital phase between the peaks. We aim to perform phase-resolved spectral analysis which is not possible with the Swift XRT data. We also compare the Swift XRT lightcurve with new lightcurves taken by Suzaku in order to test the repeatability of the X-ray orbital modulation. | GALACTIC POINT SOURCES | 4 | B | TANAKA | TAKAAKI | NULL | NULL | USA | 7 | AO7 | SUZAKU OBSERVATIONS OF A NEWLY DISCOVERED GAMMA-RAY BINARY: 1FGL J1018.6-5856 | XIS | Y |
| CYGNUS X-1 | 299.5969 | 35.1891 | 71.32710759 | 3.05572664 | 254.8701 | 56231.3416782407 | 56232.109212963 | 407072010 | 372.6 | 30000 | 1939.4 | 1990.8 | 0 | 372.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 30085.7 | 30085.7 | 66305.9 | 0 | PROCESSED | 57607.9427430556 | 56611 | 56245.5107407407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071241 | We propose for a single 30 ks observation of the accreting black hole Cygnus X-1. NuSTAR is an upcoming (to be launched in Spring 2012) hard X-ray (5-80 keV) mission that will plan its schedule to obtain simultaneous coverage of Cyg X-1 with Suzaku. The observations will be used for both science and cross-calibration. The combination of Suzaku and NuSTAR will provide the best measurement of the reflection component, including a relativistically broadened iron line and a hard X-ray excess, and the information will be used to test emission models and constrain the Cyg X-1 accretion geometry. The XIS capabilities to measure the iron line are essential for the science, and the HXD coverage is essential for the cross-calibration. | GALACTIC POINT SOURCES | 4 | A | TOMSICK | JOHN | NULL | NULL | USA | 7 | AO7 | CYGNUS X-1 WITH SUZAKU AND NUSTAR | XIS | Y |
| LMC X-3 | 84.7483 | -64.0713 | 273.56080053 | -32.07680965 | 285.8008 | 56379.6769444445 | 56382.4793634259 | 407086010 | 101809 | 100000 | 101817 | 101825 | 0 | 101809 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 92724.6 | 92724.6 | 242101.9 | 1 | PROCESSED | 57611.0169560185 | 56757 | 56391.8067592593 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 072002 | We propose a 100 ksec triggered Suzaku observation of the low/hard state of the black hole LMC X-3. This will constrain the disc emission and Fe line profile in this state, both of which are currently very controversial. LMC X-3 has very low interstellar absorption, so gives the best view of the low temperature/low luminosity disc component in this state. Its moderate flux means it can be observed in standard imaging modes without pileup (further enhancing visibility of the disc as these modes are well calibrated down to 0.4 keV) and making the Fe line profile analysis straightforward. Historically LMC X-3 enters a low/hard state on average once a year. Suzaku will be triggered based on an alert from our Swift monitoring program that the source has entered the low/hard state. | GALACTIC POINT SOURCES | 4 | A | KOLEHMAINEN | MARI | NULL | NULL | EUR | 7 | AO7-TOO | A TOO OF LMC X-3: IS THE DISC TRUNCATED IN THE LOW/HARD STATE OF BLACK HOLE BINARIES? | XIS | Y |
| 4U 0352+30 | 58.8427 | 31.0494 | 163.07655547 | -17.13553633 | 77.7002 | 56166.360150463 | 56170.0980208333 | 407088010 | 153489.3 | 150000 | 153489.3 | 153489.3 | 0 | 153489.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 140991.9 | 140991.9 | 322923.6 | 3 | PROCESSED | 57607.0637268518 | 56582 | 56212.7609722222 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 072011 | After 40 years of studies, surprisingly little is known about accreting pulsars at low-luminosities, yet these may be the most numerous class of neutron star binaries in the Galaxy. Upcoming large-scale surveys will likely reveal many such objects, but to identify them it is crucial to fully understand their properties. X Per, the archetypal source of this class, at 1 kpc from Earth is ideal target for detailed studies. In spite of that X Per is still puzzling. With the proposed program we aim to study X Per in detail, constrain its X-ray spectrum also as a function of the spin phase. Our study will be key to characterize the properties of low-luminosity X-ray pulsars population and will help to identify it in upcoming surveys. | GALACTIC POINT SOURCES | 4 | B | DOROSHENKO | VICTOR | NULL | NULL | EUR | 7 | AO7 | CRACKING THE X PER | XIS | Y |
| EXO 2030+375 | 308.0462 | 37.6555 | 77.15821576 | -1.21997822 | 58.3113 | 56070.8420717593 | 56072.789849537 | 407089010 | 77945.1 | 75000 | 77953.1 | 77956.9 | 0 | 77945.1 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 72515 | 72515 | 168255.8 | 0 | PROCESSED | 57605.5425347222 | 56449 | 56083.2088888889 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 072013 | We propose to observe the Be/X-ray binary system EXO 2030+375 in the ascending part of one of its normal periastron flares for 75ks to study the onset of the pulsar activity. Quasi-periodic hour-long flux oscillations were recently observed during INTEGRAL serendipitous observations and by EXOSAT in 1985. They appear to happen at the viscous time-scale of a disk, evidencing some kind of instability in the transition zone between the magnetosphere and the accretion disk. The broad-band coverage and sensitivity of Suzaku will allow us to investigate in detail the opening of the magnetic gate for this high-magnetic field neutron star by studying the high time resolution light curve, the shape of its pulsed signal and the spectral properties. | GALACTIC POINT SOURCES | 4 | A | FERRIGNO | CARLO | NULL | NULL | EUR | 7 | AO7 | UNVEIL ACCRETION ONSET DURING A NORMAL OUTBURST OF EXO 2030+375 | XIS | Y |
| J1620-4927 | 245.1748 | -49.4572 | 333.89109656 | 0.40900491 | 274.3002 | 56157.8029513889 | 56158.5203356482 | 407091010 | 29260.1 | 25000 | 29260.1 | 29284.1 | 0 | 29260.1 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 29840.2 | 29840.2 | 61967.9 | 0 | PROCESSED | 57606.8716898148 | 56592 | 56226.6098148148 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 072019 | The Large Area Telescope (LAT) on-board the Fermi mission is opening a new window on pulsar astrophysics, by unveiling more than 100 new gamma-ray pulsars, a third of which lacks detection at radio wavelengths despite very deep searches. For these pulsars, X-rays provide a powerful avenue for further high-energy studies. Here we propose 25ks Suzaku observations of the 9 radio-quiet gamma-ray pulsars which have no X-ray counterparts nor deep X-ray observations, in order to better understand this population's X-ray properties and to extract constraints on the crucial unknown distances. | GALACTIC POINT SOURCES | 4 | A | MARELLI | MARTINO | NULL | NULL | EUR | 7 | AO7 | SEARCHING FOR X-RAY COUNTERPARTS OF RADIO-QUIET FERMI PULSARS | XIS | Y |
| J1803-2149 | 270.7914 | -21.8184 | 8.14241987 | 0.18738401 | 269.7005 | 56191.3371643518 | 56192.1730671296 | 407092010 | 31998.6 | 25000 | 32021.8 | 32014.6 | 0 | 31998.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28881.2 | 28881.2 | 72217.9 | 1 | PROCESSED | 57607.1276736111 | 56584 | 56218.5534259259 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 072019 | The Large Area Telescope (LAT) on-board the Fermi mission is opening a new window on pulsar astrophysics, by unveiling more than 100 new gamma-ray pulsars, a third of which lacks detection at radio wavelengths despite very deep searches. For these pulsars, X-rays provide a powerful avenue for further high-energy studies. Here we propose 25ks Suzaku observations of the 9 radio-quiet gamma-ray pulsars which have no X-ray counterparts nor deep X-ray observations, in order to better understand this population's X-ray properties and to extract constraints on the crucial unknown distances. | GALACTIC POINT SOURCES | 4 | A | MARELLI | MARTINO | NULL | NULL | EUR | 7 | AO7 | SEARCHING FOR X-RAY COUNTERPARTS OF RADIO-QUIET FERMI PULSARS | XIS | Y |
| J1746-3239 | 266.7261 | -32.6662 | 356.95543166 | -2.17351712 | 72.0153 | 56365.6469675926 | 56366.4022453704 | 407093010 | 27346.9 | 25000 | 27346.9 | 27346.9 | 0 | 27346.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27005 | 27005 | 65251.9 | 2 | PROCESSED | 57610.8216087963 | 56745 | 56379.530775463 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 072019 | The Large Area Telescope (LAT) on-board the Fermi mission is opening a new window on pulsar astrophysics, by unveiling more than 100 new gamma-ray pulsars, a third of which lacks detection at radio wavelengths despite very deep searches. For these pulsars, X-rays provide a powerful avenue for further high-energy studies. Here we propose 25ks Suzaku observations of the 9 radio-quiet gamma-ray pulsars which have no X-ray counterparts nor deep X-ray observations, in order to better understand this population's X-ray properties and to extract constraints on the crucial unknown distances. | GALACTIC POINT SOURCES | 4 | A | MARELLI | MARTINO | NULL | NULL | EUR | 7 | AO7 | SEARCHING FOR X-RAY COUNTERPARTS OF RADIO-QUIET FERMI PULSARS | XIS | Y |
| J1522-5734 | 230.5286 | -57.5816 | 322.05619938 | -0.4156844 | 274.4971 | 56154.6486342593 | 56155.0078356482 | 407094010 | 30029.5 | 25000 | 30045.5 | 30029.5 | 0 | 30045.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 23686.2 | 23686.2 | 31023.9 | 0 | PROCESSED | 57606.8538194444 | 56638 | 56272.6647222222 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 072019 | The Large Area Telescope (LAT) on-board the Fermi mission is opening a new window on pulsar astrophysics, by unveiling more than 100 new gamma-ray pulsars, a third of which lacks detection at radio wavelengths despite very deep searches. For these pulsars, X-rays provide a powerful avenue for further high-energy studies. Here we propose 25ks Suzaku observations of the 9 radio-quiet gamma-ray pulsars which have no X-ray counterparts nor deep X-ray observations, in order to better understand this population's X-ray properties and to extract constraints on the crucial unknown distances. | GALACTIC POINT SOURCES | 4 | A | MARELLI | MARTINO | NULL | NULL | EUR | 7 | AO7 | SEARCHING FOR X-RAY COUNTERPARTS OF RADIO-QUIET FERMI PULSARS | XIS | Y |
| 1FGL J1018.6-5856 | 154.7461 | -58.9386 | 284.35392298 | -1.67969789 | 308.622 | 56105.7124189815 | 56106.6523611111 | 407096010 | 60432.4 | 60000 | 60432.4 | 60432.4 | 0 | 60432.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 53597.8 | 53597.8 | 81205.9 | 1 | PROCESSED | 57606.5124768518 | 56484 | 56118.0496527778 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 073113 | Recently, a modulated signal has been detected with the Fermi from the source 1FGL J1018.6-5856. The presence of a O-type star in this source, and the variable character of the signal suggested that the source is a new gamma-ray binary system. Since it is expected that X-rays in these sources has the synchrotron origin, detailed X-ray observations are very important for understanding of the processes occurring in the system. However, sensitive observations of source in the X-ray energy bands are still missing. Therefore, we propose to observe the source with Suzaku. Since a long observational campaign is planned for 2012 by the HESS collaboration, the obtained X-ray, together with TeV, data will allow a proper modeling of the physical processes behind the non-thermal emission in system. | GALACTIC POINT SOURCES | 4 | B | ODAKA | HIROKAZU | TANAKA | TAKAAKI | JUS | 7 | AO7 | X-RAY OBSERVATION OF GAMMA-RAY BINARY 1FGL J1018.6-5856 | XIS | Y |
| V4641 SGR | 274.8371 | -25.4052 | 6.77442002 | -4.78571714 | 84.0004 | 56741.9737152778 | 56744.8959722222 | 408002010 | 49223.7 | 100000 | 49223.7 | 49270.6 | 0 | 49224.2 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 89743.9 | 89743.9 | 252455.6 | 1 | PROCESSED | 57614.1632291667 | 57190 | 56821.8685532407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080009 | We propose a 100 ksec Suzaku observation of the Galactic microquasar V4641 Sgr in an outburst. V4641 Sgr has many unique charactersitics: 1)giant X-ray outbursts with fast rise and decay times, 2)violent variability in X-ray and optical bands, and 3)remarkable iron-K disk-line profiles in the X-ray spectrum. However, it is hardly understood due to the poor X-ray coverage which results from its short outburst duration and rapid intensity variations. Hence, we collaborate closely with VSNET, MAXI/GSC, Swift/XRT and Swift/BAT team for a rapid trigger. The moderate energy resolution and wideband energy coverage of Suzaku enable us to clarify the radiation mechanisms of V4641 Sgr. This observation is now planned simultaneously with Swift, many radio and optical/NIR observatories. | GALACTIC POINT SOURCES | 4 | A | YAMAOKA | KAZUTAKA | NULL | NULL | JAP | 8 | AO8-TOO | THE LARGEST-EVER CAMPAIGN OF THE GALACTIC MICROQUASAR V4641 SGR | XIS | Y |
| CRAB PULSAR | 83.6302 | 22.0185 | 184.55261516 | -5.78447613 | 87.4628 | 56551.703599537 | 56552.187650463 | 408008010 | 248.3 | 20000 | 248.3 | 248.3 | 0 | 248.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16312 | 16312 | 41817.9 | 1 | PROCESSED | 57612.6349421296 | 56956 | 56588.603599537 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080026 | We hereby submit a proposal for Suzaku/HXD observations of the Crab pulsar' hard X-ray pulses, which will be coordinated with simultaneous detection of giant radio pulses at ground radio telescopes. With these observations, we will get a statistically significant confirmation (or denial) of the existence of correlation between X-ray intensity and giant radio pulses, which has been found, with a marginal significance, during our trial observations of the Crab pulsar in which we utilized the calibration data of the HXD. If this correlation is confirmed, a new insight into the physics of pulsars' magnetospheres can be obtained. | GALACTIC POINT SOURCES | 4 | C | TERASAWA | TOSHIO | NULL | NULL | JAP | 8 | AO8 | CORRELATION STUDY OF X-RAY PULSES AND GIANT RADIO PULSES FROM CRAB PULSAR WITH SUZAKU/HXD | XIS | Y |
| 4U 0614+091 | 94.2788 | 9.1363 | 200.87717258 | -3.36522944 | 89.7995 | 56579.4227314815 | 56580.8314351852 | 408009010 | 33687 | 60000 | 33687 | 34647.4 | 0 | 34936.6 | 3 | 4 | 0 | 4 | 1 | 0 | 0 | 57701.6 | 57701.6 | 121663.9 | 0 | PROCESSED | 57612.9715393518 | 57144 | 56601.6144791667 | 3.0.22.44 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080028 | We propose an Suzaku observation of LMXB 4U 0614+091 for the study of Neutron Star Binary (NSB) in the low/hard state. An aim of this observation is to reveal a physical model of the NSB low/hard state in a same analogy of Black-Hole Binary (BHB) low/hard state. In the BHB Cyg X-1, the spectra in low/hard state radiate from a cool accretion disk and a hot comptonizing corona. A spectra of NS in low/hard state would have the same structure as Cyg X-1, but it is hard to study the fine structure of the spectra because of low luminosity. Suzaku can determine the low temperature of the disk and the high temperature of the corona, thanks to wide-band and high sensitivity detectors: XIS/BI and HXD. This observation is important for an unified model between BHB and NSB. | GALACTIC POINT SOURCES | 4 | B | SUGITA | SATOSHI | NULL | NULL | JAP | 8 | AO8 | THE SPECTRAL STUDY OF LMXB 4U 0614+091 IN THE LOW/HARD STATE | XIS | Y |
| 4U 0614+091 | 94.2826 | 9.1348 | 200.88027144 | -3.36263018 | 270.7227 | 56737.0982291667 | 56738.4584259259 | 408009020 | 15668.9 | 60000 | 15831.4 | 15668.9 | 0 | 15820.5 | 4 | 3 | 0 | 3 | 1 | 0 | 0 | 60557.4 | 60557.4 | 117501.8 | 2 | PROCESSED | 57614.0787152778 | 57144 | 56778.6809606482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080028 | We propose an Suzaku observation of LMXB 4U 0614+091 for the study of Neutron Star Binary (NSB) in the low/hard state. An aim of this observation is to reveal a physical model of the NSB low/hard state in a same analogy of Black-Hole Binary (BHB) low/hard state. In the BHB Cyg X-1, the spectra in low/hard state radiate from a cool accretion disk and a hot comptonizing corona. A spectra of NS in low/hard state would have the same structure as Cyg X-1, but it is hard to study the fine structure of the spectra because of low luminosity. Suzaku can determine the low temperature of the disk and the high temperature of the corona, thanks to wide-band and high sensitivity detectors: XIS/BI and HXD. This observation is important for an unified model between BHB and NSB. | GALACTIC POINT SOURCES | 4 | B | SUGITA | SATOSHI | NULL | NULL | JAP | 8 | AO8 | THE SPECTRAL STUDY OF LMXB 4U 0614+091 IN THE LOW/HARD STATE | XIS | Y |
| 4U 0142+61 | 26.5838 | 61.7628 | 129.37704782 | -0.4200572 | 82.997 | 56504.4205902778 | 56506.6252430556 | 408011010 | 101167.8 | 100000 | 101167.8 | 101182.8 | 0 | 101182.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 102473.9 | 102473.9 | 190463.7 | 1 | PROCESSED | 57612.1558680556 | 56953 | 56587.5059606482 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080035 | A toroidal magnetic field is thought to be formed in neutron star interior after core-collapse supernovae and become an energy source with recently observed X-ray outbursts from magnetars. Since the toroidal field is hidden in the stellar interior, it was thought to be undetectable via the well-known p-pdot method and the cyclotron resonance scattering features. However, a magnetic stress of the magnetar toroidal field is strong enough to distort the stellar shape and produce a free precession in its X-ray pulse timing if the emission pattern deviates from its axis of symmetry. From our analyses of magnetar 4U 0142+61, we found an evidence on the free precession in the hard X-ray component. To confirm and establish this evidence, we propose an additional 100 ks observation of 4U 0142+61. | GALACTIC POINT SOURCES | 4 | A | ENOTO | TERUAKI | NULL | NULL | JAP | 8 | AO8 | TOROIDAL FIELD INSIDE MAGNETARS OBSERVED WITH SUZAKU TIMING ANALYSES OF ITS FREE PRECESSION | XIS | Y |
| SGR 0501+4516 | 75.2774 | 45.2864 | 161.53821228 | 1.95483036 | 87.7054 | 56535.9761574074 | 56536.8752662037 | 408013010 | 36124.4 | 40000 | 36124.4 | 41261.1 | 0 | 41245.2 | 2 | 2 | 0 | 1 | 1 | 0 | 0 | 35717.7 | 35717.7 | 77671.9 | 1 | PROCESSED | 57612.459375 | 56974 | 56608.6586342593 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080040 | Suzaku legacy of the broadband magnetar observation is 1) ToO observations and monitorings onto activated magnetars, 2) discovery of a sign of spectral evolution correlated with their characteristic age and magnetic field, and 3) challenge to understand the magnetar environment via SNR diagnostics. To accomplish these studies, we propose three magnetar source; 1) SGR 0501+4516 (40 ks) to study the quiescent nature of transients, 2) SGR 1806-20 (70 ks) to verify the evolution, and 3) Swift J1834.9-0846 (40 ks) to accomplish the comprehensive observation of all the magnetar sources. | GALACTIC POINT SOURCES | 4 | B | ENOTO | TERUAKI | NULL | NULL | JAP | 8 | AO8 | ACCOMPLISHMENT OF SUZAKU MAGNETAR STUDY AND VERIFICATION OF ITS LEGACY | XIS | Y |
| SGR 1806-20 | 272.1614 | -20.4072 | 9.99816367 | -0.23801419 | 88.2521 | 57120.8242592593 | 57122.7405324074 | 408014010 | 70819.5 | 70000 | 70819.5 | 74773.9 | 0 | 74816.9 | 2 | 2 | 0 | 3 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57618.0034143518 | 57503 | 57135.3828356482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080040 | Suzaku legacy of the broadband magnetar observation is 1) ToO observations and monitorings onto activated magnetars, 2) discovery of a sign of spectral evolution correlated with their characteristic age and magnetic field, and 3) challenge to understand the magnetar environment via SNR diagnostics. To accomplish these studies, we propose three magnetar source; 1) SGR 0501+4516 (40 ks) to study the quiescent nature of transients, 2) SGR 1806-20 (70 ks) to verify the evolution, and 3) Swift J1834.9-0846 (40 ks) to accomplish the comprehensive observation of all the magnetar sources. | GALACTIC POINT SOURCES | 4 | B | ENOTO | TERUAKI | NULL | NULL | JAP | 8 | AO8 | ACCOMPLISHMENT OF SUZAKU MAGNETAR STUDY AND VERIFICATION OF ITS LEGACY | XIS | Y |
| SWIFT J1834.9-0846 | 278.7285 | -8.7724 | 23.24882887 | -0.35409613 | 264.9986 | 56582.3041319444 | 56583.3335300926 | 408015010 | 35931.7 | 40000 | 38111.7 | 38111.7 | 0 | 35931.7 | 2 | 2 | 0 | 3 | 1 | 0 | 0 | 31926.4 | 31926.4 | 88931.9 | 1 | PROCESSED | 57613.0148726852 | 56967 | 56601.6309953704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080040 | Suzaku legacy of the broadband magnetar observation is 1) ToO observations and monitorings onto activated magnetars, 2) discovery of a sign of spectral evolution correlated with their characteristic age and magnetic field, and 3) challenge to understand the magnetar environment via SNR diagnostics. To accomplish these studies, we propose three magnetar source; 1) SGR 0501+4516 (40 ks) to study the quiescent nature of transients, 2) SGR 1806-20 (70 ks) to verify the evolution, and 3) Swift J1834.9-0846 (40 ks) to accomplish the comprehensive observation of all the magnetar sources. | GALACTIC POINT SOURCES | 4 | B | ENOTO | TERUAKI | NULL | NULL | JAP | 8 | AO8 | ACCOMPLISHMENT OF SUZAKU MAGNETAR STUDY AND VERIFICATION OF ITS LEGACY | XIS | Y |
| SAGITTARIUS A* | 266.4197 | -29.0062 | 359.94692786 | -0.04746309 | 282.0043 | 56539.5310416667 | 56540.000162037 | 408017010 | 19457.9 | 20000 | 19478.9 | 19457.9 | 0 | 19470.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20642.3 | 20642.3 | 40521.9 | 0 | PROCESSED | 57612.4854976852 | 56974 | 56608.6493981482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080074 | With Suzaku, we will carry out the X-ray monitoring of the supermassive blackhole Sgr A*. A small gas cloud, G2, is on an orbit almost straight into Sgr A* by summer 2013. This event gives us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion at the Suzaku first window of 2013 September and a maximum at the 2014 Spring window. We then try five weekly monitoring with a 20 ksec each observation at each window. | GALACTIC POINT SOURCES | 4 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 8 | AO8 | SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE | XIS | Y |
| SAGITTARIUS A* | 266.4166 | -29.0014 | 359.94961276 | -0.04264831 | 285.0058 | 56547.2597337963 | 56547.6558101852 | 408017020 | 19276 | 20000 | 19282.3 | 19290.1 | 0 | 19276 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 21083.4 | 21083.4 | 34218 | 0 | PROCESSED | 57612.6033796296 | 56956 | 56588.7462152778 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080074 | With Suzaku, we will carry out the X-ray monitoring of the supermassive blackhole Sgr A*. A small gas cloud, G2, is on an orbit almost straight into Sgr A* by summer 2013. This event gives us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion at the Suzaku first window of 2013 September and a maximum at the 2014 Spring window. We then try five weekly monitoring with a 20 ksec each observation at each window. | GALACTIC POINT SOURCES | 4 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 8 | AO8 | SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE | XIS | Y |
| SAGITTARIUS A* | 266.4172 | -29.0091 | 359.94331347 | -0.04710749 | 285.0015 | 56554.8566087963 | 56555.4439930556 | 408017030 | 20261.3 | 20000 | 20268 | 20261.3 | 0 | 20268 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20549 | 20549 | 50741.9 | 1 | PROCESSED | 57612.6558217593 | 56956 | 56588.6928935185 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080074 | With Suzaku, we will carry out the X-ray monitoring of the supermassive blackhole Sgr A*. A small gas cloud, G2, is on an orbit almost straight into Sgr A* by summer 2013. This event gives us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion at the Suzaku first window of 2013 September and a maximum at the 2014 Spring window. We then try five weekly monitoring with a 20 ksec each observation at each window. | GALACTIC POINT SOURCES | 4 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 8 | AO8 | SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE | XIS | Y |
| SAGITTARIUS A* | 266.4179 | -29.0156 | 359.938084 | -0.05101613 | 284.9967 | 56561.9008101852 | 56562.4828587963 | 408017040 | 18328.5 | 20000 | 18342.2 | 18328.5 | 0 | 18342.2 | 3 | 2 | 0 | 3 | 1 | 0 | 0 | 18951.9 | 18951.9 | 50282 | 0 | PROCESSED | 57612.7244560185 | 56956 | 56588.4972222222 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080074 | With Suzaku, we will carry out the X-ray monitoring of the supermassive blackhole Sgr A*. A small gas cloud, G2, is on an orbit almost straight into Sgr A* by summer 2013. This event gives us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion at the Suzaku first window of 2013 September and a maximum at the 2014 Spring window. We then try five weekly monitoring with a 20 ksec each observation at each window. | GALACTIC POINT SOURCES | 4 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 8 | AO8 | SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE | XIS | Y |
| SAGITTARIUS A* | 266.4147 | -29.0052 | 359.94550345 | -0.04320951 | 106.9995 | 56723.0565277778 | 56723.5487384259 | 408017050 | 21994.9 | 20000 | 21994.9 | 22002.9 | 0 | 22014.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15862 | 15862 | 42519.9 | 1 | PROCESSED | 57613.9706828704 | 57100 | 56734.6444328704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080074 | With Suzaku, we will carry out the X-ray monitoring of the supermassive blackhole Sgr A*. A small gas cloud, G2, is on an orbit almost straight into Sgr A* by summer 2013. This event gives us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion at the Suzaku first window of 2013 September and a maximum at the 2014 Spring window. We then try five weekly monitoring with a 20 ksec each observation at each window. | GALACTIC POINT SOURCES | 4 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 8 | AO8 | SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE | XIS | Y |
| SAGITTARIUS A* | 266.4146 | -29.0065 | 359.94434823 | -0.0438121 | 107.0001 | 56728.6474537037 | 56729.1147569445 | 408017060 | 21138.7 | 20000 | 21142.7 | 21138.7 | 0 | 21159.5 | 2 | 2 | 0 | 3 | 1 | 0 | 0 | 20484.4 | 20484.4 | 40368 | 0 | PROCESSED | 57614.0078240741 | 57113 | 56747.6540972222 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080074 | With Suzaku, we will carry out the X-ray monitoring of the supermassive blackhole Sgr A*. A small gas cloud, G2, is on an orbit almost straight into Sgr A* by summer 2013. This event gives us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion at the Suzaku first window of 2013 September and a maximum at the 2014 Spring window. We then try five weekly monitoring with a 20 ksec each observation at each window. | GALACTIC POINT SOURCES | 4 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 8 | AO8 | SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE | XIS | Y |
| SAGITTARIUS A* | 266.415 | -29.0052 | 359.94564014 | -0.04343346 | 106.9998 | 56738.4724189815 | 56738.9897685185 | 408017070 | 21588.7 | 20000 | 21618.5 | 21588.7 | 0 | 21644.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19274 | 19274 | 44694 | 0 | PROCESSED | 57614.0833680556 | 57120 | 56750.8212268518 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080074 | With Suzaku, we will carry out the X-ray monitoring of the supermassive blackhole Sgr A*. A small gas cloud, G2, is on an orbit almost straight into Sgr A* by summer 2013. This event gives us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion at the Suzaku first window of 2013 September and a maximum at the 2014 Spring window. We then try five weekly monitoring with a 20 ksec each observation at each window. | GALACTIC POINT SOURCES | 4 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 8 | AO8 | SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE | XIS | Y |
| SAGITTARIUS A* | 266.415 | -29.006 | 359.94495727 | -0.04385023 | 107.0004 | 56744.9007523148 | 56745.6238541667 | 408017080 | 20481.8 | 20000 | 20491.7 | 20503.6 | 0 | 20481.8 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 19749.8 | 19749.8 | 62471.9 | 1 | PROCESSED | 57614.1384837963 | 57121 | 56756.7635185185 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080074 | With Suzaku, we will carry out the X-ray monitoring of the supermassive blackhole Sgr A*. A small gas cloud, G2, is on an orbit almost straight into Sgr A* by summer 2013. This event gives us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion at the Suzaku first window of 2013 September and a maximum at the 2014 Spring window. We then try five weekly monitoring with a 20 ksec each observation at each window. | GALACTIC POINT SOURCES | 4 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 8 | AO8 | SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE | XIS | Y |
| SAGITTARIUS A* | 266.4154 | -29.0072 | 359.94411521 | -0.04477398 | 105.699 | 56752.451400463 | 56752.9848611111 | 408017090 | 22166.8 | 20000 | 22166.8 | 23559.1 | 0 | 23570.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18874.5 | 18874.5 | 46087.8 | 1 | PROCESSED | 57614.1690740741 | 57134 | 56768.7215856482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080074 | With Suzaku, we will carry out the X-ray monitoring of the supermassive blackhole Sgr A*. A small gas cloud, G2, is on an orbit almost straight into Sgr A* by summer 2013. This event gives us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion at the Suzaku first window of 2013 September and a maximum at the 2014 Spring window. We then try five weekly monitoring with a 20 ksec each observation at each window. | GALACTIC POINT SOURCES | 4 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 8 | AO8 | SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE | XIS | Y |
| ETA CARINAE | 161.1825 | -59.711 | 287.57247158 | -0.67238651 | 329.3001 | 56476.1821296296 | 56479.0417361111 | 408018010 | 97524 | 180000 | 97524 | 97524 | 0 | 97524 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 87836.7 | 87836.7 | 247049.7 | 2 | PROCESSED | 57611.768912037 | 56861 | 56492.7286921296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080081 | Eta Carinae is a binary system containing two very massive main sequence stars orbiting with a period of 5.5 years. As reported by Sekiguchi et al. 2009 and Reitberger et al. 2012 based on Suzaku and Fermi data respectively, the system shows intense non-thermal emission extending from 20 keV to 200 GeV. Although detailed mechanism of this non-thermal emission has been clarified yet, it is now obvious that electrons and highly probably protons are accelerated to high energies by the collision of stellar winds. The aim of the present observation is to measure the spectral shape and flux of the non-thermal hard X-ray tail with the HXD, and compare with previous Suzaku observations. Based on a time variability (or non-variability), we examine proposed acceleration and emission mechanisms. | GALACTIC POINT SOURCES | 4 | B | YUASA | TAKAYUKI | NULL | NULL | JAP | 8 | AO8 | DETAILED SPECTROSCOPY OF NON-THERMAL HARD X-RAY EMISSION OF ETA CARINAE | HXD | Y |
| ETA CARINAE | 161.2758 | -59.6779 | 287.59865979 | -0.62113788 | 295.3343 | 56479.0480439815 | 56481.2890509259 | 408018020 | 83968.5 | 180000 | 83968.5 | 83968.5 | 0 | 83968.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 75778.6 | 75778.6 | 193605.8 | 3 | PROCESSED | 57611.7548263889 | 56861 | 56492.6867361111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080081 | Eta Carinae is a binary system containing two very massive main sequence stars orbiting with a period of 5.5 years. As reported by Sekiguchi et al. 2009 and Reitberger et al. 2012 based on Suzaku and Fermi data respectively, the system shows intense non-thermal emission extending from 20 keV to 200 GeV. Although detailed mechanism of this non-thermal emission has been clarified yet, it is now obvious that electrons and highly probably protons are accelerated to high energies by the collision of stellar winds. The aim of the present observation is to measure the spectral shape and flux of the non-thermal hard X-ray tail with the HXD, and compare with previous Suzaku observations. Based on a time variability (or non-variability), we examine proposed acceleration and emission mechanisms. | GALACTIC POINT SOURCES | 4 | B | YUASA | TAKAYUKI | NULL | NULL | JAP | 8 | AO8 | DETAILED SPECTROSCOPY OF NON-THERMAL HARD X-RAY EMISSION OF ETA CARINAE | XIS | Y |
| V1223 SGR | 283.7562 | -31.163 | 4.95737746 | -14.35200731 | 75.0006 | 56745.6297453704 | 56746.5002430556 | 408019010 | 29349.3 | 180000 | 29389.3 | 29349.3 | 0 | 29396.7 | 1 | 1 | 0 | 2 | 1 | 0 | 0 | 26131 | 26131 | 75192 | 1 | PROCESSED | 57614.1428703704 | 57121 | 56756.7522800926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080086 | A 180-ks observation of the magnetic cataclysmic variable V1223 Sgr is proposed. By increasing the statistics by a factor of 4 compared to the existing 45-ks data, we investigate spin-phase dependent redshift of the iron fluorescent line, in particular its line center energy and equivalent width with smaller statistical errors than results of Hayashi et al. 2011. These parameters will provide geometrical configuration, or solid angle viewed from the post-shock region, of the pre-shock cool gas and the white dwarf reflecting surface. We use this information to make our Monte-Carlo simulator of magnetic CV more physically realistic and reliable in analyzing the high-resolution iron line profiles to be obtained with the ASTRO-H/SXS. | GALACTIC POINT SOURCES | 4 | B | YUASA | TAKAYUKI | NULL | NULL | JAP | 8 | AO8 | DEEP OBSERVATION OF THE MAGNETIC CATACLYSMIC VARIABLE V1223 SGR | XIS | Y |
| V1223 SGR | 283.7576 | -31.1629 | 4.95796111 | -14.35306818 | 89.5992 | 56757.9023611111 | 56761.5211111111 | 408019020 | 150768.3 | 60000 | 150776.3 | 150776.3 | 0 | 150768.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 146315.8 | 146315.8 | 312605.7 | 3 | PROCESSED | 57614.3279976852 | 57152 | 56789.7985648148 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080086 | A 180-ks observation of the magnetic cataclysmic variable V1223 Sgr is proposed. By increasing the statistics by a factor of 4 compared to the existing 45-ks data, we investigate spin-phase dependent redshift of the iron fluorescent line, in particular its line center energy and equivalent width with smaller statistical errors than results of Hayashi et al. 2011. These parameters will provide geometrical configuration, or solid angle viewed from the post-shock region, of the pre-shock cool gas and the white dwarf reflecting surface. We use this information to make our Monte-Carlo simulator of magnetic CV more physically realistic and reliable in analyzing the high-resolution iron line profiles to be obtained with the ASTRO-H/SXS. | GALACTIC POINT SOURCES | 4 | B | YUASA | TAKAYUKI | NULL | NULL | JAP | 8 | AO8 | DEEP OBSERVATION OF THE MAGNETIC CATACLYSMIC VARIABLE V1223 SGR | XIS | Y |
| CXO J172641.7-354052 | 261.6769 | -35.6761 | 352.17176486 | -0.26901827 | 279.4529 | 56540.003275463 | 56540.8015509259 | 408021010 | 37316.5 | 40000 | 37331.7 | 37334.9 | 0 | 37316.5 | 2 | 3 | 0 | 2 | 1 | 0 | 0 | 35369.3 | 35369.3 | 68965.9 | 0 | PROCESSED | 57612.5112037037 | 56956 | 56587.7063541667 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080100 | We propose an additional Suzaku observation of an unclassified gamma-ray source detected with the Fermi LAT telescope. In previous cycles, we found an enigmatic source XSS J12270-4859 to be the first gamma-ray binary among the low-mass X-ray binaries. This proposal aims to find a second source of the same nature for the most prospective target extracted from our catalogue search. | GALACTIC POINT SOURCES | 4 | C | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 8 | AO8 | X-RAY SEARCH OF ANOTHER ENIGMATIC SOURCE IN OUR GALAXY | XIS | Y |
| V2301 OPH | 270.1519 | 8.1612 | 34.53664844 | 14.98247082 | 262.0703 | 56573.9878356482 | 56576.0002893518 | 408024010 | 40135.6 | 150000 | 40135.6 | 40135.6 | 0 | 40135.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 65684.3 | 65684.3 | 173858.7 | 1 | PROCESSED | 57612.9068981482 | 57184 | 56596.5744907407 | 3.0.22.44 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080107 | It has been believed that white dwarfs (WDs) undergo a Type I supernova explosion when they reach 1.4 solar masses (Chandrasekhar limit) via mass accretion. However the equation of state (EOS) in the WDs which determines the WD mass limit have not been cleared. Especially, a EOS involving Landau quantization allows WDs to exceed 1.4 solar masses and approach 2.3 solar masses. We will give a observational relation between WD mass and radius with this proposal, and measure the WD mass and radius with binary system parameters estimated by photometries without any theoretical mass-radius relation. When our aim is achieved, the WD mass and radius measurement without any theoretical model is first time for WDs highly magnetized (< 10^5 G) and in CVs, which undergo a Type I supernova explosion. | GALACTIC POINT SOURCES | 4 | A | HAYASHI | TAKAYUKI | NULL | NULL | JAP | 8 | AO8 | MEASUREMENT OF MASS AND RADIUS OF HIGHLY MAGNETIZED WHITE DWARF IN CATACLYSMIC VARIABLE | XIS | Y |
| V2301 OPH | 270.155 | 8.1565 | 34.53366867 | 14.97765204 | 262.0679 | 56576.0003009259 | 56577.3452314815 | 408024020 | 53188.4 | 110000 | 53188.4 | 53188.4 | 0 | 53188.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47289.2 | 47289.2 | 116189.8 | 0 | PROCESSED | 57612.9583333333 | 57184 | 56631.6754282407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080107 | It has been believed that white dwarfs (WDs) undergo a Type I supernova explosion when they reach 1.4 solar masses (Chandrasekhar limit) via mass accretion. However the equation of state (EOS) in the WDs which determines the WD mass limit have not been cleared. Especially, a EOS involving Landau quantization allows WDs to exceed 1.4 solar masses and approach 2.3 solar masses. We will give a observational relation between WD mass and radius with this proposal, and measure the WD mass and radius with binary system parameters estimated by photometries without any theoretical mass-radius relation. When our aim is achieved, the WD mass and radius measurement without any theoretical model is first time for WDs highly magnetized (< 10^5 G) and in CVs, which undergo a Type I supernova explosion. | GALACTIC POINT SOURCES | 4 | A | HAYASHI | TAKAYUKI | NULL | NULL | JAP | 8 | AO8 | MEASUREMENT OF MASS AND RADIUS OF HIGHLY MAGNETIZED WHITE DWARF IN CATACLYSMIC VARIABLE | XIS | Y |
| V2301 OPH | 270.1437 | 8.1764 | 34.54710657 | 14.99643028 | 71.9008 | 56752.9922800926 | 56754.6945949074 | 408024030 | 62925.3 | 57000 | 62941.3 | 62925.3 | 0 | 62941.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 56503.7 | 56503.7 | 147067.7 | 1 | PROCESSED | 57614.2091666667 | 57184 | 56817.8149884259 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080107 | It has been believed that white dwarfs (WDs) undergo a Type I supernova explosion when they reach 1.4 solar masses (Chandrasekhar limit) via mass accretion. However the equation of state (EOS) in the WDs which determines the WD mass limit have not been cleared. Especially, a EOS involving Landau quantization allows WDs to exceed 1.4 solar masses and approach 2.3 solar masses. We will give a observational relation between WD mass and radius with this proposal, and measure the WD mass and radius with binary system parameters estimated by photometries without any theoretical mass-radius relation. When our aim is achieved, the WD mass and radius measurement without any theoretical model is first time for WDs highly magnetized (< 10^5 G) and in CVs, which undergo a Type I supernova explosion. | GALACTIC POINT SOURCES | 4 | A | HAYASHI | TAKAYUKI | NULL | NULL | JAP | 8 | AO8 | MEASUREMENT OF MASS AND RADIUS OF HIGHLY MAGNETIZED WHITE DWARF IN CATACLYSMIC VARIABLE | XIS | Y |
| V1159 ORI | 82.2495 | -3.563 | 206.52568579 | -19.93854352 | 268.4348 | 56732.3915856482 | 56737.0939583333 | 408029010 | 200548.7 | 200000 | 200556.7 | 200548.7 | 0 | 200556.7 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 188992.7 | 188992.7 | 404022.6 | 3 | PROCESSED | 57614.1201967593 | 56383 | 56807.8867708333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081211 | We propose two 200 ks Suzaku observations of the dwarf nova V1159 Ori, chosen as our target because it is a known X-ray source with an extremely short (~4 day) outburst cycle. Each proposed observation will take ~5 calendar days and cover a complete outburst cycle. The dense X-ray coverage of the early rise in particular will be unprecedented for any dwarf nova, which is essential to further our understanding of the response of the boundary layer to the increased mass flux from the Keplerian accretion disk. We will also determine whether X-ray flux increases or decreases during quiescence to test the disk instability model. We will interpret the detailed picture of V1159 Ori in the context of existing, though less complete, X-ray campaigns on several other dwarf novae. | GALACTIC POINT SOURCES | 4 | A | MUKAI | KOJI | NULL | NULL | USA | 8 | AO8 | X-RAY EMISSION THROUGH COMPLETE OUTBURST CYCLES OF THE DWARF NOVA V1159 ORI | XIS | Y |
| SWIFT J2319.4+2619 | 349.8819 | 26.2473 | 98.48369948 | -32.22425134 | 253.9963 | 56633.8796875 | 56634.8786111111 | 408030010 | 41275.8 | 40000 | 41275.8 | 41275.8 | 0 | 41275.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 38149 | 38149 | 86287.9 | 2 | PROCESSED | 57613.5369328704 | 57039 | 56672.6300578704 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081213 | Polars are a subclass of magnetic cataclysmic variables in which a strongly magnetic white dwarf accretes matter from a late-type, Roche-lobe filling mass donor. They are usually soft X-ray bright and hard X-ray dim, due to either buried shocks or strong cyclotron cooling, depending on system parameters. However, a small subset of polars have been detected as bright hard X-ray sources in INTEGRAL and Swift BAT surveys. As a part of an effort to understand the hard-to-soft X-ray luminosity ratios of polars in general, and specifically to understand what combination of parameters make some polars hard X-ray bright, we propose Suzaku observations of two poorly studied BAT polars, Swift J2319.4+2619 and IW Eri, supported by ground-based observations including optical polarimetry. | GALACTIC POINT SOURCES | 4 | C | MUKAI | KOJI | NULL | NULL | USA | 8 | AO8 | THE HARD X-RAY BRIGHT POLARS SWIFT J2319.4+2619 AND IW ERI | XIS | Y |
| CD -28 3719 | 105.2866 | -29.1168 | 240.20191687 | -10.89157366 | 97.0723 | 56577.3593634259 | 56579.416099537 | 408032010 | 14367.9 | 90000 | 14367.9 | 90077.7 | 0 | 90077.7 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 78356.9 | 78356.9 | 177665.9 | 1 | PROCESSED | 57645.4999652778 | 57009 | 56642.7667476852 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081214 | Since they were discovered, it has been almost impossible to directly observe the accretion region in most symbiotic stars, in which a white dwarf (WD) accretes from the wind of a red giant. With the discovery that hard X-ray emission (E > 2 keV) is a common feature of WD symbiotics, that situation has finally changed. We propose to use Suzaku observations of 3 typical symbiotics with hard X-ray emission to test the hypothesis that such emission emanates from an accretion-disk boundary layer. With the proposed observations, we will determine whether the WD's magnetic field is high enough to disrupt the accretion flow, and estimate the WD mass and accretion rate. This work has implications for the study of accretion in wide binaries and symbiotics stars as progenitors of SNIa. | GALACTIC POINT SOURCES | 4 | B | SOKOLOSKI | JENNIFER | NULL | NULL | USA | 8 | AO8 | X-RAYS FROM THE ACCRETION FLOWS IN SYMBIOTIC STARS | XIS | Y |
| SERPENS X-1 | 279.9926 | 5.0265 | 36.11096598 | 4.83541867 | 266.6732 | 56566.4312037037 | 56570.3821759259 | 408033010 | 1760.5 | 250000 | 9505.6 | 34855.3 | 0 | 1760.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 130329.3 | 130329.3 | 341289.9 | 2 | PROCESSED | 57612.9481018518 | 57198 | 56588.8182060185 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081222 | Much recent work has been focused on Fe K emission lines in neutron star low-mass X-ray binaries (LMXBs). Suzaku and XMM observations appear to have revealed asymmetric line profiles characteristic of relativistic effects present at the innermost accretion disk. However, the nature of these lines are still hotly debated, with recent work suggesting that pile-up can artificially broaden lines. In order to address this critical issue, we propose a 250 ks Suzaku observation of the NS LMXB, Ser X-1. The broadband capabilities of Suzaku will allow for a robust model of the continuum either side of the Fe K line, while all CCDs will be operated in fast clocking modes to achieve pile-up free spectra. This Suzaku observation will help settle the nature of broad Fe K emission lines in NS LMXBs. | GALACTIC POINT SOURCES | 4 | B | CACKETT | EDWARD | NULL | NULL | USA | 8 | AO8 | THE NATURE OF BROAD FE KALPHA EMISSION LINES IN NEUTRON STAR LOW-MASS X-RAY BINARIES | XIS | Y |
| SERPENS X-1 | 279.9874 | 5.0445 | 36.12473115 | 4.84817413 | 93.4997 | 56729.1215277778 | 56731.6459606482 | 408033020 | 1215.4 | 120000 | 6566.6 | 24077.2 | 0 | 1215.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 82357.8 | 82357.8 | 218087.9 | 4 | PROCESSED | 57614.078912037 | 57198 | 56747.822037037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081222 | Much recent work has been focused on Fe K emission lines in neutron star low-mass X-ray binaries (LMXBs). Suzaku and XMM observations appear to have revealed asymmetric line profiles characteristic of relativistic effects present at the innermost accretion disk. However, the nature of these lines are still hotly debated, with recent work suggesting that pile-up can artificially broaden lines. In order to address this critical issue, we propose a 250 ks Suzaku observation of the NS LMXB, Ser X-1. The broadband capabilities of Suzaku will allow for a robust model of the continuum either side of the Fe K line, while all CCDs will be operated in fast clocking modes to achieve pile-up free spectra. This Suzaku observation will help settle the nature of broad Fe K emission lines in NS LMXBs. | GALACTIC POINT SOURCES | 4 | B | CACKETT | EDWARD | NULL | NULL | USA | 8 | AO8 | THE NATURE OF BROAD FE KALPHA EMISSION LINES IN NEUTRON STAR LOW-MASS X-RAY BINARIES | XIS | Y |
| SERPENS X-1 | 279.9877 | 5.0424 | 36.12298663 | 4.84695852 | 81.3009 | 56757.3507060185 | 56757.8959259259 | 408033030 | 388 | 25000 | 1807.1 | 6459.5 | 0 | 388 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 23026.6 | 23026.6 | 47097.9 | 0 | PROCESSED | 57614.2331481482 | 57198 | 56821.7352430556 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081222 | Much recent work has been focused on Fe K emission lines in neutron star low-mass X-ray binaries (LMXBs). Suzaku and XMM observations appear to have revealed asymmetric line profiles characteristic of relativistic effects present at the innermost accretion disk. However, the nature of these lines are still hotly debated, with recent work suggesting that pile-up can artificially broaden lines. In order to address this critical issue, we propose a 250 ks Suzaku observation of the NS LMXB, Ser X-1. The broadband capabilities of Suzaku will allow for a robust model of the continuum either side of the Fe K line, while all CCDs will be operated in fast clocking modes to achieve pile-up free spectra. This Suzaku observation will help settle the nature of broad Fe K emission lines in NS LMXBs. | GALACTIC POINT SOURCES | 4 | B | CACKETT | EDWARD | NULL | NULL | USA | 8 | AO8 | THE NATURE OF BROAD FE KALPHA EMISSION LINES IN NEUTRON STAR LOW-MASS X-RAY BINARIES | XIS | Y |
| GX 339-4 | 255.7085 | -48.7866 | 338.94274721 | -4.32598042 | 275.4008 | 56526.5726967593 | 56529.3592476852 | 408034010 | 101019.6 | 100000 | 101019.6 | 101019.6 | 0 | 101019.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 90316.9 | 90316.9 | 240709.7 | 1 | PROCESSED | 57612.5083680556 | 56956 | 56588.9590046296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081242 | Due to the presence of a steady jet, constraining the properties of black hole systems in their hard state is important for understanding accretion disks and jets. Along with radio observations, Suzaku is constraining theoretical models by answering the following questions: Does the inner edge of the accretion disk recede in the hard state? How is the location of the disk's inner edge related to the presence of a jet? This proposal includes the use of Suzaku, NuSTAR, and radio observations to address these questions. A main diagnostic of the accretion geometry is the Compton reflection component, and the combination of Suzaku and NuSTAR covers, with very good energy resolution and sensitivity, the iron emission line, the absorption edges, and the hard X-ray reflection bump. | GALACTIC POINT SOURCES | 4 | A | TOMSICK | JOHN | NULL | NULL | USA | 8 | AO8-TOO | CONSTRAINING THE HARD STATE ACCRETION GEOMETRY FOR BLACK HOLE BINARIES | XIS | Y |
| FS AURIGAE | 86.945 | 28.5962 | 180.53629966 | 0.22811281 | 90.5955 | 56541.1879050926 | 56542.802974537 | 408041010 | 62184.2 | 62000 | 62184.2 | 62184.2 | 0 | 62184.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 61028.7 | 61028.7 | 139515.8 | 0 | PROCESSED | 57612.5675810185 | 56981 | 56616.7165046296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 082012 | FS Aur represents one of the most unusual cataclysmic variable to have ever been observed. It is famous for a variety of uncommon and puzzling periodic photometric and spectroscopic variabilities. Tovmassian, Zharikov & Neustroev (2007) proposed that the precession of a fast-rotating magnetically accreting white dwarf can successfully explain these phenomena. We request 62 ks observations of FS Aur to detect the magnetic WD, determine its spin period, confirm the flux and spectral variability with the precession period, inconclusively detected by Chandra and Swift, and thus to check the proposed model. The theory of compact objects predicts certain relations between the spin and precession periods, and our findings will provide a good test for the theory. | GALACTIC POINT SOURCES | 4 | B | NEUSTROEV | VITALY | NULL | NULL | EUR | 8 | AO8 | PROBING THE PRECESSION OF WHITE DWARF IN CLOSE BINARY SYSTEMS - FS AURIGAE | XIS | Y |
| 4U 1735-44 | 264.7467 | -44.4484 | 346.05710105 | -6.99533469 | 268.9985 | 56917.7849884259 | 56918.9988194444 | 408043020 | 10177.2 | 60000 | 10177.2 | 10201.6 | 0 | 10304.7 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.5500925926 | 57626 | 56940.6296064815 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 082017 | We propose to observe the bursting low-mass X-ray binary 4U 1735-44 with Suzaku for a total exposure time of 60 ks. We plan to investigate the broad-band X-ray spectrum by performing a detailed spectroscopic and timing analysis in the energy range 0.4-100 keV. The main scientific aims of this observation are to detect and study the iron Kalpha line at 6.4-7 keV, simultaneously with the expected iron edge at 7-9 keV, emission lines at lower energy (such as S, Ar and Ca at 2.62 keV, 3.31 keV and 3.90 keV, respectively), and either a Compton reflection hump at 20-40 keV or a hard tail at energy above 25 keV (depending of the state of the source), thanks to the broad-band capabilities of Suzaku. This will allow to infer and probe the origin of these components, which is still debated. | GALACTIC POINT SOURCES | 4 | A | EGRON | ELISE | NULL | NULL | EUR | 8 | AO8 | BROAD-BAND SPECTRAL ANALYSIS AND STUDY OF THE DISK REFLECTION COMPONENT IN 4U 1735-44 WITH SUZAKU | XIS | Y |
| 4U 1735-44 | 264.7398 | -44.4536 | 346.05003995 | -6.99385769 | 96.4379 | 57098.6918402778 | 57099.2717824074 | 408043030 | 4366.5 | 20000 | 4366.5 | 4915.9 | 0 | 4967 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.8209027778 | 57479 | 57112.402662037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 082017 | We propose to observe the bursting low-mass X-ray binary 4U 1735-44 with Suzaku for a total exposure time of 60 ks. We plan to investigate the broad-band X-ray spectrum by performing a detailed spectroscopic and timing analysis in the energy range 0.4-100 keV. The main scientific aims of this observation are to detect and study the iron Kalpha line at 6.4-7 keV, simultaneously with the expected iron edge at 7-9 keV, emission lines at lower energy (such as S, Ar and Ca at 2.62 keV, 3.31 keV and 3.90 keV, respectively), and either a Compton reflection hump at 20-40 keV or a hard tail at energy above 25 keV (depending of the state of the source), thanks to the broad-band capabilities of Suzaku. This will allow to infer and probe the origin of these components, which is still debated. | GALACTIC POINT SOURCES | 4 | A | EGRON | ELISE | NULL | NULL | EUR | 8 | AO8 | BROAD-BAND SPECTRAL ANALYSIS AND STUDY OF THE DISK REFLECTION COMPONENT IN 4U 1735-44 WITH SUZAKU | XIS | Y |
| GRO J1008-57 | 152.4313 | -58.2999 | 282.99773034 | -1.83149103 | 115.5012 | 56660.6548148148 | 56661.5897569444 | 408044010 | 15337.4 | 20000 | 15337.4 | 15347.9 | 0 | 15337.4 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 22179.4 | 22179.4 | 55037.9 | 1 | PROCESSED | 57613.7393981482 | 57040 | 56679.7652662037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 082019 | We propose to observe the transient XRB GRO J1008−57 for 20 ks during an outburst in 2014 January after the currently ongoing giant outburst. The source exhibits regular outbursts once per orbit. Several of these outbursts have been observed in the past showing that the spectral shape remains constant between outbursts. Since we were able to improve the orbital ephemeris it is possible to predict future outbursts of the source. The source is currently (MJD 56245) exhibiting a giant type II outburst showing that the companion has ejected large amounts of material. We therefore propose to observe the system after this outburst to check for spectral and temporal changes and to study the iron line complex to derive the amount and ionization state of the material. | GALACTIC POINT SOURCES | 4 | A | KREYKENBOHM | INGO | NULL | NULL | EUR | 8 | AO8 | MEASURING THE RESIDUAL MATERIAL IN GRO J1008−57 AFTER THE GIANT OUTBURST | XIS | Y |
| X 1630-472 | 248.5014 | -47.3935 | 336.90846442 | 0.25253242 | 88.6317 | 57073.2374884259 | 57074.4111805556 | 409007010 | 6152.8 | 40000 | 6165 | 6182.3 | 0 | 6152.8 | 3 | 3 | 0 | 3 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.6570023148 | 57454 | 57087.4573032407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090015 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 9 | AO9-TOO | MULTIWAVELENGTH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | XIS | Y |
| X 1630-472 | 248.5012 | -47.3939 | 336.90807869 | 0.25236055 | 88.6321 | 57077.0625578704 | 57078.1140277778 | 409007020 | 5529.6 | 40000 | 5547 | 5565.9 | 0 | 5529.6 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.6879282407 | 57454 | 57087.4605208333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090015 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 9 | AO9-TOO | MULTIWAVELENGTH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | XIS | Y |
| X 1630-472 | 248.5011 | -47.3955 | 336.90685721 | 0.25132488 | 88.6334 | 57080.103125 | 57081.1542824074 | 409007030 | 5110.8 | 40000 | 5128 | 5145.2 | 0 | 5110.8 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.7393634259 | 57458 | 57091.4579513889 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090015 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 9 | AO9-TOO | MULTIWAVELENGTH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | XIS | Y |
| H1743-322 | 266.2607 | -32.2285 | 357.12541364 | -1.6105206 | 285.4288 | 56932.6365625 | 56933.284837963 | 409008010 | 15009.4 | 40000 | 15601.2 | 15616.9 | 0 | 15009.4 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.6096527778 | 57345 | 56979.4022569444 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090015 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 9 | AO9-TOO | MULTIWAVELENGTH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | XIS | Y |
| H1743-322 | 266.5672 | -32.2343 | 357.25542532 | -1.83494451 | 273.3773 | 56939.7339236111 | 56940.5245138889 | 409008020 | 19000.6 | 40000 | 19000.6 | 19014.5 | 0 | 19011.5 | 3 | 3 | 0 | 3 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.6317824074 | 57345 | 56979.407974537 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090015 | Growing evidence indicates that a relativistic jet from a black hole is produced during its transition from the "hard state" to the "soft state" through the "very high state". We propose to make TOO observations of a Galactic black hole binary in the early phase of ourburst with Suzaku in order to reveal the evolution of the accretion disk structure during ejection events. We will trigger a TOO observation upon MAXI. At the same time we organize multiwavelength observations in radio and infrared/optical bands to examine the exact relation between the ejection and state transition. | GALACTIC POINT SOURCES | 4 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 9 | AO9-TOO | MULTIWAVELENGTH OBSERVATIONS OF A GALACTIC BLACK HOLE IN EARLY PHASE OF OUTBURST | XIS | Y |
| SAGITTARIUS A* | 266.4193 | -29.0102 | 359.94333122 | -0.04924818 | 267.3027 | 56929.1441550926 | 56929.6668402778 | 409011010 | 20218.3 | 20000 | 20218.3 | 20330.3 | 0 | 20354.3 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.5861226852 | 56748 | 56979.4039814815 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090048 | With Suzaku, we will carry out the Suzaku monitoring of the supermassive blackhole Sgr A*. A small gas cloud, G2, is on an orbit almost straight into Sgr A* by spring 2014. This event give us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion in early 2014 and a maximum during the AO9 window. We then try five weekly monitoring with a 20 ksec each observation at each window. | GALACTIC POINT SOURCES | 4 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 9 | AO9 | SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE | XIS | Y |
| SAGITTARIUS A* | 266.4217 | -29.0078 | 359.94647323 | -0.04978962 | 278.8011 | 56938.0879861111 | 56938.4619097222 | 409011020 | 17260.5 | 20000 | 17260.5 | 17260.5 | 0 | 17260.5 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.6209606482 | 56748 | 56979.4091087963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090048 | With Suzaku, we will carry out the Suzaku monitoring of the supermassive blackhole Sgr A*. A small gas cloud, G2, is on an orbit almost straight into Sgr A* by spring 2014. This event give us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion in early 2014 and a maximum during the AO9 window. We then try five weekly monitoring with a 20 ksec each observation at each window. | GALACTIC POINT SOURCES | 4 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 9 | AO9 | SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE | XIS | Y |
| SAGITTARIUS A* | 266.415 | -29.0097 | 359.94179901 | -0.04577777 | 105.7704 | 57095.3193171296 | 57096.4952777778 | 409011030 | 25549.6 | 20000 | 25549.6 | 47355.1 | 0 | 47352.2 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.7910763889 | 56748 | 57111.394525463 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090048 | With Suzaku, we will carry out the Suzaku monitoring of the supermassive blackhole Sgr A*. A small gas cloud, G2, is on an orbit almost straight into Sgr A* by spring 2014. This event give us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion in early 2014 and a maximum during the AO9 window. We then try five weekly monitoring with a 20 ksec each observation at each window. | GALACTIC POINT SOURCES | 4 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 9 | AO9 | SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE | XIS | Y |
| SAGITTARIUS A* | 266.415 | -29.0091 | 359.94231116 | -0.0454652 | 105.8502 | 57103.3174537037 | 57103.7690162037 | 409011040 | 23242.2 | 20000 | 23242.2 | 23246.5 | 0 | 23246.5 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.8342824074 | 56748 | 57114.6078472222 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090048 | With Suzaku, we will carry out the Suzaku monitoring of the supermassive blackhole Sgr A*. A small gas cloud, G2, is on an orbit almost straight into Sgr A* by spring 2014. This event give us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion in early 2014 and a maximum during the AO9 window. We then try five weekly monitoring with a 20 ksec each observation at each window. | GALACTIC POINT SOURCES | 4 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 9 | AO9 | SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE | XIS | Y |
| SAGITTARIUS A* | 266.4146 | -29.0061 | 359.94468967 | -0.04360372 | 105.8159 | 57113.0215162037 | 57113.6827662037 | 409011050 | 28670.6 | 20000 | 28670.6 | 28670.6 | 0 | 28686.6 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.891712963 | 56748 | 57125.4008796296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090048 | With Suzaku, we will carry out the Suzaku monitoring of the supermassive blackhole Sgr A*. A small gas cloud, G2, is on an orbit almost straight into Sgr A* by spring 2014. This event give us a rare opportunity to test the mass feeding onto the blackhole by a gas. A theoretical calculation predicts a fast rise of the mass accretion in early 2014 and a maximum during the AO9 window. We then try five weekly monitoring with a 20 ksec each observation at each window. | GALACTIC POINT SOURCES | 4 | A | MAEDA | YOSHITOMO | NULL | NULL | JAP | 9 | AO9 | SUZAKU MONITORING OF SGR A* GIGIANTIC FLARE | XIS | Y |
| 1RXSJ171405.2-202747 | 258.5195 | -20.4586 | 3.21945841 | 10.61986264 | 93.18 | 57079.8384027778 | 57080.0974652778 | 409012010 | 10977.7 | 10000 | 10977.7 | 11001.7 | 0 | 10993.7 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.6641319444 | 57458 | 57091.4587847222 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090051 | We propose to study wide-band X-ray properties of 6 unidentified sources with luminosities of ~10^35 erg/s. These sources are a part of the first complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge, that is constructed from the detected sources in the ROSAT All Sky Survey (Mori 2005, PhD. thesis). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with follow-up optical identifications. This is a new step toward understanding the formation history of the bulge, and hence that of galaxies with various Hubble sequences in the universe. | GALACTIC POINT SOURCES | 4 | B | MORI | HIDEYUKI | NULL | NULL | JAP | 9 | AO9 | SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE | XIS | Y |
| 1RXSJ182853.8-241746 | 277.2212 | -24.2932 | 8.76671438 | -6.19414371 | 87.3419 | 57120.5005092593 | 57120.8217476852 | 409013010 | 9707.2 | 12000 | 9707.2 | 11842.2 | 0 | 11850.2 | 3 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.9447453704 | 57496 | 57129.4074189815 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090051 | We propose to study wide-band X-ray properties of 6 unidentified sources with luminosities of ~10^35 erg/s. These sources are a part of the first complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge, that is constructed from the detected sources in the ROSAT All Sky Survey (Mori 2005, PhD. thesis). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with follow-up optical identifications. This is a new step toward understanding the formation history of the bulge, and hence that of galaxies with various Hubble sequences in the universe. | GALACTIC POINT SOURCES | 4 | B | MORI | HIDEYUKI | NULL | NULL | JAP | 9 | AO9 | SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE | XIS | Y |
| 1RXSJ165739.1-294946 | 254.4116 | -29.828 | 353.32761408 | 8.10480043 | 98.1097 | 57103.7733333333 | 57104.2294328704 | 409014010 | 17225.5 | 12000 | 17225.5 | 17257.5 | 0 | 17233.5 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.8394212963 | 57486 | 57119.4211458333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090051 | We propose to study wide-band X-ray properties of 6 unidentified sources with luminosities of ~10^35 erg/s. These sources are a part of the first complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge, that is constructed from the detected sources in the ROSAT All Sky Survey (Mori 2005, PhD. thesis). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with follow-up optical identifications. This is a new step toward understanding the formation history of the bulge, and hence that of galaxies with various Hubble sequences in the universe. | GALACTIC POINT SOURCES | 4 | B | MORI | HIDEYUKI | NULL | NULL | JAP | 9 | AO9 | SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE | XIS | Y |
| 1RXSJ173916.2-214746 | 264.8155 | -21.7912 | 5.33311568 | 4.97377326 | 96.7097 | 57115.0060069444 | 57115.2681712963 | 409015010 | 12328 | 12000 | 12349 | 12352.3 | 0 | 12328 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.8972800926 | 57493 | 57126.415625 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090051 | We propose to study wide-band X-ray properties of 6 unidentified sources with luminosities of ~10^35 erg/s. These sources are a part of the first complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge, that is constructed from the detected sources in the ROSAT All Sky Survey (Mori 2005, PhD. thesis). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with follow-up optical identifications. This is a new step toward understanding the formation history of the bulge, and hence that of galaxies with various Hubble sequences in the universe. | GALACTIC POINT SOURCES | 4 | B | MORI | HIDEYUKI | NULL | NULL | JAP | 9 | AO9 | SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE | XIS | Y |
| 1RXSJ170856.9-235936 | 257.2347 | -23.9931 | 359.58527393 | 9.56844908 | 95.2085 | 57099.2765625 | 57099.6030324074 | 409016010 | 15376.8 | 15000 | 15376.8 | 15384.8 | 0 | 15376.8 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.8053703704 | 57479 | 57112.4072106482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090051 | We propose to study wide-band X-ray properties of 6 unidentified sources with luminosities of ~10^35 erg/s. These sources are a part of the first complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge, that is constructed from the detected sources in the ROSAT All Sky Survey (Mori 2005, PhD. thesis). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with follow-up optical identifications. This is a new step toward understanding the formation history of the bulge, and hence that of galaxies with various Hubble sequences in the universe. | GALACTIC POINT SOURCES | 4 | B | MORI | HIDEYUKI | NULL | NULL | JAP | 9 | AO9 | SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE | XIS | Y |
| 1RXSJ174559.6-370055 | 266.4961 | -37.0139 | 353.13065719 | -4.26083799 | 95.2535 | 57115.2722106482 | 57115.6653240741 | 409017010 | 14247.3 | 15000 | 14247.3 | 14247.3 | 0 | 14263.3 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.9002777778 | 57493 | 57126.4170949074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090051 | We propose to study wide-band X-ray properties of 6 unidentified sources with luminosities of ~10^35 erg/s. These sources are a part of the first complete X-ray sample in the luminosity range > 10^34 erg/s in the Galactic bulge, that is constructed from the detected sources in the ROSAT All Sky Survey (Mori 2005, PhD. thesis). Our goal is to obtain, for the first time, a clear picture about X-ray populations in the bulge, by utilizing the fine Suzaku spectra together with follow-up optical identifications. This is a new step toward understanding the formation history of the bulge, and hence that of galaxies with various Hubble sequences in the universe. | GALACTIC POINT SOURCES | 4 | B | MORI | HIDEYUKI | NULL | NULL | JAP | 9 | AO9 | SPECTRAL STUDIES OF UNIDENTIFIED X-RAY SOURCES IN THE GALACTIC BULGE | XIS | Y |
| GK PER | 52.7957 | 43.9123 | 150.94865814 | -10.09942696 | 88.9617 | 56876.7092708333 | 56879.871712963 | 409018010 | 109761.2 | 140000 | 109761.2 | 114424.2 | 0 | 114472.2 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.4851157407 | 57468 | 56902.7320023148 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090055 | A 140-ks observation of the magnetic cataclysmic variable GK Per is proposed. By fitting Suzaku broadband spectra using our multitemperature spectral model of the accretion column, we estimate a white dwarf mass with statistical fitting errors smaller than 5%. The estimated mass will be compared with one obtained from the optical lightcurve fitting method developed and applied by Hachisu and Kato in a series of papers. GK Per is the only known magnetic cataclysmic variable which underwent classical nova explosion (in 1901), and both the mass estimation methods can be applied. Cross-validated WD mass estimation methods will be of importance in studying massive white dwarfs in accretion systems, in relation with the progenitor of type Ia supernovae. | GALACTIC POINT SOURCES | 4 | A | YUASA | TAKAYUKI | NULL | NULL | JAP | 9 | AO9 | CROSS VALIDATION OF WHITE DWARF MASS ESTIMATION METHODS | XIS | Y |
| GK PER | 52.8052 | 43.8974 | 150.96310366 | -10.10758836 | 250.0842 | 57086.777037037 | 57090.7709606482 | 409018020 | 182886 | 140000 | 0 | 0 | 0 | 182886 | 0 | 0 | 0 | 2 | 1 | 0 | 0 | 134916.6 | 134916.6 | 344937.6 | 0 | PROCESSED | 57617.786712963 | 57468 | 57101.0913657407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090055 | A 140-ks observation of the magnetic cataclysmic variable GK Per is proposed. By fitting Suzaku broadband spectra using our multitemperature spectral model of the accretion column, we estimate a white dwarf mass with statistical fitting errors smaller than 5%. The estimated mass will be compared with one obtained from the optical lightcurve fitting method developed and applied by Hachisu and Kato in a series of papers. GK Per is the only known magnetic cataclysmic variable which underwent classical nova explosion (in 1901), and both the mass estimation methods can be applied. Cross-validated WD mass estimation methods will be of importance in studying massive white dwarfs in accretion systems, in relation with the progenitor of type Ia supernovae. | GALACTIC POINT SOURCES | 4 | A | YUASA | TAKAYUKI | NULL | NULL | JAP | 9 | AO9 | CROSS VALIDATION OF WHITE DWARF MASS ESTIMATION METHODS | XIS | Y |
| HD45314 | 96.8131 | 14.89 | 196.95740391 | 1.52274638 | 93.5296 | 56935.6339814815 | 56937.7981134259 | 409019010 | 82079.9 | 80000 | 82087.9 | 82087.9 | 0 | 82079.9 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.6300115741 | 57355 | 56989.5080208333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090079 | We propose a Suzaku observation of a newly-found Gamma Cas analogue HD45314. The Gamma Cas analogues constitute a small but distinctive group showing anomalously hard X-ray spectra. We propose a Suzaku observation of HD45314 and compare it with the XMM data taken previously (Rauw et al. 2013) to reveal an expected change in the X-ray spectra. This will give us a clue to understand the X-ray production mechanism of this source and the gamma Cas analogues. | GALACTIC POINT SOURCES | 4 | B | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 9 | AO9 | INVESTIGATION OF A GAMMA CAS ANALOGUES USING SUZAKU | XIS | Y |
| XTE J1855-206 | 283.8765 | -2.601 | 31.07954127 | -2.09022498 | 75.074 | 57134.7127199074 | 57137.3453125 | 409022010 | 87725 | 90000 | 87725 | 89327.4 | 0 | 89319.4 | 3 | 3 | 0 | 3 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57618.1026157407 | 57593 | 57224.4343171296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090101 | Most of High mass X-ray binaries (HMXBs) have strong magnetic fields (~10^12 G) and detected cyclotron resonance scattering features (CRSFs). Many HMXBs with CRSFs have been observed by Suzaku and we derived a new method for estimating magnetic field strength using the observational data. In this observation, we try to observe candidates of strongly magnetized neutron star in HMXBs, EXO 1722-363 and XTE J1855-206 and examine the method. | GALACTIC POINT SOURCES | 4 | C | SASANO | MAKOTO | NULL | NULL | JAP | 9 | AO9 | EXAMINATION OF A NEW METHOD FOR ESTIMATING MAGNETIC FIELD STRENGTH WITH SUZAKU | XIS | Y |
| 1E1724-3045 | 261.8859 | -30.8016 | 356.31902476 | 2.29998715 | 95.7568 | 57113.6866087963 | 57115.0028935185 | 409024010 | 60231.5 | 60000 | 60231.5 | 60251.5 | 0 | 60233.7 | 3 | 3 | 0 | 3 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.9445833333 | 57493 | 57126.4247106482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090106 | Low Mass X-ray Binaries(LMXBs) have soft and hard state. After breakthrough of hard state accretion geometry in LMXBs Sakurai et al.2012,2013), we found a clue to connect hard/soft states. first, we found that the geometry of GS1826-238 is similar to that of soft state, and is understood in the framework of Sakurai et al. (2012,2013). Second, we found a surprising relation between two physical quantities of corona, which roughly shows a continuous change of relation between soft/hard states in contrast with a dramatic change of their spectra. In order to confirm such a continuous relation between two distinct states, we propose a LMXB, which usually shows hard state with high luminosity. | GALACTIC POINT SOURCES | 4 | B | ONO | KO | NULL | NULL | JAP | 9 | AO9 | TOWARD COMPREHENSIVE UNDERSTANDING OF LMXBS ~OBSERVATION OF HARD STATE WITH SUZAKU | XIS | Y |
| SCO X-1 | 245.0164 | -15.3926 | 359.32713596 | 23.91560488 | 98.4296 | 57090.7847685185 | 57093.0903703704 | 409025010 | 84708.6 | 50000 | 0 | 0 | 0 | 84708.6 | 0 | 0 | 0 | 1 | 1 | 0 | 0 | 35377.2 | 35377.2 | 194569.9 | 0 | PROCESSED | 57617.8306365741 | 57481 | 57115.4052777778 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090108 | We propose 50 ks observation of the bright LMXB Sco X-1 (Z source) to search high energy emission above 50 keV and study Fe-K emission/absorption lines. With the combination of XIS and HXD, these properties can be studied with identifying the state of the source. Since Sco X-1 is so bright, the pointing is offset by ~15 arcmin from XIS nominal position. | GALACTIC POINT SOURCES | 4 | A | TAKAHASHI | HIROMITSU | NULL | NULL | JAP | 9 | AO9 | SUZAKU OBSERVATION OF THE BRIGHTEST LMXB SCO X-1 | XIS | Y |
| ETA CARINAE | 161.2798 | -59.6805 | 287.60165846 | -0.62249687 | 316.5996 | 56857.6091435185 | 56859.2363425926 | 409026010 | 53266.5 | 45000 | 53266.5 | 56732.5 | 0 | 56748.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28986.6 | 28986.6 | 138173.7 | 0 | PROCESSED | 57615.4364814815 | 57264 | 56898.3302777778 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091202 | Eta Carinae is an extremely massive binary system whose strong winds produce a variety of high-energy X-ray and possibly gamma-ray emission. Earlier XMM-Newton, Suzaku and INTEGRAL observations found interesting features in the extremely hard X-ray band: i) a flat spectral component above 9 keV toward the flux maximum; ii) strong 15-20 keV emission during an occultation of the wind-wind colliding plasma; iii) stable power-law emission above 25 keV. These features are signs of the highest energy processes yet detected in any colliding wind binary. Broad band X-ray observations around periastron are essential to understanding those features. We therefore propose Suzaku observations at 5 key phases around the next periastron passage of eta Carinae in 2014.6. | GALACTIC POINT SOURCES | 4 | A | HAMAGUCHI | KENJI | NULL | NULL | USA | 9 | AO9 | PROBING THE HIGHEST ENERGY PHENOMENA OF ETA CARINAE AROUND PERIASTRON IN 2014 | XIS | Y |
| ETA CARINAE | 161.2819 | -59.6866 | 287.60543966 | -0.62739972 | 356.4874 | 56894.0150810185 | 56894.6884375 | 409027010 | 34509.8 | 30000 | 34509.8 | 34525.6 | 0 | 34525.8 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.5156712963 | 57285 | 56910.6449884259 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091202 | Eta Carinae is an extremely massive binary system whose strong winds produce a variety of high-energy X-ray and possibly gamma-ray emission. Earlier XMM-Newton, Suzaku and INTEGRAL observations found interesting features in the extremely hard X-ray band: i) a flat spectral component above 9 keV toward the flux maximum; ii) strong 15-20 keV emission during an occultation of the wind-wind colliding plasma; iii) stable power-law emission above 25 keV. These features are signs of the highest energy processes yet detected in any colliding wind binary. Broad band X-ray observations around periastron are essential to understanding those features. We therefore propose Suzaku observations at 5 key phases around the next periastron passage of eta Carinae in 2014.6. | GALACTIC POINT SOURCES | 4 | A | HAMAGUCHI | KENJI | NULL | NULL | USA | 9 | AO9 | PROBING THE HIGHEST ENERGY PHENOMENA OF ETA CARINAE AROUND PERIASTRON IN 2014 | XIS | Y |
| ETA CARINAE | 161.2814 | -59.6826 | 287.60335194 | -0.62397837 | 335.8837 | 56875.8359259259 | 56876.6961111111 | 409028010 | 21545.5 | 30000 | 21545.5 | 21545.5 | 0 | 21545.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 9958.2 | 9958.2 | 22028 | 0 | PROCESSED | 57616.4668518518 | 57264 | 56898.441875 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091202 | Eta Carinae is an extremely massive binary system whose strong winds produce a variety of high-energy X-ray and possibly gamma-ray emission. Earlier XMM-Newton, Suzaku and INTEGRAL observations found interesting features in the extremely hard X-ray band: i) a flat spectral component above 9 keV toward the flux maximum; ii) strong 15-20 keV emission during an occultation of the wind-wind colliding plasma; iii) stable power-law emission above 25 keV. These features are signs of the highest energy processes yet detected in any colliding wind binary. Broad band X-ray observations around periastron are essential to understanding those features. We therefore propose Suzaku observations at 5 key phases around the next periastron passage of eta Carinae in 2014.6. | GALACTIC POINT SOURCES | 4 | A | HAMAGUCHI | KENJI | NULL | NULL | USA | 9 | AO9 | PROBING THE HIGHEST ENERGY PHENOMENA OF ETA CARINAE AROUND PERIASTRON IN 2014 | XIS | Y |
| 1RXS J032540.0-08144 | 51.413 | -8.2453 | 192.86854593 | -48.95490782 | 66.7974 | 56869.0655208333 | 56869.9960532407 | 409029010 | 39540.8 | 40000 | 39540.8 | 39916.8 | 0 | 39924.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18928.9 | 18928.9 | 53612 | 0 | PROCESSED | 57616.4538425926 | 57264 | 56898.3797453704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091211 | Cataclysmic variables (CVs) detected in the INTEGRAL and Swift BAT hard X-ray surveys are predominantly magnetic systems of the intermediate polar subtype. However, as the survey sensitivity improves, an increasing number of polars are also detected as hard X-ray sources, even though the majority of polars are soft X-ray bright and hard X-ray faint. Over the long term, we hope to understand why most polars are soft X-ray dominated, and why a subset is hard X-ray bright. Here we propose Suzaku observations of four poorly studied BAT-detected polars, 1RXS J032540.0-081442, Swift J2319.4+2619, IW Eri, and IGR J14536-5522, supported by ground-based observations including optical polarimetry, to determine their system parameters. | GALACTIC POINT SOURCES | 4 | A | MUKAI | KOJI | NULL | NULL | USA | 9 | AO9 | HARD X-RAY BRIGHT POLARS: WHY ARE THEY DIFFERENT? | XIS | Y |
| IW ERIDANI | 66.4802 | -19.763 | 216.43667954 | -40.61449502 | 63.2719 | 56870.0005092593 | 56870.9730902778 | 409030010 | 39458.1 | 40000 | 39458.1 | 39802.1 | 0 | 39834.1 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.4481134259 | 57270 | 56902.7186574074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091211 | Cataclysmic variables (CVs) detected in the INTEGRAL and Swift BAT hard X-ray surveys are predominantly magnetic systems of the intermediate polar subtype. However, as the survey sensitivity improves, an increasing number of polars are also detected as hard X-ray sources, even though the majority of polars are soft X-ray bright and hard X-ray faint. Over the long term, we hope to understand why most polars are soft X-ray dominated, and why a subset is hard X-ray bright. Here we propose Suzaku observations of four poorly studied BAT-detected polars, 1RXS J032540.0-081442, Swift J2319.4+2619, IW Eri, and IGR J14536-5522, supported by ground-based observations including optical polarimetry, to determine their system parameters. | GALACTIC POINT SOURCES | 4 | A | MUKAI | KOJI | NULL | NULL | USA | 9 | AO9 | HARD X-RAY BRIGHT POLARS: WHY ARE THEY DIFFERENT? | XIS | Y |
| IGR J14536-5522 | 223.4257 | -55.3573 | 319.76650903 | 3.46705373 | 279.1547 | 56870.9840277778 | 56872.0398263889 | 409031010 | 38882.5 | 40000 | 38882.5 | 38890.5 | 0 | 38890.5 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.4455902778 | 57270 | 56902.7225231482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091211 | Cataclysmic variables (CVs) detected in the INTEGRAL and Swift BAT hard X-ray surveys are predominantly magnetic systems of the intermediate polar subtype. However, as the survey sensitivity improves, an increasing number of polars are also detected as hard X-ray sources, even though the majority of polars are soft X-ray bright and hard X-ray faint. Over the long term, we hope to understand why most polars are soft X-ray dominated, and why a subset is hard X-ray bright. Here we propose Suzaku observations of four poorly studied BAT-detected polars, 1RXS J032540.0-081442, Swift J2319.4+2619, IW Eri, and IGR J14536-5522, supported by ground-based observations including optical polarimetry, to determine their system parameters. | GALACTIC POINT SOURCES | 4 | A | MUKAI | KOJI | NULL | NULL | USA | 9 | AO9 | HARD X-RAY BRIGHT POLARS: WHY ARE THEY DIFFERENT? | XIS | Y |
| XB1916-053 | 289.7007 | -5.2492 | 31.34828117 | -8.46968862 | 261.8039 | 56944.6811574074 | 56948.5140740741 | 409032010 | 155885.1 | 300000 | 155885.1 | 155885.1 | 0 | 155885.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 8796.8 | 8796.8 | 19727.6 | 0 | PROCESSED | 57616.6949768518 | 56748 | 57017.41125 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091221 | XB1916-053 is a prototypical dipping low mass X-ray binary (LMXB) with a dip recurrence period of 3000.6+-0.2s. However, extensive optical observations also show a longer stable period of 3027s. The former is most likely the orbital period, and the latter the superhump period caused by the precession of an elliptical accretion disk at a period of 3.9 days, representing the beat period between optical and X-ray periods. The morphology of the X-ray dips does indeed change dramatically over several days, but existing data suggest a somewhat longer period for the dip morphology cycle of 4.7 days. Here we propose a 300ks Suzaku observation of XB1916-053 with as few interruptions as possible, to conduct a definitive timing and spectroscopic study of its disk emission and dipping activity. | GALACTIC POINT SOURCES | 4 | B | SMALE | ALAN | NULL | NULL | USA | 9 | AO9 | THE PRECESSING DISK IN THE DIPPING X-RAY BINARY XB1916-053 | XIS | Y |
| XB1916-053 | 289.7015 | -5.2503 | 31.34764946 | -8.47089453 | 261.8034 | 56948.5140856482 | 56952.1112152778 | 409032020 | 140449.5 | 300000 | 140457.5 | 140465.5 | 0 | 140449.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 6887.3 | 6887.3 | 14636 | 0 | PROCESSED | 57616.6738773148 | 56748 | 57000.2058680556 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091221 | XB1916-053 is a prototypical dipping low mass X-ray binary (LMXB) with a dip recurrence period of 3000.6+-0.2s. However, extensive optical observations also show a longer stable period of 3027s. The former is most likely the orbital period, and the latter the superhump period caused by the precession of an elliptical accretion disk at a period of 3.9 days, representing the beat period between optical and X-ray periods. The morphology of the X-ray dips does indeed change dramatically over several days, but existing data suggest a somewhat longer period for the dip morphology cycle of 4.7 days. Here we propose a 300ks Suzaku observation of XB1916-053 with as few interruptions as possible, to conduct a definitive timing and spectroscopic study of its disk emission and dipping activity. | GALACTIC POINT SOURCES | 4 | B | SMALE | ALAN | NULL | NULL | USA | 9 | AO9 | THE PRECESSING DISK IN THE DIPPING X-RAY BINARY XB1916-053 | XIS | Y |
| SCT X-1 | 278.8604 | -7.62 | 24.33197703 | 0.06047842 | 260.9601 | 56940.5300810185 | 56940.854375 | 409033010 | 15161.6 | 50000 | 15178.9 | 15177.6 | 0 | 15161.6 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.6415625 | 57373 | 56979.4099421296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091222 | We propose to observe the accreting 112s pulsar Scutum X-1 with Suzaku for 50ks. The optical companion is a late type giant or supergiant, making this a rare, persistent, non-OB-type wind accreting, Symbiotic X-ray Binary (SyXB). After initial flaring in the 1970s, the source generally exhibited low flux levels and has only rarely been observed. We will constrain the broadband spectrum, check for signs of wind accretion (variable absorption, log-normal count rate distribution), search for an iron fluorescence line, update the pulse period evolution, and compare to other Suzaku observations of SyXBs, especially to a quiescent observation of the prototype SyXB 4U 1954+31. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 9 | AO9 | THE SYMBIOTIC X-RAY BINARY SCUTUM X-1 | XIS | Y |
| SCT X-1 | 278.8598 | -7.62 | 24.33170335 | 0.06100641 | 260.9954 | 56952.1146412037 | 56953.1389814815 | 409033020 | 38581.1 | 34000 | 38581.1 | 38668.7 | 0 | 38676.7 | 3 | 3 | 0 | 3 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.6602314815 | 57373 | 57006.4003240741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091222 | We propose to observe the accreting 112s pulsar Scutum X-1 with Suzaku for 50ks. The optical companion is a late type giant or supergiant, making this a rare, persistent, non-OB-type wind accreting, Symbiotic X-ray Binary (SyXB). After initial flaring in the 1970s, the source generally exhibited low flux levels and has only rarely been observed. We will constrain the broadband spectrum, check for signs of wind accretion (variable absorption, log-normal count rate distribution), search for an iron fluorescence line, update the pulse period evolution, and compare to other Suzaku observations of SyXBs, especially to a quiescent observation of the prototype SyXB 4U 1954+31. | GALACTIC POINT SOURCES | 4 | A | POTTSCHMIDT | KATJA | NULL | NULL | USA | 9 | AO9 | THE SYMBIOTIC X-RAY BINARY SCUTUM X-1 | XIS | Y |
| CEP X-4 | 324.858 | 56.9961 | 99.01064753 | 3.3270936 | 51.1039 | 56826.8679282407 | 56828.0363541667 | 409037010 | 29764.7 | 50000 | 29764.7 | 50459.7 | 0 | 30933.2 | 2 | 3 | 0 | 2 | 1 | 0 | 0 | 53313.3 | 53313.3 | 100935.8 | 1 | PROCESSED | 57615.3130671296 | 57206 | 56839.8053240741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091232 | We propose to perform Target of Opportunity observations of two accreting neutron stars that are known cyclotron line sources, out of a sample of five, in outburst. The aim is to observe the sources for 50 ks at a level of >~40 mCrab and for another 45 ks at >~200 mCrab, in order to determine the properties of the cyclotron line(s) and constrain the broad band spectrum at different luminosities. These measurements have implications for the B-field strength and geometry as well as the properties of the accreted plasma. | GALACTIC POINT SOURCES | 4 | A | FUERST | FELIX | NULL | NULL | USA | 9 | AO9-TOO | CYCLOTRON LINES IN TRANSIENT PULSARS I: PROBING THE B-FIELD | XIS | Y |
| CYGNUS X-1 | 299.5796 | 35.2119 | 71.33922039 | 3.07967202 | 58.5817 | 56796.2767476852 | 56799.3266203704 | 409049010 | 14512.7 | 30000 | 0 | 14512.7 | 0 | 0 | 0 | 3 | 0 | 0 | 1 | 0 | 0 | 113825.9 | 113825.9 | 263461.9 | 1 | PROCESSED | 57615.2053703704 | 57180 | 56811.8023958333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091241 | We propose for a 30 ks observation of the accreting black hole Cygnus X-1 to occur simultaneously with NuSTAR. In mid-2012, we obtained a joint Suzaku/NuSTAR observation of Cyg X-1 in the soft state, and we clearly see reflection features with a relativistically broadened iron line that we have used to constrain the geometry of the accretion disk, including finding possible evidence for a warped accretion disk, and the black hole spin. This TOO proposal is to observe the source in the hard state to constrain how the accretion geometry changes between states. The combination of Suzaku and NuSTAR covers, with very good energy resolution and throughput, the thermal component, the iron line complex, the iron absorption edge, and the hard X-ray reflection hump. | GALACTIC POINT SOURCES | 4 | A | TOMSICK | JOHN | NULL | NULL | USA | 9 | AO9-TOO | CYGNUS X-1 IN THE HARD STATE WITH SUZAKU AND NUSTAR | XIS | Y |
| SWIFT J1753.5-0127 | 268.3654 | -1.4463 | 24.9013847 | 12.1907035 | 84.8023 | 56750.7354398148 | 56752.4452777778 | 409051010 | 59702.8 | 50000 | 59702.8 | 59710.8 | 0 | 59722.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 53681.2 | 53681.2 | 147709.5 | 2 | PROCESSED | 57614.197025463 | 57157 | 56789.6957175926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091243 | Due to the presence of a steady jet, constraining the properties of black hole systems in their hard state is important for understanding accretion disks and jets. Along with radio observations, Suzaku is constraining theoretical models by answering the following questions: Does the inner edge of the accretion disk recede in the hard state? How is the location of the disk's inner edge related to the presence of a jet? This proposal includes the use of Suzaku, NuSTAR, and radio observations to address these questions. A main diagnostic of the accretion geometry is the Compton reflection component, and the combination of Suzaku and NuSTAR covers, with very good energy resolution and sensitivity, the iron emission line, the absorption edges, and the hard X-ray reflection hump. | GALACTIC POINT SOURCES | 4 | A | TOMSICK | JOHN | NULL | NULL | USA | 9 | AO9-TOO | CONSTRAINING THE HARD STATE ACCRETION GEOMETRY FOR BLACK HOLE BINARIES | XIS | Y |
| CPD-28 2561 | 118.9748 | -28.6234 | 245.44211654 | -0.09136967 | 288.1635 | 56775.1365509259 | 56775.9174768518 | 409055010 | 26947.1 | 25000 | 26947.1 | 26955.1 | 0 | 26963.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 23126.1 | 23126.1 | 67461.9 | 0 | PROCESSED | 57615.0079513889 | 57214 | 56848.6257638889 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 092005 | We propose SUZAKU observations of the representative members of the class of magnetic massive O-type stars. The targets have measured magnetic fields and belong to similar spectral types. SUZAKU data will allow to compare the X-ray spectra of these objects that have similar stellar and wind parameters yet different magnetospheres. These observations will result in the first firm X-ray detections of our target stars. The analysis of XIS spectra will determine the emission measures and the temperatures of the hot gas. Our careful selection of targets will allow us to study the interplay between magnetic fields and stellar winds in O-type stars. These new observations for a comparative analysis of a homogeneous class of objects will be critical for driving the development of the theory. | GALACTIC POINT SOURCES | 4 | B | OSKINOVA | LIDIA | NULL | NULL | EUR | 9 | AO9 | COMPARATIVE STUDY OF MAGNETIC O-TYPE STARS WITH SUZAKU | XIS | Y |
| H 1743+322 | 266.5667 | -32.234 | 357.25546218 | -1.83442728 | 271.9807 | 56924.2942476852 | 56927.2779861111 | 409059010 | 119088.5 | 100000 | 119088.5 | 119096.5 | 0 | 119562.6 | 3 | 2 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.6267361111 | 57310 | 56940.6644560185 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 092020 | We propose a triggered Suzaku 100 ks observation of a high-inclination Galactic black hole binary in the hard intermediate state. This will be simultaneous with an already accepted XMM-Newton observation (PI: A. Ingram) to test the Lense-Thirring model for the low frequency quasi-periodic oscillations seen in black hole (and neutron star) binaries. The Suzaku PIN data will enable us to extend the energy range over which the QPO can be studied, allowing us to get much better constraints on the reflection component in the QPO spectrum, and hence to more tightly probe the geometry and emission processes in the regions closest to the black hole. | GALACTIC POINT SOURCES | 4 | A | AXELSSON | MAGNUS | NULL | NULL | EUR | 9 | AO9-TOO | TESTING THE LENSE-THIRRING ORIGIN OF THE LOW FREQUENCY QPO IN BLACK HOLE BINARIES | XIS | Y |
| EP DRA | 286.7359 | 69.1573 | 100.08892772 | 23.87463538 | 44.5637 | 57164.4409953704 | 57166.2856365741 | 410006010 | 80234.6 | 80000 | 80234.6 | 80242.6 | 0 | 80242.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 67958.5 | 67958.5 | 155581.9 | 1 | PROCESSED | 57618.7517939815 | 57558 | 57176.3159027778 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 100018 | It has been believed that white dwarfs (WDs) undergo a Type I supernova explosion when they reach 1.4 solar mass (Chandrasekhar limit) via mass accretion. However the equation of state (EOS) in the WDs which determines the WD mass limit have not been cleared. Especially, a EOS involving Landau quantization allows WDs to exceed 1.4 solar mass and approach 3.3 solar mass. We will get observational relations between WD mass and radius for proposed targets with Suzaku. With WD masses dynamically measured, we can estimate the WD radii without any theoretical mass-radius relation. We will be able to, for the first time, observationally investigate the influence of magnetic field on EOS in WDs and the WD mass-radius relation by the estimating WD radii and masses. | GALACTIC POINT SOURCES | 4 | A | HAYASHI | TAKAYUKI | NULL | NULL | JAP | 10 | AO10 | CONSTRAINT ON MASS-RADIUS RELATION OF HIGHLY MAGNETIZED WHITE DWARFS | XIS | Y |
| SXDB2 | 305.4808 | 37.2375 | 75.63404607 | 0.19419319 | 72.9993 | 57170.7872453704 | 57171.5090972222 | 410014010 | 29392.2 | 30000 | 29395.9 | 29394.7 | 0 | 29392.2 | 3 | 3 | 0 | 3 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57618.772650463 | 57558 | 57190.4609259259 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 100037 | The soft X-ray sky below 1 keV is spatially smooth after subtracting the local extended emission structures although the interstellar X-ray absorption column density is high enough to block the extragalactic X-ray photons below 1 keV totally in the Galactic disk. Suzaku reveals the existence of "excess" emissions in the Galactic disk and our observations will allow us to study a spatial distribution of the emissions and constrain the origin. | GALACTIC POINT SOURCES | 4 | C | MITSUISHI | IKUYUKI | NULL | NULL | JAP | 10 | AO10 | EXPLORING THE ORIGIN OF SOFT X-RAY DIFFUSE BACKGROUND IN THE GALACTIC DISK | XIS | Y |
| MRK 509 | 311.0374 | -10.7203 | 35.97290357 | -29.85106035 | 73.7532 | 57143.3705671296 | 57144.6814930556 | 410017010 | 54272.8 | 50000 | 54275.7 | 54275.7 | 0 | 54272.8 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57618.0659722222 | 57593 | 57225.3881944445 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 101708 | We propose combined Suzaku 50~ks and NuSTAR 200~ks observations of the bright Seyfert 1 galaxy Mrk~509 for the purpose of making a detailed study of the spectrum of radiation reflected from the accretion disk. Our chief aim is to constrain both the spin of the black hole and the properties of the corona that illuminates the disk. The combination of NuSTAR's high-sensitivity in the hard X-ray band, the soft-band coverage of Suzaku, and our state-of-the-art relativistic reflection models will allow us to break degeneracies between different scenarios currently proposed to explain the broadband spectrum of this exceptionally bright and much-studied source. | GALACTIC POINT SOURCES | 4 | A | GARCIA | JAVIER | NULL | NULL | USA | 10 | AO10 | OBSERVING THE STRONG-FIELD REGION OF THE AGN IN MRK~509 | XIS | Y |
| CYGNUS X-1 | 299.5777 | 35.2112 | 71.33781217 | 3.08063246 | 52.2303 | 57169.4748148148 | 57170.7827893518 | 410018010 | 11017.7 | 50000 | 11017.7 | 12205.7 | 0 | 11746.9 | 4 | 3 | 0 | 3 | 1 | 0 | 0 | 26131.5 | 26131.5 | 110759.8 | 0 | PROCESSED | 57618.8568171296 | 57626 | 57183.6630902778 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 101725 | We propose to observe Cygnus X-1 with NuSTAR (for 30 ks) and Suzaku (for 50 ks) in any spectral state in order to measure the reflection component and constrain the properties of the inner accretion disk, including the location of the inner radius, the geometry of the hard X-ray source, and the inclination. Observations made in the first two years of the NuSTAR mission have raised the interesting possibility that the inner disk inclination may differ from the orbital inclination, and this could occur if the black hole spin is misaligned. The proposed NuSTAR/Suzaku observation would be at the orbital phase where absorption due to stellar wind material is at a minimum, providing a clean measurement of the iron line profile and a significant improvement over the existing observations. | GALACTIC POINT SOURCES | 4 | A | TOMSICK | JOHN | NULL | NULL | USA | 10 | AO10 | THE INNER ACCRETION DISK AROUND THE RAPIDLY ROTATING BLACK HOLE IN CYGNUS X-1 | XIS | Y |
| BULGE 3 | 274.7046 | -31.4846 | 1.3002625 | -7.49777303 | 80.4025 | 53800.3437962963 | 53801.7474421296 | 500001010 | 51846.8 | 50000 | 51854.8 | 51854.8 | 51854.8 | 51846.8 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 45078.3 | 45078.3 | 121245.9 | 0 | PROCESSED | 57533.1540972222 | 54247 | 54041.7128703704 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001014 | Leading . | GALACTIC DIFFUSE EMISSION | 5 | A | MCCAMMON | DAN | NULL | NULL | JAP | 0 | SWG | THE SOFT GALACTIC BULGE | XIS | N |
| BULGE 2 | 270.6176 | -29.5847 | 1.30042786 | -3.49803376 | 83.2679 | 53801.7493981482 | 53802.0689699074 | 500002010 | 13028 | 10000 | 13052 | 13044 | 13036 | 13028 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 10674.1 | 10674.1 | 27599.9 | 1 | PROCESSED | 57533.1394444444 | 54247 | 54041.664525463 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001014 | Leading . | GALACTIC DIFFUSE EMISSION | 5 | A | MCCAMMON | DAN | NULL | NULL | JAP | 0 | SWG | THE SOFT GALACTIC BULGE | XIS | N |
| BULGE 6 | 282.6839 | -33.8925 | 1.99857856 | -14.59644221 | 88.3467 | 53802.7373032407 | 53803.0466087963 | 500003010 | 14261.7 | 10000 | 14261.7 | 14261.7 | 14261.7 | 14261.7 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 11414 | 11414 | 26715.9 | 1 | PROCESSED | 57533.1570833333 | 54247 | 54041.7424305556 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001014 | Leading . | GALACTIC DIFFUSE EMISSION | 5 | A | MCCAMMON | DAN | NULL | NULL | JAP | 0 | SWG | THE SOFT GALACTIC BULGE | XIS | N |
| RCW86 SW | 220.2761 | -62.6782 | 315.14426109 | -2.43598628 | 109.6929 | 53778.0961689815 | 53780.2814699074 | 500004010 | 100765.9 | 100000 | 100781.9 | 100765.9 | 100781.9 | 100781.9 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 90681.9 | 90681.9 | 188791.8 | 2 | PROCESSED | 57533.035787037 | 54247 | 54041.2835648148 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001019 | The supernova remnants (SNRs) are most convincing candidates for the acceleration of cosmic-rays. Together with the TeV gamma-ray detection by CANGAROO and HESS, it is now confirmed that at least some of the SNRs can actually accelerate electrons up to > 10 TeV. However, such studies have not provided direct information on ``protons'', which is the major component of cosmic-rays. Here we propose to measure spatial distribution of accelerated protons in the shell of RCW 86, and its association with the high energy (>10 TeV) electrons which emit synchrotron X-rays up to 50 keV. Large effective area and the good detection capability of Suzaku will be ideal tools for our scientific goal. | GALACTIC DIFFUSE EMISSION | 5 | A | KATAOKA | JUN | NULL | NULL | JAP | 0 | SWG | THE FIRST DIRECT MAPPING OF ACCELERATED PROTONS IN THE SW SHELL OF RCW 86 | XIS | N |
| GC CENTER #2 | 266.7693 | -28.6295 | 0.42794484 | -0.11339991 | 74.7707 | 53821.958587963 | 53823.7585069444 | 500005010 | 88424.7 | 100000 | 88432.7 | 88424.7 | 88432.7 | 88432.7 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 64591.1 | 64591.1 | 155501.9 | 2 | PROCESSED | 57533.3630324074 | 54247 | 54133.0079861111 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001020 | We propose to obtain high quality spectrum near the GC. The objective is to resolve 6.4, 6.7, and 6.9 keV line and determine the high energy tail and sub-structures, which may be X-ray reflection from Sgr A* (6.4 keV line + 7.1 keV edge + high energy tail), thermal plasma (6.7 + 6.9 keV lines, with no hard X-ray tail), non thermal emission (e.g. line but hard X-ray tail). Unexpected spectral feature could be also found, depending on the real origin. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 0 | SWG | SUZAKU GALACTIC CENTER OBSERVATION PROJECT: #2 SGR B1 | NULL | N |
| SN 1987A | 83.8361 | -69.2786 | 279.71542477 | -31.94667609 | 132.5904 | 53677.835775463 | 53678.3475 | 500006010 | 36786.3 | 40000 | 36786.3 | 36786.3 | 36786.3 | 36786.3 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 32919.8 | 32919.8 | 44166.1 | 1 | PROCESSED | 57527.9193518518 | 54247 | 54037.1281481482 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001028 | SN1987A is providing us with a unique opportunity to study the supernova explosion itself and the very early phase of the supernova-remnants evolution. The supernova blast wave has started to strike the inner circumstellar ring. The neutrino flash observed at the time of explosion implies the formation of a neutron star, but no evidence of this has been detected yet. We propose to observe SN1987A for 40 ksec with Suzaku HXD and XIS. Our first goal is the search for a periodic hard signal from the putative pulsar. We also want to study the collision of the supernova blast wave with the inner ring. In order to follow the temporal evolution of the shock, we propose to observe the source with Suzaku in the early phase of the SWG PV-phase as a reference for further studies. | GALACTIC DIFFUSE EMISSION | 5 | A | HASINGER | GUENTHER | NULL | NULL | JAP | 0 | SWG | SUZAKU OBSERVATION OF SN1987A : SEARCH FOR PULSAR EMISSION AND STUDY OF A NEWBORN SNR | NULL | N |
| HESS J1804-216 | 271.1693 | -21.6722 | 8.44223916 | -0.04647489 | 89.0483 | 53831.6120138889 | 53832.4919328704 | 500007010 | 37522.2 | 50000 | 37522.2 | 37522.2 | 37522.2 | 37522.2 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 28933.6 | 28933.6 | 75990.1 | 0 | PROCESSED | 57533.4045138889 | 54247 | 54042.288900463 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001029 | HESS found several new TeV sources in the Galactic Plane Survey. Possible origin would be PWN or synchrotron X-ray SNR shell. However many of these new TeV sources (their sizes are ~10 arcmin) have no counterpart in any other wavelength. They can be main contributors to the Galactic Cosmic rays. In order to reveal the nature of these fantastic objects, we propose to observe the extended sources. HESS~J1616-508 is already observed and we found this source has quite low surface brightness in X-rays compared with TeV gamma-rays, indicating this is a dark particle accelerator Here, we point out HESS~J1804-216 which has possible counterparts in other wavelengths, then it might be the missing link between known Galactic accelerators and dark particle accelerators. | GALACTIC DIFFUSE EMISSION | 5 | A | BAMBA | AYA | NULL | NULL | JAP | 0 | SWG | SEARCH FOR X-RAY COUNTERPARTS OF ``DARK PARTICLE ACCELERATORS'' | XIS | N |
| HESS J1804-216 BGD | 270.9564 | -22.0176 | 8.04431311 | -0.04388906 | 89.2004 | 53832.4925462963 | 53833.454375 | 500008010 | 40717.1 | 50000 | 40717.1 | 40717.1 | 40717.1 | 40717.1 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 30642.9 | 30642.9 | 83087.9 | 1 | PROCESSED | 57533.4349537037 | 54247 | 54056.4266666667 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001029 | HESS found several new TeV sources in the Galactic Plane Survey. Possible origin would be PWN or synchrotron X-ray SNR shell. However many of these new TeV sources (their sizes are ~10 arcmin) have no counterpart in any other wavelength. They can be main contributors to the Galactic Cosmic rays. In order to reveal the nature of these fantastic objects, we propose to observe the extended sources. HESS~J1616-508 is already observed and we found this source has quite low surface brightness in X-rays compared with TeV gamma-rays, indicating this is a dark particle accelerator Here, we point out HESS~J1804-216 which has possible counterparts in other wavelengths, then it might be the missing link between known Galactic accelerators and dark particle accelerators. | GALACTIC DIFFUSE EMISSION | 5 | A | BAMBA | AYA | NULL | NULL | JAP | 0 | SWG | SEARCH FOR X-RAY COUNTERPARTS OF ``DARK PARTICLE ACCELERATORS'' | XIS | N |
| GALACTIC RIDGE | 281.0049 | -4.0776 | 28.45801897 | -0.21166151 | 265.5297 | 53671.1112037037 | 53673.8960069445 | 500009010 | 93327.6 | 100000 | 93343.6 | 93359.6 | 93343.6 | 93327.6 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 77536.4 | 77536.4 | 240575.9 | 0 | PROCESSED | 57527.7330439815 | 54247 | 54037.6929513889 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001042 | We propose to observe the blank Galactic plane field at (l,b)=(28.6,0.0) for 200 ksec to study energy spectra of Galactic Ridge X-ray Emission. This is a Chandra deep field where we have spent 100 ksec. We will carry out plasma diagnostics of the Galactic ridge emission using primarily iron lines, and also Kalpha and Kbeta lines of Ne, Mg, Si, and S. The 200 ksec Ridge observation by Suzaku enables us to compare Galactic center and ridge emission lines directly. We believe the Galactic Ridge X-ray emission is truely diffuse, based on our Chandra study. However, there is a claim that the ridge emission is preimaly composed of dim sources down to 10^-16 cgs in 2-10 keV. To end the controversy, we plan to carry out a 1Msec Chandra observation on this Chandra-Suzaku field. | GALACTIC DIFFUSE EMISSION | 5 | A | EBISAWA | KEN | NULL | NULL | JAP | 0 | SWG | ORIGIN OF THE GALACTIC RIDGE X-RAY EMISSION | NULL | N |
| GALACTIC RIDGE | 281.0036 | -4.078 | 28.45707071 | -0.21069081 | 265.5303 | 54023.0938888889 | 54025.8141087963 | 500009020 | 98858.3 | 100000 | 98874.3 | 98866.3 | 98858.3 | 98874.3 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 81951.9 | 81951.9 | 235013.9 | 1 | PROCESSED | 57535.9070023148 | 54697 | 54055.6082407407 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001042 | We propose to observe the blank Galactic plane field at (l,b)=(28.6,0.0) for 200 ksec to study energy spectra of Galactic Ridge X-ray Emission. This is a Chandra deep field where we have spent 100 ksec. We will carry out plasma diagnostics of the Galactic ridge emission using primarily iron lines, and also Kalpha and Kbeta lines of Ne, Mg, Si, and S. The 200 ksec Ridge observation by Suzaku enables us to compare Galactic center and ridge emission lines directly. We believe the Galactic Ridge X-ray emission is truely diffuse, based on our Chandra study. However, there is a claim that the ridge emission is preimaly composed of dim sources down to 10^-16 cgs in 2-10 keV. To end the controversy, we plan to carry out a 1Msec Chandra observation on this Chandra-Suzaku field. | GALACTIC DIFFUSE EMISSION | 5 | A | EBISAWA | KEN | NULL | NULL | JAP | 0 | SWG | ORIGIN OF THE GALACTIC RIDGE X-RAY EMISSION | XIS | Y |
| RXJ_0852-4622_NW | 132.2926 | -45.6157 | 265.39238743 | -1.14402175 | 137.763 | 53723.4478240741 | 53727.3016666667 | 500010010 | 175453 | 150000 | 175453 | 175525 | 175460.8 | 175461 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 230002.5 | 230002.5 | 332943.7 | 7 | PROCESSED | 57532.5654513889 | 54247 | 54059.902662037 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001048 | We propose to observe two lobes of X-ray and gamma-ray emission from the shell remnant RXJ 0852-4622 (Vela Jr) with HXD. The 1-10 keV spectrum of this remnant is essentially a featureless continuum attributed to synchrotron emission from accelerated electrons, with the X-ray and gamma-ray morphologies being very well matched. Observations at energies above 10 keV with HXD will probe the cut-off energy of the synchrotron spectrum, shedding light on the electron acceleration efficiency. The large size of the remnant makes it possible to observe different portions of the limb with separate HXD PIN observations. | GALACTIC DIFFUSE EMISSION | 5 | A | HWANG | UNA | NULL | NULL | JAP | 0 | SWG | HXD OBSERVATION OF NONTHERMAL EMISSION FROM RXJ 0852-4622 | HXD | N |
| RXJ_0852-4622_NW_offset | 135.1284 | -47.9102 | 268.39892579 | -1.13950817 | 140.267 | 53727.3040393518 | 53728.368912037 | 500010020 | 59178.4 | 50000 | 59178.4 | 59192.5 | 59202.6 | 59192.5 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 63482.1 | 63482.1 | 91995.9 | 0 | PROCESSED | 57532.4967708333 | 54247 | 54039.2486226852 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001048 | We propose to observe two lobes of X-ray and gamma-ray emission from the shell remnant RXJ 0852-4622 (Vela Jr) with HXD. The 1-10 keV spectrum of this remnant is essentially a featureless continuum attributed to synchrotron emission from accelerated electrons, with the X-ray and gamma-ray morphologies being very well matched. Observations at energies above 10 keV with HXD will probe the cut-off energy of the synchrotron spectrum, shedding light on the electron acceleration efficiency. The large size of the remnant makes it possible to observe different portions of the limb with separate HXD PIN observations. | GALACTIC DIFFUSE EMISSION | 5 | A | HWANG | UNA | NULL | NULL | JAP | 0 | SWG | HXD OBSERVATION OF NONTHERMAL EMISSION FROM RXJ 0852-4622 | HXD | N |
| SMC DIFFUSE 1 | 13.0188 | -72.8206 | 302.86615918 | -44.30756989 | 221.6864 | 53687.4452893518 | 53688.2231944445 | 500011010 | 46778.9 | 50000 | 46778.9 | 46786.9 | 46786.9 | 46786.9 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 47868.4 | 47868.4 | 67199.9 | 0 | PROCESSED | 57527.967337963 | 54247 | 54038.3531712963 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001049 | We propose to use Suzaku XIS to observe regions of diffuse emission in the Magellanic Clouds. The diffuse component was identified by ROSAT PSPC observations, but has never been studied with a true spectroscopic instrument. Suzaku is well-matched to the angular size and expected temperature of the regions of diffuse emission in the LMC. Not only will such observations give a clear view of the temperature structure of this gas, they will provide a direct measurement of ambient abundances in the Clouds. | GALACTIC DIFFUSE EMISSION | 5 | A | HWANG | UNA | NULL | NULL | JAP | 0 | SWG | DIFFUSE EMISSION IN THE MAGELLANIC CLOUDS | XIS | N |
| 73P/SW3 | 279.2884 | 33.5067 | 62.26395264 | 17.33399104 | 47.3721 | 53862.3946875 | 53862.4794444444 | 500012010 | 3250 | 5000 | 3250 | 3250 | 3250 | 3250 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2313.9 | 2313.9 | 7304 | 0 | PROCESSED | 57533.6418402778 | 54256 | 54042.1755671296 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N |
| 73P/SW3 | 279.6627 | 33.4734 | 62.35168426 | 17.03145652 | 46.5564 | 53862.4804282407 | 53862.5419444444 | 500012020 | 3248 | 5000 | 3248 | 3248 | 3248 | 3248 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2111.9 | 2111.9 | 5279.9 | 0 | PROCESSED | 57533.7332407407 | 54256 | 54042.2282175926 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N |
| 73P/SW3 | 316.717 | 24.6807 | 71.53645371 | -15.07849931 | 72.7087 | 53868.1752314815 | 53868.2085532407 | 500013010 | 2353 | 20000 | 2353 | 2353 | 2353 | 2353 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2595 | 2595 | 2871.9 | 0 | PROCESSED | 57534.2831597222 | 54256 | 54042.2312268518 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N |
| 73P/SW3 | 317.1042 | 24.5187 | 71.64340536 | -15.45205291 | 72.7099 | 53868.2091666667 | 53868.2752199074 | 500013020 | 3225 | 20000 | 3225 | 3225 | 3225 | 3225 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 3467 | 3467 | 5703.9 | 0 | PROCESSED | 57534.2879398148 | 54256 | 54042.2634027778 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N |
| 73P/SW3 | 317.5094 | 24.3437 | 71.75290875 | -15.84652301 | 72.7094 | 53868.2758333333 | 53868.3418865741 | 500013030 | 3225 | 20000 | 3225 | 3225 | 3225 | 3225 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2915 | 2915 | 5703.9 | 0 | PROCESSED | 57534.2995023148 | 54256 | 54042.2712731482 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N |
| 73P/SW3 | 317.9167 | 24.1666 | 71.86402338 | -16.24383714 | 72.7109 | 53868.3425 | 53868.4085532407 | 500013040 | 3225 | 20000 | 3225 | 3225 | 3225 | 3225 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2677 | 2677 | 5703.9 | 0 | PROCESSED | 57534.2934143518 | 54256 | 54042.2977430556 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N |
| 73P/SW3 | 318.3252 | 23.9905 | 71.97868305 | -16.64134569 | 72.7093 | 53868.4091666667 | 53868.4752199074 | 500013050 | 3225 | 20000 | 3225 | 3225 | 3225 | 3225 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2584 | 2584 | 5703.9 | 0 | PROCESSED | 57534.2992476852 | 54256 | 54089.4348611111 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N |
| 73P/SW3 | 318.7382 | 23.8104 | 72.09504522 | -17.04458663 | 72.7096 | 53868.4758333333 | 53868.5418865741 | 500013060 | 3218 | 20000 | 3218 | 3218 | 3218 | 3218 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2539 | 2539 | 5695.9 | 0 | PROCESSED | 57534.3046759259 | 54256 | 54042.3000462963 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N |
| 73P/SW3 | 319.1503 | 23.6322 | 72.21442919 | -17.44595626 | 72.7095 | 53868.5425 | 53868.6085532407 | 500013070 | 3062.4 | 20000 | 3062.4 | 3062.4 | 3062.4 | 3062.4 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2088 | 2088 | 5688 | 1 | PROCESSED | 57534.3049074074 | 54256 | 54042.3037268518 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N |
| 73P/SW3 | 319.575 | 23.4516 | 72.3420597 | -17.8575616 | 72.7092 | 53868.609212963 | 53868.6738310185 | 500013080 | 3164.4 | 20000 | 3164.4 | 3164.4 | 3164.4 | 3164.4 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2986 | 2986 | 5551.9 | 0 | PROCESSED | 57534.3120601852 | 54256 | 54042.3213657407 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N |
| 73P/SW3 | 18.4857 | -9.3839 | 140.65827116 | -71.47693301 | 59.4008 | 53893.6903703704 | 53893.7356365741 | 500014010 | 3228 | 35000 | 3228 | 3228 | 3228 | 3228 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 3312 | 3312 | 3903.9 | 0 | PROCESSED | 57534.5195486111 | 54267 | 54052.5070949074 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N |
| 73P/SW3 | 17.8447 | -9.1515 | 138.54867442 | -71.41609802 | 59.3994 | 53893.7363888889 | 53893.8023032407 | 500014020 | 3236.9 | 35000 | 3236.9 | 3236.9 | 3236.9 | 3236.9 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2478 | 2478 | 5687.9 | 0 | PROCESSED | 57534.5816435185 | 54267 | 54052.5079861111 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N |
| 73P/SW3 | 17.8996 | -9.1693 | 138.7272506 | -71.42013328 | 59.3998 | 53893.8025 | 53893.8689699074 | 500014030 | 3236.1 | 35000 | 3236.1 | 3236.1 | 3236.1 | 3236.1 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2433.1 | 2433.1 | 5735.9 | 0 | PROCESSED | 57534.5821875 | 54267 | 54052.5088310185 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N |
| 73P/SW3 | 17.9545 | -9.1915 | 138.90931762 | -71.42827213 | 59.4015 | 53893.8691666667 | 53893.9356365741 | 500014040 | 3236 | 35000 | 3236 | 3236 | 3236 | 3236 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2490.9 | 2490.9 | 5735.9 | 0 | PROCESSED | 57534.5832407407 | 54267 | 54052.5308912037 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N |
| 73P/SW3 | 18.0085 | -9.2093 | 139.0853548 | -71.43220951 | 59.4015 | 53893.9358333333 | 53894.0023032407 | 500014050 | 3235 | 35000 | 3235 | 3235 | 3235 | 3235 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2504.1 | 2504.1 | 5735.9 | 0 | PROCESSED | 57534.5878125 | 54267 | 54052.5317361111 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N |
| 73P/SW3 | 18.0599 | -9.2267 | 139.25333623 | -71.43625621 | 59.4006 | 53894.0025 | 53894.0689699074 | 500014060 | 3235 | 35000 | 3235 | 3235 | 3235 | 3235 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 2490 | 2490 | 5735.9 | 0 | PROCESSED | 57534.5883796296 | 54267 | 54052.5346759259 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N |
| 73P/SW3 | 18.1094 | -9.2436 | 139.41528011 | -71.44015907 | 59.3996 | 53894.0691666667 | 53894.1356365741 | 500014070 | 2220.9 | 35000 | 2220.9 | 2220.9 | 2220.9 | 2220.9 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 1939 | 1939 | 5735.9 | 1 | PROCESSED | 57534.589849537 | 54267 | 54052.5472800926 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N |
| 73P/SW3 | 18.1606 | -9.2654 | 139.58635244 | -71.44823165 | 59.3999 | 53894.1358333333 | 53894.2085416667 | 500014080 | 1863.7 | 35000 | 1863.7 | 1863.7 | 1863.7 | 1863.7 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 1921.2 | 1921.2 | 6277.9 | 0 | PROCESSED | 57534.5937731482 | 54267 | 54052.5243171296 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N |
| 73P/SW3 | 18.2084 | -9.2837 | 139.744498 | -71.45365551 | 59.3985 | 53894.2087384259 | 53894.2689467593 | 500014090 | 1508.9 | 35000 | 1508.9 | 1508.9 | 1508.9 | 1508.9 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 1655.2 | 1655.2 | 5202 | 0 | PROCESSED | 57534.5937037037 | 54267 | 54052.5382986111 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N |
| 73P/SW3 | 18.2503 | -9.299 | 139.88257526 | -71.45759255 | 59.3985 | 53894.2691435185 | 53894.3356134259 | 500014100 | 1312.1 | 35000 | 1312.1 | 1312.1 | 1312.1 | 1312.1 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 1322 | 1322 | 5742 | 0 | PROCESSED | 57534.5960185185 | 54267 | 54052.5405324074 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N |
| 73P/SW3 | 18.2949 | -9.3163 | 140.03044964 | -71.46265703 | 59.3979 | 53894.3358101852 | 53894.4022800926 | 500014110 | 1424.9 | 35000 | 1424.9 | 1424.9 | 1424.9 | 1424.9 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 1433 | 1433 | 5742 | 0 | PROCESSED | 57534.5994444445 | 54267 | 54052.5225694444 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N |
| 73P/SW3 | 18.338 | -9.3332 | 140.17356876 | -71.46762322 | 59.3974 | 53894.4024768518 | 53894.4682986111 | 500014120 | 1555.1 | 35000 | 1555.1 | 1555.1 | 1555.1 | 1555.1 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 1566 | 1566 | 5682 | 0 | PROCESSED | 57534.5988773148 | 54267 | 54052.5441782407 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N |
| 73P/SW3 | 18.3869 | -9.3535 | 140.33698221 | -71.47421859 | 59.3991 | 53894.4684490741 | 53894.5356365741 | 500014130 | 1693.9 | 35000 | 1693.9 | 1693.9 | 1693.9 | 1693.9 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 1694 | 1694 | 5804 | 0 | PROCESSED | 57534.6023611111 | 54267 | 54052.5234722222 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N |
| 73P/SW3 | 18.435 | -9.3697 | 140.49459076 | -71.47695116 | 59.4003 | 53894.5358333333 | 53894.6016087963 | 500014140 | 1977 | 35000 | 1977 | 1977 | 1977 | 1977 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 1951 | 1951 | 5671.9 | 0 | PROCESSED | 57534.60375 | 54267 | 54052.5450231482 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N |
| 73P/SW3 | 18.4874 | -9.3902 | 140.66879726 | -71.4825298 | 59.4036 | 53894.6018055556 | 53894.680775463 | 500014150 | 3232 | 35000 | 3232 | 3232 | 3232 | 3232 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 3293 | 3293 | 6815.9 | 0 | PROCESSED | 57534.6057638889 | 54267 | 54052.5265509259 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001050 | Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets. | GALACTIC DIFFUSE EMISSION | 5 | A | PORTER | FREDERICK | NULL | NULL | JAP | 0 | SWG | AN XIS OBSERVATION OF THE BRIGHTEST COMET OF THE DECADE: 73P/SCHWASSMANN-WACHMANN 3 | XIS | N |
| MBM12 | 44.0042 | 19.487 | 159.18888296 | -34.46916863 | 253.4644 | 53769.9600578704 | 53772.6460416667 | 500015010 | 102937.1 | 100000 | 102937.1 | 102937.1 | 102937.1 | 102937.1 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 93670.9 | 93670.9 | 232049.9 | 1 | PROCESSED | 57532.9850694444 | 54247 | 54041.1327662037 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001059 | Suzaku can potentially determine the time since the nearby supernova that created (or reheated) the Local Hot Bubble (LHB) by measuring the ratio of the O VII/O VIII lines emitted by the LHB. The LHB temperature is ~10^6 K, and in equilibrium we would expect no O VIII emission. However, the LHB is almost certainly not in equilibrium, and it is quite possible that significant O^{+7} is still recombining (and emitting O VIII) following its creation in the most recent local supernova 2-4 Myr ago. We propose to measure these lines from the LHB using the nearby molecular cloud MBM12 as a curtain to shadow more distant emission. Even if O VIII is not detected, the O VII measurement will be the first unambiguous measurement of a line from the LHB. | GALACTIC DIFFUSE EMISSION | 5 | A | SMITH | RANDALL | NULL | NULL | JAP | 0 | SWG | DATING THE LOCAL HOT BUBBLE WITH SUZAKU | XIS | N |
| SN1006 SE | 225.8656 | -42.0517 | 327.61589547 | 14.40537 | 115.0022 | 53765.3759259259 | 53766.487662037 | 500016010 | 51607.6 | 50000 | 51613.2 | 51621.2 | 51621.2 | 51607.6 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 55670.4 | 55670.4 | 96039.9 | 2 | PROCESSED | 57532.8333564815 | 54247 | 54040.6484259259 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001062 | We propose two Suzaku pointings of the Galactic supernova remnant (SNR) that exploded as a supernova in 1006. The main goal of the project is to use the XIS measure the abundances of low-Z elements in the ejecta. | GALACTIC DIFFUSE EMISSION | 5 | A | HUGHES | JOHN | NULL | NULL | JAP | 0 | SWG | THE EJECTA IN SN1006 | XIS | N |
| SN1006 NW | 225.6364 | -41.8003 | 327.59294648 | 14.70833496 | 115.0008 | 53766.4881365741 | 53767.55375 | 500017010 | 53019.4 | 50000 | 53019.4 | 53027.7 | 53027.3 | 53027.3 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 60412.3 | 60412.3 | 92067.9 | 0 | PROCESSED | 57532.8347685185 | 54247 | 54040.7669675926 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001062 | We propose two Suzaku pointings of the Galactic supernova remnant (SNR) that exploded as a supernova in 1006. The main goal of the project is to use the XIS measure the abundances of low-Z elements in the ejecta. | GALACTIC DIFFUSE EMISSION | 5 | A | HUGHES | JOHN | NULL | NULL | JAP | 0 | SWG | THE EJECTA IN SN1006 | XIS | N |
| SGR C | 266.1523 | -29.4673 | 359.43182832 | -0.08906822 | 82.0001 | 53786.5315393518 | 53789.4515509259 | 500018010 | 106921.9 | 100000 | 106921.9 | 106921.9 | 106921.9 | 106921.9 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 46606.9 | 46606.9 | 252277.8 | 2 | PROCESSED | 57533.0732175926 | 54247 | 54041.6109375 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001079 | We propose 100 ksec observation of the Sgr C cloud in the Galactic center region. The cloud emits strong 6.4-keV line, and is a candidate of X-ray reflection nebula; the molecular cloud which emits fluorescence and scattered X-rays irradiated by an external X-ray source. The past activity of Sgr~A$^*$, the Galactic nucleus, may be the origin of 6.4-keV line. We will study 6.4-keV line and verify the X-ray reflection scenario. The second objective is to study the distribution of high ionized and neutral iron lines in the GC region. Chandra observation indicates that H-like iron line is very strong in this region. With the higher energy resolution of XIS, we can confirm the Chandra results. High energy diffuse emission above 10 keV is also a important target by HXD. | GALACTIC DIFFUSE EMISSION | 5 | A | MURAKAMI | HIROSHI | NULL | NULL | JAP | 0 | SWG | FOSSILS OF THE GALACTIC CENTER ACTIVITY | XIS | N |
| SGR C BGD | 265.7856 | -29.8854 | 358.90876565 | -0.03691694 | 81.9998 | 53789.4522106482 | 53789.8349421296 | 500019010 | 13307.3 | 10000 | 13315.3 | 13315.3 | 13315.3 | 13307.3 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 12240.4 | 12240.4 | 33063.9 | 0 | PROCESSED | 57533.050462963 | 54247 | 54041.3629166667 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001079 | We propose 100 ksec observation of the Sgr C cloud in the Galactic center region. The cloud emits strong 6.4-keV line, and is a candidate of X-ray reflection nebula; the molecular cloud which emits fluorescence and scattered X-rays irradiated by an external X-ray source. The past activity of Sgr~A$^*$, the Galactic nucleus, may be the origin of 6.4-keV line. We will study 6.4-keV line and verify the X-ray reflection scenario. The second objective is to study the distribution of high ionized and neutral iron lines in the GC region. Chandra observation indicates that H-like iron line is very strong in this region. With the higher energy resolution of XIS, we can confirm the Chandra results. High energy diffuse emission above 10 keV is also a important target by HXD. | GALACTIC DIFFUSE EMISSION | 5 | A | MURAKAMI | HIROSHI | NULL | NULL | JAP | 0 | SWG | FOSSILS OF THE GALACTIC CENTER ACTIVITY | XIS | N |
| CYGNUS LOOP NE1 | 314.1885 | 31.738 | 75.60815027 | -8.84073861 | 223.0005 | 53697.7354282407 | 53698.2051388889 | 500020010 | 20343.7 | 20000 | 20351.7 | 20351.7 | 20351.7 | 20343.7 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 17992 | 17992 | 40575.9 | 0 | PROCESSED | 57528.0684837963 | 54247 | 54037.9167476852 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001093 | We propose four 20 ksec observations of the northeastern limb of the Cygnus Loop supernova remnant to study a recently discovered carbon rich region. This region seems to be the result of the interaction between the shock and an interstellar cloud or the cavity wall. Because of the superior spectral resolution and low background of the XIS in the low energy region, these pointings can also be used for the study of the C-N-O abundance ratio of the ISM in the vicinity of the Loop. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 0 | SWG | CARBON-RICH REGION ON THE NORTHEASTERN LIMB OF THE CYGNUS LOOP SUPERNOVA REMNANT | NULL | N |
| CYGNUS LOOP NE2 | 313.9681 | 31.9542 | 75.65570239 | -8.55863001 | 223.0005 | 53698.2056134259 | 53698.6766666667 | 500021010 | 21413.5 | 20000 | 21445.5 | 21437.5 | 21429.5 | 21413.5 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 21654.1 | 21654.1 | 40693.9 | 0 | PROCESSED | 57528.0693518518 | 54247 | 54038.4014351852 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001093 | We propose four 20 ksec observations of the northeastern limb of the Cygnus Loop supernova remnant to study a recently discovered carbon rich region. This region seems to be the result of the interaction between the shock and an interstellar cloud or the cavity wall. Because of the superior spectral resolution and low background of the XIS in the low energy region, these pointings can also be used for the study of the C-N-O abundance ratio of the ISM in the vicinity of the Loop. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 0 | SWG | CARBON-RICH REGION ON THE NORTHEASTERN LIMB OF THE CYGNUS LOOP SUPERNOVA REMNANT | NULL | N |
| CYGNUS LOOP NE3 | 313.7583 | 32.1826 | 75.71932756 | -8.27611719 | 222.9011 | 53703.7415162037 | 53704.2355208333 | 500022010 | 21133.8 | 20000 | 21191.6 | 21719.9 | 21133.8 | 21359.9 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 20244.5 | 20244.5 | 42679.9 | 1 | PROCESSED | 57528.1127893518 | 54247 | 54038.7522106482 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001093 | We propose four 20 ksec observations of the northeastern limb of the Cygnus Loop supernova remnant to study a recently discovered carbon rich region. This region seems to be the result of the interaction between the shock and an interstellar cloud or the cavity wall. Because of the superior spectral resolution and low background of the XIS in the low energy region, these pointings can also be used for the study of the C-N-O abundance ratio of the ISM in the vicinity of the Loop. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 0 | SWG | CARBON-RICH REGION ON THE NORTHEASTERN LIMB OF THE CYGNUS LOOP SUPERNOVA REMNANT | XIS | N |
| CYGNUS LOOP NE4 | 313.5005 | 32.369 | 75.72495347 | -7.98937114 | 221.2023 | 53704.2368287037 | 53704.7661342593 | 500023010 | 25004.9 | 20000 | 25004.9 | 25268.9 | 25006.7 | 25068.9 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 25124.9 | 25124.9 | 45726 | 1 | PROCESSED | 57532.3510763889 | 54247 | 54038.67625 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001093 | We propose four 20 ksec observations of the northeastern limb of the Cygnus Loop supernova remnant to study a recently discovered carbon rich region. This region seems to be the result of the interaction between the shock and an interstellar cloud or the cavity wall. Because of the superior spectral resolution and low background of the XIS in the low energy region, these pointings can also be used for the study of the C-N-O abundance ratio of the ISM in the vicinity of the Loop. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 0 | SWG | CARBON-RICH REGION ON THE NORTHEASTERN LIMB OF THE CYGNUS LOOP SUPERNOVA REMNANT | XIS | N |
| TYCHO SNR | 6.3244 | 64.1507 | 120.08671326 | 1.42345384 | 81.1044 | 53913.439224537 | 53915.6530555556 | 500024010 | 101127.4 | 100000 | 101143.4 | 101127.4 | 101143.4 | 101143.4 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 94512.3 | 94512.3 | 191206.8 | 3 | PROCESSED | 57534.8252199074 | 54289 | 54052.7199884259 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001099 | We propose to observe Tycho's Supernova Remnant with Suzaku. The proposal has two main goals: (1) to measure the energy spectrum of the entire remnant above 10 keV with the HXD, and (2) to study the 0.5-10 keV band spectrum as a function of position with the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | HUGHES | JOHN | NULL | NULL | JAP | 0 | SWG | SUZAKU STUDY OF TYCHO'S SUPERNOVA REMNANT | XIS | N |
| TYCHO SNR HXD BKGD | 9.2173 | 64.3076 | 121.35322514 | 1.48051733 | 84.2005 | 53915.6541782407 | 53916.7606944444 | 500025010 | 51008.8 | 50000 | 51008.8 | 51008.8 | 51008.8 | 51008.8 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 48722.4 | 48722.4 | 95593.9 | 2 | PROCESSED | 57534.8010300926 | 54302 | 54052.5940509259 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001099 | We propose to observe Tycho's Supernova Remnant with Suzaku. The proposal has two main goals: (1) to measure the energy spectrum of the entire remnant above 10 keV with the HXD, and (2) to study the 0.5-10 keV band spectrum as a function of position with the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | HUGHES | JOHN | NULL | NULL | JAP | 0 | SWG | SUZAKU STUDY OF TYCHO'S SUPERNOVA REMNANT | HXD | N |
| NEP | 272.8227 | 66.0165 | 95.79277142 | 28.663354 | 126.3033 | 53776.2556944445 | 53778.0836111111 | 500026010 | 88508.2 | 80000 | 88532.2 | 88508.2 | 88524.2 | 88532.2 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 83672.8 | 83672.8 | 157902 | 0 | PROCESSED | 57532.9856481482 | 54247 | 54041.1403703704 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000042 | We propose a second Suzaku observation of the NEP region in order to constrain the long-term and short-term valiability of OVII and OIVVV emission line intensities.Short-term variability detected in the first Suzaku observation implies existence of a charge-exchange component in oVIII linem suggesting solar wind and geo corona interaction. First purpose is to confirm this with the second observtaion.Secondly, to search a long-term variability. If it is observed, it will place a further constraints on the solar wind and interplanetary medium near the Earth. | GALACTIC DIFFUSE EMISSION | 5 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | NEP | XIS | N |
| HIGH LAT. DIFFUSE A | 246.1745 | 43.4846 | 68.4171583 | 44.39202319 | 129.9994 | 53780.2926388889 | 53781.9640509259 | 500027010 | 73578.7 | 70000 | 73586.7 | 73586.7 | 73578.7 | 73586.7 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 67399.3 | 67399.3 | 144397.9 | 3 | PROCESSED | 57533.0379976852 | 54247 | 54041.3110416667 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000044 | We propose observing the diffse background at two locations where the low temperature component is particularly string. One of the these enhancement is ostensibly an extension of the local bubble, while the other it is probably due to a region of very bright emission in the halo (z> 400 pc). We can verify the thermal nature of these sources, and look for CNO abyndance ratio differences between local disk and halo gas. It is critical to make these abundance determinations before the low energy response deteriorates any further. Note that this observation should also allow a calibration of the XIS response below the carbon edge to ~20%. | GALACTIC DIFFUSE EMISSION | 5 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | HIGH LATTITUDE DIFFUSE A & B | XIS | N |
| HIGH LAT. DIFFUSE B | 38.7468 | -52.2774 | 272.40280946 | -58.27300774 | 280.6379 | 53783.933900463 | 53786.5211111111 | 500027020 | 103553 | 100000 | 103553 | 103561 | 103561 | 103561 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 68609.4 | 68609.4 | 223523.8 | 3 | PROCESSED | 57533.0790972222 | 54247 | 54041.5670717593 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000044 | We propose observing the diffse background at two locations where the low temperature component is particularly string. One of the these enhancement is ostensibly an extension of the local bubble, while the other it is probably due to a region of very bright emission in the halo (z> 400 pc). We can verify the thermal nature of these sources, and look for CNO abyndance ratio differences between local disk and halo gas. It is critical to make these abundance determinations before the low energy response deteriorates any further. Note that this observation should also allow a calibration of the XIS response below the carbon edge to ~20%. | GALACTIC DIFFUSE EMISSION | 5 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | HIGH LATTITUDE DIFFUSE A & B | XIS | N |
| VICINITY OF LMC X-3 | 83.4844 | -63.8863 | 273.3865557 | -32.64248934 | 284.6189 | 53811.6008333333 | 53813.9168055556 | 500031010 | 82018.5 | 80000 | 82026.5 | 82018.5 | 82026.5 | 82026.5 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 74614.8 | 74614.8 | 200063.9 | 2 | PROCESSED | 57533.2849537037 | 54247 | 54056.4806828704 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 000043 | We propose to observe the vicnity of LMC X-3 for 80 ks. We expectt to determine the OVII and OVIII emission line intensities within 20% errors. Combining these results with the OVII and OVIII absorption lines observed in the energy spectra of LMC X-3 with Chandra LETG-HRC, we can determine the geometrocal extent od the hot gas along the line-of-sight direction. This will answer the long-unanswered question; from where the high lattitude OVII/OVIII emissions come ? | GALACTIC DIFFUSE EMISSION | 5 | A | SWG | NULL | NULL | NULL | JAP | 0 | SWG | VICINITY OF LMC X-3 | XIS | N |
| SKY_50.0_-62.4 | 50.0507 | -62.4328 | 278.67600391 | -47.08169247 | 281.591 | 53795.7055671296 | 53796.9369675926 | 501001010 | 80145 | 80000 | 80153 | 80145 | 80153 | 80145 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 74012.2 | 74012.2 | 106376 | 0 | PROCESSED | 57533.1282638889 | 54401 | 53905.6164930556 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011252 | We propose Suzaku XIS observations of the hot gas in the Galactic halo and Local Bubble. The spectra's bright emission lines and complexes will reveal the plasma's ionization history and thus its origins. The Local Bubble's spectrum will be garnered from an observation of a nearby opaque cloud. The halo's spectrum will be found by subtracting the Local Bubble spectrum from that of an adjacent off-cloud observation. In order to better constrain the models, we will also draw upon existing FUSE O VI emission data for these directions. With the combined O VI and soft X-ray data, we will be able to constrain the plasma's conditions and ionization history and, thus, constrain detailed models of the hot gas in the halo and Local Bubble. | GALACTIC DIFFUSE EMISSION | 5 | A | SHELTON | ROBIN | NULL | NULL | USA | 1 | AO1 | SUZAKU XIS OBSERVATIONS OF THE GALACTIC HALO AND LOCAL BUBBLE | XIS | N |
| SKY_53.3_-63.4 | 53.24 | -63.4549 | 278.62179386 | -45.30780651 | 286.1724 | 53797.8694444444 | 53800.3342476852 | 501002010 | 101475.2 | 100000 | 101475.2 | 101475.2 | 101475.2 | 101475.2 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 145431.8 | 145431.8 | 212853.9 | 4 | PROCESSED | 57533.1863425926 | 54401 | 53906.7729282407 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011252 | We propose Suzaku XIS observations of the hot gas in the Galactic halo and Local Bubble. The spectra's bright emission lines and complexes will reveal the plasma's ionization history and thus its origins. The Local Bubble's spectrum will be garnered from an observation of a nearby opaque cloud. The halo's spectrum will be found by subtracting the Local Bubble spectrum from that of an adjacent off-cloud observation. In order to better constrain the models, we will also draw upon existing FUSE O VI emission data for these directions. With the combined O VI and soft X-ray data, we will be able to constrain the plasma's conditions and ionization history and, thus, constrain detailed models of the hot gas in the halo and Local Bubble. | GALACTIC DIFFUSE EMISSION | 5 | A | SHELTON | ROBIN | NULL | NULL | USA | 1 | AO1 | SUZAKU XIS OBSERVATIONS OF THE GALACTIC HALO AND LOCAL BUBBLE | XIS | N |
| M17 | 275.2076 | -16.1829 | 15.0906551 | -0.7606192 | 110.1996 | 53805.8263425926 | 53808.5349421296 | 501003010 | 102702.1 | 100000 | 102710.1 | 102710.1 | 102702.1 | 102710.1 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 92566.1 | 92566.1 | 233967.8 | 4 | PROCESSED | 57533.2492939815 | 54394 | 53905.822662037 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010066 | Recent Chandra observations discovered that HII regions possess a few MK extended plasma, but the origin of the emission is still unknown. We propose to observe M17, which has the most spectacular sample of such emission. A superb soft-band response of XIS will enable us to measure the strengths of O and N emission lines, giving us strong arguments to elucidate the cause of the emission. A 300 ks Chandra observation is planned this year in addition to the existing 40 ks data, which will help us to discriminate the point source contribution. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 1 | AO1 | XIS INVESTIGATION FOR THE ORIGIN OF DIFFUSE X-RAY EMISSION IN GALACTIC H II REGIONS | XIS | N |
| DRACO HVC REGION A | 243.9602 | 60.0594 | 91.20688798 | 42.38144862 | 79.8192 | 53814.6161111111 | 53816.0050578704 | 501004010 | 61179.8 | 60000 | 61179.8 | 61179.8 | 61179.8 | 61179.8 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 61230.1 | 61230.1 | 119987.9 | 2 | PROCESSED | 57533.2956481482 | 54394 | 53906.0459722222 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010069 | High-Velocity Clouds (HVCs) are HI cloud at high Galactic latitude which cannot be in circular rotation about the Galactic Center. The distance to the HVCs can be anywhere between 1kpc and 1Mpc. ROSAT detected X-ray nebula at the edge of the Draco HVC 90.5+42.5-130, suggesting that the HVC is encountering the galactic disk and its kinetic energy is transferred into heat of the X-ray nebula. But it is still debatable due to the poor spectral information. With Suzaku, we determine the physical state the nebula, exam whether it is associated with the HVC and investigate the origin. | GALACTIC DIFFUSE EMISSION | 5 | A | TSURU | TAKESHI | NULL | NULL | JAP | 1 | AO1 | SUZAKU OBSERVATION OF HIGH-VELOCITY CLOUD: - ESTABLISHING A NEW CLASS OF DIFFUSE X-RAY EMISSION SOURCE - | XIS | N |
| DRACO HVC REGION B | 243.9603 | 59.1738 | 90.07720195 | 42.68363475 | 80.282 | 53816.0059953704 | 53817.4148611111 | 501005010 | 61632 | 60000 | 61644.7 | 61644 | 61632 | 61636 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 60686.5 | 60686.5 | 121709.9 | 2 | PROCESSED | 57533.3166319444 | 54400 | 53906.4964583333 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010069 | High-Velocity Clouds (HVCs) are HI cloud at high Galactic latitude which cannot be in circular rotation about the Galactic Center. The distance to the HVCs can be anywhere between 1kpc and 1Mpc. ROSAT detected X-ray nebula at the edge of the Draco HVC 90.5+42.5-130, suggesting that the HVC is encountering the galactic disk and its kinetic energy is transferred into heat of the X-ray nebula. But it is still debatable due to the poor spectral information. With Suzaku, we determine the physical state the nebula, exam whether it is associated with the HVC and investigate the origin. | GALACTIC DIFFUSE EMISSION | 5 | A | TSURU | TAKESHI | NULL | NULL | JAP | 1 | AO1 | SUZAKU OBSERVATION OF HIGH-VELOCITY CLOUD: - ESTABLISHING A NEW CLASS OF DIFFUSE X-RAY EMISSION SOURCE - | XIS | N |
| IC 443 | 94.2975 | 22.7757 | 188.8694635 | 3.11574616 | 274.0004 | 54165.4446643518 | 54166.5154398148 | 501006010 | 42011.3 | 40000 | 42011.3 | 42012.9 | 0 | 42020.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34693.4 | 34693.4 | 92509.9 | 2 | PROCESSED | 57537.6197337963 | 54736 | 54174.6613541667 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010040 | IC~443, a prototypical mixed-morphology SNR, was reported to have over-ionization plasma, in which the ionization temperature of some elements are significantly higher than the electron (i.e. continuum) temperature, and suggested that this is the key to explain how to make the morphology and there could be another phase of SNR evolution. | GALACTIC DIFFUSE EMISSION | 5 | B | OZAKI | MASANOBU | NULL | NULL | JAP | 1 | AO1 | UNIFIED MODEL OF SHELL-LIKE AND MM-SNRS AND A NEW STAGE OF EVOLUTION | XIS | Y |
| IC 443 | 94.2972 | 22.4797 | 189.13057055 | 2.97563306 | 274.0001 | 54166.5158680556 | 54167.612025463 | 501006020 | 44013.5 | 40000 | 44013.5 | 44037.5 | 0 | 44021.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36320.9 | 36320.9 | 94699.9 | 1 | PROCESSED | 57537.6255324074 | 54736 | 54172.2247800926 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010040 | IC~443, a prototypical mixed-morphology SNR, was reported to have over-ionization plasma, in which the ionization temperature of some elements are significantly higher than the electron (i.e. continuum) temperature, and suggested that this is the key to explain how to make the morphology and there could be another phase of SNR evolution. | GALACTIC DIFFUSE EMISSION | 5 | B | OZAKI | MASANOBU | NULL | NULL | JAP | 1 | AO1 | UNIFIED MODEL OF SHELL-LIKE AND MM-SNRS AND A NEW STAGE OF EVOLUTION | XIS | Y |
| CTB 37B | 258.4918 | -38.2006 | 348.64561092 | 0.37683278 | 270.1267 | 53974.0604976852 | 53976.2398032407 | 501007010 | 82815.1 | 80000 | 82871.1 | 82815.1 | 82879.1 | 82863.1 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 68860.3 | 68860.3 | 188277.9 | 2 | PROCESSED | 57535.4428703704 | 54526 | 54053.4840162037 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010042 | The Galactic Plane Survey with HESS found several new TeV sources, called as "dark particle accelerators". They must be powerful cosmic-ray accelerators, although their origin is still unknown due to the lack of information in other wavelengths. We investigate one of the extended sample with radio SNR counterpart, CTB 37B, which is marginally detected on the edge of ASCA GIS. ASCA spectrum shows rather soft power-law feature, indicating that there are both thermal and non-thermal X-ray emission. With the low background of XISs and HXD, parameters of both components are determined with 80 ks exposure. The non-thermal component suggests the new sample of accelerators, and the thermal compopent reveals the condition of the proton acceleration site, for the first time. | GALACTIC DIFFUSE EMISSION | 5 | A | BAMBA | AYA | NULL | NULL | JAP | 1 | AO1 | UNCOVERING THE NATURE OF DARK PARTICLE ACCELERATORS | XIS | N |
| GC SOUTH | 266.5016 | -29.1694 | 359.84485124 | -0.1935349 | 265.0006 | 54004.5960185185 | 54007.8925231482 | 501008010 | 129577.3 | 130000 | 129577.3 | 129577.3 | 129577.3 | 129577.3 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 111259.1 | 111259.1 | 284803.8 | 5 | PROCESSED | 57535.7712731482 | 54744 | 54021.0929050926 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010044 | Past X-ray observations have discovered diffuse X-rays extended within a hundred parsec of the Galactic center (GC) region. Moreover, Suzaku PV observation indicates that the diffuse X-rays can well be explained by a thermal emission from hot(8 keV) plasma. The most plausible energy injection sources are the multiple SNe. The huge thermal energy (10^47 J) and short timescale (10^5 yr) of the hot plasma suggest that the GC region harbors at least 10 young SNRs. To confirm the scenario, we propose to observe two SNR candidates at the south of the GC with a single pointing. One exhibits a non-thermal shell-like X-ray SNR feature, and the other shows a thin-thermal SNR feature. We also propose to observe the symmetric position with respect to the Galactic plane for the background estimation. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 1 | AO1 | SUZAKU OBSERVATIONS OF G359.79-0.26 AND G359.92-0.09: THERMAL AND NONTHERMAL SUPERNOVA REMNANTS NEAR THE GALACTIC CENTER | XIS | Y |
| GC SOUTH BGD | 266.1893 | -28.9082 | 359.92534776 | 0.17564926 | 265.0003 | 54007.8931365741 | 54009.2884143518 | 501009010 | 51190 | 50000 | 51198 | 51206 | 51190 | 51198 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 47715.7 | 47715.7 | 120547.9 | 0 | PROCESSED | 57535.7087847222 | 54735 | 54020.9371064815 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010044 | Past X-ray observations have discovered diffuse X-rays extended within a hundred parsec of the Galactic center (GC) region. Moreover, Suzaku PV observation indicates that the diffuse X-rays can well be explained by a thermal emission from hot(8 keV) plasma. The most plausible energy injection sources are the multiple SNe. The huge thermal energy (10^47 J) and short timescale (10^5 yr) of the hot plasma suggest that the GC region harbors at least 10 young SNRs. To confirm the scenario, we propose to observe two SNR candidates at the south of the GC with a single pointing. One exhibits a non-thermal shell-like X-ray SNR feature, and the other shows a thin-thermal SNR feature. We also propose to observe the symmetric position with respect to the Galactic plane for the background estimation. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 1 | AO1 | SUZAKU OBSERVATIONS OF G359.79-0.26 AND G359.92-0.09: THERMAL AND NONTHERMAL SUPERNOVA REMNANTS NEAR THE GALACTIC CENTER | XIS | Y |
| HESS J1745-303 | 266.2629 | -30.3722 | 358.71029443 | -0.64354718 | 263.6011 | 54015.0950462963 | 54016.4300810185 | 501010010 | 50670.7 | 50000 | 50670.7 | 50670.7 | 50670.7 | 50670.7 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 45689.7 | 45689.7 | 115311.9 | 1 | PROCESSED | 57535.8009837963 | 54526 | 54021.698587963 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010046 | So far, the evidence for hadron acceleration up to near the knee energy has not yet obtained. Recent galactic plane survey in the TeV gamma-ray band reveals several new unidentified sources like HESS J1745-303. It is extended, hence likely a supernova remnant. Also it coincides with an EGRET unidentified source (3EG J1744-3011), which may suggest that it is a source of accelerated protons. However, HESS J1745-303 shows rather hard spectrum that cannot be explained by the simplest version of the diffusive shock acceleration model. X-ray study on HESS J1745-303 is necessary for further discussions. We might find that observed data requires modification of the common picture that young supernova remnants are the dominant source of high-energy protons. | GALACTIC DIFFUSE EMISSION | 5 | A | YAMAZAKI | RYO | NULL | NULL | JAP | 1 | AO1 | X-RAY STUDY ON THE TEV UNIDENTIFIED SOURCE HESS J1745-303 | XIS | N |
| G344.7-0.1 | 255.9588 | -41.7032 | 344.67682908 | -0.15577285 | 89.2821 | 54152.1890393518 | 54153.2919097222 | 501011010 | 42133.6 | 40000 | 42133.6 | 42133.6 | 0 | 42133.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34201.6 | 34201.6 | 95280 | 1 | PROCESSED | 57537.4329050926 | 54777 | 54158.2352662037 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010050 | We propose an observation of a supernova remnant (SNR) G344.7-0.1 with Suzaku. In addition to emission lines from highly ionized ions (Si, S, and so on), we found a strong emission line at 6.4 keV in the spectra obtained with ASCA and XMM-Newton. This line is thought to be a K-line from the low-ionized Fe, but the origin is still unknown. Precise measurements of the line energy and the spectral parameters with the XIS will provide us with understanding the origin of the Fe-K line and the physical process in the SNR. | GALACTIC DIFFUSE EMISSION | 5 | C | YAMAUCHI | SHIGEO | NULL | NULL | JAP | 1 | AO1 | SUZAKU OBSERVATION OF G344.7-0.1 | XIS | Y |
| CYGNUS_LOOP_P1 | 313.519 | 31.9657 | 75.41990185 | -8.25713566 | 240 | 54417.6059259259 | 54418.0904976852 | 501012010 | 16738.5 | 10000 | 16738.5 | 16748.9 | 0 | 16742.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15775.8 | 15775.8 | 41860 | 1 | PROCESSED | 57540.5110648148 | 54798 | 54430.2159375 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | Y |
| CYGNUS_LOOP_P2 | 313.2729 | 31.7708 | 75.13379207 | -8.21853117 | 240.0005 | 54418.0909722222 | 54418.4168865741 | 501013010 | 16379.9 | 10000 | 16387.9 | 16387.9 | 0 | 16379.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10978.6 | 10978.6 | 28151.9 | 0 | PROCESSED | 57540.5114351852 | 54798 | 54430.1915972222 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | Y |
| CYGNUS_LOOP_P3 | 313.0409 | 31.565 | 74.84662265 | -8.19493741 | 240.0003 | 54418.4174074074 | 54418.9377083333 | 501014010 | 16764.8 | 12000 | 16781.2 | 16780.8 | 0 | 16764.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14696.2 | 14696.2 | 44943.9 | 0 | PROCESSED | 57540.5210069445 | 54798 | 54430.2624884259 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | Y |
| CYGNUS_LOOP_P4 | 312.8083 | 31.361 | 74.56035476 | -8.16867105 | 239.9997 | 54418.9382291667 | 54419.3196643518 | 501015010 | 18279 | 15000 | 18287 | 18279 | 0 | 18287 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 14286 | 14286 | 32943.9 | 0 | PROCESSED | 57540.5253935185 | 54798 | 54430.2398726852 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | Y |
| CYGNUS_LOOP_P5 | 312.5567 | 31.1701 | 74.2739834 | -8.12038976 | 239.9995 | 54419.3201388889 | 54420.0627777778 | 501016010 | 28406.2 | 22000 | 28406.2 | 28406.2 | 0 | 28406.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25370 | 25370 | 64155.9 | 1 | PROCESSED | 57540.538900463 | 54798 | 54430.4318865741 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | Y |
| CYGNUS_LOOP_P6 | 312.3057 | 30.9823 | 73.99029438 | -8.06939848 | 240.0003 | 54415.3923032407 | 54416.1668287037 | 501017010 | 28704.9 | 22000 | 28704.9 | 28704.9 | 0 | 28704.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 26887.8 | 26887.8 | 66911.9 | 0 | PROCESSED | 57540.490474537 | 54798 | 54430.18875 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | Y |
| CYGNUS_LOOP_P7 | 312.0838 | 30.7678 | 73.70103145 | -8.0534172 | 239.9966 | 54416.1673032407 | 54416.7223263889 | 501018010 | 24154.5 | 22000 | 24154.5 | 24154.5 | 0 | 24154.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18861 | 18861 | 47920 | 0 | PROCESSED | 57540.4878587963 | 54798 | 54430.1343287037 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | Y |
| CYGNUS_LOOP_P9 | 311.8173 | 30.594 | 73.41991066 | -7.98099126 | 239.9998 | 54416.7228935185 | 54417.2502199074 | 501019010 | 19565.6 | 15000 | 19565.6 | 19565.6 | 0 | 19565.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17344.6 | 17344.6 | 45537.9 | 0 | PROCESSED | 57540.4965393518 | 54798 | 54430.2327546296 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | Y |
| CYGNUS_LOOP_P10 | 311.5744 | 30.3992 | 73.13474548 | -7.93635975 | 240.0007 | 54417.2506944444 | 54417.6043402778 | 501020010 | 16795.8 | 10000 | 16795.8 | 16819.8 | 0 | 16803.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12672.9 | 12672.9 | 30549.9 | 0 | PROCESSED | 57540.5008333333 | 54798 | 54430.1578472222 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | Y |
| CYGNUS_LOOP_P8 | 313.9965 | 31.4722 | 75.29540263 | -8.88432445 | 62.5181 | 53868.0059837963 | 53868.1717476852 | 501028010 | 4870.6 | 6000 | 4870.6 | 4870.6 | 4870.6 | 4870.6 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 2328 | 2328 | 14316 | 0 | PROCESSED | 57534.2851736111 | 54394 | 53914.3326157407 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | N |
| CYGNUS_LOOP_P12 | 313.7421 | 31.2725 | 74.99964096 | -8.84356964 | 62.1405 | 53864.7943055556 | 53865.1391087963 | 501029010 | 13542.6 | 10000 | 13542.6 | 13542.6 | 13542.6 | 13542.6 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 2156.7 | 2156.7 | 29780 | 1 | PROCESSED | 57534.2604166667 | 54394 | 53914.0447916667 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | N |
| CYGNUS_LOOP_P13 | 313.4901 | 31.0708 | 74.70349314 | -8.80441033 | 68.2467 | 53865.1416666667 | 53865.5321643518 | 501030010 | 17073 | 17000 | 17073 | 17081 | 17089 | 17089 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 14269 | 14269 | 33727.9 | 0 | PROCESSED | 57534.2605092593 | 54394 | 53914.0847569444 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | N |
| CYGNUS_LOOP_P14 | 313.2365 | 30.8681 | 74.40554659 | -8.76356285 | 62.362 | 53867.6311111111 | 53868.0050462963 | 501031010 | 18580.9 | 18000 | 18580.9 | 18580.9 | 18580.9 | 18580.9 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 12737.8 | 12737.8 | 32297.9 | 0 | PROCESSED | 57534.275775463 | 54394 | 53914.3142476852 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | N |
| CYGNUS_LOOP_P15 | 312.9857 | 30.6621 | 74.106397 | -8.72540127 | 61.9987 | 53880.177974537 | 53880.6716898148 | 501032010 | 20728.9 | 21000 | 20728.9 | 20728.9 | 20728.9 | 20728.9 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 17476 | 17476 | 42634.9 | 0 | PROCESSED | 57534.4101041667 | 54394 | 53926.2440046296 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | N |
| CYGNUS_LOOP_P16 | 312.737 | 30.4592 | 73.81069789 | -8.68546284 | 61.9998 | 53877.1905439815 | 53877.7605671296 | 501033010 | 23337.5 | 22000 | 23369.5 | 23337.5 | 23369.5 | 23369.5 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 20118.4 | 20118.4 | 49243.9 | 2 | PROCESSED | 57534.3873611111 | 54398 | 53926.8416319445 | 3.0.22.43 | 6 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | N |
| CYGNUS_LOOP_P17 | 312.199 | 30.014 | 73.16561663 | -8.59879153 | 61.9999 | 53877.7613657407 | 53878.0446064815 | 501034010 | 14195.3 | 14000 | 14199.3 | 14203.3 | 14199.3 | 14195.3 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 14823.1 | 14823.1 | 24464 | 0 | PROCESSED | 57534.3944328704 | 54394 | 53926.1395833333 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | N |
| CYGNUS_LOOP_P18 | 312.0547 | 29.7111 | 72.84665082 | -8.68804998 | 237.4994 | 54087.0528819444 | 54087.3405208333 | 501035010 | 12011 | 13000 | 12915 | 12011 | 0 | 12907 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11439.4 | 11439.4 | 24835.9 | 3 | PROCESSED | 57536.3543981482 | 54750 | 54096.4390972222 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | Y |
| CYGNUS_LOOP_P19 | 311.8094 | 30.0818 | 73.00862935 | -8.2918477 | 237.4997 | 54087.3411805556 | 54087.8245833333 | 501036010 | 18595 | 17000 | 18595 | 18595 | 0 | 18595 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18355 | 18355 | 41755.9 | 0 | PROCESSED | 57536.3627199074 | 54744 | 54096.1443171296 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010052 | We propose to observe a large part of the Cygnus Loop. The objective is to study the plasma of C and N that can not be measured without the BI of the XIS. The limb regoin showing C and N lines as well as O line. The central part showing strong Si and S lines is believed to be a fossil of the explosion. The fossil contains quite a lot of metal with relatively low density. Studying the C and N lines, we can evaluate O lines from the central part of the Loop. The observation should be done as soon as possible before C and N lines can not be seen due to the degradation of the XIS. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 1 | AO1 | OBSERVATION OF THE CYGNUS LOOP | XIS | Y |
| RCW 86 | 221.2555 | -62.3618 | 315.68741681 | -2.33681001 | 278.3377 | 53959.4574652778 | 53961.1294907407 | 501037010 | 59805.4 | 60000 | 59829.4 | 59805.4 | 59829.4 | 59821.4 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 54405 | 54405 | 144420 | 1 | PROCESSED | 57535.2984259259 | 54394 | 54021.0740972222 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010054 | We propose an observation of the Northwest region of RCW 86, one of Galactic supernova remnants (SNRs). Hard X-ray continuum of RCW 86 is accompanied by Fe K line emission at 6.4keV. There is strong possibility that the origin of this line is electrons and protons accelerated in the shell of the SNR. In PV phase, the Southeast region of RCW 86 will be observed, and the density of this region is much larger than that of the Northwest region. Therefore we must compare the fluxes of Fe line and hard continuum of both regions, and discuss the correlation between the flux and the density of emitting region. Such comparative study is very useful for understanding the particle acceleration in the shell-like SNRs. | GALACTIC DIFFUSE EMISSION | 5 | B | YAMAGUCHI | HIROYA | NULL | NULL | JAP | 1 | AO1 | RCW 86:PECULIAR SNR WITH NEUTRAL FE K LINE | XIS | N |
| GC_SGR_B_EAST | 267.0203 | -28.3518 | 0.77973231 | -0.1584432 | 71.8708 | 54162.5141203704 | 54164.5273726852 | 501039010 | 96401.8 | 100000 | 96401.8 | 96401.8 | 0 | 96401.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 91082.9 | 91082.9 | 173931.8 | 3 | PROCESSED | 57537.6522800926 | 54736 | 54171.4429050926 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010060 | We detected discrete structures of 6.4-keV and 6.7-keV line with the deep observation of Sgr B. These structures are candidate of X-ray reflection nebula and supernova remnant, respectively. Both targets imply the past activities in the Galactic center region: AGN, star burst, or something else. To verify these origin, we propose extensional observation around the Sgr B region. We also investigate metal abundances in the Galactic center by using line intensity ratio at the SNR. | GALACTIC DIFFUSE EMISSION | 5 | B | KOYAMA | KATSUJI | NULL | NULL | JAP | 1 | AO1 | OBSERVATIONS OF SNR/XRN CANDIDATES NEAR THE SGR B REGION | XIS | Y |
| GC_SGR_B_NORTH | 266.6958 | -28.383 | 0.60519276 | 0.06967717 | 271.4415 | 53999.7284837963 | 54001.2863425926 | 501040010 | 61375.3 | 62000 | 61391.3 | 61375.3 | 61383.3 | 61391.3 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 53867 | 53867 | 134581.8 | 2 | PROCESSED | 57535.7042361111 | 54735 | 54021.2828472222 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010060 | We detected discrete structures of 6.4-keV and 6.7-keV line with the deep observation of Sgr B. These structures are candidate of X-ray reflection nebula and supernova remnant, respectively. Both targets imply the past activities in the Galactic center region: AGN, star burst, or something else. To verify these origin, we propose extensional observation around the Sgr B region. We also investigate metal abundances in the Galactic center by using line intensity ratio at the SNR. | GALACTIC DIFFUSE EMISSION | 5 | B | KOYAMA | KATSUJI | NULL | NULL | JAP | 1 | AO1 | OBSERVATIONS OF SNR/XRN CANDIDATES NEAR THE SGR B REGION | XIS | Y |
| GC_SGR_B_NORTH | 266.6955 | -28.3829 | 0.60514127 | 0.06995468 | 271.4417 | 54002.2105555556 | 54003.2919444444 | 501040020 | 44829.5 | 38000 | 44845.5 | 44829.5 | 44837.5 | 44853.5 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 39970.5 | 39970.5 | 93431.9 | 1 | PROCESSED | 57535.678125 | 54744 | 54021.2868055556 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010060 | We detected discrete structures of 6.4-keV and 6.7-keV line with the deep observation of Sgr B. These structures are candidate of X-ray reflection nebula and supernova remnant, respectively. Both targets imply the past activities in the Galactic center region: AGN, star burst, or something else. To verify these origin, we propose extensional observation around the Sgr B region. We also investigate metal abundances in the Galactic center by using line intensity ratio at the SNR. | GALACTIC DIFFUSE EMISSION | 5 | B | KOYAMA | KATSUJI | NULL | NULL | JAP | 1 | AO1 | OBSERVATIONS OF SNR/XRN CANDIDATES NEAR THE SGR B REGION | XIS | Y |
| SNR 0509-67.5 | 77.3855 | -67.5341 | 278.15788525 | -34.58671131 | 68.6442 | 53965.2623032407 | 53966.1640509259 | 501041010 | 51276.2 | 50000 | 51276.2 | 51276.2 | 51276.2 | 51276.2 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 50829.4 | 50829.4 | 77890 | 1 | PROCESSED | 57535.3081365741 | 54526 | 54020.7617592593 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010072 | Hot plasma in young supernova remnants (SNRs) are generally in the state of non-equilibrium ionization (NEI), hence strong L-shell lines of Si, Fe and other elements appear in soft energy band (<1keV). With the observations with Chandra and XMM, quite large ambiguity of ionization age for each element remains because of the limited energy resolution in the soft energy band. Utilizing the supreme energy resolution and background property of Suzaku/XIS, we propose the observation of the youngest type Ia SNR in the LMC, 0509-67.5. We correctly diagnose the NEI plasma of this SNR by determining the ionization age and electron temperature for each element component and constrain the ejecta structure of Type Ia SNR. | GALACTIC DIFFUSE EMISSION | 5 | C | NAKAJIMA | HIROSHI | NULL | NULL | JAP | 1 | AO1 | NEI PLASMA DIAGNOSTICS OF A YOUNG TYPE IA SNR:0509-67.5 | XIS | N |
| HESS J1614-518 | 243.5851 | -51.743 | 331.574855 | -0.5276897 | 283.402 | 53993.6672222222 | 53994.4571064815 | 501042010 | 40177.7 | 50000 | 40185.7 | 40177.7 | 40185.7 | 40185.7 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 43560.7 | 43560.7 | 68227.9 | 0 | PROCESSED | 57535.5776967593 | 54526 | 54020.8545833333 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010073 | We propose to observe unidentified TeV gamma-ray sources. HESS surveyed the Galactic Plane and found new TeV gamma-ray sources. TeV gamma-ray emissions are direct evidence for the presence of high energy particles above TeV, but, nonetheless, many of the new extended sources are very faint in any other wavelength. In fact, we observed HESS J1616-518 in Suzaku PV phase already and found its X-ray flux is quite low compared to its TeV gamma-ray flux. It is appropriate to be called ''Dark Accelerator'' and such objects might mainly contribute to the Galactic Cosmic rays. To detect these ''Dark Accelerators'' in X-ray, we propose to observe other unidentified TeV gamma-ray sources, HESS J1614-518 and HESS J1825-137. | GALACTIC DIFFUSE EMISSION | 5 | B | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | AO1 | SUZAKU OBSERVATIONS OF UNIDENTIFIED TEV GAMMA-RAY SOURECES | XIS | N |
| HESS J1614-518 BG | 242.0174 | -52.4329 | 330.3996927 | -0.37656553 | 291.2192 | 53994.4597569444 | 53995.3015509259 | 501043010 | 43555.4 | 50000 | 43563.4 | 43563.4 | 43555.4 | 43563.4 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 50592.2 | 50592.2 | 72703.9 | 1 | PROCESSED | 57535.5823726852 | 54526 | 54020.8662268518 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010073 | We propose to observe unidentified TeV gamma-ray sources. HESS surveyed the Galactic Plane and found new TeV gamma-ray sources. TeV gamma-ray emissions are direct evidence for the presence of high energy particles above TeV, but, nonetheless, many of the new extended sources are very faint in any other wavelength. In fact, we observed HESS J1616-518 in Suzaku PV phase already and found its X-ray flux is quite low compared to its TeV gamma-ray flux. It is appropriate to be called ''Dark Accelerator'' and such objects might mainly contribute to the Galactic Cosmic rays. To detect these ''Dark Accelerators'' in X-ray, we propose to observe other unidentified TeV gamma-ray sources, HESS J1614-518 and HESS J1825-137. | GALACTIC DIFFUSE EMISSION | 5 | B | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | AO1 | SUZAKU OBSERVATIONS OF UNIDENTIFIED TEV GAMMA-RAY SOURECES | XIS | N |
| HESS J1825-137 | 276.5031 | -13.6997 | 17.87105596 | -0.70261201 | 269.3213 | 54025.8175462963 | 54027.1682291667 | 501044010 | 50293 | 50000 | 50293 | 50293 | 50293 | 50293 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 42955.7 | 42955.7 | 116694 | 1 | PROCESSED | 57535.8789351852 | 54526 | 54055.4418634259 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010073 | We propose to observe unidentified TeV gamma-ray sources. HESS surveyed the Galactic Plane and found new TeV gamma-ray sources. TeV gamma-ray emissions are direct evidence for the presence of high energy particles above TeV, but, nonetheless, many of the new extended sources are very faint in any other wavelength. In fact, we observed HESS J1616-518 in Suzaku PV phase already and found its X-ray flux is quite low compared to its TeV gamma-ray flux. It is appropriate to be called ''Dark Accelerator'' and such objects might mainly contribute to the Galactic Cosmic rays. To detect these ''Dark Accelerators'' in X-ray, we propose to observe other unidentified TeV gamma-ray sources, HESS J1614-518 and HESS J1825-137. | GALACTIC DIFFUSE EMISSION | 5 | B | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | AO1 | SUZAKU OBSERVATIONS OF UNIDENTIFIED TEV GAMMA-RAY SOURECES | XIS | N |
| HESS J1825-137 BG | 276.9022 | -13.2649 | 18.4366217 | -0.84356166 | 269.33 | 54027.1689351852 | 54028.5072337963 | 501045010 | 52144.4 | 50000 | 52152.4 | 52144.4 | 52152.4 | 52144.4 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 42197.4 | 42197.4 | 115607.9 | 2 | PROCESSED | 57535.8869907407 | 54526 | 54055.6591550926 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010073 | We propose to observe unidentified TeV gamma-ray sources. HESS surveyed the Galactic Plane and found new TeV gamma-ray sources. TeV gamma-ray emissions are direct evidence for the presence of high energy particles above TeV, but, nonetheless, many of the new extended sources are very faint in any other wavelength. In fact, we observed HESS J1616-518 in Suzaku PV phase already and found its X-ray flux is quite low compared to its TeV gamma-ray flux. It is appropriate to be called ''Dark Accelerator'' and such objects might mainly contribute to the Galactic Cosmic rays. To detect these ''Dark Accelerators'' in X-ray, we propose to observe other unidentified TeV gamma-ray sources, HESS J1614-518 and HESS J1825-137. | GALACTIC DIFFUSE EMISSION | 5 | B | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | AO1 | SUZAKU OBSERVATIONS OF UNIDENTIFIED TEV GAMMA-RAY SOURECES | XIS | N |
| GALACTIC CENTER | 265.9791 | -28.902 | 359.8343278 | 0.33569605 | 108.8002 | 54169.6271990741 | 54170.1633564815 | 501046010 | 25211 | 25000 | 25227 | 25211 | 0 | 25243 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25008.7 | 25008.7 | 46291.9 | 0 | PROCESSED | 57537.6350925926 | 54736 | 54179.4773842593 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010074 | We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | KOKUBUN | MOTOHIDE | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y |
| GALACTIC CENTER GC2 | 265.779 | -29.1853 | 359.50136289 | 0.33591697 | 108.7998 | 54170.1638773148 | 54170.7946064815 | 501047010 | 25599 | 25000 | 25607 | 25599 | 0 | 25623 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 19088.6 | 19088.6 | 54479.9 | 0 | PROCESSED | 57537.6398611111 | 54736 | 54182.2693865741 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010074 | We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | KOKUBUN | MOTOHIDE | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y |
| GALACTIC CENTER GC3 | 265.5781 | -29.4684 | 359.1684549 | 0.33584661 | 108.8001 | 54170.7951273148 | 54171.3397453704 | 501048010 | 27454.6 | 25000 | 27478.6 | 27454.6 | 0 | 27478.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 24054.8 | 24054.8 | 47047.9 | 1 | PROCESSED | 57537.6483333333 | 54736 | 54182.2788425926 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010074 | We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | KOKUBUN | MOTOHIDE | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y |
| GALACTIC CENTER | 265.3803 | -29.7558 | 358.83357751 | 0.33021849 | 269 | 54016.4324074074 | 54017.0968055556 | 501049010 | 19562.7 | 20000 | 19562.7 | 19562.7 | 19562.7 | 19562.7 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 17633.6 | 17633.6 | 57395.9 | 1 | PROCESSED | 57535.7944675926 | 54735 | 54053.4403356482 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010074 | We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | KOKUBUN | MOTOHIDE | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y |
| GALACTIC CENTER | 265.9089 | -29.649 | 359.16615355 | -0.00387238 | 269 | 54017.0975115741 | 54017.5690277778 | 501050010 | 22047.7 | 20000 | 22047.7 | 22047.7 | 22047.7 | 22047.7 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 18625.6 | 18625.6 | 40735.9 | 0 | PROCESSED | 57535.8013194445 | 54735 | 54053.4127777778 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010074 | We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | KOKUBUN | MOTOHIDE | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y |
| GALACTIC CENTER | 265.7083 | -29.9322 | 358.83372455 | -0.00453222 | 269.0002 | 54017.5695486111 | 54018.2808333333 | 501051010 | 21869 | 20000 | 21877 | 21877 | 21869 | 21877 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 21132.2 | 21132.2 | 61445.9 | 0 | PROCESSED | 57535.8166435185 | 54735 | 54053.5109953704 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010074 | We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | KOKUBUN | MOTOHIDE | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y |
| GALACTIC CENTER | 265.5037 | -30.2156 | 358.49956421 | -0.00336241 | 269.0005 | 54018.2813541667 | 54018.887662037 | 501052010 | 19245.1 | 20000 | 19261.1 | 19261.1 | 19253.1 | 19245.1 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 16046.2 | 16046.2 | 52379.9 | 1 | PROCESSED | 57535.818275463 | 54735 | 54053.5074537037 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010074 | We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | KOKUBUN | MOTOHIDE | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y |
| GALACTIC CENTER | 265.2994 | -30.4982 | 358.16648703 | -0.00302139 | 269.0003 | 54018.8881828704 | 54019.4209953704 | 501053010 | 21908.6 | 20000 | 21908.6 | 21932.1 | 21916.6 | 21916.6 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 19948 | 19948 | 46031.9 | 0 | PROCESSED | 57535.8190393518 | 54735 | 54053.5019675926 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010074 | We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | KOKUBUN | MOTOHIDE | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y |
| GALACTIC CENTER GC9 | 266.6299 | -29.2499 | 359.83430056 | -0.33104727 | 109.8001 | 54171.3410532407 | 54171.9988888889 | 501054010 | 26104.4 | 25000 | 26104.4 | 26104.4 | 0 | 26104.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 23542.4 | 23542.4 | 56829.9 | 0 | PROCESSED | 57537.6542013889 | 54736 | 54182.2954166667 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010074 | We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | KOKUBUN | MOTOHIDE | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y |
| GALACTIC CENTER GC10 | 266.4308 | -29.5343 | 359.50116476 | -0.33080245 | 109.7996 | 54171.9994097222 | 54172.6529976852 | 501055010 | 27225.7 | 25000 | 27225.7 | 27249.7 | 0 | 27233.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21181.9 | 21181.9 | 56453.9 | 0 | PROCESSED | 57537.6665740741 | 54736 | 54182.3161342593 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010074 | We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | KOKUBUN | MOTOHIDE | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y |
| GALACTIC CENTER GC11 | 266.231 | -29.8182 | 359.16839231 | -0.33075371 | 109.7993 | 54172.6536111111 | 54173.2086111111 | 501056010 | 26537.4 | 25000 | 26545.4 | 26545.4 | 0 | 26537.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25278.9 | 25278.9 | 47946 | 0 | PROCESSED | 57537.6702199074 | 54736 | 54182.3328125 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010074 | We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | KOKUBUN | MOTOHIDE | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y |
| GALACTIC CENTER | 266.0341 | -30.1068 | 358.83318764 | -0.33628911 | 269.0002 | 54019.4218402778 | 54020.1446064815 | 501057010 | 20488.4 | 20000 | 20488.4 | 20496.4 | 20496.4 | 20496.4 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 19086 | 19086 | 62437.9 | 0 | PROCESSED | 57535.8262037037 | 54735 | 54053.6059837963 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010074 | We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | KOKUBUN | MOTOHIDE | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y |
| GC SGR D NORTH | 266.9758 | -27.7178 | 1.30220378 | 0.20283685 | 108.7992 | 54173.2100578704 | 54174.7883564815 | 501058010 | 63242.2 | 63000 | 63250.2 | 63242.2 | 0 | 63258.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51147.9 | 51147.9 | 136351.9 | 0 | PROCESSED | 57537.7302546296 | 54735 | 54182.440462963 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010074 | We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | KOKUBUN | MOTOHIDE | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y |
| GC SGR D | 267.0913 | -27.9356 | 1.16847417 | 0.00287016 | 108.7996 | 54174.7887847222 | 54176.2127199074 | 501059010 | 62237.2 | 63000 | 62237.2 | 62245.2 | 0 | 62245.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 54369.7 | 54369.7 | 123028 | 0 | PROCESSED | 57537.7233912037 | 54736 | 54185.4865740741 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010074 | We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | KOKUBUN | MOTOHIDE | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y |
| GC SGR D EAST | 267.2856 | -27.6502 | 1.50163715 | 0.00269695 | 108.7997 | 54176.2132407407 | 54177.8737731482 | 501060010 | 64795.3 | 63000 | 64795.3 | 64826.7 | 0 | 64811.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 54629.7 | 54629.7 | 143465.9 | 1 | PROCESSED | 57537.7151851852 | 54736 | 54185.4429050926 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010074 | We propose mapping observations of the Galactic center of 20ksx12 + 50ksx3 in total. The main purpose is to clarify an existence of the non-thermal emission component associated with the Galactic diffuse X-ray emission and to investigate the longitudinal and latitudinal variations of the brightness, index of the spectrum, and the luminosity ratio to the thermal emission. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | KOKUBUN | MOTOHIDE | JAP | 1 | AO1 | MAPPING OBSERVATION OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y |
| RXJ1713-3946 | 257.9704 | -39.5791 | 347.29183097 | -0.10508063 | 267.9995 | 53989.172025463 | 53989.5306365741 | 501063010 | 18422 | 20000 | 18422 | 18422 | 18422 | 18422 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 17759.7 | 17759.7 | 30971.9 | 1 | PROCESSED | 57535.5249537037 | 54526 | 54021.1086458333 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010158 | We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKAHASHI | TADAYUKI | NULL | NULL | JAP | 1 | AO1 | HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 | HXD | N |
| RXJ1713-3946 | 258.1633 | -39.7281 | 347.25895477 | -0.31287235 | 268.0002 | 53989.5311574074 | 53989.9216898148 | 501064010 | 21322 | 20000 | 21322 | 21322 | 21322 | 21322 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 23030.6 | 23030.6 | 33727.9 | 0 | PROCESSED | 57535.5353356482 | 54526 | 54020.8109027778 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010158 | We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKAHASHI | TADAYUKI | NULL | NULL | JAP | 1 | AO1 | HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 | HXD | N |
| RXJ1713-3946 | 258.1672 | -39.4231 | 347.50735004 | -0.13585591 | 267.9988 | 53989.9221643518 | 53990.3106712963 | 501065010 | 22011 | 20000 | 22011 | 22011 | 22011 | 22011 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 20797.3 | 20797.3 | 33557.9 | 0 | PROCESSED | 57535.5534606482 | 54526 | 54020.8390162037 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010158 | We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKAHASHI | TADAYUKI | NULL | NULL | JAP | 1 | AO1 | HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 | HXD | N |
| RXJ1713-3946 | 257.7744 | -39.7271 | 347.08325974 | -0.07081205 | 268.0001 | 53990.3113310185 | 53990.7106944444 | 501066010 | 20920.7 | 20000 | 20940.7 | 20920.7 | 20926 | 20944.7 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 20699 | 20699 | 34504 | 1 | PROCESSED | 57535.5600347222 | 54526 | 54020.8077546296 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010158 | We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKAHASHI | TADAYUKI | NULL | NULL | JAP | 1 | AO1 | HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 | HXD | N |
| RXJ1713-3946 | 257.7765 | -39.428 | 347.32530765 | 0.10490445 | 268.0003 | 53990.7111689815 | 53991.0488888889 | 501067010 | 21179.6 | 20000 | 21187.6 | 21179.6 | 21193.1 | 21195.6 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 21986.1 | 21986.1 | 29167.9 | 0 | PROCESSED | 57535.5530902778 | 54526 | 54020.8250925926 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010158 | We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKAHASHI | TADAYUKI | NULL | NULL | JAP | 1 | AO1 | HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 | HXD | N |
| RXJ1713-3946 | 258.5534 | -39.7289 | 347.43430559 | -0.55631777 | 267.9997 | 53991.0497337963 | 53991.4460300926 | 501068010 | 21001.5 | 20000 | 21017.5 | 21009.5 | 21001.5 | 21025.5 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 21209.3 | 21209.3 | 34233.9 | 1 | PROCESSED | 57535.5599537037 | 54526 | 54021.2424537037 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010158 | We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKAHASHI | TADAYUKI | NULL | NULL | JAP | 1 | AO1 | HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 | HXD | N |
| RXJ1713-3946 | 258.5524 | -39.4291 | 347.6770378 | -0.38034705 | 267.9999 | 53997.5713773148 | 53997.9140509259 | 501069010 | 18375 | 20000 | 18375 | 18375 | 18375 | 18375 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 14276.7 | 14276.7 | 29599.9 | 0 | PROCESSED | 57535.6332060185 | 54526 | 54021.1502546296 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010158 | We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKAHASHI | TADAYUKI | NULL | NULL | JAP | 1 | AO1 | HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 | HXD | N |
| RXJ1713-3946 | 258.5527 | -40.0289 | 347.19063141 | -0.73133412 | 268.0015 | 53997.9147569444 | 53998.4425925926 | 501070010 | 20744.2 | 20000 | 20744.2 | 20752.2 | 20752.2 | 20752.2 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 22026.6 | 22026.6 | 45595.9 | 1 | PROCESSED | 57535.6347685185 | 54526 | 54021.1763541667 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010158 | We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKAHASHI | TADAYUKI | NULL | NULL | JAP | 1 | AO1 | HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 | HXD | N |
| RXJ1713-3946 | 258.942 | -39.4278 | 347.8535904 | -0.62405701 | 268.0013 | 53998.4433912037 | 53998.8467476852 | 501071010 | 21174.1 | 20000 | 21174.1 | 21198.1 | 21190.1 | 21182.1 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 18338.7 | 18338.7 | 34839.9 | 0 | PROCESSED | 57535.634537037 | 54526 | 54020.8878009259 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010158 | We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKAHASHI | TADAYUKI | NULL | NULL | JAP | 1 | AO1 | HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 | HXD | N |
| RXJ1713-3946 | 258.9408 | -39.7267 | 347.60984156 | -0.7970823 | 268.0009 | 54013.3138541667 | 54013.877974537 | 501072010 | 19981.7 | 20000 | 19981.7 | 19981.7 | 19981.7 | 19981.7 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 16299.7 | 16299.7 | 48718 | 1 | PROCESSED | 57535.7676736111 | 54526 | 54021.6599652778 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010158 | We propose mapping observations of the bright hard X-ray/TeV SNR RXJ1713-3946. 10 x 20 ks observations are performed. Main perpose is to derive an acuurate hard X-ray spectra up to 50 keV based on results of PV observations. This allows us to solve the origin of strong correlation between X-ray and TeV gamma-ray images and also to understand the particle acceleration in this SNR. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKAHASHI | TADAYUKI | NULL | NULL | JAP | 1 | AO1 | HARD X-RAY MAPPING OBSERVATIONS OF THE BRIGHT HARD X-RAY/TEV SNR RXJ1713-3946 | HXD | N |
| G156.2+5.7E | 75.8128 | 51.6405 | 156.70319129 | 6.10796494 | 274.6638 | 54149.9177893518 | 54151.1750231482 | 501074010 | 53333.1 | 50000 | 53349.4 | 53349.1 | 0 | 53333.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 50821.8 | 50821.8 | 108619.9 | 2 | PROCESSED | 57537.4302893518 | 54773 | 54158.2839583333 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011235 | G156.2+5.7 (RX J04591+5147) is thought to be a 26,000 yr old Type Ia remnant expanding in a low density medium. Ginga and ASCA observations reveal a hard emission component, interpreted as arising from shock-accelerated electrons, making this the oldest SNR in which shock acceleration has been found. Recent reanalysis of the ASCA data leaves ambiguity about the existence of this component. The importance of understanding the evolution of shock acceleration in SNRs makes vital confirming the existence of the hard component and localizing it. We propose 50 ks XIS observations of 3 locations to localize the hard component. Given its angular size, lack of small high contrast features, 0.4 keV thermal component with strong lines, and hard component, G156.2+5.7 is an ideal Suzaku target. | GALACTIC DIFFUSE EMISSION | 5 | C | PETRE | ROBERT | NULL | NULL | USA | 1 | AO1 | A SEARCH FOR HARD X-RAY EMISSION FROM THE EVOLVED SNR G156.2+5.7 | XIS | Y |
| G156.2+5.7NW | 74.223 | 52.4174 | 155.48379099 | 5.80912082 | 273.883 | 54147.6530902778 | 54148.7558333333 | 501075010 | 50546.8 | 50000 | 50546.8 | 50546.8 | 0 | 50546.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46195.8 | 46195.8 | 95259.9 | 0 | PROCESSED | 57537.3885763889 | 54695 | 54153.2775 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011235 | G156.2+5.7 (RX J04591+5147) is thought to be a 26,000 yr old Type Ia remnant expanding in a low density medium. Ginga and ASCA observations reveal a hard emission component, interpreted as arising from shock-accelerated electrons, making this the oldest SNR in which shock acceleration has been found. Recent reanalysis of the ASCA data leaves ambiguity about the existence of this component. The importance of understanding the evolution of shock acceleration in SNRs makes vital confirming the existence of the hard component and localizing it. We propose 50 ks XIS observations of 3 locations to localize the hard component. Given its angular size, lack of small high contrast features, 0.4 keV thermal component with strong lines, and hard component, G156.2+5.7 is an ideal Suzaku target. | GALACTIC DIFFUSE EMISSION | 5 | C | PETRE | ROBERT | NULL | NULL | USA | 1 | AO1 | A SEARCH FOR HARD X-RAY EMISSION FROM THE EVOLVED SNR G156.2+5.7 | XIS | Y |
| SNR 0103-72.6 | 16.2944 | -72.389 | 301.47055063 | -44.70024477 | 13.8765 | 53848.0156018518 | 53849.3773032407 | 501077010 | 49271.5 | 50000 | 49279.5 | 49287.5 | 49287.5 | 49271.5 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 37190.5 | 37190.5 | 117629.9 | 3 | PROCESSED | 57533.5571296296 | 54401 | 53907.4220023148 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011241 | We propose Suzaku observations of O-rich supernova remnants (SNRs) 0103-72.6 and 0049-73.6 in the Small Magellanic Cloud (SMC). These SMC SNRs are oldest members (18000 and 14000 yr old) of O-rich SNRs and share X-ray spectral characteristics with a young (1000 yr old) O-rich SNR 0102-7219 which is also in the SMC. While sharing similar spectral features with 0102-7219, the morphologies of 0103-72.6 and 0049-73.6 indicate more evolved phases of the SNR in a similar interstellar environment as 0102-7219. Cross-comparison studies with the high spectral resolution Suzaku/XIS observations among 0103-72.6/0049-73.6 (this proposal) and 0102-7219 (scheduled/observed for the instrument calibrations) will provide a unique opportunity for the study of a long-term evolution of an O-rich SNR. | GALACTIC DIFFUSE EMISSION | 5 | A | PARK | SANGWOOK | NULL | NULL | USA | 1 | AO1 | BACK TO THE FUTURE: LONG-TERM EVOLUTION OF OXYGET-RICH SUPERNOVA REMNANTS IN THE SMALL MAGELLANIC CLOUD | XIS | N |
| SNR G93.3+6.9 CENTER | 312.9805 | 55.373 | 93.25121789 | 6.97467523 | 40.9208 | 53905.2215509259 | 53905.6480787037 | 501079010 | 20537.2 | 20000 | 20545.2 | 20545.2 | 20545.2 | 20537.2 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 20008 | 20008 | 36815.9 | 0 | PROCESSED | 57534.7200347222 | 54401 | 53926.792962963 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011242 | The high-latitude supernova remnant G93.3+6.9 (DA 530), with a well-defined shell-like radio morphology and an exceptionally small ratio of X-ray to radio luminosities, evolves in a very low density medium. We propose Suzaku raster observations to map out the remnant. We will examine the type of the supernova and the X-ray radiation mechanism as well as the thermal, chemical and ionization states of the remnant. We will also spectroscopically characterize an extended hard X-ray emission feature, detected in a Chandra observation and spatially coincident with a radio peak near the remnant center, to test the hypothesis that it is a pulsar wind nebula. This study will facilitate an unprecedented test of our understanding of supernova remnants in a very low density environment. | GALACTIC DIFFUSE EMISSION | 5 | B | WANG | Q. DANIEL | NULL | NULL | USA | 1 | AO1 | G93.3+6.9: A TESTBED FOR SUPERNOVA REMNANT PHYSICS IN A VERY LOW-DENSITY MEDIUM | HXD | N |
| SNR G93.3+6.9 S1 | 313.1088 | 55.5284 | 93.41888838 | 7.01647125 | 40.6424 | 53905.6486458333 | 53905.9696064815 | 501080010 | 15875 | 15000 | 15875 | 15890.2 | 15891 | 15883 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 12758.8 | 12758.8 | 27727.9 | 1 | PROCESSED | 57534.7111805556 | 54401 | 53926.199212963 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011242 | The high-latitude supernova remnant G93.3+6.9 (DA 530), with a well-defined shell-like radio morphology and an exceptionally small ratio of X-ray to radio luminosities, evolves in a very low density medium. We propose Suzaku raster observations to map out the remnant. We will examine the type of the supernova and the X-ray radiation mechanism as well as the thermal, chemical and ionization states of the remnant. We will also spectroscopically characterize an extended hard X-ray emission feature, detected in a Chandra observation and spatially coincident with a radio peak near the remnant center, to test the hypothesis that it is a pulsar wind nebula. This study will facilitate an unprecedented test of our understanding of supernova remnants in a very low density environment. | GALACTIC DIFFUSE EMISSION | 5 | B | WANG | Q. DANIEL | NULL | NULL | USA | 1 | AO1 | G93.3+6.9: A TESTBED FOR SUPERNOVA REMNANT PHYSICS IN A VERY LOW-DENSITY MEDIUM | HXD | N |
| SNR G93.3+6.9 S2 | 312.6887 | 55.4958 | 93.24230604 | 7.18061007 | 40.0056 | 53905.9701736111 | 53906.4293865741 | 501081010 | 16009.2 | 15000 | 16035.2 | 16027.2 | 16009.2 | 16035.2 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 18375.7 | 18375.7 | 39667.9 | 1 | PROCESSED | 57534.7256134259 | 54401 | 53927.314537037 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011242 | The high-latitude supernova remnant G93.3+6.9 (DA 530), with a well-defined shell-like radio morphology and an exceptionally small ratio of X-ray to radio luminosities, evolves in a very low density medium. We propose Suzaku raster observations to map out the remnant. We will examine the type of the supernova and the X-ray radiation mechanism as well as the thermal, chemical and ionization states of the remnant. We will also spectroscopically characterize an extended hard X-ray emission feature, detected in a Chandra observation and spatially coincident with a radio peak near the remnant center, to test the hypothesis that it is a pulsar wind nebula. This study will facilitate an unprecedented test of our understanding of supernova remnants in a very low density environment. | GALACTIC DIFFUSE EMISSION | 5 | B | WANG | Q. DANIEL | NULL | NULL | USA | 1 | AO1 | G93.3+6.9: A TESTBED FOR SUPERNOVA REMNANT PHYSICS IN A VERY LOW-DENSITY MEDIUM | HXD | N |
| SNR G93.3+6.9 S3 | 313.171 | 55.2801 | 93.24775568 | 6.83197363 | 40.0152 | 53906.4300462963 | 53906.7266087963 | 501082010 | 16334.7 | 15000 | 16334.7 | 16358.7 | 16350.7 | 16342.7 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 13918.6 | 13918.6 | 25615.9 | 0 | PROCESSED | 57534.7339814815 | 54401 | 53926.2481365741 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011242 | The high-latitude supernova remnant G93.3+6.9 (DA 530), with a well-defined shell-like radio morphology and an exceptionally small ratio of X-ray to radio luminosities, evolves in a very low density medium. We propose Suzaku raster observations to map out the remnant. We will examine the type of the supernova and the X-ray radiation mechanism as well as the thermal, chemical and ionization states of the remnant. We will also spectroscopically characterize an extended hard X-ray emission feature, detected in a Chandra observation and spatially coincident with a radio peak near the remnant center, to test the hypothesis that it is a pulsar wind nebula. This study will facilitate an unprecedented test of our understanding of supernova remnants in a very low density environment. | GALACTIC DIFFUSE EMISSION | 5 | B | WANG | Q. DANIEL | NULL | NULL | USA | 1 | AO1 | G93.3+6.9: A TESTBED FOR SUPERNOVA REMNANT PHYSICS IN A VERY LOW-DENSITY MEDIUM | HXD | N |
| SNR G93.3+6.9 S4 | 312.7524 | 55.2472 | 93.07038921 | 6.99620044 | 39.4008 | 53906.7271296296 | 53907.0550347222 | 501083010 | 15366.2 | 15000 | 15366.2 | 15366.2 | 15366.2 | 15366.2 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 14469.4 | 14469.4 | 28327.9 | 1 | PROCESSED | 57534.7341550926 | 54401 | 53926.117662037 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011242 | The high-latitude supernova remnant G93.3+6.9 (DA 530), with a well-defined shell-like radio morphology and an exceptionally small ratio of X-ray to radio luminosities, evolves in a very low density medium. We propose Suzaku raster observations to map out the remnant. We will examine the type of the supernova and the X-ray radiation mechanism as well as the thermal, chemical and ionization states of the remnant. We will also spectroscopically characterize an extended hard X-ray emission feature, detected in a Chandra observation and spatially coincident with a radio peak near the remnant center, to test the hypothesis that it is a pulsar wind nebula. This study will facilitate an unprecedented test of our understanding of supernova remnants in a very low density environment. | GALACTIC DIFFUSE EMISSION | 5 | B | WANG | Q. DANIEL | NULL | NULL | USA | 1 | AO1 | G93.3+6.9: A TESTBED FOR SUPERNOVA REMNANT PHYSICS IN A VERY LOW-DENSITY MEDIUM | HXD | N |
| MONOGEM RING WEST | 118.3557 | 8.2507 | 212.50229712 | 17.5030797 | 287.8334 | 53865.545462963 | 53867.1127199074 | 501084010 | 54268.5 | 50000 | 54268.5 | 54268.5 | 54268.5 | 54268.5 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 43231.2 | 43231.2 | 135389.9 | 2 | PROCESSED | 57534.3136689815 | 54401 | 53914.2479282407 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011243 | We propose to acquire the first high-quality, CCD resolution spectrum of the Monogem Ring SNR. The Monogem Ring is a large (D~25 degrees), old (t~10^5 yr) SNR with a soft X-ray spectrum. A 50 ks observation with Suzaku will detect and measure the OVII Triplet and OVIII Lyman-alpha line fluxes. We will use the ratio of these two line complexes to constrain the temperature and ionization timescale of the plasma in this region of the Monogem Ring. Determing the plasma conditions in such evolved SNRs is important for understanding how these remnants merge with and affect the interstellar medium. | GALACTIC DIFFUSE EMISSION | 5 | B | PLUCINSKY | PAUL | NULL | NULL | USA | 1 | AO1 | THE MONOGEM RING: MEASURING THE O LINE EMISSION WITH SUZAKU | XIS | N |
| VELA FRAGMENT B | 135.5139 | -43.4767 | 265.2464603 | 1.98991007 | 89.0012 | 54044.6051388889 | 54046.4341898148 | 501085010 | 57880.4 | 60000 | 57896.4 | 57880.4 | 57896.4 | 57896.4 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 56965.2 | 56965.2 | 158021.9 | 2 | PROCESSED | 57536.0751157407 | 54695 | 54091.4107175926 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011245 | Ejecta fragments from the nearby Vela supernova remnant provide a unique opportunity to examine supernova ejecta as they shock and finally merge into the interstellar medium (ISM). Fragments "A" and "D", observed with Chandra and XMM-Newton, show strongly enhanced but very different abundances. These fragments are indeed ejecta, but originating in different layers of the precursor. We propose to observe another fragment, "B". The abundances and distribution will provide further evidence about the origin and evolution of these ejecta clumps, In combination with the existing observations of fragments A and D, these data will provide a much more complete picture of the variation in ejecta fragment abundances and their interaction with the remnant shell and the surrounding ISM. | GALACTIC DIFFUSE EMISSION | 5 | C | GAETZ | TERRANCE | NULL | NULL | USA | 1 | AO1 | SEARCHING FOR EJECTA IN VELA SNR FRAGMENT B | XIS | Y |
| PUP A : BEK | 125.942 | -42.9405 | 260.51799115 | -3.16426215 | 276.3687 | 53842.2933449074 | 53842.5807407407 | 501086010 | 16091.3 | 15000 | 16091.3 | 16099.3 | 16091.3 | 16091.3 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 9698.5 | 9698.5 | 24797 | 0 | PROCESSED | 57533.4850115741 | 54401 | 53906.8467708333 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011246 | We propose to use Suzaku XIS to locate X-ray emitting oxygen ejecta in Puppis A, a middle-aged oxygen-rich supernova remnant. The ejecta are seen in optical emission, and enhanced X-ray oxygen line emission is detected but not localized. Puppis A has never been surveyed with an adequate combination of bandpass and spectral resolution, and Suzaku offers a unique capability for providing such observations. The line emission will also provide diagnostics of plasma conditions throughout the remnant through their intensity ratios in addition to conventional broadband spectral fits. We propose five fields to cover the eastern portion of the remnant where the oxygen ejecta are expected to be present. | GALACTIC DIFFUSE EMISSION | 5 | A | HWANG | UNA | NULL | NULL | USA | 1 | AO1 | MAPPING OXYGEN IN PUPPIS A | XIS | N |
| PUP A : NE | 125.7583 | -42.7117 | 260.25284038 | -3.14403225 | 277.1213 | 53842.913287037 | 53843.3091319445 | 501087010 | 20710.9 | 20000 | 20733.6 | 20734.9 | 20718.9 | 20710.9 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 19744.3 | 19744.3 | 34189.9 | 1 | PROCESSED | 57533.5127083333 | 54401 | 53906.9450231482 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011246 | We propose to use Suzaku XIS to locate X-ray emitting oxygen ejecta in Puppis A, a middle-aged oxygen-rich supernova remnant. The ejecta are seen in optical emission, and enhanced X-ray oxygen line emission is detected but not localized. Puppis A has never been surveyed with an adequate combination of bandpass and spectral resolution, and Suzaku offers a unique capability for providing such observations. The line emission will also provide diagnostics of plasma conditions throughout the remnant through their intensity ratios in addition to conventional broadband spectral fits. We propose five fields to cover the eastern portion of the remnant where the oxygen ejecta are expected to be present. | GALACTIC DIFFUSE EMISSION | 5 | A | HWANG | UNA | NULL | NULL | USA | 1 | AO1 | MAPPING OXYGEN IN PUPPIS A | XIS | N |
| PUP A : INTERIOR | 125.5916 | -42.8951 | 260.333956 | -3.34905821 | 276.8883 | 53842.5813541667 | 53842.9127199074 | 501088010 | 20270.9 | 20000 | 20292.4 | 20294.9 | 20278.9 | 20270.9 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 19951.9 | 19951.9 | 28623.9 | 0 | PROCESSED | 57533.5042476852 | 54401 | 53906.8948611111 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011246 | We propose to use Suzaku XIS to locate X-ray emitting oxygen ejecta in Puppis A, a middle-aged oxygen-rich supernova remnant. The ejecta are seen in optical emission, and enhanced X-ray oxygen line emission is detected but not localized. Puppis A has never been surveyed with an adequate combination of bandpass and spectral resolution, and Suzaku offers a unique capability for providing such observations. The line emission will also provide diagnostics of plasma conditions throughout the remnant through their intensity ratios in addition to conventional broadband spectral fits. We propose five fields to cover the eastern portion of the remnant where the oxygen ejecta are expected to be present. | GALACTIC DIFFUSE EMISSION | 5 | A | HWANG | UNA | NULL | NULL | USA | 1 | AO1 | MAPPING OXYGEN IN PUPPIS A | XIS | N |
| PUP A : SE | 126.0128 | -43.1802 | 260.74447692 | -3.25911558 | 277.1832 | 53843.3098842593 | 53843.8328009259 | 501089010 | 29749.3 | 30000 | 29749.3 | 29817.2 | 29765.2 | 29761.2 | 4 | 2 | 4 | 4 | 1 | 0 | 0 | 22886.7 | 22886.7 | 45174 | 0 | PROCESSED | 57533.5119675926 | 54401 | 53907.001412037 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011246 | We propose to use Suzaku XIS to locate X-ray emitting oxygen ejecta in Puppis A, a middle-aged oxygen-rich supernova remnant. The ejecta are seen in optical emission, and enhanced X-ray oxygen line emission is detected but not localized. Puppis A has never been surveyed with an adequate combination of bandpass and spectral resolution, and Suzaku offers a unique capability for providing such observations. The line emission will also provide diagnostics of plasma conditions throughout the remnant through their intensity ratios in addition to conventional broadband spectral fits. We propose five fields to cover the eastern portion of the remnant where the oxygen ejecta are expected to be present. | GALACTIC DIFFUSE EMISSION | 5 | A | HWANG | UNA | NULL | NULL | USA | 1 | AO1 | MAPPING OXYGEN IN PUPPIS A | XIS | N |
| PUP A : S | 125.6829 | -43.1445 | 260.57740663 | -3.43620983 | 277.8865 | 53843.8334606482 | 53844.4397569444 | 501090010 | 31144.5 | 30000 | 31160.5 | 31152.5 | 31144.5 | 31168.5 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 26585.6 | 26585.6 | 52371.9 | 1 | PROCESSED | 57533.5191550926 | 54401 | 53907.0902199074 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011246 | We propose to use Suzaku XIS to locate X-ray emitting oxygen ejecta in Puppis A, a middle-aged oxygen-rich supernova remnant. The ejecta are seen in optical emission, and enhanced X-ray oxygen line emission is detected but not localized. Puppis A has never been surveyed with an adequate combination of bandpass and spectral resolution, and Suzaku offers a unique capability for providing such observations. The line emission will also provide diagnostics of plasma conditions throughout the remnant through their intensity ratios in addition to conventional broadband spectral fits. We propose five fields to cover the eastern portion of the remnant where the oxygen ejecta are expected to be present. | GALACTIC DIFFUSE EMISSION | 5 | A | HWANG | UNA | NULL | NULL | USA | 1 | AO1 | MAPPING OXYGEN IN PUPPIS A | XIS | N |
| N11 SB | 74.1823 | -66.412 | 277.1886014 | -36.07081942 | 146.432 | 54046.4407291667 | 54047.232037037 | 501091010 | 30452 | 30000 | 30452 | 30452 | 30452 | 30452 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 26405 | 26405 | 68365.9 | 0 | PROCESSED | 57536.0384953704 | 54455 | 54088.5643287037 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011251 | Clusters of massive stars, through their stellar winds and supernovae, form large diffuse structures known as superbubbles (SBs), which play an essential role in shaping the local interstellar medium. Most SB models indicate that these objects should be dominated by thermal plasma processes. However, observations of 2 SBs have detected significant nonthermal contributions to their X-ray emission, which raises many questions. Is it generated by synchrotron, inverse-Compton, or nonthermal Bremsstrahlung processes? Are colliding stellar winds or internal supernova remnants responsible? We therefore propose to examine the X-ray emission from 4 X-ray bright SBs, to search for nonthermal X-ray emission, and if possible place strong constraints on the source of this emission. | GALACTIC DIFFUSE EMISSION | 5 | C | WILLIAMS | ROSA | NULL | NULL | USA | 1 | AO1 | A SEARCH FOR NONTHERMAL X-RAY EMISSION FROM SUPERBUBBLES | XIS | N |
| LMC X-3 OFF FIELD 1 | 85.5783 | -64.5441 | 274.09377866 | -31.6918405 | 324.0002 | 53847.1442361111 | 53848.0099421296 | 501097010 | 43606.7 | 50000 | 43606.7 | 43606.7 | 43606.7 | 43606.7 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 42026.1 | 42026.1 | 74745.9 | 0 | PROCESSED | 57533.5339583333 | 54526 | 53907.3335763889 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011256 | The Galactic corona is believed to play an essential role in the ``eco-system'' of the Galaxy. But the extent as well as the physical properties of the corona are yet to be determined. We request deep Suzaku XIS observations of the soft X-ray background in the vicinity of LMC X-3, toward which we have already conducted far-UV and X-ray absorption line spectroscopy. We have developed a software tool for a joint model fit to the absorption and emission data, allowing for statistical tests of various models and constraints on such parameters as hot gas temperature, density, and scale. The results will provide a unique calibration of our understanding of the corona. | GALACTIC DIFFUSE EMISSION | 5 | A | WANG | Q. DANIEL | NULL | NULL | USA | 1 | AO1 | A JOINT EMISSION AND ABSORPTION STUDY OF THE GALACTIC CORONA | XIS | N |
| LMC X-3 OFF FIELD 1 | 85.5246 | -64.555 | 274.10794908 | -31.71433471 | 145.4977 | 54039.3159722222 | 54039.7509722222 | 501097020 | 15374.9 | 10000 | 15374.9 | 15382.9 | 15382.9 | 15382.9 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 14926.3 | 14926.3 | 37580 | 0 | PROCESSED | 57536.0002314815 | 54526 | 54088.8072222222 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011256 | The Galactic corona is believed to play an essential role in the ``eco-system'' of the Galaxy. But the extent as well as the physical properties of the corona are yet to be determined. We request deep Suzaku XIS observations of the soft X-ray background in the vicinity of LMC X-3, toward which we have already conducted far-UV and X-ray absorption line spectroscopy. We have developed a software tool for a joint model fit to the absorption and emission data, allowing for statistical tests of various models and constraints on such parameters as hot gas temperature, density, and scale. The results will provide a unique calibration of our understanding of the corona. | GALACTIC DIFFUSE EMISSION | 5 | A | WANG | Q. DANIEL | NULL | NULL | USA | 1 | AO1 | A JOINT EMISSION AND ABSORPTION STUDY OF THE GALACTIC CORONA | XIS | N |
| CAR-D1 | 162.0244 | -59.5887 | 287.89332648 | -0.36746291 | 282.973 | 53891.5567361111 | 53892.6343055556 | 501099010 | 76907.4 | 75000 | 76924 | 76932 | 76931.4 | 76907.4 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 64257.6 | 64257.6 | 93089.9 | 0 | PROCESSED | 57534.5127430556 | 54401 | 53926.947974537 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011257 | Soft X-ray emission nebulae with kT =0.1-0.8 keV, log Lx =33-35 ergs/s, and the size of 1-1000 pc accompany a number of giant HII region, but the origin is not understood yet. The Carinae Nebula is 10-100 times more luminous than any other giant HII region in our Galaxy in soft X-rays. From an XMM-Newton observation of the eastern tip of the nebula called Car-D1, we found marginal CVI, CV and OVII lines. If it is real, the carbon abundance should be more than >6 solar, and the OVII line requires more than 2-temperature components. To detect those emission lines clearly and address the origin and environment of the diffuse plasma, we propose a Suzaku observation of the Car-D1 region, optimized for the XIS BI chip. | GALACTIC DIFFUSE EMISSION | 5 | B | HAMAGUCHI | KENJI | NULL | NULL | USA | 1 | AO1 | ORIGIN OF THE DIFFUSE X-RAY EMISSION AROUND THE CARINA NEBULA, A MASSIVE STAR FORMING REGION | XIS | N |
| GALACTIC PLANE 111 | 347.9369 | 61.9538 | 111.50111702 | 1.31488521 | 81.8498 | 53892.6499652778 | 53893.680775463 | 501100010 | 72140.9 | 75000 | 72164.9 | 72164.9 | 72164.9 | 72140.9 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 61025 | 61025 | 89034.9 | 1 | PROCESSED | 57534.5221064815 | 54401 | 53927.3325115741 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011258 | We propose to observe the line of sight towards (l,b)=(111.5,1.3). This line of sight was observed by XMM because the line of sight is particularly simple, allowing the isolation of the spectrum of the Local Hot Bubble (LHB). The XMM observation did not isolate the LHB, but did reveal the existance of a cool (kT~0.18 keV) X-ray emitting component between 200 and 2000 pcs away that was morphologically unidentifiable in the ROSAT All-Sky Survey. This component may represent the gas responsible for the 3/4 keV "infill problem", and may represent a previously overlooked high filling factor component of the hot ISM. Suzaku observations along this line of sight, coupled with the Suzaku observation towards MBM12, will allow the isolation of this component. | GALACTIC DIFFUSE EMISSION | 5 | B | KUNTZ | K. | NULL | NULL | USA | 1 | AO1 | BEYOND THE LOCAL HOT BUBBLE TOWARDS L=111 | XIS | N |
| DRACO ENHANCEMENT | 239.3128 | 61.2868 | 93.98685674 | 43.98646489 | 194.9053 | 54048.1213888889 | 54049.8515509259 | 501101010 | 43862.8 | 75000 | 79427.4 | 79427.4 | 43862.8 | 79419.4 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 75874.1 | 75874.1 | 149474 | 1 | PROCESSED | 57536.1016319444 | 54455 | 54088.7470486111 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011259 | We propose to observe the Draco Enhancement, a region of very bright 1/4 keV emission in the northern Galactic halo that is only 15 degrees from the Suzaku observation of the North Ecliptic Pole. A decomposition of the spectrum of the Galactic halo by Kuntz & Snowden showed that, to within the uncertainties of the ROSAT All-Sky Survey, the halo emission was composed of two thermal components; a uniform hot component with kT~0.25 keV, and a very patchy soft component with kT~0.1 keV. The soft component is found in only a few isolated regions of the sky, of which the Draco Enhancement is the brightest. This emission is too soft to be studied with XMM. Suzaku will allow us to determine the temperature of the soft component or place very strict upper limits on its temperature. | GALACTIC DIFFUSE EMISSION | 5 | C | KUNTZ | K. | NULL | NULL | USA | 1 | AO1 | THE SOFT COMPONENT OF THE GALACTIC HALO | XIS | N |
| MBM12 OFF-CLOUD | 41.3205 | 18.3346 | 157.33933963 | -36.81758445 | 247.4802 | 53772.648599537 | 53774.618275463 | 501104010 | 75329.2 | 70000 | 75337.2 | 75329.2 | 75337.2 | 75337.2 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 67769 | 67769 | 170115.9 | 1 | PROCESSED | 57532.9691550926 | 54401 | 53905.9757523148 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011262 | Suzaku will observe MBM 12, a nearby molecular cloud which shadows all but the most local soft X-ray emission. The goal of that observation is to measure the O VII and O VIII emission from the Local Hot Bubble, taking advantage of Suzaku's low energy sensitivity and low background. In light of this, we propose to observe the diffuse background near the MBM 12 position. This will: (1) Measure the O VII and O VIII emission from the Galactic disk and halo, after subtracting the local emission, and (2) confirm that this background emission does not contaminate the initial observation. The absolute measure of the strength of the O VII line, as well as the O VIII/O VII ratio, is essential to understanding the origin of the Galactic component to the 3/4 keV diffuse emission. | GALACTIC DIFFUSE EMISSION | 5 | B | SMITH | RANDALL | NULL | NULL | USA | 1 | AO1 | THE ORIGIN OF THE GALACTIC DIFFUSE 3/4 KEV X-RAY BACKGROUND | XIS | N |
| HESS J1718-385 | 259.5512 | -38.6075 | 348.79652534 | -0.53531102 | 91.2393 | 54154.3587731482 | 54154.7773611111 | 501105010 | 20744 | 19000 | 20744 | 20744 | 0 | 20744 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15836.5 | 15836.5 | 36151.9 | 0 | PROCESSED | 57537.4491435185 | 54527 | 54158.2865740741 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012044 | HESS J1718-385 is a newly discovered TeV gamma-ray source, with an unusually hard energy spectrum, which lies in close proximity to an energetic pulsar. It is likely that this object belongs to the class of offset pulsar wind nebula (PWN), accelerating electrons and positrons up to ~100 TeV. So far no sensitive X-ray observations of this region have taken place. The synchrotron spectrum of the nebula is predicted to peak in the energy range of the Suzaku HXD. The unprecedented high energy sensitivity of this instrument is required to study the highest energy particles accelerated in this object. Spectral measurements by Suzaku would confirm the inverse-Compton origin of the VHE gamma-rays and place tight constraints on the maximum energy of accelerated electrons. | GALACTIC DIFFUSE EMISSION | 5 | A | HINTON | JAMES | NULL | NULL | EUR | 1 | AO1 | PROBING THE LIMITS OF PARTICLE ACCELERATION IN A NEW HARD SPECTRUM TEV GAMMA-RAY SOURCE | XIS | N |
| G156.2+5.7 CENTER | 74.723 | 51.7342 | 156.21466687 | 5.62934315 | 273.4473 | 54148.7568171296 | 54149.9169444444 | 501106010 | 51214.2 | 50000 | 51222.2 | 51230.2 | 0 | 51214.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 46482 | 46482 | 100199.9 | 0 | PROCESSED | 57537.3992824074 | 54695 | 54158.4264351852 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 013079 | Recent observations revealed that about 10 shell-like supernova remnants (SNRs) exhibit power-law X-ray spectra with no emission line which are considered to be synchrotron radiation from high-energy electrons (larger than 1 TeV). However, all those samples are young SNRs (ages about 300-2000 yr). G156.2+5.7 is an old SNR (age about 10^4 year), but emits hard X-rays in addition to usual thin thermal emission (about 0.5 keV temperature). We propose a Suzaku observation on a center region of this SNR, where diffuse hard X-rays were detected with ASCA and XMM. Our primary objective is to determine whether or not the hard tail is synchrotron X-rays, and study cosmic-ray acceleration in this old SNR. | GALACTIC DIFFUSE EMISSION | 5 | B | UENO | MASARU | PETRE | ROBERT | JUS | 1 | AO1 | REVEALING THE ORIGIN OF HARD X-RAY EMISSION FROM AN OLD SNR, G156.2+5.7 | XIS | Y |
| VELA X (REGION A) | 128.7666 | -45.458 | 263.74862198 | -2.99483781 | 337.7597 | 53927.7846990741 | 53929.4703819444 | 501107010 | 60773.5 | 60000 | 60773.5 | 60773.5 | 60773.5 | 60773.5 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 54161.1 | 54161.1 | 145605.8 | 3 | PROCESSED | 57534.9641203704 | 54401 | 53942.4562037037 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 014211 | The nature of Vela X, the radio-bright central region of the Vela SNR, has remained a mystery for three decades. Particulary puzzling is the brightest filament of Vela X. It has an apparent X-ray counterpart which was thought to be the jet of the Vela pulsar energizing the Vela X complex. This seemingly straightforward interpretation has been ruled out by the Chandra discovery of the true pulsar jets. To elucidate the nature of the filament and the Vela X complex and their connection to the Vela pulsar, we propose spatially-resolved spectroscopy of the radio/X-ray filament with XIS. Simultaneously, we will measure the spectra of the Vela pulsar and PWN between 10 and 600 keV and perform phase-resolved spectroscopy of the pulsar in the 20-50 keV band. | GALACTIC DIFFUSE EMISSION | 5 | B | KARGALTSEV | OLEG | MORI | KOJI | USJ | 1 | AO1 | THE ORIGIN OF VELA X: CONNECTION TO THE PULSAR | XIS | N |
| VELA X (REGION C) | 127.7806 | -46.2716 | 263.99736145 | -4.03006469 | 349.189 | 53933.9133796296 | 53934.7730787037 | 501108010 | 29202.8 | 30000 | 29202.8 | 29202.8 | 29202.8 | 29202.8 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 25592.9 | 25592.9 | 74248 | 1 | PROCESSED | 57534.9868055556 | 54404 | 53943.4988773148 | 3.0.22.43 | 7 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 014211 | The nature of Vela X, the radio-bright central region of the Vela SNR, has remained a mystery for three decades. Particulary puzzling is the brightest filament of Vela X. It has an apparent X-ray counterpart which was thought to be the jet of the Vela pulsar energizing the Vela X complex. This seemingly straightforward interpretation has been ruled out by the Chandra discovery of the true pulsar jets. To elucidate the nature of the filament and the Vela X complex and their connection to the Vela pulsar, we propose spatially-resolved spectroscopy of the radio/X-ray filament with XIS. Simultaneously, we will measure the spectra of the Vela pulsar and PWN between 10 and 600 keV and perform phase-resolved spectroscopy of the pulsar in the 20-50 keV band. | GALACTIC DIFFUSE EMISSION | 5 | B | KARGALTSEV | OLEG | MORI | KOJI | USJ | 1 | AO1 | THE ORIGIN OF VELA X: CONNECTION TO THE PULSAR | XIS | N |
| VELA PULSAR/PWN 1 | 128.7701 | -45.1981 | 263.5414959 | -2.83747227 | 337.9628 | 53926.0492592593 | 53927.7841782407 | 501109010 | 60291.3 | 60000 | 60344.6 | 60291.3 | 60331.3 | 60323.3 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 52689.9 | 52689.9 | 149865.9 | 1 | PROCESSED | 57534.9239699074 | 54401 | 53942.4588078704 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 014211 | The nature of Vela X, the radio-bright central region of the Vela SNR, has remained a mystery for three decades. Particulary puzzling is the brightest filament of Vela X. It has an apparent X-ray counterpart which was thought to be the jet of the Vela pulsar energizing the Vela X complex. This seemingly straightforward interpretation has been ruled out by the Chandra discovery of the true pulsar jets. To elucidate the nature of the filament and the Vela X complex and their connection to the Vela pulsar, we propose spatially-resolved spectroscopy of the radio/X-ray filament with XIS. Simultaneously, we will measure the spectra of the Vela pulsar and PWN between 10 and 600 keV and perform phase-resolved spectroscopy of the pulsar in the 20-50 keV band. | GALACTIC DIFFUSE EMISSION | 5 | B | KARGALTSEV | OLEG | MORI | KOJI | USJ | 1 | AO1 | THE ORIGIN OF VELA X: CONNECTION TO THE PULSAR | HXD | N |
| VELA PULSAR/PWN 3 | 128.6368 | -45.8007 | 263.96966687 | -3.27226783 | 344.1164 | 53925.347974537 | 53926.0467476852 | 501110010 | 17588.6 | 20000 | 17604.6 | 17588.6 | 17588.6 | 17604.6 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 17225.2 | 17225.2 | 60351.9 | 0 | PROCESSED | 57534.8715509259 | 54401 | 53930.634224537 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 014211 | The nature of Vela X, the radio-bright central region of the Vela SNR, has remained a mystery for three decades. Particulary puzzling is the brightest filament of Vela X. It has an apparent X-ray counterpart which was thought to be the jet of the Vela pulsar energizing the Vela X complex. This seemingly straightforward interpretation has been ruled out by the Chandra discovery of the true pulsar jets. To elucidate the nature of the filament and the Vela X complex and their connection to the Vela pulsar, we propose spatially-resolved spectroscopy of the radio/X-ray filament with XIS. Simultaneously, we will measure the spectra of the Vela pulsar and PWN between 10 and 600 keV and perform phase-resolved spectroscopy of the pulsar in the 20-50 keV band. | GALACTIC DIFFUSE EMISSION | 5 | B | KARGALTSEV | OLEG | MORI | KOJI | USJ | 1 | AO1 | THE ORIGIN OF VELA X: CONNECTION TO THE PULSAR | XIS | N |
| G12.0-0.1 | 273.0232 | -18.6277 | 11.94868379 | -0.09019508 | 259.2908 | 54375.5953819444 | 54376.9863310185 | 502001010 | 53752.1 | 53000 | 53752.1 | 53752.1 | 0 | 53752.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47183 | 47183 | 120172 | 1 | PROCESSED | 57540.1741898148 | 54751 | 54403.1207986111 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020010 | We propose an observation of a supernova remnant (SNR) G12.0-0.1 with Suzaku. ASCA discovered X-ray emission from this SNR. The X-ray spectrum exhibit a power-law shape, and the radius and X-ray luminosity estimated from the ASCA results are similar to those of SN 1006, which suggests that it is a SN 1006-like SNR. However, due to the poor statistics, we could not conclude that G12.0-0.1 is SN 1006-like SNR. Precise measurements of the X-ray spectrum with the XIS will provide us with understanding the physical process in the SNR. | GALACTIC DIFFUSE EMISSION | 5 | B | YAMAUCHI | SHIGEO | NULL | NULL | JAP | 2 | AO2 | SUZAKU OBSERVATION OF G12.0-0.1 | XIS | Y |
| GC14 | 267.1584 | -29.141 | 0.16624555 | -0.66947426 | 260.5381 | 54382.6950694444 | 54383.1530555556 | 502002010 | 23190.3 | 20000 | 23206.3 | 23190.3 | 0 | 23206.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 20932.9 | 20932.9 | 39559.9 | 0 | PROCESSED | 57540.2209490741 | 54771 | 54402.7240740741 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020013 | We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated. | GALACTIC DIFFUSE EMISSION | 5 | B | KOKUBUN | MOTOHIDE | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y |
| GC15 | 266.9617 | -29.4257 | 359.83382525 | -0.66952641 | 260.7835 | 54383.1536226852 | 54383.6391666667 | 502003010 | 21467.1 | 20000 | 21475.1 | 21467.1 | 0 | 21475.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18922.5 | 18922.5 | 41943.9 | 0 | PROCESSED | 57540.2312731482 | 54771 | 54402.7485532407 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020013 | We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated. | GALACTIC DIFFUSE EMISSION | 5 | B | KOKUBUN | MOTOHIDE | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y |
| GC16 | 267.4868 | -29.3131 | 0.16607902 | -1.00376926 | 260.5335 | 54383.6397800926 | 54384.0419444444 | 502004010 | 19873 | 20000 | 19873 | 19890.3 | 0 | 19874.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 18832.1 | 18832.1 | 34736 | 0 | PROCESSED | 57540.2356597222 | 54771 | 54402.5680208333 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020013 | We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated. | GALACTIC DIFFUSE EMISSION | 5 | B | KOKUBUN | MOTOHIDE | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y |
| GC17 | 267.2896 | -29.5968 | 359.83441438 | -1.00224826 | 260.2809 | 54384.0425578704 | 54384.480787037 | 502005010 | 20603.5 | 20000 | 20603.5 | 20603.5 | 0 | 20603.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18174.3 | 18174.3 | 37854 | 1 | PROCESSED | 57540.245787037 | 54777 | 54402.5689583333 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020013 | We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated. | GALACTIC DIFFUSE EMISSION | 5 | B | KOKUBUN | MOTOHIDE | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y |
| GC18 | 266.183 | -28.6222 | 0.16630142 | 0.32982124 | 260.5302 | 54384.4819560185 | 54384.9633564815 | 502006010 | 22631.1 | 20000 | 22631.1 | 22641.3 | 0 | 22635.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21670.2 | 21670.2 | 41584.1 | 1 | PROCESSED | 57540.2503356482 | 54771 | 54402.6632291667 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020013 | We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated. | GALACTIC DIFFUSE EMISSION | 5 | B | KOKUBUN | MOTOHIDE | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y |
| GC19 | 265.8593 | -28.4466 | 0.1669402 | 0.66404713 | 262.6738 | 54384.9647569444 | 54385.4112731482 | 502007010 | 22017.4 | 20000 | 22017.4 | 22041.4 | 0 | 22025.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19524.8 | 19524.8 | 38572 | 0 | PROCESSED | 57540.2498842593 | 54771 | 54402.4381365741 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020013 | We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated. | GALACTIC DIFFUSE EMISSION | 5 | B | KOKUBUN | MOTOHIDE | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y |
| GC20 | 265.6604 | -28.73 | 359.83402449 | 0.66365416 | 262.9349 | 54385.4117939815 | 54385.9099421296 | 502008010 | 23778.6 | 20000 | 23790.6 | 23786.6 | 0 | 23778.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22923.4 | 22923.4 | 43032 | 0 | PROCESSED | 57540.2572337963 | 54771 | 54403.0227314815 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020013 | We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated. | GALACTIC DIFFUSE EMISSION | 5 | B | KOKUBUN | MOTOHIDE | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y |
| GC21 | 267.484 | -27.3686 | 1.83363899 | -0.00346152 | 261.5433 | 54385.9113888889 | 54386.3127199074 | 502009010 | 20861.5 | 20000 | 20861.5 | 20861.5 | 0 | 20861.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19648.3 | 19648.3 | 34663.9 | 1 | PROCESSED | 57540.2599189815 | 54771 | 54402.5769444444 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020013 | We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated. | GALACTIC DIFFUSE EMISSION | 5 | B | KOKUBUN | MOTOHIDE | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y |
| GC22 | 266.3806 | -28.337 | 0.50023196 | 0.3305092 | 262.5049 | 54386.3138888889 | 54386.785 | 502010010 | 21621.4 | 20000 | 21621.4 | 21621.4 | 0 | 21621.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21194.4 | 21194.4 | 40662 | 1 | PROCESSED | 57540.2655439815 | 54771 | 54402.6900231482 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020013 | We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated. | GALACTIC DIFFUSE EMISSION | 5 | B | KOKUBUN | MOTOHIDE | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y |
| GC23 | 266.578 | -28.0524 | 0.83380185 | 0.3300796 | 262.2345 | 54386.7855208333 | 54387.2294444444 | 502011010 | 23013 | 20000 | 23013 | 23021 | 0 | 23029 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 22071.2 | 22071.2 | 38319.9 | 2 | PROCESSED | 57540.2674305556 | 54777 | 54402.5316898148 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020013 | We propose 20 ks x 12 mapping observations around the Galactic Center region with Suzaku. The existence of the non-thermal hard X-ray component in addition to the well-known thermal emission has been almost clarified from the past observations during the SWG and AO-1 phase. Through these additional mapping observations, the latitudinal distribution and longitudinal symmetry of the non-thermal component would be verified, and the co-existence of the two different emission component will be for the first time investigated. | GALACTIC DIFFUSE EMISSION | 5 | B | KOKUBUN | MOTOHIDE | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE GALACTIC CENTER REGION WITH SUZAKU | XIS | Y |
| HESS J1745-303 1 | 266.2249 | -30.1096 | 358.91712668 | -0.478438 | 70.5005 | 54527.7555555556 | 54529.7363310185 | 502016010 | 70529.1 | 67000 | 70537.1 | 70529.1 | 0 | 70545.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 61793.2 | 61793.2 | 171095.9 | 3 | PROCESSED | 57541.8000810185 | 54908 | 54539.3190509259 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020023 | A TeV gamma-ray source HESS J1745-303 shows the hardest TeV spectrum, which cannot be explained by diffusive shock acceleration theory at adiabatic shocks. This source may accelerate protons of 100TeV or more. This TeV source is extended, hence likely a supernova remnant (SNR). There are two scenarios on the nature of this source: one is a young SNR in which the proton acceleration is so efficient, and the other is an old SNR with radiative shock. We have already observed this source by Suzaku AO-1, and found a faint, diffuse, nonthermal X-ray emission. However, the current data prevents us from concluding which scenario is favorable since entire region is not yet covered by X-ray observation. In order to clarify the nature of this source, we propose X-ray mapping observations by Suzaku. | GALACTIC DIFFUSE EMISSION | 5 | B | YAMAZAKI | RYO | NULL | NULL | JAP | 2 | AO2 | SEARCH FOR NONTHERMAL DIFFUSE X-RAYS OF A PROTON ACCELERATOR HESS J1745-303 | XIS | Y |
| HESS J1745-303 2 | 266.4705 | -30.0867 | 359.0474588 | -0.64781783 | 70.5003 | 54531.5601388889 | 54533.6669444444 | 502017010 | 72544.3 | 67000 | 72552.3 | 72552.3 | 0 | 72544.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 63972.3 | 63972.3 | 182014.9 | 2 | PROCESSED | 57541.8457291667 | 54919 | 54550.4057986111 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020023 | A TeV gamma-ray source HESS J1745-303 shows the hardest TeV spectrum, which cannot be explained by diffusive shock acceleration theory at adiabatic shocks. This source may accelerate protons of 100TeV or more. This TeV source is extended, hence likely a supernova remnant (SNR). There are two scenarios on the nature of this source: one is a young SNR in which the proton acceleration is so efficient, and the other is an old SNR with radiative shock. We have already observed this source by Suzaku AO-1, and found a faint, diffuse, nonthermal X-ray emission. However, the current data prevents us from concluding which scenario is favorable since entire region is not yet covered by X-ray observation. In order to clarify the nature of this source, we propose X-ray mapping observations by Suzaku. | GALACTIC DIFFUSE EMISSION | 5 | B | YAMAZAKI | RYO | NULL | NULL | JAP | 2 | AO2 | SEARCH FOR NONTHERMAL DIFFUSE X-RAYS OF A PROTON ACCELERATOR HESS J1745-303 | XIS | Y |
| HESS J1745-303 3 | 266.0567 | -30.2413 | 358.72882707 | -0.42335991 | 69.0003 | 54533.6682523148 | 54535.8752199074 | 502018010 | 79016.2 | 67000 | 79016.2 | 79040.2 | 0 | 79024.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70201 | 70201 | 190658 | 2 | PROCESSED | 57541.8566898148 | 54919 | 54550.3420601852 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020023 | A TeV gamma-ray source HESS J1745-303 shows the hardest TeV spectrum, which cannot be explained by diffusive shock acceleration theory at adiabatic shocks. This source may accelerate protons of 100TeV or more. This TeV source is extended, hence likely a supernova remnant (SNR). There are two scenarios on the nature of this source: one is a young SNR in which the proton acceleration is so efficient, and the other is an old SNR with radiative shock. We have already observed this source by Suzaku AO-1, and found a faint, diffuse, nonthermal X-ray emission. However, the current data prevents us from concluding which scenario is favorable since entire region is not yet covered by X-ray observation. In order to clarify the nature of this source, we propose X-ray mapping observations by Suzaku. | GALACTIC DIFFUSE EMISSION | 5 | B | YAMAZAKI | RYO | NULL | NULL | JAP | 2 | AO2 | SEARCH FOR NONTHERMAL DIFFUSE X-RAYS OF A PROTON ACCELERATOR HESS J1745-303 | XIS | Y |
| SGR D SNR | 267.1922 | -28.1274 | 1.05009547 | -0.17236121 | 267.8977 | 54349.018599537 | 54352.6738310185 | 502020010 | 139080.8 | 133000 | 139080.8 | 139080.8 | 0 | 139080.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 124502.5 | 124502.5 | 315779.8 | 1 | PROCESSED | 57540.026087963 | 54776 | 54371.5203472222 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020031 | We propose a 100 ksec observation of the Sgr D region. This region contains a supernova remnant (SNR), a massive molecular cloud, an HII region and diffuse TeV gamma-ray emission. The objectives are to detect Sgr D SNR and diffuse X-rays from the TeV source, to discover new SNRs and X-ray Reflection Nebulae (XRNe), and to investigate the spatial distribution of high temperature plasma connecting the Galactic center and the Galactic ridge regions. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 2 | AO2 | OBSERVATIONS OF SGR D SNR, A TEV SOURCE AND DIFFUSE X-RAYS | XIS | Y |
| ANTICENTER | 113.3357 | -19.5305 | 234.9976882 | 0.00424804 | 280.7829 | 54212.8606481482 | 54215.4197222222 | 502021010 | 89542.9 | 80000 | 89550.9 | 89558.9 | 0 | 89542.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 78988.7 | 78988.7 | 221050.8 | 3 | PROCESSED | 57538.5236689815 | 54744 | 54223.2040046296 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020032 | We propose to observe diffuse radiation from the Galactic plane in the general direction of the anticenter. Absolute measurement of the O VII and O VIII line fluxes will help establish the origin of this mysterious component of the diffuse background. This will allow a search for spectral signatures of non-thermal emission, i.e. charge- exchange emission, in the 3/4 keV band and the determination of abundances in hot gas thermal emission without risk of confusion by emission from hot gas in the Galactic Bulge. | GALACTIC DIFFUSE EMISSION | 5 | B | MASUI | KENSUKE | NULL | NULL | JAP | 2 | AO2 | SOFT X-RAY DIFFUSE EMISSION FROM THE GALACTIC DISK | XIS | Y |
| (L,B)=(0.25,-0.27) | 266.8068 | -28.8823 | 0.22878525 | -0.27253682 | 265.3343 | 54343.5232986111 | 54346.7919560185 | 502022010 | 134790.4 | 133000 | 134798.4 | 134806.4 | 0 | 134790.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 116842.5 | 116842.5 | 282375.9 | 1 | PROCESSED | 57539.9810185185 | 54724 | 54356.5238657407 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020044 | The Suzaku PV observations found that the diffuse X-rays (6.7 and 6.9 keV-lines) from the GC region can well be explained by a thermal emission from hot plasma with kT=6-7keV (GCDX). The comparison of Suzaku and VLA 90cm images show a hit for special correlation, suggest a magnetic confinement of GCDX. Thus, in order to search for new SNRs and investigate the galactic latitude dependency of the GCDX, we make a GC observation with the aiming point of (l,b)=(0.25, -0.27). We also see the correlation of GCDX with the radio. | GALACTIC DIFFUSE EMISSION | 5 | B | TSURU | TAKESHI | NULL | NULL | JAP | 2 | AO2 | GLOBAL STRUCTURES OF THE GALACTIC CENTER DIFFUSE X-RAY PLASMA (GCDX) | XIS | Y |
| VELA JR P1 | 131.9787 | -45.8064 | 265.40235777 | -1.43438498 | 347.0031 | 54285.3151273148 | 54285.6904398148 | 502023010 | 10649.6 | 10000 | 10649.6 | 10657.6 | 0 | 10657.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 9044.6 | 9044.6 | 32419.9 | 0 | PROCESSED | 57539.086412037 | 54696 | 54328.4268402778 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y |
| VELA JR P2 | 132.1691 | -45.7748 | 265.4613949 | -1.31133586 | 347.0033 | 54285.6908217593 | 54285.9036342593 | 502024010 | 10850.2 | 10000 | 10874.2 | 10866.2 | 0 | 10850.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9603.7 | 9603.7 | 18375.9 | 0 | PROCESSED | 57539.0914467593 | 54696 | 54328.4167361111 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y |
| VELA JR P3 | 132.1192 | -45.6039 | 265.30669647 | -1.23070071 | 347.0044 | 54285.9040162037 | 54286.1057175926 | 502025010 | 10298 | 10000 | 10298 | 10298 | 0 | 10298 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 6726 | 6726 | 17423.9 | 0 | PROCESSED | 57539.0955902778 | 54696 | 54328.4516782407 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y |
| VELA JR P4 | 132.5157 | -45.5453 | 265.43667302 | -0.97855833 | 347.0031 | 54286.1062847222 | 54286.4480787037 | 502026010 | 10972.4 | 10000 | 10972.4 | 10972.4 | 0 | 10972.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11295.9 | 11295.9 | 29511.9 | 1 | PROCESSED | 57539.0994791667 | 54759 | 54328.4405787037 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y |
| VELA JR P5 | 132.9105 | -45.488 | 265.56829981 | -0.72857938 | 347.002 | 54286.4486458333 | 54286.7502777778 | 502027010 | 10977 | 10000 | 10977 | 10977 | 0 | 10977 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10785.8 | 10785.8 | 26053.9 | 0 | PROCESSED | 57539.1013541667 | 54696 | 54328.4697800926 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y |
| VELA JR P6 | 133.325 | -45.4847 | 265.75161327 | -0.50306307 | 347.0024 | 54286.7508449074 | 54286.9863888889 | 502028010 | 11507.2 | 10000 | 11531.2 | 11523.2 | 0 | 11507.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8257.9 | 8257.9 | 20343.9 | 0 | PROCESSED | 57539.1055324074 | 54696 | 54328.3854166667 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y |
| VELA JR P7 | 133.7759 | -45.5828 | 266.02998701 | -0.32446592 | 347.0033 | 54286.9870023148 | 54287.3023032407 | 502029010 | 14583.8 | 10000 | 14583.8 | 14583.8 | 0 | 14583.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12605 | 12605 | 27239.9 | 0 | PROCESSED | 57539.1100810185 | 54696 | 54328.4686111111 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y |
| VELA JR P8 | 133.862 | -45.8612 | 266.28131071 | -0.45847751 | 347.0005 | 54287.3028240741 | 54287.7009722222 | 502030010 | 13219.6 | 10000 | 13219.6 | 13219.6 | 0 | 13219.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14441 | 14441 | 34391.9 | 0 | PROCESSED | 57539.112662037 | 54703 | 54333.4507175926 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y |
| VELA JR P9 | 133.4161 | -45.7633 | 266.00615013 | -0.63304204 | 347.0009 | 54287.7015856482 | 54287.9516666667 | 502031010 | 13252.4 | 10000 | 13268.4 | 13252.4 | 0 | 13268.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9887.7 | 9887.7 | 21599.9 | 0 | PROCESSED | 57539.1152546296 | 54703 | 54333.4413657407 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y |
| VELA JR P10 | 132.9993 | -45.7656 | 265.8217159 | -0.85784968 | 347.0018 | 54287.9522337963 | 54288.2308564815 | 502032010 | 13040 | 10000 | 13048 | 13040 | 0 | 13056 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10698.8 | 10698.8 | 24067.9 | 0 | PROCESSED | 57539.1146527778 | 54703 | 54333.4328240741 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y |
| VELA JR P11 | 132.5986 | -45.8258 | 265.69032827 | -1.11165473 | 347.0024 | 54288.2314236111 | 54288.6112731482 | 502033010 | 11283.3 | 10000 | 11283.3 | 11283.3 | 0 | 11283.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12207.9 | 12207.9 | 32790.1 | 1 | PROCESSED | 57539.1206828704 | 54696 | 54328.4031944445 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y |
| VELA JR P12 | 132.2515 | -46.051 | 265.71195175 | -1.4410688 | 347.0011 | 54289.0722106482 | 54289.4078009259 | 502034010 | 9947.9 | 10000 | 9947.9 | 9947.9 | 0 | 9947.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10494 | 10494 | 28983.9 | 0 | PROCESSED | 57539.1227546296 | 54696 | 54328.4792939815 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y |
| VELA JR P13 | 131.851 | -46.106 | 265.57984888 | -1.69160478 | 347.0011 | 54290.1290162037 | 54290.4411342593 | 502035010 | 9408.9 | 10000 | 9408.9 | 9408.9 | 0 | 9408.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 8953.1 | 8953.1 | 26963.9 | 0 | PROCESSED | 57539.1321412037 | 54696 | 54328.4906134259 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y |
| VELA JR P14 | 131.9312 | -46.3861 | 265.83284327 | -1.824218 | 347.0017 | 54290.4416087963 | 54290.675150463 | 502036010 | 11034 | 10000 | 11034 | 11042 | 0 | 11042 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11139.1 | 11139.1 | 20167.9 | 0 | PROCESSED | 57539.1311226852 | 54696 | 54328.4740277778 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y |
| VELA JR P15 | 132.3334 | -46.3288 | 265.96324441 | -1.57253381 | 347.0016 | 54291.1946064815 | 54291.46 | 502037010 | 8876 | 10000 | 8876 | 8876 | 0 | 8876 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 7341.1 | 7341.1 | 22912.1 | 1 | PROCESSED | 57539.1396990741 | 54696 | 54328.472962963 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y |
| VELA JR P16 | 132.6844 | -46.1051 | 265.94403391 | -1.24290223 | 347.0001 | 54291.4605671296 | 54291.7363773148 | 502038010 | 16442 | 10000 | 16450 | 16450 | 0 | 16442 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16277 | 16277 | 23823.9 | 1 | PROCESSED | 57539.143900463 | 54696 | 54328.4979398148 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y |
| VELA JR P17 | 133.087 | -46.0455 | 266.0760896 | -0.98967894 | 347.0002 | 54291.7369444444 | 54291.9238773148 | 502039010 | 13032.6 | 10000 | 13064.5 | 13064.6 | 0 | 13032.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8827.2 | 8827.2 | 16143.9 | 0 | PROCESSED | 57539.1455555556 | 54707 | 54333.4040277778 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y |
| VELA JR P18 | 133.5064 | -46.0415 | 266.25968404 | -0.76370949 | 347.0006 | 54291.9244444444 | 54292.1668634259 | 502040010 | 15012.3 | 10000 | 15012.3 | 15036.2 | 0 | 15020.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12895.2 | 12895.2 | 20943.9 | 1 | PROCESSED | 57539.1482407407 | 54696 | 54328.4716666667 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020049 | We propose to perform mapping obervations of the SNR Vela Jr (RX J0852.0-4622). Recent HESS data have revealed a shell-like morphology in TeV gamma-rays, which motivates us to map the remnant's shell with Suzaku XIS and HXD. The sensitivity of Suzaku HXD PIN detector in the 10-50 keV range is high enough to detect the hard X-ray synchrotron emission from the northwest and north rims. With Suzaku XIS, we will measure keV-to-TeV flux ratios in a wide area of the remnant. The Suzaku X-ray data sets, combined with new HESS data, allow us to investigate the origin of TeV gamma-rays and the nature of cosmic-ray acceleration in supernova shells with an unprecedented level. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY MAPPING OF THE BRIGHT TEV SNR VELA JR | XIS | Y |
| SN1006 | 225.7268 | -41.9424 | 327.58003425 | 14.55159393 | 117.0193 | 54521.6264351852 | 54526.8613310185 | 502046010 | 211737.3 | 200000 | 211745.3 | 211737.3 | 0 | 211745.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 184362.2 | 184362.2 | 417275.9 | 6 | PROCESSED | 57541.8622337963 | 54904 | 54535.729375 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020052 | Thermal plasma incident SN1006 has very interesting characteristic. Suzaku PV spectrum revealed ionization parameter of the plasma is significantly low. We investigated the spatial variation of the ionization parameter, and found the outer region of SN1006 has lower ionization parameter than the inner region. However, since the center region of SN1006 is placed on the edge of FOV in the PV observation, the spectra have poor statistics, and the ionization state and the metal abundance cannot be decided with good precision. We propose to observe the center region of SN1006 deeply to decide the physical condition of the plasma of young SNR. Necessary exposure time is 150ksec. | GALACTIC DIFFUSE EMISSION | 5 | A | YAMAGUCHI | HIROYA | NULL | NULL | JAP | 2 | AO2 | THE CENTER REGION OF SN1006 | XIS | Y |
| LOW_LATITUDE_86-21 | 332.3169 | 30.2173 | 86.0039952 | -20.78963339 | 82.7457 | 54229.0809259259 | 54230.9966898148 | 502047010 | 81548.6 | 80000 | 81548.6 | 81548.6 | 0 | 81548.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 72293.1 | 72293.1 | 165509.9 | 2 | PROCESSED | 57538.6557986111 | 54744 | 54244.7948032407 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020061 | High galactic-latitude Suzaku observations of soft X-ray diffuse emission so far made show general tendency that the OVII emission line becomes stronger with decreasing abs(b). This suggests that the major part of the emission is originating from the halo of our galaxy. However, we cannot rule out the possibility that the data is contaminated by solar wind charge exchange emission from the entire heliosphere. In oder to confirm the abs(b) dependency and to constrain the spatial distribution of the halo emission, we propose to observe diffuse radiation at a low galactic latitude of abs(b) ~ 20 deg, where the galactic absorption still does not affect the line intensity significantly. | GALACTIC DIFFUSE EMISSION | 5 | B | YOSHINO | TOMOTAKA | NULL | NULL | JAP | 2 | AO2 | SOFT X-RAY DIFFUSE EMISSION AT A LOW GALACTIC LATITUDE | XIS | Y |
| 47 TUCANAE | 6.2112 | -71.9961 | 305.8317488 | -44.9821189 | 65.5967 | 54261.1765162037 | 54263.5404976852 | 502048010 | 132105.2 | 133000 | 132145.2 | 132105.2 | 0 | 132137.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 132904.2 | 132904.2 | 204231.9 | 1 | PROCESSED | 57538.9491666667 | 54745 | 54271.5258796296 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020066 | We propose a 100 ks observation of the globular cluster 47 Tuc. An extended (~2') hard x-ray emission, presumably of non-thermal origin, was detected with Chandra from a position ~6' toward north east of its center. However, the Chandra ACIS spectrum does not allow us to determine with confidence whether it is a non-thermal emission or a high temperature thermal source. Utilizing the high sensitivity of the XIS, we try to distinguish between these two cases. If confirmed, the result may provide valuable information on particle acceleration in non-relativistic shocks, with potential relations the galactic-ridge x-ray emission. We perform a single pointing observation placing the center of the diffuse emission onto XIS nominal position. | GALACTIC DIFFUSE EMISSION | 5 | B | YUASA | TAKAYUKI | NULL | NULL | JAP | 2 | AO2 | OBSERVATIONAL INVESTIGATION OF PARTICLE ACCELERATION IN A GLOBULAR CLUSTER SHOCK | XIS | Y |
| HESS J1702-420 | 255.6874 | -42.0709 | 344.26217794 | -0.21974248 | 106.4451 | 54550.458599537 | 54555.625162037 | 502049010 | 215693.2 | 200000 | 215705.3 | 215693.2 | 0 | 215705.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 140637.5 | 140637.5 | 395721.5 | 6 | PROCESSED | 57542.1678356482 | 54933 | 54566.9486458333 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020067 | The Galactic Plane Survey with HESS found several new TeV sources, called as "dark particle accelerators". They must be powerful cosmic-ray accelerators, although their origin is still unknown due to the lack of information in other wavelengths. We investigate one of the most mysterious sample, HESS J1702-420, which has the brightest HESS compact source without clear counterparts. ASCA Galactic plane survey shows no evidence of X-ray emission although the exposure was too short. With the large effective area and the low background of XISs, we will be able to detect quite dim counterpart or make strong upper-limit in the hard X-ray band. This result will lead us to distinguish that HESS J1702-420 is the true "dark" protonic accelerator, or a hypothetical PWN powered by PSR J1702-4128. | GALACTIC DIFFUSE EMISSION | 5 | B | BAMBA | AYA | NULL | NULL | JAP | 2 | AO2 | RESOLVING THE DARKEST DARK PARTICLE ACCELERATOR | XIS | Y |
| GC_G0.9+0.1 | 266.9332 | -28.1474 | 0.91503767 | 0.01290063 | 105.8953 | 54536.2637152778 | 54540.229375 | 502051010 | 138761.4 | 133000 | 138761.4 | 138761.4 | 0 | 138761.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 122221.4 | 122221.4 | 342576.8 | 1 | PROCESSED | 57541.9299305556 | 54919 | 54550.6988078704 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020071 | The Suzaku PV observations found that the diffuse X-rays (6.7 and 6.9 keV-lines) from the GC region can well be explained by a thermal emission from hot plasma (6-7 keV). The most plausible energy injection source is multiple SNe. The huge thermal energy (10^54 ergs) and short timescale (10^5 yr) of the hot plasma suggest that the GC region harbors at least 10 young SNRs. To confirm this scenario, we propose to observe the shell of G0.9+0.1 and the connecting region of Sgr B and D. The first objective is to detect a thermal emission from the shell of G0.9+0.1 and the second is to discover new SNRs. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 2 | AO2 | SNR G0.9+0.1 AND THE CONNECTING REGION OF SGR B AND D | XIS | Y |
| M17 EAST | 275.3895 | -16.2062 | 15.15230897 | -0.92571433 | 271.9996 | 54377.3569907407 | 54380.0940277778 | 502052010 | 114569.5 | 107000 | 114577.5 | 114569.5 | 0 | 114577.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 100887.3 | 100887.3 | 236449.8 | 3 | PROCESSED | 57540.2317939815 | 54771 | 54403.5436111111 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020085 | We continue our XIS study of the soft extended X-ray emission in M17. The first study conducted in a region close to the OB association brought a detailed surface brightness distribution and the highest S/N ratio spectrum of the diffuse emission. In this proposed study, we move our eyes to the west to observe another bright emission outside of the previously studied regions. DSS and ROSAT all-sky survey images suggest that this is a shocked region, in which OB stellar winds impinge upon ISM. We aim to obtain the surface brightness map of this region and measure the plasma temperature difference in and out of the possible shocked region. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 2 | AO2 | FURTHER XIS INVESTIGATION OF M17 - X-RAY SPECTROSCOPY OF A POSSIBLE SHOCK BY MASSIVE STAR WINDS - | XIS | Y |
| M17 EAST BKG | 275.6441 | -15.5803 | 15.81995827 | -0.84785909 | 271.9998 | 54380.0947800926 | 54381.7571064815 | 502053010 | 71494 | 67000 | 71494 | 71508.5 | 0 | 71502 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 62554.9 | 62554.9 | 143610 | 1 | PROCESSED | 57540.2032175926 | 54771 | 54403.2344791667 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020085 | We continue our XIS study of the soft extended X-ray emission in M17. The first study conducted in a region close to the OB association brought a detailed surface brightness distribution and the highest S/N ratio spectrum of the diffuse emission. In this proposed study, we move our eyes to the west to observe another bright emission outside of the previously studied regions. DSS and ROSAT all-sky survey images suggest that this is a shocked region, in which OB stellar winds impinge upon ISM. We aim to obtain the surface brightness map of this region and measure the plasma temperature difference in and out of the possible shocked region. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUJIMOTO | MASAHIRO | NULL | NULL | JAP | 2 | AO2 | FURTHER XIS INVESTIGATION OF M17 - X-RAY SPECTROSCOPY OF A POSSIBLE SHOCK BY MASSIVE STAR WINDS - | XIS | Y |
| GALACTIC BULGE | 268.3774 | -29.9651 | 359.99980668 | -2.0020922 | 279.4328 | 54372.0700347222 | 54375.590462963 | 502059010 | 136824 | 133000 | 136824 | 136824 | 0 | 136824 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 110515.6 | 110515.6 | 304130.6 | 2 | PROCESSED | 57540.2260185185 | 54770 | 54402.653275463 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020118 | We propose a 100 ks observation on the Galactic Bulge (b=-2.0) with Suzaku. The origin of thermal diffuse X-ray emission will be for the first time clarified with a fine spectroscopy with Suzaku XIS, especially from the Fe-K line analysis. The non-thermal emission from the Galactic Bulge will be also investigated with HXD-PIN. | GALACTIC DIFFUSE EMISSION | 5 | A | KOKUBUN | MOTOHIDE | NULL | NULL | JAP | 2 | AO2 | INVESTIGATION ON THE GALACTIC BULGE DIFFUSE X-RAY EMISSION WITH SUZAKU | XIS | Y |
| COMET_8P_TUTTLE-P1_BGD-1 | 28.5142 | 5.254 | 150.31676982 | -54.25438929 | 248.4996 | 54471.3338888889 | 54471.5001273148 | 502061010 | 8390 | 6000 | 8390 | 8390 | 0 | 8390 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7441.9 | 7441.9 | 14343.9 | 0 | PROCESSED | 57541.2728935185 | 54908 | 54542.2616319444 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y |
| COMET_8P_TUTTLE-P1_BGD-2 | 28.5654 | 5.0072 | 150.57128999 | -54.45813442 | 248.5002 | 54471.5006018518 | 54471.6876273148 | 502061020 | 5682.1 | 4000 | 5690.1 | 5682.1 | 0 | 5696.7 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 5598 | 5598 | 16151.9 | 0 | PROCESSED | 57541.2728819444 | 54908 | 54542.2619097222 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y |
| COMET_8P_TUTTLE-P1-1 | 27.7163 | 7.989 | 147.31647839 | -52.04673223 | 248.4436 | 54470.5233333333 | 54470.5821759259 | 502062010 | 680.3 | 2000 | 680.3 | 680.3 | 0 | 680.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 632 | 632 | 5080 | 0 | PROCESSED | 57540.9802199074 | 54908 | 54542.4502083333 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y |
| COMET_8P_TUTTLE-P1-2 | 27.9946 | 7.7582 | 147.87340904 | -52.1573456 | 248.4994 | 54470.5826041667 | 54470.6488310185 | 502062020 | 2219.3 | 2000 | 2219.3 | 2219.3 | 0 | 2219.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 2164 | 2164 | 5718 | 0 | PROCESSED | 57540.985162037 | 54908 | 54542.2129166667 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y |
| COMET_8P_TUTTLE-P1-3 | 28.0473 | 7.5049 | 148.10975305 | -52.37174422 | 248.4997 | 54470.6493055556 | 54470.7154861111 | 502062030 | 1963.3 | 2000 | 1963.3 | 1963.3 | 0 | 1963.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 1905 | 1905 | 5718 | 0 | PROCESSED | 57540.9903935185 | 54908 | 54542.2294791667 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y |
| COMET_8P_TUTTLE-P1-4 | 28.0997 | 7.2516 | 148.34803657 | -52.5857522 | 248.4989 | 54470.7159143518 | 54470.7821527778 | 502062040 | 1723.3 | 2000 | 1723.3 | 1723.3 | 0 | 1723.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 1456.7 | 1456.7 | 5722 | 0 | PROCESSED | 57540.9953125 | 54908 | 54542.2187847222 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y |
| COMET_8P_TUTTLE-P1-5 | 28.1493 | 7.0036 | 148.58110255 | -52.79544349 | 248.5006 | 54470.7825810185 | 54470.8487384259 | 502062050 | 1674.6 | 2000 | 1674.6 | 1674.6 | 0 | 1674.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 1703 | 1703 | 5686.1 | 0 | PROCESSED | 57540.9980208333 | 54908 | 54542.2043055556 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y |
| COMET_8P_TUTTLE-P1-6 | 28.2017 | 6.7525 | 148.82276905 | -53.00641332 | 248.5018 | 54470.8491666667 | 54470.9154050926 | 502062060 | 2026.6 | 2000 | 2026.6 | 2026.6 | 0 | 2026.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 2044 | 2044 | 5664 | 0 | PROCESSED | 57541.0007986111 | 54908 | 54542.2318634259 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y |
| COMET_8P_TUTTLE-P1-7 | 28.2572 | 6.4878 | 149.08057764 | -53.2281425 | 248.4991 | 54470.9158333333 | 54470.9820717593 | 502062070 | 3219 | 2000 | 3219 | 3219 | 0 | 3219 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3459 | 3459 | 5664 | 0 | PROCESSED | 57541.0036805556 | 54908 | 54542.2385532407 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y |
| COMET_8P_TUTTLE-P1-8 | 28.3076 | 6.2429 | 149.32011202 | -53.43313536 | 248.4984 | 54470.9825 | 54471.0487384259 | 502062080 | 3219 | 3200 | 3219 | 3219 | 0 | 3219 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3374 | 3374 | 5664 | 0 | PROCESSED | 57541.0065046296 | 54908 | 54542.2264583333 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y |
| COMET_8P_TUTTLE-P1-9 | 28.3593 | 5.9969 | 149.56477648 | -53.63811023 | 248.4989 | 54471.0491666667 | 54471.1154050926 | 502062090 | 3218.6 | 3200 | 3218.6 | 3218.6 | 0 | 3218.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 2439 | 2439 | 5664 | 0 | PROCESSED | 57541.0088425926 | 54908 | 54542.2348611111 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y |
| COMET_8P_TUTTLE-P1-10 | 28.408 | 5.7525 | 149.8061723 | -53.84230192 | 248.5015 | 54471.1158333333 | 54471.1820717593 | 502062100 | 3219.6 | 3200 | 3219.6 | 3219.6 | 0 | 3219.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 2166 | 2166 | 5679.9 | 0 | PROCESSED | 57541.2676967593 | 54908 | 54542.2429513889 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y |
| COMET_8P_TUTTLE-P1-11 | 28.4619 | 5.5053 | 150.05998726 | -54.04643055 | 248.5015 | 54471.1825 | 54471.2487384259 | 502062110 | 3219 | 3200 | 3219 | 3219 | 0 | 3219 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 2035.6 | 2035.6 | 5688 | 0 | PROCESSED | 57541.2689699074 | 54908 | 54542.2871990741 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y |
| COMET_8P_TUTTLE-P1-12 | 28.5143 | 5.2526 | 150.31791041 | -54.25562458 | 248.4993 | 54471.2491666667 | 54471.3154050926 | 502062120 | 3219.6 | 3200 | 3219.6 | 3219.6 | 0 | 3219.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 2162 | 2162 | 5696 | 0 | PROCESSED | 57541.268587963 | 54908 | 54542.261400463 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y |
| COMET_8P_TUTTLE-P1-13 | 28.5683 | 5.0085 | 150.57488577 | -54.45575395 | 248.5007 | 54471.3158333333 | 54471.3334606482 | 502062130 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1503.9 | 0 | PROCESSED | 57541.2672337963 | 54910 | 54544.4202893518 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y |
| COMET_8P_TUTTLE-P2_01 | 39.6412 | -35.6843 | 240.18300744 | -65.68930545 | 257.5577 | 54490.0082291667 | 54490.1627083333 | 502063010 | 4346.8 | 5000 | 4346.8 | 4346.8 | 0 | 4346.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 4402.9 | 4402.9 | 13327.9 | 1 | PROCESSED | 57541.3739236111 | 54912 | 54546.0974189815 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y |
| COMET_8P_TUTTLE-P2_02 | 39.704 | -35.8295 | 240.49763907 | -65.60654763 | 257.6692 | 54490.1630902778 | 54490.2960069444 | 502063020 | 5204.9 | 5000 | 5204.9 | 5204.9 | 0 | 5204.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 5591.9 | 5591.9 | 11449.9 | 0 | PROCESSED | 57541.3791898148 | 54912 | 54546.1091666667 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y |
| COMET_8P_TUTTLE-P2_03 | 39.7649 | -35.9737 | 240.80897167 | -65.5250468 | 257.7596 | 54490.2964351852 | 54490.4293287037 | 502063030 | 6038.9 | 6000 | 6054.9 | 6038.9 | 0 | 6054.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 6601.1 | 6601.1 | 11463.9 | 0 | PROCESSED | 57541.3810532407 | 54912 | 54546.1040046296 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y |
| COMET_8P_TUTTLE-P2_04 | 39.8249 | -36.1145 | 241.11100541 | -65.44459708 | 257.8515 | 54490.4297106482 | 54490.562662037 | 502063040 | 6687.6 | 6700 | 6687.6 | 6719.1 | 0 | 6687.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7388.7 | 7388.7 | 11479.9 | 0 | PROCESSED | 57541.3859375 | 54912 | 54546.1129513889 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y |
| COMET_8P_TUTTLE-P2_05 | 39.8852 | -36.2545 | 241.40935004 | -65.36366996 | 257.9439 | 54490.5630439815 | 54490.6959953704 | 502063050 | 6697.4 | 6700 | 6697.6 | 6697.6 | 0 | 6697.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 6161.9 | 6161.9 | 11479.9 | 0 | PROCESSED | 57541.3887847222 | 54912 | 54546.126712963 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y |
| COMET_8P_TUTTLE-P2_06 | 39.9457 | -36.3936 | 241.70384829 | -65.28238509 | 258.0349 | 54490.6963773148 | 54490.8293287037 | 502063060 | 6690.4 | 6700 | 6690.6 | 6690.6 | 0 | 6690.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 4338 | 4338 | 11479.9 | 0 | PROCESSED | 57541.3927893518 | 54912 | 54546.1201736111 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y |
| COMET_8P_TUTTLE-P2_07 | 40.0041 | -36.5319 | 241.99586619 | -65.20252382 | 258.1285 | 54490.8297106482 | 54490.962662037 | 502063070 | 5267.6 | 5000 | 5291.6 | 5267.6 | 0 | 5299.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 2753 | 2753 | 11479.9 | 0 | PROCESSED | 57541.3952777778 | 54912 | 54546.130462963 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y |
| COMET_8P_TUTTLE-P2_08 | 40.0642 | -36.6693 | 242.2833952 | -65.12116443 | 253.2206 | 54490.9649421296 | 54491.0959953704 | 502063080 | 3541.6 | 4000 | 3549.6 | 3541.6 | 0 | 3557.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 3564 | 3564 | 11311.9 | 0 | PROCESSED | 57541.3990509259 | 54912 | 54546.1411689815 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y |
| COMET_8P_TUTTLE-P2_09 | 40.126 | -36.804 | 242.56232387 | -65.03879756 | 253.3121 | 54491.0963773148 | 54491.2292824074 | 502063090 | 4397.9 | 4000 | 4397.9 | 4397.9 | 0 | 4397.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 4752 | 4752 | 11443.9 | 0 | PROCESSED | 57541.402662037 | 54912 | 54546.2142592593 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y |
| COMET_8P_TUTTLE-P2_10 | 40.1849 | -36.9375 | 242.83840601 | -64.95862507 | 253.4045 | 54491.2297106482 | 54491.362662037 | 502063100 | 5730.4 | 5000 | 5738.4 | 5738.4 | 0 | 5730.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 6209.1 | 6209.1 | 11473.9 | 0 | PROCESSED | 57541.4028472222 | 54912 | 54546.1949884259 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y |
| COMET_8P_TUTTLE-P2_11 | 40.2448 | -37.071 | 243.11250517 | -64.87732742 | 253.5002 | 54491.3630439815 | 54491.4959953704 | 502063110 | 6382.2 | 6700 | 6390.2 | 6382.2 | 0 | 6390.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 6838.5 | 6838.5 | 11479.9 | 0 | PROCESSED | 57541.406712963 | 54912 | 54546.1994097222 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y |
| COMET_8P_TUTTLE-P2_12 | 40.3045 | -37.2045 | 243.38522043 | -64.79583615 | 253.5926 | 54491.4963773148 | 54491.6293287037 | 502063120 | 6608.2 | 6700 | 6608.2 | 6608.2 | 0 | 6624.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 6469.8 | 6469.8 | 11479.9 | 0 | PROCESSED | 57541.4099884259 | 54912 | 54546.2619675926 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y |
| COMET_8P_TUTTLE-P2_13 | 40.3641 | -37.3366 | 243.65335896 | -64.71445889 | 253.6857 | 54491.6297106482 | 54491.762662037 | 502063130 | 6590.7 | 6700 | 6614.7 | 6598.7 | 0 | 6590.7 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 5022.1 | 5022.1 | 11479.9 | 0 | PROCESSED | 57541.4103356482 | 54912 | 54546.2204861111 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y |
| COMET_8P_TUTTLE-P2_14 | 40.423 | -37.4668 | 243.91615364 | -64.63380941 | 253.7796 | 54491.7630439815 | 54491.8959953704 | 502063140 | 6562.7 | 6700 | 6562.7 | 6586.7 | 0 | 6562.7 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3833 | 3833 | 11479.9 | 0 | PROCESSED | 57541.4134143518 | 54912 | 54546.2568518518 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y |
| COMET_8P_TUTTLE-P2_15 | 40.4836 | -37.5961 | 244.17467378 | -64.55180166 | 253.8725 | 54491.8963773148 | 54492.0293287037 | 502063150 | 3471.7 | 4000 | 3479.7 | 3471.7 | 0 | 3487.7 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 2346.1 | 2346.1 | 11479.9 | 1 | PROCESSED | 57541.4238657407 | 54912 | 54546.2153587963 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y |
| COMET_8P_TUTTLE-P2_16 | 40.5411 | -37.7213 | 244.42429467 | -64.47300408 | 253.9693 | 54492.0297106482 | 54492.162662037 | 502063160 | 3770.5 | 4000 | 3770.5 | 3770.5 | 0 | 3770.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3988.1 | 3988.1 | 11479.9 | 0 | PROCESSED | 57541.4170833333 | 54912 | 54546.2311574074 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y |
| COMET_8P_TUTTLE-P2_17 | 40.6015 | -37.8518 | 244.68288405 | -64.39021906 | 254.0645 | 54492.1630439815 | 54492.2959953704 | 502063170 | 5149.5 | 5000 | 5149.5 | 5149.5 | 0 | 5149.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 5414.2 | 5414.2 | 11432 | 0 | PROCESSED | 57541.4188425926 | 54912 | 54546.2465509259 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y |
| COMET_8P_TUTTLE-P2_18 | 40.6547 | -37.9803 | 244.9394556 | -64.31314542 | 254.1595 | 54492.2963773148 | 54492.4293287037 | 502063180 | 6150.5 | 6000 | 6150.5 | 6150.5 | 0 | 6150.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 6613.3 | 6613.3 | 11479.9 | 0 | PROCESSED | 57541.4227083333 | 54912 | 54546.2369675926 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y |
| COMET_8P_TUTTLE-P2_BGD-1 | 40.599 | -37.8517 | 244.68396515 | -64.39213957 | 254.2787 | 54492.4296643518 | 54492.562662037 | 502064010 | 6570.7 | 5000 | 6570.7 | 6602.4 | 0 | 6586.7 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 6629.3 | 6629.3 | 11487.9 | 0 | PROCESSED | 57541.4243518518 | 54912 | 54546.2413888889 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y |
| COMET_8P_TUTTLE-P2_BGD-2 | 40.4817 | -37.5941 | 244.17118034 | -64.55380496 | 254.4101 | 54492.5631365741 | 54492.7293287037 | 502064020 | 6979.7 | 5000 | 6979.7 | 7003.7 | 0 | 6987.7 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 5547.1 | 5547.1 | 14351.9 | 0 | PROCESSED | 57554.5355671296 | 54912 | 54546.2537847222 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021001 | We propose two observations of comet 8P/Tuttle with Suzaku's XIS to measure the composition of the solar wind. The first for 30 ksec on January 6, 2008, the second observation is on January 25 for 100 ksec, when the comet is at perihelion, is 0.479 AU from the Earth, 1.03 AU from the Sun, and has a solar latitude of -20.3 degrees, i.e., when it is located in the transition region of the solar wind. These observations will be simultaneous with the Solar Wind Ion Composition Spectrometer measurements of the Advanced Composition Explorer and the Ulysses satellite. | GALACTIC DIFFUSE EMISSION | 5 | A | BROWN | GREGORY | NULL | NULL | USA | 2 | AO2 | SAMPLING THE SOLAR WIND WITH THE XIS X-RAY SPECTRUM OF THE COMET 8P/TUTTLE | XIS | Y |
| G21.5-0.9 | 278.4035 | -10.5067 | 21.56184596 | -0.8687642 | 103.5554 | 54188.7945023148 | 54189.6252199074 | 502065010 | 25141.6 | 100000 | 25156 | 25141.6 | 0 | 25156 | 1 | 2 | 0 | 1 | 1 | 0 | 0 | 22889 | 22889 | 71769.9 | 1 | PROCESSED | 57538.0286921296 | 54695 | 54209.5181018518 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021211 | We propose an observation of the supernova remnant (SNR) G21.5--0.9. This SNR has a centrally peaked X-ray morphology which coupled with its non-thermal emission, suggested that the SNR's central engine was an undetected pulsar. Last year, a radio pulsar associated with the remnant was discovered (Gupta et al. 2005; Camilo et al. 2006). These announcements concur on the period of the pulsar and its period derivative making it the second highest spin-down luminosity pulsar. Deep Chandra imaging uncovered the missing shell (Matheson & Safi-Harb, 2005). Recent INTEGRAL and SWIFT/BAT slew observations detected G21.5--0.9 at more than 10 and 8 sigma respectively. The proposed observation will be the first self-consistent broad-band timing and spectral analysis from soft to very hard X-ray. | GALACTIC DIFFUSE EMISSION | 5 | B | HARRUS | ILANA | NULL | NULL | USA | 2 | AO2 | SUZAKU OBSERVATIONS OF THE SUPERNOVA REMNANT G21.5-0.9 | HXD | Y |
| G21.5-0.9 | 278.4038 | -10.5066 | 21.56207071 | -0.86897985 | 103.5553 | 54190.0674074074 | 54191.7405671296 | 502065020 | 53526.1 | 100000 | 53526.1 | 53551 | 0 | 53566.1 | 1 | 2 | 0 | 1 | 1 | 0 | 0 | 48618 | 48618 | 144541.8 | 0 | PROCESSED | 57538.0817013889 | 54695 | 54200.5054861111 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021211 | We propose an observation of the supernova remnant (SNR) G21.5--0.9. This SNR has a centrally peaked X-ray morphology which coupled with its non-thermal emission, suggested that the SNR's central engine was an undetected pulsar. Last year, a radio pulsar associated with the remnant was discovered (Gupta et al. 2005; Camilo et al. 2006). These announcements concur on the period of the pulsar and its period derivative making it the second highest spin-down luminosity pulsar. Deep Chandra imaging uncovered the missing shell (Matheson & Safi-Harb, 2005). Recent INTEGRAL and SWIFT/BAT slew observations detected G21.5--0.9 at more than 10 and 8 sigma respectively. The proposed observation will be the first self-consistent broad-band timing and spectral analysis from soft to very hard X-ray. | GALACTIC DIFFUSE EMISSION | 5 | B | HARRUS | ILANA | NULL | NULL | USA | 2 | AO2 | SUZAKU OBSERVATIONS OF THE SUPERNOVA REMNANT G21.5-0.9 | HXD | Y |
| G332.5-5.6 CENTER | 250.7335 | -54.5135 | 332.53119736 | -5.54004522 | 262.5079 | 54330.694224537 | 54331.8731944444 | 502066010 | 70148.8 | 80000 | 70148.8 | 70148.8 | 0 | 70156.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 71490.7 | 71490.7 | 101839.9 | 0 | PROCESSED | 57539.62875 | 54721 | 54354.4910300926 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021216 | We propose to observe G332.5-5.6, a puzzling supernova remnant with several unusual features: high radio polarization, central emission with bilaterally symmetric limbs, and evidence for enhanced nitrogen suggesting interaction with processed circumstellar material. Very little is known about G332.5-5.6, so our observations will provide information on the remnant shock speed, age, and evolutionary state; on the possible presence of nonthermal emission, either due to a pulsar in the center or to shock-accelerated electrons in the limbs; and on abundances, which might identify ejecta emission and allow the classification of the supernova. | GALACTIC DIFFUSE EMISSION | 5 | B | REYNOLDS | STEPHEN | NULL | NULL | USA | 2 | AO2 | G332.5-5.6: AN UNUSUAL SUPERNOVA REMNANT WITH CIRCUMSTELLAR INTERACTION | XIS | Y |
| G332.5-5.6 NE | 251.0925 | -54.3783 | 332.77088512 | -5.61037777 | 77.916 | 54504.4521296296 | 54505.6669444444 | 502067010 | 71192.6 | 80000 | 71200.6 | 71208.6 | 0 | 71192.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 65250.8 | 65250.8 | 104941.8 | 0 | PROCESSED | 57541.5340277778 | 54883 | 54515.6965509259 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021216 | We propose to observe G332.5-5.6, a puzzling supernova remnant with several unusual features: high radio polarization, central emission with bilaterally symmetric limbs, and evidence for enhanced nitrogen suggesting interaction with processed circumstellar material. Very little is known about G332.5-5.6, so our observations will provide information on the remnant shock speed, age, and evolutionary state; on the possible presence of nonthermal emission, either due to a pulsar in the center or to shock-accelerated electrons in the limbs; and on abundances, which might identify ejecta emission and allow the classification of the supernova. | GALACTIC DIFFUSE EMISSION | 5 | B | REYNOLDS | STEPHEN | NULL | NULL | USA | 2 | AO2 | G332.5-5.6: AN UNUSUAL SUPERNOVA REMNANT WITH CIRCUMSTELLAR INTERACTION | XIS | Y |
| G296.1-0.5N | 177.8287 | -62.3875 | 296.02814016 | -0.3243747 | 322.3815 | 54321.2538541667 | 54323.4522453704 | 502068010 | 77175.9 | 67000 | 77175.9 | 77175.9 | 0 | 77175.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 68484.6 | 68484.6 | 189923.7 | 1 | PROCESSED | 57539.4859953704 | 54716 | 54347.5137268518 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021218 | Supernova (SN) explosions within wind-blown bubbles are common among core-collapse (CC) SNe, and are expected to occur for some Type Ia SNe. We propose observations of an X-ray bright supernova remnant (SNR), G296.1-0.5, with very strong evidence for an explosion within a bubble. Spectroscopy with Suzaku will provide us with temperatures, abundances, and ionization ages of the X-ray emitting gas. If we detect SN ejecta, we will distinguish between a CC or a Type Ia progenitor. Gas temperatures will provide us with the shock speeds, while ionization ages will tell us when this gas was shocked. We will infer how progenitor winds affected the ambient medium prior to the explosion. The proposed observations will advance our knowledge of poorly understood SNR evolution in wind-blown bubbles. | GALACTIC DIFFUSE EMISSION | 5 | B | BORKOWSKI | KAZIMIERZ | NULL | NULL | USA | 2 | AO2 | G296.1-0.5: A SUPERNOVA EXPLOSION WITHIN A BUBBLE | XIS | Y |
| G296.1-0.5S | 177.6962 | -62.7172 | 296.04515802 | -0.65925146 | 111.5869 | 54482.7727662037 | 54484.6668402778 | 502069010 | 69213 | 67000 | 69213 | 69213 | 0 | 69213 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 61009.6 | 61009.6 | 163623.7 | 2 | PROCESSED | 57541.3665740741 | 54929 | 54563.4417824074 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021218 | Supernova (SN) explosions within wind-blown bubbles are common among core-collapse (CC) SNe, and are expected to occur for some Type Ia SNe. We propose observations of an X-ray bright supernova remnant (SNR), G296.1-0.5, with very strong evidence for an explosion within a bubble. Spectroscopy with Suzaku will provide us with temperatures, abundances, and ionization ages of the X-ray emitting gas. If we detect SN ejecta, we will distinguish between a CC or a Type Ia progenitor. Gas temperatures will provide us with the shock speeds, while ionization ages will tell us when this gas was shocked. We will infer how progenitor winds affected the ambient medium prior to the explosion. The proposed observations will advance our knowledge of poorly understood SNR evolution in wind-blown bubbles. | GALACTIC DIFFUSE EMISSION | 5 | C | BORKOWSKI | KAZIMIERZ | NULL | NULL | USA | 2 | AO2 | G296.1-0.5: A SUPERNOVA EXPLOSION WITHIN A BUBBLE | XIS | Y |
| ARC1 | 40.8605 | -42.0069 | 253.28744097 | -62.75503946 | 235.1247 | 54480.7980787037 | 54482.7640509259 | 502070010 | 104369.4 | 100000 | 104377.4 | 104385.4 | 0 | 104369.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 115420.2 | 115420.2 | 169837.7 | 3 | PROCESSED | 57541.3640277778 | 54860 | 54490.7270717593 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021222 | Outside of the largest loops in the northern sky, few X-ray bright regions in the Galactic halo are understood. Here, we propose to study of a medium sized (~10 degree) bright feature in the southern sky. The feature is arc-shaped, suspiciously like the edge of a hot bubble. We propose to make three Suzaku observations along a radial line through the arc. With them, we will be able to determine the thermal properties of the region and whether or not the plasma temperature decreases with radius from the projected center, as expected for middle aged supernova remnants. | GALACTIC DIFFUSE EMISSION | 5 | C | SHELTON | ROBIN | NULL | NULL | USA | 2 | AO2 | A CLOSER LOOK AT HOT HALO GAS: AN EXAMINATION OF AN X-RAY BRIGHT ARC | XIS | Y |
| ARC2 | 39.9365 | -39.101 | 247.81076012 | -64.49485898 | 35.5401 | 54256.3120486111 | 54258.149525463 | 502071010 | 105727.1 | 100000 | 105735.1 | 105735.1 | 0 | 105727.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 82923.6 | 82923.6 | 158741.8 | 1 | PROCESSED | 57538.8944097222 | 54702 | 54264.533275463 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021222 | Outside of the largest loops in the northern sky, few X-ray bright regions in the Galactic halo are understood. Here, we propose to study of a medium sized (~10 degree) bright feature in the southern sky. The feature is arc-shaped, suspiciously like the edge of a hot bubble. We propose to make three Suzaku observations along a radial line through the arc. With them, we will be able to determine the thermal properties of the region and whether or not the plasma temperature decreases with radius from the projected center, as expected for middle aged supernova remnants. | GALACTIC DIFFUSE EMISSION | 5 | B | SHELTON | ROBIN | NULL | NULL | USA | 2 | AO2 | A CLOSER LOOK AT HOT HALO GAS: AN EXAMINATION OF AN X-RAY BRIGHT ARC | XIS | Y |
| ARC_BACKGROUND | 39.8321 | -35.8483 | 240.48423372 | -65.50115915 | 257.6627 | 54496.6274537037 | 54499.812662037 | 502072010 | 0 | 100000 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1 | 0 | 0 | 105161 | 105161 | 275153.7 | 4 | PROCESSED | 57541.5227314815 | 54883 | 54515.6371875 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021222 | Outside of the largest loops in the northern sky, few X-ray bright regions in the Galactic halo are understood. Here, we propose to study of a medium sized (~10 degree) bright feature in the southern sky. The feature is arc-shaped, suspiciously like the edge of a hot bubble. We propose to make three Suzaku observations along a radial line through the arc. With them, we will be able to determine the thermal properties of the region and whether or not the plasma temperature decreases with radius from the projected center, as expected for middle aged supernova remnants. | GALACTIC DIFFUSE EMISSION | 5 | C | SHELTON | ROBIN | NULL | NULL | USA | 2 | AO2 | A CLOSER LOOK AT HOT HALO GAS: AN EXAMINATION OF AN X-RAY BRIGHT ARC | XIS | Y |
| MBM20 | 68.9409 | -14.6227 | 211.39642208 | -36.55928879 | 252.4258 | 54507.612025463 | 54510.6980439815 | 502075010 | 107066.8 | 100000 | 107066.8 | 107066.8 | 0 | 107066.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 92803.6 | 92803.6 | 266603.6 | 2 | PROCESSED | 57541.6362847222 | 54889 | 54522.4496527778 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021224 | We propose a study of the X-ray Emission from the Local Bubble (LB) and the Galactic Halo pointing toward the neutral hydrogen cloud MBM20 and a nearby low hydrogen column density, high latitude line of sight (called the Eridanus Hole). MBM20 absorbs about 75% of the foreground emission in the keV energy band, while the Eridanus Hole absorbs only 8%. The shadow of the cloud will be used to study the energy distribution of the X-ray foreground in the energy range 0.4-2 keV, to separate O VII and O VIII lines and study the composition and evolution of the LB. The comparison with the spectrum from the Eridanus Hole will be used to estimate the background emission due to the galactic halo and extragalactic source. | GALACTIC DIFFUSE EMISSION | 5 | B | GALEAZZI | MASSIMILIANO | NULL | NULL | USA | 2 | AO2 | STUDYING THE PROPERTIES OF THE LOCAL BUBBLE AND GALACTIC HALO TOWARD MBM20 | XIS | Y |
| ERIDANUS HOLE | 67.1401 | -17.0746 | 213.43674881 | -39.09232011 | 64.2755 | 54311.0359606482 | 54313.2161921296 | 502076010 | 103752.3 | 100000 | 103752.3 | 103752.3 | 0 | 103752.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 92209.1 | 92209.1 | 188351.8 | 2 | PROCESSED | 57539.4003356482 | 54710 | 54340.7341898148 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021224 | We propose a study of the X-ray Emission from the Local Bubble (LB) and the Galactic Halo pointing toward the neutral hydrogen cloud MBM20 and a nearby low hydrogen column density, high latitude line of sight (called the Eridanus Hole). MBM20 absorbs about 75% of the foreground emission in the keV energy band, while the Eridanus Hole absorbs only 8%. The shadow of the cloud will be used to study the energy distribution of the X-ray foreground in the energy range 0.4-2 keV, to separate O VII and O VIII lines and study the composition and evolution of the LB. The comparison with the spectrum from the Eridanus Hole will be used to estimate the background emission due to the galactic halo and extragalactic source. | GALACTIC DIFFUSE EMISSION | 5 | B | GALEAZZI | MASSIMILIANO | NULL | NULL | USA | 2 | AO2 | STUDYING THE PROPERTIES OF THE LOCAL BUBBLE AND GALACTIC HALO TOWARD MBM20 | XIS | Y |
| G54.1+0.3 | 292.6593 | 18.8091 | 54.05763723 | 0.20765467 | 245.096 | 54403.6644560185 | 54406.3335532407 | 502077010 | 101641.1 | 100000 | 101641.1 | 101649.1 | 0 | 101649.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 92923.5 | 92923.5 | 230585.7 | 3 | PROCESSED | 57540.4530324074 | 54786 | 54417.8870833333 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 022032 | A proprietary XMM-Newton observation reveals that the pulsar wind nebula G54.1+0.3 has a very hard spectrum (gamma ~ 1.5) and possibly a break between 5 and 10 keV. We propose a 100 ks SUZAKU observation to confirm unambiguously the presence of the break. If confirmed, the break would pose stringent constraints on models of electron emission and propagation in pulsar wind nebulae. | GALACTIC DIFFUSE EMISSION | 5 | C | BOCCHINO | FABRIZIO | NULL | NULL | EUR | 2 | AO2 | THE BREAK IN THE HARD X-RAY ENERGY OF THE PULSAR WIND NEBULA G54.1+0.3 | HXD | Y |
| KEPLER | 262.6698 | -21.4886 | 4.51918955 | 6.82146946 | 98.2145 | 54514.1665393518 | 54516.9793287037 | 502078010 | 116963.6 | 100000 | 116963.6 | 116963.6 | 0 | 116963.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 98955.1 | 98955.1 | 242995.6 | 3 | PROCESSED | 57541.7751388889 | 54894 | 54525.6176851852 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 023074 | We propose to observe the Kepler's SNR in which evidence of particle acceleration will be found. Aim of the observation is to determine power-law contribution in the hard-tail spectrum above 10 keV with HXD-PIN. If we also find the Fe-Kb and Ni-K emission lines with XIS which have not observed in any previous missions, temperature and nt parameter of a NEI model will be fixed. The determination will help to distinguish the power-law component from the thermal one. We also memtioned that the amount of Fe and Ni will be a good estimator to determine the type of Kepler's SNR. | GALACTIC DIFFUSE EMISSION | 5 | B | TAMAGAWA | TORU | Park | Sangwook | JUS | 2 | AO2 | SEARCH FOR EVIDENCE OF COSMIC-RAY ACCELERATION IN THE KEPLER'S SNR | XIS | Y |
| RCW86_WEST | 220.2753 | -62.427 | 315.24703456 | -2.20673417 | 96.1553 | 54864.7563194444 | 54866.0134259259 | 503001010 | 53551.9 | 50000 | 53551.9 | 53551.9 | 0 | 53551.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48908.1 | 48908.1 | 108602 | 1 | PROCESSED | 57545.4580324074 | 55329 | 54880.570462963 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030011 | Suzaku PV and AO-1 observations revealed that the 6.4 keV Fe-K line from RCW86 originates from Fe-rich ejecta heated by reverse shock very recently. We propose the mapping observations on whole RCW86 in order to find the structure of the reverse shock by investigating the morphology of the Fe-line emission. At the same time, we can perform the hard X-ray mapping. Using the wideband non-thermal X-ray spectra with great accuracy, we will determine the origin of the TeV gamma-ray emission detected by H.E.S.S. recently. | GALACTIC DIFFUSE EMISSION | 5 | B | YAMAGUCHI | HIROYA | NULL | NULL | JAP | 3 | AO3 | RCW86 MAPPING OBSERVATION | XIS | Y |
| RCW86_NORTH | 220.4956 | -62.2074 | 315.43082177 | -2.04872285 | 96.1584 | 54860.901099537 | 54862.1175231482 | 503002010 | 55376 | 50000 | 55384 | 55384 | 0 | 55376 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 50273.1 | 50273.1 | 105081.8 | 2 | PROCESSED | 57545.4267939815 | 55329 | 54880.5551041667 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030011 | Suzaku PV and AO-1 observations revealed that the 6.4 keV Fe-K line from RCW86 originates from Fe-rich ejecta heated by reverse shock very recently. We propose the mapping observations on whole RCW86 in order to find the structure of the reverse shock by investigating the morphology of the Fe-line emission. At the same time, we can perform the hard X-ray mapping. Using the wideband non-thermal X-ray spectra with great accuracy, we will determine the origin of the TeV gamma-ray emission detected by H.E.S.S. recently. | GALACTIC DIFFUSE EMISSION | 5 | B | YAMAGUCHI | HIROYA | NULL | NULL | JAP | 3 | AO3 | RCW86 MAPPING OBSERVATION | XIS | Y |
| RCW86_SOUTH | 220.8315 | -62.6734 | 315.37853465 | -2.53716675 | 96.1597 | 54862.1182291667 | 54863.3647569445 | 503003010 | 54818.1 | 50000 | 54818.1 | 54818.1 | 0 | 54834.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47348.3 | 47348.3 | 107684.8 | 1 | PROCESSED | 57545.4382175926 | 55329 | 54880.5892361111 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030011 | Suzaku PV and AO-1 observations revealed that the 6.4 keV Fe-K line from RCW86 originates from Fe-rich ejecta heated by reverse shock very recently. We propose the mapping observations on whole RCW86 in order to find the structure of the reverse shock by investigating the morphology of the Fe-line emission. At the same time, we can perform the hard X-ray mapping. Using the wideband non-thermal X-ray spectra with great accuracy, we will determine the origin of the TeV gamma-ray emission detected by H.E.S.S. recently. | GALACTIC DIFFUSE EMISSION | 5 | B | YAMAGUCHI | HIROYA | NULL | NULL | JAP | 3 | AO3 | RCW86 MAPPING OBSERVATION | XIS | Y |
| RCW86_SE | 221.3859 | -62.671 | 315.61056381 | -2.64231092 | 96.79 | 54863.365787037 | 54864.7550115741 | 503004010 | 53327.4 | 50000 | 53359.4 | 53327.4 | 0 | 53359.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47813.6 | 47813.6 | 119987.9 | 0 | PROCESSED | 57545.4381481482 | 55329 | 54880.5420138889 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030011 | Suzaku PV and AO-1 observations revealed that the 6.4 keV Fe-K line from RCW86 originates from Fe-rich ejecta heated by reverse shock very recently. We propose the mapping observations on whole RCW86 in order to find the structure of the reverse shock by investigating the morphology of the Fe-line emission. At the same time, we can perform the hard X-ray mapping. Using the wideband non-thermal X-ray spectra with great accuracy, we will determine the origin of the TeV gamma-ray emission detected by H.E.S.S. recently. | GALACTIC DIFFUSE EMISSION | 5 | B | YAMAGUCHI | HIROYA | NULL | NULL | JAP | 3 | AO3 | RCW86 MAPPING OBSERVATION | XIS | Y |
| ANTICENTER2 | 12.9862 | 62.9112 | 122.98962226 | 0.03950805 | 69.9598 | 54679.0120717593 | 54680.8411921296 | 503006010 | 86110.1 | 80000 | 86123 | 86123 | 0 | 86110.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 106785 | 106785 | 158019.8 | 1 | PROCESSED | 57543.2173726852 | 55070 | 54693.3237847222 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030020 | We propose to observe diffuse radiation from the Galactic plane in the general direction of the anticenter. The ROSAT 3/4 keV band all sky map does not show significant dip in intensity at galactic plane, where the CXB component is totally absorbed by galactic absorption. Thus unknown emission must be compensating the CXB component in this energy band. Our AO-2 observation of a general direction of the anticenter direction gives a clear clue to understand the origin of the mysterious emission. We propose to make additional observation in order to confirm the emission component detected in the AO-2 observation generally exist in the galactic plane. | GALACTIC DIFFUSE EMISSION | 5 | B | MASUI | KENSUKE | NULL | NULL | JAP | 3 | AO3 | SOFT X-RAY DIFFUSE EMISSION FROM THE GALACTIC DISK | XIS | Y |
| GC_LARGEPROJECT1 | 266.4387 | -28.5683 | 0.32941305 | 0.16640393 | 260.8767 | 54711.4273958333 | 54712.9530555556 | 503007010 | 52152.3 | 50000 | 52152.3 | 52152.3 | 0 | 52152.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44183.8 | 44183.8 | 131793.8 | 2 | PROCESSED | 57543.7627546296 | 54557 | 54780.6858796296 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y |
| GC_LARGEPROJECT2 | 266.7785 | -29.1292 | 0.00479668 | -0.37932142 | 260.8763 | 54712.9538078704 | 54714.2891087963 | 503008010 | 53638.8 | 50000 | 53654.8 | 53638.8 | 0 | 53654.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42811.1 | 42811.1 | 115333.8 | 0 | PROCESSED | 57543.7762615741 | 54557 | 54780.4880092593 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y |
| GC_LARGEPROJECT3 | 266.4525 | -29.3384 | 359.67825031 | -0.24492188 | 260.8779 | 54714.2896759259 | 54715.6634722222 | 503009010 | 52397.5 | 50000 | 52405.5 | 52397.5 | 0 | 52411.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40269.1 | 40269.1 | 118677.8 | 2 | PROCESSED | 57543.769375 | 54557 | 54780.6767476852 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y |
| GC_LARGEPROJECT4 | 266.0398 | -29.5556 | 359.30535174 | -0.05184233 | 261.05 | 54715.6640393518 | 54717.0690277778 | 503010010 | 53105.6 | 50000 | 53121.6 | 53105.6 | 0 | 53113.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37064.6 | 37064.6 | 121366 | 1 | PROCESSED | 57543.7725694444 | 54557 | 54780.6585648148 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y |
| GC_LARGEPROJECT5 | 265.9469 | -29.8331 | 359.02671432 | -0.12852462 | 265.43 | 54717.3806597222 | 54718.8981365741 | 503011010 | 57633.4 | 50000 | 57633.4 | 57633.4 | 0 | 57633.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40155.5 | 40155.5 | 131099.8 | 1 | PROCESSED | 57543.8408449074 | 54557 | 54780.6683912037 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y |
| GC_LARGEPROJECT6 | 266.2992 | -29.9408 | 359.09468885 | -0.44519015 | 265.9621 | 54723.8160532407 | 54725.0348842593 | 503012010 | 57685.5 | 50000 | 57693.5 | 57685.5 | 0 | 57698.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51903.2 | 51903.2 | 105287.8 | 1 | PROCESSED | 57543.8433217593 | 54557 | 54780.6521643518 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y |
| GC_LARGEPROJECT7 | 265.6744 | -30.0704 | 358.7007591 | -0.05229538 | 265.9998 | 54725.0356365741 | 54727.1975 | 503013010 | 104769 | 100000 | 104777 | 104777 | 0 | 104769 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 93901.3 | 93901.3 | 186709.8 | 3 | PROCESSED | 57543.8883564815 | 54557 | 54780.5885532407 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y |
| GC_LARGEPROJECT8 | 265.1842 | -30.7499 | 357.90048261 | -0.05223369 | 268.8911 | 54727.1991782407 | 54728.3141203704 | 503014010 | 55365.1 | 50000 | 55365.1 | 55389.1 | 0 | 55365.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51206.9 | 51206.9 | 96311.8 | 1 | PROCESSED | 57543.8756481482 | 54557 | 54783.7018055556 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y |
| GC_LARGEPROJECT9 | 265.0297 | -30.9626 | 357.64981902 | -0.05267713 | 269.1132 | 54728.3146412037 | 54729.4140393518 | 503015010 | 56771.6 | 50000 | 56779.6 | 56771.6 | 0 | 56787.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 52845.4 | 52845.4 | 94975.9 | 0 | PROCESSED | 57543.8851041667 | 54557 | 54780.4933564815 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y |
| GC_LARGEPROJECT10 | 264.8736 | -31.1751 | 357.39875369 | -0.05245192 | 268.5898 | 54731.2832060185 | 54732.3383912037 | 503016010 | 52171.2 | 50000 | 52171.2 | 52179.2 | 0 | 52179.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 49291.3 | 49291.3 | 91163.9 | 1 | PROCESSED | 57543.9863425926 | 54557 | 54780.6078935185 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y |
| GC_LARGEPROJECT11 | 264.7183 | -31.3859 | 357.14965021 | -0.05250387 | 268.3335 | 54732.3390046296 | 54733.3897337963 | 503017010 | 51286.5 | 50000 | 51294.5 | 51286.5 | 0 | 51302.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48583.4 | 48583.4 | 90775.9 | 2 | PROCESSED | 57543.9868287037 | 54557 | 54780.6941550926 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y |
| GC_LARGEPROJECT12 | 264.5602 | -31.5978 | 356.8985011 | -0.05173107 | 288.0843 | 54733.394375 | 54733.9377777778 | 503018010 | 29401.2 | 50000 | 29412.5 | 29412.5 | 0 | 29401.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26671.6 | 26671.6 | 46942 | 0 | PROCESSED | 57543.9951851852 | 54557 | 54780.4814583333 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y |
| GC_LARGEPROJECT12 | 264.5606 | -31.5967 | 356.89961278 | -0.05143068 | 268.4538 | 54742.7536226852 | 54743.154375 | 503018020 | 12246.6 | 10000 | 12246.6 | 12246.6 | 0 | 12246.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10232 | 10232 | 34617.9 | 1 | PROCESSED | 57544.0096527778 | 54557 | 54780.5624652778 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y |
| GC_LARGEPROJECT12 | 264.5561 | -31.5945 | 356.89942182 | -0.04701536 | 96.416 | 54881.313900463 | 54881.6919444445 | 503018030 | 11914 | 10000 | 11922 | 11922 | 0 | 11914 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10090.9 | 10090.9 | 32657.9 | 1 | PROCESSED | 57545.5776041667 | 54557 | 54895.5872106482 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y |
| GC_LARGEPROJECT13 | 264.4001 | -31.8052 | 356.65040302 | -0.04773216 | 95.4712 | 54881.6929282407 | 54883.0522453704 | 503019010 | 52776.4 | 50000 | 52776.4 | 52797.2 | 0 | 52784.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42439.5 | 42439.5 | 117433.8 | 0 | PROCESSED | 57545.6322106482 | 54557 | 54902.1118171296 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y |
| GC_LARGEPROJECT14 | 264.2413 | -32.0163 | 356.39993487 | -0.04727305 | 95.7088 | 54883.0527199074 | 54884.7911342593 | 503020010 | 61044.1 | 50000 | 61068.1 | 61044.1 | 0 | 61060.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51718.5 | 51718.5 | 150131.9 | 1 | PROCESSED | 57545.6307175926 | 54557 | 54895.6029166667 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y |
| GC_LARGEPROJECT15 | 265.2338 | -30.2129 | 358.37855715 | 0.19604348 | 267.777 | 54743.1555902778 | 54744.4565277778 | 503021010 | 53826 | 50000 | 53834 | 53834 | 0 | 53826 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 49640.5 | 49640.5 | 112378.1 | 0 | PROCESSED | 57544.0429861111 | 54557 | 54780.430150463 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030022 | We propose a big project of the Galactic center (GC), with a main objective to reveal the origin of the Galactic center and Galactic ridge diffuse X-ray (GCDX/GRDX), particularly those of the 6.4 keV and 6.7/6.96 keV lines. As for the GCDX, we have already found many facts to support that, neither 6.7 keV nor 6.4 keV is attributable to a single origin like integrated point sources. In this project, we will extend the same study to the GRDX, and solve the origin of the GRDX and reveal possible relation to the GCDX. In addition, the GC region is a treasure house of high energy astrophysics, hence will certainly produce many scientific results (many refereed papers), as we have already demonstrated in the PV and AO1 phase observations: 12 accepted refereed papers with 1.2 M-sec observations. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 3 | AO3 | ORIGIN OF THE DIFFUSE X-RAYS FROM THE GALACTIC CENTER AND RIDGE | XIS | Y |
| LOOP 1 L=356.00 | 263.2426 | -31.9466 | 356.00010804 | 0.70279756 | 93.3363 | 54908.96625 | 54909.8933333333 | 503022010 | 41319.3 | 40000 | 41319.3 | 41319.3 | 0 | 41319.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34318.7 | 34318.7 | 80069.9 | 0 | PROCESSED | 57545.8730671296 | 55330 | 54923.2640162037 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030023 | NANTEN telescope discovered huge molecular loops in the galactic center region. The model that the huge loops is due to magnetic buoyancy caused by the Parkey instability is proposed. The loops size is 12 order of magnitude larger than the solar loops, but the physics would be common. X-ray emission from shock heated and/or accelerated particles would be expected at the foot point of the loops. We propose an X-ray observation at the foot point of the molecular loop with Suzaku and investigate the magnetic activity in the galactic scale. | GALACTIC DIFFUSE EMISSION | 5 | C | YAMAUCHI | SHIGEO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF MOLECULAR LOOPS IN THE GALACTIC CENTER | XIS | Y |
| LOOP 2 L=356.33 | 263.4562 | -31.667 | 356.33349006 | 0.70266893 | 94.2779 | 54916.2757060185 | 54917.0786921296 | 503023010 | 31152.7 | 40000 | 31152.7 | 31152.7 | 0 | 31152.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28234.6 | 28234.6 | 69369.9 | 0 | PROCESSED | 57545.9012615741 | 55330 | 54930.234849537 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030023 | NANTEN telescope discovered huge molecular loops in the galactic center region. The model that the huge loops is due to magnetic buoyancy caused by the Parkey instability is proposed. The loops size is 12 order of magnitude larger than the solar loops, but the physics would be common. X-ray emission from shock heated and/or accelerated particles would be expected at the foot point of the loops. We propose an X-ray observation at the foot point of the molecular loop with Suzaku and investigate the magnetic activity in the galactic scale. | GALACTIC DIFFUSE EMISSION | 5 | C | YAMAUCHI | SHIGEO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF MOLECULAR LOOPS IN THE GALACTIC CENTER | XIS | Y |
| HESS J1800-240A | 270.4845 | -23.9659 | 6.13495239 | -0.62617494 | 86.9255 | 54558.6209606482 | 54559.3266087963 | 503025010 | 34782.2 | 30000 | 34782.2 | 34790.2 | 0 | 34790.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25703.3 | 25703.3 | 60967.9 | 0 | PROCESSED | 57542.0259837963 | 54953 | 54574.0504861111 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030043 | H.E.S.S. observations (2004--2006) have revealed extended TeV gamma-ray emission in the W28 regin. The strongest gamma-ray emission is located in a region outside of baundary of SNR W28 towards the south of it. We propose Suzaku observations (90 ksec in 3x30 ksec pointings) of this southern gamma-ray source for which, at present, no dedicated coverage at X-ray energies exists. A potential counterpart for this TeV gamma-ray source is the ultra-compact HII region W28A2, exhibiting a powerful bipolar molecular outflow and being a bright radio and IR source. With the X-ray data, we will be able to test this hypothesis, and also to unveil the role that the relatively old SNR W28 plays in this part of the unique region. | GALACTIC DIFFUSE EMISSION | 5 | A | TANAKA | TAKAAKI | NULL | NULL | JAP | 3 | AO3 | OBSERVATION OF NEWLY DISCOVERED TEV GAMMA-RAY SOURCES IN THE W28 REGION | XIS | Y |
| HESS J1800-240B | 270.1124 | -24.0578 | 5.8867537 | -0.376417 | 87.1402 | 54562.3157523148 | 54563.0141666667 | 503026010 | 31672.8 | 30000 | 31672.8 | 31672.8 | 0 | 31672.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 26769.8 | 26769.8 | 60320 | 1 | PROCESSED | 57542.2491319444 | 54953 | 54580.1793402778 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030043 | H.E.S.S. observations (2004--2006) have revealed extended TeV gamma-ray emission in the W28 regin. The strongest gamma-ray emission is located in a region outside of baundary of SNR W28 towards the south of it. We propose Suzaku observations (90 ksec in 3x30 ksec pointings) of this southern gamma-ray source for which, at present, no dedicated coverage at X-ray energies exists. A potential counterpart for this TeV gamma-ray source is the ultra-compact HII region W28A2, exhibiting a powerful bipolar molecular outflow and being a bright radio and IR source. With the X-ray data, we will be able to test this hypothesis, and also to unveil the role that the relatively old SNR W28 plays in this part of the unique region. | GALACTIC DIFFUSE EMISSION | 5 | A | TANAKA | TAKAAKI | NULL | NULL | JAP | 3 | AO3 | OBSERVATION OF NEWLY DISCOVERED TEV GAMMA-RAY SOURCES IN THE W28 REGION | XIS | Y |
| HESS J1800-240C | 269.7173 | -24.0469 | 5.71665641 | -0.05804766 | 87.3071 | 54563.0147337963 | 54563.6877662037 | 503027010 | 30975.5 | 30000 | 30975.5 | 30975.5 | 0 | 30975.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27815.5 | 27815.5 | 58123.9 | 1 | PROCESSED | 57542.2510185185 | 54953 | 54580.1897453704 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030043 | H.E.S.S. observations (2004--2006) have revealed extended TeV gamma-ray emission in the W28 regin. The strongest gamma-ray emission is located in a region outside of baundary of SNR W28 towards the south of it. We propose Suzaku observations (90 ksec in 3x30 ksec pointings) of this southern gamma-ray source for which, at present, no dedicated coverage at X-ray energies exists. A potential counterpart for this TeV gamma-ray source is the ultra-compact HII region W28A2, exhibiting a powerful bipolar molecular outflow and being a bright radio and IR source. With the X-ray data, we will be able to test this hypothesis, and also to unveil the role that the relatively old SNR W28 plays in this part of the unique region. | GALACTIC DIFFUSE EMISSION | 5 | A | TANAKA | TAKAAKI | NULL | NULL | JAP | 3 | AO3 | OBSERVATION OF NEWLY DISCOVERED TEV GAMMA-RAY SOURCES IN THE W28 REGION | XIS | Y |
| HESS J1825-137 | 276.5024 | -13.9965 | 17.60816681 | -0.84042551 | 271.0002 | 54754.9096064815 | 54756.458599537 | 503028010 | 57210.4 | 50000 | 57210.4 | 57210.4 | 0 | 57210.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51548.5 | 51548.5 | 133793.8 | 1 | PROCESSED | 57544.1955324074 | 55148 | 54780.7053703704 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030044 | The TeV gamma-ray source HESS J1825-137 has been discovered in a survey of the Galactic plane performed by HESS. This source is one of the most interesting source in the HESS catalog since it is the first and the only TeV gamma-ray emitter that shows energy dependent morphology. However, all the gamma-ray emitting region is not covered by X-ray observatories. We propose Suzaku observations of HESS J1825-137 region, which has not been covered by other X-ray satellites. By comparing the spectral and morphological properties of X-ray emission with those of TeV gamma-rays, we can probe the morophology and strength of the magnetic fiels, which should reveal the physical processes of acceleration, diffusion, and radiation of relativistic electrons. | GALACTIC DIFFUSE EMISSION | 5 | B | TANAKA | TAKAAKI | NULL | NULL | JAP | 3 | AO3 | MAPPING OBSERVATIONS OF HESS J1825-137 | XIS | Y |
| HESS_J1825-137_2 | 276.1969 | -13.7002 | 17.73170044 | -0.43977824 | 271.0001 | 54756.4591666667 | 54758.1953009259 | 503029010 | 57199.3 | 50000 | 57199.3 | 57199.3 | 0 | 57199.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51185 | 51185 | 149985.8 | 0 | PROCESSED | 57544.2276157407 | 55148 | 54780.5081365741 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030044 | The TeV gamma-ray source HESS J1825-137 has been discovered in a survey of the Galactic plane performed by HESS. This source is one of the most interesting source in the HESS catalog since it is the first and the only TeV gamma-ray emitter that shows energy dependent morphology. However, all the gamma-ray emitting region is not covered by X-ray observatories. We propose Suzaku observations of HESS J1825-137 region, which has not been covered by other X-ray satellites. By comparing the spectral and morphological properties of X-ray emission with those of TeV gamma-rays, we can probe the morophology and strength of the magnetic fiels, which should reveal the physical processes of acceleration, diffusion, and radiation of relativistic electrons. | GALACTIC DIFFUSE EMISSION | 5 | B | TANAKA | TAKAAKI | NULL | NULL | JAP | 3 | AO3 | MAPPING OBSERVATIONS OF HESS J1825-137 | XIS | Y |
| HESS_J1825-137_3 | 276.1966 | -13.9971 | 17.46909054 | -0.57831059 | 271.0001 | 54758.195775463 | 54759.7917476852 | 503030010 | 55499.6 | 50000 | 55499.6 | 55499.6 | 0 | 55499.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47325.2 | 47325.2 | 137837.9 | 1 | PROCESSED | 57544.2257407407 | 55148 | 54780.7804050926 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030044 | The TeV gamma-ray source HESS J1825-137 has been discovered in a survey of the Galactic plane performed by HESS. This source is one of the most interesting source in the HESS catalog since it is the first and the only TeV gamma-ray emitter that shows energy dependent morphology. However, all the gamma-ray emitting region is not covered by X-ray observatories. We propose Suzaku observations of HESS J1825-137 region, which has not been covered by other X-ray satellites. By comparing the spectral and morphological properties of X-ray emission with those of TeV gamma-rays, we can probe the morophology and strength of the magnetic fiels, which should reveal the physical processes of acceleration, diffusion, and radiation of relativistic electrons. | GALACTIC DIFFUSE EMISSION | 5 | B | TANAKA | TAKAAKI | NULL | NULL | JAP | 3 | AO3 | MAPPING OBSERVATIONS OF HESS J1825-137 | XIS | Y |
| VELA JR P19 | 133.9797 | -46.1476 | 266.55257885 | -0.58147519 | 346.9993 | 54650.629849537 | 54651.2362731482 | 503031010 | 19817.4 | 10000 | 19817.4 | 19817.4 | 0 | 19817.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17156.4 | 17156.4 | 52383.9 | 1 | PROCESSED | 57542.9517824074 | 55036 | 54665.3240393518 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y |
| VELA JR P20 | 133.6175 | -46.3272 | 266.52787238 | -0.88873335 | 346.9997 | 54651.2368402778 | 54651.5828009259 | 503032010 | 16823.7 | 10000 | 16823.7 | 16831.7 | 0 | 16831.7 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 14798.2 | 14798.2 | 29887.9 | 0 | PROCESSED | 57542.9499074074 | 55036 | 54665.3228125 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y |
| VELA JR P21 | 133.1972 | -46.3295 | 266.34323773 | -1.11269222 | 347.0005 | 54651.5833680556 | 54652.0557175926 | 503033010 | 14287.2 | 10000 | 14295.2 | 14287.2 | 0 | 14303.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12066.5 | 12066.5 | 40801.9 | 1 | PROCESSED | 57542.9629398148 | 55036 | 54665.3234375 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y |
| VELA JR P22 | 132.4428 | -46.6127 | 266.23093455 | -1.69368029 | 346.9992 | 54652.0565625 | 54652.3891087963 | 503034010 | 15264.3 | 10000 | 15264.3 | 15270.9 | 0 | 15270.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14971.7 | 14971.7 | 28728 | 0 | PROCESSED | 57542.966099537 | 55036 | 54670.1353125 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y |
| VELA JR P23 | 132.7881 | -46.3947 | 266.21323714 | -1.3716571 | 347.0013 | 54652.3896759259 | 54652.7710416667 | 503035010 | 15690.1 | 10000 | 15698.1 | 15690.1 | 0 | 15706.1 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11039 | 11039 | 32943.9 | 1 | PROCESSED | 57542.9759490741 | 55031 | 54664.7904513889 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y |
| VELA JR P24 | 132.0303 | -46.6729 | 266.0989339 | -1.95139979 | 347.001 | 54652.7719328704 | 54653.1668865741 | 503036010 | 12373.5 | 10000 | 12373.5 | 12373.5 | 0 | 12373.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12254.8 | 12254.8 | 34120 | 1 | PROCESSED | 57542.9791203704 | 55048 | 54679.3185763889 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y |
| VELA JR P25 | 132.5224 | -46.8921 | 266.48184745 | -1.82836861 | 347.0024 | 54653.1675462963 | 54653.4335532407 | 503037010 | 13160 | 10000 | 13160 | 13160 | 0 | 13160 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12432.5 | 12432.5 | 22975.9 | 0 | PROCESSED | 57542.9817476852 | 55048 | 54679.3166203704 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y |
| VELA JR P26 | 132.8787 | -46.6693 | 266.46476457 | -1.49839932 | 347.0019 | 54653.4341203704 | 54653.837025463 | 503038010 | 14553 | 10000 | 14553 | 14553 | 0 | 14553 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10953.6 | 10953.6 | 34783.9 | 0 | PROCESSED | 57542.9869675926 | 55048 | 54679.3709606482 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y |
| VELA JR P27 | 133.2844 | -46.6061 | 266.59417196 | -1.24373956 | 347.0008 | 54653.8375925926 | 54654.1668865741 | 503039010 | 11033.7 | 10000 | 11041.7 | 11041.7 | 0 | 11033.7 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11337.2 | 11337.2 | 28447.9 | 0 | PROCESSED | 57542.9844560185 | 55048 | 54679.3497222222 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y |
| VELA JR P28 | 133.7109 | -46.6037 | 266.78076878 | -1.01777641 | 347.0004 | 54654.1674537037 | 54654.4259143518 | 503040010 | 13093 | 10000 | 13101 | 13093 | 0 | 13101 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12054 | 12054 | 22296 | 0 | PROCESSED | 57542.9904282407 | 55048 | 54679.3674421296 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y |
| VELA JR P29 | 134.0711 | -46.43 | 266.80859879 | -0.71638658 | 347 | 54654.4264814815 | 54654.7203703704 | 503041010 | 11368.5 | 10000 | 11380.2 | 11368.5 | 0 | 11380.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8222.5 | 8222.5 | 25367.9 | 0 | PROCESSED | 57542.9909606482 | 55048 | 54679.3958217593 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y |
| VELA JR P30 | 134.1665 | -46.7036 | 267.059354 | -0.84402772 | 347.0006 | 54654.7208449074 | 54655.0844328704 | 503042010 | 10115.9 | 10000 | 10115.9 | 10115.9 | 0 | 10115.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10053.6 | 10053.6 | 31383.9 | 0 | PROCESSED | 57542.9967592593 | 55048 | 54679.397962963 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y |
| VELA JR P31 | 133.8003 | -46.8845 | 267.03483855 | -1.15221367 | 347.0003 | 54655.085 | 54655.3273032407 | 503043010 | 11209.5 | 10000 | 11217.5 | 11225.5 | 0 | 11209.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11542 | 11542 | 20927.9 | 0 | PROCESSED | 57542.9998263889 | 55048 | 54679.372974537 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y |
| VELA JR P32 | 133.3695 | -46.8865 | 266.8467839 | -1.37881435 | 347.0018 | 54655.3279166667 | 54655.5648032407 | 503044010 | 11264.9 | 10000 | 11272.9 | 11264.9 | 0 | 11280.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8337.5 | 8337.5 | 20455.9 | 0 | PROCESSED | 57543.0006828704 | 55048 | 54679.381087963 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y |
| VELA JR P33 | 133.4681 | -47.1616 | 267.10091899 | -1.50393046 | 347.0007 | 54655.5652777778 | 54656.0084837963 | 503045010 | 12015.5 | 10000 | 12015.5 | 12015.5 | 0 | 12015.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11011.6 | 11011.6 | 38289.9 | 0 | PROCESSED | 57543.0047106482 | 55048 | 54679.4195601852 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y |
| VELA JR P34 | 132.1138 | -46.9499 | 266.35035002 | -2.0812575 | 347.0005 | 54656.0096990741 | 54656.2634143518 | 503046010 | 11042.1 | 10000 | 11058.1 | 11042.1 | 0 | 11058.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11130.6 | 11130.6 | 21916 | 0 | PROCESSED | 57543.0076967593 | 55037 | 54670.2236342593 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y |
| VELA JR P35 | 132.966 | -46.9473 | 266.71715615 | -1.62954887 | 347.0008 | 54656.2642592593 | 54656.5141087963 | 503047010 | 11562.1 | 10000 | 11586.1 | 11562.1 | 0 | 11594.1 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9619.8 | 9619.8 | 21583.9 | 0 | PROCESSED | 57543.0120486111 | 55037 | 54670.2319212963 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y |
| VELA JR P36 | 133.0606 | -47.2239 | 266.97132611 | -1.75647675 | 346.9998 | 54656.5145833333 | 54656.9168634259 | 503048010 | 11122.6 | 10000 | 11130.6 | 11122.6 | 0 | 11138.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 9383.8 | 9383.8 | 34749.9 | 1 | PROCESSED | 57543.0132175926 | 55037 | 54670.2692361111 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y |
| VELA JR P37 | 132.6136 | -47.1701 | 266.73640279 | -1.95651055 | 346.9993 | 54656.9174768518 | 54657.2418287037 | 503049010 | 12529.4 | 10000 | 12541.4 | 12529.4 | 0 | 12545.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12852.7 | 12852.7 | 28020 | 0 | PROCESSED | 57543.0205671296 | 55037 | 54670.278900463 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y |
| VELA JR P38 | 132.2003 | -47.2308 | 266.60579829 | -2.21244802 | 347.0003 | 54657.2423958333 | 54657.5209953704 | 503050010 | 14043.6 | 10000 | 14043.6 | 14043.6 | 0 | 14059.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11426 | 11426 | 24063.9 | 0 | PROCESSED | 57543.0197800926 | 55037 | 54670.2561111111 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030048 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southern hemisphere of the remnant. Suzaku XIS images obtained by our AO3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) detecting hard X-ray emission with the HXD PIN, (2) measureing a keV-to-TeV ratio over the face of the remnant, and (3) confirming the presence of thermal X-ray emission in Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIYAMA | YASUNOBU | NULL | NULL | JAP | 3 | AO3 | COMPLETING SUZAKU MAPPING OF VELA JR SNR | XIS | Y |
| WESTERLUND 2 | 156.0088 | -57.7448 | 284.2643696 | -0.3172737 | 343.7602 | 54687.6527199074 | 54689.327962963 | 503053010 | 73670 | 100000 | 73670 | 73670 | 0 | 73670 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 86577.6 | 86577.6 | 144729.8 | 0 | PROCESSED | 57543.2480555556 | 55252 | 54706.476412037 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030059 | Although young open clusters with many massive stars have been recognized as gamma-ray sources, the emission mechanism of the gamma-ray is hardly known. We propose a Suzaku observation of an open cluster Westerlund 2 (RCW 49), from which gamma-ray emission has been detected with H.E.S.S. We observe this cluster to detect X-ray nonthermal emission from open clusters with TeV gamma-ray emission for the first time. We try to find out whether the emission comes from electrons or protons, and discuss the particle acceleration in open clusters. | GALACTIC DIFFUSE EMISSION | 5 | A | FUJITA | YUTAKA | NULL | NULL | JAP | 3 | AO3 | NONTHERMAL EMISSION FROM AN OPEN CLUSTER WESTERLUND 2 | XIS | Y |
| WESTERLUND 2 | 155.9878 | -57.7462 | 284.25564056 | -0.32444098 | 166.5036 | 54866.5949189815 | 54867.1669444444 | 503053020 | 33492.4 | 30000 | 33500.4 | 33492.4 | 0 | 33500.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32073 | 32073 | 49415.9 | 1 | PROCESSED | 57545.4584606482 | 55329 | 54880.5574189815 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030059 | Although young open clusters with many massive stars have been recognized as gamma-ray sources, the emission mechanism of the gamma-ray is hardly known. We propose a Suzaku observation of an open cluster Westerlund 2 (RCW 49), from which gamma-ray emission has been detected with H.E.S.S. We observe this cluster to detect X-ray nonthermal emission from open clusters with TeV gamma-ray emission for the first time. We try to find out whether the emission comes from electrons or protons, and discuss the particle acceleration in open clusters. | GALACTIC DIFFUSE EMISSION | 5 | A | FUJITA | YUTAKA | NULL | NULL | JAP | 3 | AO3 | NONTHERMAL EMISSION FROM AN OPEN CLUSTER WESTERLUND 2 | XIS | Y |
| RCW 38 | 134.7638 | -47.5154 | 267.93999829 | -1.06526988 | 109.8553 | 54788.5064351852 | 54790.699525463 | 503054010 | 81537.7 | 80000 | 81549.5 | 81537.7 | 0 | 81541.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 60928.1 | 60928.1 | 189459.7 | 1 | PROCESSED | 57544.5092013889 | 55171 | 54811.741099537 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030069 | We propose to make Suzaku observation of HII region RCW 38 for 80 ksec in order to study non-thermal phenomena in a massive star-forming region. The region is thought to be a site of high energy particle acceleration by interaction of strong stellar wind from high-mass stars. The main purpose is to observe extended emission from RCW 38. The high resolution spectroscopy by XIS enables us to distinguish non-thermal emission from thermal component and to obtain properties of non-thermal component. In addition, HXD will detect non-thermal radiation from RCW 38. | GALACTIC DIFFUSE EMISSION | 5 | C | ODAKA | HIROKAZU | NULL | NULL | JAP | 3 | AO3 | SEARCH FOR NONTHERMAL RADIATION FROM MASSIVE STAR-FORMING REGION RCW 38 | XIS | Y |
| CYGNUS LOOP (P11) | 312.4425 | 31.5127 | 74.4826992 | -7.83027866 | 49.9999 | 54595.9014814815 | 54596.7391087963 | 503055010 | 31894.7 | 25000 | 31902.7 | 31894.7 | 0 | 31910.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25073.8 | 25073.8 | 72359.9 | 0 | PROCESSED | 57542.4981712963 | 54972 | 54606.1436342593 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030074 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks. | GALACTIC DIFFUSE EMISSION | 5 | B | TSUNEMI | HIROSHI | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATIONS OF THE CYGNUS LOOP | XIS | Y |
| CYGNUS LOOP (P20) | 311.9894 | 31.1824 | 73.97872298 | -7.73281487 | 50.0002 | 54596.7397685185 | 54597.51 | 503056010 | 30112.9 | 25000 | 30112.9 | 30134.3 | 0 | 30120.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27205.7 | 27205.7 | 66533.9 | 0 | PROCESSED | 57545.8695023148 | 54972 | 54606.1121759259 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030074 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks. | GALACTIC DIFFUSE EMISSION | 5 | B | TSUNEMI | HIROSHI | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATIONS OF THE CYGNUS LOOP | XIS | Y |
| CYGNUS LOOP (P21) | 313.196 | 32.4197 | 75.60030214 | -7.75821821 | 61.9243 | 54619.9401967593 | 54620.2975 | 503057010 | 16170.3 | 15000 | 16178.3 | 16170.3 | 0 | 16178.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12890.3 | 12890.3 | 30863.9 | 0 | PROCESSED | 57542.700474537 | 55003 | 54636.2238078704 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030074 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks. | GALACTIC DIFFUSE EMISSION | 5 | B | TSUNEMI | HIROSHI | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATIONS OF THE CYGNUS LOOP | XIS | Y |
| CYGNUS LOOP (P22) | 312.8353 | 32.4047 | 75.39493092 | -7.53123997 | 61.4354 | 54620.2981134259 | 54620.7522453704 | 503058010 | 19287.3 | 15000 | 19287.3 | 19287.3 | 0 | 19287.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17220.3 | 17220.3 | 39212 | 0 | PROCESSED | 57542.7062037037 | 55003 | 54636.2807638889 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030074 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks. | GALACTIC DIFFUSE EMISSION | 5 | B | TSUNEMI | HIROSHI | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATIONS OF THE CYGNUS LOOP | XIS | Y |
| CYGNUS LOOP (P23) | 312.4772 | 32.3587 | 75.1675214 | -7.32455162 | 61.8892 | 54620.7530439815 | 54621.1473842593 | 503059010 | 19457 | 15000 | 19457 | 19457 | 0 | 19457 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17277.1 | 17277.1 | 34063.9 | 0 | PROCESSED | 57542.7106944444 | 55003 | 54636.2328240741 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030074 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks. | GALACTIC DIFFUSE EMISSION | 5 | B | TSUNEMI | HIROSHI | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATIONS OF THE CYGNUS LOOP | XIS | Y |
| CYGNUS LOOP (P24) | 312.134 | 32.2905 | 74.93132331 | -7.14055521 | 61.3941 | 54621.1479513889 | 54621.6271875 | 503060010 | 18504.6 | 15000 | 18504.6 | 18504.6 | 0 | 18504.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14999 | 14999 | 41397.9 | 1 | PROCESSED | 57542.7234027778 | 55003 | 54637.4594675926 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030074 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks. | GALACTIC DIFFUSE EMISSION | 5 | B | TSUNEMI | HIROSHI | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATIONS OF THE CYGNUS LOOP | XIS | Y |
| CYGNUS LOOP (P25) | 311.8608 | 32.1678 | 74.68970828 | -7.03578766 | 60.8878 | 54621.6278472222 | 54622.1488888889 | 503061010 | 25995.9 | 20000 | 25995.9 | 25995.9 | 0 | 25995.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 23879.1 | 23879.1 | 45010 | 0 | PROCESSED | 57542.7242476852 | 55003 | 54636.2508217593 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030074 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks. | GALACTIC DIFFUSE EMISSION | 5 | B | TSUNEMI | HIROSHI | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATIONS OF THE CYGNUS LOOP | XIS | Y |
| CYGNUS LOOP (P26) | 314.1252 | 30.3135 | 74.46090737 | -9.70687059 | 49.7995 | 54599.1203587963 | 54599.5474421296 | 503062010 | 16924.7 | 15000 | 16924.7 | 16932.7 | 0 | 16932.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15441 | 15441 | 36892 | 1 | PROCESSED | 57542.5181944444 | 54975 | 54609.1293981482 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030074 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks. | GALACTIC DIFFUSE EMISSION | 5 | B | TSUNEMI | HIROSHI | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATIONS OF THE CYGNUS LOOP | XIS | Y |
| CYGNUS LOOP (P27) | 313.8328 | 30.0104 | 74.06049539 | -9.7037521 | 49.6211 | 54599.5480092593 | 54600.0494675926 | 503063010 | 22784.3 | 20000 | 22792.3 | 22784.3 | 0 | 22800.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20068.8 | 20068.8 | 43323.9 | 0 | PROCESSED | 57542.5253587963 | 54975 | 54609.1396990741 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030074 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks. | GALACTIC DIFFUSE EMISSION | 5 | B | TSUNEMI | HIROSHI | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATIONS OF THE CYGNUS LOOP | XIS | Y |
| CYGNUS LOOP (P28) | 313.4797 | 29.8934 | 73.77252886 | -9.54040793 | 49.1005 | 54600.0501273148 | 54600.5334953704 | 503064010 | 18169.3 | 15000 | 18177.3 | 18185.3 | 0 | 18169.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16443 | 16443 | 41756 | 0 | PROCESSED | 57542.5291898148 | 54975 | 54609.1904282407 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030074 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a region in the central part of the Loop where the shell is very thin. The observation in this region will show the precise mass of the progenitor star. We found most of the shell region showed extremely low abundance. This may suggest that the plasma in the shell region consists of a thin thermal spectrum and a non-thermal spectrum. We may be able to find a region showing non-thermal emission. We propose to observe the Cygnus Loop for 180ks. | GALACTIC DIFFUSE EMISSION | 5 | B | TSUNEMI | HIROSHI | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATIONS OF THE CYGNUS LOOP | XIS | Y |
| RABBIT | 214.6544 | -60.9713 | 313.31134091 | 0.131367 | 105.7763 | 54876.850787037 | 54877.5224421296 | 503071010 | 21274 | 20000 | 21282 | 21274 | 0 | 21290 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 18012.6 | 18012.6 | 57984 | 0 | PROCESSED | 57545.5405439815 | 55330 | 54892.945162037 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030076 | K3/PSR J1420-6048 is one of the TeV gamma-ray pulsar wind nebulae detected by HESS, which are thought to be main particle accelerators to the Galactic Cosmic rays. It was also detected by EGRET and its X-ray spectrum is very hard. In order to reveal the radiation mechanism, we propose to observe the extended source for 50 ksec on HXD nominal position and contamination source for 20 ksec on XIS nominal position. The main purpose of this observation is to obtain the hard X-ray spectrum up to about 40 keV. | GALACTIC DIFFUSE EMISSION | 5 | C | KISHISHITA | TETSUICHI | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF TEV GAMMA-RAY PWN K3/PSR J1420-6048 | XIS | Y |
| EXTENDED CHIMNEY | 265.9856 | -29.2095 | 359.57541621 | 0.16970004 | 69.9995 | 54896.1105555556 | 54899.1218171296 | 503072010 | 140573.3 | 133000 | 140573.3 | 140573.3 | 0 | 140573.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 135478.4 | 135478.4 | 260128 | 1 | PROCESSED | 57545.7802546296 | 55330 | 54916.5067361111 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030086 | We have discovered a chimney structure in the Sgr C region with Suzaku. The Suzaku spectrum of the chimney shows typical parameters of a super nova remnant. However, the chimney has a linear shape, which is inconsistent with a SNR. Thus, we are considering that the chimney is a blowout from super bubble in the Sgr C region. Another possible scenario is that the chimney would be a part of a shell structure formed by explosions (starburst activities, Sgr A*, magnetic reconnection) in the region of Sgr A and Sgr C. Thus, in this proposal, we would like to investigate the structure extending from the chimney. | GALACTIC DIFFUSE EMISSION | 5 | B | TSURU | TAKESHI | NULL | NULL | JAP | 3 | AO3 | THE CHIMNEY OF SGR C : A PART OF A SUPER BUBBLE = A SUPER SHELL ? | XIS | Y |
| HESSJ1614-A | 243.5214 | -52.1022 | 331.29897546 | -0.76107386 | 283.3889 | 54729.7629050926 | 54730.562662037 | 503073010 | 53649.4 | 50000 | 53657.4 | 53649.4 | 0 | 53665.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 40871.3 | 40871.3 | 69071.9 | 0 | PROCESSED | 57543.9752662037 | 55148 | 54780.4246990741 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030088 | The TeV image of HESSJ1614-518 is double peaked, and we observed one of them during the AO-1 with the Suzaku XIS. We discovered extended X-ray emission which coincides with the TeV emission. Then we propose to observe the other peak. We also found a bright object between the double peaks. HESSJ1614 may be a pulsar wind nebula, and the object may be a pulsar driving the nebula. However, the object was just at the edge of the XIS field of view, we could not study it in detail. Then, we propose another position to observe the object. Furthermore, we discovered soft diffuse emission around HESSJ1614. We propose the other position to study the spatial extension of the diffuse emission. | GALACTIC DIFFUSE EMISSION | 5 | B | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 3 | AO3 | MAPPING OBSERVATION OF HESSJ1614-518 | XIS | Y |
| HESSJ1614-B | 243.5783 | -51.8962 | 331.46625372 | -0.63583262 | 283.7142 | 54730.5632291667 | 54731.2779166667 | 503074010 | 52634.2 | 50000 | 52642.2 | 52634.2 | 0 | 52634.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42953 | 42953 | 61735.9 | 0 | PROCESSED | 57543.9760763889 | 55148 | 54780.4609490741 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030088 | The TeV image of HESSJ1614-518 is double peaked, and we observed one of them during the AO-1 with the Suzaku XIS. We discovered extended X-ray emission which coincides with the TeV emission. Then we propose to observe the other peak. We also found a bright object between the double peaks. HESSJ1614 may be a pulsar wind nebula, and the object may be a pulsar driving the nebula. However, the object was just at the edge of the XIS field of view, we could not study it in detail. Then, we propose another position to observe the object. Furthermore, we discovered soft diffuse emission around HESSJ1614. We propose the other position to study the spatial extension of the diffuse emission. | GALACTIC DIFFUSE EMISSION | 5 | B | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 3 | AO3 | MAPPING OBSERVATION OF HESSJ1614-518 | XIS | Y |
| LOW_LATITUDE_97-10 | 311.8076 | 60.1112 | 96.61384914 | 10.40907029 | 101.0346 | 54571.1324652778 | 54572.8890509259 | 503075010 | 79811.9 | 80000 | 79819.9 | 79827.9 | 0 | 79811.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 80810.5 | 80810.5 | 151749.8 | 2 | PROCESSED | 57542.342962963 | 54953 | 54581.3271643518 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030105 | Suzaku observations of diffuse background emission indicate galactic-latitude dependence of OVII intensity. The result of our AO-2 observation strongly supports this dependence. This suggests that the major part of the emission is originating from the halo or the extended disk of our galaxy. In order to confirm the galactic-latitude dependency and to constrain the spatial distribution of the OVII emitting gas, we propose to observe diffuse radiation at a low galactic latitude of ~ 10 deg. | GALACTIC DIFFUSE EMISSION | 5 | B | YOSHINO | TOMOTAKA | NULL | NULL | JAP | 3 | AO3 | RESOLVING LARGE-SCALE SPATIAL DEPENDENCE OF SOFT X-RAY DIFFUSE EMISSION | XIS | Y |
| HESSJ1741-A | 265.3548 | -30.1316 | 358.50289854 | 0.15030933 | 73.8229 | 54886.7117013889 | 54888.0419328704 | 503076010 | 52932.3 | 50000 | 52932.3 | 52932.3 | 0 | 52932.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43770.8 | 43770.8 | 114915.8 | 1 | PROCESSED | 57545.6752546296 | 55330 | 54902.4869791667 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030113 | HESSJ1741-302 is one of the most darkest TeV unidentified objects which was discovered with the H.E.S.S. telescope recently. The location strongly suggests that the object is physically connected to the diffuse TeV gamma-ray emission along the Galactic plane. On the other hand, there is a pulsar near the object, and it may be an off-set pulsar wind nebula. To clarify the origin of the object, we propose to the observation of HESSJ1741. | GALACTIC DIFFUSE EMISSION | 5 | C | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 3 | AO3 | DARKEST TEV UNIDENTIFIED OBJECT HESSJ1741-302 | XIS | Y |
| HESSJ1741-B | 265.2407 | -30.3098 | 358.29952005 | 0.1396669 | 74.0024 | 54888.0423611111 | 54889.4828587963 | 503077010 | 51261.6 | 50000 | 51269.6 | 51261.6 | 0 | 51269.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43707.2 | 43707.2 | 124423.9 | 1 | PROCESSED | 57545.6763773148 | 55330 | 54908.5791550926 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030113 | HESSJ1741-302 is one of the most darkest TeV unidentified objects which was discovered with the H.E.S.S. telescope recently. The location strongly suggests that the object is physically connected to the diffuse TeV gamma-ray emission along the Galactic plane. On the other hand, there is a pulsar near the object, and it may be an off-set pulsar wind nebula. To clarify the origin of the object, we propose to the observation of HESSJ1741. | GALACTIC DIFFUSE EMISSION | 5 | C | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 3 | AO3 | DARKEST TEV UNIDENTIFIED OBJECT HESSJ1741-302 | XIS | Y |
| HESS_J1809-193_N | 272.4044 | -19.3551 | 11.02929838 | 0.07166066 | 112.001 | 54556.5874421296 | 54557.6877662037 | 503078010 | 51530.9 | 40000 | 51538.9 | 51530.9 | 0 | 51546.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34818.6 | 34818.6 | 95051.8 | 2 | PROCESSED | 57542.0290740741 | 54950 | 54571.3638888889 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030126 | A survey of the Galactic plane with H.E.S.S. has revealed the existance of several new very-high-energy (VHE) gamma-ray sources. As gamma rays are produced by interactions of relativistic particles, observing VHE emission reveals the acceleration sites of particles. Although it had been thought that such acceleration occur in the shock of SNR, it became clear that several VHE sources are pulsar wind nebulae (PWNe). This indicates that PWNe are also the acceleration sites of particles. HESS J1809-193 is a diffuse and a pulsar wind nebula candidate source, but details of the VHE emission mechanisms have been unclear yet. With the high sensitivity of XIS, we investigate spatial distribution of the spectrum around HESS J1809-193 and reveal its nature and the VHE emission mechanism. | GALACTIC DIFFUSE EMISSION | 5 | A | ANADA | TAKAYASU | NULL | NULL | JAP | 3 | AO3 | INVESTIGATION OF THE SPACIAL DISTRIBUTION OF THE SPECTRAL SHAPE AROUND VHE SOURCE HESS J1809-193 | XIS | Y |
| HESS_J1809-193_S | 272.3365 | -19.5311 | 10.84429394 | 0.04252392 | 106.4999 | 54557.6901851852 | 54558.6161805556 | 503079010 | 44248.1 | 40000 | 44248.1 | 44248.1 | 0 | 44248.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32214.2 | 32214.2 | 79969.8 | 1 | PROCESSED | 57542.0277546296 | 54950 | 54570.1866666667 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030126 | A survey of the Galactic plane with H.E.S.S. has revealed the existance of several new very-high-energy (VHE) gamma-ray sources. As gamma rays are produced by interactions of relativistic particles, observing VHE emission reveals the acceleration sites of particles. Although it had been thought that such acceleration occur in the shock of SNR, it became clear that several VHE sources are pulsar wind nebulae (PWNe). This indicates that PWNe are also the acceleration sites of particles. HESS J1809-193 is a diffuse and a pulsar wind nebula candidate source, but details of the VHE emission mechanisms have been unclear yet. With the high sensitivity of XIS, we investigate spatial distribution of the spectrum around HESS J1809-193 and reveal its nature and the VHE emission mechanism. | GALACTIC DIFFUSE EMISSION | 5 | A | ANADA | TAKAYASU | NULL | NULL | JAP | 3 | AO3 | INVESTIGATION OF THE SPACIAL DISTRIBUTION OF THE SPECTRAL SHAPE AROUND VHE SOURCE HESS J1809-193 | XIS | Y |
| CAS A | 351.0231 | 59.0265 | 111.88943817 | -1.95981315 | 208.1115 | 54876.0965740741 | 54876.8363310185 | 503080010 | 30035.5 | 30000 | 30035.5 | 30035.5 | 0 | 30035.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30073.1 | 30073.1 | 63913.9 | 0 | PROCESSED | 57545.551087963 | 55330 | 54892.9889699074 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030127 | Cas A is the youngest supernova remnant(SNR) in our Galaxy. Recently, the Spitzer Space Telescope discovered moving structures nearly at the speed of light outside the shell of the SNR. These structures are likely infrared echoes, where interstellar dust is heated by the outward moving photon shell of a bright flash. The bright flash is probably due to a giant flare from the central point source of Cas A, and if so, it requires that the central point source is a magnetar. Magnetars are known to emit luminous flares in the X-ray band, so it is expected that we can detect Fe-K fluorescence emission accompanied by IR echo. Here, we propose to observe on IR-emitting cloud around Cas A for 30ks to search for Fe-K emission which is naturally expected if the central point source is a magnetar. | GALACTIC DIFFUSE EMISSION | 5 | C | AONO | HIROYUKI | NULL | NULL | JAP | 3 | AO3 | INVESTIGATION OF A X-RAY ECHO NEAR THE SUPERNOVA REMNANT CASSIOPEIA A | XIS | Y |
| GC(0,-1.6) | 268.0544 | -29.7594 | 0.03481768 | -1.65633011 | 65.7488 | 54899.6540509259 | 54900.8168865741 | 503081010 | 59223.3 | 50000 | 59223.3 | 59223.3 | 0 | 59223.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 57601.8 | 57601.8 | 100453.8 | 1 | PROCESSED | 57545.7843402778 | 55330 | 54916.3813194444 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030131 | We propose a 50 ksec observation of very enigmatic diffuse structure at 1.6 degree south from the Galactic center. We first discovered this structure with ROSAT. Then with ASCA, we found that the spectrum exhibits thin thermal emission accompanied with a hard tail which may be nonthermal radiation from high energy electrons. These results imply presence of a strong shock in this region, possibly due to a jet from Sgr A*. The diffuse emission may be a fossil of the past activities. With the observation of Suzaku, we obtain the richest statistics ever achieved. Then we will reveal the shock front from the image, and verify the past activities of the massive blackhole. | GALACTIC DIFFUSE EMISSION | 5 | B | MURAKAMI | HIROSHI | NULL | NULL | JAP | 3 | AO3 | NEW EVIDENCE OF THE PAST ACTIVITY IN THE GALACTIC CENTER REGION | XIS | Y |
| VICINITY_OF_PKS_2155-1 | 329.2367 | -30.5281 | 17.16872193 | -51.86657338 | 55.8337 | 54585.7726736111 | 54588.3542592593 | 503082010 | 90181.2 | 80000 | 90181.2 | 90181.2 | 0 | 90181.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 76792.1 | 76792.1 | 223023.7 | 4 | PROCESSED | 57542.4840277778 | 54975 | 54608.3373726852 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030135 | The highly ionized absorption lines of OVII, OVIII, and NeIX at z = 0 have been unambiguously detected toward the bright AGN PKS 2155-304 by the high-resolution spectrometers onboard Chandra and XMM-Newton. However, the spatial extent and thus the nature of the absorbing warm-hot gas are yet unknown; it can be from 1 Mpc scale WHIM (Warm-hot intergalactic medium) to a few kpc scale galactic wind. We propose to observe the very vicinity of the AGN to determine the OVII, OVIII and NeIX emission line intensities and the temperature of the warm-hot gas. Joint analysis of absorption and emission lines will unambiguously constrain the spatial extent of the warm-hot gas. | GALACTIC DIFFUSE EMISSION | 5 | A | HAGIHARA | TOSHISHIGE | NULL | NULL | JAP | 3 | AO3 | STUDY OF WARM-HOT GAS TOWARD PKS 2155-304 | XIS | Y |
| VICINITY_OF_PKS_2155-2 | 330.1861 | -29.9649 | 18.22929909 | -52.62033555 | 55.8323 | 54588.3553356482 | 54590.7293865741 | 503083010 | 87327.4 | 80000 | 87327.4 | 87327.4 | 0 | 87327.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 75845.1 | 75845.1 | 205105.9 | 3 | PROCESSED | 57542.4726736111 | 54975 | 54608.2608912037 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030135 | The highly ionized absorption lines of OVII, OVIII, and NeIX at z = 0 have been unambiguously detected toward the bright AGN PKS 2155-304 by the high-resolution spectrometers onboard Chandra and XMM-Newton. However, the spatial extent and thus the nature of the absorbing warm-hot gas are yet unknown; it can be from 1 Mpc scale WHIM (Warm-hot intergalactic medium) to a few kpc scale galactic wind. We propose to observe the very vicinity of the AGN to determine the OVII, OVIII and NeIX emission line intensities and the temperature of the warm-hot gas. Joint analysis of absorption and emission lines will unambiguously constrain the spatial extent of the warm-hot gas. | GALACTIC DIFFUSE EMISSION | 5 | A | HAGIHARA | TOSHISHIGE | NULL | NULL | JAP | 3 | AO3 | STUDY OF WARM-HOT GAS TOWARD PKS 2155-304 | XIS | Y |
| W49B | 287.7847 | 9.1157 | 43.28157058 | -0.18360003 | 89.2671 | 54919.1063888889 | 54920.4689583333 | 503084010 | 52154.9 | 40000 | 52154.9 | 52154.9 | 0 | 52154.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43951.2 | 43951.2 | 117709.9 | 2 | PROCESSED | 57547.7422685185 | 55330 | 54931.3622106482 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030142 | Observations of the W49B supernova remnant for 40 ks is proposed to reveal whether it is a remnant of an anomalous Type Ia supernova or not. To determine the type of the supernova, detailed measurement of less abundand elements such as Cr and Mn will be performed, and abundance of Ni and Ti will be examined. The abundance pattern of those elements in W49B will be compared to that of Tycho's SNR we measured by Suzaku. | GALACTIC DIFFUSE EMISSION | 5 | C | TAMAGAWA | TORU | NULL | NULL | JAP | 3 | AO3 | IS W49B A REMNANT OF AN ANOMALOUS TYPE IA SUPERNOVA? | XIS | Y |
| TYCHO SNR | 6.3139 | 64.1469 | 120.08177164 | 1.42013769 | 53.7834 | 54682.0646759259 | 54686.9529398148 | 503085010 | 312892 | 400000 | 312916 | 312892 | 0 | 312908 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 289949.4 | 289949.4 | 307869.9 | 3 | PROCESSED | 57543.3766782407 | 54557 | 54707.038287037 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031003 | Recent Suzaku studies of the Type Ia supernova remnant, Tycho, have revealed tantalizing evidence for secondary Fe-peak elements (specifically Cr and Mn) in the integrated X-ray spectrum. Here we propose to confirm and extend these detections by measuring the spatial variation of Cr/Fe line fluxes across the remnant, paying particular attention to the composition of a previously known Fe-rich region along the eastern limb. The unique capabilities of the XIS onboard Suzaku (high spectral resolution and large effective area) are crucial to the proposed study and no other operating instrument can detect the weak lines from these trace species within reasonable exposure times. | GALACTIC DIFFUSE EMISSION | 5 | A | HUGHES | JOHN | NULL | NULL | USA | 3 | AO3 | SECONDARY FE-PEAK ELEMENTS AS A PROBE OF SN IA EXPLOSION PHYSICS | XIS | Y |
| TYCHO SNR | 6.3115 | 64.1447 | 120.08050675 | 1.41805528 | 43.1557 | 54689.3425578704 | 54690.918275463 | 503085020 | 102855.6 | 100000 | 102855.6 | 102855.6 | 0 | 102855.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 91907.8 | 91907.8 | 136103.9 | 1 | PROCESSED | 57543.2895717593 | 54557 | 54706.7896412037 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031003 | Recent Suzaku studies of the Type Ia supernova remnant, Tycho, have revealed tantalizing evidence for secondary Fe-peak elements (specifically Cr and Mn) in the integrated X-ray spectrum. Here we propose to confirm and extend these detections by measuring the spatial variation of Cr/Fe line fluxes across the remnant, paying particular attention to the composition of a previously known Fe-rich region along the eastern limb. The unique capabilities of the XIS onboard Suzaku (high spectral resolution and large effective area) are crucial to the proposed study and no other operating instrument can detect the weak lines from these trace species within reasonable exposure times. | GALACTIC DIFFUSE EMISSION | 5 | A | HUGHES | JOHN | NULL | NULL | USA | 3 | AO3 | SECONDARY FE-PEAK ELEMENTS AS A PROBE OF SN IA EXPLOSION PHYSICS | XIS | Y |
| G18.0-0.7 | 276.56 | -13.5781 | 18.00442084 | -0.69482715 | 92.0001 | 54909.8982060185 | 54911.080775463 | 503086010 | 52059.2 | 50000 | 52059.2 | 52067.2 | 0 | 52067.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46303.6 | 46303.6 | 102145.8 | 2 | PROCESSED | 57547.7369560185 | 55329 | 54923.3684490741 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031203 | By studying pulsar wind nebulae, the synchrotron nebulae powered by a neutron star's loss of rotational energy, it is possible to determine the energetics of both the progenitor supernova and central neutron star. This requires estimates of the expansion velocity and mass swept-up the pulsar wind nebulae, best obtained by analyzing the spectrum of the thermal X-rays emitting by this material. In the proposal, we request a 50ks observation of four of the most energetic pulsar wind nebulae in the Milky Way to both detect such thermal X-ray emission and use the measured spectral properties to infer the ejecta mass and kinetic energy of their progenitor supernova and the initial spin period of the central neutron star -- all currently unmeasurable using the currently available information. | GALACTIC DIFFUSE EMISSION | 5 | C | GELFAND | JOSEPH | NULL | NULL | USA | 3 | AO3 | STUDYING THE PROGENITOR SUPERNOVA AND CENTRAL NEUTRON STAR OF PULSAR WIND NEBULAE | XIS | Y |
| G12.8-0.0 | 273.3975 | -17.831 | 12.81826803 | -0.01988984 | 90.5577 | 54894.8233680556 | 54896.1050810185 | 503087010 | 56202.6 | 50000 | 56202.6 | 56202.6 | 0 | 56205.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51531.2 | 51531.2 | 110727.8 | 1 | PROCESSED | 57545.7287962963 | 55329 | 54908.5701388889 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031203 | By studying pulsar wind nebulae, the synchrotron nebulae powered by a neutron star's loss of rotational energy, it is possible to determine the energetics of both the progenitor supernova and central neutron star. This requires estimates of the expansion velocity and mass swept-up the pulsar wind nebulae, best obtained by analyzing the spectrum of the thermal X-rays emitting by this material. In the proposal, we request a 50ks observation of four of the most energetic pulsar wind nebulae in the Milky Way to both detect such thermal X-ray emission and use the measured spectral properties to infer the ejecta mass and kinetic energy of their progenitor supernova and the initial spin period of the central neutron star -- all currently unmeasurable using the currently available information. | GALACTIC DIFFUSE EMISSION | 5 | C | GELFAND | JOSEPH | NULL | NULL | USA | 3 | AO3 | STUDYING THE PROGENITOR SUPERNOVA AND CENTRAL NEUTRON STAR OF PULSAR WIND NEBULAE | XIS | Y |
| B1920+10(1) | 293.0298 | 10.9618 | 47.34140504 | -3.87470613 | 252.2888 | 54772.350462963 | 54774.137662037 | 503090010 | 73603.3 | 70000 | 73612.4 | 73603.3 | 0 | 73611.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 66668.2 | 66668.2 | 154403.9 | 3 | PROCESSED | 57544.3491550926 | 55154 | 54788.4472337963 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031204 | A bow-shock pulsar wind nebula with an exceptionally long tail has been detected in X-ray observations of the pulsar PSR B1929+10. Recent observations suggest that such long structures may be associated with many other pulsars. Being the longest extended structures observed around Galactic compact objects. The physical processes responsible for the formation of such tails are not well understood, and the existing numerical models may only be valid at small distances from the pulsar. To determine the major factors governing the post-shock wind, we propose to observe the tail of PSR B1929+10, measure its full extent, map the surface brightness distribution, and perform spatially resolved spectroscopy. We will also measure the pulsar spectrum to study the properties of its polar caps. | GALACTIC DIFFUSE EMISSION | 5 | C | MISANOVIC | ZDENKA | NULL | NULL | USA | 3 | AO3 | STUDYING THE LONG PULSAR TAIL OF THE PSR B1929+10 WITH SUZAKU | XIS | Y |
| B1920+10(2) | 292.8971 | 10.8605 | 47.18977478 | -3.80874006 | 248.6642 | 54783.7420833333 | 54785.8981365741 | 503091010 | 100457.7 | 100000 | 100457.7 | 100457.7 | 0 | 100457.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 93873.1 | 93873.1 | 186248 | 0 | PROCESSED | 57544.4390972222 | 55167 | 54797.1537731482 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031204 | A bow-shock pulsar wind nebula with an exceptionally long tail has been detected in X-ray observations of the pulsar PSR B1929+10. Recent observations suggest that such long structures may be associated with many other pulsars. Being the longest extended structures observed around Galactic compact objects. The physical processes responsible for the formation of such tails are not well understood, and the existing numerical models may only be valid at small distances from the pulsar. To determine the major factors governing the post-shock wind, we propose to observe the tail of PSR B1929+10, measure its full extent, map the surface brightness distribution, and perform spatially resolved spectroscopy. We will also measure the pulsar spectrum to study the properties of its polar caps. | GALACTIC DIFFUSE EMISSION | 5 | C | MISANOVIC | ZDENKA | NULL | NULL | USA | 3 | AO3 | STUDYING THE LONG PULSAR TAIL OF THE PSR B1929+10 WITH SUZAKU | XIS | Y |
| HESS J1023-575 | 155.5616 | -57.7533 | 284.06754503 | -0.45248582 | 284.3289 | 54617.1411458333 | 54617.4515509259 | 503092010 | 13826 | 10000 | 13826 | 13826 | 0 | 13826 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11057.3 | 11057.3 | 26815.9 | 1 | PROCESSED | 57542.6773842593 | 54999 | 54633.6961458333 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031207 | We propose to search the neighborhood of two extended TeV sources to determine if there are X-ray sources that are potentially pulsar wind nebulae powering them. One source is near the colliding wind binary RCW 49, which has been suggested as the accelerator, and would therefore represent a new source class if there is no other plausible accelerator in the neighborhood. The other is a very bright source first detected by MILAGRO in the Galactic plane, which has been shown to be a large, extended source by HESS. While there is in each case a proposed X-ray counterpart, only a part of each nebula has been imaged in hard X-rays, and so it is unknown if there are other, more plausible counterparts. | GALACTIC DIFFUSE EMISSION | 5 | B | ROBERTS | MALLORY | NULL | NULL | USA | 3 | AO3 | SEARCHING FOR X-RAY COUNTERPARTS OF TWO GALACTIC TEV SOURCES | XIS | Y |
| SNR 0049-73.6 | 12.7817 | -73.3677 | 302.96274339 | -43.76053264 | 62.7682 | 54629.4818518518 | 54632.7605787037 | 503094010 | 120478 | 120000 | 120486 | 120478 | 0 | 120486 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 107707.9 | 107707.9 | 283241.9 | 3 | PROCESSED | 57542.894525463 | 55008 | 54642.6050694444 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031211 | We propose to observe the O-rich supernova remnant (SNR) 0049-73.6 in the Small Magellanic Cloud (SMC). SNR 0049-73.6 shares some similarities and differences with another O-rich SNR 0103-72.6 in the SMC. High resolution X-ray spectroscopy of these SNRs with Suzaku/XIS observations should provide a useful insight for the details of thermal evolution of a core-collapse SNR. We began this program with an AO1 Suzaku/XIS observation of SNR 0103-72.6. We here propose to continue this program with our AO3 Suzaku observation of 0049-73.6. We request for a 120 ks Suzaku/XIS observation of 0049-73.6. | GALACTIC DIFFUSE EMISSION | 5 | B | PARK | SANGWOOK | NULL | NULL | USA | 3 | AO3 | OXYGEN-RICH SUPERNOVA REMNANT 0049-73.6 IN THE SMC | XIS | Y |
| VELA FRAGMENT C | 136.2696 | -44.691 | 266.51473212 | 1.58715492 | 269.3614 | 54580.6978703704 | 54582.3056481482 | 503095010 | 84116.7 | 70000 | 84116.7 | 84116.7 | 0 | 84116.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 91354.7 | 91354.7 | 138901.8 | 2 | PROCESSED | 57542.4305439815 | 54960 | 54594.2480324074 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031212 | Ejecta fragments projecting from the nearby Vela supernova remnant provide a unique opportunity to examine supernova ejecta as they shock and finally merge into the interstellar medium (ISM). Fragments "A" and "D", observed with Chandra and XMM, and Fragment "B", observed with Suzaku, show strongly enhanced (but very different) abundances. These fragments are indeed ejecta, but originating in different layers of the precursor. We propose to observe two of the remaining ejecta fragments. In combination with the existing observations of Fragments A, B, and D, these data will provide a much more complete picture of the variation in ejecta fragment abundances and their interactions with the remnant shell and the surrounding ISM. | GALACTIC DIFFUSE EMISSION | 5 | B | GAETZ | TERRANCE | NULL | NULL | USA | 3 | AO3 | SEARCHING FOR EJECTA IN THE VELA SUPERNOVA REMNANT FRAGMENTS | XIS | Y |
| VELA FRAGMENT E | 119.9016 | -44.3755 | 259.34445053 | -7.61175769 | 281.1138 | 54582.309224537 | 54583.7849421296 | 503096010 | 79200.4 | 70000 | 79218.9 | 79200.4 | 0 | 79232.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 84252.9 | 84252.9 | 127489.9 | 1 | PROCESSED | 57542.4144212963 | 54960 | 54594.2098842593 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031212 | Ejecta fragments projecting from the nearby Vela supernova remnant provide a unique opportunity to examine supernova ejecta as they shock and finally merge into the interstellar medium (ISM). Fragments "A" and "D", observed with Chandra and XMM, and Fragment "B", observed with Suzaku, show strongly enhanced (but very different) abundances. These fragments are indeed ejecta, but originating in different layers of the precursor. We propose to observe two of the remaining ejecta fragments. In combination with the existing observations of Fragments A, B, and D, these data will provide a much more complete picture of the variation in ejecta fragment abundances and their interactions with the remnant shell and the surrounding ISM. | GALACTIC DIFFUSE EMISSION | 5 | B | GAETZ | TERRANCE | NULL | NULL | USA | 3 | AO3 | SEARCHING FOR EJECTA IN THE VELA SUPERNOVA REMNANT FRAGMENTS | XIS | Y |
| GCL1 | 265.1726 | -28.5274 | 359.7799359 | 1.13423351 | 69.7267 | 54900.8188425926 | 54901.4557175926 | 503099010 | 29706 | 25000 | 29724.1 | 29722 | 0 | 29706 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30564.9 | 30564.9 | 55020 | 1 | PROCESSED | 57545.7841782407 | 55329 | 54916.3706828704 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031234 | We request 110ks of XIS observations to cover four pointings towards the large-scale Galactic Center Lobe (GCL). The GCL consists of a collection of remarkable thermal and nonthermal coherent components with a scale length of about 150 pc perpendicular to the Galactic plane. There is circumstantial evidence for a mild starburst activity and the GCL is viewed as a manifestation of powerful massive stars affecting their surrounding ISM in a starburst episode. The proposed X-ray observations of diffuse soft and hard X-ray emission from the GCL, away from the plane is critical in order to examine the starburst model. The analysis of X-ray emission can be used to distinguish between different scenarios of starburst activity in the nucleus of our activity. | GALACTIC DIFFUSE EMISSION | 5 | B | YUSEF-ZADEH | FARHAD | NULL | NULL | USA | 3 | AO3 | A SUZAKU SURVEY OF THE GALACTIC CENTER LOBE: A NUCLEAR STARBURST? | XIS | Y |
| GCL2 | 264.8888 | -28.9255 | 359.31035513 | 1.13376438 | 106.9569 | 54905.2789467593 | 54905.9169444444 | 503100010 | 25717.9 | 25000 | 25717.9 | 25717.9 | 0 | 25717.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 24146 | 24146 | 55119.9 | 1 | PROCESSED | 57545.8116666667 | 55329 | 54917.3744675926 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031234 | We request 110ks of XIS observations to cover four pointings towards the large-scale Galactic Center Lobe (GCL). The GCL consists of a collection of remarkable thermal and nonthermal coherent components with a scale length of about 150 pc perpendicular to the Galactic plane. There is circumstantial evidence for a mild starburst activity and the GCL is viewed as a manifestation of powerful massive stars affecting their surrounding ISM in a starburst episode. The proposed X-ray observations of diffuse soft and hard X-ray emission from the GCL, away from the plane is critical in order to examine the starburst model. The analysis of X-ray emission can be used to distinguish between different scenarios of starburst activity in the nucleus of our activity. | GALACTIC DIFFUSE EMISSION | 5 | B | YUSEF-ZADEH | FARHAD | NULL | NULL | USA | 3 | AO3 | A SUZAKU SURVEY OF THE GALACTIC CENTER LOBE: A NUCLEAR STARBURST? | XIS | Y |
| GCL3 | 265.2728 | -28.8569 | 359.5469331 | 0.88519 | 106.9023 | 54906.6133912037 | 54907.3252777778 | 503101010 | 33891.1 | 25000 | 33899.1 | 33899.1 | 0 | 33891.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30830.9 | 30830.9 | 61497.9 | 0 | PROCESSED | 57545.8349652778 | 55329 | 54917.3115393518 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031234 | We request 110ks of XIS observations to cover four pointings towards the large-scale Galactic Center Lobe (GCL). The GCL consists of a collection of remarkable thermal and nonthermal coherent components with a scale length of about 150 pc perpendicular to the Galactic plane. There is circumstantial evidence for a mild starburst activity and the GCL is viewed as a manifestation of powerful massive stars affecting their surrounding ISM in a starburst episode. The proposed X-ray observations of diffuse soft and hard X-ray emission from the GCL, away from the plane is critical in order to examine the starburst model. The analysis of X-ray emission can be used to distinguish between different scenarios of starburst activity in the nucleus of our activity. | GALACTIC DIFFUSE EMISSION | 5 | B | YUSEF-ZADEH | FARHAD | NULL | NULL | USA | 3 | AO3 | A SUZAKU SURVEY OF THE GALACTIC CENTER LOBE: A NUCLEAR STARBURST? | XIS | Y |
| GCL4 | 265.3437 | -29.192 | 359.29532739 | 0.65531706 | 106.9407 | 54907.3257986111 | 54908.0711111111 | 503102010 | 33655.4 | 25000 | 33679.4 | 33655.8 | 0 | 33655.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30052.1 | 30052.1 | 64389.9 | 0 | PROCESSED | 57545.8492939815 | 55329 | 54920.054837963 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031234 | We request 110ks of XIS observations to cover four pointings towards the large-scale Galactic Center Lobe (GCL). The GCL consists of a collection of remarkable thermal and nonthermal coherent components with a scale length of about 150 pc perpendicular to the Galactic plane. There is circumstantial evidence for a mild starburst activity and the GCL is viewed as a manifestation of powerful massive stars affecting their surrounding ISM in a starburst episode. The proposed X-ray observations of diffuse soft and hard X-ray emission from the GCL, away from the plane is critical in order to examine the starburst model. The analysis of X-ray emission can be used to distinguish between different scenarios of starburst activity in the nucleus of our activity. | GALACTIC DIFFUSE EMISSION | 5 | B | YUSEF-ZADEH | FARHAD | NULL | NULL | USA | 3 | AO3 | A SUZAKU SURVEY OF THE GALACTIC CENTER LOBE: A NUCLEAR STARBURST? | XIS | Y |
| SLX 1737-282 | 265.2352 | -28.3094 | 359.99405573 | 1.20298654 | 69.9745 | 54901.4562384259 | 54901.8035648148 | 503103010 | 18316 | 10000 | 18332.4 | 18332 | 0 | 18316 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16365.9 | 16365.9 | 30001.9 | 0 | PROCESSED | 57545.7980208333 | 55329 | 54916.9907638889 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031234 | We request 110ks of XIS observations to cover four pointings towards the large-scale Galactic Center Lobe (GCL). The GCL consists of a collection of remarkable thermal and nonthermal coherent components with a scale length of about 150 pc perpendicular to the Galactic plane. There is circumstantial evidence for a mild starburst activity and the GCL is viewed as a manifestation of powerful massive stars affecting their surrounding ISM in a starburst episode. The proposed X-ray observations of diffuse soft and hard X-ray emission from the GCL, away from the plane is critical in order to examine the starburst model. The analysis of X-ray emission can be used to distinguish between different scenarios of starburst activity in the nucleus of our activity. | GALACTIC DIFFUSE EMISSION | 5 | C | YUSEF-ZADEH | FARHAD | NULL | NULL | USA | 3 | AO3 | A SUZAKU SURVEY OF THE GALACTIC CENTER LOBE: A NUCLEAR STARBURST? | XIS | Y |
| ARC_BACKGROUND | 39.2055 | -35.7283 | 240.48717091 | -66.02341726 | 233.8071 | 54830.2554861111 | 54835.3468055556 | 503104010 | 201877.5 | 140000 | 201957.5 | 201877.5 | 0 | 201981.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 5502.8 | 5502.8 | 14506 | 0 | PROCESSED | 57545.0672685185 | 55328 | 54851.4354166667 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031235 | Aside from the lengthy bright arcs in the northern sky, few X-ray bright, high latitude regions are understood. Yet, studying this gas is important for understanding the Galactic halo. Here, we propose to study a medium-sized (~7 degree) bright feature in the southern sky. The feature is arc-shaped, suspiciously like the edge of a hot bubble. We propose to make Suzaku observations of the arc and nearby background. With them and an existing Suzaku observation, we will be able to determine the thermal properties of the arc plasma and if the arc is the bright limb of a hot bubble. | GALACTIC DIFFUSE EMISSION | 5 | B | SHELTON | ROBIN | NULL | NULL | USA | 3 | AO3 | A CLOSER LOOT AT HOT HALO GAS: A SUZAKU STUDY OF AN X-RAY BRIGHT ARC | XIS | Y |
| HESS J1718-385 | 259.5578 | -38.4584 | 348.92137939 | -0.45364037 | 266.9006 | 54706.233599537 | 54706.9286342593 | 503108010 | 23509.7 | 20000 | 23509.7 | 23509.7 | 0 | 23509.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19440.2 | 19440.2 | 60047.9 | 1 | PROCESSED | 57543.4301851852 | 55093 | 54720.4386689815 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 032026 | HESS J1718-385 is a newly discovered Very High Energy (VHE) source with an unusually hard energy spectrum, close to an energetic pulsar. The classification as a VHE Pulsar Wind Nebula (PWN) was confirmed by observations of the region with XMM-Newton and Suzaku. XMM showed a compact X-ray PWN around the pulsar, whereas Suzaku revealed low surface brightness emission close to the VHE source. To morphologically connect this low surface brightness emission to the X-ray PWN, we propose another short, 20 ksec Suzaku pointing, aiming between the VHE source center and the pulsar location. The data will allow to identify the new Suzaku source with the compact X-ray PWN. The spectra will be used to investigate the unusual particle energy distribution that is derived from the hard VHE spectrum. | GALACTIC DIFFUSE EMISSION | 5 | A | PUEHLHOFER | GERD | NULL | NULL | EUR | 3 | AO3 | SUZAKU OBSERVATIONS OF THE LOW SURFACE BRIGHTNESS X-RAY PULSAR WIND NEBULA CANDIDATE ASSOCIATED WITH HESS J1718-385 | XIS | Y |
| K3/PSR J1420-6048 | 215.0274 | -60.7627 | 313.55205119 | 0.26755801 | 90.771 | 54842.5598263889 | 54843.8801388889 | 503110010 | 50269 | 50000 | 50269 | 50269 | 0 | 50269 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 50061.8 | 50061.8 | 114063.9 | 2 | PROCESSED | 57545.1792013889 | 55328 | 54854.3728703704 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 033076 | K3/PSR J1420-6048 is one of the TeV gamma-ray pulsar wind nebulae detected by HESS, which are thought to be main particle accelerators to the Galactic Cosmic rays. It was also detected by EGRET and its X-ray spectrum is very hard. In order to reveal the radiation mechanism, we propose to observe the extended source for 50 ksec on HXD nominal position and contamination source for 20 ksec on XIS nominal position. The main purpose of this observation is to obtain the hard X-ray spectrum up to about 40 keV. | GALACTIC DIFFUSE EMISSION | 5 | C | KISHISHITA | TETSUICHI | ROMANI | ROGER | JUS | 3 | AO3 | SUZAKU OBSERVATION OF TEV GAMMA-RAY PWN K3/PSR J1420-6048 | HXD | Y |
| HESS J1745-303A | 265.7791 | -30.3241 | 358.53258375 | -0.26269922 | 103.33 | 55253.3854166667 | 55254.6758796296 | 504001010 | 51153.8 | 50000 | 51161.8 | 51153.8 | 0 | 51168.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42219.6 | 42219.6 | 111458.1 | 1 | PROCESSED | 57550.7381134259 | 55636 | 55267.2568634259 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040001 | The Galactic Center Region (GC) exhibits two distinguish features; the diffuse TeV gamma and strong 6.4 keV line emissions. These are not uniform but are clumpy, and show a good spatial correlation. Suzaku found that an unidentified source located in the GC direction, HESS J1745-303 has no hard X-ray continuum, hence a "dark accelerator". Unlike to the other TeV sources, this exhibits a hint of the 6.4-keV line. With follow-up observations, we will set a severer upper-limit of the continuum hard X-rays. We then examine if the 6.4-keV line is really associated to HESS J1745-303. This may be good tool to determine the 3-dimentinal position (distance) of this peculiar source. | GALACTIC DIFFUSE EMISSION | 5 | B | KOYAMA | KATSUJI | NULL | NULL | JAP | 4 | AO4 | DOES HESS J1745-303 ASSOCIATE WITH A MOLECULAR CLOUD IN THE GC ? : CORRELATION STUDY | XIS | Y |
| HESS J1745-303B | 266.0577 | -30.545 | 358.47050833 | -0.58308172 | 102.2921 | 55254.6768634259 | 55255.9515509259 | 504002010 | 53060.9 | 50000 | 53060.9 | 53060.9 | 0 | 53060.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46585 | 46585 | 110121.9 | 1 | PROCESSED | 57550.7606481482 | 55636 | 55267.2715856482 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040001 | The Galactic Center Region (GC) exhibits two distinguish features; the diffuse TeV gamma and strong 6.4 keV line emissions. These are not uniform but are clumpy, and show a good spatial correlation. Suzaku found that an unidentified source located in the GC direction, HESS J1745-303 has no hard X-ray continuum, hence a "dark accelerator". Unlike to the other TeV sources, this exhibits a hint of the 6.4-keV line. With follow-up observations, we will set a severer upper-limit of the continuum hard X-rays. We then examine if the 6.4-keV line is really associated to HESS J1745-303. This may be good tool to determine the 3-dimentinal position (distance) of this peculiar source. | GALACTIC DIFFUSE EMISSION | 5 | B | KOYAMA | KATSUJI | NULL | NULL | JAP | 4 | AO4 | DOES HESS J1745-303 ASSOCIATE WITH A MOLECULAR CLOUD IN THE GC ? : CORRELATION STUDY | XIS | Y |
| HESS J1745-303C | 266.3881 | -30.6242 | 358.55151469 | -0.86700864 | 101.7444 | 55252.1897800926 | 55253.3842476852 | 504003010 | 50906.5 | 50000 | 50914.5 | 50914.5 | 0 | 50906.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41270.8 | 41270.8 | 103187.8 | 3 | PROCESSED | 57550.7231365741 | 55632 | 55264.3901157407 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040001 | The Galactic Center Region (GC) exhibits two distinguish features; the diffuse TeV gamma and strong 6.4 keV line emissions. These are not uniform but are clumpy, and show a good spatial correlation. Suzaku found that an unidentified source located in the GC direction, HESS J1745-303 has no hard X-ray continuum, hence a "dark accelerator". Unlike to the other TeV sources, this exhibits a hint of the 6.4-keV line. With follow-up observations, we will set a severer upper-limit of the continuum hard X-rays. We then examine if the 6.4-keV line is really associated to HESS J1745-303. This may be good tool to determine the 3-dimentinal position (distance) of this peculiar source. | GALACTIC DIFFUSE EMISSION | 5 | B | KOYAMA | KATSUJI | NULL | NULL | JAP | 4 | AO4 | DOES HESS J1745-303 ASSOCIATE WITH A MOLECULAR CLOUD IN THE GC ? : CORRELATION STUDY | XIS | Y |
| SGR_B2 | 266.8776 | -28.4437 | 0.63615824 | -0.0985299 | 266.3663 | 55095.6093518518 | 55096.0418287037 | 504004010 | 10057.2 | 200000 | 10057.2 | 10057.2 | 0 | 10057.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 9432.8 | 9432.8 | 37340.9 | 0 | PROCESSED | 57548.6152314815 | 55476 | 55110.2035763889 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040002 | The Galactic center diffuse X-ray emission (GCDX) consists of the hot plasma, neutral iron line, and hard tail. While we have demonstrated the hot plasma truly extending, origins of the others are still under discussion. We found time variability of the neutral Fe line intensity and marginally detected neutral lines of S, Ar, and Ca from Sagittarius B2. Our purpose is to clearly detect the neutral lines of S, Ar, Ca, and time variability of the hard tail of the GCDX up to 40 keV. This observation will resolve the remaining mysteries of the GCDX. | GALACTIC DIFFUSE EMISSION | 5 | A | NOBUKAWA | MASAYOSHI | NULL | NULL | JAP | 4 | AO4 | SUZAKU OBSERVATION OF SAGITTARIUS B2 -NEW APPROACH TO THE GALACTIC CENTER DIFFUSE X-RAY EMISSION- | XIS | Y |
| SGR_B2 | 266.8788 | -28.4436 | 0.63679 | -0.09938091 | 266.4718 | 55096.836412037 | 55102.6667592593 | 504004020 | 202094.5 | 200000 | 202094.5 | 202102.5 | 0 | 202094.5 | 3 | 4 | 0 | 3 | 1 | 0 | 0 | 178283.1 | 178283.1 | 303543.7 | 4 | PROCESSED | 57548.82125 | 55500 | 55133.4505092593 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040002 | The Galactic center diffuse X-ray emission (GCDX) consists of the hot plasma, neutral iron line, and hard tail. While we have demonstrated the hot plasma truly extending, origins of the others are still under discussion. We found time variability of the neutral Fe line intensity and marginally detected neutral lines of S, Ar, and Ca from Sagittarius B2. Our purpose is to clearly detect the neutral lines of S, Ar, Ca, and time variability of the hard tail of the GCDX up to 40 keV. This observation will resolve the remaining mysteries of the GCDX. | GALACTIC DIFFUSE EMISSION | 5 | A | NOBUKAWA | MASAYOSHI | NULL | NULL | JAP | 4 | AO4 | SUZAKU OBSERVATION OF SAGITTARIUS B2 -NEW APPROACH TO THE GALACTIC CENTER DIFFUSE X-RAY EMISSION- | XIS | Y |
| RIM1 | 311.6421 | 31.883 | 74.34868893 | -7.06658523 | 247.7276 | 55152.9451273148 | 55153.9488888889 | 504005010 | 40747.3 | 38000 | 40747.3 | 40747.3 | 0 | 40747.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34511.2 | 34511.2 | 86715.9 | 0 | PROCESSED | 57549.4623726852 | 55534 | 55166.4923148148 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040007 | The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. | GALACTIC DIFFUSE EMISSION | 5 | B | TSUNEMI | HIROSHI | NULL | NULL | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y |
| RIM2 | 311.426 | 31.5946 | 74.00572356 | -7.09996284 | 246.8661 | 55153.9497337963 | 55154.4843055556 | 504006010 | 26305.9 | 24000 | 26305.9 | 26305.9 | 0 | 26305.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 22237 | 22237 | 46183.9 | 0 | PROCESSED | 57549.4609490741 | 55534 | 55166.4447916667 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040007 | The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. | GALACTIC DIFFUSE EMISSION | 5 | B | TSUNEMI | HIROSHI | NULL | NULL | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y |
| RIM3 | 311.3232 | 31.2993 | 73.71675058 | -7.21258663 | 246.4181 | 55154.4849189815 | 55155.1204166667 | 504007010 | 21556.6 | 19000 | 21556.6 | 21556.6 | 0 | 21556.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17481 | 17481 | 54903.9 | 0 | PROCESSED | 57549.4865277778 | 55534 | 55166.4304166667 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040007 | The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. | GALACTIC DIFFUSE EMISSION | 5 | B | TSUNEMI | HIROSHI | NULL | NULL | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y |
| RIM4 | 311.4678 | 31.0131 | 73.56601773 | -7.48621797 | 246.0303 | 55155.1210763889 | 55155.3579166667 | 504008010 | 12102.5 | 10000 | 12102.5 | 12118.5 | 0 | 12110.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8666 | 8666 | 20455.9 | 0 | PROCESSED | 57549.475462963 | 55534 | 55166.425787037 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040007 | The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. | GALACTIC DIFFUSE EMISSION | 5 | B | TSUNEMI | HIROSHI | NULL | NULL | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y |
| RIM5 | 311.5286 | 30.6813 | 73.33464134 | -7.73161485 | 255.8951 | 55155.3611689815 | 55155.7953356482 | 504009010 | 15850.2 | 15000 | 15850.2 | 15850.2 | 0 | 15850.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12289.1 | 12289.1 | 37503.9 | 0 | PROCESSED | 57549.4934259259 | 55534 | 55166.4265277778 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040007 | The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. | GALACTIC DIFFUSE EMISSION | 5 | B | TSUNEMI | HIROSHI | NULL | NULL | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y |
| RIM6 | 314.3771 | 31.4503 | 75.4881661 | -9.14820234 | 247.047 | 55155.7987615741 | 55156.1745833333 | 504010010 | 14327.5 | 11000 | 14347.5 | 14343.5 | 0 | 14327.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10715.2 | 10715.2 | 32468 | 0 | PROCESSED | 57549.4929513889 | 55534 | 55166.4272916667 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040007 | The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. | GALACTIC DIFFUSE EMISSION | 5 | B | TSUNEMI | HIROSHI | NULL | NULL | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y |
| BLOWOUT1 | 312.2225 | 31.7347 | 74.53998499 | -7.54540267 | 244.0864 | 55158.2754166667 | 55158.9655555556 | 504011010 | 24185.4 | 23000 | 24201.4 | 24185.4 | 0 | 24193.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19476.8 | 19476.8 | 59603.9 | 1 | PROCESSED | 57549.5243055556 | 55545 | 55176.2112731482 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040007 | The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. | GALACTIC DIFFUSE EMISSION | 5 | B | TSUNEMI | HIROSHI | NULL | NULL | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y |
| BLOWOUT2 | 311.9515 | 31.5359 | 74.23825049 | -7.48819964 | 243.427 | 55158.9662615741 | 55159.5106944444 | 504012010 | 26549.4 | 23000 | 26565.4 | 26549.4 | 0 | 26573.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 19940.1 | 19940.1 | 47031.9 | 1 | PROCESSED | 57549.5397800926 | 55545 | 55176.2336921296 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040007 | The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. | GALACTIC DIFFUSE EMISSION | 5 | B | TSUNEMI | HIROSHI | NULL | NULL | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y |
| BLOWOUT3 | 311.7021 | 31.3134 | 73.92913651 | -7.4588166 | 242.4356 | 55160.1363888889 | 55160.4723611111 | 504013010 | 16159.9 | 16000 | 16159.9 | 16159.9 | 0 | 16159.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11810.1 | 11810.1 | 29021.9 | 0 | PROCESSED | 57549.5443634259 | 55545 | 55176.2365740741 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040007 | The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. | GALACTIC DIFFUSE EMISSION | 5 | B | TSUNEMI | HIROSHI | NULL | NULL | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y |
| BLOWOUT4 | 312.7282 | 31.6832 | 74.77065214 | -7.91349372 | 242.7253 | 55160.4733564815 | 55161.0044444445 | 504014010 | 17769.6 | 15000 | 17825.7 | 17769.6 | 0 | 17825.6 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 14265.7 | 14265.7 | 45876 | 0 | PROCESSED | 57549.5615509259 | 55545 | 55176.2692939815 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040007 | The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. | GALACTIC DIFFUSE EMISSION | 5 | B | TSUNEMI | HIROSHI | NULL | NULL | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y |
| BLOWOUT5 | 312.2204 | 31.3402 | 74.2273165 | -7.78955911 | 225.5762 | 55176.0660532407 | 55176.7307175926 | 504015010 | 30406.4 | 25000 | 30406.4 | 30406.4 | 0 | 30406.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28692.1 | 28692.1 | 57423.9 | 0 | PROCESSED | 57549.7666898148 | 55555 | 55189.2693981482 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040007 | The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. | GALACTIC DIFFUSE EMISSION | 5 | B | TSUNEMI | HIROSHI | NULL | NULL | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y |
| BLOWOUT6 | 311.7638 | 30.9468 | 73.67127235 | -7.72686898 | 241.7587 | 55165.8330787037 | 55166.2883449074 | 504016010 | 21000 | 19000 | 21008 | 21016 | 0 | 21000 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17712.9 | 17712.9 | 39327.9 | 0 | PROCESSED | 57549.644849537 | 55547 | 55181.2630324074 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040007 | The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. | GALACTIC DIFFUSE EMISSION | 5 | B | TSUNEMI | HIROSHI | NULL | NULL | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y |
| FESI1 | 313.4345 | 30.6099 | 74.31119672 | -9.05841998 | 226.3696 | 55182.5546180556 | 55183.3334837963 | 504017010 | 32287.6 | 24000 | 32287.6 | 32287.6 | 0 | 32287.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27212.9 | 27212.9 | 67285.9 | 0 | PROCESSED | 57549.881099537 | 55575 | 55204.4679976852 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040007 | The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. | GALACTIC DIFFUSE EMISSION | 5 | B | TSUNEMI | HIROSHI | NULL | NULL | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y |
| FESI2 | 313.183 | 30.3797 | 73.99193661 | -9.03499466 | 225.2405 | 55174.9860300926 | 55175.7904398148 | 504018010 | 34590.4 | 34000 | 34590.4 | 34590.4 | 0 | 34590.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30318 | 30318 | 69493.9 | 0 | PROCESSED | 57549.7573032407 | 55555 | 55189.1622916667 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040007 | The Cygnus Loop is a middle-aged (10,000 yr) supernova remnant. Our past observations have revealed the complex structure of the Loop. We found the abundance inhomogeneity at the edge of the shell, suggesting the existence of the non-thermal component. We also found the blowout region at the center of the Loop. Also, we found the asymmetry of the ejecta distributions, suggesting the asymmetric supernova explosion. Then, our purposes of this observation are summarized in the following three points: 1. To clarify the origin of the abundance inhomogeneity from the shell regions. 2. To determine the accurate structure of the blowout region we found. 3. To investigate the distributions of the heavy elements derived from the hot ejecta component. We propose the 410ks observations in total. | GALACTIC DIFFUSE EMISSION | 5 | B | TSUNEMI | HIROSHI | NULL | NULL | JAP | 4 | AO4 | OBSERVATION OF THE CYGNUS LOOP WITH THE SUZAKU XIS | XIS | Y |
| RXJ1713-3946_ID1 | 257.9616 | -39.5166 | 347.33828294 | -0.06271892 | 87.0007 | 55242.129375 | 55243.2502199074 | 504027010 | 61533.1 | 60000 | 61557.8 | 61533.1 | 0 | 61573.8 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 46725.9 | 46725.9 | 96823.8 | 0 | PROCESSED | 57550.6101273148 | 55622 | 55253.4734259259 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040021 | We propose to observe the brightest part of RXJ1713-3946 to study the change of the brightness profile predicted from our results by Chandra (Nature 2007). We compare the hard X-ray image and spectrum with those obtained in 2006 and also with the data to be obtained by Chandra in 2009. | GALACTIC DIFFUSE EMISSION | 5 | B | TAKAHASHI | TADAYUKI | NULL | NULL | JAP | 4 | AO4 | STUDY OF RAPID PARTICLE ACCELERATION IN RXJ1713-3946 | XIS | Y |
| RXJ1713-3946_ID2 | 258.3083 | -40.2394 | 346.91054647 | -0.70324775 | 87.0013 | 55243.7284722222 | 55244.1258564815 | 504028010 | 19009.3 | 20000 | 19009.3 | 19017.3 | 0 | 19017.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11826.3 | 11826.3 | 34331.9 | 0 | PROCESSED | 57550.6004976852 | 55622 | 55256.0518171296 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040021 | We propose to observe the brightest part of RXJ1713-3946 to study the change of the brightness profile predicted from our results by Chandra (Nature 2007). We compare the hard X-ray image and spectrum with those obtained in 2006 and also with the data to be obtained by Chandra in 2009. | GALACTIC DIFFUSE EMISSION | 5 | B | TAKAHASHI | TADAYUKI | NULL | NULL | JAP | 4 | AO4 | STUDY OF RAPID PARTICLE ACCELERATION IN RXJ1713-3946 | XIS | Y |
| RXJ1713-3946_ID3 | 258.1658 | -40.0306 | 347.01547145 | -0.49239611 | 87.0009 | 55244.1262847222 | 55244.4779398148 | 504029010 | 20871.6 | 20000 | 20903.6 | 20903.6 | 0 | 20871.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 20886.8 | 20886.8 | 30375.9 | 0 | PROCESSED | 57550.6116087963 | 55622 | 55256.0720601852 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040021 | We propose to observe the brightest part of RXJ1713-3946 to study the change of the brightness profile predicted from our results by Chandra (Nature 2007). We compare the hard X-ray image and spectrum with those obtained in 2006 and also with the data to be obtained by Chandra in 2009. | GALACTIC DIFFUSE EMISSION | 5 | B | TAKAHASHI | TADAYUKI | NULL | NULL | JAP | 4 | AO4 | STUDY OF RAPID PARTICLE ACCELERATION IN RXJ1713-3946 | XIS | Y |
| RXJ1713-3946_ID4 | 258.9125 | -40.0131 | 347.36417887 | -0.94594655 | 86.0017 | 55244.4787384259 | 55244.8903587963 | 504030010 | 22153.4 | 20000 | 22177.4 | 22169.4 | 0 | 22153.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19719.3 | 19719.3 | 35557.9 | 1 | PROCESSED | 57550.6146412037 | 55622 | 55256.0824768518 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040021 | We propose to observe the brightest part of RXJ1713-3946 to study the change of the brightness profile predicted from our results by Chandra (Nature 2007). We compare the hard X-ray image and spectrum with those obtained in 2006 and also with the data to be obtained by Chandra in 2009. | GALACTIC DIFFUSE EMISSION | 5 | B | TAKAHASHI | TADAYUKI | NULL | NULL | JAP | 4 | AO4 | STUDY OF RAPID PARTICLE ACCELERATION IN RXJ1713-3946 | XIS | Y |
| HESS J1731-347 SW | 263.0074 | -34.9458 | 353.3803333 | -0.77058494 | 92.6086 | 55245.72 | 55246.5231365741 | 504031010 | 41861.5 | 40000 | 41877.9 | 41861.5 | 0 | 41869.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34102.8 | 34102.8 | 69382 | 0 | PROCESSED | 57550.6419675926 | 55623 | 55257.0493981482 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040026 | Supernova Remnants (SNRs) detected with TeV gamma-rays and synchrotron X-rays (TeV SNRs) are the most plausible acceleration sites of Galactic cosmic rays. However, the environments of such SNRs, temperature, density, and so on, are still unknown due to the lack of thermal X-ray emission in their spectra. HESS J1731-347 is one of only 3 TeV SNRs which have a radio shell and possible thermal X-rays. With good statistics and low background observation of Suzaku XIS, we will detect thermal X-rays from the shell of HESS J1731-347 for the first time. Determining the thermal parameters will reveal us what kind of environment makes ordinal SNRs to TeV SNRs and how TeV SNRs accelerate cosmic rays in such condition. | GALACTIC DIFFUSE EMISSION | 5 | B | BAMBA | AYA | NULL | NULL | JAP | 4 | AO4 | DISCOVERING THERMAL EMISSION FROM THE ACCELERATION SITE IN TEV SNR HESS J1731-347 | XIS | Y |
| HESS J1731-347 N | 262.8483 | -34.6425 | 353.56257635 | -0.49517094 | 91.6366 | 55244.8937037037 | 55245.7189699074 | 504032010 | 41526.3 | 40000 | 41526.3 | 41526.3 | 0 | 41526.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32865.3 | 32865.3 | 71271.9 | 0 | PROCESSED | 57550.6405555556 | 55623 | 55257.0108449074 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040026 | Supernova Remnants (SNRs) detected with TeV gamma-rays and synchrotron X-rays (TeV SNRs) are the most plausible acceleration sites of Galactic cosmic rays. However, the environments of such SNRs, temperature, density, and so on, are still unknown due to the lack of thermal X-ray emission in their spectra. HESS J1731-347 is one of only 3 TeV SNRs which have a radio shell and possible thermal X-rays. With good statistics and low background observation of Suzaku XIS, we will detect thermal X-rays from the shell of HESS J1731-347 for the first time. Determining the thermal parameters will reveal us what kind of environment makes ordinal SNRs to TeV SNRs and how TeV SNRs accelerate cosmic rays in such condition. | GALACTIC DIFFUSE EMISSION | 5 | B | BAMBA | AYA | NULL | NULL | JAP | 4 | AO4 | DISCOVERING THERMAL EMISSION FROM THE ACCELERATION SITE IN TEV SNR HESS J1731-347 | XIS | Y |
| HESS J1427-608 | 216.9609 | -60.8505 | 314.40487303 | -0.14444396 | 90.5578 | 55209.5761458333 | 55212.1891666667 | 504034010 | 104137.9 | 100000 | 104137.9 | 104137.9 | 0 | 104137.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 71261.1 | 71261.1 | 225737.8 | 1 | PROCESSED | 57550.2389930556 | 55594 | 55225.4958449074 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040066 | Pulsar wind nebula (PWN) has began to be recognized as the best candidate of a large fraction of the HESS-unidentified (unID) sources. It could be true for some sources like HESS J1825-137, while other PWN candidates are sometimes listed simply because they satisfy one or two of the necessary conditions (e.g., there is an energetic pulsar nearby). We then propose a Suzaku observation of HESS J1427-608, which is the most ``unlike'' HESS-unID source to be a PWN. The advantage that we can safely exclude a PWN for its candidate allows us to identify the emission mechanism/origin of HESS J1427-608 more unambiguously compared to other unID sources. We request a 150 ks exposure to constrain the ratio between X-ray and TeV fluxes, which is a good measure of the emission mechanism of TeV sources. | GALACTIC DIFFUSE EMISSION | 5 | C | MORI | KOJI | NULL | NULL | JAP | 4 | AO4 | A SUZAKU OBSERVATION OF HESS J1427-608 | XIS | Y |
| W49B | 287.7847 | 9.1153 | 43.2812159 | -0.18378496 | 89.2674 | 54921.5302662037 | 54923.0613425926 | 504035010 | 61782.5 | 100000 | 61790.5 | 61784.5 | 0 | 61782.5 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 55155.6 | 55155.6 | 132273.9 | 3 | PROCESSED | 57546.0146412037 | 55324 | 54949.4493287037 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040075 | Observation of the W49B supernova remnant for 100 ksec is proposed to detect Ti emission line at the 3 sigma confidence level. In order to reveal whether it is a remnant of Type Ia supernova or not, detailed measurement of the rare metal elements such as Cr, Mn, Ni, and Ti is essential. We determine the type by Ti to Cr, Mn to Cr, and Ni to Fe ratios. Furthermore, we investigate whether its plasma is in the overionized status or not. | GALACTIC DIFFUSE EMISSION | 5 | B | OZAWA | MIDORI | NULL | NULL | JAP | 4 | AO4 | UNMASK THE NATURE OF W49B ! | XIS | Y |
| TORNADO | 265.1272 | -30.949 | 357.70572925 | -0.11631727 | 269.1137 | 55072.5037037037 | 55075.0093055556 | 504036010 | 125069.2 | 120000 | 125069.2 | 125077.2 | 0 | 125077.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 97091.3 | 97091.3 | 216459.8 | 3 | PROCESSED | 57548.5178356482 | 55454 | 55088.3064814815 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040076 | The Tornado is an unusual and intense radio source located in the galactic center region. It has a polarized non-thermal radio spectrum. t has very unique morphology of elongated and loop-like structure. However, no crucial observational result determining the nature has been obtained. With the Suzaku AO3 observation of the Tornado (50ks), we found interesting signs of 2.45-keV He like S-K line, diffuse emission from the "tail" and the whole "head". The purpose of this observation is to obtain precise spectrum and spatial distribution. If the thermal S-K line is confirmed and it has a high metal abundance, the nature of the Tornado is an SNR. We also investigate the extreme structure of the tail and search for power-law component in spectra. | GALACTIC DIFFUSE EMISSION | 5 | A | TSURU | TAKESHI | NULL | NULL | JAP | 4 | AO4 | REVEALING THE UNUSUAL SOURCE, THE NATURE OF THE "TORNADO", IN THE GALACTIC CENTER REGION | XIS | Y |
| GALACTICDISC3-1 | 15.309 | 67.9759 | 123.85392042 | 5.12169353 | 244.2747 | 55214.8348148148 | 55216.0225 | 504038010 | 55227.9 | 50000 | 55227.9 | 55227.9 | 0 | 55227.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43332.9 | 43332.9 | 102599.8 | 2 | PROCESSED | 57550.2600231482 | 55594 | 55228.2005092593 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040097 | To elucidate the vertical structure of the yet-not-understood excess soft X-ray emission from the galactic disk, we propose to observe two offset directions from the plane along l = 123 degree. We expect the spectra contains the 0.75 keV emission component which we discovered in the energy spectra of two midplane observations. The proposed observations will strongly constrain the nature of the sources which are responsible for the excess emission, in particular the vertical distribution in the Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | C | KIMURA | SHUNSUKE | NULL | NULL | JAP | 4 | AO4 | STUDY OF SOFT X-RAY DIFFUSE EMISSION FROM THE GALACTIC DISK: VERTICAL STRUCTURE | XIS | Y |
| GALACTICDISC3-2 | 16.1096 | 72.7817 | 123.90816526 | 9.93459858 | 241.5401 | 55216.0250115741 | 55217.5772685185 | 504039010 | 73528.2 | 70000 | 73528.2 | 73528.2 | 0 | 73528.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 54648 | 54648 | 134105.8 | 1 | PROCESSED | 57550.3049884259 | 55602 | 55236.1178240741 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040097 | To elucidate the vertical structure of the yet-not-understood excess soft X-ray emission from the galactic disk, we propose to observe two offset directions from the plane along l = 123 degree. We expect the spectra contains the 0.75 keV emission component which we discovered in the energy spectra of two midplane observations. The proposed observations will strongly constrain the nature of the sources which are responsible for the excess emission, in particular the vertical distribution in the Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | C | KIMURA | SHUNSUKE | NULL | NULL | JAP | 4 | AO4 | STUDY OF SOFT X-RAY DIFFUSE EMISSION FROM THE GALACTIC DISK: VERTICAL STRUCTURE | XIS | Y |
| ASO0382 | 265.491 | -20.8915 | 6.43327069 | 4.9108593 | 101.5727 | 55276.7369328704 | 55277.3869675926 | 504040010 | 21222.3 | 20000 | 21222.3 | 21222.3 | 0 | 21222.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 3974 | 3974 | 56108.9 | 2 | PROCESSED | 57550.9335069444 | 55665 | 55299.411875 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040101 | Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. | GALACTIC DIFFUSE EMISSION | 5 | A | KAWAI | NOBUYUKI | NULL | NULL | JAP | 4 | AO4 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y |
| ASO0078 | 59.472 | 32.09 | 162.76236061 | -16.0043339 | 83.0007 | 55045.8202777778 | 55046.3273032407 | 504041010 | 21312 | 20000 | 21320 | 21320 | 0 | 21312 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 21295.9 | 21295.9 | 43799.9 | 0 | PROCESSED | 57548.0349074074 | 55430 | 55064.0383912037 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040101 | Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. | GALACTIC DIFFUSE EMISSION | 5 | A | KAWAI | NOBUYUKI | NULL | NULL | JAP | 4 | AO4 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y |
| ASO0402 | 273.3436 | -12.7608 | 17.24676471 | 2.45193699 | 68.9842 | 55277.3929513889 | 55277.9793287037 | 504042010 | 25712.5 | 20000 | 25712.5 | 25712.5 | 0 | 25712.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16015.2 | 16015.2 | 50655.9 | 1 | PROCESSED | 57550.9498958333 | 55784 | 55417.0893865741 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040101 | Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. | GALACTIC DIFFUSE EMISSION | 5 | A | KAWAI | NOBUYUKI | NULL | NULL | JAP | 4 | AO4 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y |
| ASO0431 | 286.9632 | 6.0295 | 40.16756672 | -0.88470452 | 90.0004 | 54936.153287037 | 54936.8141666667 | 504043010 | 24522.2 | 20000 | 24522.2 | 24522.2 | 0 | 24522.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18105 | 18105 | 57073.9 | 0 | PROCESSED | 57546.1491087963 | 55324 | 54949.5652777778 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040101 | Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. | GALACTIC DIFFUSE EMISSION | 5 | A | KAWAI | NOBUYUKI | NULL | NULL | JAP | 4 | AO4 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y |
| ASO0449 | 299.6429 | 28.7759 | 65.87759933 | -0.32938525 | 56.1427 | 54974.6386921296 | 54975.5786342593 | 504044010 | 38733.7 | 20000 | 38733.7 | 38741.7 | 0 | 38741.7 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 35220 | 35220 | 81199.9 | 2 | PROCESSED | 57546.6654050926 | 55356 | 54987.4424652778 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040101 | Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. | GALACTIC DIFFUSE EMISSION | 5 | A | KAWAI | NOBUYUKI | NULL | NULL | JAP | 4 | AO4 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y |
| ASO0218 | 157.1332 | -58.313 | 285.06973918 | -0.48663651 | 315.2825 | 55020.3423148148 | 55020.9467476852 | 504045010 | 22844.9 | 20000 | 22844.9 | 22844.9 | 0 | 22844.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21154.4 | 21154.4 | 52217.9 | 1 | PROCESSED | 57547.7933680556 | 55400 | 55034.2716898148 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040101 | Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. | GALACTIC DIFFUSE EMISSION | 5 | A | KAWAI | NOBUYUKI | NULL | NULL | JAP | 4 | AO4 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y |
| ASO0447 | 298.557 | 28.6365 | 65.2636943 | 0.41202338 | 90.516 | 54928.7514699074 | 54929.253587963 | 504046010 | 20545.7 | 20000 | 20545.7 | 20545.7 | 0 | 20545.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16907.1 | 16907.1 | 43377.9 | 1 | PROCESSED | 57546.0447106482 | 55324 | 54949.4485300926 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040101 | Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. | GALACTIC DIFFUSE EMISSION | 5 | A | KAWAI | NOBUYUKI | NULL | NULL | JAP | 4 | AO4 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y |
| ASO0147 | 98.4346 | 6.5402 | 205.09585789 | -0.932863 | 292.0552 | 54931.9181481482 | 54932.5036921296 | 504047010 | 24041.3 | 20000 | 24041.3 | 24041.3 | 0 | 24041.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 23240.9 | 23240.9 | 50562 | 1 | PROCESSED | 57546.1122685185 | 55324 | 54949.5271180556 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040101 | Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. | GALACTIC DIFFUSE EMISSION | 5 | A | KAWAI | NOBUYUKI | NULL | NULL | JAP | 4 | AO4 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y |
| ASO0505 | 339.5988 | 59.0734 | 106.55945745 | 0.49758229 | 62.7751 | 55001.185775463 | 55001.7494675926 | 504048010 | 26361.6 | 20000 | 26369.6 | 26361.6 | 0 | 26377.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 23841.6 | 23841.6 | 48695.9 | 1 | PROCESSED | 57547.5983449074 | 55381 | 55015.2523148148 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040101 | Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. | GALACTIC DIFFUSE EMISSION | 5 | A | KAWAI | NOBUYUKI | NULL | NULL | JAP | 4 | AO4 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y |
| ASO0376 | 263.1417 | -31.5448 | 356.29011362 | 0.99386623 | 267.5095 | 55082.1506365741 | 55083.1084606482 | 504049010 | 37227.8 | 20000 | 38987.8 | 39259.8 | 0 | 37227.8 | 5 | 4 | 0 | 4 | 1 | 0 | 0 | 31813.4 | 31813.4 | 82729.9 | 1 | PROCESSED | 57548.4976041667 | 55479 | 55113.2260069444 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040101 | Fermi Gamma-Ray Space Telescope has detected 29 gamma-ray pulsars in its first three month operation. We propose Suzaku observation of 10 new pulsars among them that have little previous coverage in X-ray band. We search for X-ray emission originating from (1) pulsar magnetosphere, (2) neutron star surface, (3) pulsar wind nebula, or (4) associated supernova remnant, with which we investigate the distance, environment, age and wind properties of these pulsars. Based on this information we aim to study the emission mechanism and particle acceleration in pulsars. | GALACTIC DIFFUSE EMISSION | 5 | A | KAWAI | NOBUYUKI | NULL | NULL | JAP | 4 | AO4 | X-RAY COUNTERPARTS OF NEW FERMI GAMMA-RAY PULSARS | XIS | Y |
| (L,B)=(0.107,-1.425) | 267.8602 | -29.5833 | 0.10035042 | -1.42140103 | 68.0986 | 55261.1636226852 | 55263.893275463 | 504050010 | 100399.1 | 100000 | 100431.1 | 100399.1 | 0 | 100423.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 80536 | 80536 | 235821.8 | 1 | PROCESSED | 57550.8323726852 | 55645 | 55278.4832523148 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040109 | In order to resolve origin of the Galactic bulge/ridge emission, we propose to observe the blank field 1.5 deg from the Galactic center where Chandra recently performed the deepest exposure (900 ksec) aiming to resolve the Galactic "diffuse" emission into point sources. Goals of the present observation are the following: (1) Resolve the three iron emission lines (6.41 keV, 6.67 keV and 6.97 keV) with Suzaku, and compare with the point source population determined by Chandra to clarify what kinds of sources are responsible for which emission line. (2) Study Galactic latitudinal variation of the three emission lines comparing with the existent Suzaku observation at (l,b)=(0.0, -2.0). (3) Constrain the hard-tail emission above 10 keV, and study its Galactic latitudinal variation. | GALACTIC DIFFUSE EMISSION | 5 | B | EBISAWA | KEN | NULL | NULL | JAP | 4 | AO4 | RESOLVING ORIGIN OF THE IRON EMISSION LINES FROM THE GALACTIC BULGE | XIS | Y |
| ASO0418 | 279.775 | -5.7085 | 26.44714681 | 0.13153934 | 86.843 | 54934.6472800926 | 54935.7578587963 | 504052010 | 41068.4 | 40000 | 41080.2 | 41084.4 | 0 | 41068.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 33525.8 | 33525.8 | 95937.8 | 0 | PROCESSED | 57546.1671296296 | 55324 | 54949.5662268518 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040112 | We propose Suzaku observations of the fields of four Fermi-LAT sources on the Galactic plane. With the improved Fermi-LAT locations, we expect to identify the X-ray counterparts based on their morphologies and spectra, and categorize them into classes of known GeV gamma-ray sources (pulsars and AGNs) and VHE gamma-ray sources (SNRs, PWNe and colliding wind binaries), and possibly find a new class of objects. With these studies we hope to understand the population and emission mechanism of high energy sources in the Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KAWAI | NOBUYUKI | NULL | NULL | JAP | 4 | AO4 | UNIDENTIFIED FERMI-LAT GAMMA-RAY SOURCES ON THE GALACTIC PLANE | XIS | Y |
| ASO0215 | 154.6836 | -58.9426 | 284.32918046 | -1.70077172 | 314.5017 | 55019.3141782407 | 55020.3404976852 | 504053010 | 40086.8 | 40000 | 40086.8 | 40086.8 | 0 | 40086.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35478.2 | 35478.2 | 88659.8 | 0 | PROCESSED | 57547.8126851852 | 55399 | 55029.2468055556 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040112 | We propose Suzaku observations of the fields of four Fermi-LAT sources on the Galactic plane. With the improved Fermi-LAT locations, we expect to identify the X-ray counterparts based on their morphologies and spectra, and categorize them into classes of known GeV gamma-ray sources (pulsars and AGNs) and VHE gamma-ray sources (SNRs, PWNe and colliding wind binaries), and possibly find a new class of objects. With these studies we hope to understand the population and emission mechanism of high energy sources in the Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KAWAI | NOBUYUKI | NULL | NULL | JAP | 4 | AO4 | UNIDENTIFIED FERMI-LAT GAMMA-RAY SOURCES ON THE GALACTIC PLANE | XIS | Y |
| ASO0304 | 213.3355 | -62.0808 | 312.3597658 | -0.71761471 | 280.2937 | 55036.9044907407 | 55038.1453935185 | 504054010 | 44248.5 | 40000 | 44248.5 | 44248.5 | 0 | 44248.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41083.9 | 41083.9 | 107201.8 | 1 | PROCESSED | 57547.9369791667 | 55415 | 55048.3203819444 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040112 | We propose Suzaku observations of the fields of four Fermi-LAT sources on the Galactic plane. With the improved Fermi-LAT locations, we expect to identify the X-ray counterparts based on their morphologies and spectra, and categorize them into classes of known GeV gamma-ray sources (pulsars and AGNs) and VHE gamma-ray sources (SNRs, PWNe and colliding wind binaries), and possibly find a new class of objects. With these studies we hope to understand the population and emission mechanism of high energy sources in the Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KAWAI | NOBUYUKI | NULL | NULL | JAP | 4 | AO4 | UNIDENTIFIED FERMI-LAT GAMMA-RAY SOURCES ON THE GALACTIC PLANE | XIS | Y |
| ASO0319 | 224.8822 | -60.8823 | 317.89227503 | -1.78687667 | 277.7774 | 55049.7078125 | 55051.0238425926 | 504055010 | 42361.3 | 40000 | 42361.3 | 42366.8 | 0 | 42377.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37523.3 | 37523.3 | 113685.9 | 0 | PROCESSED | 57548.1027083333 | 55430 | 55062.2941782407 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040112 | We propose Suzaku observations of the fields of four Fermi-LAT sources on the Galactic plane. With the improved Fermi-LAT locations, we expect to identify the X-ray counterparts based on their morphologies and spectra, and categorize them into classes of known GeV gamma-ray sources (pulsars and AGNs) and VHE gamma-ray sources (SNRs, PWNe and colliding wind binaries), and possibly find a new class of objects. With these studies we hope to understand the population and emission mechanism of high energy sources in the Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KAWAI | NOBUYUKI | NULL | NULL | JAP | 4 | AO4 | UNIDENTIFIED FERMI-LAT GAMMA-RAY SOURCES ON THE GALACTIC PLANE | XIS | Y |
| HESSJ1616_PSRJ1617 | 244.3756 | -50.9175 | 332.50297445 | -0.27465368 | 270.0711 | 55059.1110763889 | 55060.8328009259 | 504056010 | 65833.1 | 50000 | 65889.1 | 65833.1 | 0 | 65897.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41750.4 | 41750.4 | 148725.8 | 0 | PROCESSED | 57548.1892708333 | 55437 | 55071.2513425926 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040115 | HESSJ1616-508 is one of the most energetic unidentified TeV object. Previously, we showed that there is no clear X-ray counterpart to this object with a Suzaku observation, and hence we argued that the object is a real dark particle accelerator. However, there is a young energetic pulsar PSRJ1617-5055 10 arcmin away from HESSJ1616, and another possibility has been proposed that HESSJ1616 is an offset pulsar wind nebula (PWN) driven by the pulsar. If this possibility is correct, a powerful X-ray PWN should be observed as HESSJ1825-137, but such PWN has not been reported. The lack of the detection may be due to small sensitivity of Chandra and XMM-Newton for a diffuse hard X-ray emission. We propose to observe PSRJ1617 to see if there is an extended PWN around this pulsar. | GALACTIC DIFFUSE EMISSION | 5 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 4 | AO4 | IS THE MOST ENERGETIC UNIDENTIFIED TEV OBJECT HESSJ1616-508 A PULSAR WIND NEBULA? | XIS | Y |
| VICINITY OF NGC 4051 | 180.4686 | 44.1146 | 150.13143213 | 70.30340869 | 109.3717 | 55184.3459606482 | 55186.5140509259 | 504062010 | 89630.5 | 80000 | 89638.5 | 89646.5 | 0 | 89630.5 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 37075.8 | 37075.8 | 187281.9 | 2 | PROCESSED | 57549.977337963 | 55581 | 55209.4570833333 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040120 | The highly ionized absorption lines of OVII and OVII at z = 0 have been unambiguously detected toward the bright AGN NGC 4051 by the high-resolution spectrometers onboard Chandra and XMM-Newton. However, the spatial extent and thus the nature of the absorbing warm-hot gas are yet unknown; it can be from 1 Mpc scale WHIM (Warm-hot intergalactic medium) to a few kpc scale galactic wind. We propose to observe the very vicinity of the AGN to determine the OVII and OVIII emission line intensities and the temperature of the warm-hot gas. Joint analysis of absorption and emission lines will unambiguously constrain the spatial extent of the warm-hot gas. | GALACTIC DIFFUSE EMISSION | 5 | C | HAGIHARA | TOSHISHIGE | NULL | NULL | JAP | 4 | AO4 | STUDY OF WARM-HOT GAS TOWARD NGC 4051 | XIS | Y |
| VELA SOUTHWEST 1 | 126.2671 | -48.2152 | 264.99036518 | -5.99332729 | 119.5649 | 55164.9700925926 | 55165.818900463 | 504063010 | 32733.1 | 30000 | 32749.2 | 32733.1 | 0 | 32741.1 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 23767.4 | 23767.4 | 73309.9 | 0 | PROCESSED | 57549.6219791667 | 55546 | 55179.268587963 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040121 | We propose 2 pointing-observations of south western part of Vela supernova remnant. Vela SNR has the largest angular size of 8 degree in diameter, so it is suitable to carry out spatial resolved spectroscopy with Suzaku. | GALACTIC DIFFUSE EMISSION | 5 | C | HIRAGA | JUNKO | NULL | NULL | JAP | 4 | AO4 | X-RAY STUDY ON THE NEAREST SUPERNOVA REMNANT, VELA | XIS | Y |
| W51NW | 290.6858 | 14.2133 | 49.11550833 | -0.31636783 | 105.4558 | 55283.4893634259 | 55284.555 | 504066010 | 44112.5 | 40000 | 44120.5 | 44120.5 | 0 | 44112.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8896.1 | 8896.1 | 92063.9 | 0 | PROCESSED | 57551.0258217593 | 55671 | 55302.5003240741 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040129 | We propose to observe the supernova remnant (SNR) W51C with Suzaku XIS. The thermal energy of plasma in W51C, ~3x10^51ergs, is much larger than typical kinetic energy of supernova and can give a large amount of energy to cosmic-ray acceleration. The SNR interactes with the giant molecler cloud and is expected to emit gamma-rays from cosmic-ray interaction. We search for non-thermal X-ray diffuse emission from electron bremsstrahlung or synchrotron emission of secondary electrons produced by decaying charged pions created by p-p interaction. | GALACTIC DIFFUSE EMISSION | 5 | C | KATAGIRI | HIDEAKI | NULL | NULL | JAP | 4 | AO4 | ENERGETIC PATICLE ACCELERATOR AT THE SAGITTARIUS ARM : SUPERNOVA REMNANT W51C | XIS | Y |
| W51SW | 290.8908 | 14.1062 | 49.1149541 | -0.54215584 | 104.3698 | 55285.3081944444 | 55286.3752314815 | 504067010 | 43728.7 | 40000 | 43728.7 | 43728.7 | 0 | 43728.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 9813.7 | 9813.7 | 92179.9 | 0 | PROCESSED | 57551.0856597222 | 55671 | 55302.2468055556 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040129 | We propose to observe the supernova remnant (SNR) W51C with Suzaku XIS. The thermal energy of plasma in W51C, ~3x10^51ergs, is much larger than typical kinetic energy of supernova and can give a large amount of energy to cosmic-ray acceleration. The SNR interactes with the giant molecler cloud and is expected to emit gamma-rays from cosmic-ray interaction. We search for non-thermal X-ray diffuse emission from electron bremsstrahlung or synchrotron emission of secondary electrons produced by decaying charged pions created by p-p interaction. | GALACTIC DIFFUSE EMISSION | 5 | C | KATAGIRI | HIDEAKI | NULL | NULL | JAP | 4 | AO4 | ENERGETIC PATICLE ACCELERATOR AT THE SAGITTARIUS ARM : SUPERNOVA REMNANT W51C | XIS | Y |
| SEP #1 | 89.966 | -66.5774 | 276.40322057 | -29.82494721 | 141.7136 | 55149.1175925926 | 55150.2141087963 | 504069010 | 51862.1 | 50000 | 51870.1 | 51862.1 | 0 | 51870.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48353.4 | 48353.4 | 94725.9 | 2 | PROCESSED | 57549.3577546296 | 54922 | 55160.1496296296 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041101 | We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe. | GALACTIC DIFFUSE EMISSION | 5 | A | SNOWDEN | STEVEN | NULL | NULL | USA | 4 | AO4 | OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE | XIS | Y |
| NEP #1 | 270.0492 | 66.5597 | 96.38280784 | 29.79186901 | 217.1802 | 55150.229212963 | 55151.1953587963 | 504070010 | 56336.7 | 50000 | 56336.7 | 56344.7 | 0 | 56344.7 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 41434.5 | 41434.5 | 83471.9 | 2 | PROCESSED | 57549.3863657407 | 54922 | 55162.2062268518 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041101 | We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe. | GALACTIC DIFFUSE EMISSION | 5 | A | SNOWDEN | STEVEN | NULL | NULL | USA | 4 | AO4 | OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE | XIS | Y |
| SEP #2 | 89.966 | -66.5714 | 276.39630454 | -29.82495373 | 163.7813 | 55170.9454166667 | 55172.4863194444 | 504071010 | 57999.1 | 50000 | 58007.1 | 57999.1 | 0 | 58007.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35415.2 | 35415.2 | 133112 | 1 | PROCESSED | 57549.7252546296 | 54922 | 55187.4854398148 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041101 | We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe. | GALACTIC DIFFUSE EMISSION | 5 | A | SNOWDEN | STEVEN | NULL | NULL | USA | 4 | AO4 | OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE | XIS | Y |
| NEP #2 | 270.0521 | 66.5655 | 96.38949161 | 29.79071779 | 194.6438 | 55172.5015162037 | 55173.6411342593 | 504072010 | 48697.7 | 50000 | 48697.7 | 48697.7 | 0 | 48697.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38458.2 | 38458.2 | 98456 | 1 | PROCESSED | 57549.730775463 | 54922 | 55190.01875 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041101 | We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe. | GALACTIC DIFFUSE EMISSION | 5 | A | SNOWDEN | STEVEN | NULL | NULL | USA | 4 | AO4 | OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE | XIS | Y |
| SEP #3 | 89.9578 | -66.5683 | 276.39273536 | -29.82821774 | 172.4885 | 55179.5059259259 | 55180.9169444444 | 504073010 | 44408 | 50000 | 44408 | 44416 | 0 | 44416 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 23878.4 | 23878.4 | 121901.8 | 1 | PROCESSED | 57549.8504282407 | 54922 | 55200.462337963 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041101 | We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe. | GALACTIC DIFFUSE EMISSION | 5 | A | SNOWDEN | STEVEN | NULL | NULL | USA | 4 | AO4 | OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE | XIS | Y |
| NEP #3 | 270.0483 | 66.5696 | 96.39421541 | 29.79223028 | 188.0738 | 55180.9320949074 | 55182.0557638889 | 504074010 | 50176.9 | 50000 | 50176.9 | 50176.9 | 0 | 50176.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 33337.4 | 33337.4 | 97049.9 | 1 | PROCESSED | 57549.895162037 | 54922 | 55200.4707291667 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041101 | We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe. | GALACTIC DIFFUSE EMISSION | 5 | A | SNOWDEN | STEVEN | NULL | NULL | USA | 4 | AO4 | OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE | XIS | Y |
| SEP #4 | 89.9798 | -66.5683 | 276.39272547 | -29.81946932 | 185.1981 | 55192.0059490741 | 55193.3995833333 | 504075010 | 49956.6 | 50000 | 49956.6 | 49956.6 | 0 | 49956.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45143 | 45143 | 120393.9 | 1 | PROCESSED | 57549.980474537 | 54922 | 55225.3094907407 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041101 | We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe. | GALACTIC DIFFUSE EMISSION | 5 | A | SNOWDEN | STEVEN | NULL | NULL | USA | 4 | AO4 | OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE | XIS | Y |
| NEP #4 | 270.0449 | 66.5788 | 96.40481628 | 29.79358389 | 165.3654 | 55193.4146875 | 55194.4579166667 | 504076010 | 49849.1 | 50000 | 49857.1 | 49857.1 | 0 | 49849.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43503.9 | 43503.9 | 90114 | 0 | PROCESSED | 57550.0085648148 | 54922 | 55246.2930787037 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041101 | We propose a series of four coupled north and south ecliptic pole pointings to observe solar wind charge exchange (SWCX) emission from the interplanetary density enhancement of the He focusing cone. The purpose of the observations is to test, verify, and calibrate models for diffuse X-ray emission from the heliosphere, the source of both a significant contamination for observations of extended structures in the cosmic diffuse X-ray background as well as a source of diagnostic information for the solar wind and structure within the solar system. A well-calibrated model for heliospheric SWCX emission can be used to untangle the very local and more distant components of the observed soft X-ray background affecting our understanding of the Milky Way and the local universe. | GALACTIC DIFFUSE EMISSION | 5 | A | SNOWDEN | STEVEN | NULL | NULL | USA | 4 | AO4 | OBSERVING SOLAR WIND CHARGE EXCHANGE EMISSION FROM THE INTERPLANETARY HELIUM FOCUSING CONE | XIS | Y |
| HESS J1809-193A | 273.0012 | -19.0034 | 11.60922783 | -0.25253702 | 270.0939 | 55083.2051967593 | 55084.4828009259 | 504077010 | 52110.9 | 50000 | 52174.5 | 52190.8 | 0 | 52110.9 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 44109 | 44109 | 110376 | 1 | PROCESSED | 57548.5474189815 | 55475 | 55109.4207638889 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041303 | We propose a detailed study of the extended VHE source HESS J1809-193 neighboring young PSR J1809-1917 with a known X-ray pulsar-wind nebula (PWN). As the chance coincidence is very unlikely, there should be a connection between the two. Furthermore, previous short Chandra observations of this field have revealed a large-scale asymmetric PWN extending toward the center of the TeV source. Thus, this is an excellent case for testing whether the unidentified TeV sources near young pulsars are, in fact, relic PWNe crushed by the asymmetric SNR reverse shock. We will probe the nature of the X-ray emission by measuring the surface brightness and spatially-resolved spectra across the large extent of the TeV source. Suzaku XIS is ideally suited for this purpose because of its low background. | GALACTIC DIFFUSE EMISSION | 5 | A | KARGALTSEV | OLEG | NULL | NULL | USA | 4 | AO4 | CRUSHED PLERION HESS J1809-193: TEV TO X-RAY CONNECTION | XIS | Y |
| HESS J1809-193B | 272.6789 | -19.1585 | 11.32661741 | -0.06027609 | 269.0544 | 55084.4838773148 | 55085.7488310185 | 504078010 | 52474.8 | 50000 | 52474.8 | 52474.8 | 0 | 52474.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43373.3 | 43373.3 | 109275.8 | 1 | PROCESSED | 57548.5486226852 | 55475 | 55109.4280555556 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041303 | We propose a detailed study of the extended VHE source HESS J1809-193 neighboring young PSR J1809-1917 with a known X-ray pulsar-wind nebula (PWN). As the chance coincidence is very unlikely, there should be a connection between the two. Furthermore, previous short Chandra observations of this field have revealed a large-scale asymmetric PWN extending toward the center of the TeV source. Thus, this is an excellent case for testing whether the unidentified TeV sources near young pulsars are, in fact, relic PWNe crushed by the asymmetric SNR reverse shock. We will probe the nature of the X-ray emission by measuring the surface brightness and spatially-resolved spectra across the large extent of the TeV source. Suzaku XIS is ideally suited for this purpose because of its low background. | GALACTIC DIFFUSE EMISSION | 5 | A | KARGALTSEV | OLEG | NULL | NULL | USA | 4 | AO4 | CRUSHED PLERION HESS J1809-193: TEV TO X-RAY CONNECTION | XIS | Y |
| HESS J1809-193E | 272.0013 | -19.5033 | 10.71539243 | 0.332309 | 270.1011 | 55085.7498148148 | 55087.1564351852 | 504079010 | 51028.9 | 50000 | 51028.9 | 51028.9 | 0 | 51028.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41875.3 | 41875.3 | 121519.8 | 2 | PROCESSED | 57548.5914699074 | 55465 | 55098.3372337963 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041303 | We propose a detailed study of the extended VHE source HESS J1809-193 neighboring young PSR J1809-1917 with a known X-ray pulsar-wind nebula (PWN). As the chance coincidence is very unlikely, there should be a connection between the two. Furthermore, previous short Chandra observations of this field have revealed a large-scale asymmetric PWN extending toward the center of the TeV source. Thus, this is an excellent case for testing whether the unidentified TeV sources near young pulsars are, in fact, relic PWNe crushed by the asymmetric SNR reverse shock. We will probe the nature of the X-ray emission by measuring the surface brightness and spatially-resolved spectra across the large extent of the TeV source. Suzaku XIS is ideally suited for this purpose because of its low background. | GALACTIC DIFFUSE EMISSION | 5 | A | KARGALTSEV | OLEG | NULL | NULL | USA | 4 | AO4 | CRUSHED PLERION HESS J1809-193: TEV TO X-RAY CONNECTION | XIS | Y |
| G156.2+5.7 (S) | 74.9073 | 51.0204 | 156.85145441 | 5.28162006 | 265.6871 | 55259.9832407407 | 55261.1495833333 | 504080010 | 52641.3 | 50000 | 52649.3 | 52641.3 | 0 | 52649.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47656.6 | 47656.6 | 100757.8 | 0 | PROCESSED | 57550.7899189815 | 55689 | 55323.2891666667 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041311 | The large Galactic (R=50') supernova remnant (SNR) G156.2+5.7 is one of the few evolved SNRs with possible X-ray non-thermal (hard-tail) emission. Based on our recent observations with the Suzaku XIS, we found an indication of correlation between the X-ray hard-tail emission and radio emission. In addition, we confirmed the existence of metal-rich ejecta in the central portion, but found no evidence of ejecta in the rim regions. To investigate the correlation between the X-ray hard-tail emission and the radio emission, and the distributions of the X-ray emitting ejecta in this SNR, we propose to extend our observations with the Suzaku XIS. We request three pointings with a total exposure time of 150 ks. | GALACTIC DIFFUSE EMISSION | 5 | C | KATSUDA | SATORU | NULL | NULL | USA | 4 | AO4 | REVEALING X-RAY HARD-TAIL AND EJECTA STRUCTURES IN THE EVOLVED SNR G156.2+5.7 | XIS | Y |
| G156.2+5.7 (NW2) | 74.4322 | 52.0607 | 155.84514532 | 5.68920631 | 266.0115 | 55258.7553587963 | 55259.9821643518 | 504081010 | 52864.6 | 50000 | 52867.8 | 52867.8 | 0 | 52864.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 49386.6 | 49386.6 | 105991 | 1 | PROCESSED | 57550.7899189815 | 55689 | 55322.3173842593 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041311 | The large Galactic (R=50') supernova remnant (SNR) G156.2+5.7 is one of the few evolved SNRs with possible X-ray non-thermal (hard-tail) emission. Based on our recent observations with the Suzaku XIS, we found an indication of correlation between the X-ray hard-tail emission and radio emission. In addition, we confirmed the existence of metal-rich ejecta in the central portion, but found no evidence of ejecta in the rim regions. To investigate the correlation between the X-ray hard-tail emission and the radio emission, and the distributions of the X-ray emitting ejecta in this SNR, we propose to extend our observations with the Suzaku XIS. We request three pointings with a total exposure time of 150 ks. | GALACTIC DIFFUSE EMISSION | 5 | C | KATSUDA | SATORU | NULL | NULL | USA | 4 | AO4 | REVEALING X-RAY HARD-TAIL AND EJECTA STRUCTURES IN THE EVOLVED SNR G156.2+5.7 | XIS | Y |
| G156.2+5.7 (E2) | 75.2673 | 51.6789 | 156.46612231 | 5.86221802 | 271.6298 | 55248.7736574074 | 55250.0369675926 | 504082010 | 50330.8 | 50000 | 50346.8 | 50330.8 | 0 | 50346.8 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 46142.4 | 46142.4 | 109137.9 | 0 | PROCESSED | 57550.6943865741 | 55632 | 55266.2981597222 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041311 | The large Galactic (R=50') supernova remnant (SNR) G156.2+5.7 is one of the few evolved SNRs with possible X-ray non-thermal (hard-tail) emission. Based on our recent observations with the Suzaku XIS, we found an indication of correlation between the X-ray hard-tail emission and radio emission. In addition, we confirmed the existence of metal-rich ejecta in the central portion, but found no evidence of ejecta in the rim regions. To investigate the correlation between the X-ray hard-tail emission and the radio emission, and the distributions of the X-ray emitting ejecta in this SNR, we propose to extend our observations with the Suzaku XIS. We request three pointings with a total exposure time of 150 ks. | GALACTIC DIFFUSE EMISSION | 5 | C | KATSUDA | SATORU | NULL | NULL | USA | 4 | AO4 | REVEALING X-RAY HARD-TAIL AND EJECTA STRUCTURES IN THE EVOLVED SNR G156.2+5.7 | XIS | Y |
| 330.2+1.0 | 240.2338 | -51.588 | 330.14009051 | 0.98414205 | 285.0002 | 55078.1480671296 | 55080.8126736111 | 504083010 | 127774.6 | 150000 | 127782.6 | 127774.6 | 0 | 127774.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 112848.4 | 112848.4 | 230157.8 | 1 | PROCESSED | 57548.4938657407 | 55455 | 55089.3295949074 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041312 | Observations of G330.2+1.0 have revealed that it is a rare supernova remnant whose X-ray emission is dominated by synchrotron radiation. The available X-ray data provides rather poor constraints on the physical properties of the remnant. We propose to perform a deep Suzaku observation to obtain good spectral data. Joint spectral analyses of Suzaku and radio data will enable us to accurately and precisely measure the synchrotron spectral index and cutoff frequency, the electron temperature, the emission measure, and, perhaps, the relative elemental abundances. As a result, it will be possible to compute accurate and precise values for the spectral index and maximum energy of the nonthermal electrons, the strength of the magnetic field, and the ambient density, age, and shock velocity. | GALACTIC DIFFUSE EMISSION | 5 | B | ALLEN | GLENN | NULL | NULL | USA | 4 | AO4 | MULTIWAVELENGTH SPECTROSCOPY OF 330.2 1.0 | XIS | Y |
| 330.2+1.0 | 240.2338 | -51.5878 | 330.14022152 | 0.98429318 | 285.0004 | 55081.4851273148 | 55082.1453472222 | 504083020 | 30889.6 | 30000 | 30889.6 | 30889.6 | 0 | 30897.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27076.4 | 27076.4 | 57037.9 | 0 | PROCESSED | 57548.4451736111 | 55458 | 55092.1620949074 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041312 | Observations of G330.2+1.0 have revealed that it is a rare supernova remnant whose X-ray emission is dominated by synchrotron radiation. The available X-ray data provides rather poor constraints on the physical properties of the remnant. We propose to perform a deep Suzaku observation to obtain good spectral data. Joint spectral analyses of Suzaku and radio data will enable us to accurately and precisely measure the synchrotron spectral index and cutoff frequency, the electron temperature, the emission measure, and, perhaps, the relative elemental abundances. As a result, it will be possible to compute accurate and precise values for the spectral index and maximum energy of the nonthermal electrons, the strength of the magnetic field, and the ambient density, age, and shock velocity. | GALACTIC DIFFUSE EMISSION | 5 | B | ALLEN | GLENN | NULL | NULL | USA | 4 | AO4 | MULTIWAVELENGTH SPECTROSCOPY OF 330.2 1.0 | XIS | Y |
| 330.2+1.0 | 240.2384 | -51.525 | 330.18352169 | 1.02987491 | 98.9027 | 55239.832025463 | 55242.125150463 | 504083030 | 92505 | 30000 | 92513 | 92505 | 0 | 92521 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 86096.5 | 86096.5 | 198089.7 | 4 | PROCESSED | 57550.6564699074 | 55622 | 55253.5397685185 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041312 | Observations of G330.2+1.0 have revealed that it is a rare supernova remnant whose X-ray emission is dominated by synchrotron radiation. The available X-ray data provides rather poor constraints on the physical properties of the remnant. We propose to perform a deep Suzaku observation to obtain good spectral data. Joint spectral analyses of Suzaku and radio data will enable us to accurately and precisely measure the synchrotron spectral index and cutoff frequency, the electron temperature, the emission measure, and, perhaps, the relative elemental abundances. As a result, it will be possible to compute accurate and precise values for the spectral index and maximum energy of the nonthermal electrons, the strength of the magnetic field, and the ambient density, age, and shock velocity. | GALACTIC DIFFUSE EMISSION | 5 | B | ALLEN | GLENN | NULL | NULL | USA | 4 | AO4 | MULTIWAVELENGTH SPECTROSCOPY OF 330.2 1.0 | XIS | Y |
| NGC 6888 | 303.111 | 38.3992 | 75.54872423 | 2.39562358 | 36.3096 | 54999.0718981482 | 55001.1793287037 | 504084010 | 88846.8 | 75000 | 88854.8 | 88846.8 | 0 | 88854.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 82405.2 | 82405.2 | 182067.9 | 2 | PROCESSED | 57547.6754976852 | 55378 | 55012.4221180556 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041321 | Fast winds from massive stars create large cavities in the surrounding interstellar medium filled with hot gas, known as Wind-Blown Bubbles (WBB). We propose to obtain XIS imaging spectroscopy of the prototype WBB NGC 6888. Thanks to the XIS excellent sensitivity and energy resolution in the soft X-ray band, we will: (i) obtain a high quality CCD spectrum which can be used to constrain the temperature of the hot plasma and the efficiency of thermal conduction across the bubble wall, (ii) determine the spatial distribution and properties of X-ray emitting plasma, (iii) therefore, test and refine shock physics models of bubbles by a direct confrontation of their results with observations. | GALACTIC DIFFUSE EMISSION | 5 | A | ZHEKOV | SVETOZAR | NULL | NULL | USA | 4 | AO4 | X-RAYS FROM THE PROTOTYPE WIND-BLOWN BUBBLE NGC 6888 | XIS | Y |
| NGC 6888 | 302.9954 | 38.2382 | 75.36419968 | 2.38310331 | 253.873 | 55139.4126388889 | 55141.3127777778 | 504085010 | 77349 | 75000 | 77461 | 77349 | 0 | 77461 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 62100.2 | 62100.2 | 164155.8 | 0 | PROCESSED | 57549.1334837963 | 55518 | 55152.1455671296 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041321 | Fast winds from massive stars create large cavities in the surrounding interstellar medium filled with hot gas, known as Wind-Blown Bubbles (WBB). We propose to obtain XIS imaging spectroscopy of the prototype WBB NGC 6888. Thanks to the XIS excellent sensitivity and energy resolution in the soft X-ray band, we will: (i) obtain a high quality CCD spectrum which can be used to constrain the temperature of the hot plasma and the efficiency of thermal conduction across the bubble wall, (ii) determine the spatial distribution and properties of X-ray emitting plasma, (iii) therefore, test and refine shock physics models of bubbles by a direct confrontation of their results with observations. | GALACTIC DIFFUSE EMISSION | 5 | A | ZHEKOV | SVETOZAR | NULL | NULL | USA | 4 | AO4 | X-RAYS FROM THE PROTOTYPE WIND-BLOWN BUBBLE NGC 6888 | XIS | Y |
| MRK 421 OFFSET | 166.8026 | 37.7335 | 180.50489089 | 65.69633084 | 129.0398 | 55144.0655092593 | 55145.8091087963 | 504086010 | 75259.5 | 75000 | 75267.5 | 75259.5 | 0 | 75267.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51940 | 51940 | 150628.8 | 2 | PROCESSED | 57549.2648148148 | 55542 | 55176.2291319444 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041324 | The OVII, OVIII, and NeIX absorption lines at z~0 have been discovered in the Chandra/XMM spectra of several bright AGNs, but the location of these absorptions has been debated since their discoveries. Here we request Suzaku observations of the soft X-ray background emission in the vicinity of Mrk 421, to conduct a joint analysis of the emission data with the extensive Chandra absorption data. This analysis will naturally yield an effective length of the absorbing/emitting gas. We have performed pilot studies and obtained a scale length of several kpc for the hot absorbing/emitting gas toward LMC X-3 and Mrk 421. The requested Suzaku observations are particular important to check these results and to further test the models we have developed in our study. | GALACTIC DIFFUSE EMISSION | 5 | B | YAO | YANGSEN | NULL | NULL | USA | 4 | AO4 | A JOINT X-RAY ABSORPTION AND EMISSION STUDY OF THE HOT GAS TOWARD MRK 421 | XIS | Y |
| MRK 421 OFFSET | 165.3836 | 38.6302 | 179.31913311 | 64.35556561 | 121.9647 | 55146.4480092593 | 55148.3176388889 | 504087010 | 86014.4 | 75000 | 86014.4 | 86014.4 | 0 | 86014.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 64880.4 | 64880.4 | 161519.9 | 3 | PROCESSED | 57549.3389583333 | 55531 | 55160.2701041667 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041324 | The OVII, OVIII, and NeIX absorption lines at z~0 have been discovered in the Chandra/XMM spectra of several bright AGNs, but the location of these absorptions has been debated since their discoveries. Here we request Suzaku observations of the soft X-ray background emission in the vicinity of Mrk 421, to conduct a joint analysis of the emission data with the extensive Chandra absorption data. This analysis will naturally yield an effective length of the absorbing/emitting gas. We have performed pilot studies and obtained a scale length of several kpc for the hot absorbing/emitting gas toward LMC X-3 and Mrk 421. The requested Suzaku observations are particular important to check these results and to further test the models we have developed in our study. | GALACTIC DIFFUSE EMISSION | 5 | B | YAO | YANGSEN | NULL | NULL | USA | 4 | AO4 | A JOINT X-RAY ABSORPTION AND EMISSION STUDY OF THE HOT GAS TOWARD MRK 421 | XIS | Y |
| GALACTIC_BULGE1 | 267.2201 | -29.3677 | 359.99969448 | -0.83243485 | 274.7 | 55118.4798148148 | 55119.6453587963 | 504088010 | 47230 | 50000 | 47230 | 47230 | 0 | 47230 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32613.9 | 32613.9 | 100700 | 2 | PROCESSED | 57548.8825231482 | 54922 | 55134.0688425926 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 046001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 4 | AO4 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y |
| GALACTIC_BULGE2 | 267.5552 | -29.599 | 359.95115697 | -1.20153587 | 277.9812 | 55113.1708217593 | 55114.5903472222 | 504089010 | 55260.1 | 50000 | 55267.1 | 55260.1 | 0 | 55273.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40226 | 40226 | 122633.8 | 1 | PROCESSED | 57548.8316666667 | 54922 | 55131.3309953704 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 046001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 4 | AO4 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y |
| GALACTIC_BULGE7 | 266.6764 | -30.8281 | 358.50617228 | -1.18471698 | 274.4326 | 55117.1787037037 | 55118.4785416667 | 504090010 | 41260.7 | 50000 | 41260.7 | 52903.3 | 0 | 52903.3 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 34964 | 34964 | 112293.8 | 2 | PROCESSED | 57548.8825694444 | 54922 | 55133.2421643518 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 046001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 4 | AO4 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y |
| GALACTIC_BULGE8 | 267.0897 | -31.0498 | 358.49976827 | -1.60277837 | 260.4349 | 55088.8177777778 | 55090.3043287037 | 504091010 | 51331.6 | 50000 | 51331.6 | 51339.2 | 0 | 51331.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47751.4 | 47751.4 | 128425.8 | 2 | PROCESSED | 57548.5976041667 | 54922 | 55109.4226736111 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 046001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 4 | AO4 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y |
| GALACTIC_BULGE9 | 267.6768 | -31.2805 | 358.55970985 | -2.15232996 | 265.3076 | 55090.3066550926 | 55091.5758564815 | 504092010 | 50919.9 | 50000 | 50943.9 | 50935.9 | 0 | 50919.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45574.4 | 45574.4 | 109645.9 | 1 | PROCESSED | 57548.6135069444 | 54922 | 55109.4315740741 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 046001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 4 | AO4 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y |
| GALACTIC_BULGE10 | 268.297 | -31.6627 | 358.49964198 | -2.80216044 | 277.1297 | 55091.579525463 | 55093.1508564815 | 504093010 | 53241.6 | 50000 | 53249.5 | 53241.6 | 0 | 53257.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46907.2 | 46907.2 | 135734 | 1 | PROCESSED | 57548.6254513889 | 54922 | 55110.3193865741 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 046001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 4 | AO4 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y |
| GALACTIC_BULGE11 | 269.3164 | -32.1646 | 358.50010375 | -3.80248777 | 271.7893 | 55093.1531365741 | 55095.6064699074 | 504094010 | 93140.3 | 50000 | 93140.3 | 93140.3 | 0 | 93140.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 82954.3 | 82954.3 | 211953.8 | 1 | PROCESSED | 57548.674224537 | 54922 | 55110.4114236111 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 046001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 4 | AO4 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y |
| GALACTIC_BULGE12 | 270.5539 | -32.7559 | 358.50046577 | -5.00243267 | 271.4834 | 55119.6475462963 | 55120.7502199074 | 504095010 | 48262.2 | 50000 | 48262.2 | 48262.2 | 0 | 48262.2 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 38358 | 38358 | 95261.9 | 1 | PROCESSED | 57548.9040856482 | 54922 | 55133.2742824074 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 046001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 4 | AO4 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y |
| G346.6-0.2 | 257.5822 | -40.1827 | 346.62898747 | -0.22219097 | 278.7363 | 55111.704525463 | 55113.1668287037 | 504096010 | 56754.3 | 50000 | 56754.3 | 56762.3 | 0 | 56770.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42412.1 | 42412.1 | 126323.9 | 0 | PROCESSED | 57548.806724537 | 54922 | 55127.3766898148 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 046001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 4 | AO4 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y |
| G348.5+0.1 | 258.6301 | -38.5295 | 348.44223752 | 0.09652262 | 91.401 | 55247.6321180556 | 55248.7592476852 | 504097010 | 53810.6 | 50000 | 53810.6 | 53810.6 | 0 | 53810.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46392.9 | 46392.9 | 97359.8 | 1 | PROCESSED | 57550.6723842593 | 54922 | 55257.0343287037 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 046001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 4 | AO4 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y |
| G355.6-0.0 | 263.7798 | -32.6083 | 355.69106204 | -0.03789327 | 90.0013 | 55246.5249074074 | 55247.6293287037 | 504098010 | 52504.4 | 50000 | 52527.5 | 52520.4 | 0 | 52504.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43734.6 | 43734.6 | 95411.8 | 0 | PROCESSED | 57550.6569560185 | 54922 | 55257.1119444444 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 046001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 4 | AO4 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y |
| G25.5+0.0 | 279.4506 | -6.6057 | 25.50196825 | 0.00652115 | 74.2354 | 54927.1234490741 | 54928.7446064815 | 504099010 | 52737.5 | 50000 | 52737.5 | 52737.5 | 0 | 52737.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44570.3 | 44570.3 | 140042 | 3 | PROCESSED | 57546.0819675926 | 54922 | 54949.4845023148 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 046001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 4 | AO4 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y |
| KEPLER_BG_GE | 263.5353 | -20.2634 | 5.99742641 | 6.79731937 | 272.7609 | 55087.1593171296 | 55088.3606365741 | 504101010 | 46989.5 | 60000 | 46989.5 | 46989.5 | 0 | 46989.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40899.3 | 40899.3 | 103786 | 0 | PROCESSED | 57548.5758564815 | 54922 | 55099.2516782407 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 046004 | The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors. | GALACTIC DIFFUSE EMISSION | 5 | A | PARK | SANGWOOK | NULL | NULL | USA | 4 | AO4 | A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR | XIS | Y |
| KEPLER_BG_GE | 263.5357 | -20.2632 | 5.99779838 | 6.79710869 | 273.0028 | 55072.0030208333 | 55072.5002662037 | 504101020 | 24722.7 | 60000 | 24746.7 | 24738.7 | 0 | 24722.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19252.8 | 19252.8 | 42955.9 | 0 | PROCESSED | 57548.3891550926 | 54922 | 55109.4155324074 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 046004 | The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors. | GALACTIC DIFFUSE EMISSION | 5 | A | PARK | SANGWOOK | NULL | NULL | USA | 4 | AO4 | A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR | XIS | Y |
| KEPLER_BG_GW | 261.806 | -22.7684 | 2.99933771 | 6.7960859 | 273.0885 | 55109.2984143518 | 55111.1057175926 | 504102010 | 65294.9 | 60000 | 65302.9 | 65294.9 | 0 | 65302.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 50782.1 | 50782.1 | 156128 | 1 | PROCESSED | 57548.8038425926 | 54922 | 55125.6963888889 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 046004 | The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors. | GALACTIC DIFFUSE EMISSION | 5 | A | PARK | SANGWOOK | NULL | NULL | USA | 4 | AO4 | A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR | XIS | Y |
| KEPLER_BG_GN | 261.9141 | -20.2308 | 5.199252 | 8.09662946 | 270.3619 | 55105.4689699074 | 55107.4279976852 | 504103010 | 68604.3 | 60000 | 68604.3 | 68604.3 | 0 | 68612.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 55801.4 | 55801.4 | 169227.9 | 1 | PROCESSED | 57548.7547800926 | 54922 | 55125.6331828704 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 046004 | The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors. | GALACTIC DIFFUSE EMISSION | 5 | A | PARK | SANGWOOK | NULL | NULL | USA | 4 | AO4 | A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR | XIS | Y |
| KEPLER_BG_GS | 263.1005 | -22.949 | 3.49961978 | 5.69692486 | 272.6396 | 55107.43 | 55109.2973842593 | 504104010 | 67250.8 | 60000 | 67250.8 | 67280.5 | 0 | 67274.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 53158.5 | 53158.5 | 161329.8 | 1 | PROCESSED | 57548.7538425926 | 54922 | 55125.3521180556 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 046004 | The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors. | GALACTIC DIFFUSE EMISSION | 5 | A | PARK | SANGWOOK | NULL | NULL | USA | 4 | AO4 | A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR | XIS | Y |
| IC443 NORTHWEST | 93.9975 | 22.7552 | 188.75644855 | 2.86235674 | 91.4819 | 55456.3191435185 | 55458.2829050926 | 505001010 | 83191.7 | 80000 | 83191.7 | 83191.7 | 0 | 83191.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 69678.6 | 69678.6 | 169645.7 | 2 | PROCESSED | 57553.4791087963 | 55836 | 55469.4041087963 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050001 | Suzaku discovered the radiative recombination continua (RRC) of Si and S from the supernova remnant IC443. This new phenomenon (the RRC) would be due to either pre-ionization by X-ray flash of gamma-ray burst, or adiabatic cooling in a rarefied ambient medium, or yet-unknown process. In any case, the RRC have essential and new clues for the mechanisms, evolution and/or even the cosmic-ray acceleration of IC443. Spectra of the rim regions provide key information for the RRC origin. We thus propose the East and West periphery of IC443 for total 200 ksec. | GALACTIC DIFFUSE EMISSION | 5 | C | OZAWA | MIDORI | NULL | NULL | JAP | 5 | AO5 | EXPLORING THE ORIGIN OF THE RADIATIVE RECOMBINATION CONTINUUM OF IC443 | XIS | Y |
| W44 | 284.0351 | 1.3886 | 34.70383121 | -0.41279271 | 90.6817 | 55296.8229513889 | 55298.1591898148 | 505004010 | 61143.3 | 60000 | 61151.3 | 61143.3 | 0 | 61151.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 53712.9 | 53712.9 | 115399.9 | 2 | PROCESSED | 57551.2065625 | 55287 | 55313.4281597222 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050002 | We found the strong Radiative Recombination Continuum (RRC) from The Mixed Morphology SNRs, IC443, W49 and G359.1-0.5. In the analogy of the past discovery of Non-Equilibrium Ionization (NEI) in the SNR plasmas, the discovery of the RRC will provide new insight on the explosion mechanisms and evolution of SNRs. Since the SNR-RRC is diffuse X-ray structure, systematic study of RRC can be a legacy of Suzaku as well as the key science for the Astro-H project. The next process to develop the newly born RRC science is to search for what underlying physics does determine the presence or absence of the RRC structure. Thus we propose to observe several non-shell-like thermal SNRs. The results can be the data-base for future studies. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 5 | AO5 | RESEARCH FOR NEW ASPECTS OF THE EXPLOSION MECHANISMS AND EVOLUTION OF SNRS WITH THE RADIATIVE RECOMBINATION CONTINUUM | XIS | Y |
| W28_CENTER | 270.074 | -23.3664 | 6.46943001 | -0.00256773 | 84.9544 | 55289.3078935185 | 55290.9918287037 | 505005010 | 73003.6 | 70000 | 73043.7 | 73003.6 | 0 | 73043.6 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 57298.1 | 57298.1 | 145451.9 | 2 | PROCESSED | 57551.1131944444 | 55287 | 55322.3694675926 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050002 | We found the strong Radiative Recombination Continuum (RRC) from The Mixed Morphology SNRs, IC443, W49 and G359.1-0.5. In the analogy of the past discovery of Non-Equilibrium Ionization (NEI) in the SNR plasmas, the discovery of the RRC will provide new insight on the explosion mechanisms and evolution of SNRs. Since the SNR-RRC is diffuse X-ray structure, systematic study of RRC can be a legacy of Suzaku as well as the key science for the Astro-H project. The next process to develop the newly born RRC science is to search for what underlying physics does determine the presence or absence of the RRC structure. Thus we propose to observe several non-shell-like thermal SNRs. The results can be the data-base for future studies. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 5 | AO5 | RESEARCH FOR NEW ASPECTS OF THE EXPLOSION MECHANISMS AND EVOLUTION OF SNRS WITH THE RADIATIVE RECOMBINATION CONTINUUM | XIS | Y |
| W28_EASTSHELL | 270.3727 | -23.2858 | 6.67541903 | -0.20080463 | 88.0003 | 55617.4542939815 | 55620.1723032407 | 505006010 | 99981.6 | 100000 | 99981.6 | 99981.6 | 0 | 99981.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 83677.2 | 83677.2 | 234815.7 | 3 | PROCESSED | 57601.1152430556 | 55287 | 55642.1946643518 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050002 | We found the strong Radiative Recombination Continuum (RRC) from The Mixed Morphology SNRs, IC443, W49 and G359.1-0.5. In the analogy of the past discovery of Non-Equilibrium Ionization (NEI) in the SNR plasmas, the discovery of the RRC will provide new insight on the explosion mechanisms and evolution of SNRs. Since the SNR-RRC is diffuse X-ray structure, systematic study of RRC can be a legacy of Suzaku as well as the key science for the Astro-H project. The next process to develop the newly born RRC science is to search for what underlying physics does determine the presence or absence of the RRC structure. Thus we propose to observe several non-shell-like thermal SNRs. The results can be the data-base for future studies. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 5 | AO5 | RESEARCH FOR NEW ASPECTS OF THE EXPLOSION MECHANISMS AND EVOLUTION OF SNRS WITH THE RADIATIVE RECOMBINATION CONTINUUM | XIS | Y |
| 3C_391 | 282.3812 | -0.9417 | 31.87573789 | -0.00377867 | 261.9952 | 55491.0759722222 | 55493.8224537037 | 505007010 | 99388.7 | 100000 | 99460.7 | 99388.7 | 0 | 99468.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 89374 | 89374 | 237277.9 | 2 | PROCESSED | 57553.8698032407 | 55287 | 55502.3356597222 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050002 | We found the strong Radiative Recombination Continuum (RRC) from The Mixed Morphology SNRs, IC443, W49 and G359.1-0.5. In the analogy of the past discovery of Non-Equilibrium Ionization (NEI) in the SNR plasmas, the discovery of the RRC will provide new insight on the explosion mechanisms and evolution of SNRs. Since the SNR-RRC is diffuse X-ray structure, systematic study of RRC can be a legacy of Suzaku as well as the key science for the Astro-H project. The next process to develop the newly born RRC science is to search for what underlying physics does determine the presence or absence of the RRC structure. Thus we propose to observe several non-shell-like thermal SNRs. The results can be the data-base for future studies. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 5 | AO5 | RESEARCH FOR NEW ASPECTS OF THE EXPLOSION MECHANISMS AND EVOLUTION OF SNRS WITH THE RADIATIVE RECOMBINATION CONTINUUM | XIS | Y |
| 3C_397 | 286.9038 | 7.1223 | 41.11064468 | -0.32936267 | 256.5108 | 55493.8258449074 | 55495.8022337963 | 505008010 | 69326.6 | 70000 | 69326.6 | 69326.6 | 0 | 69326.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 62165.3 | 62165.3 | 170731.9 | 0 | PROCESSED | 57553.8922800926 | 55287 | 55505.3393981482 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050002 | We found the strong Radiative Recombination Continuum (RRC) from The Mixed Morphology SNRs, IC443, W49 and G359.1-0.5. In the analogy of the past discovery of Non-Equilibrium Ionization (NEI) in the SNR plasmas, the discovery of the RRC will provide new insight on the explosion mechanisms and evolution of SNRs. Since the SNR-RRC is diffuse X-ray structure, systematic study of RRC can be a legacy of Suzaku as well as the key science for the Astro-H project. The next process to develop the newly born RRC science is to search for what underlying physics does determine the presence or absence of the RRC structure. Thus we propose to observe several non-shell-like thermal SNRs. The results can be the data-base for future studies. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 5 | AO5 | RESEARCH FOR NEW ASPECTS OF THE EXPLOSION MECHANISMS AND EVOLUTION OF SNRS WITH THE RADIATIVE RECOMBINATION CONTINUUM | XIS | Y |
| CYGNUS LOOP 1 | 313.2462 | 32.1399 | 75.40840203 | -7.96786776 | 81.7816 | 55300.7096759259 | 55301.0293402778 | 505009010 | 15999.2 | 13000 | 15999.2 | 15999.2 | 0 | 15999.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12242 | 12242 | 27612 | 0 | PROCESSED | 57551.2105787037 | 55287 | 55362.3098726852 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050005 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS | XIS | Y |
| CYGNUS LOOP 2 | 312.7259 | 32.1633 | 75.14683323 | -7.61088939 | 81.0273 | 55301.0300925926 | 55301.2897569444 | 505010010 | 12932 | 10000 | 12932 | 12932 | 0 | 12932 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11924 | 11924 | 22431.9 | 0 | PROCESSED | 57551.2143402778 | 55287 | 55362.2959375 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050005 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS | XIS | Y |
| CYGNUS LOOP 3 | 312.9529 | 31.9301 | 75.08571271 | -7.90709143 | 81.0389 | 55301.2902777778 | 55301.6209953704 | 505011010 | 13444.8 | 12000 | 13444.8 | 13444.8 | 0 | 13444.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10427 | 10427 | 28571.9 | 0 | PROCESSED | 57551.2233333333 | 55287 | 55362.3557060185 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050005 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS | XIS | Y |
| CYGNUS LOOP 4 | 312.482 | 31.9468 | 74.84594636 | -7.58533627 | 81.0154 | 55301.6216087963 | 55301.8912037037 | 505012010 | 12453.5 | 12000 | 12453.5 | 12453.5 | 0 | 12453.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12182 | 12182 | 23280.1 | 1 | PROCESSED | 57551.2226736111 | 55287 | 55362.3160763889 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050005 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS | XIS | Y |
| CYGNUS LOOP 5 | 312.0188 | 31.9594 | 74.60885135 | -7.27014396 | 81.8368 | 55305.8645833333 | 55306.4578125 | 505013010 | 26845.2 | 26000 | 26845.2 | 26845.2 | 0 | 26845.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 21277 | 21277 | 51232 | 2 | PROCESSED | 57551.2602083333 | 55287 | 55364.2036458333 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050005 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS | XIS | Y |
| CYGNUS LOOP 6 | 314.1656 | 31.2305 | 75.19999907 | -9.14964477 | 81.8988 | 55301.8924189815 | 55302.1398148148 | 505014010 | 12462.3 | 10000 | 12478.3 | 12462.3 | 0 | 12478.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12068.3 | 12068.3 | 21359.9 | 0 | PROCESSED | 57551.2257060185 | 55287 | 55362.3410532407 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050005 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS | XIS | Y |
| CYGNUS LOOP 7 | 313.929 | 31.0152 | 74.90122685 | -9.13052292 | 81.814 | 55306.459212963 | 55306.7974189815 | 505015010 | 13591.8 | 12000 | 13591.8 | 13599.8 | 0 | 13599.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12682 | 12682 | 29195.9 | 0 | PROCESSED | 57551.269212963 | 55287 | 55393.2216203704 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050005 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS | XIS | Y |
| CYGNUS LOOP 8 | 313.6776 | 30.8178 | 74.60811536 | -9.08900254 | 81.5524 | 55306.7979398148 | 55307.2786689815 | 505016010 | 23553.4 | 21000 | 23561.4 | 23553.4 | 0 | 23569.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 20198.9 | 20198.9 | 41527.9 | 0 | PROCESSED | 57551.2800462963 | 55287 | 55364.2401967593 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050005 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS | XIS | Y |
| CYGNUS LOOP 9 | 312.876 | 30.2229 | 73.70000859 | -8.9268412 | 80.5836 | 55307.2796064815 | 55308.0106597222 | 505017010 | 29996.8 | 29000 | 29996.8 | 29996.8 | 0 | 29996.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27628.1 | 27628.1 | 63149.9 | 1 | PROCESSED | 57551.2933217593 | 55287 | 55364.2675347222 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050005 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS | XIS | Y |
| CYGNUS LOOP 10 | 314.1171 | 30.7461 | 74.79486269 | -9.42625359 | 82.0017 | 55328.2812152778 | 55328.6981134259 | 505018010 | 16268 | 16000 | 16276 | 16276 | 0 | 16268 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12655.1 | 12655.1 | 36012 | 0 | PROCESSED | 57551.4785069444 | 55287 | 55393.3335069445 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050005 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS | XIS | Y |
| CYGNUS LOOP 11 | 313.8693 | 30.5587 | 74.51088669 | -9.3807208 | 82.002 | 55328.698587963 | 55329.1251736111 | 505019010 | 18897.6 | 18000 | 18905.6 | 18897.6 | 0 | 18913.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14904.8 | 14904.8 | 36853.9 | 1 | PROCESSED | 57551.490150463 | 55287 | 55393.3619791667 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050005 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS | XIS | Y |
| CYGNUS LOOP 12 | 313.6077 | 30.3526 | 74.20451075 | -9.33661335 | 82.0022 | 55329.1256944444 | 55329.8391666667 | 505020010 | 27842.7 | 28000 | 27850.7 | 27850.7 | 0 | 27842.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21052.2 | 21052.2 | 61640 | 0 | PROCESSED | 57551.5093055556 | 55287 | 55393.4203009259 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050005 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS | XIS | Y |
| CYGNUS LOOP 13 | 313.3172 | 30.1574 | 73.89066537 | -9.26489611 | 82.0018 | 55329.8397337963 | 55330.4925694444 | 505021010 | 21565 | 21000 | 21565 | 21597 | 0 | 21565 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18120 | 18120 | 56399.9 | 1 | PROCESSED | 57551.5081597222 | 55287 | 55393.3656712963 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050005 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS | XIS | Y |
| CYGNUS LOOP 14 | 313.0411 | 29.9656 | 73.58742167 | -9.19932348 | 67.2195 | 55334.4727893518 | 55335.1146759259 | 505022010 | 29251.2 | 29000 | 29251.2 | 29251.2 | 0 | 29251.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 24783.2 | 24783.2 | 55451.9 | 0 | PROCESSED | 57551.5599305556 | 55287 | 55348.0488888889 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050005 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS | XIS | Y |
| CYGNUS LOOP 15 | 313.2124 | 29.6854 | 73.46064198 | -9.49078141 | 50.2914 | 55343.3019791667 | 55343.6994675926 | 505023010 | 19295.3 | 19000 | 19295.3 | 19295.3 | 0 | 19295.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16514 | 16514 | 34320 | 1 | PROCESSED | 57551.5915972222 | 55287 | 55355.1545833333 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050005 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS | XIS | Y |
| CYGNUS LOOP 16 | 312.8966 | 29.5255 | 73.15999246 | -9.37678246 | 49.3574 | 55343.7003125 | 55344.4932407407 | 505024010 | 34833.8 | 34000 | 34833.8 | 34833.8 | 0 | 34833.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32418.2 | 32418.2 | 68507.9 | 1 | PROCESSED | 57551.6200231482 | 55287 | 55355.2000115741 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050005 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell shows relatively low temperature with low metal abundance and high non-uniformity in intensity. The interior shows high temperature with high abundance. It also shows the abundance non-uniformity. The inner plasma is the fossil of the progenitor star. The abundance non-uniformity indicates the asymmetric explosion. We propose to observe the rest of the Cygnus Loop for 310ks with three objectives that are tightly correlated to each other. The first is to establish the metal structure that is the key to study the asymmetric explosion. The second is to measure the amount of metal that can determine the progenitor mass. The last one is to search for a compact object such as a neutron star. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP WITH SUZAKU XIS | XIS | Y |
| G22.0+0.0 | 277.823 | -9.7151 | 22.00005623 | 0.00370699 | 89.3658 | 55302.6023842593 | 55303.7272222222 | 505025010 | 50529.4 | 50000 | 50529.4 | 50529.4 | 0 | 50529.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44620.8 | 44620.8 | 97159.8 | 0 | PROCESSED | 57551.270775463 | 55737 | 55375.7533101852 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050009 | ASCA galactic plane survey discovered many extended X-ray sources on the galactic plane. They have hard X-ray spectra with significant low energy absorption. However, due to poor photon statistics, we could not conclude whether they are thermal emission or non-thermal emission. We propose observations of the extended X-ray sources with Suzaku. Precise measurements of the X-ray structure and spectrum with the Suzaku XIS will reveal their nature. | GALACTIC DIFFUSE EMISSION | 5 | B | YAMAUCHI | SHIGEO | NULL | NULL | JAP | 5 | AO5 | SUZAKU OBSERVATIONS OF EXTENDED SOURCES DISCOVERED WITH ASCA | XIS | Y |
| G23.5+0.1 | 278.489 | -8.375 | 23.49243074 | 0.03918587 | 261.7121 | 55489.5657291667 | 55491.0730439815 | 505026010 | 48976.1 | 50000 | 48976.1 | 48976.1 | 0 | 48976.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43788.4 | 43788.4 | 130191.9 | 0 | PROCESSED | 57553.8193981482 | 55868 | 55502.1887962963 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050009 | ASCA galactic plane survey discovered many extended X-ray sources on the galactic plane. They have hard X-ray spectra with significant low energy absorption. However, due to poor photon statistics, we could not conclude whether they are thermal emission or non-thermal emission. We propose observations of the extended X-ray sources with Suzaku. Precise measurements of the X-ray structure and spectrum with the Suzaku XIS will reveal their nature. | GALACTIC DIFFUSE EMISSION | 5 | B | YAMAUCHI | SHIGEO | NULL | NULL | JAP | 5 | AO5 | SUZAKU OBSERVATIONS OF EXTENDED SOURCES DISCOVERED WITH ASCA | XIS | Y |
| G37.0-0.1 | 284.8009 | 3.5813 | 37.00394757 | -0.09218404 | 68.6266 | 55303.7327893518 | 55304.8814583333 | 505027010 | 50969.4 | 50000 | 50977.4 | 50977.4 | 0 | 50969.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45336.1 | 45336.1 | 99230 | 1 | PROCESSED | 57551.2689699074 | 55693 | 55326.2903125 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050009 | ASCA galactic plane survey discovered many extended X-ray sources on the galactic plane. They have hard X-ray spectra with significant low energy absorption. However, due to poor photon statistics, we could not conclude whether they are thermal emission or non-thermal emission. We propose observations of the extended X-ray sources with Suzaku. Precise measurements of the X-ray structure and spectrum with the Suzaku XIS will reveal their nature. | GALACTIC DIFFUSE EMISSION | 5 | B | YAMAUCHI | SHIGEO | NULL | NULL | JAP | 5 | AO5 | SUZAKU OBSERVATIONS OF EXTENDED SOURCES DISCOVERED WITH ASCA | XIS | Y |
| FVW319.8+0.3 | 225.913 | -58.2332 | 319.61922846 | 0.28881447 | 278.3756 | 55413.1563888889 | 55413.9307291667 | 505029010 | 51384 | 50000 | 51400 | 51384 | 0 | 51400 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45416 | 45416 | 66893.9 | 2 | PROCESSED | 57552.8424421296 | 55793 | 55427.1529976852 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050010 | Forbidden-velocity wings (FVWs) are unknown HI clouds with high velocity dispersion. They could be old supernova remnants or star-forming bubbles, although the origin is unknown. Recently, TeV gamma-rays have been detected from one of the FVWs, FVW319.8+0.3, implying that it is a cosmic-ray accelerator. We will investigate this FVW with low-background observations of Suzaku, in order to search for thermal emission from the undiscovered supernova remnant. It is not only the first discovery of X-rays from FVWs, but also the first clue of the cosmic-ray acceleration in FVWs. Even if we could detect nothing, we can conclude that this source is a kind of gdark particle accelerators h with the proposed exposure. | GALACTIC DIFFUSE EMISSION | 5 | A | BAMBA | AYA | NULL | NULL | JAP | 5 | AO5 | SEARCHING FOR COSMIC ACCELERATION IN A FORBIDDEN-VELOCITY WING: A NEW OLD SUPERNOVA REMNANT ? | XIS | Y |
| FVW319.8+0.3_BGD | 225.4141 | -58.3766 | 319.32044374 | 0.28957352 | 278.3765 | 55413.9313888889 | 55414.6724768518 | 505030010 | 51626.2 | 50000 | 51626.2 | 51663.6 | 0 | 51647.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40050.3 | 40050.3 | 64017.9 | 1 | PROCESSED | 57552.8534837963 | 55793 | 55427.2012152778 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050010 | Forbidden-velocity wings (FVWs) are unknown HI clouds with high velocity dispersion. They could be old supernova remnants or star-forming bubbles, although the origin is unknown. Recently, TeV gamma-rays have been detected from one of the FVWs, FVW319.8+0.3, implying that it is a cosmic-ray accelerator. We will investigate this FVW with low-background observations of Suzaku, in order to search for thermal emission from the undiscovered supernova remnant. It is not only the first discovery of X-rays from FVWs, but also the first clue of the cosmic-ray acceleration in FVWs. Even if we could detect nothing, we can conclude that this source is a kind of gdark particle accelerators h with the proposed exposure. | GALACTIC DIFFUSE EMISSION | 5 | A | BAMBA | AYA | NULL | NULL | JAP | 5 | AO5 | SEARCHING FOR COSMIC ACCELERATION IN A FORBIDDEN-VELOCITY WING: A NEW OLD SUPERNOVA REMNANT ? | XIS | Y |
| SGR_C | 266.2461 | -29.3903 | 359.54016882 | -0.1184914 | 267.0744 | 55464.5256481482 | 55466.608599537 | 505031010 | 99916 | 100000 | 99956.1 | 99916 | 0 | 99956 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 89071.2 | 89071.2 | 179949.9 | 2 | PROCESSED | 57553.5757175926 | 55853 | 55484.3402777778 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050018 | The Sagittarius C Complex (Sgr C) @is composed of many giant molecular clouds (MCs) in two distinct velocity zones, indicating two separate line-of-sight positions of the MCs. Past X-ray flares of Sgr A* likely produced the FeI 6.4 keV emission in the MCs (XRN: X-ray Reflection Nebulae). In Sgr C, the XRN have been solely found in one of the velocity zones. We hence propose to find new XRN in the other velocity zone, which is possibly located at the different distance from the known XRN. With the Suzaku observation, we will determine the 3-dimensional positions of the XRN. Since the presence (or absence) of the XRN largely depends on the epoch of the Sgr A* flares and the 3-dimensional positions of the MCs, Sgr C is a "Rosetta Stone" of the origin and production of the XRN. | GALACTIC DIFFUSE EMISSION | 5 | A | NOBUKAWA | MASAYOSHI | NULL | NULL | JAP | 5 | AO5 | THE SAGITTARIUS C COMPLEX A ROSETTA STONE OF THE PAST ACTIVITY OF SAGITTARIUS A* | XIS | Y |
| DEM L 86 | 77.4674 | -68.8946 | 279.75652902 | -34.25087364 | 194.4731 | 55552.1478703704 | 55552.9495601852 | 505041010 | 51468.1 | 50000 | 51499.7 | 51499.7 | 0 | 51468.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44258.9 | 44258.9 | 69257.9 | 0 | PROCESSED | 57554.4839236111 | 55973 | 55607.0926851852 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050061 | Some of the Supper bubbles (SBs), the large hot cavities created by the combined actions of strong stellar winds and supernova explosions of massive stars, have proved to be the strong emitters of non-thermal X-rays. By observing two brightest SBs (DEM L 86 and DEM L 199) in the LMC, we investigate the universality of particle acceleration in SBs, and make the conclusion if SBs are the primary acceleration cites of the galactic cosmic rays. We also investigate the energy crisis problem in SBs, that is, there is a large discrepancy between energy income (SN and stellar wind) and its outlays (thermal/kinetic energy of the shell). By estimating the thermal energies of the SB shells precisely, we measure the amount of missing energy and the conversion efficiency to the non-thermal particles. | GALACTIC DIFFUSE EMISSION | 5 | C | NAKAJIMA | HIROSHI | NULL | NULL | JAP | 5 | AO5 | UNIVERSALITY OF PARTICLE ACCELERATION IN SUPERBUBBLES AND SOLVING THEIR ENERGY CRISIS | XIS | Y |
| DEM L 199 | 81.6473 | -68.8371 | 279.33316137 | -32.78488249 | 187.7916 | 55551.3246759259 | 55552.146099537 | 505042010 | 51743.4 | 50000 | 51756.4 | 51743.4 | 0 | 51756.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48207.9 | 48207.9 | 70965.9 | 0 | PROCESSED | 57554.4832523148 | 55961 | 55593.2050231482 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050061 | Some of the Supper bubbles (SBs), the large hot cavities created by the combined actions of strong stellar winds and supernova explosions of massive stars, have proved to be the strong emitters of non-thermal X-rays. By observing two brightest SBs (DEM L 86 and DEM L 199) in the LMC, we investigate the universality of particle acceleration in SBs, and make the conclusion if SBs are the primary acceleration cites of the galactic cosmic rays. We also investigate the energy crisis problem in SBs, that is, there is a large discrepancy between energy income (SN and stellar wind) and its outlays (thermal/kinetic energy of the shell). By estimating the thermal energies of the SB shells precisely, we measure the amount of missing energy and the conversion efficiency to the non-thermal particles. | GALACTIC DIFFUSE EMISSION | 5 | C | NAKAJIMA | HIROSHI | NULL | NULL | JAP | 5 | AO5 | UNIVERSALITY OF PARTICLE ACCELERATION IN SUPERBUBBLES AND SOLVING THEIR ENERGY CRISIS | XIS | Y |
| L139_B-32 | 28.093 | 28.6837 | 138.75887563 | -32.3084393 | 253.9538 | 55569.4091319444 | 55571.3188541667 | 505044010 | 84004.1 | 80000 | 84004.1 | 84004.1 | 0 | 84004.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 79037.7 | 79037.7 | 164983.9 | 0 | PROCESSED | 57600.6057175926 | 55962 | 55595.2037615741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050064 | Suzaku measurements of the large scale variation of the Halo emission surrounding our Galaxy are proposed. To minimize the local emission and absorption structure, we selected three pointings toward the anti-center region (l=140) of the Galactic latitude between-20 and -40. | GALACTIC DIFFUSE EMISSION | 5 | C | YAMASAKI | NORIKO | NULL | NULL | JAP | 5 | AO5 | STRUCTURE OF THE GALACTIC HALO EMISSION TOWARD THE ANTI-CENTER REGION | XIS | Y |
| WESTERLUND1_1 | 251.8398 | -46.6023 | 339.00946678 | -0.92860911 | 283.3468 | 55449.7733217593 | 55451.2015740741 | 505049010 | 51932 | 50000 | 51932 | 51932 | 0 | 51932 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44843.7 | 44843.7 | 123386.1 | 1 | PROCESSED | 57553.3910532407 | 55829 | 55461.3235069444 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050078 | TeV emission surrounding Westerlund 1, the only super star cluster in our Galaxy, has been discovered. Molecular clouds associated with the TeV emission have been also discovered. This coincidence between the TeV emission and the molecular clouds suggests the proton origin of the TeV emission. However, the TeV emission should include the contribution from high-energy electrons. We observe Westerlund 1 with Suzaku to clarify the electron distribution and to examine the proton acceleration in the star cluster. | GALACTIC DIFFUSE EMISSION | 5 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 5 | AO5 | IS THE SUPER STAR CLUSTER WESTERLUND 1 ACCERELATING PROTONS? | XIS | Y |
| WESTERLUND1_2 | 252.808 | -46.1402 | 339.79276992 | -1.14410237 | 285.6981 | 55451.2033912037 | 55452.6077777778 | 505050010 | 52654.1 | 50000 | 52654.1 | 52654.1 | 0 | 52654.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42753.6 | 42753.6 | 121309.9 | 0 | PROCESSED | 57553.3934375 | 55829 | 55463.2091435185 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050078 | TeV emission surrounding Westerlund 1, the only super star cluster in our Galaxy, has been discovered. Molecular clouds associated with the TeV emission have been also discovered. This coincidence between the TeV emission and the molecular clouds suggests the proton origin of the TeV emission. However, the TeV emission should include the contribution from high-energy electrons. We observe Westerlund 1 with Suzaku to clarify the electron distribution and to examine the proton acceleration in the star cluster. | GALACTIC DIFFUSE EMISSION | 5 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 5 | AO5 | IS THE SUPER STAR CLUSTER WESTERLUND 1 ACCERELATING PROTONS? | XIS | Y |
| WESTERLUND1_3 | 252.0931 | -46.1953 | 339.43313351 | -0.79934014 | 282.1087 | 55462.25625 | 55463.3946296296 | 505051010 | 50204.6 | 50000 | 50204.6 | 50204.6 | 0 | 50204.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40796.6 | 40796.6 | 98343.8 | 1 | PROCESSED | 57553.5465162037 | 55840 | 55474.0771180556 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050078 | TeV emission surrounding Westerlund 1, the only super star cluster in our Galaxy, has been discovered. Molecular clouds associated with the TeV emission have been also discovered. This coincidence between the TeV emission and the molecular clouds suggests the proton origin of the TeV emission. However, the TeV emission should include the contribution from high-energy electrons. We observe Westerlund 1 with Suzaku to clarify the electron distribution and to examine the proton acceleration in the star cluster. | GALACTIC DIFFUSE EMISSION | 5 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 5 | AO5 | IS THE SUPER STAR CLUSTER WESTERLUND 1 ACCERELATING PROTONS? | XIS | Y |
| WESTERLUND1_4 | 253.5509 | -45.3005 | 340.7711384 | -1.01287357 | 288.2868 | 55463.3974652778 | 55464.5203587963 | 505052010 | 49627 | 50000 | 49627 | 49627 | 0 | 49627 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40213.7 | 40213.7 | 97007.9 | 1 | PROCESSED | 57553.5510416667 | 55840 | 55474.1080208333 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050078 | TeV emission surrounding Westerlund 1, the only super star cluster in our Galaxy, has been discovered. Molecular clouds associated with the TeV emission have been also discovered. This coincidence between the TeV emission and the molecular clouds suggests the proton origin of the TeV emission. However, the TeV emission should include the contribution from high-energy electrons. We observe Westerlund 1 with Suzaku to clarify the electron distribution and to examine the proton acceleration in the star cluster. | GALACTIC DIFFUSE EMISSION | 5 | A | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 5 | AO5 | IS THE SUPER STAR CLUSTER WESTERLUND 1 ACCERELATING PROTONS? | XIS | Y |
| G1.9+0.3 | 267.1951 | -27.1633 | 1.87759006 | 0.32236452 | 104.4114 | 55643.1608217593 | 55645.2856481482 | 505053010 | 100923.5 | 100000 | 100923.5 | 100931.5 | 0 | 100931.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 83425.1 | 83425.1 | 183565.7 | 1 | PROCESSED | 57601.3345833333 | 56025 | 55658.2502546296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050084 | We propose to observe the youngest (100yr) SNR G1.9+0.3 with Suzaku for 100 ks. The expected scientific fruits are to reveal the earliest stage of SNR evolution via the time variation of synchrotron emission, and to investigate the nuclear synthesis in the SN explosion via the detection of gamma-ray lines from 44Ti. | GALACTIC DIFFUSE EMISSION | 5 | A | KOKUBUN | MOTOHIDE | NULL | NULL | JAP | 5 | AO5 | INVESTIGATION OF THE YOUNGEST SNR G1.9+0.3 WITH SUZAKU | XIS | Y |
| L106_B3 | 337.3111 | 61.2453 | 106.66847152 | 2.94694679 | 86.3781 | 55332.0617013889 | 55333.5078587963 | 505054010 | 59380.4 | 60000 | 59380.4 | 59380.4 | 0 | 59380.4 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 54055.1 | 54055.1 | 124908 | 3 | PROCESSED | 57551.5609259259 | 55765 | 55393.2646759259 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050086 | We propose observarions of two fields on and near midplane (b = 0 and 3 deg.) in order to study bump-like emission peaked at 0.9 keV observed in midplane. The two fields proposed for observations has been observed by Chandra. By comparing the spectra taken by Suzaku and Chandra, we will determine the contribution of point sources (stars), and investigate posisble contribution of diffuse thermal plasma. | GALACTIC DIFFUSE EMISSION | 5 | B | TAKEI | YOH | NULL | NULL | JAP | 5 | AO5 | ORIGIN OF SOFT X-RAY EMISSION IN THE MILKY-WAY DISK | XIS | Y |
| BLOWOUT SHELL 1 | 311.9978 | 28.9736 | 72.22846422 | -9.10440661 | 48.7676 | 55360.0953587963 | 55361.2627546296 | 505055010 | 52194.5 | 50000 | 52218.5 | 52194.5 | 0 | 52218.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 43692.7 | 43692.7 | 100855.9 | 1 | PROCESSED | 57552.0261226852 | 55741 | 55375.7594907407 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050088 | The Cygnus Loop is a typical shell-like middle-aged SNR. The origin of this SNR is considered to be a cavity explosion. Many previous studies show the abundance of the Cygnus Loop's shell is wholly low (0.2 solar) while that of the ambient medium is typically 0.5 solar. Based on our previous observations, we found some shell regions show 0.5 solar abundances which are consistent with that of the ISM. To explain this result, we formed a hypothesis that the cavity wall density is low in such region and that the forward shock is now propagating outside the cavity, interacting with the ambient medium. In order to verify this hypothesis, we propose to observe the shell of the blowout region which originates from a large break of the cavity wall. We propose to observe two regions for 100ks. | GALACTIC DIFFUSE EMISSION | 5 | B | UCHIDA | HIROYUKI | NULL | NULL | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP BLOWOUT REGION | XIS | Y |
| BLOWOUT SHELL 2 | 312.2035 | 28.7297 | 72.14669544 | -9.39669734 | 48.0881 | 55361.263599537 | 55362.5155439815 | 505056010 | 52069.8 | 50000 | 52069.8 | 52069.8 | 0 | 52069.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46082.7 | 46082.7 | 108155.8 | 1 | PROCESSED | 57552.3493634259 | 55741 | 55375.7627893518 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050088 | The Cygnus Loop is a typical shell-like middle-aged SNR. The origin of this SNR is considered to be a cavity explosion. Many previous studies show the abundance of the Cygnus Loop's shell is wholly low (0.2 solar) while that of the ambient medium is typically 0.5 solar. Based on our previous observations, we found some shell regions show 0.5 solar abundances which are consistent with that of the ISM. To explain this result, we formed a hypothesis that the cavity wall density is low in such region and that the forward shock is now propagating outside the cavity, interacting with the ambient medium. In order to verify this hypothesis, we propose to observe the shell of the blowout region which originates from a large break of the cavity wall. We propose to observe two regions for 100ks. | GALACTIC DIFFUSE EMISSION | 5 | B | UCHIDA | HIROYUKI | NULL | NULL | JAP | 5 | AO5 | X-RAY OBSERVATION OF THE CYGNUS LOOP BLOWOUT REGION | XIS | Y |
| VICINITY_4U1957+11 | 300.5977 | 12.1307 | 52.0534723 | -9.74567764 | 252.1551 | 55499.6275578704 | 55501.8265625 | 505057010 | 80583.9 | 80000 | 80583.9 | 80583.9 | 0 | 80583.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 59204.2 | 59204.2 | 189975.9 | 2 | PROCESSED | 57553.9949305556 | 55882 | 55515.3752083333 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050090 | We propose for an observation of the vicinity of 4U 1957+11, in order to study the Galactic low-latitude hot gas. Recently, detection of OVII and NeIX aborption lines was reported in the spectrum of 4U 1957+11 (Yao et al. 2008). By combining a Suzaku observation of diffuse hot plasma around the object with the reported absorption line equivalnet widths, we will constrain the temperature, line-of-sight length, density of the hot plasma of the direction. Not only to understand the Galactic gas, but also to understand feedback mechanism from a galaxy to the intergalactic space will our study play an important role. | GALACTIC DIFFUSE EMISSION | 5 | B | TAKEI | YOH | NULL | NULL | JAP | 5 | AO5 | EMISSION/ABSORPTION COMBINATION STUDY OF GALACTIC LOW-LATITUDE HOT GAS | XIS | Y |
| L168_B53 | 153.7378 | 48.0763 | 167.64470811 | 53.18666692 | 109.5667 | 55519.8069328704 | 55521.5828356482 | 505058010 | 79499.9 | 80000 | 79499.9 | 79499.9 | 0 | 79499.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35661.9 | 35661.9 | 153421.8 | 1 | PROCESSED | 57554.2060763889 | 55898 | 55530.2748842593 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050106 | A dark patch extending degrees scale was found in the R4-band ROSAT All Sky Survey data from our re-analysis of the map based on the recent Suzaku results. The deficiency is small in R5 band . Strikingly the area well coincides with the dark patch in the 408 MHz emission. This indicates the low cosmic-ray and magnetic pressure of this area. We propose to observe this area to determine the temperature of the halo emission using Oxygen lines and to constrain the thermal pressure of hot interstellar medium. | GALACTIC DIFFUSE EMISSION | 5 | C | SEKIYA | NORIO | NULL | NULL | JAP | 5 | AO5 | DARK PATCH IN THE GALACTIC HALO X-RAY EMISSION AND ITS POSSIBLE RELATION TO RADIO SYNCHROTRON RADIATION | XIS | Y |
| HE FOCUSING CONE | 49.5833 | 10.9603 | 170.9618047 | -37.8533007 | 73.6953 | 55410.7011921296 | 55413.1439699074 | 505061010 | 101965.1 | 100000 | 101973.1 | 101973.1 | 0 | 101965.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 89145.2 | 89145.2 | 211045.9 | 2 | PROCESSED | 57552.9158796296 | 55808 | 55441.4075694444 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050129 | We propose the observation though the Helium Focusng Cone. This region seems to make the strong enhancement of Solarwind Charge exchange and cause the annual variation of it. We develop the best observation of the cone by using the area where the abosorption by molecular cloud is huge. By this observation, we investigate the mistery of the emission of Our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | B | YOSHITAKE | HIROSHI | NULL | NULL | JAP | 5 | AO5 | OBSERVATION THROUGH THE HELIUM FOCUSING CONE: SEARCH FOR THE VARIABILITY OF THE HELIOSPHERIC SOLAR WIND CHARGE EXCHANGE | XIS | Y |
| HE FOCUSING CONE | 49.5928 | 10.9507 | 170.97872575 | -37.85410489 | 253.7002 | 55591.1307291667 | 55593.7710763889 | 505062010 | 100167.8 | 100000 | 100167.8 | 100167.8 | 0 | 100167.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 82785.2 | 82785.2 | 228103.7 | 2 | PROCESSED | 57600.8639351852 | 55973 | 55607.305462963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050129 | We propose the observation though the Helium Focusng Cone. This region seems to make the strong enhancement of Solarwind Charge exchange and cause the annual variation of it. We develop the best observation of the cone by using the area where the abosorption by molecular cloud is huge. By this observation, we investigate the mistery of the emission of Our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | B | YOSHITAKE | HIROSHI | NULL | NULL | JAP | 5 | AO5 | OBSERVATION THROUGH THE HELIUM FOCUSING CONE: SEARCH FOR THE VARIABILITY OF THE HELIOSPHERIC SOLAR WIND CHARGE EXCHANGE | XIS | Y |
| DEM L238 | 83.8177 | -70.5927 | 281.24911245 | -31.77318091 | 307.401 | 55308.023125 | 55312.9730902778 | 505063010 | 199779.5 | 200000 | 199779.5 | 199779.5 | 0 | 199779.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 167835.5 | 167835.5 | 427629.7 | 5 | PROCESSED | 57551.4910069444 | 55287 | 55326.6889699074 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051102 | Type Ia SNe play a central role in modern astrophysics, and yet we know little about their progenitors. Some of these progenitors are expected to significantly modify ambient medium around them prior to SN explosions. A standard Type Ia SNR model, a white dwarf explosion in a uniform ambient medium, fails to account for bright Fe-rich ejecta and faint blast waves seen in majority of Type Ia SNRs in the Magellanic Clouds. A promising explanation involves presence of dense circumstellar medium (CSM) around their progenitors. We propose a Suzaku study of 4 mature Type Ia SNRs in the LMC, with the goal of determining chemical abundances, temperatures and ionization ages within their ejecta. This will allow us to construct dynamical SNR models, and learn about their CSM and progenitors. | GALACTIC DIFFUSE EMISSION | 5 | A | BORKOWSKI | KAZIMIERZ | NULL | NULL | USA | 5 | AO5 | TYPE IA REMNANTS IN THE LARGE MAGELLANIC CLOUD: WHAT PROGENITORS? | XIS | Y |
| 0534-69.9 | 83.5094 | -69.9134 | 280.47493809 | -31.97334872 | 273.4822 | 55286.3873726852 | 55289.2981597222 | 505064010 | 109236.7 | 100000 | 109268.7 | 109236.7 | 0 | 109276.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 79826.2 | 79826.2 | 251443.7 | 2 | PROCESSED | 57551.1453819445 | 55287 | 55302.4291898148 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051102 | Type Ia SNe play a central role in modern astrophysics, and yet we know little about their progenitors. Some of these progenitors are expected to significantly modify ambient medium around them prior to SN explosions. A standard Type Ia SNR model, a white dwarf explosion in a uniform ambient medium, fails to account for bright Fe-rich ejecta and faint blast waves seen in majority of Type Ia SNRs in the Magellanic Clouds. A promising explanation involves presence of dense circumstellar medium (CSM) around their progenitors. We propose a Suzaku study of 4 mature Type Ia SNRs in the LMC, with the goal of determining chemical abundances, temperatures and ionization ages within their ejecta. This will allow us to construct dynamical SNR models, and learn about their CSM and progenitors. | GALACTIC DIFFUSE EMISSION | 5 | A | BORKOWSKI | KAZIMIERZ | NULL | NULL | USA | 5 | AO5 | TYPE IA REMNANTS IN THE LARGE MAGELLANIC CLOUD: WHAT PROGENITORS? | XIS | Y |
| 0548-70.4 | 86.9619 | -70.4173 | 280.90214015 | -30.75163284 | 12.6051 | 55378.8779861111 | 55381.6286689815 | 505065010 | 103674.6 | 100000 | 103674.6 | 103674.6 | 0 | 103674.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 156971.6 | 156971.6 | 237635.8 | 1 | PROCESSED | 57552.5583912037 | 55287 | 55434.3854513889 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051102 | Type Ia SNe play a central role in modern astrophysics, and yet we know little about their progenitors. Some of these progenitors are expected to significantly modify ambient medium around them prior to SN explosions. A standard Type Ia SNR model, a white dwarf explosion in a uniform ambient medium, fails to account for bright Fe-rich ejecta and faint blast waves seen in majority of Type Ia SNRs in the Magellanic Clouds. A promising explanation involves presence of dense circumstellar medium (CSM) around their progenitors. We propose a Suzaku study of 4 mature Type Ia SNRs in the LMC, with the goal of determining chemical abundances, temperatures and ionization ages within their ejecta. This will allow us to construct dynamical SNR models, and learn about their CSM and progenitors. | GALACTIC DIFFUSE EMISSION | 5 | B | BORKOWSKI | KAZIMIERZ | NULL | NULL | USA | 5 | AO5 | TYPE IA REMNANTS IN THE LARGE MAGELLANIC CLOUD: WHAT PROGENITORS? | XIS | Y |
| VELA SNR CB1 | 130.2067 | -44.4709 | 263.57895082 | -1.58638955 | 294.2634 | 55318.1574074074 | 55318.5738425926 | 505068010 | 23666.5 | 20000 | 23666.5 | 23678 | 0 | 23666.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 18818 | 18818 | 35975.9 | 1 | PROCESSED | 57551.3448842593 | 55696 | 55330.1358449074 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051304 | The Vela SNR is known to have ejecta bullets outside the main shell. In addition to these bullets, signatures of ejecta inside the main shell have been uncovered in recent X-ray studies. Mostly, these are rich in light metals such as O, Ne, or Mg, whereas no Fe-rich ejecta had yet been detected. Based on archival XMM-Newton data, we found a possible Fe-rich ejecta bullet headed roughly in the opposite direction of Vela pulsar's motion. This would provide us with a window into the core-collapse SN explosion of the Vela SNR. Since its electron temperature is very low (~0.1 keV), the good Suzaku XIS response below 0.5 keV is suitable to study this object. We propose to observe it in four pointings. The requested exposure time is 20 ks each, resulting in a total exposure time of 80 ks. | GALACTIC DIFFUSE EMISSION | 5 | B | KATSUDA | SATORU | NULL | NULL | USA | 5 | AO5 | IRON-RICH EJECTA BULLET IN THE VELA SNR | XIS | Y |
| VELA SNR CB2 | 130.2058 | -44.7742 | 263.81853128 | -1.77251278 | 293.5729 | 55318.5746412037 | 55318.9238425926 | 505069010 | 19380.5 | 20000 | 19412.5 | 19404.5 | 0 | 19380.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 18829.8 | 18829.8 | 30167.9 | 0 | PROCESSED | 57551.3535763889 | 55696 | 55330.2121643518 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051304 | The Vela SNR is known to have ejecta bullets outside the main shell. In addition to these bullets, signatures of ejecta inside the main shell have been uncovered in recent X-ray studies. Mostly, these are rich in light metals such as O, Ne, or Mg, whereas no Fe-rich ejecta had yet been detected. Based on archival XMM-Newton data, we found a possible Fe-rich ejecta bullet headed roughly in the opposite direction of Vela pulsar's motion. This would provide us with a window into the core-collapse SN explosion of the Vela SNR. Since its electron temperature is very low (~0.1 keV), the good Suzaku XIS response below 0.5 keV is suitable to study this object. We propose to observe it in four pointings. The requested exposure time is 20 ks each, resulting in a total exposure time of 80 ks. | GALACTIC DIFFUSE EMISSION | 5 | B | KATSUDA | SATORU | NULL | NULL | USA | 5 | AO5 | IRON-RICH EJECTA BULLET IN THE VELA SNR | XIS | Y |
| VELA SNR CB3 | 129.7826 | -44.6964 | 263.57338638 | -1.96329272 | 278.1748 | 55318.927974537 | 55319.3418402778 | 505070010 | 18171.8 | 20000 | 18171.8 | 18171.8 | 0 | 18171.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17154.4 | 17154.4 | 35753.9 | 1 | PROCESSED | 57551.3562847222 | 55696 | 55330.1275925926 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051304 | The Vela SNR is known to have ejecta bullets outside the main shell. In addition to these bullets, signatures of ejecta inside the main shell have been uncovered in recent X-ray studies. Mostly, these are rich in light metals such as O, Ne, or Mg, whereas no Fe-rich ejecta had yet been detected. Based on archival XMM-Newton data, we found a possible Fe-rich ejecta bullet headed roughly in the opposite direction of Vela pulsar's motion. This would provide us with a window into the core-collapse SN explosion of the Vela SNR. Since its electron temperature is very low (~0.1 keV), the good Suzaku XIS response below 0.5 keV is suitable to study this object. We propose to observe it in four pointings. The requested exposure time is 20 ks each, resulting in a total exposure time of 80 ks. | GALACTIC DIFFUSE EMISSION | 5 | B | KATSUDA | SATORU | NULL | NULL | USA | 5 | AO5 | IRON-RICH EJECTA BULLET IN THE VELA SNR | XIS | Y |
| VELA SNR CB-LBG | 130.6266 | -44.6167 | 263.87788945 | -1.43970243 | 293.482 | 55319.3460648148 | 55319.7940046296 | 505071010 | 27179.9 | 20000 | 27179.9 | 27179.9 | 0 | 27179.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25094.5 | 25094.5 | 38693.9 | 1 | PROCESSED | 57551.3691203704 | 55696 | 55330.1543981482 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051304 | The Vela SNR is known to have ejecta bullets outside the main shell. In addition to these bullets, signatures of ejecta inside the main shell have been uncovered in recent X-ray studies. Mostly, these are rich in light metals such as O, Ne, or Mg, whereas no Fe-rich ejecta had yet been detected. Based on archival XMM-Newton data, we found a possible Fe-rich ejecta bullet headed roughly in the opposite direction of Vela pulsar's motion. This would provide us with a window into the core-collapse SN explosion of the Vela SNR. Since its electron temperature is very low (~0.1 keV), the good Suzaku XIS response below 0.5 keV is suitable to study this object. We propose to observe it in four pointings. The requested exposure time is 20 ks each, resulting in a total exposure time of 80 ks. | GALACTIC DIFFUSE EMISSION | 5 | B | KATSUDA | SATORU | NULL | NULL | USA | 5 | AO5 | IRON-RICH EJECTA BULLET IN THE VELA SNR | XIS | Y |
| SNR G106.3+2.7 P2 | 336.9121 | 60.9439 | 106.34649405 | 2.79001657 | 12.2687 | 55423.4230787037 | 55424.0209837963 | 505072010 | 24556.2 | 50000 | 24572.2 | 24556.2 | 0 | 24572.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 26614.7 | 26614.7 | 51655.9 | 1 | PROCESSED | 57553.084212963 | 55807 | 55441.2685069444 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051305 | After two decades searching for the origin of the GeV emission from 3EG J2227+6122, it is now identified with PSR J2229+6114 and its PWN.~This highly energetic young pulsar lies within the arcmin diameter Boomerang radio nebula. Now, recently discovered nearby extended TeV emission suggest a second Vela-like "cocoon" feed by relic electrons from the PWN, blowing out the vast degree-scale radio feature.~Interactions of the SNR shock front with overlapping molecular cloud material can also contribute in the gamma-ray production.~An XIS mosaic will allow us to search for soft and hard X-ray emission similar to Vela's "Cocoon" and resolve the nature of the TeV emission and its connection to the Boomerang and the radio feature. | GALACTIC DIFFUSE EMISSION | 5 | C | ALIU | ESTER | NULL | NULL | USA | 5 | AO5 | ORIGIN OF THE VHE GAMMA-RAY EMISSION FROM SNR G106.3+2.7 | XIS | Y |
| SNR G106.3+2.7 P3 | 336.5055 | 60.7692 | 106.0859109 | 2.74547808 | 12.2692 | 55424.0215509259 | 55424.9841782407 | 505073010 | 50454.8 | 50000 | 50462.8 | 50454.8 | 0 | 50463.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 50210.5 | 50210.5 | 83163.9 | 1 | PROCESSED | 57553.1155439815 | 55805 | 55439.1312037037 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051305 | After two decades searching for the origin of the GeV emission from 3EG J2227+6122, it is now identified with PSR J2229+6114 and its PWN.~This highly energetic young pulsar lies within the arcmin diameter Boomerang radio nebula. Now, recently discovered nearby extended TeV emission suggest a second Vela-like "cocoon" feed by relic electrons from the PWN, blowing out the vast degree-scale radio feature.~Interactions of the SNR shock front with overlapping molecular cloud material can also contribute in the gamma-ray production.~An XIS mosaic will allow us to search for soft and hard X-ray emission similar to Vela's "Cocoon" and resolve the nature of the TeV emission and its connection to the Boomerang and the radio feature. | GALACTIC DIFFUSE EMISSION | 5 | C | ALIU | ESTER | NULL | NULL | USA | 5 | AO5 | ORIGIN OF THE VHE GAMMA-RAY EMISSION FROM SNR G106.3+2.7 | XIS | Y |
| SNR G304.6+0.1 | 196.4463 | -62.6951 | 304.57643925 | 0.13082789 | 321.0575 | 55442.9126736111 | 55445.5356828704 | 505074010 | 99581.7 | 100000 | 99621.7 | 99581.7 | 0 | 99629.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 90565.3 | 90565.3 | 226531.9 | 1 | PROCESSED | 57553.3505555556 | 55827 | 55461.4231712963 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051306 | Galactic supernova remnants are believed to be the primary source of cosmic rays below 10^15.5 eV even though the exact acceleration mechanism remains unknown. This uncertainty results from the lack of remnants with synchrotron X-ray and GeV emission, needed to distinguish accelerated electrons from protons using broadband spectral modeling. An analysis of recent XMM and Fermi data suggests SNR G304.6+0.1 is just the third remnant with both, but the observed hard X-ray excess is also consistent with bremsstrahlung emission. We request a deep Suzaku observation of this source to determine the nature of its hard X-ray emission - critical for identifying the underlying acceleration mechanism. | GALACTIC DIFFUSE EMISSION | 5 | B | GELFAND | JOSEPH | NULL | NULL | USA | 5 | AO5 | THE ORIGIN OF THE HARD X-RAY AND GEV GAMMA-RAY EMISSION OF SNR G304.6+0.1 | XIS | Y |
| CARINA SW | 160.2531 | -60.104 | 287.34811018 | -1.23919183 | 109.6766 | 55542.7308333333 | 55543.4438888889 | 505075010 | 47003.9 | 45000 | 47003.9 | 47011.9 | 0 | 47011.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 42434.1 | 42434.1 | 61599.9 | 0 | PROCESSED | 57554.3916435185 | 55960 | 55592.9230324074 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051312 | X-ray nebulae with kT =0.1-0.8 keV, log Lx up to 35 ergs/s, and size of 1-1000 pc accompany a number of giant HII region. The Carinae Nebula is the best region to study their origin with 10-100 times more luminous soft X-rays than any other giant HII regions in our Galaxy. X-ray observations especially with Suzaku revealed that a part, or all, of the diffuse plasma would heat up by earlier supernova explosions, but it is unknown when these explosions occurred and how they made the current X-ray nebula. The Chandra Carina Complex Project displayed that the southern part of the nebula emits strong hydrogen-like oxygen line. We will measure helium-like oxygen line with Suzaku to measure its plasma temperature and abundance to help understand relation with plasma in the nebula center. | GALACTIC DIFFUSE EMISSION | 5 | C | HAMAGUCHI | KENJI | NULL | NULL | USA | 5 | AO5 | SOUTHERN PART OF DIFFUSE PLASMA IN THE CARINA NEBULA - RICH IN OXYGEN? | XIS | Y |
| AX J1714.1-3912 | 258.5249 | -39.1972 | 347.85266774 | -0.22742448 | 85.6964 | 55608.0538078704 | 55608.9654050926 | 505076010 | 32601.7 | 30000 | 32601.7 | 32601.7 | 0 | 32601.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28336.2 | 28336.2 | 78757.9 | 1 | PROCESSED | 57600.9625115741 | 55988 | 55621.1409027778 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 052012 | Molecular clouds are predicted to emit strong non-thermal X-rays when they are close to particle-accelerating SNRs, but this emission has not been confirmed yet. We propose to observe the non-thermal X-ray source AX J1714.1-3912 to investigate its relationship with the SNR RX J1713.7-3946. ASCA observations have shown that the hard spectrum of the source may be associated with bremsstrahlung emission from particles accelerated in the SNR and diffusing in a nearby molecular cloud. This emission has never been observed in other SNRs. However, the association of the source with the remnant is still controversial and the ASCA data do not allow us to constrain the spectral properties. We aim at verifying the association with the remnant and at investigating the physical origin of the emission. | GALACTIC DIFFUSE EMISSION | 5 | A | MICELI | MARCO | NULL | NULL | EUR | 5 | AO5 | INVESTIGATING THE PHYSICAL ORIGIN OF AX J1714.1-3912 | XIS | Y |
| GALACTIC_BULGE3 | 267.9488 | -29.7963 | 359.95634845 | -1.5962466 | 107.1729 | 55624.8013310185 | 55626.2292939815 | 505078010 | 51275.6 | 50000 | 51275.6 | 51275.6 | 0 | 51275.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39312.4 | 39312.4 | 123361.8 | 0 | PROCESSED | 57601.0957407407 | 55287 | 55642.1205787037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 5 | AO5 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y |
| GALACTIC_BULGE4 | 269.1417 | -30.4015 | 359.95546853 | -2.79264334 | 69.3552 | 55632.2752314815 | 55633.4287152778 | 505079010 | 50219.3 | 50000 | 50227.3 | 50219.3 | 0 | 50227.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43375 | 43375 | 99648 | 1 | PROCESSED | 57601.1540277778 | 55287 | 55645.5706134259 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 5 | AO5 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y |
| GALACTIC_BULGE5 | 270.1525 | -30.903 | 359.95222621 | -3.79644913 | 86.7823 | 55293.7188657407 | 55295.8849074074 | 505080010 | 56139.6 | 50000 | 56139.6 | 56139.6 | 0 | 56139.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 55149.8 | 55149.8 | 185005.8 | 1 | PROCESSED | 57553.0630439815 | 55287 | 55441.4355555556 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 5 | AO5 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y |
| GALACTIC_BULGE6 | 271.3758 | -31.4828 | 359.95693453 | -4.99276165 | 88.0304 | 55639.361087963 | 55640.3565162037 | 505081010 | 50166.9 | 50000 | 50171.4 | 50166.9 | 0 | 50179.5 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 43635.7 | 43635.7 | 85989.8 | 0 | PROCESSED | 57601.2415277778 | 55287 | 55649.2186574074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 5 | AO5 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y |
| GALACTIC_BULGE13 | 264.5912 | -32.1955 | 356.40747371 | -0.39354159 | 92.0351 | 55635.5794907407 | 55636.621099537 | 505082010 | 48496.9 | 50000 | 48512.9 | 48512.9 | 0 | 48496.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41255 | 41255 | 89979.8 | 0 | PROCESSED | 57601.201412037 | 55287 | 55648.3385763889 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 5 | AO5 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y |
| GALACTIC_BULGE14 | 264.9946 | -32.433 | 356.38820164 | -0.80858885 | 270.5244 | 55479.5865509259 | 55480.8980671296 | 505083010 | 52938.3 | 50000 | 52938.3 | 52938.3 | 0 | 52938.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 42407.3 | 42407.3 | 113303.9 | 1 | PROCESSED | 57553.7064236111 | 55287 | 55491.0402893518 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 5 | AO5 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y |
| GALACTIC_BULGE15 | 265.6963 | -32.7784 | 356.40742505 | -1.49294303 | 89.8786 | 55626.2338425926 | 55627.5424884259 | 505084010 | 50309.7 | 50000 | 50317.2 | 50309.7 | 0 | 50325.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 37509.5 | 37509.5 | 113055.9 | 0 | PROCESSED | 57601.1030439815 | 55287 | 55645.2697222222 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 5 | AO5 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y |
| GALACTIC_BULGE16 | 266.5113 | -33.2224 | 356.38592507 | -2.30771737 | 275.4625 | 55482.2533217593 | 55483.5626967593 | 505085010 | 55031.5 | 50000 | 55031.5 | 55031.5 | 0 | 55031.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48634.1 | 48634.1 | 113113.9 | 1 | PROCESSED | 57553.750787037 | 55287 | 55502.290150463 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 5 | AO5 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y |
| GALACTIC_BULGE17 | 267.7467 | -33.8391 | 356.3863118 | -3.50805248 | 275.261 | 55483.5637731482 | 55485.0627893518 | 505086010 | 53126.6 | 50000 | 53126.6 | 54089.5 | 0 | 54089.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46276.9 | 46276.9 | 129493.8 | 1 | PROCESSED | 57553.7652430556 | 55287 | 55508.2025694444 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 5 | AO5 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y |
| GALACTIC_BULGE18 | 269.3126 | -34.5716 | 356.40349802 | -4.99577293 | 70.9023 | 55633.4308101852 | 55634.5273263889 | 505087010 | 51428.4 | 50000 | 51468.4 | 51428.4 | 0 | 51475.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 44207.2 | 44207.2 | 94727.9 | 1 | PROCESSED | 57601.1565046296 | 55287 | 55649.0417824074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 5 | AO5 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y |
| HESS J1841-55 1 | 279.8307 | -5.8897 | 26.31151486 | -0.00077944 | 87.7391 | 55645.2916782407 | 55646.4446180556 | 505088010 | 49652 | 50000 | 49652 | 49652 | 0 | 49652 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39860.4 | 39860.4 | 99597.8 | 0 | PROCESSED | 57601.3329976852 | 55287 | 55658.1566087963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 5 | AO5 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y |
| HESS J1841-55 2 | 280.1473 | -5.9564 | 26.39650339 | -0.31125339 | 87.3564 | 55646.4452777778 | 55647.6391550926 | 505089010 | 50005.3 | 50000 | 50030.4 | 50005.3 | 0 | 50030.4 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 43178.9 | 43178.9 | 103113.9 | 0 | PROCESSED | 57601.3264236111 | 55287 | 55658.2084606482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 5 | AO5 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y |
| HESS J1841-55 3 | 280.1471 | -5.609 | 26.70525302 | -0.15199861 | 87.0298 | 55647.6397685185 | 55648.791875 | 505090010 | 49549 | 50000 | 49581 | 49549 | 0 | 49581 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42793.5 | 42793.5 | 99523.9 | 1 | PROCESSED | 57601.3633101852 | 55287 | 55666.2655439815 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 5 | AO5 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y |
| HESS J1841-55 4 | 280.4555 | -5.2917 | 27.12788601 | -0.27973073 | 86.6744 | 55648.7926273148 | 55649.9633449074 | 505091010 | 51253.9 | 50000 | 51253.9 | 51253.9 | 0 | 51253.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45007.8 | 45007.8 | 101142 | 1 | PROCESSED | 57601.3663310185 | 55287 | 55666.3000115741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056001 | We propose to observe three classes of objects, which seem independent subjects, but are closely related with each others. These subjects are the Galactic center and the ridge diffuse X-rays (GCDX & GRDX), Unidentified sources (UIDHESS) found with HESS and the hard X-rays from radio faint supernova remnants (Hard SNR) found with ASCA. Our objectives are to study individual science on each subject, combined the results, and to finally approach to a unified picture on the diffuse high energy aspects in our Galaxy. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 5 | AO5 | SYSTEMATIC STUDY OF THE DIFFUSE HIGH ENERGY OBJECTS IN OUR GALAXY | XIS | Y |
| THE KEPLER SNR | 262.6745 | -21.5044 | 4.50818409 | 6.8092486 | 272.4561 | 55469.9826736111 | 55470.368287037 | 505092010 | 17714.1 | 620000 | 17722.1 | 17730.1 | 0 | 17714.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17869.4 | 17869.4 | 33307.9 | 0 | PROCESSED | 57553.595 | 55287 | 55482.4747453704 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056004 | The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors. | GALACTIC DIFFUSE EMISSION | 5 | A | PARK | SANGWOOK | NULL | NULL | USA | 5 | AO5 | A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR | XIS | Y |
| THE KEPLER SNR | 262.6737 | -21.5073 | 4.50532186 | 6.80830692 | 272.2663 | 55475.6914583333 | 55478.2863194445 | 505092020 | 111194.1 | 620000 | 111194.1 | 111202.1 | 0 | 111202.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 99841.3 | 99841.3 | 224143.7 | 2 | PROCESSED | 57553.7268402778 | 55287 | 55488.3311689815 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056004 | The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors. | GALACTIC DIFFUSE EMISSION | 5 | A | PARK | SANGWOOK | NULL | NULL | USA | 5 | AO5 | A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR | XIS | Y |
| THE KEPLER SNR | 262.6706 | -21.4823 | 4.52493262 | 6.82424916 | 102.5027 | 55615.8474421296 | 55616.8174768518 | 505092030 | 34201.5 | 150000 | 34209.5 | 34201.5 | 0 | 34209.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 29119.9 | 29119.9 | 83795.8 | 0 | PROCESSED | 57601.0436342593 | 55287 | 55628.1747569444 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056004 | The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors. | GALACTIC DIFFUSE EMISSION | 5 | A | PARK | SANGWOOK | NULL | NULL | USA | 5 | AO5 | A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR | XIS | Y |
| THE KEPLER SNR | 262.6707 | -21.4823 | 4.52498329 | 6.82417088 | 98.3356 | 55620.8079166667 | 55624.797337963 | 505092040 | 146233.7 | 250000 | 146233.7 | 146254.1 | 0 | 146257.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 113802.2 | 113802.2 | 344657.7 | 6 | PROCESSED | 57601.192337963 | 55287 | 55642.4090046296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056004 | The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors. | GALACTIC DIFFUSE EMISSION | 5 | A | PARK | SANGWOOK | NULL | NULL | USA | 5 | AO5 | A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR | XIS | Y |
| THE KEPLER SNR | 262.671 | -21.4826 | 4.5248811 | 6.82377384 | 98.1034 | 55628.0376736111 | 55632.2696643518 | 505092050 | 84591.3 | 100000 | 84591.3 | 85663.2 | 0 | 85719.2 | 4 | 3 | 0 | 3 | 1 | 0 | 0 | 122488.1 | 122488.1 | 365616 | 3 | PROCESSED | 57601.284537037 | 55287 | 55648.4964699074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056004 | The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors. | GALACTIC DIFFUSE EMISSION | 5 | A | PARK | SANGWOOK | NULL | NULL | USA | 5 | AO5 | A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR | XIS | Y |
| THE KEPLER SNR | 262.6712 | -21.4826 | 4.52498243 | 6.82361728 | 97.9009 | 55634.5331712963 | 55635.5759606482 | 505092060 | 46496.1 | 100000 | 46640.1 | 46496.1 | 0 | 46640.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38611.8 | 38611.8 | 90050 | 1 | PROCESSED | 57601.1934143518 | 55287 | 55648.2987731482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056004 | The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors. | GALACTIC DIFFUSE EMISSION | 5 | A | PARK | SANGWOOK | NULL | NULL | USA | 5 | AO5 | A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR | XIS | Y |
| THE KEPLER SNR | 262.671 | -21.485 | 4.52284766 | 6.82247636 | 99.4153 | 55649.9685416667 | 55653.0828356482 | 505092070 | 133390.6 | 90000 | 133398.6 | 133398.6 | 0 | 133390.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 112217.2 | 112217.2 | 269027.8 | 1 | PROCESSED | 57601.4459490741 | 55287 | 55666.5226736111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056004 | The detailed nature of the progenitor of Type Ia supernovae (SNe) is elusive. X-ray line emission from low abundant elements (Cr, Mn, and Ni) in young supernova remnants (SNR) provides an excellent opportunity to study the Type Ia SN nucleosynthesis and thus to reveal the metallicity of the progenitor. Suzaku XIS observations are an efficient tool for such an X-ray spectroscopy. We propose a deep Suzaku XIS observation of Kepler's SNR to study the peculiar nature of its Type Ia SN progenitor. Our proposed Suzaku X-ray study of the Cr, Mn, and Ni line emission in Kepler will reveal the progenitor's metallicity in an unprecedented detail, which will be an excellent complementary work to the existing Suzaku Long Program of Tycho's SNR to reveal the nature of Type Ia SN progenitors. | GALACTIC DIFFUSE EMISSION | 5 | A | PARK | SANGWOOK | NULL | NULL | USA | 5 | AO5 | A DEEP OBSERVATION OF THE KEPLER SUPERNOVA REMNANT: NUCLEOSYNTHESIS OF A TYPE IA SUPERNOVA WITH A PECULIAR PROGENITOR | XIS | Y |
| BD+43 3654 | 308.4185 | 44.0658 | 82.48241574 | 2.36274642 | 104.8287 | 55655.0785416667 | 55657.0925231482 | 506004010 | 97047.8 | 100000 | 98963.8 | 97047.8 | 0 | 98963.8 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 88925.6 | 88925.6 | 173987.7 | 0 | PROCESSED | 57601.4465972222 | 56037 | 55670.3073842593 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060010 | It is very important to search for possible particle-acceleration sites among the astrophysical objects. Very recently, synchrotron emission has been discovered with the VLA radio observation from a bow shock region of a runaway star, BD+43 3654, having a very fast stellar wind whose velocity reaches up to 2300 km/s. The maximum energy is estimated to be about 10 TeV, and thus the emission should come to the X-ray band. Here, we propose to perform the 100 ksec observation of BD+43 3654 with Suzaku, in order to determine the strength of the shock from the temperature of the post-shock plasma and to determine the maximum energy of the accelerated electrons. | GALACTIC DIFFUSE EMISSION | 5 | A | TERADA | YUKIKATSU | NULL | NULL | JAP | 6 | AO6 | SUZAKU OBSERVATION OF NON-THERMAL EMISSION FROM A BOW SHOCK REGION OF A RUNAWAY STAR, BD+43 3654 | XIS | Y |
| HB21 SOUTH | 311.2512 | 50.6016 | 88.85305014 | 4.80482025 | 105.492 | 55660.3542361111 | 55662.8155208333 | 506005010 | 132363 | 150000 | 132371 | 132371 | 0 | 132363 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 141788.7 | 141788.7 | 212635.9 | 1 | PROCESSED | 57601.4958564815 | 56159 | 55677.2811342593 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060011 | Over-ionization in SNRs is one of the biggest mystery Suzaku discovered. It affects a lot the study on chemical and thermal evolution of universe, but the origin is still unknown. HB21 is an old SNR with molecular cloud interaction and GeV gamma-rays, which remind us typical over-ionization SNRs. On the other hand, the interacting molecular cloud is much smaller or thinner than those interacting with over-ionization SNRs, and as a result, HB21 can be the key target to study the origin of over-ionization. Suzaku deep observation of HB21 south (interacting point) will determine the condition of plasma and judge whether it is in over-ionization or not, which will show us the origin of over-ionizing plasma. | GALACTIC DIFFUSE EMISSION | 5 | A | BAMBA | AYA | NULL | NULL | JAP | 6 | AO6 | ORIGIN OF OVER-IONIZATION OF SNR PLASMAS | XIS | Y |
| HB21 SOUTH | 311.2245 | 50.5821 | 88.82715261 | 4.80607932 | 6.557 | 55767.8922337963 | 55768.4953819444 | 506005020 | 23460.7 | 20000 | 23468.7 | 23476.7 | 0 | 23460.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26264.9 | 26264.9 | 52103.9 | 1 | PROCESSED | 57602.6622685185 | 56159 | 55792.1611458333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060011 | Over-ionization in SNRs is one of the biggest mystery Suzaku discovered. It affects a lot the study on chemical and thermal evolution of universe, but the origin is still unknown. HB21 is an old SNR with molecular cloud interaction and GeV gamma-rays, which remind us typical over-ionization SNRs. On the other hand, the interacting molecular cloud is much smaller or thinner than those interacting with over-ionization SNRs, and as a result, HB21 can be the key target to study the origin of over-ionization. Suzaku deep observation of HB21 south (interacting point) will determine the condition of plasma and judge whether it is in over-ionization or not, which will show us the origin of over-ionizing plasma. | GALACTIC DIFFUSE EMISSION | 5 | A | BAMBA | AYA | NULL | NULL | JAP | 6 | AO6 | ORIGIN OF OVER-IONIZATION OF SNR PLASMAS | XIS | Y |
| JUPITER | 28.6779 | 10.4549 | 147.25964186 | -49.40473582 | 249.1856 | 55929.8714467593 | 55930.8243865741 | 506006010 | 33533.1 | 160000 | 33533.1 | 33533.1 | 0 | 33533.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32136.9 | 32136.9 | 82323.9 | 1 | PROCESSED | 57604.310625 | 56316 | 55946.1978472222 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060017 | Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose to observe Jupiter again in a different epoch. Comparison with the previous spectra and image will reveal how Jovian magnetosphere interacts with the solar wind and will give us clues about how electrons are accelerated in such a large region around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | B | ISHIKAWA | KUMI | NULL | NULL | JAP | 6 | AO6 | STUDY OF DIFFUSE X-RAY EMISSION FROM JOVIAN MAGNETOSPHERE | XIS | Y |
| JUPITER | 28.7092 | 10.4688 | 147.29554938 | -49.38035583 | 249.1847 | 55930.8245717593 | 55931.8508564815 | 506006020 | 35518 | 160000 | 35522 | 35518 | 0 | 35526 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34367 | 34367 | 88659.9 | 0 | PROCESSED | 57604.3110185185 | 56316 | 55946.2294097222 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060017 | Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose to observe Jupiter again in a different epoch. Comparison with the previous spectra and image will reveal how Jovian magnetosphere interacts with the solar wind and will give us clues about how electrons are accelerated in such a large region around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | B | ISHIKAWA | KUMI | NULL | NULL | JAP | 6 | AO6 | STUDY OF DIFFUSE X-RAY EMISSION FROM JOVIAN MAGNETOSPHERE | XIS | Y |
| JUPITER | 28.9811 | 10.6021 | 147.5984875 | -49.15640747 | 249.1843 | 55937.2038773148 | 55938.208599537 | 506006030 | 34894.2 | 160000 | 34902.2 | 34910.2 | 0 | 34894.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32208.1 | 32208.1 | 86791.8 | 2 | PROCESSED | 57604.3101273148 | 56319 | 55952.170787037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060017 | Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose to observe Jupiter again in a different epoch. Comparison with the previous spectra and image will reveal how Jovian magnetosphere interacts with the solar wind and will give us clues about how electrons are accelerated in such a large region around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | B | ISHIKAWA | KUMI | NULL | NULL | JAP | 6 | AO6 | STUDY OF DIFFUSE X-RAY EMISSION FROM JOVIAN MAGNETOSPHERE | XIS | Y |
| JUPITER | 29.0345 | 10.6283 | 147.65759499 | -49.11229838 | 249.1849 | 55938.2087962963 | 55939.2481944444 | 506006040 | 38628.9 | 160000 | 38628.9 | 38636.7 | 0 | 38636.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 31769.2 | 31769.2 | 89785.9 | 0 | PROCESSED | 57604.3463657407 | 56388 | 56020.1680208333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060017 | Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose to observe Jupiter again in a different epoch. Comparison with the previous spectra and image will reveal how Jovian magnetosphere interacts with the solar wind and will give us clues about how electrons are accelerated in such a large region around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | B | ISHIKAWA | KUMI | NULL | NULL | JAP | 6 | AO6 | STUDY OF DIFFUSE X-RAY EMISSION FROM JOVIAN MAGNETOSPHERE | XIS | Y |
| JUPITER | 29.0829 | 10.6504 | 147.71201597 | -49.07381266 | 249.1851 | 55939.2483912037 | 55939.8634722222 | 506006050 | 23282.7 | 160000 | 23290.7 | 23282.7 | 0 | 23295.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19267.9 | 19267.9 | 53136 | 0 | PROCESSED | 57604.3330902778 | 56331 | 55960.1390740741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060017 | Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose to observe Jupiter again in a different epoch. Comparison with the previous spectra and image will reveal how Jovian magnetosphere interacts with the solar wind and will give us clues about how electrons are accelerated in such a large region around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | B | ISHIKAWA | KUMI | NULL | NULL | JAP | 6 | AO6 | STUDY OF DIFFUSE X-RAY EMISSION FROM JOVIAN MAGNETOSPHERE | XIS | Y |
| CYGNUS LOOP W-B-N | 311.1498 | 30.6623 | 73.11766027 | -7.48614398 | 71.1125 | 55692.7736574074 | 55693.7709606482 | 506007010 | 45900.6 | 44000 | 45900.6 | 45900.6 | 0 | 45900.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40833.7 | 40833.7 | 86133.9 | 0 | PROCESSED | 57602.0331597222 | 56072 | 55705.1432523148 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060042 | The Cygnus Loop is a prototypical middle-aged SNR. Based on our previous observations, the shell region shows relatively low temperature with low metal abundance. The interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Its abundance non-uniformity indicates the asymmetric explosion. There are two blow-out features: a south-break with one degree diameter and a west-break with half degree diameter. The west-break shows a half-moon shape indicating a rapid expansion in a tenuous plasma. We propose to observe the west-break with SUZAKU for 100 ksec. The plasma in the west-break must be a pure fossil plasma of the SN. We want to study the plasma structure that is almost free from obscuration by the ISM. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 6 | AO6 | HUNT FOR THE FOSSIL OF THE PROGENITOR STAR IN THE WEST BREAK OF THE CYGNUS LOOP SUPERNOVA REMNANT | XIS | Y |
| CYGNUS LOOP W-B-S | 311.1967 | 30.3719 | 72.9110541 | -7.69596159 | 71.021 | 55693.7715277778 | 55694.9794212963 | 506008010 | 55649.9 | 56000 | 55649.9 | 55649.9 | 0 | 55649.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 49851.6 | 49851.6 | 104325.9 | 1 | PROCESSED | 57602.0472916667 | 56072 | 55705.1847800926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060042 | The Cygnus Loop is a prototypical middle-aged SNR. Based on our previous observations, the shell region shows relatively low temperature with low metal abundance. The interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Its abundance non-uniformity indicates the asymmetric explosion. There are two blow-out features: a south-break with one degree diameter and a west-break with half degree diameter. The west-break shows a half-moon shape indicating a rapid expansion in a tenuous plasma. We propose to observe the west-break with SUZAKU for 100 ksec. The plasma in the west-break must be a pure fossil plasma of the SN. We want to study the plasma structure that is almost free from obscuration by the ISM. | GALACTIC DIFFUSE EMISSION | 5 | A | TSUNEMI | HIROSHI | NULL | NULL | JAP | 6 | AO6 | HUNT FOR THE FOSSIL OF THE PROGENITOR STAR IN THE WEST BREAK OF THE CYGNUS LOOP SUPERNOVA REMNANT | XIS | Y |
| CYGNUS LOOP BLOWOUT1 | 312.1499 | 29.2487 | 72.53069275 | -9.03908096 | 78.1532 | 55686.7775578704 | 55687.8494907407 | 506011010 | 48564.1 | 50000 | 48564.1 | 48564.1 | 0 | 48564.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42042.9 | 42042.9 | 92579.9 | 1 | PROCESSED | 57601.954224537 | 56066 | 55698.3278472222 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060053 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a strong Si-K line emission from the southernmost blowout region where the shell is very thin. The complete observation of this region will reveal a pure ejecta of this remnant. We may also be able to reveal a whole picture of an asymmetric ejecta distribution of the Cygnus Loop. We propose 6-pointing observation of the Cygnus Loop's blowout region for 240ks. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIDA | HIROYUKI | NULL | NULL | JAP | 6 | AO6 | MEASUREMENT OF ABUNDANCES INSIDE THE SOUTHERNMOST PART OF THE CYGNUS LOOP, BLOWOUT REGION | XIS | Y |
| CYGNUS LOOP BLOWOUT2 | 312.4423 | 29.4154 | 72.82314938 | -9.13589092 | 78.1524 | 55687.8500578704 | 55688.6488310185 | 506012010 | 35655 | 35000 | 35655 | 35655 | 0 | 35655 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 31481.5 | 31481.5 | 68982.1 | 0 | PROCESSED | 57601.9748263889 | 56066 | 55700.4593865741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060053 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a strong Si-K line emission from the southernmost blowout region where the shell is very thin. The complete observation of this region will reveal a pure ejecta of this remnant. We may also be able to reveal a whole picture of an asymmetric ejecta distribution of the Cygnus Loop. We propose 6-pointing observation of the Cygnus Loop's blowout region for 240ks. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIDA | HIROYUKI | NULL | NULL | JAP | 6 | AO6 | MEASUREMENT OF ABUNDANCES INSIDE THE SOUTHERNMOST PART OF THE CYGNUS LOOP, BLOWOUT REGION | XIS | Y |
| CYGNUS LOOP BLOWOUT3 | 312.3799 | 29.0257 | 72.47923846 | -9.33489782 | 78.1517 | 55688.6493981482 | 55689.9654976852 | 506013010 | 60266.9 | 60000 | 60266.9 | 60274.9 | 0 | 60266.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 55980.3 | 55980.3 | 113628.8 | 1 | PROCESSED | 57601.9873611111 | 56066 | 55700.4602083333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060053 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a strong Si-K line emission from the southernmost blowout region where the shell is very thin. The complete observation of this region will reveal a pure ejecta of this remnant. We may also be able to reveal a whole picture of an asymmetric ejecta distribution of the Cygnus Loop. We propose 6-pointing observation of the Cygnus Loop's blowout region for 240ks. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIDA | HIROYUKI | NULL | NULL | JAP | 6 | AO6 | MEASUREMENT OF ABUNDANCES INSIDE THE SOUTHERNMOST PART OF THE CYGNUS LOOP, BLOWOUT REGION | XIS | Y |
| CYGNUS LOOP BLOWOUT4 | 312.6611 | 29.185 | 72.76042835 | -9.42856877 | 61.4261 | 55707.9937268518 | 55708.6620486111 | 506014010 | 26055.1 | 25000 | 26055.1 | 26063.1 | 0 | 26071.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20271.3 | 20271.3 | 57737.9 | 0 | PROCESSED | 57602.1387037037 | 56092 | 55725.2494097222 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060053 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a strong Si-K line emission from the southernmost blowout region where the shell is very thin. The complete observation of this region will reveal a pure ejecta of this remnant. We may also be able to reveal a whole picture of an asymmetric ejecta distribution of the Cygnus Loop. We propose 6-pointing observation of the Cygnus Loop's blowout region for 240ks. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIDA | HIROYUKI | NULL | NULL | JAP | 6 | AO6 | MEASUREMENT OF ABUNDANCES INSIDE THE SOUTHERNMOST PART OF THE CYGNUS LOOP, BLOWOUT REGION | XIS | Y |
| CYGNUS LOOP BLOWOUT5 | 312.5999 | 28.7931 | 72.41540255 | -9.63024021 | 60.972 | 55708.6627546296 | 55709.5335185185 | 506015010 | 36755.2 | 35000 | 36763.2 | 36755.2 | 0 | 36769.5 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 31631.7 | 31631.7 | 75216 | 1 | PROCESSED | 57602.1728935185 | 56093 | 55725.2447569444 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060053 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a strong Si-K line emission from the southernmost blowout region where the shell is very thin. The complete observation of this region will reveal a pure ejecta of this remnant. We may also be able to reveal a whole picture of an asymmetric ejecta distribution of the Cygnus Loop. We propose 6-pointing observation of the Cygnus Loop's blowout region for 240ks. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIDA | HIROYUKI | NULL | NULL | JAP | 6 | AO6 | MEASUREMENT OF ABUNDANCES INSIDE THE SOUTHERNMOST PART OF THE CYGNUS LOOP, BLOWOUT REGION | XIS | Y |
| CYGNUS LOOP BLOWOUT6 | 312.8964 | 28.9665 | 72.71699713 | -9.72555156 | 78.1534 | 55691.9894791667 | 55692.7710069445 | 506016010 | 36374.4 | 35000 | 36374.4 | 36374.4 | 0 | 36374.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32756.8 | 32756.8 | 67503.9 | 0 | PROCESSED | 57602.0240277778 | 56068 | 55701.1981828704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060053 | The Cygnus Loop is a prototypical middle-aged SNR. Based on the previous observation, the shell region shows relatively low temperature with low metal abundance while the interior shows high temperature with high metal abundance. The plasma in the interior is the fossil of the progenitor star. Recently, we found a strong Si-K line emission from the southernmost blowout region where the shell is very thin. The complete observation of this region will reveal a pure ejecta of this remnant. We may also be able to reveal a whole picture of an asymmetric ejecta distribution of the Cygnus Loop. We propose 6-pointing observation of the Cygnus Loop's blowout region for 240ks. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIDA | HIROYUKI | NULL | NULL | JAP | 6 | AO6 | MEASUREMENT OF ABUNDANCES INSIDE THE SOUTHERNMOST PART OF THE CYGNUS LOOP, BLOWOUT REGION | XIS | Y |
| GAMMACYGNI_NWSHELL1 | 304.9359 | 40.8711 | 78.38707497 | 2.60425327 | 82.9977 | 55664.4219675926 | 55665.3022222222 | 506017010 | 39027.1 | 40000 | 39027.1 | 39027.1 | 0 | 39027.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37696.5 | 37696.5 | 76052 | 0 | PROCESSED | 57601.5010416667 | 56058 | 55690.9556597222 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060059 | We propose deep X-ray observations of outer edge of gamma Cygni SNR north-west shell with Suzaku. Radio observation shows that this SNR has shell-type structure in the north-west and south-east. High energy diffuse gamma-ray emission have been recently detected from the north-west shell by Fermi gamma-ray space telescope and VERITAS TeV telescope. Main objective of this proposal is to reveal the emission mechanisms not only in X-ray band but also in GeV and TeV bands through the extent of the X-ray emission and spectroscopy. Only Suzaku can achieve this, because the background level of XIS is very low and the broadness of the energy band. | GALACTIC DIFFUSE EMISSION | 5 | B | TANAKA | YASUYUKI | NULL | NULL | JAP | 6 | AO6 | SUZAKU X-RAY OBSERVATION OF OUTER EDGE OF GAMMA CYGNI SNR NORTH-WEST SHELL | XIS | Y |
| GAMMACYGNI_NWSHELL2 | 304.652 | 40.6975 | 78.12229495 | 2.68416641 | 82.9982 | 55665.3027430556 | 55666.2688657407 | 506018010 | 39712 | 40000 | 39712 | 39712 | 0 | 39712 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36116.5 | 36116.5 | 83437.9 | 0 | PROCESSED | 57601.5048032407 | 56058 | 55690.9818402778 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060059 | We propose deep X-ray observations of outer edge of gamma Cygni SNR north-west shell with Suzaku. Radio observation shows that this SNR has shell-type structure in the north-west and south-east. High energy diffuse gamma-ray emission have been recently detected from the north-west shell by Fermi gamma-ray space telescope and VERITAS TeV telescope. Main objective of this proposal is to reveal the emission mechanisms not only in X-ray band but also in GeV and TeV bands through the extent of the X-ray emission and spectroscopy. Only Suzaku can achieve this, because the background level of XIS is very low and the broadness of the energy band. | GALACTIC DIFFUSE EMISSION | 5 | B | TANAKA | YASUYUKI | NULL | NULL | JAP | 6 | AO6 | SUZAKU X-RAY OBSERVATION OF OUTER EDGE OF GAMMA CYGNI SNR NORTH-WEST SHELL | XIS | Y |
| HESSJ1857-A | 284.2126 | 2.7519 | 35.99783049 | 0.0515802 | 269.8116 | 55822.9197800926 | 55823.984212963 | 506019010 | 40924.9 | 40000 | 40924.9 | 40924.9 | 0 | 40924.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35846.9 | 35846.9 | 91927.9 | 1 | PROCESSED | 57603.2046180556 | 56233 | 55865.2326157407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060061 | Many TeV gamma-ray objects discovered on the Galactic plane are classified as pulsar wind nebulae (PWNe), just because there exists a pulsar in the vicinity of them. X-ray observations can directly show the physical connection between the TeV emission and PWNe by presenting the existence of X-ray PWNe. HESSJ1857 and HESSJ1832 are unidentified TeV objects, but they may be TeV PWNe driven by pulsars close to them. We propose to observe them to study whether the pulsars have X-ray PWNe or not. | GALACTIC DIFFUSE EMISSION | 5 | B | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 6 | AO6 | ARE THE TEV UNIDENTIFIED OBJECTS, HESSJ1857+026 AND HESSJ1832-084, PULSAR WIND NEBULAE? | XIS | Y |
| HESSJ1857-B | 284.5485 | 2.7494 | 36.14879968 | -0.24805898 | 252.48 | 55866.7917592593 | 55867.6946990741 | 506020010 | 40686.9 | 40000 | 40686.9 | 40694.9 | 0 | 40694.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40051.3 | 40051.3 | 78011.9 | 0 | PROCESSED | 57603.6841435185 | 56246 | 55879.1725 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060061 | Many TeV gamma-ray objects discovered on the Galactic plane are classified as pulsar wind nebulae (PWNe), just because there exists a pulsar in the vicinity of them. X-ray observations can directly show the physical connection between the TeV emission and PWNe by presenting the existence of X-ray PWNe. HESSJ1857 and HESSJ1832 are unidentified TeV objects, but they may be TeV PWNe driven by pulsars close to them. We propose to observe them to study whether the pulsars have X-ray PWNe or not. | GALACTIC DIFFUSE EMISSION | 5 | B | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 6 | AO6 | ARE THE TEV UNIDENTIFIED OBJECTS, HESSJ1857+026 AND HESSJ1832-084, PULSAR WIND NEBULAE? | XIS | Y |
| HESSJ1832 | 278.156 | -8.4222 | 23.29856204 | 0.30967904 | 88.1963 | 55659.2543518518 | 55660.3454282407 | 506021010 | 40343.2 | 40000 | 40343.2 | 40343.2 | 0 | 40343.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34851.3 | 34851.3 | 94257.8 | 1 | PROCESSED | 57601.464224537 | 56043 | 55673.2950925926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060061 | Many TeV gamma-ray objects discovered on the Galactic plane are classified as pulsar wind nebulae (PWNe), just because there exists a pulsar in the vicinity of them. X-ray observations can directly show the physical connection between the TeV emission and PWNe by presenting the existence of X-ray PWNe. HESSJ1857 and HESSJ1832 are unidentified TeV objects, but they may be TeV PWNe driven by pulsars close to them. We propose to observe them to study whether the pulsars have X-ray PWNe or not. | GALACTIC DIFFUSE EMISSION | 5 | B | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 6 | AO6 | ARE THE TEV UNIDENTIFIED OBJECTS, HESSJ1857+026 AND HESSJ1832-084, PULSAR WIND NEBULAE? | XIS | Y |
| 3C 59 VICINITY 1 | 32.0992 | 30.0806 | 142.1363254 | -29.90513458 | 254.1341 | 55940.8410763889 | 55942.215474537 | 506024010 | 55858.1 | 50000 | 55858.1 | 55858.1 | 0 | 55858.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46040.4 | 46040.4 | 118737.9 | 1 | PROCESSED | 57604.3853356482 | 56331 | 55960.1998032407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060067 | We propose for an observation of the vicinities of 3C 59, in order to study the radial extent of the Galactic hot gas. We have conducted joint analysis of absorption and emission lines toward several targets until now and successfully constrained the temperature, line-of-sight length, and density of the hot gas of the directions. However, all the line-of-sight lengths of the hot gas for the past surveys stay within the Galactic disc with the radius of 10 kpc, therefore the radial extent of the gas is still unknown. Emission analysis of low-latitude and almost anti-center directed 3C 59 will constrain the extent, and the result will be unambiguous when emission and absorption lines are jointly analyzed. | GALACTIC DIFFUSE EMISSION | 5 | C | SAKAI | KAZUHIRO | NULL | NULL | JAP | 6 | AO6 | STUDY OF RADIAL DISTRIBUTION OF THE HOT INTERSTELLAR MEDIUM | XIS | Y |
| 3C 59 VICINITY 2 | 31.4351 | 28.9234 | 141.95387958 | -31.18906496 | 250.3 | 55952.5116435185 | 55957.4238773148 | 506025010 | 173347 | 50000 | 173347 | 173355 | 0 | 173355 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 547.9 | 547.9 | 86854 | 0 | PROCESSED | 57604.5146759259 | 56526 | 56167.6426388889 | 3.0.22.44 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060067 | We propose for an observation of the vicinities of 3C 59, in order to study the radial extent of the Galactic hot gas. We have conducted joint analysis of absorption and emission lines toward several targets until now and successfully constrained the temperature, line-of-sight length, and density of the hot gas of the directions. However, all the line-of-sight lengths of the hot gas for the past surveys stay within the Galactic disc with the radius of 10 kpc, therefore the radial extent of the gas is still unknown. Emission analysis of low-latitude and almost anti-center directed 3C 59 will constrain the extent, and the result will be unambiguous when emission and absorption lines are jointly analyzed. | GALACTIC DIFFUSE EMISSION | 5 | C | SAKAI | KAZUHIRO | NULL | NULL | JAP | 6 | AO6 | STUDY OF RADIAL DISTRIBUTION OF THE HOT INTERSTELLAR MEDIUM | XIS | Y |
| MBM12 | 43.9954 | 19.5008 | 159.17119109 | -34.46234987 | 73.4994 | 55776.7501388889 | 55780.4398263889 | 506026010 | 150320.2 | 150000 | 150320.2 | 150320.2 | 0 | 150320.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 143534.9 | 143534.9 | 280761.8 | 5 | PROCESSED | 57602.8321180556 | 56169 | 55802.465625 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060068 | We propose an observation toward dense molecular cloud region MBM12 that is in front of the Local Hot Bubble. Solar wind charge exchange induced emission, reacted with neutrals in the heliosphere (H-SWCX), is considered to have significant influence to the soft diffuse X-ray background under 1 keV. However, there is no significant evidence of the H-SWCX. From this observation, we try to reveal the existence of H-SWCX induced emission by comparing the OVII line emission (0.57 keV) with Suzaku archive data. We also aim to constrain the time variability of H-SWCX emission, depending on the 12 year solar activity. | GALACTIC DIFFUSE EMISSION | 5 | A | YOSHITAKE | HIROSHI | NULL | NULL | JAP | 6 | AO6 | OBSERVATION TOWARD MOLECULAR CLOUD MBM12 : VERIFYING SOLAR WIND CHARGE EXCHANGE EMISSION IN THE HELIOSPHERE | XIS | Y |
| NGC 7618 | 349.8326 | 42.9144 | 105.51742003 | -16.82119292 | 269.9991 | 55911.4056828704 | 55913.6161458333 | 506027010 | 101177.2 | 100000 | 101185.2 | 101177.2 | 0 | 101185.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 95774 | 95774 | 190939.9 | 0 | PROCESSED | 57604.196712963 | 56289 | 55922.1112847222 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060073 | We propose to observe nearby merging galaxy group NGC 7618. The asymmetric X-ray shape with a tail and a sharp brightness discontinuity were discoverd by observations of ASCA and Chandra. This is due to a merging with an another galaxy group, UGC 12491, which has similar mass of NGC 7618. The pair is in the primary stage of merging, then we need to obtain the information of the gas outside region to clarify the process of the merging. By taking advantage of low background and high energy resolution of XIS, we estimate accurately distribuion of temperature and metal abundances around both galaxy groups. Then we aim to clarify the process of the merging system of the galaxy groups. | GALACTIC DIFFUSE EMISSION | 5 | C | HAYASHI | KATSUHIRO | NULL | NULL | JAP | 6 | AO6 | OBSERVATION OF NEARBY MERGING GALAXY GROUP NGC 7618 | XIS | Y |
| H2356_VICINITY_A | 359.8969 | -30.2089 | 14.71906615 | -78.22459894 | 68.0006 | 55696.8464583333 | 55698.0938773148 | 506028010 | 52165.7 | 50000 | 52165.7 | 52165.7 | 0 | 52165.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46579.1 | 46579.1 | 107753.9 | 1 | PROCESSED | 57602.0723148148 | 56075 | 55708.0697106482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060075 | We propose to observe the two vicinities of H2356-309 for 50 ks each. Absorption lines from ions at z=0 and z=0.03 has been observed with grating spectrometers in the spectrum of H2356-309. Emission analysis with Suzaku will provide independent information on the medium responsible for the absorption lines. By combining the emission surface brightness and aborption equivalent width, we will constrain the temperature and physical length of the interstellar and intergalactic medium. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKEI | YOH | NULL | NULL | JAP | 6 | AO6 | EMISSION/ABSORPTION COMBINATION STUDY OF GALACTIC AND INTERGALACTIC WARM-HOT GAS | XIS | Y |
| H2356_VICINITY_B | 359.9868 | -29.9493 | 15.89682365 | -78.35224854 | 69.5008 | 55698.0951388889 | 55699.3474305556 | 506029010 | 51407.2 | 50000 | 51431.2 | 51423.2 | 0 | 51407.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42546 | 42546 | 108155.9 | 1 | PROCESSED | 57602.0868402778 | 56075 | 55708.1035069444 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060075 | We propose to observe the two vicinities of H2356-309 for 50 ks each. Absorption lines from ions at z=0 and z=0.03 has been observed with grating spectrometers in the spectrum of H2356-309. Emission analysis with Suzaku will provide independent information on the medium responsible for the absorption lines. By combining the emission surface brightness and aborption equivalent width, we will constrain the temperature and physical length of the interstellar and intergalactic medium. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKEI | YOH | NULL | NULL | JAP | 6 | AO6 | EMISSION/ABSORPTION COMBINATION STUDY OF GALACTIC AND INTERGALACTIC WARM-HOT GAS | XIS | Y |
| S147_NE | 85.8826 | 28.3008 | 180.30181638 | -0.72311498 | 273.9004 | 55996.1741666667 | 55997.2919097222 | 506030010 | 48014.2 | 45000 | 48030.2 | 48014.2 | 0 | 48038.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42608 | 42608 | 96555.9 | 0 | PROCESSED | 57604.8622685185 | 56385 | 56016.6658912037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060080 | We propose to observe the very old supernova remnant (SNR) S147 with Suzaku/XIS. S147 has a jet like structure suggesting that it was a core collapse supernova. The formation mechanism of the jet remains unclear for the progenitor which has a small mass and creates a neutron star by its explosion. An asymmetric explosion causes a inhomogeneous metallicity abundance. Therefore, we investigate the inhomogeneous by the plasma diagnosis in the X-ray band to obtain the evidence of the jet formation. This will be the limit of theoretical model for the supernova explosion. S147 is also the GeV gamma-ray source. Therefore, we can study the acceleration mechanism of the cosmic rays in the very old SNR if we detect the nonthermal X-ray emission from it. | GALACTIC DIFFUSE EMISSION | 5 | C | HANABATA | YOSHITAKA | NULL | NULL | JAP | 6 | AO6 | STUDYING THE SUPERNOVA REMNANT S147 WITH JET STRUCTURE AND GEV GAMMA-RAY EMISSION | XIS | Y |
| S147_N | 87.0463 | 27.5187 | 181.50494456 | -0.25223067 | 273.8998 | 55997.2930324074 | 55998.555787037 | 506031010 | 54883.3 | 55000 | 54891.3 | 54883.3 | 0 | 54891.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 52191.9 | 52191.9 | 109054 | 1 | PROCESSED | 57604.8728472222 | 56385 | 56016.6668287037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060080 | We propose to observe the very old supernova remnant (SNR) S147 with Suzaku/XIS. S147 has a jet like structure suggesting that it was a core collapse supernova. The formation mechanism of the jet remains unclear for the progenitor which has a small mass and creates a neutron star by its explosion. An asymmetric explosion causes a inhomogeneous metallicity abundance. Therefore, we investigate the inhomogeneous by the plasma diagnosis in the X-ray band to obtain the evidence of the jet formation. This will be the limit of theoretical model for the supernova explosion. S147 is also the GeV gamma-ray source. Therefore, we can study the acceleration mechanism of the cosmic rays in the very old SNR if we detect the nonthermal X-ray emission from it. | GALACTIC DIFFUSE EMISSION | 5 | C | HANABATA | YOSHITAKA | NULL | NULL | JAP | 6 | AO6 | STUDYING THE SUPERNOVA REMNANT S147 WITH JET STRUCTURE AND GEV GAMMA-RAY EMISSION | XIS | Y |
| CTB1_SW | 359.716 | 62.4332 | 116.89133919 | 0.1796486 | 252.1748 | 55924.1262037037 | 55924.6251736111 | 506034010 | 28941.9 | 50000 | 28941.9 | 28949.9 | 0 | 28949.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25385 | 25385 | 43108 | 0 | PROCESSED | 57604.2594675926 | 56313 | 55972.6473958333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060086 | CTB 1 is an old (9 - 44 thousand years) galactic supernova remnant (SNR). The ASCA observation of CTB 1 suggested a hard X-ray emission in the 3 - 10 keV band. The hard emission may be originated in synchrotron radiation (non-thermal) or in thermal bremsstrahlung (kT ~ 3 keV). In the case of the non-thermal origin, the old SNR still accelerate electrons up to 100 TeV. On the other hand, the thermal origin indicates that very hot plasma is still kept in such an old SNR. In order to clean up the nature of the hard emission which would give a large impact for the mechanism of particle acceleration and SNR evolution, we propose the Suzaku observation of CTB 1. | GALACTIC DIFFUSE EMISSION | 5 | C | NAKASHIMA | SHINYA | NULL | NULL | JAP | 6 | AO6 | NON-THERMAL EMISSION FROM THE MOST ANCIENT SUPERNOVA REMNANT | XIS | Y |
| CTB1_NE | 0.2869 | 62.6043 | 117.18345572 | 0.29518062 | 253.7193 | 55923.0281134259 | 55924.1251736111 | 506035010 | 52666 | 50000 | 52666 | 52666 | 0 | 52666 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48310.8 | 48310.8 | 94775.9 | 3 | PROCESSED | 57604.2722569444 | 56313 | 55972.6734490741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060086 | CTB 1 is an old (9 - 44 thousand years) galactic supernova remnant (SNR). The ASCA observation of CTB 1 suggested a hard X-ray emission in the 3 - 10 keV band. The hard emission may be originated in synchrotron radiation (non-thermal) or in thermal bremsstrahlung (kT ~ 3 keV). In the case of the non-thermal origin, the old SNR still accelerate electrons up to 100 TeV. On the other hand, the thermal origin indicates that very hot plasma is still kept in such an old SNR. In order to clean up the nature of the hard emission which would give a large impact for the mechanism of particle acceleration and SNR evolution, we propose the Suzaku observation of CTB 1. | GALACTIC DIFFUSE EMISSION | 5 | C | NAKASHIMA | SHINYA | NULL | NULL | JAP | 6 | AO6 | NON-THERMAL EMISSION FROM THE MOST ANCIENT SUPERNOVA REMNANT | XIS | Y |
| W28WEST | 269.8372 | -23.6072 | 6.15250357 | 0.06606197 | 270.1135 | 55844.0583217593 | 55848.1342708333 | 506036010 | 151089.2 | 150000 | 151097.2 | 151089.2 | 0 | 151092.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 128979.7 | 128979.7 | 352125.9 | 2 | PROCESSED | 57603.4758449074 | 56240 | 55872.5113425926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060095 | W28 is a mixed-morphology supernova remnant (MM SNR). Recently, GeV and TeV gamma-ray emission have been detected from the eastern edge of W28. On the other hand, we have observed the central region of W28 and have detected an over-ionized plasma, which can not be produced in the canonical evolution of SNRs. Several SNRs have been turned out to host a over-ionized plasma. All of them are MM SNR and are showing GeV and/or TeV emission. This indicates that there are some physical connections between the existence of high-energy cosmic rays and over-ionized plasma. W28 is the best place to study this possible connection due to the large apparent size. Thus, we propose Suzaku observation of western region of W28, which has not been covered by the previous mapping observations. | GALACTIC DIFFUSE EMISSION | 5 | A | SAWADA | MAKOTO | NULL | NULL | JAP | 6 | AO6 | THE SNR W28 - SEARCHING FOR THE PHYSICAL CONNECTION BETWEEN HIGH-ENERGY COSMIC RAYS AND OVER-IONIZED PLASMA | XIS | Y |
| CTB109 NOTHWEST | 345.2638 | 59.0349 | 109.14185824 | -0.84931137 | 252.0017 | 55908.2838078704 | 55909.1988078704 | 506037010 | 40748.8 | 40000 | 40748.8 | 40756.8 | 0 | 40764.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39201 | 39201 | 79044 | 0 | PROCESSED | 57604.1345601852 | 56288 | 55921.0397685185 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060100 | Supernova remnant CTB109 with AX 1E 2259+586 are suitable object which allows us to get infomation of magnetas formations. | GALACTIC DIFFUSE EMISSION | 5 | C | NAKANO | TOSHIO | NULL | NULL | JAP | 6 | AO6 | SUPERNOVA REMNANT CTB109 ASSOCIATED WITH AX 1E 2259+586 | XIS | Y |
| CTB109 SOUTHWEST | 345.0971 | 58.7572 | 108.94859975 | -1.06655489 | 252.0045 | 55909.1993287037 | 55910.0807407407 | 506038010 | 41382.4 | 40000 | 41390.4 | 41382.4 | 0 | 41398.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38779 | 38779 | 76135.8 | 0 | PROCESSED | 57604.1454282407 | 56289 | 55921.9811574074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060100 | Supernova remnant CTB109 with AX 1E 2259+586 are suitable object which allows us to get infomation of magnetas formations. | GALACTIC DIFFUSE EMISSION | 5 | C | NAKANO | TOSHIO | NULL | NULL | JAP | 6 | AO6 | SUPERNOVA REMNANT CTB109 ASSOCIATED WITH AX 1E 2259+586 | XIS | Y |
| CTB109 NORTHEAST | 345.764 | 59.0015 | 109.36320905 | -0.98507066 | 252.0025 | 55910.0815393518 | 55910.7522106482 | 506039010 | 30405.8 | 30000 | 30405.8 | 30405.8 | 0 | 30405.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30747.3 | 30747.3 | 57921.9 | 1 | PROCESSED | 57604.1437268518 | 56289 | 55921.9865277778 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060100 | Supernova remnant CTB109 with AX 1E 2259+586 are suitable object which allows us to get infomation of magnetas formations. | GALACTIC DIFFUSE EMISSION | 5 | C | NAKANO | TOSHIO | NULL | NULL | JAP | 6 | AO6 | SUPERNOVA REMNANT CTB109 ASSOCIATED WITH AX 1E 2259+586 | XIS | Y |
| CTB109 SOUTHEAST | 345.764 | 58.7015 | 109.24155205 | -1.25930647 | 252.0022 | 55910.7526851852 | 55911.4007638889 | 506040010 | 30445.5 | 30000 | 30445.5 | 30445.5 | 0 | 30445.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28751.1 | 28751.1 | 55987.9 | 1 | PROCESSED | 57604.1444212963 | 56289 | 55922.0080555556 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060100 | Supernova remnant CTB109 with AX 1E 2259+586 are suitable object which allows us to get infomation of magnetas formations. | GALACTIC DIFFUSE EMISSION | 5 | C | NAKANO | TOSHIO | NULL | NULL | JAP | 6 | AO6 | SUPERNOVA REMNANT CTB109 ASSOCIATED WITH AX 1E 2259+586 | XIS | Y |
| VELA PWN NE1 | 129.3684 | -44.9817 | 263.62243766 | -2.36980886 | 142.6395 | 55916.6230439815 | 55917.0070601852 | 506041010 | 15408 | 15000 | 15424 | 15408 | 0 | 15424 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11568.1 | 11568.1 | 33175.9 | 1 | PROCESSED | 57604.1925347222 | 56305 | 55937.7788310185 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061302 | Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles. | GALACTIC DIFFUSE EMISSION | 5 | C | KATSUDA | SATORU | NULL | NULL | USA | 6 | AO6 | THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA | XIS | Y |
| VELA PWN NE2 | 130.6211 | -44.2844 | 263.6136326 | -1.23809583 | 141.8635 | 55917.0080439815 | 55917.6126273148 | 506042010 | 18514 | 15000 | 18538 | 18514 | 0 | 18514 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16875.5 | 16875.5 | 52225.9 | 0 | PROCESSED | 57604.2062962963 | 56305 | 55937.7869212963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061302 | Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles. | GALACTIC DIFFUSE EMISSION | 5 | C | KATSUDA | SATORU | NULL | NULL | USA | 6 | AO6 | THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA | XIS | Y |
| VELA PWN NE3 | 131.0442 | -44.0836 | 263.64329985 | -0.87547181 | 123.9937 | 55895.188900463 | 55895.621724537 | 506043010 | 17799.9 | 15000 | 17806.6 | 17799.9 | 0 | 17806.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13012 | 13012 | 37395.9 | 0 | PROCESSED | 57604.0129050926 | 56274 | 55907.1603703704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061302 | Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles. | GALACTIC DIFFUSE EMISSION | 5 | C | KATSUDA | SATORU | NULL | NULL | USA | 6 | AO6 | THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA | XIS | Y |
| VELA PWN E1 | 129.1398 | -45.2732 | 263.75797839 | -2.67419196 | 142.334 | 55916.0561226852 | 55916.622337963 | 506044010 | 17718 | 15000 | 17718 | 17718 | 0 | 17718 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16628.4 | 16628.4 | 48895.9 | 0 | PROCESSED | 57604.1814814815 | 56305 | 55937.7696527778 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061302 | Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles. | GALACTIC DIFFUSE EMISSION | 5 | C | KATSUDA | SATORU | NULL | NULL | USA | 6 | AO6 | THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA | XIS | Y |
| VELA PWN E2 | 129.5733 | -45.3227 | 263.98172095 | -2.46094632 | 304.5019 | 55711.9038773148 | 55712.1328935185 | 506045010 | 13904 | 15000 | 13920 | 13904 | 0 | 13920 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8404 | 8404 | 19775.9 | 0 | PROCESSED | 57602.1624074074 | 56092 | 55725.2563888889 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061302 | Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles. | GALACTIC DIFFUSE EMISSION | 5 | B | KATSUDA | SATORU | NULL | NULL | USA | 6 | AO6 | THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA | XIS | Y |
| VELA PWN E3 | 129.9962 | -45.3672 | 264.19786494 | -2.25193357 | 304.5033 | 55712.1335069444 | 55712.4099305556 | 506046010 | 14178.7 | 15000 | 14202.7 | 14194.7 | 0 | 14178.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12659.9 | 12659.9 | 23875.9 | 0 | PROCESSED | 57602.1638078704 | 56093 | 55725.9978240741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061302 | Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles. | GALACTIC DIFFUSE EMISSION | 5 | B | KATSUDA | SATORU | NULL | NULL | USA | 6 | AO6 | THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA | XIS | Y |
| VELA PWN E4 | 130.4202 | -45.4045 | 264.40968594 | -2.03918199 | 304.5026 | 55712.4105902778 | 55712.7362268518 | 506047010 | 17031.4 | 15000 | 17035.4 | 17054.9 | 0 | 17031.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15107.8 | 15107.8 | 28128 | 0 | PROCESSED | 57602.173900463 | 56093 | 55726.0290046296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061302 | Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles. | GALACTIC DIFFUSE EMISSION | 5 | B | KATSUDA | SATORU | NULL | NULL | USA | 6 | AO6 | THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA | XIS | Y |
| VELA PWN E5 | 130.8405 | -45.4455 | 264.62375514 | -1.83200273 | 304.5067 | 55712.7368402778 | 55712.9570601852 | 506048010 | 15919.6 | 15000 | 15919.6 | 15919.6 | 0 | 15943.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11912.9 | 11912.9 | 19015.9 | 0 | PROCESSED | 57602.1724305556 | 56093 | 55726.0610185185 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061302 | Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles. | GALACTIC DIFFUSE EMISSION | 5 | B | KATSUDA | SATORU | NULL | NULL | USA | 6 | AO6 | THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA | XIS | Y |
| VELA PWN E6 | 131.2685 | -45.4809 | 264.83769354 | -1.61837696 | 304.5065 | 55712.9576273148 | 55713.2292939815 | 506049010 | 18196.8 | 15000 | 18204.8 | 18196.8 | 0 | 18212.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14209 | 14209 | 23469.9 | 0 | PROCESSED | 57602.1814699074 | 56103 | 55735.9387268518 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061302 | Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles. | GALACTIC DIFFUSE EMISSION | 5 | B | KATSUDA | SATORU | NULL | NULL | USA | 6 | AO6 | THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA | XIS | Y |
| VELA PWN E7 | 131.6969 | -45.5129 | 265.05012769 | -1.40367097 | 303.5042 | 55713.2300925926 | 55713.4688310185 | 506050010 | 13045.4 | 15000 | 13049.4 | 13045.4 | 0 | 13053.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11075.1 | 11075.1 | 20622 | 0 | PROCESSED | 57602.181875 | 56093 | 55726.0999768518 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061302 | Located only ~290 pc from Earth, the Vela PWN is one of the best targets for the study of PWNe. Its radio and gamma-ray surface brightness peaks to the south of the pulsar, suggesting that the nebula was crushed by the reverse shock which propagated more rapidly from the north than the south through an inhomogeneous ambient medium. The X-ray morphology is not yet known. Recently, we found that the X-ray extent is larger than the radio extent in the northeastern and eastern directions. We here propose ten Suzaku XIS observations in these two directions to study the history of the Vela PWN; for instance, to investigate whether the radio-emitting PWN is the relic of PWN-reverse shock interactions, whereas the X-ray-emitting PWN is more recently formed by freshly injected particles. | GALACTIC DIFFUSE EMISSION | 5 | B | KATSUDA | SATORU | NULL | NULL | USA | 6 | AO6 | THE X-RAY MORPHOLOGY OF THE VELA PULSAR WIND NEBULA | XIS | Y |
| G18.8+0.3 | 275.9435 | -12.3781 | 18.78460262 | 0.39706413 | 83.4994 | 55994.9180324074 | 55996.1598958333 | 506051010 | 52020.5 | 50000 | 52020.5 | 52028.5 | 0 | 52036.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44882 | 44882 | 107263.9 | 1 | PROCESSED | 57604.8541435185 | 56382 | 56016.6717708333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061311 | We propose a 50 ks exploratory observation of an interesting first-quadrant supernova remnant, G18.8+0.3, for which radio-continuum and CO data indicate interaction with a molecular cloud. Prior X-ray studies are limited to a 14 ks ROSAT PSPC observation producing about 500 counts. We expect about 12,000 counts with Suzaku, which should permit basic characterization of the spectrum and morphology of X-rays: shell-type, mixed-morphology (central thermal emission) or even composite (central PWN). Spectral analysis will allow us to determine or estimate shock speed, age, ambient density, and swept-up mass. As more middle-aged remnants are found to have unusual properties such as GeV-TeV emission, the study of objects like G18.8+0.3 assumes greater importance. | GALACTIC DIFFUSE EMISSION | 5 | C | REYNOLDS | STEPHEN | NULL | NULL | USA | 6 | AO6 | G18.8+0.3: A SUPERNOVA REMNANT WITH STRONG MOLECULAR INTERACTION | XIS | Y |
| G352.7-0.1 | 261.9227 | -35.1119 | 352.75195989 | -0.12120729 | 94.0335 | 55988.8605671296 | 55993.5536111111 | 506052010 | 201547.4 | 200000 | 201547.4 | 201547.4 | 0 | 201547.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 171544 | 171544 | 405439.6 | 4 | PROCESSED | 57604.9422569445 | 56375 | 56008.397337963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061315 | Supernova remnants showing strong Fe K emission are relatively rare, and primarily of Type Ia. We propose a long observation of one of the least well-studied Fe-rich Galactic SNRs, G352.7-0.1, with the goal of characterizing the Fe emission, confirming its likely identification as the remnant of a Type Ia supernova, and constraining the properties of ejected material and the dynamics of the explosion. Its thermal X-ray spectrum is strikingly similar to Tycho's SNR, but unexpectedly X-rays are uniformly distributed throughout the remnant. Our proposed observation will produce high-quality spectra, adequate for detailed studies with some spatial information, that will greatly aid in understanding of this very interesting young remnant. | GALACTIC DIFFUSE EMISSION | 5 | C | BORKOWSKI | KAZIMIERZ | NULL | NULL | USA | 6 | AO6 | STRONG IRON EMISSION IN THE SUPERNOVA REMNANT G352.7-0.1 | XIS | Y |
| MONOGEM RING W1 | 100.4191 | 15.2834 | 198.20484712 | 4.79777248 | 269.9998 | 55998.5603356482 | 56000.0002314815 | 506053010 | 61126.6 | 60000 | 61126.7 | 61126.6 | 0 | 61126.6 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 59074 | 59074 | 124373.9 | 1 | PROCESSED | 57604.899849537 | 56382 | 56016.6737152778 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061316 | We propose to observe the oldest, nearby SNR, the Monogem Ring, with the Suzaku XIS to study the plasma conditions in two locations which are near the Galactic plane and where there is evidence of a significant interaction with cooler (10^4 - 10^5 K), denser material. We chose one pointing where the turbulent mixing of hot and cooler gas should be large, and an adjacent pointing where the mixing should be small. From our previous Suzaku observation at a region far from the plane, we derived an ionization timescale for the non-equilibrium plasma which is apparently inconsistent with the age of the SNR. Our proposed observations will allow a detailed comparison of the plasma conditions in these regions with very different histories, and initial and current conditions. | GALACTIC DIFFUSE EMISSION | 5 | C | PLUCINSKY | PAUL | NULL | NULL | USA | 6 | AO6 | STUDYING THE PLASMA EVOLUTION IN THE MONOGEM RING | XIS | Y |
| MONOGEM RING W2 | 97.483 | 17.0349 | 195.35325463 | 3.08684005 | 270 | 56001.1430439815 | 56002.5487384259 | 506054010 | 62593.3 | 60000 | 62593.3 | 62593.3 | 0 | 62593.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 59966.9 | 59966.9 | 121443.9 | 1 | PROCESSED | 57604.9251967593 | 56385 | 56019.3467592593 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061316 | We propose to observe the oldest, nearby SNR, the Monogem Ring, with the Suzaku XIS to study the plasma conditions in two locations which are near the Galactic plane and where there is evidence of a significant interaction with cooler (10^4 - 10^5 K), denser material. We chose one pointing where the turbulent mixing of hot and cooler gas should be large, and an adjacent pointing where the mixing should be small. From our previous Suzaku observation at a region far from the plane, we derived an ionization timescale for the non-equilibrium plasma which is apparently inconsistent with the age of the SNR. Our proposed observations will allow a detailed comparison of the plasma conditions in these regions with very different histories, and initial and current conditions. | GALACTIC DIFFUSE EMISSION | 5 | C | PLUCINSKY | PAUL | NULL | NULL | USA | 6 | AO6 | STUDYING THE PLASMA EVOLUTION IN THE MONOGEM RING | XIS | Y |
| G236+38 ON | 146.5345 | 0.5057 | 235.93345442 | 38.21375915 | 307.3884 | 55713.4761574074 | 55715.0002314815 | 506055010 | 69802.5 | 70000 | 69802.5 | 69802.5 | 0 | 69802.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 64348.8 | 64348.8 | 131674 | 0 | PROCESSED | 57602.2264351852 | 56127 | 55757.6954050926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061321 | Interstellar clouds cast shadows in the soft X-ray background (SXRB). Observations of these shadows enable us to disentangle the various components of the SXRB. Unfortunately, to date, shadowing observations with XMM or Suzaku have only been published for three directions, all in the southern Galactic hemisphere. We propose two new pairs of on- and off-cloud shadowing observations, in order to sample the northern Galactic hemisphere. Our particular goal is to obtain accurate X-ray spectra of the Galactic halo, which we will compare with the predictions of models of galactic fountains and infalling extragalactic material. | GALACTIC DIFFUSE EMISSION | 5 | B | HENLEY | DAVID | NULL | NULL | USA | 6 | AO6 | UNDERSTANDING THE ORIGIN OF THE GALACTIC HALO USING SHADOWING OBSERVATIONS | XIS | Y |
| G236+38 OFF | 149.4117 | 1.4719 | 237.07053965 | 41.11953464 | 293.1755 | 55719.6375462963 | 55721.2780092593 | 506056010 | 70813.5 | 70000 | 70821.5 | 70829.5 | 0 | 70813.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 64444.4 | 64444.4 | 141727.8 | 0 | PROCESSED | 57602.2364583333 | 56127 | 55757.6968518518 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061321 | Interstellar clouds cast shadows in the soft X-ray background (SXRB). Observations of these shadows enable us to disentangle the various components of the SXRB. Unfortunately, to date, shadowing observations with XMM or Suzaku have only been published for three directions, all in the southern Galactic hemisphere. We propose two new pairs of on- and off-cloud shadowing observations, in order to sample the northern Galactic hemisphere. Our particular goal is to obtain accurate X-ray spectra of the Galactic halo, which we will compare with the predictions of models of galactic fountains and infalling extragalactic material. | GALACTIC DIFFUSE EMISSION | 5 | B | HENLEY | DAVID | NULL | NULL | USA | 6 | AO6 | UNDERSTANDING THE ORIGIN OF THE GALACTIC HALO USING SHADOWING OBSERVATIONS | XIS | Y |
| VELAFRAGG TAIL | 125.0448 | -47.7009 | 264.09848727 | -6.37839252 | 263.1844 | 55658.0366898148 | 55658.8565162037 | 506057010 | 49354.3 | 50000 | 49370.3 | 49354.3 | 0 | 49370.3 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 43958.1 | 43958.1 | 70825.9 | 1 | PROCESSED | 57601.4287268518 | 56043 | 55673.1976736111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 062021 | The Vela supernova remnant (SNR) displays remarkable features which appear to be ejecta ``shrapnel'' visible beyond the main shell. One of these shrapnel (A) is distinct from the others in that its X-ray spectrum exhibits a high Si abundance, while the other shrapnel exhibit enhanced O, Ne, and Mg abundances. One unexplored ejecta shrapnel (G) is located on the opposite side of the remnant from shrapnel A, suggesting that the SN explosion may have resulted in a jet-counterjet Si-rich structure, reminiscent of Cas A. We propose to observe this shrapnel for the first time to determine if it is also Si-rich like shrapnel A. If this is the case, the Vela SNR may be the first direct evidence of a jet-induced SN explosion. | GALACTIC DIFFUSE EMISSION | 5 | A | BOCCHINO | FABRIZIO | NULL | NULL | EUR | 6 | AO6 | ASYMMETRIC SN EXPLOSION IN VELA SNR | XIS | Y |
| KES 79 | 283.1953 | 0.6959 | 33.70438491 | 0.01846016 | 73.5801 | 55674.9437152778 | 55676.4716782407 | 506059010 | 50897 | 50000 | 50897 | 50897 | 0 | 50897 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40897.8 | 40897.8 | 131960 | 2 | PROCESSED | 57601.597025463 | 55652 | 55697.1427083333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066001 | Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 6 | AO6-KP | NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS | XIS | Y |
| G272.2-3.2 | 136.7114 | -52.1231 | 272.22308022 | -3.18374401 | 297.1287 | 55709.5476041667 | 55711.9009490741 | 506060010 | 130078.2 | 150000 | 130086.2 | 130094.2 | 0 | 130078.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 121830.3 | 121830.3 | 203305.8 | 3 | PROCESSED | 57602.216087963 | 55652 | 55735.3493171296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066001 | Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 6 | AO6-KP | NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS | XIS | Y |
| G272.2-3.2 | 136.7067 | -52.1223 | 272.22054405 | -3.18534238 | 101.7643 | 55877.9477777778 | 55878.6272916667 | 506060020 | 25526.5 | 20000 | 25534.5 | 25534.5 | 0 | 25526.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27028 | 27028 | 58706 | 0 | PROCESSED | 57603.7829282407 | 55652 | 55895.0737962963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066001 | Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 6 | AO6-KP | NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS | XIS | Y |
| G290.1-0.8 | 165.7447 | -60.8884 | 290.11957377 | -0.7436408 | 293.2659 | 55737.4551388889 | 55740.5883333333 | 506061010 | 110593.1 | 110000 | 110609.1 | 110593.1 | 0 | 110601.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 99359.6 | 99359.6 | 270659.6 | 4 | PROCESSED | 57602.4993634259 | 55652 | 55775.3693287037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066001 | Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 6 | AO6-KP | NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS | XIS | Y |
| G292.0+1.8 | 171.1489 | -59.2723 | 292.03159099 | 1.74911685 | 309.5957 | 55764.9604050926 | 55765.6883449074 | 506062010 | 43659.2 | 40000 | 43659.2 | 43659.2 | 0 | 43659.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40236.4 | 40236.4 | 62885.9 | 1 | PROCESSED | 57602.6430902778 | 55652 | 55785.0141782407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066001 | Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 6 | AO6-KP | NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS | XIS | Y |
| KES 27 | 237.1872 | -53.7777 | 327.32071311 | 0.47884394 | 101.6269 | 55983.5400231482 | 55985.4633217593 | 506063010 | 109353.5 | 120000 | 109401.5 | 109353.5 | 0 | 109401.5 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 115332.1 | 115332.1 | 166148 | 4 | PROCESSED | 57604.7717592593 | 55652 | 55995.1904976852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066001 | Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 6 | AO6-KP | NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS | XIS | Y |
| G349.7+0.2 | 259.4954 | -37.4452 | 349.72102569 | 0.17051597 | 282.4112 | 55833.4324537037 | 55838.1341898148 | 506064010 | 160402.4 | 160000 | 160426.4 | 160402.4 | 0 | 160434.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 144615.1 | 144615.1 | 404220 | 5 | PROCESSED | 57603.3931134259 | 55652 | 55858.5356018518 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066001 | Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 6 | AO6-KP | NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS | XIS | Y |
| G350.1-0.3 | 260.2697 | -37.4549 | 350.06545974 | -0.33871818 | 266.4234 | 55821.2580787037 | 55822.9126388889 | 506065010 | 70181.3 | 70000 | 70197.3 | 70181.3 | 0 | 70197.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 60070.4 | 60070.4 | 142915.9 | 0 | PROCESSED | 57603.2088541667 | 55652 | 55865.2679282407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066001 | Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 6 | AO6-KP | NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS | XIS | Y |
| FERMI_BUBBLE_N1 | 234.2494 | 5.0833 | 11.24626366 | 44.86747445 | 287.5001 | 56144.9615277778 | 56145.3981365741 | 507001010 | 21048.5 | 20000 | 21048.5 | 21048.5 | 0 | 21048.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17527.5 | 17527.5 | 37719.9 | 1 | PROCESSED | 57606.7753703704 | 56533 | 56167.2004166667 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070006 | Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model. | GALACTIC DIFFUSE EMISSION | 5 | A | KATAOKA | JUN | NULL | NULL | JAP | 7 | AO7 | SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER | XIS | Y |
| FERMI_BUBBLE_N2 | 234.4045 | 4.1242 | 10.25580888 | 44.20015183 | 287.5 | 56145.3990740741 | 56145.971099537 | 507002010 | 22491 | 20000 | 22491 | 22491 | 0 | 22491 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22500 | 22500 | 49405.9 | 0 | PROCESSED | 57606.7805555556 | 56630 | 56264.5602662037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070006 | Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model. | GALACTIC DIFFUSE EMISSION | 5 | A | KATAOKA | JUN | NULL | NULL | JAP | 7 | AO7 | SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER | XIS | Y |
| FERMI_BUBBLE_N3 | 234.0339 | 6.0902 | 12.27048516 | 45.60209416 | 287.4996 | 56145.9724537037 | 56146.4377893518 | 507003010 | 22484.6 | 20000 | 22484.6 | 22508.6 | 0 | 22492.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19836 | 19836 | 40195.9 | 0 | PROCESSED | 57606.7866782407 | 56535 | 56169.009837963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070006 | Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model. | GALACTIC DIFFUSE EMISSION | 5 | A | KATAOKA | JUN | NULL | NULL | JAP | 7 | AO7 | SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER | XIS | Y |
| FERMI_BUBBLE_N4 | 233.8333 | 7.0797 | 13.3126084 | 46.30488493 | 287.5 | 56146.4387268518 | 56146.9862615741 | 507004010 | 20946.9 | 20000 | 20950.9 | 20946.9 | 0 | 20954.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20704.8 | 20704.8 | 47306 | 2 | PROCESSED | 57606.7955787037 | 56535 | 56169.0484375 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070006 | Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model. | GALACTIC DIFFUSE EMISSION | 5 | A | KATAOKA | JUN | NULL | NULL | JAP | 7 | AO7 | SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER | XIS | Y |
| FERMI_BUBBLE_N5 | 233.6225 | 8.0718 | 14.37791019 | 47.00724717 | 287.4992 | 56146.9871990741 | 56147.4320949074 | 507005010 | 21722.2 | 20000 | 21722.2 | 21722.2 | 0 | 21722.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19555.9 | 19555.9 | 38429.9 | 1 | PROCESSED | 57606.7961921296 | 56535 | 56169.0806944444 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070006 | Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model. | GALACTIC DIFFUSE EMISSION | 5 | A | KATAOKA | JUN | NULL | NULL | JAP | 7 | AO7 | SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER | XIS | Y |
| FERMI_BUBBLE_N6 | 233.4001 | 9.0706 | 15.47217439 | 47.71191257 | 287.5008 | 56147.4330324074 | 56147.9606134259 | 507006010 | 20607 | 20000 | 20607 | 20624.6 | 0 | 20619 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20304.5 | 20304.5 | 45580 | 0 | PROCESSED | 57606.8039467593 | 56626 | 56260.4951851852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070006 | Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model. | GALACTIC DIFFUSE EMISSION | 5 | A | KATAOKA | JUN | NULL | NULL | JAP | 7 | AO7 | SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER | XIS | Y |
| FERMI_BUBBLE_N7 | 234.5505 | 3.1681 | 9.28415113 | 43.5333275 | 287.4999 | 56147.9630787037 | 56148.4306944444 | 507007010 | 22799.1 | 20000 | 22807.1 | 22799.1 | 0 | 22815.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21008.4 | 21008.4 | 40399.9 | 0 | PROCESSED | 57606.8138541667 | 56536 | 56169.1051388889 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070006 | Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model. | GALACTIC DIFFUSE EMISSION | 5 | A | KATAOKA | JUN | NULL | NULL | JAP | 7 | AO7 | SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER | XIS | Y |
| FERMI_BUBBLE_N8 | 234.713 | 2.1937 | 8.32709248 | 42.83416107 | 287.4999 | 56148.4316782407 | 56148.9953240741 | 507008010 | 22115 | 20000 | 22119 | 22115 | 0 | 22123 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 22324.6 | 22324.6 | 48694 | 0 | PROCESSED | 57606.8152546296 | 56536 | 56169.1379976852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070006 | Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model. | GALACTIC DIFFUSE EMISSION | 5 | A | KATAOKA | JUN | NULL | NULL | JAP | 7 | AO7 | SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER | XIS | Y |
| FERMI_BUBBLE_S1 | 329.068 | -46.6182 | 351.41726681 | -50.59485428 | 44.0071 | 56034.6949884259 | 56035.2070717593 | 507009010 | 25314.9 | 20000 | 25314.9 | 25322.9 | 0 | 25322.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 24797.3 | 24797.3 | 44239.9 | 0 | PROCESSED | 57605.1828703704 | 56420 | 56049.2134722222 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070006 | Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model. | GALACTIC DIFFUSE EMISSION | 5 | A | KATAOKA | JUN | NULL | NULL | JAP | 7 | AO7 | SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER | XIS | Y |
| FERMI_BUBBLE_S2 | 330.2693 | -46.4894 | 351.28666586 | -51.42688059 | 44.0074 | 56035.2081018518 | 56035.6736921296 | 507010010 | 20349.6 | 20000 | 20357.6 | 20349.6 | 0 | 20364.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14278 | 14278 | 40213.9 | 0 | PROCESSED | 57605.1975231482 | 56420 | 56049.1880555556 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070006 | Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model. | GALACTIC DIFFUSE EMISSION | 5 | A | KATAOKA | JUN | NULL | NULL | JAP | 7 | AO7 | SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER | XIS | Y |
| FERMI_BUBBLE_S3 | 327.8758 | -46.7423 | 351.52788223 | -49.77060768 | 44.0052 | 56035.6752777778 | 56036.133587963 | 507011010 | 21233.6 | 20000 | 21233.6 | 21233.6 | 0 | 21233.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20914 | 20914 | 39596 | 0 | PROCESSED | 57605.205787037 | 56420 | 56049.1986458333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070006 | Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model. | GALACTIC DIFFUSE EMISSION | 5 | A | KATAOKA | JUN | NULL | NULL | JAP | 7 | AO7 | SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER | XIS | Y |
| FERMI_BUBBLE_S4 | 331.467 | -46.3468 | 351.15250978 | -52.26066971 | 44.0063 | 56036.1354976852 | 56036.5905324074 | 507012010 | 21163.7 | 20000 | 21171.7 | 21163.7 | 0 | 21171.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15381.6 | 15381.6 | 39303.9 | 0 | PROCESSED | 57605.2132291667 | 56434 | 56068.6280671296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070006 | Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model. | GALACTIC DIFFUSE EMISSION | 5 | A | KATAOKA | JUN | NULL | NULL | JAP | 7 | AO7 | SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER | XIS | Y |
| FERMI_BUBBLE_S5 | 332.6607 | -46.1905 | 351.01438321 | -53.09632639 | 44.0062 | 56036.5915625 | 56037.1140972222 | 507013010 | 21004.4 | 20000 | 21012.4 | 21020.4 | 0 | 21004.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20885.4 | 20885.4 | 45109.9 | 0 | PROCESSED | 57605.2184259259 | 56420 | 56049.260787037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070006 | Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model. | GALACTIC DIFFUSE EMISSION | 5 | A | KATAOKA | JUN | NULL | NULL | JAP | 7 | AO7 | SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER | XIS | Y |
| FERMI_BUBBLE_S6 | 326.677 | -46.8481 | 351.64382858 | -48.94656928 | 44.0056 | 56037.1166087963 | 56037.6009027778 | 507014010 | 19643.9 | 20000 | 19651.9 | 19643.9 | 0 | 19659.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 14182.7 | 14182.7 | 41839.9 | 1 | PROCESSED | 57605.2222916667 | 56420 | 56054.1845833333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070006 | Fermi-LAT data reveal two large gamma-ray bubbles, extending 50 deg above and below the Galactic center (GC), which has a significantly hard gamma-ray spectrum. The edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We propose a series of Suzaku observations across the North and South edges of the lobe, 20 ksec x 14 (8 from North and 6 from South) in total. Assuming these bubbles are created by outflow from the GC in the past, we can investigate total energy accumulated in the lobe, shock structure near the edges where non-thermal and thermal pressure is expected to balance. We will study the evolution of supermassive blackhole in the context of Relatively Inefficient Accretion Flow (RIAF), and possible impact to the AGN unification model. | GALACTIC DIFFUSE EMISSION | 5 | A | KATAOKA | JUN | NULL | NULL | JAP | 7 | AO7 | SUZAKU OBSERVATION OF GALACTIC GAMMA-RAY BUBBLE AS A LIVING PROOF OF PAST AGN ACTIVITY IN OUR GALACTIC CENTER | XIS | Y |
| IC 443 | 94.2974 | 22.7535 | 188.8890151 | 3.10517693 | 91.6993 | 56197.2290277778 | 56199.7780324074 | 507015010 | 101802.3 | 400000 | 101810.3 | 101802.3 | 0 | 101810.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 91994 | 91994 | 220187.7 | 0 | PROCESSED | 57607.2728472222 | 56018 | 56225.5965162037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070015 | The thermal spectra in SNRs are the subject to challenge the intrinsic physics and/or dynamics of plasma. One of the breakthrough for this study is the recent discovery of an over-ionized plasma from mixed-morphology SNRs. We propose a deep observation on IC443, the best sample of over-ionized plasma, to solve the over-ionized plasma in position and each elements. The data will provide a quantitative scenario of the structure and evolution of MM-SNRs, and also will be used as the best path-finder for the observational strategy of Astro-H. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 7 | AO7 | DEEP OBSERVATION OF IC443 -- TOWARD THE ORIGIN OF OVER-IONIZED PLASMA -- | XIS | Y |
| IC 443 | 94.3028 | 22.7465 | 188.89754986 | 3.10625906 | 259.0005 | 56378.1771527778 | 56379.6668865741 | 507015020 | 59271.2 | 300000 | 59271.2 | 59271.2 | 0 | 59271.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51270.5 | 51270.5 | 128687.8 | 3 | PROCESSED | 57610.9601388889 | 56018 | 56391.749224537 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070015 | The thermal spectra in SNRs are the subject to challenge the intrinsic physics and/or dynamics of plasma. One of the breakthrough for this study is the recent discovery of an over-ionized plasma from mixed-morphology SNRs. We propose a deep observation on IC443, the best sample of over-ionized plasma, to solve the over-ionized plasma in position and each elements. The data will provide a quantitative scenario of the structure and evolution of MM-SNRs, and also will be used as the best path-finder for the observational strategy of Astro-H. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 7 | AO7 | DEEP OBSERVATION OF IC443 -- TOWARD THE ORIGIN OF OVER-IONIZED PLASMA -- | XIS | Y |
| IC 443 | 94.3026 | 22.7461 | 188.89781567 | 3.10590753 | 258.9991 | 56382.4892824074 | 56385.8835763889 | 507015030 | 131182.3 | 300000 | 131182.3 | 131182.3 | 0 | 131182.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 113851.4 | 113851.4 | 293247.8 | 1 | PROCESSED | 57611.0338194444 | 56018 | 56394.7872337963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070015 | The thermal spectra in SNRs are the subject to challenge the intrinsic physics and/or dynamics of plasma. One of the breakthrough for this study is the recent discovery of an over-ionized plasma from mixed-morphology SNRs. We propose a deep observation on IC443, the best sample of over-ionized plasma, to solve the over-ionized plasma in position and each elements. The data will provide a quantitative scenario of the structure and evolution of MM-SNRs, and also will be used as the best path-finder for the observational strategy of Astro-H. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 7 | AO7 | DEEP OBSERVATION OF IC443 -- TOWARD THE ORIGIN OF OVER-IONIZED PLASMA -- | XIS | Y |
| IC 443 | 94.3024 | 22.7479 | 188.89613959 | 3.10659531 | 258.9994 | 56388.2234837963 | 56390.0835763889 | 507015040 | 75642.7 | 300000 | 75642.8 | 75642.7 | 0 | 75642.7 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 68728.4 | 68728.4 | 160675.9 | 1 | PROCESSED | 57611.01125 | 56018 | 56401.615775463 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070015 | The thermal spectra in SNRs are the subject to challenge the intrinsic physics and/or dynamics of plasma. One of the breakthrough for this study is the recent discovery of an over-ionized plasma from mixed-morphology SNRs. We propose a deep observation on IC443, the best sample of over-ionized plasma, to solve the over-ionized plasma in position and each elements. The data will provide a quantitative scenario of the structure and evolution of MM-SNRs, and also will be used as the best path-finder for the observational strategy of Astro-H. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 7 | AO7 | DEEP OBSERVATION OF IC443 -- TOWARD THE ORIGIN OF OVER-IONIZED PLASMA -- | XIS | Y |
| RADIO_ARC_SOUTH | 266.9853 | -29.0688 | 0.15000746 | -0.5026703 | 267.1998 | 56186.0290509259 | 56188.8203472222 | 507016010 | 103472 | 100000 | 103472 | 103472 | 0 | 103472 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 89190.6 | 89190.6 | 241131.9 | 4 | PROCESSED | 57607.146875 | 56668 | 56303.6234490741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070016 | The 6.4 keV emission associated with giant molecular clouds is the most prominent feature in the Galactic center region. So far, the origin has only been found and discussed in the X-ray reflection process. We propose deep observation at the Radio Arc to discover the 6.4 keV emission in the particle origin, which would open the window to study the nature of the Galactic cosmic ray. | GALACTIC DIFFUSE EMISSION | 5 | A | RYU | SYUKYO | NULL | NULL | JAP | 7 | AO7 | X-RAY OBSERVATION OF THE RADIO ARC -- DISCOVERY OF THE GALACTIC 6.4 KEV EMISSION IN PARTICLE ORIGIN -- | XIS | Y |
| RADIO_ARC_S_E | 267.1914 | -28.7693 | 0.49965543 | -0.50260843 | 267.4999 | 56199.7928125 | 56200.9349652778 | 507017010 | 54178.2 | 50000 | 54202.2 | 54178.2 | 0 | 54202 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 51793.6 | 51793.6 | 98679.9 | 0 | PROCESSED | 57607.2277777778 | 56592 | 56226.621400463 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070016 | The 6.4 keV emission associated with giant molecular clouds is the most prominent feature in the Galactic center region. So far, the origin has only been found and discussed in the X-ray reflection process. We propose deep observation at the Radio Arc to discover the 6.4 keV emission in the particle origin, which would open the window to study the nature of the Galactic cosmic ray. | GALACTIC DIFFUSE EMISSION | 5 | A | RYU | SYUKYO | NULL | NULL | JAP | 7 | AO7 | X-RAY OBSERVATION OF THE RADIO ARC -- DISCOVERY OF THE GALACTIC 6.4 KEV EMISSION IN PARTICLE ORIGIN -- | XIS | Y |
| RADIO_ARC_S_W | 266.7778 | -29.3674 | 359.8007683 | -0.50226251 | 267.1999 | 56200.9358101852 | 56202.0120601852 | 507018010 | 51080.7 | 50000 | 51104.7 | 51096.7 | 0 | 51080.7 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 49115 | 49115 | 92979.9 | 0 | PROCESSED | 57607.2580324074 | 56592 | 56226.6169675926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070016 | The 6.4 keV emission associated with giant molecular clouds is the most prominent feature in the Galactic center region. So far, the origin has only been found and discussed in the X-ray reflection process. We propose deep observation at the Radio Arc to discover the 6.4 keV emission in the particle origin, which would open the window to study the nature of the Galactic cosmic ray. | GALACTIC DIFFUSE EMISSION | 5 | A | RYU | SYUKYO | NULL | NULL | JAP | 7 | AO7 | X-RAY OBSERVATION OF THE RADIO ARC -- DISCOVERY OF THE GALACTIC 6.4 KEV EMISSION IN PARTICLE ORIGIN -- | XIS | Y |
| HESS J1356-645 1 | 209.4297 | -64.5068 | 309.98959301 | -2.54712319 | 106.5083 | 56318.4192939815 | 56320.0002083333 | 507019010 | 55748.9 | 50000 | 55762 | 55756.9 | 0 | 55748.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 65102.3 | 65102.3 | 136567.8 | 2 | PROCESSED | 57608.6328587963 | 56708 | 56342.6666319444 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070017 | Recently, pulsar wind nebulae is focused on one of the electron accelerators in our Galaxy. Especially TeV pulsar wind nebulae are supposed to have a largely extended X-ray emission. Since the X-ray emission is much larger than the size considering the typical electron lifetime, high energy electrons strangely seem to be transferred too fast or without cooling. To study the electron diffusion of young pulsar wind nebula, we propose observations of HESS J1356-645, which is off the Galactic plane and is free from the Galactic ridge X-ray emission. | GALACTIC DIFFUSE EMISSION | 5 | C | FUJINAGA | TAKAHISA | NULL | NULL | JAP | 7 | AO7 | OFF-PLANE TEV GAMMA-RAY SOURCE HESS J1356-645 | XIS | Y |
| HESS J1356-645 2 | 208.8016 | -64.5041 | 309.72820731 | -2.47708999 | 123.7329 | 56340.1852430556 | 56341.4863425926 | 507020010 | 51259.4 | 50000 | 51263.6 | 51259.4 | 0 | 51259.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45150.5 | 45150.5 | 112405.9 | 2 | PROCESSED | 57610.6176157407 | 56718 | 56352.5089930556 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070017 | Recently, pulsar wind nebulae is focused on one of the electron accelerators in our Galaxy. Especially TeV pulsar wind nebulae are supposed to have a largely extended X-ray emission. Since the X-ray emission is much larger than the size considering the typical electron lifetime, high energy electrons strangely seem to be transferred too fast or without cooling. To study the electron diffusion of young pulsar wind nebula, we propose observations of HESS J1356-645, which is off the Galactic plane and is free from the Galactic ridge X-ray emission. | GALACTIC DIFFUSE EMISSION | 5 | C | FUJINAGA | TAKAHISA | NULL | NULL | JAP | 7 | AO7 | OFF-PLANE TEV GAMMA-RAY SOURCE HESS J1356-645 | XIS | Y |
| HESSJ1507-622_CENTER | 226.7316 | -62.3464 | 317.95199358 | -3.49348671 | 301.8082 | 56181.4881712963 | 56183.9549189815 | 507025010 | 79886.9 | 80000 | 79894.9 | 79902.9 | 0 | 79886.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 74195.8 | 74195.8 | 213103.7 | 1 | PROCESSED | 57607.0557986111 | 56582 | 56212.7347337963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070033 | HESS J1507-622 is one of the unidentified TeV-gamma-ray sources discovered in the H.E.S.S. Galactic plane survey. The object is unique in the sense of the location, off the Galactic plane. There are no counterparts in radio, infrared, X-ray bands and thus the origin is still mystery, but the object represents several hints; X-ray source like pulsar wind nebula exists near the object, and the location is at the edge of the large molecular cloud near a radio supernova remnant. The main purpose of the Suzaku observation with the best use of high sensitive capability in diffuse X-rays and of a unique low galactic-absorption feature of the object is to determine the origin of TeV emission, such as old supernova remnant with molecular cloud, pulsar-wind driven radiations, or darkest accelerator. | GALACTIC DIFFUSE EMISSION | 5 | B | TERADA | YUKIKATSU | MATSUMOTO | HIRONORI | JAP | 7 | AO7 | SUZAKU OBSERVATION OF HESS J1507-622; A UNIQUE TEV UNIDENTIFIED SOURCE OFF THE GALACTIC PLANE | XIS | Y |
| HESSJ1507-622_OFFSET | 227.1815 | -62.1646 | 318.2247639 | -3.44071412 | 303.001 | 56183.9562268518 | 56185.1042939815 | 507026010 | 40912.2 | 40000 | 40912.2 | 40941.8 | 0 | 40933.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38033.6 | 38033.6 | 99179.8 | 1 | PROCESSED | 57607.0490162037 | 56582 | 56212.7288078704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070033 | HESS J1507-622 is one of the unidentified TeV-gamma-ray sources discovered in the H.E.S.S. Galactic plane survey. The object is unique in the sense of the location, off the Galactic plane. There are no counterparts in radio, infrared, X-ray bands and thus the origin is still mystery, but the object represents several hints; X-ray source like pulsar wind nebula exists near the object, and the location is at the edge of the large molecular cloud near a radio supernova remnant. The main purpose of the Suzaku observation with the best use of high sensitive capability in diffuse X-rays and of a unique low galactic-absorption feature of the object is to determine the origin of TeV emission, such as old supernova remnant with molecular cloud, pulsar-wind driven radiations, or darkest accelerator. | GALACTIC DIFFUSE EMISSION | 5 | B | TERADA | YUKIKATSU | MATSUMOTO | HIRONORI | JAP | 7 | AO7 | SUZAKU OBSERVATION OF HESS J1507-622; A UNIQUE TEV UNIDENTIFIED SOURCE OFF THE GALACTIC PLANE | XIS | Y |
| HESS J1457-593 | 224.4524 | -59.4762 | 318.36335314 | -0.44487967 | 305.8997 | 56185.1060185185 | 56186.0216782407 | 507027010 | 31047.9 | 30000 | 31047.9 | 31047.9 | 0 | 31047.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28099.4 | 28099.4 | 79105.9 | 1 | PROCESSED | 57607.0753819445 | 56584 | 56218.5178009259 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070037 | We propose an X-ray observation of the putative SNR-molecular cloud interaction HESS J1457-593 with the Suzaku XIS detector for 30 ks. The aim of the observation is to clarify whether the TeV gamma-ray emission is of a leptonic or hadronic origin by searching for an X-ray counterpart to a level down to $10^{-14}$~erg cm$^{-2}$ s$^{-1}$. A non-detection of an X-ray nebula would strongly disfavor a leptonic origin of the TeV emission and add to the already strong multi-wavelength data which all suggests a hadronic origin of the emission. Since the spectrum of this unique source extends above many tens of TeV this would mean that we see, for the first time, evidence for hadronic cosmic rays being accelerated up to PeV energies. | GALACTIC DIFFUSE EMISSION | 5 | B | ODAKA | HIROKAZU | NULL | NULL | JAP | 7 | AO7 | INVESTIGATING A PUTATIVE COSMIC-RAY PEVATRON WITH SUZAKU | XIS | Y |
| GC_SOUTH_1 | 268.0988 | -29.4771 | 0.29758282 | -1.54591478 | 274.6002 | 56190.0385069444 | 56191.3341435185 | 507028010 | 51761.9 | 50000 | 51761.9 | 51769.9 | 0 | 51769.9 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 41153.4 | 41153.4 | 111931.8 | 1 | PROCESSED | 57607.1304398148 | 56584 | 56218.5464930556 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070042 | We have discovered the large and peculiar plasma emission from the south of the galactic center (around l=0, b=-1.5 degree). Observed column density shows that this plasma is located in the galactic center region. Assuming the distance of 8 kpc, the size of the plasma is 40 pc x 120 pc. Then, the estimated total energy of the plasma reaches 8e51 ergs. What is the engine creating such a energetic plasma ? Moreover, the ionization temperature of this plasma is larger than the electron temperature (over-ionized plasma). This condition is peculiar in the standard heating mechanism of a plasma. What is the origin of the over-ionized plasma ? Since the previous Suzaku observation covers only a part of the plasma, we propose the observation of the other part for the further investigation. | GALACTIC DIFFUSE EMISSION | 5 | A | NAKASHIMA | SHINYA | NULL | NULL | JAP | 7 | AO7 | OBSERVATION OF THE LARGE PLASMA IN THE THE SOUTHERN GALACTIC CENTER | XIS | Y |
| GC_SOUTH_2 | 268.3751 | -29.7084 | 0.22024801 | -1.8703349 | 273.7998 | 56192.7899421296 | 56194.081412037 | 507029010 | 52446.9 | 50000 | 52462.9 | 52446.9 | 0 | 52454.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 45230.7 | 45230.7 | 111575.9 | 1 | PROCESSED | 57607.1634259259 | 56689 | 56321.5121875 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070042 | We have discovered the large and peculiar plasma emission from the south of the galactic center (around l=0, b=-1.5 degree). Observed column density shows that this plasma is located in the galactic center region. Assuming the distance of 8 kpc, the size of the plasma is 40 pc x 120 pc. Then, the estimated total energy of the plasma reaches 8e51 ergs. What is the engine creating such a energetic plasma ? Moreover, the ionization temperature of this plasma is larger than the electron temperature (over-ionized plasma). This condition is peculiar in the standard heating mechanism of a plasma. What is the origin of the over-ionized plasma ? Since the previous Suzaku observation covers only a part of the plasma, we propose the observation of the other part for the further investigation. | GALACTIC DIFFUSE EMISSION | 5 | A | NAKASHIMA | SHINYA | NULL | NULL | JAP | 7 | AO7 | OBSERVATION OF THE LARGE PLASMA IN THE THE SOUTHERN GALACTIC CENTER | XIS | Y |
| GC_SOUTH_3 | 268.18 | -29.2061 | 0.56701913 | -1.46906711 | 273.9841 | 56205.6096412037 | 56206.6341898148 | 507030010 | 51741.8 | 50000 | 51749.8 | 51749.8 | 0 | 51741.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 52191.1 | 52191.1 | 88515.9 | 0 | PROCESSED | 57607.309537037 | 56595 | 56226.549212963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070042 | We have discovered the large and peculiar plasma emission from the south of the galactic center (around l=0, b=-1.5 degree). Observed column density shows that this plasma is located in the galactic center region. Assuming the distance of 8 kpc, the size of the plasma is 40 pc x 120 pc. Then, the estimated total energy of the plasma reaches 8e51 ergs. What is the engine creating such a energetic plasma ? Moreover, the ionization temperature of this plasma is larger than the electron temperature (over-ionized plasma). This condition is peculiar in the standard heating mechanism of a plasma. What is the origin of the over-ionized plasma ? Since the previous Suzaku observation covers only a part of the plasma, we propose the observation of the other part for the further investigation. | GALACTIC DIFFUSE EMISSION | 5 | A | NAKASHIMA | SHINYA | NULL | NULL | JAP | 7 | AO7 | OBSERVATION OF THE LARGE PLASMA IN THE THE SOUTHERN GALACTIC CENTER | XIS | Y |
| GC_SOUTH_4 | 268.4148 | -29.4524 | 0.45858363 | -1.77042753 | 273.9837 | 56206.6347106482 | 56207.6987731482 | 507031010 | 52874.3 | 50000 | 52890.3 | 52890.3 | 0 | 52874.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 54140.2 | 54140.2 | 91919.9 | 0 | PROCESSED | 57607.3059837963 | 56595 | 56226.5383449074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070042 | We have discovered the large and peculiar plasma emission from the south of the galactic center (around l=0, b=-1.5 degree). Observed column density shows that this plasma is located in the galactic center region. Assuming the distance of 8 kpc, the size of the plasma is 40 pc x 120 pc. Then, the estimated total energy of the plasma reaches 8e51 ergs. What is the engine creating such a energetic plasma ? Moreover, the ionization temperature of this plasma is larger than the electron temperature (over-ionized plasma). This condition is peculiar in the standard heating mechanism of a plasma. What is the origin of the over-ionized plasma ? Since the previous Suzaku observation covers only a part of the plasma, we propose the observation of the other part for the further investigation. | GALACTIC DIFFUSE EMISSION | 5 | A | NAKASHIMA | SHINYA | NULL | NULL | JAP | 7 | AO7 | OBSERVATION OF THE LARGE PLASMA IN THE THE SOUTHERN GALACTIC CENTER | XIS | Y |
| ERIDANUS_ARCB_SPOT | 53.3104 | -9.6904 | 196.20250346 | -48.10218961 | 67.1761 | 56138.1083101852 | 56139.0792476852 | 507032010 | 40618.6 | 40000 | 40618.6 | 40618.6 | 0 | 40618.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35171 | 35171 | 83869.9 | 1 | PROCESSED | 57606.7122337963 | 56528 | 56162.0431018518 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070046 | We propose Suzaku spectroscopic observations of the Edinanus Super Bubble, the nearest super bubble in our Galaxy. This is a good site to study the density, temperature, metalicity, and ionization status etc. at the rim of super bubbles which might be sources of the Galactic halo or fountains. A series of observations will reveal how the hot plasma is heated and expands as a bubble. | GALACTIC DIFFUSE EMISSION | 5 | C | YAMASAKI | NORIKO | NULL | NULL | JAP | 7 | AO7 | SUZAKU OBSERVATION OF THE ERIDANUS SUPER BUBBLE | XIS | Y |
| G32.8-0.1 NORTH | 282.8355 | -0.0511 | 32.87550481 | -0.00195799 | 74.4992 | 56037.6100347222 | 56038.7897685185 | 507035010 | 55147.5 | 50000 | 55147.5 | 55147.5 | 0 | 55147.5 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 53483.4 | 53483.4 | 101925.9 | 0 | PROCESSED | 57605.250162037 | 56421 | 56054.2396990741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070047 | A key element to untangle the Galactic origin of the cosmic-ray is the acceleration of high energy particles that occurs in the shocks of the supernova remnants (SNRs). Recent Fermi surveys revealed that particles are more efficiently escaping from the acceleration system when the SNRs get older. However what is still unknown is the plasma condition environment that makes the mechanism more efficient. X-ray observations are an excellent tool to understand the plasma condition but there has not been a systematic X-ray follow-up observations of these Fermi SNRs. The Suzaku Observatory is ideal for such X-ray systematic study because of his low background. We propose here X-ray observations of 4 SNRs detected by Fermi to solve cosmic-ray escape problem. | GALACTIC DIFFUSE EMISSION | 5 | B | BAMBA | AYA | NULL | NULL | JAP | 7 | AO7 | SUZAKU SYSTEMATIC STUDY OF FERMI DETECTED SNRS | XIS | Y |
| G32.8-0.1 SOUTH | 282.8163 | -0.2514 | 32.68848527 | -0.07620379 | 74.5004 | 56038.7902430556 | 56039.916087963 | 507036010 | 52232.4 | 50000 | 52240.4 | 52232.4 | 0 | 52248.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 50243.2 | 50243.2 | 97268 | 1 | PROCESSED | 57605.2444560185 | 56421 | 56055.0208564815 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070047 | A key element to untangle the Galactic origin of the cosmic-ray is the acceleration of high energy particles that occurs in the shocks of the supernova remnants (SNRs). Recent Fermi surveys revealed that particles are more efficiently escaping from the acceleration system when the SNRs get older. However what is still unknown is the plasma condition environment that makes the mechanism more efficient. X-ray observations are an excellent tool to understand the plasma condition but there has not been a systematic X-ray follow-up observations of these Fermi SNRs. The Suzaku Observatory is ideal for such X-ray systematic study because of his low background. We propose here X-ray observations of 4 SNRs detected by Fermi to solve cosmic-ray escape problem. | GALACTIC DIFFUSE EMISSION | 5 | B | BAMBA | AYA | NULL | NULL | JAP | 7 | AO7 | SUZAKU SYSTEMATIC STUDY OF FERMI DETECTED SNRS | XIS | Y |
| G298.6-0.0 | 183.3899 | -62.6356 | 298.59488766 | -0.08324812 | 319.8129 | 56150.8519097222 | 56152.08625 | 507037010 | 17238.8 | 50000 | 17238.8 | 17238.8 | 0 | 17238.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 19174.6 | 19174.6 | 106616 | 0 | PROCESSED | 57606.8422222222 | 56721 | 56291.7215162037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070047 | A key element to untangle the Galactic origin of the cosmic-ray is the acceleration of high energy particles that occurs in the shocks of the supernova remnants (SNRs). Recent Fermi surveys revealed that particles are more efficiently escaping from the acceleration system when the SNRs get older. However what is still unknown is the plasma condition environment that makes the mechanism more efficient. X-ray observations are an excellent tool to understand the plasma condition but there has not been a systematic X-ray follow-up observations of these Fermi SNRs. The Suzaku Observatory is ideal for such X-ray systematic study because of his low background. We propose here X-ray observations of 4 SNRs detected by Fermi to solve cosmic-ray escape problem. | GALACTIC DIFFUSE EMISSION | 5 | B | BAMBA | AYA | NULL | NULL | JAP | 7 | AO7 | SUZAKU SYSTEMATIC STUDY OF FERMI DETECTED SNRS | XIS | Y |
| G298.6-0.0 | 183.3873 | -62.6234 | 298.59191859 | -0.0713547 | 133.8706 | 56341.7597222222 | 56342.6981712963 | 507037020 | 39724.7 | 35000 | 39724.7 | 39724.7 | 0 | 39724.7 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 36262.1 | 36262.1 | 81069.9 | 0 | PROCESSED | 57610.644849537 | 56721 | 56362.8029861111 | 3.0.22.44 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070047 | A key element to untangle the Galactic origin of the cosmic-ray is the acceleration of high energy particles that occurs in the shocks of the supernova remnants (SNRs). Recent Fermi surveys revealed that particles are more efficiently escaping from the acceleration system when the SNRs get older. However what is still unknown is the plasma condition environment that makes the mechanism more efficient. X-ray observations are an excellent tool to understand the plasma condition but there has not been a systematic X-ray follow-up observations of these Fermi SNRs. The Suzaku Observatory is ideal for such X-ray systematic study because of his low background. We propose here X-ray observations of 4 SNRs detected by Fermi to solve cosmic-ray escape problem. | GALACTIC DIFFUSE EMISSION | 5 | B | BAMBA | AYA | NULL | NULL | JAP | 7 | AO7 | SUZAKU SYSTEMATIC STUDY OF FERMI DETECTED SNRS | XIS | Y |
| CAS A | 350.8607 | 58.8031 | 111.73599633 | -2.14263527 | 251.3043 | 56281.1375115741 | 56283.3466666667 | 507038010 | 102411 | 100000 | 102419 | 102411 | 0 | 102426 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 126710.3 | 126710.3 | 190845.8 | 0 | PROCESSED | 57608.4566435185 | 56683 | 56316.9831365741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070050 | We will propose a follow-up 120 ksec observations of a young supernova remnant Cassiopeia A. The long exposure provides us a high quality of the broad band spectrum from XIS to HXD GSO band. We will try to detect Mn-K line at 6.1 keV for the first time. The element Mn as well as Cr gives constraint on the explosion mechanism of the ejecta. We also test a predicted flux variation of a non-thermal emission in the PIN band for the first time. The variation gives critical information to solve the physical parameters in the reverse shock of the ejecta. | GALACTIC DIFFUSE EMISSION | 5 | C | MAEDA | YOSHITOMO | NULL | NULL | JAP | 7 | AO7 | MN/CR-K AND HARD X-RAY EMISSION IN CASSIOPEIA A | XIS | Y |
| MSH15-56_SW | 238.0528 | -56.3239 | 326.11105465 | -1.81589779 | 86.2015 | 56326.3325 | 56327.8577314815 | 507039010 | 86012.2 | 100000 | 86012.2 | 86012.2 | 0 | 86012.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 88391.2 | 88391.2 | 131771.9 | 2 | PROCESSED | 57610.534849537 | 56714 | 56345.5312847222 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070055 | The magnetic field upstream the shock front of the SN blast wave is the key parameter for discussing particle acceleration. In this study we try to constrain the upstream magnetic field and its amplification based on the ionization parameter of heated ISM just behind the shock. For this purpose, we propose a 100 ks XIS observation of an middle aged SNR MSH 15-56 with non-thermal filaments and an anomalously large ionization age for its dynamical age. | GALACTIC DIFFUSE EMISSION | 5 | C | YATSU | YOICHI | NULL | NULL | JAP | 7 | AO7 | A STUDY OF PARTICLE ACCELERATION BASED ON THE THERMAL PLASMA BEHIND THE SHOCK | XIS | Y |
| CYG_COCOON | 306.8026 | 40.9389 | 79.25133167 | 1.48664873 | 218.8996 | 56279.1800231482 | 56280.1654976852 | 507040010 | 51072.4 | 50000 | 51072.4 | 51093.6 | 0 | 51080.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42783.3 | 42783.3 | 85143.9 | 0 | PROCESSED | 57608.3232291667 | 56683 | 56316.5705324074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070060 | The long-standing questions on the origin of Galactic cosmic-rays (GCR) is still not settled, and star-forming regions are promising sites for the production of GCR. We propose deep observation of nearby star-forming region Cygnus X, aiming at GeV gamma-ray excess revealed by Fermi. By utilizing the high sensitivity of Suzaku XIS, particularly for diffuse X-rays, we can identify particle species (electrons or protons) and evaluate the cosmic-ray energy density in this important object. | GALACTIC DIFFUSE EMISSION | 5 | C | MIZUNO | TSUNEFUMI | NULL | NULL | JAP | 7 | AO7 | SUZAKU INVESTIGATION OF PARTICLE ACCELERATION IN NEARBY STAR-FORMING REGION CYGNUS X | XIS | Y |
| CYG_BGD1 | 306.6527 | 39.4856 | 78.0015669 | 0.73572902 | 218.9004 | 56280.1666666667 | 56280.6286458333 | 507041010 | 26932.4 | 25000 | 26940.4 | 26932.4 | 0 | 26940.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 20452.7 | 20452.7 | 39911.9 | 0 | PROCESSED | 57608.3151273148 | 56683 | 56316.5312268518 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070060 | The long-standing questions on the origin of Galactic cosmic-rays (GCR) is still not settled, and star-forming regions are promising sites for the production of GCR. We propose deep observation of nearby star-forming region Cygnus X, aiming at GeV gamma-ray excess revealed by Fermi. By utilizing the high sensitivity of Suzaku XIS, particularly for diffuse X-rays, we can identify particle species (electrons or protons) and evaluate the cosmic-ray energy density in this important object. | GALACTIC DIFFUSE EMISSION | 5 | C | MIZUNO | TSUNEFUMI | NULL | NULL | JAP | 7 | AO7 | SUZAKU INVESTIGATION OF PARTICLE ACCELERATION IN NEARBY STAR-FORMING REGION CYGNUS X | XIS | Y |
| CYG_BGD2 | 306.9576 | 42.391 | 80.50042704 | 2.23726855 | 218.3998 | 56280.6304166667 | 56281.1313888889 | 507042010 | 25624.9 | 25000 | 25624.9 | 25624.9 | 0 | 25648.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25025 | 25025 | 43273.9 | 1 | PROCESSED | 57608.3181018518 | 56683 | 56316.5346990741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070060 | The long-standing questions on the origin of Galactic cosmic-rays (GCR) is still not settled, and star-forming regions are promising sites for the production of GCR. We propose deep observation of nearby star-forming region Cygnus X, aiming at GeV gamma-ray excess revealed by Fermi. By utilizing the high sensitivity of Suzaku XIS, particularly for diffuse X-rays, we can identify particle species (electrons or protons) and evaluate the cosmic-ray energy density in this important object. | GALACTIC DIFFUSE EMISSION | 5 | C | MIZUNO | TSUNEFUMI | NULL | NULL | JAP | 7 | AO7 | SUZAKU INVESTIGATION OF PARTICLE ACCELERATION IN NEARBY STAR-FORMING REGION CYGNUS X | XIS | Y |
| (L,B)=(-20,0) | 276.6688 | -11.87 | 19.56512772 | 0.0074406 | 263.6004 | 56215.5456944444 | 56219.7479861111 | 507044010 | 171823.1 | 200000 | 171823.1 | 171823.1 | 0 | 171823.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 147119.2 | 147119.2 | 363037.7 | 4 | PROCESSED | 57607.9036342593 | 56602 | 56238.7999884259 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070084 | We will observe the region at (l,b)=(19.57, 0.0112) to measure spatial and temporal fluctuations of the Galactic Ridge X-ray Emission (GRXE). Measuring these fluctuations is a good test to check the scenarios of point sources and star flare for the GRXE origin. Combined with archival data of XMM-Newton, 200 ks observation of Suzaku makes us able to detect the fluctuations lager than 3% of the GRXE flux. The observation mode of XIS is planed to be a normal clocking mode with no window option. | GALACTIC DIFFUSE EMISSION | 5 | B | UCHIYAMA | HIDEKI | NULL | NULL | JAP | 7 | AO7 | SUZAKU STUDY OF SPATIAL AND TEMPORAL FLUCTUATIONS IN THE GALACTIC RIDGE X-RAY EMISSION | XIS | Y |
| VELA PWN N1 | 128.8231 | -44.9507 | 263.36545364 | -2.659461 | 324.0013 | 56108.9552083333 | 56109.3487962963 | 507048010 | 17801.4 | 15000 | 17809.4 | 17801.4 | 0 | 17809.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 19204.7 | 19204.7 | 33999.9 | 1 | PROCESSED | 57606.5230439815 | 56592 | 56226.6327083333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070103 | We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent in the eastern direction from the pulsar, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the northern direction. Our immediate objective is to investigate how much extended the Vela PWN is in the north where the thermal pressure is significantly higher than that in the east we observed so far. The comparison of the X-ray extent in two directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component. | GALACTIC DIFFUSE EMISSION | 5 | C | MORI | KOJI | NULL | NULL | JAP | 7 | AO7 | HOW MUCH EXTENDED IS THE VELA PULSAR WIND NEBULA? | XIS | Y |
| VELA PWN N2 | 128.845 | -44.6374 | 263.12360018 | -2.45940596 | 325.4993 | 56109.3500115741 | 56109.7210185185 | 507049010 | 18411.8 | 15000 | 18419.8 | 18411.8 | 0 | 18419.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 18762.3 | 18762.3 | 32024 | 0 | PROCESSED | 57606.5242939815 | 56493 | 56127.0941319444 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070103 | We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent in the eastern direction from the pulsar, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the northern direction. Our immediate objective is to investigate how much extended the Vela PWN is in the north where the thermal pressure is significantly higher than that in the east we observed so far. The comparison of the X-ray extent in two directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component. | GALACTIC DIFFUSE EMISSION | 5 | C | MORI | KOJI | NULL | NULL | JAP | 7 | AO7 | HOW MUCH EXTENDED IS THE VELA PULSAR WIND NEBULA? | XIS | Y |
| VELA PWN N3 | 128.8419 | -44.3423 | 262.88578161 | -2.28439697 | 325.9006 | 56109.7216782407 | 56110.0161574074 | 507050010 | 12398.4 | 15000 | 12398.4 | 12398.4 | 0 | 12398.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13245.4 | 13245.4 | 25431.9 | 1 | PROCESSED | 57606.5311805556 | 56493 | 56127.104849537 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070103 | We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent in the eastern direction from the pulsar, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the northern direction. Our immediate objective is to investigate how much extended the Vela PWN is in the north where the thermal pressure is significantly higher than that in the east we observed so far. The comparison of the X-ray extent in two directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component. | GALACTIC DIFFUSE EMISSION | 5 | C | MORI | KOJI | NULL | NULL | JAP | 7 | AO7 | HOW MUCH EXTENDED IS THE VELA PULSAR WIND NEBULA? | XIS | Y |
| VELA PWN N4 | 128.8415 | -44.0453 | 262.64764922 | -2.10667439 | 326.4998 | 56110.0169097222 | 56110.3459953704 | 507051010 | 17289 | 15000 | 17289 | 17289 | 0 | 17289 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17655.8 | 17655.8 | 28401.9 | 0 | PROCESSED | 57606.5331018518 | 56646 | 56280.6029050926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070103 | We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent in the eastern direction from the pulsar, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the northern direction. Our immediate objective is to investigate how much extended the Vela PWN is in the north where the thermal pressure is significantly higher than that in the east we observed so far. The comparison of the X-ray extent in two directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component. | GALACTIC DIFFUSE EMISSION | 5 | C | MORI | KOJI | NULL | NULL | JAP | 7 | AO7 | HOW MUCH EXTENDED IS THE VELA PULSAR WIND NEBULA? | XIS | Y |
| VELA PWN N5 | 128.8386 | -43.7507 | 262.41040878 | -1.9318018 | 327.6005 | 56110.3470717593 | 56110.6620138889 | 507052010 | 18148.6 | 15000 | 18156.6 | 18148.6 | 0 | 18156.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17458.2 | 17458.2 | 27208 | 1 | PROCESSED | 57606.5339930556 | 56493 | 56127.126712963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070103 | We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent in the eastern direction from the pulsar, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the northern direction. Our immediate objective is to investigate how much extended the Vela PWN is in the north where the thermal pressure is significantly higher than that in the east we observed so far. The comparison of the X-ray extent in two directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component. | GALACTIC DIFFUSE EMISSION | 5 | C | MORI | KOJI | NULL | NULL | JAP | 7 | AO7 | HOW MUCH EXTENDED IS THE VELA PULSAR WIND NEBULA? | XIS | Y |
| VELA PWN N6 | 128.8205 | -43.4604 | 262.17003306 | -1.76832201 | 122.021 | 56258.4379050926 | 56258.805625 | 507053010 | 15340.1 | 15000 | 15348.1 | 15348.1 | 0 | 15340.1 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13901.3 | 13901.3 | 31759.9 | 0 | PROCESSED | 57608.0978819444 | 56641 | 56275.6586111111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070103 | We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent in the eastern direction from the pulsar, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the northern direction. Our immediate objective is to investigate how much extended the Vela PWN is in the north where the thermal pressure is significantly higher than that in the east we observed so far. The comparison of the X-ray extent in two directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component. | GALACTIC DIFFUSE EMISSION | 5 | C | MORI | KOJI | NULL | NULL | JAP | 7 | AO7 | HOW MUCH EXTENDED IS THE VELA PULSAR WIND NEBULA? | XIS | Y |
| SNR HB3 SE-A | 35.6022 | 61.9246 | 133.41628397 | 0.91883689 | 247.499 | 56322.7203935185 | 56323.4079050926 | 507056010 | 46748 | 40000 | 46748 | 46751.7 | 0 | 46759.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43962.8 | 43962.8 | 59393.9 | 0 | PROCESSED | 57608.6541666667 | 56709 | 56342.6336921296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071316 | We propose to study the large SNR HB3, which is classified as the mixed-morphology SNRs. The Fermi LAT revealed recently bright gamma-ray emissions adjacent to the southeastern shell of HB3, indicating the gamma rays originate in shocked molecular clouds associated with the nearby HII region W3/W4. However it is difficult to determine the gamma-ray origins since the HII regions are dominant in all energy bands except for X-ray. Our aim is to obtain the spatial structure and the temperature of thermal X-ray emissions at this site. These information will help us to understand whether HB3 interacts with molecular clouds. For this purpose, we require high sensitivities and the wide field of view to cover the southeastern shell. Suzaku is an ideal X-ray observatory to achieve this objective. | GALACTIC DIFFUSE EMISSION | 5 | C | KATSUTA | JUNICHIRO | NULL | NULL | USA | 7 | AO7 | SUZAKU OBSERVATION OF A GAMMA-RAY EMISSION SNR, HB3 | XIS | Y |
| SNR HB3 SE-B | 35.7593 | 62.192 | 133.39304715 | 1.19520932 | 247.4986 | 56323.4084259259 | 56323.7710532407 | 507057010 | 25836.6 | 20000 | 25844.6 | 25836.6 | 0 | 25852.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 19309.2 | 19309.2 | 31327.9 | 1 | PROCESSED | 57608.6657638889 | 56711 | 56345.4750462963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071316 | We propose to study the large SNR HB3, which is classified as the mixed-morphology SNRs. The Fermi LAT revealed recently bright gamma-ray emissions adjacent to the southeastern shell of HB3, indicating the gamma rays originate in shocked molecular clouds associated with the nearby HII region W3/W4. However it is difficult to determine the gamma-ray origins since the HII regions are dominant in all energy bands except for X-ray. Our aim is to obtain the spatial structure and the temperature of thermal X-ray emissions at this site. These information will help us to understand whether HB3 interacts with molecular clouds. For this purpose, we require high sensitivities and the wide field of view to cover the southeastern shell. Suzaku is an ideal X-ray observatory to achieve this objective. | GALACTIC DIFFUSE EMISSION | 5 | C | KATSUTA | JUNICHIRO | NULL | NULL | USA | 7 | AO7 | SUZAKU OBSERVATION OF A GAMMA-RAY EMISSION SNR, HB3 | XIS | Y |
| SNR HB3 SE-C | 36.0358 | 62.4578 | 133.42083063 | 1.4890972 | 247.4994 | 56323.7716666667 | 56324.1585532407 | 507058010 | 24142 | 20000 | 24161.6 | 24142 | 0 | 24169.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 23454.7 | 23454.7 | 33423.9 | 0 | PROCESSED | 57608.6786342593 | 56711 | 56345.4779976852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071316 | We propose to study the large SNR HB3, which is classified as the mixed-morphology SNRs. The Fermi LAT revealed recently bright gamma-ray emissions adjacent to the southeastern shell of HB3, indicating the gamma rays originate in shocked molecular clouds associated with the nearby HII region W3/W4. However it is difficult to determine the gamma-ray origins since the HII regions are dominant in all energy bands except for X-ray. Our aim is to obtain the spatial structure and the temperature of thermal X-ray emissions at this site. These information will help us to understand whether HB3 interacts with molecular clouds. For this purpose, we require high sensitivities and the wide field of view to cover the southeastern shell. Suzaku is an ideal X-ray observatory to achieve this objective. | GALACTIC DIFFUSE EMISSION | 5 | C | KATSUTA | JUNICHIRO | NULL | NULL | USA | 7 | AO7 | SUZAKU OBSERVATION OF A GAMMA-RAY EMISSION SNR, HB3 | XIS | Y |
| G299.5-0.6 | 184.8049 | -63.1515 | 299.30360744 | -0.50694599 | 313.6989 | 56144.5663773148 | 56144.9523032407 | 507064010 | 13835.1 | 10000 | 13843.1 | 13835.1 | 0 | 13843.1 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13272.2 | 13272.2 | 33335.9 | 0 | PROCESSED | 57606.7635763889 | 56630 | 56264.5463541667 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 072014 | We propose to investigate the four brightest and most-promising RASS-detected SNR candidates. With the observations we will be able to determine if the objects are supernova remnants, and if so, measure their spectral characteristics (temperature, abundance), details of their morphology (angular size) and their expansion velocity. This study will complete previous surveys of SNR in other wavelength and provide insight into the structure and composition of the ISM. Follow-up radio continuum and linear polarization observations, and optical studies will be performed. | GALACTIC DIFFUSE EMISSION | 5 | A | PRINZ | TOBIAS | NULL | NULL | EUR | 7 | AO7 | IDENTIFICATION OF X-RAY SELECTED SUPERNOVA REMNANTS | XIS | Y |
| G7.6+2.0 | 268.7973 | -21.391 | 7.58937554 | 2.00788461 | 270.4016 | 56194.0843865741 | 56194.4237037037 | 507065010 | 16521 | 10000 | 16529 | 16521 | 0 | 16534.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12160.3 | 12160.3 | 29313.9 | 2 | PROCESSED | 57607.1654050926 | 56676 | 56315.5110069444 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 072014 | We propose to investigate the four brightest and most-promising RASS-detected SNR candidates. With the observations we will be able to determine if the objects are supernova remnants, and if so, measure their spectral characteristics (temperature, abundance), details of their morphology (angular size) and their expansion velocity. This study will complete previous surveys of SNR in other wavelength and provide insight into the structure and composition of the ISM. Follow-up radio continuum and linear polarization observations, and optical studies will be performed. | GALACTIC DIFFUSE EMISSION | 5 | A | PRINZ | TOBIAS | NULL | NULL | EUR | 7 | AO7 | IDENTIFICATION OF X-RAY SELECTED SUPERNOVA REMNANTS | XIS | Y |
| G276.2-7.7 | 135.4479 | -58.0976 | 276.2324482 | -7.68832918 | 319.4197 | 56102.2534722222 | 56102.610625 | 507066010 | 10299.4 | 10000 | 10299.4 | 10299.4 | 0 | 10299.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11627.5 | 11627.5 | 30855.9 | 0 | PROCESSED | 57605.7340972222 | 56582 | 56219.6536458333 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 072014 | We propose to investigate the four brightest and most-promising RASS-detected SNR candidates. With the observations we will be able to determine if the objects are supernova remnants, and if so, measure their spectral characteristics (temperature, abundance), details of their morphology (angular size) and their expansion velocity. This study will complete previous surveys of SNR in other wavelength and provide insight into the structure and composition of the ISM. Follow-up radio continuum and linear polarization observations, and optical studies will be performed. | GALACTIC DIFFUSE EMISSION | 5 | A | PRINZ | TOBIAS | NULL | NULL | EUR | 7 | AO7 | IDENTIFICATION OF X-RAY SELECTED SUPERNOVA REMNANTS | XIS | Y |
| G278.0+12.4 | 158.151 | -43.7043 | 278.01040448 | 12.3478226 | 304.0284 | 56102.6152199074 | 56102.9842476852 | 507067010 | 18996 | 17500 | 19004 | 18996 | 0 | 19004 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16442 | 16442 | 31879.9 | 0 | PROCESSED | 57605.7438078704 | 56582 | 56219.6572916667 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 072014 | We propose to investigate the four brightest and most-promising RASS-detected SNR candidates. With the observations we will be able to determine if the objects are supernova remnants, and if so, measure their spectral characteristics (temperature, abundance), details of their morphology (angular size) and their expansion velocity. This study will complete previous surveys of SNR in other wavelength and provide insight into the structure and composition of the ISM. Follow-up radio continuum and linear polarization observations, and optical studies will be performed. | GALACTIC DIFFUSE EMISSION | 5 | A | PRINZ | TOBIAS | NULL | NULL | EUR | 7 | AO7 | IDENTIFICATION OF X-RAY SELECTED SUPERNOVA REMNANTS | XIS | Y |
| G337.2-0.7 | 249.8782 | -47.8314 | 337.20769447 | -0.7291284 | 280.8005 | 56172.5530439815 | 56181.2598263889 | 507068010 | 304148.4 | 300000 | 304156.4 | 304148.4 | 0 | 304148.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 275844.8 | 275844.8 | 461263.8 | 9 | PROCESSED | 57607.2211111111 | 56018 | 56271.4641203704 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076001 | Suzaku found recombining plasma (RP) from the mixed-morphology SNRs (MM-SNRs). Since the standard evolution of SNR does not predict RP, the Suzaku discovery requires a dramatic change on the scenario of SNR dynamics and evolution. Suggestive facts are that all RP detected SNRs have OH masers and all RP-detected SNRs have TeV/GeV emissions. The most important issue at this stage, however, is not model making, but systematic and comprehensive observations to study which kind of SNRs, and/or which circum SN conditions, are responsible to RP. This is our primary objective. The second aim of this proposal is to provide path-finding data for the Astro-H science. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 7 | Ao7 | NEW SCENARIO FOR THE THERMAL PLASMA IN SNRS | XIS | Y |
| GRXE_E_2 | 267.6193 | -27.2463 | 2.00029183 | -0.04392641 | 105.0002 | 56366.4085532407 | 56368.7772569444 | 507069010 | 103687.3 | 100000 | 103687.3 | 103687.3 | 0 | 103687.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 95583.4 | 95583.4 | 204625.9 | 2 | PROCESSED | 57610.8702314815 | 56018 | 56379.6047106482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076002 | We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies. | GALACTIC DIFFUSE EMISSION | 5 | A | TSURU | TAKESHI | NULL | NULL | JAP | 7 | AO7 | ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE) | XIS | Y |
| GRXE_E_3 | 267.7634 | -27.0307 | 2.25114568 | -0.04369036 | 105.0001 | 56368.7777314815 | 56371.1111458333 | 507070010 | 101172.6 | 100000 | 101180.6 | 101172.6 | 0 | 101180.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 103602.8 | 103602.8 | 201589.8 | 0 | PROCESSED | 57610.8916782407 | 56018 | 56380.5799768518 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076002 | We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies. | GALACTIC DIFFUSE EMISSION | 5 | A | TSURU | TAKESHI | NULL | NULL | JAP | 7 | AO7 | ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE) | XIS | Y |
| GRXE_E_4 | 267.9068 | -26.8159 | 2.50111874 | -0.04382328 | 104.4995 | 56371.1118518518 | 56373.3049421296 | 507071010 | 101208.6 | 100000 | 101216.6 | 101208.6 | 0 | 101216.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 105649.1 | 105649.1 | 189451.9 | 1 | PROCESSED | 57610.9065625 | 56018 | 56384.6094560185 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076002 | We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies. | GALACTIC DIFFUSE EMISSION | 5 | A | TSURU | TAKESHI | NULL | NULL | JAP | 7 | AO7 | ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE) | XIS | Y |
| GRXE_E_5 | 268.0495 | -26.6011 | 2.75089625 | -0.04390767 | 105.4995 | 56373.3059722222 | 56375.3646990741 | 507072010 | 101243.5 | 100000 | 101243.5 | 101243.5 | 0 | 101243.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 102667.6 | 102667.6 | 177865.8 | 1 | PROCESSED | 57610.9241087963 | 56018 | 56384.595787037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076002 | We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies. | GALACTIC DIFFUSE EMISSION | 5 | A | TSURU | TAKESHI | NULL | NULL | JAP | 7 | AO7 | ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE) | XIS | Y |
| GRXE_E_6 | 268.1913 | -26.3855 | 3.00107417 | -0.0433749 | 104.9996 | 56375.3653125 | 56377.4119444445 | 507073010 | 101674.5 | 100000 | 101674.5 | 101674.5 | 0 | 101674.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 100247.3 | 100247.3 | 176807.8 | 1 | PROCESSED | 57610.9396296296 | 56018 | 56387.5561574074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076002 | We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies. | GALACTIC DIFFUSE EMISSION | 5 | A | TSURU | TAKESHI | NULL | NULL | JAP | 7 | AO7 | ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE) | XIS | Y |
| GRXE_E_9 | 268.0849 | -26.1545 | 3.15134991 | 0.15632851 | 103.0998 | 56385.8984490741 | 56388.2085648148 | 507074010 | 98651.6 | 100000 | 98659.6 | 98659.6 | 0 | 98651.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 83026.9 | 83026.9 | 199575.7 | 2 | PROCESSED | 57611.012650463 | 56018 | 56401.6405092593 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076002 | We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies. | GALACTIC DIFFUSE EMISSION | 5 | A | TSURU | TAKESHI | NULL | NULL | JAP | 7 | AO7 | ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE) | XIS | Y |
| GRXE_E_10 | 267.9015 | -25.9408 | 3.25115356 | 0.4070413 | 105.0001 | 56362.3793865741 | 56364.8778472222 | 507075010 | 101342.8 | 100000 | 101342.8 | 101342.8 | 0 | 101342.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 88242.2 | 88242.2 | 215806 | 2 | PROCESSED | 57610.8450462963 | 56018 | 56377.5882175926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076002 | We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies. | GALACTIC DIFFUSE EMISSION | 5 | A | TSURU | TAKESHI | NULL | NULL | JAP | 7 | AO7 | ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE) | XIS | Y |
| MBM16 | 49.752 | 11.6015 | 170.57212752 | -37.26756171 | 73.5786 | 56139.0841666667 | 56140.9710416667 | 507076010 | 24949.9 | 80000 | 24949.9 | 24949.9 | 0 | 24949.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18237.6 | 18237.6 | 162962 | 1 | PROCESSED | 57606.7578703704 | 56018 | 56260.533125 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076003 | Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions. | GALACTIC DIFFUSE EMISSION | 5 | A | GALEAZZI | MASSIMILIANO | NULL | NULL | USA | 7 | AO7 | CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE | XIS | Y |
| MBM16 | 49.7694 | 11.5801 | 170.60605682 | -37.27197306 | 254.9211 | 56331.4284606482 | 56333.553587963 | 507076020 | 80950.6 | 80000 | 80974.6 | 80950.6 | 0 | 80974.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 69307.6 | 69307.6 | 183583.9 | 2 | PROCESSED | 57610.5874074074 | 56018 | 56349.5813657407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076003 | Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions. | GALACTIC DIFFUSE EMISSION | 5 | A | GALEAZZI | MASSIMILIANO | NULL | NULL | USA | 7 | AO7 | CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE | XIS | Y |
| MBM36 | 238.3612 | -4.7913 | 4.00454082 | 35.69817373 | 279.4993 | 56155.0155787037 | 56156.7563425926 | 507077010 | 81015.8 | 80000 | 81015.8 | 81017.6 | 0 | 81017.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 80330.1 | 80330.1 | 150387.7 | 4 | PROCESSED | 57606.8991782407 | 56018 | 56170.1653240741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076003 | Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions. | GALACTIC DIFFUSE EMISSION | 5 | A | GALEAZZI | MASSIMILIANO | NULL | NULL | USA | 7 | AO7 | CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE | XIS | Y |
| LDN1563 | 75.5223 | 13.867 | 187.14890409 | -16.70886793 | 81.7388 | 56161.9528356482 | 56164.0488194444 | 507078010 | 78669.3 | 80000 | 78669.3 | 78669.3 | 0 | 78669.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 69680.1 | 69680.1 | 181061.9 | 0 | PROCESSED | 57606.963275463 | 56018 | 56212.8492476852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076003 | Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions. | GALACTIC DIFFUSE EMISSION | 5 | A | GALEAZZI | MASSIMILIANO | NULL | NULL | USA | 7 | AO7 | CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE | XIS | Y |
| MBM20 | 68.9377 | -14.6308 | 211.4041789 | -36.56532035 | 78.376 | 56164.0544328704 | 56166.3530092593 | 507079010 | 82881.4 | 80000 | 82881.4 | 82881.4 | 0 | 82881.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 73866.8 | 73866.8 | 198557.7 | 2 | PROCESSED | 57606.9726851852 | 56018 | 56212.7316087963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076003 | Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions. | GALACTIC DIFFUSE EMISSION | 5 | A | GALEAZZI | MASSIMILIANO | NULL | NULL | USA | 7 | AO7 | CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE | XIS | Y |
| 3C 397 | 286.9092 | 7.1226 | 41.11337729 | -0.33398163 | 251.9939 | 56595.6848611111 | 56597.9106828704 | 508001010 | 103515.7 | 100000 | 103515.7 | 103515.7 | 0 | 103515.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 98675.3 | 98675.3 | 192293.7 | 2 | PROCESSED | 57613.2313425926 | 57012 | 56645.6863541667 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080011 | 3C 397 is a Galactic Supernova remnant (SNR) ,whose X-ray spectrum has prominent Fe K line emission. We analyzed Suzaku AO5 data, it resulted in finding of Fe Lya Line. This is a symptomatic of over-ionized (recombining) plasma. On the other hand, the Fe K line center indicates under-ionized (ionizing) plasma. This means that 3C 397 may consisting of two opposite type of plasma: ionizing and recombining. Such a strange state of plasma is not discovered in any SNR.This discovery will be a key to uncovering a mystery of the origin of recombining plasma. However, we still not detect Fe Radiative recombination continuum (RRC),which is a evidence of recombining plasma. To detect the Fe RRC, we propose 150 ks additional observation of 3C 397. | GALACTIC DIFFUSE EMISSION | 5 | C | SUGAWARA | RYUSUKE | NULL | NULL | JAP | 8 | AO8 | THE INDICATION OF RECOMBINING PLASMA COEXISTING WITH IONIZING PLASMA IN 3C 397 | XIS | Y |
| W44_WEST | 283.939 | 1.3216 | 34.60037354 | -0.35787423 | 254.9999 | 56589.5109953704 | 56590.9655324074 | 508002010 | 61107.8 | 60000 | 61139.8 | 61107.8 | 0 | 61139.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 58445.8 | 58445.8 | 125667.8 | 1 | PROCESSED | 57613.10125 | 56970 | 56603.7391087963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080012 | W44 is a middle-aged supernova remnant (SNR) categorized to mixed-morphology SNR. We have observed the center region of W44 with Suzaku in the AO5 phase. The spectra are well reproduced by a thermal plasma in a recombining phase. While such plasmas have been found from several SNRs, the origin is still unclear. We also discover hard X-ray emission which shows an arc-like structure spatially-correlated with a radio continuum filament. No conventional model for particle acceleration could explain the mechanism of the hard X-ray emission. The entire plasma distribution of W44 will provide a clue to resolve the origins of the reombining plasma and the hard X-ray emission. We therefore require four pointing observations for totally 280 ks. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIDA | HIROYUKI | NULL | NULL | JAP | 8 | AO8 | MAPPING THE SPATIAL DISTRIBUTION OF HARD AND SOFT X-RAYS IN W44 | XIS | Y |
| W44_SOUTH | 284.0612 | 1.21 | 34.55680978 | -0.51750637 | 254.9998 | 56587.9436921296 | 56589.5105671296 | 508003010 | 66719.3 | 100000 | 66733.3 | 66728.4 | 0 | 66719.3 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 59540 | 59540 | 135343.9 | 0 | PROCESSED | 57613.1119675926 | 57193 | 56603.6796180556 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080012 | W44 is a middle-aged supernova remnant (SNR) categorized to mixed-morphology SNR. We have observed the center region of W44 with Suzaku in the AO5 phase. The spectra are well reproduced by a thermal plasma in a recombining phase. While such plasmas have been found from several SNRs, the origin is still unclear. We also discover hard X-ray emission which shows an arc-like structure spatially-correlated with a radio continuum filament. No conventional model for particle acceleration could explain the mechanism of the hard X-ray emission. The entire plasma distribution of W44 will provide a clue to resolve the origins of the reombining plasma and the hard X-ray emission. We therefore require four pointing observations for totally 280 ks. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIDA | HIROYUKI | NULL | NULL | JAP | 8 | AO8 | MAPPING THE SPATIAL DISTRIBUTION OF HARD AND SOFT X-RAYS IN W44 | XIS | Y |
| W44_SOUTH | 284.0546 | 1.2208 | 34.56340933 | -0.50670684 | 73.0006 | 56756.507025463 | 56757.3474074074 | 508003020 | 32369.6 | 33000 | 32377.6 | 32377.6 | 0 | 32369.6 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 29503.4 | 29503.4 | 72595.9 | 1 | PROCESSED | 57614.2259837963 | 57193 | 56825.6834027778 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080012 | W44 is a middle-aged supernova remnant (SNR) categorized to mixed-morphology SNR. We have observed the center region of W44 with Suzaku in the AO5 phase. The spectra are well reproduced by a thermal plasma in a recombining phase. While such plasmas have been found from several SNRs, the origin is still unclear. We also discover hard X-ray emission which shows an arc-like structure spatially-correlated with a radio continuum filament. No conventional model for particle acceleration could explain the mechanism of the hard X-ray emission. The entire plasma distribution of W44 will provide a clue to resolve the origins of the reombining plasma and the hard X-ray emission. We therefore require four pointing observations for totally 280 ks. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIDA | HIROYUKI | NULL | NULL | JAP | 8 | AO8 | MAPPING THE SPATIAL DISTRIBUTION OF HARD AND SOFT X-RAYS IN W44 | XIS | Y |
| W44_EAST | 284.1459 | 1.2991 | 34.67473844 | -0.5521979 | 254.9985 | 56583.3375231482 | 56584.8897337963 | 508004010 | 58296.5 | 60000 | 58304.5 | 58296.5 | 0 | 58314.9 | 3 | 2 | 0 | 3 | 1 | 0 | 0 | 52727.6 | 52727.6 | 134095.8 | 2 | PROCESSED | 57613.0782407407 | 57004 | 56637.6520949074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080012 | W44 is a middle-aged supernova remnant (SNR) categorized to mixed-morphology SNR. We have observed the center region of W44 with Suzaku in the AO5 phase. The spectra are well reproduced by a thermal plasma in a recombining phase. While such plasmas have been found from several SNRs, the origin is still unclear. We also discover hard X-ray emission which shows an arc-like structure spatially-correlated with a radio continuum filament. No conventional model for particle acceleration could explain the mechanism of the hard X-ray emission. The entire plasma distribution of W44 will provide a clue to resolve the origins of the reombining plasma and the hard X-ray emission. We therefore require four pointing observations for totally 280 ks. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIDA | HIROYUKI | NULL | NULL | JAP | 8 | AO8 | MAPPING THE SPATIAL DISTRIBUTION OF HARD AND SOFT X-RAYS IN W44 | XIS | Y |
| W44_NORTH | 283.9599 | 1.4928 | 34.76225024 | -0.29835298 | 254.9998 | 56584.8902083333 | 56586.2084837963 | 508005010 | 55645.9 | 60000 | 55701.9 | 55645.9 | 0 | 55700.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 47453.1 | 47453.1 | 113895.8 | 1 | PROCESSED | 57613.0578356482 | 56967 | 56597.6717824074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080012 | W44 is a middle-aged supernova remnant (SNR) categorized to mixed-morphology SNR. We have observed the center region of W44 with Suzaku in the AO5 phase. The spectra are well reproduced by a thermal plasma in a recombining phase. While such plasmas have been found from several SNRs, the origin is still unclear. We also discover hard X-ray emission which shows an arc-like structure spatially-correlated with a radio continuum filament. No conventional model for particle acceleration could explain the mechanism of the hard X-ray emission. The entire plasma distribution of W44 will provide a clue to resolve the origins of the reombining plasma and the hard X-ray emission. We therefore require four pointing observations for totally 280 ks. | GALACTIC DIFFUSE EMISSION | 5 | A | UCHIDA | HIROYUKI | NULL | NULL | JAP | 8 | AO8 | MAPPING THE SPATIAL DISTRIBUTION OF HARD AND SOFT X-RAYS IN W44 | XIS | Y |
| W28_SOUTH | 270.2522 | -23.558 | 6.38418356 | -0.23955939 | 89.9033 | 56738.9940393518 | 56740.1793518518 | 508006010 | 40851.8 | 100000 | 40883.8 | 40851.8 | 0 | 40894.2 | 1 | 1 | 0 | 2 | 1 | 0 | 0 | 35456.8 | 35456.8 | 102407.8 | 1 | PROCESSED | 57614.1110648148 | 57359 | 56754.6877083333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080017 | A series of discoveries of recombining plasma (RP) in mixed-morphology (MM) SNRs inspires us with a new scenario for SNR evolution. The observed spectra are well described by the picture that the plasma has experienced sudden cooling in the past and currently undergoes gradual recombination to ionization equilibrium. In the MM SNR W28, we found the spatial correlation between the radio brightness and the thermal evolution (recombination) phase. Hence, the radio-fainter region may have less recombined plasma. Such a plasma should emit strong Fe-K line from the He-like ions. The line flux reflects the initial temperature of RP, which brings the key information of the explosion environment of MM SNRs. For this purpose, we propose a 100-ks observation of W28 south, the possible 'youngest' RP. | GALACTIC DIFFUSE EMISSION | 5 | A | SAWADA | MAKOTO | NULL | NULL | JAP | 8 | AO8 | INITIAL PARAMETERS OF RECOMBINING PLASMA IN SUPERNOVA REMNANTS EXPLORED THROUGH W28 | XIS | Y |
| W28_SOUTH | 270.2594 | -23.5602 | 6.38554367 | -0.24638203 | 269.9307 | 56938.465162037 | 56939.7308101852 | 508006020 | 61734.6 | 60000 | 61734.6 | 61738.5 | 0 | 61746.5 | 3 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.6318402778 | 57359 | 56993.4258333333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080017 | A series of discoveries of recombining plasma (RP) in mixed-morphology (MM) SNRs inspires us with a new scenario for SNR evolution. The observed spectra are well described by the picture that the plasma has experienced sudden cooling in the past and currently undergoes gradual recombination to ionization equilibrium. In the MM SNR W28, we found the spatial correlation between the radio brightness and the thermal evolution (recombination) phase. Hence, the radio-fainter region may have less recombined plasma. Such a plasma should emit strong Fe-K line from the He-like ions. The line flux reflects the initial temperature of RP, which brings the key information of the explosion environment of MM SNRs. For this purpose, we propose a 100-ks observation of W28 south, the possible 'youngest' RP. | GALACTIC DIFFUSE EMISSION | 5 | A | SAWADA | MAKOTO | NULL | NULL | JAP | 8 | AO8 | INITIAL PARAMETERS OF RECOMBINING PLASMA IN SUPERNOVA REMNANTS EXPLORED THROUGH W28 | XIS | Y |
| NW_SRC | 221.7499 | -1.3162 | 351.9522425 | 50.22344256 | 289.0003 | 56499.3402430556 | 56499.8412037037 | 508007010 | 23554 | 20000 | 23554 | 23555.4 | 0 | 23554 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 24103 | 24103 | 43274 | 0 | PROCESSED | 57612.0357986111 | 56955 | 56587.4553819444 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080020 | Fermi Bubble is the giant gamma-ray structure discovered by Fermi-LAT, which provides direct evidence/hints for AGN activity of our Galactic center in the past. Very recently, MAXI has detected an isolated X-ray gisland h at the outermost part of NW edges of the bubble only seen at above 2keV, not associated with any structures or sources. Moreover, MAXI confirmed the presence of a thermal projection at the base of the Southern bubble embedded in the Galactic diffuse emission. Together with our knowledge obtained from AO7 observations across the North/South bubble edges, we propose to observe these two regions as a collaborative work with the MAXI-SSC team. We try to derive physical parameters of these giant X-ray structures and its possible association, interaction with the Fermi Bubble. | GALACTIC DIFFUSE EMISSION | 5 | B | TAHARA | MASAYA | NULL | NULL | JAP | 8 | AO8 | SUZAKU OBSERVATION OF THE GIGANTIC X-RAY STRUCTURES POSSIBLY ASSOCIATED WITH THE GFERMI BUBBLE H | XIS | Y |
| NW_BGD | 233.685 | -9.8963 | 355.50550051 | 35.80785483 | 289.7923 | 56499.8451041667 | 56500.4266319445 | 508008010 | 24127.5 | 20000 | 24127.5 | 24127.5 | 0 | 24127.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22040.2 | 22040.2 | 50216 | 1 | PROCESSED | 57612.0809953704 | 56955 | 56587.4600578704 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080020 | Fermi Bubble is the giant gamma-ray structure discovered by Fermi-LAT, which provides direct evidence/hints for AGN activity of our Galactic center in the past. Very recently, MAXI has detected an isolated X-ray gisland h at the outermost part of NW edges of the bubble only seen at above 2keV, not associated with any structures or sources. Moreover, MAXI confirmed the presence of a thermal projection at the base of the Southern bubble embedded in the Galactic diffuse emission. Together with our knowledge obtained from AO7 observations across the North/South bubble edges, we propose to observe these two regions as a collaborative work with the MAXI-SSC team. We try to derive physical parameters of these giant X-ray structures and its possible association, interaction with the Fermi Bubble. | GALACTIC DIFFUSE EMISSION | 5 | B | TAHARA | MASAYA | NULL | NULL | JAP | 8 | AO8 | SUZAKU OBSERVATION OF THE GIGANTIC X-RAY STRUCTURES POSSIBLY ASSOCIATED WITH THE GFERMI BUBBLE H | XIS | Y |
| SE_SRC | 287.3947 | -27.2493 | 9.97288902 | -15.74410072 | 84.5985 | 56404.7026967593 | 56405.330775463 | 508009010 | 20328.7 | 20000 | 20328.7 | 20328.7 | 0 | 20328.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17593.8 | 17593.8 | 54263.9 | 1 | PROCESSED | 57611.1595833333 | 56792 | 56425.5555092593 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080020 | Fermi Bubble is the giant gamma-ray structure discovered by Fermi-LAT, which provides direct evidence/hints for AGN activity of our Galactic center in the past. Very recently, MAXI has detected an isolated X-ray gisland h at the outermost part of NW edges of the bubble only seen at above 2keV, not associated with any structures or sources. Moreover, MAXI confirmed the presence of a thermal projection at the base of the Southern bubble embedded in the Galactic diffuse emission. Together with our knowledge obtained from AO7 observations across the North/South bubble edges, we propose to observe these two regions as a collaborative work with the MAXI-SSC team. We try to derive physical parameters of these giant X-ray structures and its possible association, interaction with the Fermi Bubble. | GALACTIC DIFFUSE EMISSION | 5 | B | TAHARA | MASAYA | NULL | NULL | JAP | 8 | AO8 | SUZAKU OBSERVATION OF THE GIGANTIC X-RAY STRUCTURES POSSIBLY ASSOCIATED WITH THE GFERMI BUBBLE H | XIS | Y |
| SE_BGD | 288.7458 | -25.773 | 11.87589948 | -16.28754896 | 81.8427 | 56405.3324537037 | 56405.8329050926 | 508010010 | 20965.3 | 20000 | 20969.3 | 20965.3 | 0 | 20973.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18762.6 | 18762.6 | 43234 | 0 | PROCESSED | 57618.7907291667 | 56792 | 56425.5426851852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080020 | Fermi Bubble is the giant gamma-ray structure discovered by Fermi-LAT, which provides direct evidence/hints for AGN activity of our Galactic center in the past. Very recently, MAXI has detected an isolated X-ray gisland h at the outermost part of NW edges of the bubble only seen at above 2keV, not associated with any structures or sources. Moreover, MAXI confirmed the presence of a thermal projection at the base of the Southern bubble embedded in the Galactic diffuse emission. Together with our knowledge obtained from AO7 observations across the North/South bubble edges, we propose to observe these two regions as a collaborative work with the MAXI-SSC team. We try to derive physical parameters of these giant X-ray structures and its possible association, interaction with the Fermi Bubble. | GALACTIC DIFFUSE EMISSION | 5 | B | TAHARA | MASAYA | NULL | NULL | JAP | 8 | AO8 | SUZAKU OBSERVATION OF THE GIGANTIC X-RAY STRUCTURES POSSIBLY ASSOCIATED WITH THE GFERMI BUBBLE H | XIS | Y |
| CAS A | 350.8704 | 58.8069 | 111.74200441 | -2.14072863 | 228.5251 | 56672.9492708333 | 56673.8064699074 | 508011010 | 0 | 120000 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57613.771412037 | 56717 | 56712.601400463 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080021 | We will propose a follow-up 120 ksec observations of a young supernova remnant Cassiopeia A. The long exposure provides us a high quality of the broad band spectrum from XIS to HXD GSO band. We will try to detect Mn-K line at 6.1 keV for the first time. The element Mn as well as Cr gives constraint on the explosion mechanism of the ejecta. We also test a predicted flux variation of a non-thermal emission in the PIN band for the first time. The variation gives critical information to solve the physical parameters in the reverse shock of the ejecta. | GALACTIC DIFFUSE EMISSION | 5 | B | MAEDA | YOSHITOMO | NULL | NULL | JAP | 8 | AO8 | MN/CR-K AND HARD X-RAY EMISSION IN CASSIOPEIA A | XIS | Y |
| CAS A | 350.8384 | 58.8278 | 111.73335389 | -2.11549771 | 73.3126 | 56828.040162037 | 56828.7711111111 | 508011020 | 28073.2 | 30000 | 28081.2 | 28073.2 | 0 | 29740.2 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 30997.1 | 30997.1 | 63143.9 | 2 | PROCESSED | 57615.2981712963 | 57206 | 56839.7807986111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080021 | We will propose a follow-up 120 ksec observations of a young supernova remnant Cassiopeia A. The long exposure provides us a high quality of the broad band spectrum from XIS to HXD GSO band. We will try to detect Mn-K line at 6.1 keV for the first time. The element Mn as well as Cr gives constraint on the explosion mechanism of the ejecta. We also test a predicted flux variation of a non-thermal emission in the PIN band for the first time. The variation gives critical information to solve the physical parameters in the reverse shock of the ejecta. | GALACTIC DIFFUSE EMISSION | 5 | B | MAEDA | YOSHITOMO | NULL | NULL | JAP | 8 | AO8 | MN/CR-K AND HARD X-RAY EMISSION IN CASSIOPEIA A | XIS | Y |
| HESS J1534-571 1 | 234.0464 | -57.1146 | 323.88573784 | -1.10331415 | 295.9997 | 56543.4345138889 | 56544.0210300926 | 508013010 | 36891 | 40000 | 36899 | 36891 | 0 | 36899 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 36070.4 | 36070.4 | 50671.9 | 0 | PROCESSED | 57612.5616319444 | 56990 | 56622.6022569444 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080024 | Supernova Remnants (SNRs) detected with TeV gamma-rays and synchrotron X-rays (TeV SNRs) are the most plausible acceleration sites of Galactic cosmic rays. However, the environments of such SNRs, temperature, density, and so on, are still unknown due to the lack of thermal X-ray emission in their spectra. HESS J1534-571 is a candidate of only several TeV SNRs which is located off Galactic plane. With good statistics and low background observation of Suzaku XIS, we will detect X-rays from this object for the first time, and identifying as a TeV SNR and if possible, detecting thermal X-rays from the target for the first time. Determining the thermal parameters will reveal us what kind of environment makes ordinal SNRs to TeV SNRs and how TeV SNRs accelerate cosmic rays in such condition. | GALACTIC DIFFUSE EMISSION | 5 | A | BAMBA | AYA | NULL | NULL | JAP | 8 | AO8 | RESOLVING THERMAL X-RAYS FROM A TEV SNR CANDIDATE HESS J1534-571 | XIS | Y |
| HESS J1534-571 2 | 233.1754 | -57.1 | 323.50919975 | -0.81659232 | 295.9986 | 56544.0219212963 | 56544.6695949074 | 508014010 | 38918.6 | 40000 | 38942.6 | 38918.6 | 0 | 38950.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36856.5 | 36856.5 | 55953.9 | 0 | PROCESSED | 57612.5722916667 | 56990 | 56622.6062268518 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080024 | Supernova Remnants (SNRs) detected with TeV gamma-rays and synchrotron X-rays (TeV SNRs) are the most plausible acceleration sites of Galactic cosmic rays. However, the environments of such SNRs, temperature, density, and so on, are still unknown due to the lack of thermal X-ray emission in their spectra. HESS J1534-571 is a candidate of only several TeV SNRs which is located off Galactic plane. With good statistics and low background observation of Suzaku XIS, we will detect X-rays from this object for the first time, and identifying as a TeV SNR and if possible, detecting thermal X-rays from the target for the first time. Determining the thermal parameters will reveal us what kind of environment makes ordinal SNRs to TeV SNRs and how TeV SNRs accelerate cosmic rays in such condition. | GALACTIC DIFFUSE EMISSION | 5 | A | BAMBA | AYA | NULL | NULL | JAP | 8 | AO8 | RESOLVING THERMAL X-RAYS FROM A TEV SNR CANDIDATE HESS J1534-571 | XIS | Y |
| HESS J1534-571 3 | 234.1055 | -57.4189 | 323.73309574 | -1.36851406 | 296.0043 | 56544.6705787037 | 56545.1793171296 | 508015010 | 38748.7 | 40000 | 38772.7 | 38764.7 | 0 | 38748.7 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 29947 | 29947 | 43943.9 | 0 | PROCESSED | 57612.5739814815 | 56956 | 56588.8303125 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080024 | Supernova Remnants (SNRs) detected with TeV gamma-rays and synchrotron X-rays (TeV SNRs) are the most plausible acceleration sites of Galactic cosmic rays. However, the environments of such SNRs, temperature, density, and so on, are still unknown due to the lack of thermal X-ray emission in their spectra. HESS J1534-571 is a candidate of only several TeV SNRs which is located off Galactic plane. With good statistics and low background observation of Suzaku XIS, we will detect X-rays from this object for the first time, and identifying as a TeV SNR and if possible, detecting thermal X-rays from the target for the first time. Determining the thermal parameters will reveal us what kind of environment makes ordinal SNRs to TeV SNRs and how TeV SNRs accelerate cosmic rays in such condition. | GALACTIC DIFFUSE EMISSION | 5 | A | BAMBA | AYA | NULL | NULL | JAP | 8 | AO8 | RESOLVING THERMAL X-RAYS FROM A TEV SNR CANDIDATE HESS J1534-571 | XIS | Y |
| HESS J1534-571 4 | 233.6872 | -56.8979 | 323.85352453 | -0.81317458 | 295.9989 | 56545.1801157407 | 56545.8042708333 | 508016010 | 42169.6 | 40000 | 42169.6 | 42193.6 | 0 | 42177.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39941.9 | 39941.9 | 53919.9 | 0 | PROCESSED | 57612.5878587963 | 56990 | 56625.6134953704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080024 | Supernova Remnants (SNRs) detected with TeV gamma-rays and synchrotron X-rays (TeV SNRs) are the most plausible acceleration sites of Galactic cosmic rays. However, the environments of such SNRs, temperature, density, and so on, are still unknown due to the lack of thermal X-ray emission in their spectra. HESS J1534-571 is a candidate of only several TeV SNRs which is located off Galactic plane. With good statistics and low background observation of Suzaku XIS, we will detect X-rays from this object for the first time, and identifying as a TeV SNR and if possible, detecting thermal X-rays from the target for the first time. Determining the thermal parameters will reveal us what kind of environment makes ordinal SNRs to TeV SNRs and how TeV SNRs accelerate cosmic rays in such condition. | GALACTIC DIFFUSE EMISSION | 5 | A | BAMBA | AYA | NULL | NULL | JAP | 8 | AO8 | RESOLVING THERMAL X-RAYS FROM A TEV SNR CANDIDATE HESS J1534-571 | XIS | Y |
| RX J1713.7-3946 NE | 258.6449 | -39.4419 | 347.70840856 | -0.44579664 | 85.9991 | 56714.667349537 | 56716.5279513889 | 508017010 | 100672.8 | 100000 | 100704.8 | 100696.8 | 0 | 100672.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 104394 | 104394 | 160727.7 | 1 | PROCESSED | 57613.9490162037 | 57093 | 56727.6718865741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080029 | We proposed Suzaku observation of a thermal emission line in the young TeV gamma-ray SNR RX J1713.7-3946. Most recently, we found the candidate of thermal emission line toward North-East of the SNR analyzed with Suzaku archive data. The region is present in the vicinity of the small molecular cloud interacts with the SNR shock wave. Main purpose is significant detection of the Si line about 5 sigma. This observation will be observable only with Suzaku and lead to a large step forward on cosmic-ray acceleration and shock-cloud interaction in the SNR. | GALACTIC DIFFUSE EMISSION | 5 | A | SANO | HIDETOSHI | NULL | NULL | JAP | 8 | AO8 | SUZAKU OBSERVATION OF A THERMAL EMISSION LINE IN THE SNR RX J1713.7-3946 | XIS | Y |
| SGR B | 266.8769 | -28.4429 | 0.6365241 | -0.09758916 | 267.0001 | 56556.6453472222 | 56559.2640740741 | 508018010 | 101955.8 | 100000 | 101955.8 | 101955.8 | 0 | 101955.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 87894 | 87894 | 226243.8 | 0 | PROCESSED | 57612.7499768518 | 56956 | 56588.5828125 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080043 | X-ray emissions from giant molecular clouds (X-ray reflection nebula) in the Galactic center region show past activity of the super-massive black hole, Sagittarius (Sgr) A*. Using Suzaku, we have found that Sgr A* had been in the active phase for almost a thousand years and dropped down to the quiescent level tens of years ago. However, no detailed information during the active phase and transition has been obtained from observations to study a mechanism of the sudden phase change. We aim to observe new information about time variability and relative positions from X-ray reflection nebulae to find the past light curve of Sgr A*. This work will be the grand sum for the Suzaku observation of the Galactic center. | GALACTIC DIFFUSE EMISSION | 5 | A | NOBUKAWA | MASAYOSHI | NULL | NULL | JAP | 8 | AO8 | PAST HISTORY OF THE SUPER-MASSIVE BLACK HOLE IN THE GALAXY | XIS | Y |
| SGR C | 266.1575 | -29.4721 | 359.43010365 | -0.09543697 | 265.018 | 56559.2657060185 | 56561.8960763889 | 508019010 | 104225.6 | 100000 | 104249.5 | 104241.5 | 0 | 104225.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 91197.5 | 91197.5 | 227241.9 | 1 | PROCESSED | 57612.8165277778 | 56956 | 56588.6596643518 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080043 | X-ray emissions from giant molecular clouds (X-ray reflection nebula) in the Galactic center region show past activity of the super-massive black hole, Sagittarius (Sgr) A*. Using Suzaku, we have found that Sgr A* had been in the active phase for almost a thousand years and dropped down to the quiescent level tens of years ago. However, no detailed information during the active phase and transition has been obtained from observations to study a mechanism of the sudden phase change. We aim to observe new information about time variability and relative positions from X-ray reflection nebulae to find the past light curve of Sgr A*. This work will be the grand sum for the Suzaku observation of the Galactic center. | GALACTIC DIFFUSE EMISSION | 5 | A | NOBUKAWA | MASAYOSHI | NULL | NULL | JAP | 8 | AO8 | PAST HISTORY OF THE SUPER-MASSIVE BLACK HOLE IN THE GALAXY | XIS | Y |
| CYG_COCOON2 | 306.1992 | 40.9463 | 78.99355785 | 1.86268914 | 253.1744 | 56603.8842939815 | 56605.000162037 | 508020010 | 46448.9 | 50000 | 46448.9 | 46448.9 | 0 | 46448.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44656.9 | 44656.9 | 96373.9 | 3 | PROCESSED | 57613.2763194444 | 57018 | 56652.6462152778 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080048 | The long-standing question on the origin of Galactic cosmic-rays (GCRs) is still not settled, and star-forming regions are promising sites for the production of GCRs. We propose deep observations of nearby star-forming region Cygnus X, aiming at GeV gamma-ray excess revealed by Fermi. By utilizing high sensitivity of the Suzaku XIS, particularly for diffuse X-rays, we can identify particle species (electrons or protons) and evaluate the cosmic-ray energy density and spatial distribution in this important object. | GALACTIC DIFFUSE EMISSION | 5 | C | MIZUNO | TSUNEFUMI | NULL | NULL | JAP | 8 | AO8 | SUZAKU INVESTIGATION OF PARTICLE ACCELERATION IN NEARBY STAR-FORMING REGION CYGNUS X | XIS | Y |
| HESSJ1858-A | 284.5878 | 2.0823 | 35.57325236 | -0.58765875 | 251.7991 | 56592.8339467593 | 56593.9759027778 | 508021010 | 51653.1 | 50000 | 51661.1 | 51669.1 | 0 | 51653.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48779.2 | 48779.2 | 98655.8 | 1 | PROCESSED | 57613.1533796296 | 56975 | 56608.6801388889 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080052 | HESS J1858+020 is one of the unidentified TeV objects which are candidates for the origin of the cosmic-ray protons. Recently a supernova remnant G35.6-0.4 and molecular clouds were discovered in the vicinity of HESSJ1858+020. The TeV emission may be generated through the interaction between protons accelerated in the SNR and the molecular clouds. However, a star forming region in the cloud was also discovered by an infrared observation, and the region may be responsible for the acceleration of protons. We propose Suzaku observations of HESSJ1858+020 to clarify what particles are the origin of the TeV emission, and to clarify what accelerates the particles. | GALACTIC DIFFUSE EMISSION | 5 | B | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 8 | AO8 | DECISION OF PARTICLE ACCELERATION SOURCE OF HESS J1858+020 WITH SUZAKU | XIS | Y |
| HESSJ1858-B | 284.4324 | 2.2013 | 35.60820996 | -0.39516335 | 251.7997 | 56593.9763310185 | 56595.1313541667 | 508022010 | 52595 | 50000 | 52619 | 52611 | 0 | 52595 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 49994.1 | 49994.1 | 99785.8 | 2 | PROCESSED | 57613.1665393518 | 56975 | 56608.7129166667 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080052 | HESS J1858+020 is one of the unidentified TeV objects which are candidates for the origin of the cosmic-ray protons. Recently a supernova remnant G35.6-0.4 and molecular clouds were discovered in the vicinity of HESSJ1858+020. The TeV emission may be generated through the interaction between protons accelerated in the SNR and the molecular clouds. However, a star forming region in the cloud was also discovered by an infrared observation, and the region may be responsible for the acceleration of protons. We propose Suzaku observations of HESSJ1858+020 to clarify what particles are the origin of the TeV emission, and to clarify what accelerates the particles. | GALACTIC DIFFUSE EMISSION | 5 | B | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 8 | AO8 | DECISION OF PARTICLE ACCELERATION SOURCE OF HESS J1858+020 WITH SUZAKU | XIS | Y |
| JUPITER | 103.7993 | 23.1163 | 192.50244401 | 11.09547038 | 264.3793 | 56762.0858912037 | 56762.3890277778 | 508023010 | 13090.5 | 160000 | 13090.5 | 13090.5 | 0 | 13090.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13005 | 13005 | 26183.9 | 0 | PROCESSED | 57614.2446527778 | 57212 | 56778.6117708333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080061 | Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 8 | AO8 | SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE | XIS | Y |
| JUPITER | 103.8407 | 23.1129 | 192.5219391 | 11.12856775 | 264.3937 | 56762.3891782407 | 56762.7223611111 | 508023020 | 15408.3 | 160000 | 15408.3 | 15408.3 | 0 | 15408.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12274.4 | 12274.4 | 28783.9 | 1 | PROCESSED | 57614.2553819445 | 57212 | 56778.6154166667 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080061 | Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 8 | AO8 | SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE | XIS | Y |
| JUPITER | 103.8837 | 23.1078 | 192.54363279 | 11.16228902 | 264.4065 | 56762.7225115741 | 56763.066099537 | 508023030 | 8912.5 | 160000 | 8912.5 | 8912.5 | 0 | 8912.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 6906.3 | 6906.3 | 22646.9 | 0 | PROCESSED | 57614.254212963 | 57212 | 56833.5559722222 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080061 | Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 8 | AO8 | SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE | XIS | Y |
| JUPITER | 103.925 | 23.1078 | 192.55993514 | 11.19674467 | 264.4254 | 56763.06625 | 56763.3890162037 | 508023040 | 14569.3 | 160000 | 14577.3 | 14569.3 | 0 | 14584.7 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57614.9505902778 | 57212 | 56839.6932175926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080061 | Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 8 | AO8 | SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE | XIS | Y |
| JUPITER | 103.9685 | 23.1027 | 192.5818164 | 11.23089407 | 264.4391 | 56763.3891666667 | 56763.722349537 | 508023050 | 14310.6 | 160000 | 14310.6 | 14320.7 | 0 | 14320.7 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57614.9511111111 | 57212 | 56782.4912731482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080061 | Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 8 | AO8 | SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE | XIS | Y |
| JUPITER | 104.0103 | 23.0994 | 192.60135744 | 11.26438783 | 264.454 | 56763.7225 | 56764.0627083333 | 508023060 | 8869.6 | 160000 | 8877.6 | 8869.6 | 0 | 8885.6 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57614.9524652778 | 57212 | 56846.5928472222 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080061 | Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 8 | AO8 | SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE | XIS | Y |
| JUPITER | 104.0402 | 23.0972 | 192.61518388 | 11.28841687 | 264.4641 | 56764.0628125 | 56764.1911805556 | 508023070 | 4557.7 | 160000 | 4557.7 | 4557.7 | 0 | 4573.7 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57614.9502777778 | 57212 | 56782.4904976852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080061 | Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 8 | AO8 | SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE | XIS | Y |
| JUPITER | 104.3277 | 23.0738 | 192.75008442 | 11.51865374 | 264.5662 | 56766.1211111111 | 56766.4481365741 | 508023080 | 15961.6 | 160000 | 15977.6 | 15961.6 | 0 | 15980.6 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57614.9566782407 | 57212 | 56782.5045486111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080061 | Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 8 | AO8 | SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE | XIS | Y |
| JUPITER | 104.3715 | 23.0706 | 192.77027841 | 11.55390373 | 264.582 | 56766.448287037 | 56766.781400463 | 508023090 | 11945.4 | 160000 | 11953.4 | 11945.4 | 0 | 11961.4 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57614.9588773148 | 57212 | 56782.506099537 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080061 | Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 8 | AO8 | SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE | XIS | Y |
| JUPITER | 104.4171 | 23.0664 | 192.79210183 | 11.59024455 | 264.5983 | 56766.7815972222 | 56767.1147916667 | 508023100 | 9375.9 | 160000 | 9383.9 | 9391.9 | 0 | 9375.9 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57614.9623263889 | 57212 | 56782.4942824074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080061 | Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 8 | AO8 | SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE | XIS | Y |
| JUPITER | 104.4639 | 23.0622 | 192.81439153 | 11.62759441 | 264.6138 | 56767.1149421296 | 56767.448125 | 508023110 | 16741.7 | 160000 | 16741.7 | 16773.7 | 0 | 16765.7 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57614.9630671296 | 57212 | 56789.801712963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080061 | Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 8 | AO8 | SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE | XIS | Y |
| JUPITER | 104.5088 | 23.0594 | 192.8346306 | 11.66394816 | 267.1301 | 56767.4497106482 | 56767.7814583333 | 508023120 | 11189.4 | 160000 | 11189.4 | 11196.1 | 0 | 11197.4 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57614.962974537 | 57212 | 56789.8021759259 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080061 | Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 8 | AO8 | SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE | XIS | Y |
| JUPITER | 104.5549 | 23.0543 | 192.85746904 | 11.70034918 | 267.1462 | 56767.7816087963 | 56768.1147916667 | 508023130 | 10090.6 | 160000 | 10098.6 | 10098.6 | 0 | 10090.6 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57614.9649652778 | 57212 | 56782.5091782407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080061 | Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 8 | AO8 | SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE | XIS | Y |
| JUPITER | 104.585 | 23.053 | 192.87049462 | 11.72496816 | 267.157 | 56768.1148958333 | 56768.2245138889 | 508023140 | 5248.2 | 160000 | 5264.2 | 5248.2 | 0 | 5270.8 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57614.9659259259 | 57212 | 56846.5934143518 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080061 | Suzaku observation of Jupiter in early 2006 detected diffuse hard X-ray emission, with spatial size 6 times the Jovian diameter and elongation along the inner radiation belt. This indicates that electrons are accelerated up to several tens of MeV and confined in a very large region. We propose simultaneous X-ray, EUV, and radio observations of Jupiter's magnetosphere with Suzaku, EXCEED, and the Tohoku radio telescope. Unprecedented wide band observations covering the inner radiation belt, the Io plasma torus, and Jupiter's aurorae will reveal how electrons are accelerated around Jupiter. | GALACTIC DIFFUSE EMISSION | 5 | A | EZOE | YUICHIRO | NULL | NULL | JAP | 8 | AO8 | SIMULTANEOUS X-RAY, EUV, AND RADIO OBSERVATIONS OF JUPITER'S MAGNETOSPHERE | XIS | Y |
| SS433_JET_KNOT | 288.5694 | 4.9037 | 39.90628699 | -2.82264549 | 256.6998 | 56597.9130555556 | 56600.2502314815 | 508024010 | 106894.2 | 100000 | 106894.2 | 106894.2 | 0 | 106894.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 102458.3 | 102458.3 | 201889.7 | 3 | PROCESSED | 57613.2427777778 | 56980 | 56611.6875578704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080065 | We propose an observation of the jet of SS 433. Our purpose is to detect high-temperature diffuse plasma component made by the black hole jet. | GALACTIC DIFFUSE EMISSION | 5 | C | UCHIYAMA | HIDEKI | NULL | NULL | JAP | 8 | AO8 | SEARCHING DIFFUSE HOT-PLASMA COMPONENT MADE BY A BLACK HOLE JET OF SS 433 | XIS | Y |
| VELA JR WEST1 | 131.7706 | -46.5645 | 265.90247722 | -2.02224689 | 126.9994 | 56630.5848611111 | 56631.1640162037 | 508036010 | 28550.9 | 30000 | 28558.9 | 28558.9 | 0 | 28550.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27350 | 27350 | 50017.9 | 0 | PROCESSED | 57613.5034375 | 57061 | 56695.6005092593 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080082 | We propose to observe toward West-rim of the SNR Vela Jr (RX J0852.0-4622). Recent our CO and HI data have revealed a dense interaction between SNR shock wave and the interstellar gas. Particularly, we found the synchrotron X-ray enhancement around the molecular core in the West-rim. This results indicate an efficient particle acceleration cased by shock-cloud interaction. This further observation allow us to investigate a more detail spectrum analysis comparable for the molecular core distribution. | GALACTIC DIFFUSE EMISSION | 5 | C | SANO | HIDETOSHI | NULL | NULL | JAP | 8 | AO8 | FURTHER OBSERVATIONS TOWARD WEST-RIM OF THE SNR VELA JR. WITH SUZAKU | XIS | Y |
| VELA JR WEST2 | 131.7715 | -45.9871 | 265.452568 | -1.6600557 | 116.213 | 56619.4434490741 | 56620.0800115741 | 508037010 | 29185 | 30000 | 29193 | 29201 | 0 | 29185 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35065.2 | 35065.2 | 54985.9 | 1 | PROCESSED | 57613.3840277778 | 56995 | 56629.6443055556 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080082 | We propose to observe toward West-rim of the SNR Vela Jr (RX J0852.0-4622). Recent our CO and HI data have revealed a dense interaction between SNR shock wave and the interstellar gas. Particularly, we found the synchrotron X-ray enhancement around the molecular core in the West-rim. This results indicate an efficient particle acceleration cased by shock-cloud interaction. This further observation allow us to investigate a more detail spectrum analysis comparable for the molecular core distribution. | GALACTIC DIFFUSE EMISSION | 5 | C | SANO | HIDETOSHI | NULL | NULL | JAP | 8 | AO8 | FURTHER OBSERVATIONS TOWARD WEST-RIM OF THE SNR VELA JR. WITH SUZAKU | XIS | Y |
| VELA JR WEST3 | 131.773 | -46.2743 | 265.67717372 | -1.83917649 | 116.21 | 56620.0804861111 | 56620.7320949074 | 508038010 | 34961.1 | 30000 | 34991.1 | 34961.1 | 0 | 34961.1 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 40443.4 | 40443.4 | 56295.9 | 0 | PROCESSED | 57613.4017708333 | 56995 | 56629.6399421296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080082 | We propose to observe toward West-rim of the SNR Vela Jr (RX J0852.0-4622). Recent our CO and HI data have revealed a dense interaction between SNR shock wave and the interstellar gas. Particularly, we found the synchrotron X-ray enhancement around the molecular core in the West-rim. This results indicate an efficient particle acceleration cased by shock-cloud interaction. This further observation allow us to investigate a more detail spectrum analysis comparable for the molecular core distribution. | GALACTIC DIFFUSE EMISSION | 5 | C | SANO | HIDETOSHI | NULL | NULL | JAP | 8 | AO8 | FURTHER OBSERVATIONS TOWARD WEST-RIM OF THE SNR VELA JR. WITH SUZAKU | XIS | Y |
| VELA PWN W1 | 128.3503 | -45.1912 | 263.35940671 | -3.07091685 | 303.5014 | 56438.6169444444 | 56439.0342476852 | 508042010 | 14117.2 | 15000 | 14117.2 | 14125.2 | 0 | 14125.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13284.4 | 13284.4 | 36023.9 | 0 | PROCESSED | 57611.3765046296 | 56864 | 56498.6138888889 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080090 | We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the western direction. Our immediate objective is to investigate how much extended the Vela PWN is in the west where the thermal pressure is significantly lower than that in the other directions we observed so far. The comparison of the X-ray extent in different directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component. The GeV PWN is also covered. | GALACTIC DIFFUSE EMISSION | 5 | B | MORI | KOJI | NULL | NULL | JAP | 8 | AO8 | SUZAKU REVEALS AN UNKNOWN DIFFUSE COMPONENT OF THE VELA PULSAR WIND NEBULA | XIS | Y |
| VELA PWN W2 | 127.3498 | -45.1919 | 262.94388066 | -3.64107383 | 303.5006 | 56439.0351851852 | 56439.4696643518 | 508043010 | 19584.4 | 15000 | 19592.4 | 19584.4 | 0 | 19600.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15626.6 | 15626.6 | 37533.9 | 1 | PROCESSED | 57611.391875 | 56816 | 56450.7935532407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080090 | We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the western direction. Our immediate objective is to investigate how much extended the Vela PWN is in the west where the thermal pressure is significantly lower than that in the other directions we observed so far. The comparison of the X-ray extent in different directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component. The GeV PWN is also covered. | GALACTIC DIFFUSE EMISSION | 5 | B | MORI | KOJI | NULL | NULL | JAP | 8 | AO8 | SUZAKU REVEALS AN UNKNOWN DIFFUSE COMPONENT OF THE VELA PULSAR WIND NEBULA | XIS | Y |
| VELA PWN W3 | 126.9052 | -45.2087 | 262.77480933 | -3.90558145 | 95.0008 | 56590.9784606482 | 56591.4343055556 | 508044010 | 13871 | 15000 | 13871 | 13871 | 0 | 13871 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11344.8 | 11344.8 | 39379.9 | 1 | PROCESSED | 57613.1197106482 | 57009 | 56643.6595949074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080090 | We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the western direction. Our immediate objective is to investigate how much extended the Vela PWN is in the west where the thermal pressure is significantly lower than that in the other directions we observed so far. The comparison of the X-ray extent in different directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component. The GeV PWN is also covered. | GALACTIC DIFFUSE EMISSION | 5 | B | MORI | KOJI | NULL | NULL | JAP | 8 | AO8 | SUZAKU REVEALS AN UNKNOWN DIFFUSE COMPONENT OF THE VELA PULSAR WIND NEBULA | XIS | Y |
| VELA PWN W4 | 126.476 | -45.2086 | 262.5995548 | -4.15230559 | 95.0003 | 56591.4348726852 | 56591.8813888889 | 508045010 | 16858.8 | 15000 | 16884.3 | 16858.8 | 0 | 16874.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16005.5 | 16005.5 | 38578 | 0 | PROCESSED | 57613.1152893518 | 57009 | 56643.6542708333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080090 | We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the western direction. Our immediate objective is to investigate how much extended the Vela PWN is in the west where the thermal pressure is significantly lower than that in the other directions we observed so far. The comparison of the X-ray extent in different directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component. The GeV PWN is also covered. | GALACTIC DIFFUSE EMISSION | 5 | B | MORI | KOJI | NULL | NULL | JAP | 8 | AO8 | SUZAKU REVEALS AN UNKNOWN DIFFUSE COMPONENT OF THE VELA PULSAR WIND NEBULA | XIS | Y |
| VELA PWN W5 | 126.0444 | -45.2057 | 262.42223435 | -4.39970467 | 94.9992 | 56591.8819560185 | 56592.3202777778 | 508046010 | 15856.9 | 15000 | 15872.9 | 15856.9 | 0 | 15880.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12735.8 | 12735.8 | 37863.9 | 0 | PROCESSED | 57613.1438657407 | 57009 | 56643.6567824074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080090 | We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the western direction. Our immediate objective is to investigate how much extended the Vela PWN is in the west where the thermal pressure is significantly lower than that in the other directions we observed so far. The comparison of the X-ray extent in different directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component. The GeV PWN is also covered. | GALACTIC DIFFUSE EMISSION | 5 | B | MORI | KOJI | NULL | NULL | JAP | 8 | AO8 | SUZAKU REVEALS AN UNKNOWN DIFFUSE COMPONENT OF THE VELA PULSAR WIND NEBULA | XIS | Y |
| VELA PWN W6 | 125.6171 | -45.2116 | 262.25511101 | -4.65051542 | 95.0008 | 56592.3208912037 | 56592.8209722222 | 508047010 | 17239.8 | 15000 | 17247.8 | 17239.8 | 0 | 17239.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16229.9 | 16229.9 | 43199.9 | 0 | PROCESSED | 57613.1284606482 | 57011 | 56645.5849421296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080090 | We have recently revealed that the X-ray extent of the Vela pulsar wind nebula (PWN) is larger than the radio extent, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. We here propose a mapping observation in the western direction. Our immediate objective is to investigate how much extended the Vela PWN is in the west where the thermal pressure is significantly lower than that in the other directions we observed so far. The comparison of the X-ray extent in different directions with different environmental conditions will provide key information of origin of the faint, newly-discovered component. The GeV PWN is also covered. | GALACTIC DIFFUSE EMISSION | 5 | B | MORI | KOJI | NULL | NULL | JAP | 8 | AO8 | SUZAKU REVEALS AN UNKNOWN DIFFUSE COMPONENT OF THE VELA PULSAR WIND NEBULA | XIS | Y |
| G359.0-0.9 NE | 266.7211 | -30.1578 | 359.09932581 | -0.86996543 | 100.9984 | 56720.9624537037 | 56722.041875 | 508057010 | 49815.6 | 50000 | 49815.6 | 49839.6 | 0 | 49823.6 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 45009.7 | 45009.7 | 93247.9 | 1 | PROCESSED | 57613.9450925926 | 57102 | 56740.6678009259 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080113 | We detected X-ray emission along the radio shell of G359.0-0.9 located toward the Galactic Center region. The spectral structure shows strong emission like structures at H-like Mg Ly alpha, H-like Si Ly alpha, He-like Ne RRC and He-like Mg RRC. This is the first hint for over ionized plasma in a shell-type SNR. We make three pointing observations with XIS covering the whole of G359.0-0.9 and obtain firm evidence for the ionized plasma. | GALACTIC DIFFUSE EMISSION | 5 | A | TSURU | TAKESHI | NULL | NULL | JAP | 8 | AO8 | FIRST DETECTION OF OVER IONIZED PLASMA IN A SHELL TYPE SNR : OBSERVATION OF G359.0-0.9 IN THE GALACTIC CENTER REGION | XIS | Y |
| G359.0-0.9 NW | 266.56 | -30.3287 | 358.88098313 | -0.83974756 | 102 | 56723.5510648148 | 56724.8162268518 | 508058010 | 52088.5 | 50000 | 52088.5 | 52096.5 | 0 | 52104.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45573.8 | 45573.8 | 109275.8 | 2 | PROCESSED | 57613.9935416667 | 57100 | 56734.6649189815 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080113 | We detected X-ray emission along the radio shell of G359.0-0.9 located toward the Galactic Center region. The spectral structure shows strong emission like structures at H-like Mg Ly alpha, H-like Si Ly alpha, He-like Ne RRC and He-like Mg RRC. This is the first hint for over ionized plasma in a shell-type SNR. We make three pointing observations with XIS covering the whole of G359.0-0.9 and obtain firm evidence for the ionized plasma. | GALACTIC DIFFUSE EMISSION | 5 | A | TSURU | TAKESHI | NULL | NULL | JAP | 8 | AO8 | FIRST DETECTION OF OVER IONIZED PLASMA IN A SHELL TYPE SNR : OBSERVATION OF G359.0-0.9 IN THE GALACTIC CENTER REGION | XIS | Y |
| G359.0-0.9 S | 266.8698 | -30.3116 | 359.03431589 | -1.05952932 | 101.9997 | 56724.8167013889 | 56726.0627662037 | 508059010 | 53496.1 | 50000 | 53496.1 | 53503.1 | 0 | 53520.1 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 47992.1 | 47992.1 | 107655.9 | 1 | PROCESSED | 57614.0007175926 | 57106 | 56740.7217013889 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080113 | We detected X-ray emission along the radio shell of G359.0-0.9 located toward the Galactic Center region. The spectral structure shows strong emission like structures at H-like Mg Ly alpha, H-like Si Ly alpha, He-like Ne RRC and He-like Mg RRC. This is the first hint for over ionized plasma in a shell-type SNR. We make three pointing observations with XIS covering the whole of G359.0-0.9 and obtain firm evidence for the ionized plasma. | GALACTIC DIFFUSE EMISSION | 5 | A | TSURU | TAKESHI | NULL | NULL | JAP | 8 | AO8 | FIRST DETECTION OF OVER IONIZED PLASMA IN A SHELL TYPE SNR : OBSERVATION OF G359.0-0.9 IN THE GALACTIC CENTER REGION | XIS | Y |
| VELA JR SE1 | 133.9641 | -46.7818 | 267.02895458 | -1.00032542 | 109.9994 | 56621.589525463 | 56622.3175462963 | 508060010 | 40599.6 | 40000 | 40599.6 | 40599.6 | 0 | 40605.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46653.5 | 46653.5 | 62895.9 | 0 | PROCESSED | 57613.4271990741 | 56998 | 56632.5928240741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080117 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southeastern rim of the remnant. Suzaku XIS images obtained by our AO2 and 3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) completing the X-ray image, (2) separating the radiation from the pulsar wind nebula PSR J0855-4644 which exists nearby Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | C | FUKUYAMA | TARO | NULL | NULL | JAP | 8 | AO8 | OBSERVATION OF SOUTHEASTERN RIM OF THE SUPARNOVA REMNANT VELA JR. | XIS | Y |
| VELA JR SE2 | 133.8563 | -47.0644 | 267.19687484 | -1.23927515 | 109.9991 | 56620.734375 | 56621.062650463 | 508061010 | 14449.2 | 15000 | 14449.2 | 14471.1 | 0 | 14457.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 18799.7 | 18799.7 | 28359.9 | 0 | PROCESSED | 57613.398912037 | 56998 | 56632.5722685185 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080117 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southeastern rim of the remnant. Suzaku XIS images obtained by our AO2 and 3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) completing the X-ray image, (2) separating the radiation from the pulsar wind nebula PSR J0855-4644 which exists nearby Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | C | FUKUYAMA | TARO | NULL | NULL | JAP | 8 | AO8 | OBSERVATION OF SOUTHEASTERN RIM OF THE SUPARNOVA REMNANT VELA JR. | XIS | Y |
| VELA JR SE3 | 133.7724 | -47.2478 | 267.30006641 | -1.40128647 | 110.0008 | 56629.9618055556 | 56630.5806828704 | 508062010 | 27363.8 | 25000 | 27364.4 | 27363.8 | 0 | 27365.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21714.1 | 21714.1 | 53459.9 | 1 | PROCESSED | 57613.4843055556 | 57005 | 56639.5938888889 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080117 | We propose to complete our mapping observations of SNR Vela Jr (RX J0852.0-4622) by covering the southeastern rim of the remnant. Suzaku XIS images obtained by our AO2 and 3 program clearly reveal an energy-dependent morphology of Vela Jr for the first time, which strenghens our motivation to cover the whole remnant with Suzaku. We are aiming at (1) completing the X-ray image, (2) separating the radiation from the pulsar wind nebula PSR J0855-4644 which exists nearby Vela Jr. | GALACTIC DIFFUSE EMISSION | 5 | C | FUKUYAMA | TARO | NULL | NULL | JAP | 8 | AO8 | OBSERVATION OF SOUTHEASTERN RIM OF THE SUPARNOVA REMNANT VELA JR. | XIS | Y |
| SGR A | 266.5133 | -28.9285 | 0.05589981 | -0.0769322 | 266.9997 | 56555.4484490741 | 56556.6446875 | 508064010 | 50456.9 | 50000 | 50456.9 | 50456.9 | 0 | 50456.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45224.8 | 45224.8 | 103308 | 0 | PROCESSED | 57612.6971527778 | 56956 | 56588.757025463 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080143 | X-ray emissions from giant molecular clouds (X-ray reflection nebula) in the Galactic center region show past activity of the super-massive black hole, Sagittarius (Sgr) A*. Using Suzaku, we have found that Sgr A* had been in the active phase for almost a thousand years and dropped down to the quiescent level tens of years ago. However, no detailed information during the active phase and transition has been obtained from observations to study a mechanism of the sudden phase change. We aim to observe new information about time variability and relative positions from X-ray reflection nebulae to find the past light curve of Sgr A*. This work will be the grand sum for the Suzaku observation of the Galactic center. | GALACTIC DIFFUSE EMISSION | 5 | A | NOBUKAWA | MASAYOSHI | MAEDA | YOSHITOMO | JAP | 8 | AO8 | PAST HISTORY OF THE SUPER-MASSIVE BLACK HOLE IN THE GALAXY | XIS | Y |
| RX J1713 SOUTHEAST | 258.9281 | -40.015 | 347.36958165 | -0.95677146 | 84 | 56711.6431018518 | 56713.2190046296 | 508067010 | 80077.4 | 80000 | 80085.4 | 80085.4 | 0 | 80077.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 74929.1 | 74929.1 | 118006.9 | 0 | PROCESSED | 57613.9112152778 | 57173 | 56806.6951851852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081313 | Detecting thermal emission and determining the ambient density are the missing keys to constrain hadronic acceleration in X-ray synchrotron-dominated SNRs. In the prototypical CR accelerator RX J1713.7-3946, X-ray thermal emission has been sought for over a decade, without success. Deep Suzaku observations will constrain either the conditions of the ambient medium in which the SNR is evolving, or the SN progenitor type (core-collapse or thermonuclear) and nucleosynthesis yield. | GALACTIC DIFFUSE EMISSION | 5 | A | ACERO | FABIO | NULL | NULL | USA | 8 | AO8 | STUDY OF THE THERMAL EMISSION IN THE SYNCHROTRON DOMINATED SNR RX J1713.7-3946 | XIS | Y |
| RX J1713 CENTER | 258.5686 | -39.6657 | 347.49241435 | -0.52884605 | 86.0002 | 56713.2203125 | 56714.6669212963 | 508068010 | 82061.5 | 80000 | 82069.5 | 82069.5 | 0 | 82061.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34805.9 | 34805.9 | 50331.9 | 0 | PROCESSED | 57613.9125231482 | 57089 | 56723.6064699074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081313 | Detecting thermal emission and determining the ambient density are the missing keys to constrain hadronic acceleration in X-ray synchrotron-dominated SNRs. In the prototypical CR accelerator RX J1713.7-3946, X-ray thermal emission has been sought for over a decade, without success. Deep Suzaku observations will constrain either the conditions of the ambient medium in which the SNR is evolving, or the SN progenitor type (core-collapse or thermonuclear) and nucleosynthesis yield. | GALACTIC DIFFUSE EMISSION | 5 | B | ACERO | FABIO | NULL | NULL | USA | 8 | AO8 | STUDY OF THE THERMAL EMISSION IN THE SYNCHROTRON DOMINATED SNR RX J1713.7-3946 | XIS | Y |
| N63A | 83.9019 | -66.0368 | 275.90835505 | -32.28360929 | 166.1398 | 56628.8025347222 | 56629.9556828704 | 508071010 | 82038.7 | 80000 | 82046.7 | 82038.7 | 0 | 82046.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70812.9 | 70812.9 | 99611.9 | 3 | PROCESSED | 57613.5008680556 | 56383 | 56639.6281365741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081315 | We propose deep observations of the LMC SNRs N63A and 0509-67.5. The Chandra observation of N63A showed possible signatures of He-like Fe emission and radiative recombination continua of Si and S. With the new observation by Suzaku, we will determine the plasma state of this SNR. The remarkable characteristic of 0509-67.5 is its extremely-low ionization age. This SNR, therefore, provides us a unique opportunity to explore detailed emission features of lowly-ionized atoms. The immediate objective of this observation is to accurately measure the Fe K-beta to K-alpha flux ratio to constrain the dominant charge state of the Fe ejecta. Both observations will provide us crucial datasets useful to improve our knowledge of SNR plasma and atomic physics. | GALACTIC DIFFUSE EMISSION | 5 | B | YAMAGUCHI | HIROYA | NULL | NULL | USA | 8 | AO8 | LEAVING A LEGACY OF SUZAKU: HIGH-QUALITY SPECTRAL DATASET ON IMPORTANT SNRS | XIS | Y |
| 0509-67.5 | 77.4163 | -67.5163 | 278.13367069 | -34.57909379 | 302.8449 | 56393.0595949074 | 56397.1258912037 | 508072010 | 175919.2 | 320000 | 175935.2 | 175919.2 | 0 | 175943.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 166666.8 | 166666.8 | 351291.6 | 3 | PROCESSED | 57611.1504513889 | 56383 | 56425.6930439815 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081315 | We propose deep observations of the LMC SNRs N63A and 0509-67.5. The Chandra observation of N63A showed possible signatures of He-like Fe emission and radiative recombination continua of Si and S. With the new observation by Suzaku, we will determine the plasma state of this SNR. The remarkable characteristic of 0509-67.5 is its extremely-low ionization age. This SNR, therefore, provides us a unique opportunity to explore detailed emission features of lowly-ionized atoms. The immediate objective of this observation is to accurately measure the Fe K-beta to K-alpha flux ratio to constrain the dominant charge state of the Fe ejecta. Both observations will provide us crucial datasets useful to improve our knowledge of SNR plasma and atomic physics. | GALACTIC DIFFUSE EMISSION | 5 | B | YAMAGUCHI | HIROYA | NULL | NULL | USA | 8 | AO8 | LEAVING A LEGACY OF SUZAKU: HIGH-QUALITY SPECTRAL DATASET ON IMPORTANT SNRS | XIS | Y |
| 0509-67.5 | 77.4191 | -67.5347 | 278.15520093 | -34.57404921 | 36.9172 | 56491.0670601852 | 56495.4689583333 | 508072020 | 152651.7 | 150000 | 152699.7 | 152651.7 | 0 | 152699.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 139753.6 | 139753.6 | 380299.4 | 7 | PROCESSED | 57612.009537037 | 56383 | 56509.8769097222 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081315 | We propose deep observations of the LMC SNRs N63A and 0509-67.5. The Chandra observation of N63A showed possible signatures of He-like Fe emission and radiative recombination continua of Si and S. With the new observation by Suzaku, we will determine the plasma state of this SNR. The remarkable characteristic of 0509-67.5 is its extremely-low ionization age. This SNR, therefore, provides us a unique opportunity to explore detailed emission features of lowly-ionized atoms. The immediate objective of this observation is to accurately measure the Fe K-beta to K-alpha flux ratio to constrain the dominant charge state of the Fe ejecta. Both observations will provide us crucial datasets useful to improve our knowledge of SNR plasma and atomic physics. | GALACTIC DIFFUSE EMISSION | 5 | B | YAMAGUCHI | HIROYA | NULL | NULL | USA | 8 | AO8 | LEAVING A LEGACY OF SUZAKU: HIGH-QUALITY SPECTRAL DATASET ON IMPORTANT SNRS | XIS | Y |
| MBM16-OFF | 46.1075 | 13.1563 | 165.8625544 | -38.38773927 | 69.5985 | 56513.919849537 | 56515.9119791667 | 508073010 | 83056.5 | 80000 | 83056.5 | 83056.5 | 0 | 83056.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 81138.6 | 81138.6 | 172097.9 | 2 | PROCESSED | 57612.2143981482 | 56953 | 56587.5588541667 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081322 | We propose the observation of three off-cloud targets near the targets of the Solar Wind Charge Exchange (SWCX) Key Project to study the properties of the Diffuse X-ray Background below 1 keV, with particular focus on the characterization of the Galactic Halo. The Key Project targets are at a distance of a few hundreds pc from the Sun and their high density portions shields about 90% of X-rays at the O VII energy, our proposed targets, instead, shield only about 50% of the Galactic Halo emission. The contrast between on- and off-cloud allows us to disentangle the foreground and background emissions. In particular we will focus on the properties of the galactic halo, which dominates the oxygen background emission. | GALACTIC DIFFUSE EMISSION | 5 | A | URSINO | EUGENIO | NULL | NULL | USA | 8 | AO8 | PROPERTIES OF THE GALACTIC HALO THROUGH SHADOW OBSERVATIONS | XIS | Y |
| MBM36-OFF | 238.9304 | -1.7878 | 7.39248129 | 37.0792042 | 270.0134 | 56533.8916319444 | 56535.9634606482 | 508074010 | 74156.5 | 80000 | 74164.5 | 74164.5 | 0 | 74156.5 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 64252.1 | 64252.1 | 178982 | 1 | PROCESSED | 57612.4561574074 | 56970 | 56603.6967476852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081322 | We propose the observation of three off-cloud targets near the targets of the Solar Wind Charge Exchange (SWCX) Key Project to study the properties of the Diffuse X-ray Background below 1 keV, with particular focus on the characterization of the Galactic Halo. The Key Project targets are at a distance of a few hundreds pc from the Sun and their high density portions shields about 90% of X-rays at the O VII energy, our proposed targets, instead, shield only about 50% of the Galactic Halo emission. The contrast between on- and off-cloud allows us to disentangle the foreground and background emissions. In particular we will focus on the properties of the galactic halo, which dominates the oxygen background emission. | GALACTIC DIFFUSE EMISSION | 5 | A | URSINO | EUGENIO | NULL | NULL | USA | 8 | AO8 | PROPERTIES OF THE GALACTIC HALO THROUGH SHADOW OBSERVATIONS | XIS | Y |
| GRXE_E_1 | 267.4747 | -27.4596 | 1.75131157 | -0.04310182 | 105.3995 | 56726.0649537037 | 56728.6459722222 | 508075010 | 103533.1 | 100000 | 103549.1 | 103533.1 | 0 | 103555.9 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 85344.6 | 85344.6 | 222981.8 | 2 | PROCESSED | 57614.0622453704 | 56383 | 56740.8547453704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 086001 | We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies. | GALACTIC DIFFUSE EMISSION | 5 | A | TSURU | TAKESHI | NULL | NULL | JAP | 8 | AO8 | ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE) | XIS | Y |
| GRXE_E_7 | 268.3325 | -26.1696 | 3.2513581 | -0.04270444 | 86.7249 | 56716.5321296296 | 56718.7084953704 | 508076010 | 102684.8 | 100000 | 102697.8 | 102686.8 | 0 | 102684.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 96453.9 | 96453.9 | 188019.8 | 3 | PROCESSED | 57613.9520486111 | 56383 | 56727.7217013889 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 086001 | We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies. | GALACTIC DIFFUSE EMISSION | 5 | A | TSURU | TAKESHI | NULL | NULL | JAP | 8 | AO8 | ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE) | XIS | Y |
| GRXE_E_8 | 268.4708 | -25.9492 | 3.50431952 | -0.037979 | 86.7223 | 56718.7089236111 | 56720.9585069445 | 508077010 | 103132 | 100000 | 103140 | 103132 | 0 | 103140 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 94853.8 | 94853.8 | 194344.9 | 2 | PROCESSED | 57613.971712963 | 56383 | 56775.6980787037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 086001 | We make high statistics observation of the 6.4-keV line in the region of l= +1.5 ~ +4 deg, which is key to resolve the origin of the Galactic Ridge X-ray Emission (GRXE). It also clarifies the origin of the 6.7-keV line. The concrete aims are (1) to determine the asymmetry of the GRXE between the east- and the west-sides of the Galactic center, (2) to separate spectral components of the 6.7-keV and 6.4-keV lines, (3) to constrain the origin of the 6.4-keV line (presumably from diffuse origin) and (4) to provide a "Suzaku Legacy" of the Galactic diffuse X-ray emission (the GRXE and GCDX) covering the wide region of l= -4 ~ +4 deg with high statistics and precise spectroscopy, which will be immediately used as best path-finder for Astro-H and standard data set for the multi-band studies. | GALACTIC DIFFUSE EMISSION | 5 | A | TSURU | TAKESHI | NULL | NULL | JAP | 8 | AO8 | ORIGIN OF THE 6.4KEV LINE OF THE GALACTIC RIDGE X-RAY EMISSION (GRXE) | XIS | Y |
| MBM16 | 49.7645 | 11.5821 | 170.59989958 | -37.2737153 | 77.5997 | 56511.9409027778 | 56513.916875 | 508078010 | 82324.6 | 80000 | 82324.6 | 82324.6 | 0 | 82324.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 79071.8 | 79071.8 | 170689.8 | 2 | PROCESSED | 57612.2763541667 | 56383 | 56587.6759490741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 086002 | Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions. | GALACTIC DIFFUSE EMISSION | 5 | A | GALEAZZI | MASSIMILIANO | NULL | NULL | USA | 8 | AO8 | CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE | XIS | Y |
| MBM16 | 49.7705 | 11.5801 | 170.60706006 | -37.27124926 | 254.3335 | 56691.5957175926 | 56693.5209953704 | 508078020 | 87850.9 | 80000 | 87850.9 | 87858.9 | 0 | 87858.9 | 3 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57613.7866782407 | 56383 | 56706.5234375 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 086002 | Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions. | GALACTIC DIFFUSE EMISSION | 5 | A | GALEAZZI | MASSIMILIANO | NULL | NULL | USA | 8 | AO8 | CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE | XIS | Y |
| MBM36 | 238.3604 | -4.7951 | 4.00027103 | 35.69642682 | 294.5973 | 56525.2685300926 | 56526.5655092593 | 508079010 | 49655.5 | 80000 | 49655.5 | 49655.5 | 0 | 49655.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42879.9 | 42879.9 | 112045.8 | 2 | PROCESSED | 57612.3808912037 | 56383 | 56587.6359027778 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 086002 | Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions. | GALACTIC DIFFUSE EMISSION | 5 | A | GALEAZZI | MASSIMILIANO | NULL | NULL | USA | 8 | AO8 | CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE | XIS | Y |
| MBM36 | 238.3853 | -4.8926 | 3.92555744 | 35.61619893 | 279.5456 | 56531.6987268518 | 56533.8883333333 | 508079020 | 79606.7 | 80000 | 79606.7 | 79606.7 | 0 | 79606.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 67717 | 67717 | 189166 | 2 | PROCESSED | 57612.4621064815 | 56383 | 56603.7246875 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 086002 | Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions. | GALACTIC DIFFUSE EMISSION | 5 | A | GALEAZZI | MASSIMILIANO | NULL | NULL | USA | 8 | AO8 | CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE | XIS | Y |
| LDN1563 | 75.5195 | 13.8744 | 187.14092451 | -16.70693442 | 81.1182 | 56523.4274768518 | 56525.2535648148 | 508080010 | 83588 | 80000 | 83588 | 83596 | 0 | 83604 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 79674.1 | 79674.1 | 157753.8 | 2 | PROCESSED | 57612.368912037 | 56383 | 56587.8175694445 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 086002 | Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions. | GALACTIC DIFFUSE EMISSION | 5 | A | GALEAZZI | MASSIMILIANO | NULL | NULL | USA | 8 | AO8 | CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE | XIS | Y |
| MBM20 | 68.9307 | -14.6229 | 211.39181931 | -36.56844204 | 64.9904 | 56520.8174074074 | 56522.5001967593 | 508081010 | 56490.5 | 80000 | 56490.5 | 56490.5 | 0 | 56490.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 55086 | 55086 | 145380 | 1 | PROCESSED | 57612.3311111111 | 56383 | 56587.6432291667 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 086002 | Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions. | GALACTIC DIFFUSE EMISSION | 5 | A | GALEAZZI | MASSIMILIANO | NULL | NULL | USA | 8 | AO8 | CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE | XIS | Y |
| W49B | 287.7839 | 9.1153 | 43.2808507 | -0.18308455 | 82.0062 | 57122.7467013889 | 57125.7127777778 | 509001010 | 81476.3 | 400000 | 81476.3 | 113909.8 | 0 | 113916.2 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.986724537 | 56748 | 57136.5735300926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090007 | W49B is an unique SNR which shows the radiative recombination continuum of He-like Fe. The plasma code of recombining plasma is very limited, due to a lack of accurate information of this plasma process. Since the transient time scale of the recombining plasma in laboratory is very short, useful information is hard to obtain. The recombination features of Fe are located in the energy band of 6-10 keV, where no other prominent structure is found. Therefore the spectrum of W49B in this energy band is ideal to study details of the recombining plasma. We hence propose 400-ksec observations on W49B. This deep observation will serve the fundamental data of the recombining plasma from the space plasma for the first time, which is key information for the future study of space plasma with ASTRO-H. | GALACTIC DIFFUSE EMISSION | 5 | B | KOYAMA | KATSUJI | NULL | NULL | JAP | 9 | AO9 | DEEP OBSERVATIONS OF W49B | XIS | Y |
| W49B | 287.7842 | 9.1154 | 43.28107632 | -0.18330097 | 82.0063 | 57125.7127893518 | 57128.6891087963 | 509001020 | 103042.6 | 400000 | 103042.6 | 113187.5 | 0 | 113179.5 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57618.0199537037 | 56748 | 57142.3645138889 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090007 | W49B is an unique SNR which shows the radiative recombination continuum of He-like Fe. The plasma code of recombining plasma is very limited, due to a lack of accurate information of this plasma process. Since the transient time scale of the recombining plasma in laboratory is very short, useful information is hard to obtain. The recombination features of Fe are located in the energy band of 6-10 keV, where no other prominent structure is found. Therefore the spectrum of W49B in this energy band is ideal to study details of the recombining plasma. We hence propose 400-ksec observations on W49B. This deep observation will serve the fundamental data of the recombining plasma from the space plasma for the first time, which is key information for the future study of space plasma with ASTRO-H. | GALACTIC DIFFUSE EMISSION | 5 | B | KOYAMA | KATSUJI | NULL | NULL | JAP | 9 | AO9 | DEEP OBSERVATIONS OF W49B | XIS | Y |
| W49B | 287.7843 | 9.1147 | 43.28050127 | -0.18371216 | 82.0064 | 57128.6891203704 | 57131.6619328704 | 509001030 | 100995.9 | 400000 | 100995.9 | 106420.7 | 0 | 106396.7 | 4 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57618.0043518518 | 56748 | 57220.3809722222 | 3.0.22.44 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090007 | W49B is an unique SNR which shows the radiative recombination continuum of He-like Fe. The plasma code of recombining plasma is very limited, due to a lack of accurate information of this plasma process. Since the transient time scale of the recombining plasma in laboratory is very short, useful information is hard to obtain. The recombination features of Fe are located in the energy band of 6-10 keV, where no other prominent structure is found. Therefore the spectrum of W49B in this energy band is ideal to study details of the recombining plasma. We hence propose 400-ksec observations on W49B. This deep observation will serve the fundamental data of the recombining plasma from the space plasma for the first time, which is key information for the future study of space plasma with ASTRO-H. | GALACTIC DIFFUSE EMISSION | 5 | B | KOYAMA | KATSUJI | NULL | NULL | JAP | 9 | AO9 | DEEP OBSERVATIONS OF W49B | XIS | Y |
| W49B | 287.784 | 9.1149 | 43.28054167 | -0.18335704 | 82.0063 | 57131.6619444445 | 57133.5779513889 | 509001040 | 67318.2 | 400000 | 67318.2 | 67318.2 | 0 | 67326.2 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57618.0264699074 | 56748 | 57224.4531481482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090007 | W49B is an unique SNR which shows the radiative recombination continuum of He-like Fe. The plasma code of recombining plasma is very limited, due to a lack of accurate information of this plasma process. Since the transient time scale of the recombining plasma in laboratory is very short, useful information is hard to obtain. The recombination features of Fe are located in the energy band of 6-10 keV, where no other prominent structure is found. Therefore the spectrum of W49B in this energy band is ideal to study details of the recombining plasma. We hence propose 400-ksec observations on W49B. This deep observation will serve the fundamental data of the recombining plasma from the space plasma for the first time, which is key information for the future study of space plasma with ASTRO-H. | GALACTIC DIFFUSE EMISSION | 5 | B | KOYAMA | KATSUJI | NULL | NULL | JAP | 9 | AO9 | DEEP OBSERVATIONS OF W49B | XIS | Y |
| G1.9+0.3 | 267.1939 | -27.1714 | 1.87009843 | 0.31910459 | 104.2133 | 57099.6072569445 | 57101.7854976852 | 509003010 | 92031.3 | 100000 | 92031.3 | 97085.9 | 0 | 97069.9 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.8499189815 | 57527 | 57160.6404861111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090030 | We propose a Suzaku observations of the youngest supernova remnant (SNR) G1.9+0.3. We aim to detect flux increase and spectral hardening of synchrotron X-rays since 2011 when the previous Suzaku observation was performed. The measurement should provide us with important information about the maximum acceleration energy attainable by diffusive shock acceleration in SNRs. Suzaku XIS is the most suitable detector since it has the large effective area even in the hard band up to 10 keV. If X-ray flux increase is significantly larger than that measured in the radio band, we can conclude that maximum acceleration energy is becoming higher at present. | GALACTIC DIFFUSE EMISSION | 5 | A | TANAKA | TAKAAKI | UCHIYAMA | YASUNOBU | JAP | 9 | AO9 | MEASUREMENT OF TIME VARIABILITY OF SYNCHROTRON X-RAYS FROM THE YOUNGEST SUPERNOVA REMNANT G1.9+0.3 | XIS | Y |
| HOT BLOB 2 | 131.2547 | 53.3234 | 164.89716269 | 38.20704104 | 284.8982 | 57137.3573842593 | 57139.1293055556 | 509008010 | 46022.4 | 80000 | 46022.4 | 77979.5 | 0 | 78011.5 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57618.041412037 | 57520 | 57154.4516087963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090044 | Hot blobs including plasma of temperature kT = 0.6 - 1.0 keV in the Milky-Way Halo were found in 1/10 of the sky by systematical analysis of the soft X-ray diffuse background in Suzaku/XIS observations. They can play a role in matter and energy transportation among the Galactic plane, the Milky-Way Halo and intergalactic space. In order to reveal origin and physical condition of them, we focus on the part of a hot blob in (ell, b) = (161.505, 40.696) and propose to observe neighboring this area to constrain its size. | GALACTIC DIFFUSE EMISSION | 5 | C | SEKIYA | NORIO | NULL | NULL | JAP | 9 | AO9 | ORIGIN AND PHYSICAL CONDITION OF HOT BLOBS IN THE MILKY-WAY HALO | XIS | Y |
| HOT BLOB 3 | 127.507 | 51.0389 | 167.88407696 | 36.01101877 | 263.6154 | 57139.1338657407 | 57140.9141319444 | 509009010 | 81118.3 | 80000 | 81118.3 | 81542.3 | 0 | 81550.3 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57644.5780902778 | 57591 | 57224.4589351852 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090044 | Hot blobs including plasma of temperature kT = 0.6 - 1.0 keV in the Milky-Way Halo were found in 1/10 of the sky by systematical analysis of the soft X-ray diffuse background in Suzaku/XIS observations. They can play a role in matter and energy transportation among the Galactic plane, the Milky-Way Halo and intergalactic space. In order to reveal origin and physical condition of them, we focus on the part of a hot blob in (ell, b) = (161.505, 40.696) and propose to observe neighboring this area to constrain its size. | GALACTIC DIFFUSE EMISSION | 5 | C | SEKIYA | NORIO | NULL | NULL | JAP | 9 | AO9 | ORIGIN AND PHYSICAL CONDITION OF HOT BLOBS IN THE MILKY-WAY HALO | XIS | Y |
| HESS J1641-463 | 250.6069 | -46.2544 | 338.71856162 | -0.05766971 | 282.1914 | 56898.1501736111 | 56898.2719907407 | 509010010 | 0 | 40000 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.5288773148 | 56748 | 56979.4106944445 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090045 | The origin of cosmic rays has been one of the biggest problems in modern astrophysics. TeV gamma-ray observations provide indirect evidences of cosmic ray acceleration, although the sources detected so far have softer spectra than what would be expected by particle accelerators to explain the observed distribution of cosmic rays at the knee. HESS J1641-463 is the hardest TeV gamma-ray source ever found. With Suzaku's large effective area, and low and stable background, we will perform the first deep X-ray observation of this source to seek for its X-ray counterpart, and to identify its nature. It will provide a direct look into the physics of the highest energy particle accelerators in our Galaxy, responsible for the cosmic ray spectrum up to the spectral knee at PeV energies. | GALACTIC DIFFUSE EMISSION | 5 | A | BAMBA | AYA | NULL | NULL | JAP | 9 | AO9 | IDENTIFYING THE X-RAY COUNTERPART OF THE HARDEST SOURCE HUMAN EVER DETECTED | XIS | Y |
| HESS J1641-463 | 250.2616 | -46.3013 | 338.52580532 | 0.09066192 | 282.4572 | 56900.1342939815 | 56902.1166435185 | 509010020 | 0 | 40000 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.5303356482 | 56748 | 57122.3887268518 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090045 | The origin of cosmic rays has been one of the biggest problems in modern astrophysics. TeV gamma-ray observations provide indirect evidences of cosmic ray acceleration, although the sources detected so far have softer spectra than what would be expected by particle accelerators to explain the observed distribution of cosmic rays at the knee. HESS J1641-463 is the hardest TeV gamma-ray source ever found. With Suzaku's large effective area, and low and stable background, we will perform the first deep X-ray observation of this source to seek for its X-ray counterpart, and to identify its nature. It will provide a direct look into the physics of the highest energy particle accelerators in our Galaxy, responsible for the cosmic ray spectrum up to the spectral knee at PeV energies. | GALACTIC DIFFUSE EMISSION | 5 | A | BAMBA | AYA | NULL | NULL | JAP | 9 | AO9 | IDENTIFYING THE X-RAY COUNTERPART OF THE HARDEST SOURCE HUMAN EVER DETECTED | XIS | N |
| VELA PWN GEV1 | 127.6995 | -44.6062 | 262.61398048 | -3.09706524 | 119.7191 | 56985.3954282407 | 56985.8502546296 | 509011010 | 19149.2 | 15000 | 19157.2 | 19165.2 | 0 | 19149.2 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.8102893518 | 57365 | 57009.4123726852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090046 | We have recently revealed that the Vela pulsar wind nebula (PWN) is more extended in X-ray than in radio, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. On the other hand, Fermi-LAT shows that GeV PWN has a totally different spatial distribution from either X-ray or radio PWN. We here propose a mapping observation of GeV PWN in order to investigate if there is yet another population. We also propose to observe the south end of the X-ray PWN into which direction radio PWN is more extended. | GALACTIC DIFFUSE EMISSION | 5 | C | MORI | KOJI | NULL | NULL | JAP | 9 | AO9 | X-RAY MAPPING OF THE VELA PULSAR WIND NEBULA WITH SUZAKU | XIS | Y |
| VELA PWN GEV2 | 128.4409 | -44.9066 | 263.16834954 | -2.85026128 | 119.7193 | 56985.851099537 | 56986.5001273148 | 509012010 | 19107.8 | 15000 | 19139.8 | 19123.8 | 0 | 19107.8 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.8168981482 | 57366 | 57009.4112268518 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090046 | We have recently revealed that the Vela pulsar wind nebula (PWN) is more extended in X-ray than in radio, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. On the other hand, Fermi-LAT shows that GeV PWN has a totally different spatial distribution from either X-ray or radio PWN. We here propose a mapping observation of GeV PWN in order to investigate if there is yet another population. We also propose to observe the south end of the X-ray PWN into which direction radio PWN is more extended. | GALACTIC DIFFUSE EMISSION | 5 | C | MORI | KOJI | NULL | NULL | JAP | 9 | AO9 | X-RAY MAPPING OF THE VELA PULSAR WIND NEBULA WITH SUZAKU | XIS | Y |
| VELA PWN GEV3 | 128.0196 | -44.9062 | 262.99085627 | -3.09029782 | 119.9755 | 56986.5006481482 | 56986.9105439815 | 509013010 | 18489.3 | 15000 | 18489.3 | 18496.9 | 0 | 18489.3 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.8178009259 | 57366 | 57002.4411226852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090046 | We have recently revealed that the Vela pulsar wind nebula (PWN) is more extended in X-ray than in radio, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. On the other hand, Fermi-LAT shows that GeV PWN has a totally different spatial distribution from either X-ray or radio PWN. We here propose a mapping observation of GeV PWN in order to investigate if there is yet another population. We also propose to observe the south end of the X-ray PWN into which direction radio PWN is more extended. | GALACTIC DIFFUSE EMISSION | 5 | C | MORI | KOJI | NULL | NULL | JAP | 9 | AO9 | X-RAY MAPPING OF THE VELA PULSAR WIND NEBULA WITH SUZAKU | XIS | Y |
| VELA PWN GEV4 | 127.5996 | -44.9062 | 262.81539743 | -3.33071285 | 121.1346 | 56986.9114814815 | 56987.558587963 | 509014010 | 17981.7 | 15000 | 17981.7 | 17989.7 | 0 | 17997.7 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.8244328704 | 57368 | 57002.4392824074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090046 | We have recently revealed that the Vela pulsar wind nebula (PWN) is more extended in X-ray than in radio, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. On the other hand, Fermi-LAT shows that GeV PWN has a totally different spatial distribution from either X-ray or radio PWN. We here propose a mapping observation of GeV PWN in order to investigate if there is yet another population. We also propose to observe the south end of the X-ray PWN into which direction radio PWN is more extended. | GALACTIC DIFFUSE EMISSION | 5 | C | MORI | KOJI | NULL | NULL | JAP | 9 | AO9 | X-RAY MAPPING OF THE VELA PULSAR WIND NEBULA WITH SUZAKU | XIS | Y |
| VELA PWN GEV5 | 128.1777 | -45.5057 | 263.54099229 | -3.35509044 | 120.3003 | 56987.5594328704 | 56987.9009490741 | 509015010 | 16188.9 | 15000 | 16188.9 | 16212.7 | 0 | 16196.9 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.822025463 | 57368 | 57002.4333564815 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090046 | We have recently revealed that the Vela pulsar wind nebula (PWN) is more extended in X-ray than in radio, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. On the other hand, Fermi-LAT shows that GeV PWN has a totally different spatial distribution from either X-ray or radio PWN. We here propose a mapping observation of GeV PWN in order to investigate if there is yet another population. We also propose to observe the south end of the X-ray PWN into which direction radio PWN is more extended. | GALACTIC DIFFUSE EMISSION | 5 | C | MORI | KOJI | NULL | NULL | JAP | 9 | AO9 | X-RAY MAPPING OF THE VELA PULSAR WIND NEBULA WITH SUZAKU | XIS | Y |
| VELA PWN GEV6 | 128.0698 | -45.8067 | 263.73946045 | -3.59392918 | 121.6832 | 56987.9020717593 | 56988.5530324074 | 509016010 | 18092.6 | 15000 | 18108.6 | 18092.6 | 0 | 18108.6 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.8287037037 | 57450 | 57083.4111574074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090046 | We have recently revealed that the Vela pulsar wind nebula (PWN) is more extended in X-ray than in radio, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. On the other hand, Fermi-LAT shows that GeV PWN has a totally different spatial distribution from either X-ray or radio PWN. We here propose a mapping observation of GeV PWN in order to investigate if there is yet another population. We also propose to observe the south end of the X-ray PWN into which direction radio PWN is more extended. | GALACTIC DIFFUSE EMISSION | 5 | C | MORI | KOJI | NULL | NULL | JAP | 9 | AO9 | X-RAY MAPPING OF THE VELA PULSAR WIND NEBULA WITH SUZAKU | XIS | Y |
| VELA PWN S1 | 128.1818 | -46.8811 | 264.65396784 | -4.16648977 | 122.1894 | 56988.5541087963 | 56988.8905324074 | 509017010 | 15463.8 | 15000 | 15463.8 | 15487.8 | 0 | 15783.8 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.8238194444 | 57368 | 57002.4344328704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090046 | We have recently revealed that the Vela pulsar wind nebula (PWN) is more extended in X-ray than in radio, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. On the other hand, Fermi-LAT shows that GeV PWN has a totally different spatial distribution from either X-ray or radio PWN. We here propose a mapping observation of GeV PWN in order to investigate if there is yet another population. We also propose to observe the south end of the X-ray PWN into which direction radio PWN is more extended. | GALACTIC DIFFUSE EMISSION | 5 | C | MORI | KOJI | NULL | NULL | JAP | 9 | AO9 | X-RAY MAPPING OF THE VELA PULSAR WIND NEBULA WITH SUZAKU | XIS | Y |
| VELA PWN S2 | 128.0787 | -47.1859 | 264.85904608 | -4.40317226 | 122.1879 | 56989.4162847222 | 56989.8404976852 | 509018010 | 17477.4 | 15000 | 17477.4 | 17477.4 | 0 | 17477.4 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.4063773148 | 57368 | 57002.436087963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090046 | We have recently revealed that the Vela pulsar wind nebula (PWN) is more extended in X-ray than in radio, suggesting that the Vela PWN consists of two distinct populations: one is a bright, well-known component defining the radio boundary and the other is faint, newly-discovered one defining the X-ray boundary. On the other hand, Fermi-LAT shows that GeV PWN has a totally different spatial distribution from either X-ray or radio PWN. We here propose a mapping observation of GeV PWN in order to investigate if there is yet another population. We also propose to observe the south end of the X-ray PWN into which direction radio PWN is more extended. | GALACTIC DIFFUSE EMISSION | 5 | C | MORI | KOJI | NULL | NULL | JAP | 9 | AO9 | X-RAY MAPPING OF THE VELA PULSAR WIND NEBULA WITH SUZAKU | XIS | Y |
| G166.0+4.3_NE | 81.7708 | 42.9893 | 166.12860985 | 4.39756168 | 84.8043 | 56919.0138773148 | 56920.3092824074 | 509022010 | 54394.2 | 60000 | 54394.2 | 61593.1 | 0 | 61593.1 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.5656134259 | 57296 | 56940.6693981482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090092 | Rarefaction by a blow-out is an important candidate for the formation of recombining plasmas discovered recently in several SNRs. G166.0+4.3 (G166 hereafter) is a unique SNR with which we can examine it. The morphology suggests that the shell of G166 follows the normal evolutional scenario of SNR and the wing is formed by blow-out into cavity on the way of the evolution. Observing G166 with Suzaku as a laboratory of recombining plasma, 1) we examine if a recombining plasma in a SNR is created through rarefaction by blow-out. 2) We construct a model of creation of a recombining plasma in a SNR. Using the parameters of G166 such as age and SN energy obtained from the shell, we reconstruct the recombining plasma created by the blow-out in the wing and compare it with the observation. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKATA | AKIHIRO | NULL | NULL | JAP | 9 | AO9 | G166.0+4.3 : THE LABORATORY FOR RAREFACTION FORMING OVER-IONIZED PLASMA IN SNR | XIS | Y |
| G166.0+4.3_NE | 81.7715 | 42.9863 | 166.13139999 | 4.39632756 | 84.8097 | 56922.0215740741 | 56923.3544444444 | 509022020 | 58559.8 | 60000 | 58559.8 | 61503.9 | 0 | 61487.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 2207 | 2207 | 5696 | 0 | PROCESSED | 57616.5872685185 | 57312 | 56945.1963657407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090092 | Rarefaction by a blow-out is an important candidate for the formation of recombining plasmas discovered recently in several SNRs. G166.0+4.3 (G166 hereafter) is a unique SNR with which we can examine it. The morphology suggests that the shell of G166 follows the normal evolutional scenario of SNR and the wing is formed by blow-out into cavity on the way of the evolution. Observing G166 with Suzaku as a laboratory of recombining plasma, 1) we examine if a recombining plasma in a SNR is created through rarefaction by blow-out. 2) We construct a model of creation of a recombining plasma in a SNR. Using the parameters of G166 such as age and SN energy obtained from the shell, we reconstruct the recombining plasma created by the blow-out in the wing and compare it with the observation. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKATA | AKIHIRO | NULL | NULL | JAP | 9 | AO9 | G166.0+4.3 : THE LABORATORY FOR RAREFACTION FORMING OVER-IONIZED PLASMA IN SNR | XIS | Y |
| G166.0+4.3_NW | 81.4339 | 42.9094 | 166.05797128 | 4.14809941 | 85.1436 | 56920.3100347222 | 56921.2397106482 | 509023010 | 39798.2 | 40000 | 39798.2 | 42033.9 | 0 | 42025.9 | 3 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.5613078704 | 57298 | 56940.6722569444 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090092 | Rarefaction by a blow-out is an important candidate for the formation of recombining plasmas discovered recently in several SNRs. G166.0+4.3 (G166 hereafter) is a unique SNR with which we can examine it. The morphology suggests that the shell of G166 follows the normal evolutional scenario of SNR and the wing is formed by blow-out into cavity on the way of the evolution. Observing G166 with Suzaku as a laboratory of recombining plasma, 1) we examine if a recombining plasma in a SNR is created through rarefaction by blow-out. 2) We construct a model of creation of a recombining plasma in a SNR. Using the parameters of G166 such as age and SN energy obtained from the shell, we reconstruct the recombining plasma created by the blow-out in the wing and compare it with the observation. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKATA | AKIHIRO | NULL | NULL | JAP | 9 | AO9 | G166.0+4.3 : THE LABORATORY FOR RAREFACTION FORMING OVER-IONIZED PLASMA IN SNR | XIS | Y |
| G166.0+4.3_SE | 81.6669 | 42.6537 | 166.36639381 | 4.14814693 | 85.0186 | 56921.2402777778 | 56922.0209606482 | 509024010 | 31273.1 | 60000 | 31273.1 | 34217.1 | 0 | 34273.1 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.5684722222 | 57626 | 56945.4935532407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090092 | Rarefaction by a blow-out is an important candidate for the formation of recombining plasmas discovered recently in several SNRs. G166.0+4.3 (G166 hereafter) is a unique SNR with which we can examine it. The morphology suggests that the shell of G166 follows the normal evolutional scenario of SNR and the wing is formed by blow-out into cavity on the way of the evolution. Observing G166 with Suzaku as a laboratory of recombining plasma, 1) we examine if a recombining plasma in a SNR is created through rarefaction by blow-out. 2) We construct a model of creation of a recombining plasma in a SNR. Using the parameters of G166 such as age and SN energy obtained from the shell, we reconstruct the recombining plasma created by the blow-out in the wing and compare it with the observation. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKATA | AKIHIRO | NULL | NULL | JAP | 9 | AO9 | G166.0+4.3 : THE LABORATORY FOR RAREFACTION FORMING OVER-IONIZED PLASMA IN SNR | XIS | Y |
| G166.0+4.3_SE | 81.6718 | 42.6436 | 166.37682371 | 4.1455421 | 266.8508 | 57094.5870486111 | 57095.305 | 509024020 | 26032.9 | 27000 | 26032.9 | 27392.9 | 0 | 27392.9 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.780625 | 57478 | 57108.4092939815 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090092 | Rarefaction by a blow-out is an important candidate for the formation of recombining plasmas discovered recently in several SNRs. G166.0+4.3 (G166 hereafter) is a unique SNR with which we can examine it. The morphology suggests that the shell of G166 follows the normal evolutional scenario of SNR and the wing is formed by blow-out into cavity on the way of the evolution. Observing G166 with Suzaku as a laboratory of recombining plasma, 1) we examine if a recombining plasma in a SNR is created through rarefaction by blow-out. 2) We construct a model of creation of a recombining plasma in a SNR. Using the parameters of G166 such as age and SN energy obtained from the shell, we reconstruct the recombining plasma created by the blow-out in the wing and compare it with the observation. | GALACTIC DIFFUSE EMISSION | 5 | A | TAKATA | AKIHIRO | NULL | NULL | JAP | 9 | AO9 | G166.0+4.3 : THE LABORATORY FOR RAREFACTION FORMING OVER-IONIZED PLASMA IN SNR | XIS | Y |
| CIZA J1358.9-4750_NE | 209.8984 | -47.6059 | 314.66509294 | 13.70714471 | 293.0012 | 56879.8864467593 | 56880.8606481482 | 509025010 | 40274.8 | 40000 | 40282.8 | 40282.8 | 0 | 40274.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 7746.8 | 7746.8 | 19736 | 0 | PROCESSED | 57616.4833333333 | 57270 | 56902.1990972222 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090102 | Recently we have discovered the merging nature of a nearby galaxy cluster, CIZA J1358.9-4750. This cluster has two subclusters, both showing ICM temperatures of 4-6 keV, and a bright "bridge" region which connects the two cores. The "bridge" exhibits a high temperature of about 9 keV. This cluster is an archetypal case showing clear and unique symptoms of shock heating and particle acceleration in a probably early stage of major merger. To further clarify the merging geometry, and to quantify the scale and energetic of shock heating, we propose to observe this cluster with four new pointings using the Suzaku XIS. | GALACTIC DIFFUSE EMISSION | 5 | B | KATO | YUICHI | NULL | NULL | JAP | 9 | AO9 | OBSERVATIONS OF NEARBY EARLY MERGING CLUSTERS OF GALAXIES CIZA J1358.9-4750 | XIS | Y |
| CIZA J1358.9-4750_SE | 209.9655 | -47.9267 | 314.62109256 | 13.3860264 | 293 | 56881.8273032407 | 56882.7188773148 | 509026010 | 41360.1 | 40000 | 41360.1 | 41360.1 | 0 | 41360.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 5850.9 | 5850.9 | 14040 | 0 | PROCESSED | 57616.4947800926 | 57270 | 56902.1901273148 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090102 | Recently we have discovered the merging nature of a nearby galaxy cluster, CIZA J1358.9-4750. This cluster has two subclusters, both showing ICM temperatures of 4-6 keV, and a bright "bridge" region which connects the two cores. The "bridge" exhibits a high temperature of about 9 keV. This cluster is an archetypal case showing clear and unique symptoms of shock heating and particle acceleration in a probably early stage of major merger. To further clarify the merging geometry, and to quantify the scale and energetic of shock heating, we propose to observe this cluster with four new pointings using the Suzaku XIS. | GALACTIC DIFFUSE EMISSION | 5 | B | KATO | YUICHI | NULL | NULL | JAP | 9 | AO9 | OBSERVATIONS OF NEARBY EARLY MERGING CLUSTERS OF GALAXIES CIZA J1358.9-4750 | XIS | Y |
| CIZA J1358.9-4750_SW | 209.5053 | -47.9232 | 314.31638856 | 13.47131455 | 293 | 56882.719537037 | 56883.5528356482 | 509027010 | 42030.8 | 40000 | 42030.8 | 42054.8 | 0 | 42038.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 7010.9 | 7010.9 | 14276 | 0 | PROCESSED | 57616.4982175926 | 57267 | 56898.5152662037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090102 | Recently we have discovered the merging nature of a nearby galaxy cluster, CIZA J1358.9-4750. This cluster has two subclusters, both showing ICM temperatures of 4-6 keV, and a bright "bridge" region which connects the two cores. The "bridge" exhibits a high temperature of about 9 keV. This cluster is an archetypal case showing clear and unique symptoms of shock heating and particle acceleration in a probably early stage of major merger. To further clarify the merging geometry, and to quantify the scale and energetic of shock heating, we propose to observe this cluster with four new pointings using the Suzaku XIS. | GALACTIC DIFFUSE EMISSION | 5 | B | KATO | YUICHI | NULL | NULL | JAP | 9 | AO9 | OBSERVATIONS OF NEARBY EARLY MERGING CLUSTERS OF GALAXIES CIZA J1358.9-4750 | XIS | Y |
| CIZA J1358.9-4750_NW | 209.4473 | -47.6057 | 314.36323033 | 13.78794346 | 293.0002 | 56880.8612615741 | 56881.8265972222 | 509028010 | 41501 | 40000 | 41501 | 41525 | 0 | 41509 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 7991.8 | 7991.8 | 20640 | 0 | PROCESSED | 57616.4817939815 | 57267 | 56898.4888657407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090102 | Recently we have discovered the merging nature of a nearby galaxy cluster, CIZA J1358.9-4750. This cluster has two subclusters, both showing ICM temperatures of 4-6 keV, and a bright "bridge" region which connects the two cores. The "bridge" exhibits a high temperature of about 9 keV. This cluster is an archetypal case showing clear and unique symptoms of shock heating and particle acceleration in a probably early stage of major merger. To further clarify the merging geometry, and to quantify the scale and energetic of shock heating, we propose to observe this cluster with four new pointings using the Suzaku XIS. | GALACTIC DIFFUSE EMISSION | 5 | B | KATO | YUICHI | NULL | NULL | JAP | 9 | AO9 | OBSERVATIONS OF NEARBY EARLY MERGING CLUSTERS OF GALAXIES CIZA J1358.9-4750 | XIS | Y |
| VERJ2019_P2 | 305.0647 | 36.873 | 75.14540231 | 0.26023113 | 251.4317 | 56970.0347453704 | 56971.0419097222 | 509029010 | 40494.1 | 40000 | 40494.1 | 40502.1 | 0 | 40502.1 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7544791667 | 57436 | 57071.4171527778 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090120 | The long-standing question on the origin of Galactic cosmic-rays (GCRs) is still not settled, and star-forming regions are promising sites for the production of GCRs. We propose deep observations of nearby star-forming region Cygnus X, aiming at elongated TeV gamma-ray emission found by Milagro and recently resolved by VERITAS. Although an energetic pulsar PSR J2021+3651 coincides with one of TeV peaks, most of gamma-ray emission still remains unexplained. By utilizing high sensitivity of the Suzaku XIS, particularly for diffuse X-rays, we aim to detect X-ray counterparts, presumably unknown pulsar wind nebulae. Connection with a Wolf-Rayet star and an HII region inside this region, which positionally coincide with the gamma-ray peak, will also be investigated. | GALACTIC DIFFUSE EMISSION | 5 | C | MIZUNO | TSUNEFUMI | NULL | NULL | JAP | 9 | AO9 | SEARCH FOR TEV ACCELERATORS IN NEARBY STAR-FORMING REGION CYGNUS-X WITH SUZAKU | XIS | Y |
| VERJ2019_P3 | 304.792 | 36.828 | 74.98489793 | 0.41476969 | 250.4389 | 56971.0428009259 | 56972.0349537037 | 509030010 | 41071.5 | 40000 | 41079.5 | 41071.5 | 0 | 41087.5 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7632175926 | 57352 | 56982.4314467593 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090120 | The long-standing question on the origin of Galactic cosmic-rays (GCRs) is still not settled, and star-forming regions are promising sites for the production of GCRs. We propose deep observations of nearby star-forming region Cygnus X, aiming at elongated TeV gamma-ray emission found by Milagro and recently resolved by VERITAS. Although an energetic pulsar PSR J2021+3651 coincides with one of TeV peaks, most of gamma-ray emission still remains unexplained. By utilizing high sensitivity of the Suzaku XIS, particularly for diffuse X-rays, we aim to detect X-ray counterparts, presumably unknown pulsar wind nebulae. Connection with a Wolf-Rayet star and an HII region inside this region, which positionally coincide with the gamma-ray peak, will also be investigated. | GALACTIC DIFFUSE EMISSION | 5 | C | MIZUNO | TSUNEFUMI | NULL | NULL | JAP | 9 | AO9 | SEARCH FOR TEV ACCELERATORS IN NEARBY STAR-FORMING REGION CYGNUS-X WITH SUZAKU | XIS | Y |
| HB9-WEST | 74.7057 | 46.2322 | 160.54700874 | 2.22396757 | 74.7402 | 56930.7930671296 | 56931.9168518518 | 509032010 | 49768.8 | 50000 | 49768.8 | 49768.8 | 0 | 49768.8 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.5952662037 | 57345 | 56979.4048611111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091312 | We propose to conduct two pointed observations of the Galactic supernova remnant (SNR) HB9 (G160.9+2.6) with Suzaku. HB9 is a member of the class of Galactic SNRs which are distinguished by their contrasting radio and X-ray morphologies. Prior X-ray observations of HB9 have suggested that the SNR may have a hard component to its X-ray emission, but the true nature of this emission and its origin (a background AGN, intercluster gas associated with the cluster that harbors the AGN or the SNR itself) remains elusive. Our proposed observations will help identify the true nature of the hard emission as well as search for spectral variations (and possible overionization) in the properties of the X-ray emitting plasma associated with the SNR. | GALACTIC DIFFUSE EMISSION | 5 | A | PANNUTI | THOMAS | NULL | NULL | USA | 9 | AO9 | SUZAKU OBSERVATIONS OF THE GALACTIC SUPERNOVA REMNANT HB9 (G160.9+2.6) | XIS | Y |
| HB9-EAST | 75.4362 | 46.2793 | 160.82107477 | 2.65100841 | 76.7663 | 56929.6809722222 | 56930.7918518518 | 509033010 | 51058.1 | 50000 | 51058.1 | 51058.1 | 0 | 51058.1 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.6020949074 | 57358 | 56986.4031481482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091312 | We propose to conduct two pointed observations of the Galactic supernova remnant (SNR) HB9 (G160.9+2.6) with Suzaku. HB9 is a member of the class of Galactic SNRs which are distinguished by their contrasting radio and X-ray morphologies. Prior X-ray observations of HB9 have suggested that the SNR may have a hard component to its X-ray emission, but the true nature of this emission and its origin (a background AGN, intercluster gas associated with the cluster that harbors the AGN or the SNR itself) remains elusive. Our proposed observations will help identify the true nature of the hard emission as well as search for spectral variations (and possible overionization) in the properties of the X-ray emitting plasma associated with the SNR. | GALACTIC DIFFUSE EMISSION | 5 | A | PANNUTI | THOMAS | NULL | NULL | USA | 9 | AO9 | SUZAKU OBSERVATIONS OF THE GALACTIC SUPERNOVA REMNANT HB9 (G160.9+2.6) | XIS | Y |
| G189 NORTH | 94.8937 | 22.8595 | 189.05453502 | 3.64004382 | 92.0693 | 56941.8561458333 | 56944.6669328704 | 509035010 | 100650 | 100000 | 100650 | 102898 | 0 | 102922 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.652337963 | 57362 | 56996.4204282407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091314 | We propose observations of G189.6+3.3, a large candidate supernova remnant (SNR) that overlaps with the much better studied remnant IC 443. Little is known about G189; ROSAT images show a shell-like structure about 1.5$^{circ}$ in diameter, but it has never been observed with modern X-ray telescopes. Its association, or lack thereof, with IC 443 is unknown. It may not be a supernova remnant at all; a superbubble origin for the X-ray emission also provides an intriguing possibility. Spatially-resolved spectroscopy with Suzaku will allow the detailed measurement of the plasma properties, illuminating the nature of this object. Determining the nature of G189 will help to probe the evolution of the ISM driven by the deaths of massive stars. | GALACTIC DIFFUSE EMISSION | 5 | B | WILLIAMS | BRIAN | NULL | NULL | USA | 9 | AO9 | OBSERVATIONS OF G189.6+3.3: AN SNR COMPANION TO IC 443? | XIS | Y |
| G189 EAST | 95.4705 | 22.4826 | 189.63783855 | 3.93426331 | 258.2106 | 57096.5099652778 | 57098.6780324074 | 509036010 | 66052.9 | 85000 | 66052.9 | 86223.7 | 0 | 86239.7 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.8236226852 | 57524 | 57157.5685416667 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091314 | We propose observations of G189.6+3.3, a large candidate supernova remnant (SNR) that overlaps with the much better studied remnant IC 443. Little is known about G189; ROSAT images show a shell-like structure about 1.5$^{circ}$ in diameter, but it has never been observed with modern X-ray telescopes. Its association, or lack thereof, with IC 443 is unknown. It may not be a supernova remnant at all; a superbubble origin for the X-ray emission also provides an intriguing possibility. Spatially-resolved spectroscopy with Suzaku will allow the detailed measurement of the plasma properties, illuminating the nature of this object. Determining the nature of G189 will help to probe the evolution of the ISM driven by the deaths of massive stars. | GALACTIC DIFFUSE EMISSION | 5 | B | WILLIAMS | BRIAN | NULL | NULL | USA | 9 | AO9 | OBSERVATIONS OF G189.6+3.3: AN SNR COMPANION TO IC 443? | XIS | Y |
| KES 69 | 278.2575 | -10.136 | 21.8245316 | -0.57033928 | 267.6495 | 56927.2830902778 | 56929.1391435185 | 509037010 | 77379.5 | 80000 | 77379.5 | 77970.8 | 0 | 77995.3 | 2 | 2 | 0 | 3 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.5892361111 | 57345 | 56979.4056944444 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091315 | We propose to conduct Suzaku observations of the Galactic supernova remnants (SNRs) Kes 69 (G21.8-0.6) and 3C 396 (G39.2-0.3). These SNRs were detected in the infrared by Spitzer and their infrared colors suggest that shocked molecules produce the observed emission. Published analyses of the X-ray emission from these SNRs (along with our own analysis of archival XMM-Newton and Chandra observations of these sources) reveals that the emission from both Kes 69 and 3C 396 is thermal and that they may both be mixed-morphology SNRs (MMSNRs) but deeper observations are needed to clarify their X-ray spectral properties. In particular, we will investigate whether these X-ray emitting plasmas are overionized, which is observed for other MMSNRs. | GALACTIC DIFFUSE EMISSION | 5 | A | PANNUTI | THOMAS | NULL | NULL | USA | 9 | AO9 | SUZAKU OBSERVATIONS OF THE SPITZER-DETECTED GALACTIC SUPERNOVA REMNANTS KES 69 (G21.8-0.6) AND 3C 396 (G39.2-0.3) | XIS | Y |
| 3C 396 | 285.987 | 5.4347 | 39.1930056 | -0.29514711 | 64.6066 | 56773.2792592593 | 56775.1223726852 | 509038010 | 82792.2 | 80000 | 82792.2 | 82792.2 | 0 | 82792.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 1011.1 | 1011.1 | 1744 | 0 | PROCESSED | 57614.9978703704 | 57157 | 56789.6241782407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091315 | We propose to conduct Suzaku observations of the Galactic supernova remnants (SNRs) Kes 69 (G21.8-0.6) and 3C 396 (G39.2-0.3). These SNRs were detected in the infrared by Spitzer and their infrared colors suggest that shocked molecules produce the observed emission. Published analyses of the X-ray emission from these SNRs (along with our own analysis of archival XMM-Newton and Chandra observations of these sources) reveals that the emission from both Kes 69 and 3C 396 is thermal and that they may both be mixed-morphology SNRs (MMSNRs) but deeper observations are needed to clarify their X-ray spectral properties. In particular, we will investigate whether these X-ray emitting plasmas are overionized, which is observed for other MMSNRs. | GALACTIC DIFFUSE EMISSION | 5 | B | PANNUTI | THOMAS | NULL | NULL | USA | 9 | AO9 | SUZAKU OBSERVATIONS OF THE SPITZER-DETECTED GALACTIC SUPERNOVA REMNANTS KES 69 (G21.8-0.6) AND 3C 396 (G39.2-0.3) | XIS | Y |
| G93.3+6.9 SE RIM | 313.3308 | 55.275 | 93.30192448 | 6.7583673 | 52.5 | 56812.4202314815 | 56814.806412037 | 509039010 | 108049.3 | 100000 | 108049.3 | 108049.3 | 0 | 108049.3 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.2124074074 | 57205 | 56835.7633912037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091316 | We propose three relatively long observations (totaling 280 ksec) of the high Galactic latitude supernova remnant G093.3+6.9, previously observed in AO-1 with a series of short exposures. This remnant is of particular interest because it is expanding in a low-density medium, appears sub-energetic, and has mixed-morphology, with central thermal X-ray emission surrounded by a radio synchrotron shell. Fits to the spectrum suggest a Type Ia SNR, but the possible presence of a pulsar wind nebula challenges that interpretation. The new pointings will significantly improve the statistics for key regions (rims and background), allowing us to type the remnant, determine its age, study its energetics, place limits on nonthermal X-ray emission, and better characterize the PWN. | GALACTIC DIFFUSE EMISSION | 5 | C | STAGE | MICHAEL | NULL | NULL | USA | 9 | AO9 | G093.3+6.9: SUPERNOVA PHYSICS IN A LOW-DENSITY MEDIUM | XIS | Y |
| G93.3+6.9 NW RIM | 312.9527 | 55.5354 | 93.368132 | 7.08938459 | 52.0991 | 56814.8070023148 | 56817.24125 | 509040010 | 107898.6 | 100000 | 107906.6 | 107906.6 | 0 | 107898.6 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.2100115741 | 57236 | 56869.6106481482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091316 | We propose three relatively long observations (totaling 280 ksec) of the high Galactic latitude supernova remnant G093.3+6.9, previously observed in AO-1 with a series of short exposures. This remnant is of particular interest because it is expanding in a low-density medium, appears sub-energetic, and has mixed-morphology, with central thermal X-ray emission surrounded by a radio synchrotron shell. Fits to the spectrum suggest a Type Ia SNR, but the possible presence of a pulsar wind nebula challenges that interpretation. The new pointings will significantly improve the statistics for key regions (rims and background), allowing us to type the remnant, determine its age, study its energetics, place limits on nonthermal X-ray emission, and better characterize the PWN. | GALACTIC DIFFUSE EMISSION | 5 | C | STAGE | MICHAEL | NULL | NULL | USA | 9 | AO9 | G093.3+6.9: SUPERNOVA PHYSICS IN A LOW-DENSITY MEDIUM | XIS | Y |
| G93.3+6.9 SOUTH | 313.0658 | 55.1877 | 93.13746865 | 6.81993623 | 52.2984 | 56817.2417708333 | 56819.1057638889 | 509041010 | 85469.5 | 80000 | 85713.2 | 85469.5 | 0 | 85713.1 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.2181712963 | 57201 | 56835.7539236111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091316 | We propose three relatively long observations (totaling 280 ksec) of the high Galactic latitude supernova remnant G093.3+6.9, previously observed in AO-1 with a series of short exposures. This remnant is of particular interest because it is expanding in a low-density medium, appears sub-energetic, and has mixed-morphology, with central thermal X-ray emission surrounded by a radio synchrotron shell. Fits to the spectrum suggest a Type Ia SNR, but the possible presence of a pulsar wind nebula challenges that interpretation. The new pointings will significantly improve the statistics for key regions (rims and background), allowing us to type the remnant, determine its age, study its energetics, place limits on nonthermal X-ray emission, and better characterize the PWN. | GALACTIC DIFFUSE EMISSION | 5 | C | STAGE | MICHAEL | NULL | NULL | USA | 9 | AO9 | G093.3+6.9: SUPERNOVA PHYSICS IN A LOW-DENSITY MEDIUM | XIS | Y |
| OFF-FIELD2 | 312.2284 | -9.8925 | 37.42106637 | -30.55240738 | 73.668 | 56784.946724537 | 56787.0627314815 | 509043010 | 80156 | 80000 | 80156 | 80156 | 0 | 80156 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 69614.2 | 69614.2 | 182807.9 | 1 | PROCESSED | 57615.1427430556 | 56748 | 56861.5828240741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091321 | Our special vantage point in our Galaxy allows us to study the Galactic warm-hot halo along several sightlines and determine its physical properties. The combination of absorption and emission measurements provides a powerful tool in this regard. Instead of average emission and absorption measures used in previous studies, one immediate step forward would be to use emission measures close to absorption sightlines. With proposed observations we will determine emission measures close to five sightlines in which we have the most accurate absorption measurements with Chandra. This will break the degeneracy between density and path-length and robustly measure the extent and mass of the warm-hot halo, placing strongest constraints yet on the fraction of missing baryons in the warm-hot plasma. | GALACTIC DIFFUSE EMISSION | 5 | A | GUPTA | ANJALI | NULL | NULL | USA | 9 | AO9 | CIRCUM-GALACTIC MEDIUM OF THE MILKY WAY | XIS | Y |
| OFF-FIELD3 | 339.5497 | 30.5758 | 91.73533627 | -24.10496467 | 65.4693 | 56819.1115625 | 56821.2502199074 | 509044010 | 97334.3 | 80000 | 97334.3 | 97334.3 | 0 | 97334.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38618 | 38618 | 77040 | 0 | PROCESSED | 57615.247974537 | 56748 | 56834.8146527778 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091321 | Our special vantage point in our Galaxy allows us to study the Galactic warm-hot halo along several sightlines and determine its physical properties. The combination of absorption and emission measurements provides a powerful tool in this regard. Instead of average emission and absorption measures used in previous studies, one immediate step forward would be to use emission measures close to absorption sightlines. With proposed observations we will determine emission measures close to five sightlines in which we have the most accurate absorption measurements with Chandra. This will break the degeneracy between density and path-length and robustly measure the extent and mass of the warm-hot halo, placing strongest constraints yet on the fraction of missing baryons in the warm-hot plasma. | GALACTIC DIFFUSE EMISSION | 5 | C | GUPTA | ANJALI | NULL | NULL | USA | 9 | AO9 | CIRCUM-GALACTIC MEDIUM OF THE MILKY WAY | XIS | Y |
| OFF-FIELD4 | 173.7625 | -36.8508 | 286.33839516 | 23.54732297 | 109.4045 | 57008.1600925926 | 57009.6814699074 | 509045010 | 81321 | 80000 | 81321 | 81321 | 0 | 81321 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.5308680556 | 56748 | 57112.4059490741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091321 | Our special vantage point in our Galaxy allows us to study the Galactic warm-hot halo along several sightlines and determine its physical properties. The combination of absorption and emission measurements provides a powerful tool in this regard. Instead of average emission and absorption measures used in previous studies, one immediate step forward would be to use emission measures close to absorption sightlines. With proposed observations we will determine emission measures close to five sightlines in which we have the most accurate absorption measurements with Chandra. This will break the degeneracy between density and path-length and robustly measure the extent and mass of the warm-hot halo, placing strongest constraints yet on the fraction of missing baryons in the warm-hot plasma. | GALACTIC DIFFUSE EMISSION | 5 | C | GUPTA | ANJALI | NULL | NULL | USA | 9 | AO9 | CIRCUM-GALACTIC MEDIUM OF THE MILKY WAY | XIS | Y |
| OFF-FIELD5 | 318.3256 | -10.4856 | 39.92155172 | -36.21028826 | 81.4906 | 56787.0661226852 | 56789.4168171296 | 509046010 | 80908 | 80000 | 80908 | 80908 | 0 | 80908 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 71340.4 | 71340.4 | 203069.7 | 2 | PROCESSED | 57615.126724537 | 56748 | 56806.674212963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091321 | Our special vantage point in our Galaxy allows us to study the Galactic warm-hot halo along several sightlines and determine its physical properties. The combination of absorption and emission measurements provides a powerful tool in this regard. Instead of average emission and absorption measures used in previous studies, one immediate step forward would be to use emission measures close to absorption sightlines. With proposed observations we will determine emission measures close to five sightlines in which we have the most accurate absorption measurements with Chandra. This will break the degeneracy between density and path-length and robustly measure the extent and mass of the warm-hot halo, placing strongest constraints yet on the fraction of missing baryons in the warm-hot plasma. | GALACTIC DIFFUSE EMISSION | 5 | A | GUPTA | ANJALI | NULL | NULL | USA | 9 | AO9 | CIRCUM-GALACTIC MEDIUM OF THE MILKY WAY | XIS | Y |
| FERMI_JET_COCOON_1 | 324.2719 | -34.1434 | 11.0027102 | -48.00136957 | 252.0162 | 56980.9718402778 | 56981.4029166667 | 509047010 | 23164.7 | 20000 | 23164.7 | 23188.7 | 0 | 23172.7 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.793125 | 57444 | 57076.4062037037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091322 | The Fermi bubbles are two large gamma-ray emitting objects near the Galactic center that may result from a time when Sgr A* was active, expelling mass and energy into the Galactic halo. Additional data from Fermi reinforce this hypothesis due to the detection of jet and cocoon structures in the southern bubble. There are signatures of the bubbles at X-ray energies, implying they contain relatively cool gas (10^6 K) and/or are influencing the Milky Way's hot gas halo. We propose Suzaku XIS observations to analyze the soft X-ray emission from these regions, which will allow us to constrain the density, temperature, and expansion velocity of these features. These observations will be crucial in understanding the evolution of the Fermi bubbles and their role in the evolution of the Milky Way. | GALACTIC DIFFUSE EMISSION | 5 | C | MILLER | MATTHEW | NULL | NULL | USA | 9 | AO9 | OBSERVING THE ''JET'' AND ''COCOON'' FEATURES OF THE FERMI BUBBLES | XIS | Y |
| FERMI_JET_COCOON_2 | 320.2279 | -29.504 | 17.00065384 | -44.00205209 | 255.063 | 56981.4053356482 | 56981.8683217593 | 509048010 | 19903.2 | 20000 | 19903.2 | 19903.2 | 0 | 19903.2 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7951736111 | 57362 | 56995.5937268518 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091322 | The Fermi bubbles are two large gamma-ray emitting objects near the Galactic center that may result from a time when Sgr A* was active, expelling mass and energy into the Galactic halo. Additional data from Fermi reinforce this hypothesis due to the detection of jet and cocoon structures in the southern bubble. There are signatures of the bubbles at X-ray energies, implying they contain relatively cool gas (10^6 K) and/or are influencing the Milky Way's hot gas halo. We propose Suzaku XIS observations to analyze the soft X-ray emission from these regions, which will allow us to constrain the density, temperature, and expansion velocity of these features. These observations will be crucial in understanding the evolution of the Fermi bubbles and their role in the evolution of the Milky Way. | GALACTIC DIFFUSE EMISSION | 5 | C | MILLER | MATTHEW | NULL | NULL | USA | 9 | AO9 | OBSERVING THE ''JET'' AND ''COCOON'' FEATURES OF THE FERMI BUBBLES | XIS | Y |
| FERMI_JET_COCOON_3 | 314.5039 | -35.288 | 8.28342789 | -40.13197139 | 258.2411 | 56980.5600694445 | 56980.9689583333 | 509049010 | 18674.2 | 20000 | 18674.2 | 18674.2 | 0 | 18674.2 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7925347222 | 57362 | 56995.6103240741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091322 | The Fermi bubbles are two large gamma-ray emitting objects near the Galactic center that may result from a time when Sgr A* was active, expelling mass and energy into the Galactic halo. Additional data from Fermi reinforce this hypothesis due to the detection of jet and cocoon structures in the southern bubble. There are signatures of the bubbles at X-ray energies, implying they contain relatively cool gas (10^6 K) and/or are influencing the Milky Way's hot gas halo. We propose Suzaku XIS observations to analyze the soft X-ray emission from these regions, which will allow us to constrain the density, temperature, and expansion velocity of these features. These observations will be crucial in understanding the evolution of the Fermi bubbles and their role in the evolution of the Milky Way. | GALACTIC DIFFUSE EMISSION | 5 | C | MILLER | MATTHEW | NULL | NULL | USA | 9 | AO9 | OBSERVING THE ''JET'' AND ''COCOON'' FEATURES OF THE FERMI BUBBLES | XIS | Y |
| FERMI_JET_COCOON_4 | 313.0188 | -30.9125 | 13.57103518 | -38.16097703 | 249.0341 | 56968.206412037 | 56968.8473958333 | 509050010 | 21676.7 | 20000 | 21676.7 | 21812.7 | 0 | 21820.7 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7496412037 | 57358 | 56982.4333333333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091322 | The Fermi bubbles are two large gamma-ray emitting objects near the Galactic center that may result from a time when Sgr A* was active, expelling mass and energy into the Galactic halo. Additional data from Fermi reinforce this hypothesis due to the detection of jet and cocoon structures in the southern bubble. There are signatures of the bubbles at X-ray energies, implying they contain relatively cool gas (10^6 K) and/or are influencing the Milky Way's hot gas halo. We propose Suzaku XIS observations to analyze the soft X-ray emission from these regions, which will allow us to constrain the density, temperature, and expansion velocity of these features. These observations will be crucial in understanding the evolution of the Fermi bubbles and their role in the evolution of the Milky Way. | GALACTIC DIFFUSE EMISSION | 5 | C | MILLER | MATTHEW | NULL | NULL | USA | 9 | AO9 | OBSERVING THE ''JET'' AND ''COCOON'' FEATURES OF THE FERMI BUBBLES | XIS | Y |
| FERMI_JET_COCOON_5 | 306.4609 | -33.261 | 9.28791468 | -33.23258901 | 260.3818 | 56968.8506481482 | 56969.3612847222 | 509051010 | 22043.8 | 20000 | 22051.8 | 22043.8 | 0 | 22057.3 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7478125 | 57358 | 56982.4350694445 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091322 | The Fermi bubbles are two large gamma-ray emitting objects near the Galactic center that may result from a time when Sgr A* was active, expelling mass and energy into the Galactic halo. Additional data from Fermi reinforce this hypothesis due to the detection of jet and cocoon structures in the southern bubble. There are signatures of the bubbles at X-ray energies, implying they contain relatively cool gas (10^6 K) and/or are influencing the Milky Way's hot gas halo. We propose Suzaku XIS observations to analyze the soft X-ray emission from these regions, which will allow us to constrain the density, temperature, and expansion velocity of these features. These observations will be crucial in understanding the evolution of the Fermi bubbles and their role in the evolution of the Milky Way. | GALACTIC DIFFUSE EMISSION | 5 | C | MILLER | MATTHEW | NULL | NULL | USA | 9 | AO9 | OBSERVING THE ''JET'' AND ''COCOON'' FEATURES OF THE FERMI BUBBLES | XIS | Y |
| FERMI_JET_COCOON_6 | 319.6218 | -32.8375 | 12.30967968 | -44.01160773 | 252.671 | 56969.3646296296 | 56970.0259375 | 509052010 | 21358.3 | 20000 | 21358.3 | 21358.3 | 0 | 21358.3 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7516782407 | 57358 | 56982.4382407407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091322 | The Fermi bubbles are two large gamma-ray emitting objects near the Galactic center that may result from a time when Sgr A* was active, expelling mass and energy into the Galactic halo. Additional data from Fermi reinforce this hypothesis due to the detection of jet and cocoon structures in the southern bubble. There are signatures of the bubbles at X-ray energies, implying they contain relatively cool gas (10^6 K) and/or are influencing the Milky Way's hot gas halo. We propose Suzaku XIS observations to analyze the soft X-ray emission from these regions, which will allow us to constrain the density, temperature, and expansion velocity of these features. These observations will be crucial in understanding the evolution of the Fermi bubbles and their role in the evolution of the Milky Way. | GALACTIC DIFFUSE EMISSION | 5 | C | MILLER | MATTHEW | NULL | NULL | USA | 9 | AO9 | OBSERVING THE ''JET'' AND ''COCOON'' FEATURES OF THE FERMI BUBBLES | XIS | Y |
| DIFFUSE1CENTER | 201.5497 | 7.7363 | 327.54309857 | 68.93048937 | 123.2999 | 57014.2523842593 | 57014.7820949074 | 509058010 | 20530.8 | 20000 | 20530.8 | 20530.8 | 0 | 20530.8 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.5530555556 | 57475 | 57107.4252546296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091324 | In the course of a program to fit spatial models to the Galactic hot gas content, we discovered a few fields that were highly discrepant in the strength of their O VII and/or O VIII line strengths. These are rare emission regions, occurring in fewer than 1% of the fields and they are not due to known extended emission regions (SNR, galaxy clusters, etc.). These emission anomalies probably signify locations of unusual physics, such as shocks, conductive heating, or local heat injection. We propose observations to determine the angular extent of these unusual regions and to better define the intensities of the O VII and O VIII lines. These observations will help identify the relevant physical process and the nature of the phenomenon causing them. | GALACTIC DIFFUSE EMISSION | 5 | C | BREGMAN | JOEL | NULL | NULL | USA | 9 | AO9 | UNIDENTIFIED BRIGHT X-RAY BACKGROUND REGIONS | XIS | Y |
| DIFFUSE1B | 201.171 | 8.6653 | 327.54408522 | 69.93225444 | 119.3004 | 57014.7841898148 | 57015.2196759259 | 509059010 | 20733.5 | 20000 | 20733.5 | 20741.5 | 0 | 20733.5 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.558275463 | 57475 | 57107.4265162037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091324 | In the course of a program to fit spatial models to the Galactic hot gas content, we discovered a few fields that were highly discrepant in the strength of their O VII and/or O VIII line strengths. These are rare emission regions, occurring in fewer than 1% of the fields and they are not due to known extended emission regions (SNR, galaxy clusters, etc.). These emission anomalies probably signify locations of unusual physics, such as shocks, conductive heating, or local heat injection. We propose observations to determine the angular extent of these unusual regions and to better define the intensities of the O VII and O VIII lines. These observations will help identify the relevant physical process and the nature of the phenomenon causing them. | GALACTIC DIFFUSE EMISSION | 5 | C | BREGMAN | JOEL | NULL | NULL | USA | 9 | AO9 | UNIDENTIFIED BRIGHT X-RAY BACKGROUND REGIONS | XIS | Y |
| DIFFUSE1C | 201.9274 | 6.8104 | 327.54723828 | 67.93166205 | 123.897 | 57015.2219560185 | 57015.3450115741 | 509060010 | 5511.7 | 20000 | 5527.7 | 5519.7 | 0 | 5511.7 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.5590393518 | 57417 | 57049.4528587963 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091324 | In the course of a program to fit spatial models to the Galactic hot gas content, we discovered a few fields that were highly discrepant in the strength of their O VII and/or O VIII line strengths. These are rare emission regions, occurring in fewer than 1% of the fields and they are not due to known extended emission regions (SNR, galaxy clusters, etc.). These emission anomalies probably signify locations of unusual physics, such as shocks, conductive heating, or local heat injection. We propose observations to determine the angular extent of these unusual regions and to better define the intensities of the O VII and O VIII lines. These observations will help identify the relevant physical process and the nature of the phenomenon causing them. | GALACTIC DIFFUSE EMISSION | 5 | C | BREGMAN | JOEL | NULL | NULL | USA | 9 | AO9 | UNIDENTIFIED BRIGHT X-RAY BACKGROUND REGIONS | XIS | Y |
| DIFFUSE1E | 200.6072 | 7.3824 | 324.76377809 | 68.9302329 | 123.5311 | 57011.0086458333 | 57011.5252083333 | 509062010 | 23976.2 | 20000 | 23976.2 | 24536.2 | 0 | 24536.2 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.5495023148 | 57475 | 57107.4289583333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091324 | In the course of a program to fit spatial models to the Galactic hot gas content, we discovered a few fields that were highly discrepant in the strength of their O VII and/or O VIII line strengths. These are rare emission regions, occurring in fewer than 1% of the fields and they are not due to known extended emission regions (SNR, galaxy clusters, etc.). These emission anomalies probably signify locations of unusual physics, such as shocks, conductive heating, or local heat injection. We propose observations to determine the angular extent of these unusual regions and to better define the intensities of the O VII and O VIII lines. These observations will help identify the relevant physical process and the nature of the phenomenon causing them. | GALACTIC DIFFUSE EMISSION | 5 | C | BREGMAN | JOEL | NULL | NULL | USA | 9 | AO9 | UNIDENTIFIED BRIGHT X-RAY BACKGROUND REGIONS | XIS | Y |
| 3C400.2 NW | 294.5044 | 17.3912 | 53.66788209 | -2.01364052 | 81.5888 | 56770.4644907407 | 56770.9410763889 | 509068010 | 21470 | 20000 | 21485.3 | 21486 | 0 | 21470 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20967.8 | 20967.8 | 41171.9 | 0 | PROCESSED | 57614.9785416667 | 57152 | 56789.6036805556 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 092010 | Mixed morphology supernova remnants are an important, but peculiar class of supernova remnants. They have a shell-type morphology in the radio, but the X-ray emission is centrally dominated. X-ray spectroscopy of several of these supernova remnants, indicate that their central plasma is often over-ionised and have enhanced abundances. Here we propose to study a typical member of this class, which has so far not received much attention, despite being bright and only mildly absorbed: 3C400.2. The remnant can be covered with four pointings, and is bright enough for imaging spectroscopy on the scale of the Suzaku PSF. This will enable us to study spectroscopic variation, confirm the preliminary detection of an RRC and map its distribution, and study the abundances. | GALACTIC DIFFUSE EMISSION | 5 | A | VINK | JACCO | NULL | NULL | EUR | 9 | AO9 | THE MIXED-MORPHOLOGY SUPERNOVA REMNANT 3C400.2 | XIS | Y |
| 3C400.2 SW | 294.5545 | 17.147 | 53.47817432 | -2.17482828 | 81.5886 | 56761.5284375 | 56762.0730555556 | 509069010 | 24152.8 | 20000 | 24152.8 | 24152.8 | 0 | 24153.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 23915 | 23915 | 47047.9 | 3 | PROCESSED | 57614.2434027778 | 57138 | 56772.6111226852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 092010 | Mixed morphology supernova remnants are an important, but peculiar class of supernova remnants. They have a shell-type morphology in the radio, but the X-ray emission is centrally dominated. X-ray spectroscopy of several of these supernova remnants, indicate that their central plasma is often over-ionised and have enhanced abundances. Here we propose to study a typical member of this class, which has so far not received much attention, despite being bright and only mildly absorbed: 3C400.2. The remnant can be covered with four pointings, and is bright enough for imaging spectroscopy on the scale of the Suzaku PSF. This will enable us to study spectroscopic variation, confirm the preliminary detection of an RRC and map its distribution, and study the abundances. | GALACTIC DIFFUSE EMISSION | 5 | A | VINK | JACCO | NULL | NULL | EUR | 9 | AO9 | THE MIXED-MORPHOLOGY SUPERNOVA REMNANT 3C400.2 | XIS | Y |
| 3C400.2 SE | 294.8215 | 17.1213 | 53.58084569 | -2.4098547 | 81.5889 | 56770.9416898148 | 56771.4758449074 | 509070010 | 24946.7 | 20000 | 24954.7 | 24946.7 | 0 | 24962.7 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 22749.4 | 22749.4 | 46135.9 | 0 | PROCESSED | 57614.9903009259 | 57152 | 56789.6293865741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 092010 | Mixed morphology supernova remnants are an important, but peculiar class of supernova remnants. They have a shell-type morphology in the radio, but the X-ray emission is centrally dominated. X-ray spectroscopy of several of these supernova remnants, indicate that their central plasma is often over-ionised and have enhanced abundances. Here we propose to study a typical member of this class, which has so far not received much attention, despite being bright and only mildly absorbed: 3C400.2. The remnant can be covered with four pointings, and is bright enough for imaging spectroscopy on the scale of the Suzaku PSF. This will enable us to study spectroscopic variation, confirm the preliminary detection of an RRC and map its distribution, and study the abundances. | GALACTIC DIFFUSE EMISSION | 5 | A | VINK | JACCO | NULL | NULL | EUR | 9 | AO9 | THE MIXED-MORPHOLOGY SUPERNOVA REMNANT 3C400.2 | XIS | Y |
| 3C400.2 NE | 294.7841 | 17.3445 | 53.75798011 | -2.26924911 | 81.5891 | 56770.0289351852 | 56770.4640162037 | 509071010 | 20231 | 20000 | 20239 | 20239 | 0 | 20231 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 18505 | 18505 | 37583.8 | 0 | PROCESSED | 57614.9798148148 | 57152 | 56789.6056712963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 092010 | Mixed morphology supernova remnants are an important, but peculiar class of supernova remnants. They have a shell-type morphology in the radio, but the X-ray emission is centrally dominated. X-ray spectroscopy of several of these supernova remnants, indicate that their central plasma is often over-ionised and have enhanced abundances. Here we propose to study a typical member of this class, which has so far not received much attention, despite being bright and only mildly absorbed: 3C400.2. The remnant can be covered with four pointings, and is bright enough for imaging spectroscopy on the scale of the Suzaku PSF. This will enable us to study spectroscopic variation, confirm the preliminary detection of an RRC and map its distribution, and study the abundances. | GALACTIC DIFFUSE EMISSION | 5 | A | VINK | JACCO | NULL | NULL | EUR | 9 | AO9 | THE MIXED-MORPHOLOGY SUPERNOVA REMNANT 3C400.2 | XIS | Y |
| G306.3-0.9 | 200.4753 | -63.5602 | 306.31531317 | -0.88874973 | 306.5675 | 56889.7845833333 | 56894.0099768518 | 509072010 | 190011.4 | 200000 | 190018.1 | 190011.4 | 0 | 190011.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14451.5 | 14451.5 | 20220 | 0 | PROCESSED | 57616.5396759259 | 57305 | 56938.2302777778 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 093109 | The origin of the distorted, inhomogeneous structure of mixed-morphology SNRs (MM SNRs) is a mystery. Recently we have discovered recombining plasma from MM SNRs. The existence of recombining plasma implies rapid cooling process in past. Recombining plasma, together with the peculiar morphologies, would indicate a new SNR evolution scenario. Our systematic analysis of recombining SNRs shows that the recombination ages are almost the same, although their dynamical ages range over an order of magnitude. Such a trend can be explained by past rapid rarefaction. This hypothesis can be tested by measuring a recombination age of a dynamically young recombining SNR. We thus propose a 100-ks Suzaku observation of G306.3-0.9, a candidate of the youngest recombining SNR ever. | GALACTIC DIFFUSE EMISSION | 5 | A | SAWADA | MAKOTO | Reynolds,Matsumura | NULL | JUS | 9 | AO9 | THE DYNAMICS OF MIXED-MORPHOLOGY SNRS PROBED BY THE YOUNGEST RECOMBINING PLASMA | XIS | Y |
| MBM16 | 49.7641 | 11.5835 | 170.59835317 | -37.27294118 | 77.8263 | 56867.2632638889 | 56869.0606018518 | 509073010 | 78810 | 80000 | 78818 | 78818 | 0 | 78810 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.4583449074 | 56748 | 56902.6996180556 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 096001 | Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions. | GALACTIC DIFFUSE EMISSION | 5 | A | GALEAZZI | MASSIMILIANO | NULL | NULL | USA | 9 | AO9 | CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE | XIS | Y |
| MBM16 | 49.7701 | 11.5795 | 170.60720168 | -37.27195697 | 254.3636 | 57057.0973726852 | 57059.5349421296 | 509073020 | 92042.5 | 80000 | 92042.5 | 92066.5 | 0 | 92066.5 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.6060763889 | 56748 | 57107.434224537 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 096001 | Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions. | GALACTIC DIFFUSE EMISSION | 5 | A | GALEAZZI | MASSIMILIANO | NULL | NULL | USA | 9 | AO9 | CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE | XIS | Y |
| MBM36 | 238.3613 | -4.7912 | 4.0047136 | 35.6981582 | 275.8793 | 56894.6980324074 | 56896.6598958333 | 509074010 | 83188.7 | 80000 | 83196.7 | 83188.7 | 0 | 83196.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 3755 | 3755 | 8940 | 0 | PROCESSED | 57616.559525463 | 56748 | 56929.2087615741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 096001 | Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions. | GALACTIC DIFFUSE EMISSION | 5 | A | GALEAZZI | MASSIMILIANO | NULL | NULL | USA | 9 | AO9 | CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE | XIS | Y |
| LDN1563 | 75.5225 | 13.8674 | 187.1486738 | -16.70848186 | 83.2339 | 56902.1301041667 | 56904.0071643518 | 509075010 | 41115.5 | 80000 | 41139.6 | 41139.5 | 0 | 41115.5 | 3 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.5646296296 | 56748 | 56926.5705439815 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 096001 | Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions. | GALACTIC DIFFUSE EMISSION | 5 | A | GALEAZZI | MASSIMILIANO | NULL | NULL | USA | 9 | AO9 | CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE | XIS | Y |
| MBM20 | 68.9408 | -14.6235 | 211.39729046 | -36.55969232 | 255.8156 | 57069.9923842593 | 57071.9654050926 | 509076010 | 81154 | 80000 | 81154 | 81162 | 0 | 81162 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.624537037 | 56748 | 57083.4173032407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 096001 | Solar Wind Charge Exchange (SWCX) contributes a significant background to X-ray observations of extended objects, and separate background observations may produce incorrect results, as the emission strength and spectrum are temporally variable. Characterizing and modeling SWCX emission requires understanding the distribution of neutral material in the magnetosheath and heliosphere, the properties and distribution of the solar wind, and the interaction cross-sections. We propose a multi-year monitoring campaign to measure and characterize the SWCX properties. The results will be used to verify and improve models of SWCX emission, an invaluable tool for the proper analysis and interpretation of data from current and future X-ray missions. | GALACTIC DIFFUSE EMISSION | 5 | A | GALEAZZI | MASSIMILIANO | NULL | NULL | USA | 9 | AO9 | CHARACTERIZATION OF SOLAR WIND CHARGE EXCHANGE | XIS | Y |
| GB_NORTH_1 | 266.1004 | -28.3619 | 0.35022505 | 0.52781175 | 106.0661 | 57104.6393981482 | 57106.6752777778 | 509077010 | 98240.7 | 100000 | 98240.7 | 98440.7 | 0 | 98440.7 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.8715277778 | 56748 | 57120.4153125 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 096002 | The Galactic Bulge (GB) regions are less contaminated by the strong Galactic X-ray background, and hence are more suitable to extract pure phenomena associated with the Galactic center (GC) activities. However, the covered area of the GB have been limited. We thus propose a new Key project focusing on the GB region. Objectives are (I) a search for an over-ionized plasma north of the GB as a counterpart of GB south, a relic of past Sgr A* activity, and (II) discovering unexpected features with unprecedented sensitivity of Suzaku for diffuse faint emissions. This Key project, together with the previous Key project on the GC, can complete the data set of the extended GC region as the Suzaku legacy. The data set will assist in making an observational strategy for the upcoming ASTRO-H project. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 9 | AO9 | MAPPING THE GALACTIC BULGE REGION -RELICS OF GC ACTIVITIES AND SUZAKU LEGACY- | XIS | Y |
| GB_NORTH_2 | 265.5401 | -28.4005 | 0.05846164 | 0.92703829 | 108.0199 | 57106.6765856482 | 57108.7243634259 | 509078010 | 95389.3 | 100000 | 95389.3 | 99828.4 | 0 | 99812.4 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.8717361111 | 56748 | 57119.4143981482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 096002 | The Galactic Bulge (GB) regions are less contaminated by the strong Galactic X-ray background, and hence are more suitable to extract pure phenomena associated with the Galactic center (GC) activities. However, the covered area of the GB have been limited. We thus propose a new Key project focusing on the GB region. Objectives are (I) a search for an over-ionized plasma north of the GB as a counterpart of GB south, a relic of past Sgr A* activity, and (II) discovering unexpected features with unprecedented sensitivity of Suzaku for diffuse faint emissions. This Key project, together with the previous Key project on the GC, can complete the data set of the extended GC region as the Suzaku legacy. The data set will assist in making an observational strategy for the upcoming ASTRO-H project. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 9 | AO9 | MAPPING THE GALACTIC BULGE REGION -RELICS OF GC ACTIVITIES AND SUZAKU LEGACY- | XIS | Y |
| GB_NORTH_3 | 265.8335 | -28.3716 | 0.21886292 | 0.72273612 | 108.0564 | 57108.7249074074 | 57110.9703703704 | 509079010 | 106967.4 | 100000 | 106967.4 | 108188.9 | 0 | 108188.9 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.8792939815 | 56748 | 57119.4192708333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 096002 | The Galactic Bulge (GB) regions are less contaminated by the strong Galactic X-ray background, and hence are more suitable to extract pure phenomena associated with the Galactic center (GC) activities. However, the covered area of the GB have been limited. We thus propose a new Key project focusing on the GB region. Objectives are (I) a search for an over-ionized plasma north of the GB as a counterpart of GB south, a relic of past Sgr A* activity, and (II) discovering unexpected features with unprecedented sensitivity of Suzaku for diffuse faint emissions. This Key project, together with the previous Key project on the GC, can complete the data set of the extended GC region as the Suzaku legacy. The data set will assist in making an observational strategy for the upcoming ASTRO-H project. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 9 | AO9 | MAPPING THE GALACTIC BULGE REGION -RELICS OF GC ACTIVITIES AND SUZAKU LEGACY- | XIS | Y |
| GB_NORTH_4 | 264.8998 | -28.3109 | 359.83607677 | 1.45248781 | 106.6967 | 57110.9717708333 | 57113.0203472222 | 509080010 | 88194.1 | 100000 | 88194.1 | 95045.5 | 0 | 95061.5 | 3 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.8835648148 | 56748 | 57125.4051736111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 096002 | The Galactic Bulge (GB) regions are less contaminated by the strong Galactic X-ray background, and hence are more suitable to extract pure phenomena associated with the Galactic center (GC) activities. However, the covered area of the GB have been limited. We thus propose a new Key project focusing on the GB region. Objectives are (I) a search for an over-ionized plasma north of the GB as a counterpart of GB south, a relic of past Sgr A* activity, and (II) discovering unexpected features with unprecedented sensitivity of Suzaku for diffuse faint emissions. This Key project, together with the previous Key project on the GC, can complete the data set of the extended GC region as the Suzaku legacy. The data set will assist in making an observational strategy for the upcoming ASTRO-H project. | GALACTIC DIFFUSE EMISSION | 5 | A | KOYAMA | KATSUJI | NULL | NULL | JAP | 9 | AO9 | MAPPING THE GALACTIC BULGE REGION -RELICS OF GC ACTIVITIES AND SUZAKU LEGACY- | XIS | Y |
| SN1006_SE1 | 225.8641 | -42.0384 | 327.62177329 | 14.41744154 | 286.0629 | 56883.8521064815 | 56887.5210648148 | 509082010 | 201832.2 | 480000 | 201832.2 | 202488.1 | 0 | 202520.1 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.5228240741 | 56748 | 56910.6390509259 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 096004 | We propose deep XIS observations of SN1006, a Type Ia supernova remnant (SNR) in the Galaxy. Our immediate objective is to detect weak emissions, Cr K-alpha, Mn K-alpha, and Fe K-beta lines, which are key to diagnosing the evolution of the Type Ia SN progenitor and the efficiency of collisionless electron heating at the SNR reverse shock. Although the total requested exposure is quite long, the observation is well worth the risk and will certainly provide a heritage dataset prominent in the legacy of Suzaku. This proposal consists of the two steps. The first science goal requires the 400-ks exposure, while the second goal requires additional 800 ks. Approval of only the first step will be accepted. | GALACTIC DIFFUSE EMISSION | 5 | A | YAMAGUCHI | HIROYA | NULL | NULL | USA | 9 | AO9 | THERMAL X-RAYS FROM SN 1006: THE UNIQUE TYPE IA SNR IN THE EXTREMELY LOW-DENSITY AND LOW-METALLICITY ENVIRONMENT | XIS | Y |
| SN1006_SE1 | 225.857 | -42.039 | 327.61674963 | 14.4195613 | 107.6985 | 57063.4521643518 | 57069.9807060185 | 509082020 | 258382 | 280000 | 258382 | 278790.1 | 0 | 278854.1 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.6457523148 | 56748 | 57080.4416898148 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 096004 | We propose deep XIS observations of SN1006, a Type Ia supernova remnant (SNR) in the Galaxy. Our immediate objective is to detect weak emissions, Cr K-alpha, Mn K-alpha, and Fe K-beta lines, which are key to diagnosing the evolution of the Type Ia SN progenitor and the efficiency of collisionless electron heating at the SNR reverse shock. Although the total requested exposure is quite long, the observation is well worth the risk and will certainly provide a heritage dataset prominent in the legacy of Suzaku. This proposal consists of the two steps. The first science goal requires the 400-ks exposure, while the second goal requires additional 800 ks. Approval of only the first step will be accepted. | GALACTIC DIFFUSE EMISSION | 5 | A | YAMAGUCHI | HIROYA | NULL | NULL | USA | 9 | AO9 | THERMAL X-RAYS FROM SN 1006: THE UNIQUE TYPE IA SNR IN THE EXTREMELY LOW-DENSITY AND LOW-METALLICITY ENVIRONMENT | XIS | Y |
| SN1006_BGD1 | 225.9444 | -42.5002 | 327.43636425 | 13.98792654 | 286.4314 | 56887.5218171296 | 56888.0141203704 | 509083010 | 32100.9 | 30000 | 32108.9 | 32108.9 | 0 | 32100.9 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.5011111111 | 56748 | 56910.6401736111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 096004 | We propose deep XIS observations of SN1006, a Type Ia supernova remnant (SNR) in the Galaxy. Our immediate objective is to detect weak emissions, Cr K-alpha, Mn K-alpha, and Fe K-beta lines, which are key to diagnosing the evolution of the Type Ia SN progenitor and the efficiency of collisionless electron heating at the SNR reverse shock. Although the total requested exposure is quite long, the observation is well worth the risk and will certainly provide a heritage dataset prominent in the legacy of Suzaku. This proposal consists of the two steps. The first science goal requires the 400-ks exposure, while the second goal requires additional 800 ks. Approval of only the first step will be accepted. | GALACTIC DIFFUSE EMISSION | 5 | A | YAMAGUCHI | HIROYA | NULL | NULL | USA | 9 | AO9 | THERMAL X-RAYS FROM SN 1006: THE UNIQUE TYPE IA SNR IN THE EXTREMELY LOW-DENSITY AND LOW-METALLICITY ENVIRONMENT | XIS | Y |
| SN1006_BGD2 | 226.2226 | -42.2202 | 327.76465581 | 14.12663913 | 286.4366 | 56888.0146875 | 56888.6460416667 | 509084010 | 34849.7 | 30000 | 34879.3 | 34881.7 | 0 | 34849.7 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.5054050926 | 56748 | 56910.6406365741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 096004 | We propose deep XIS observations of SN1006, a Type Ia supernova remnant (SNR) in the Galaxy. Our immediate objective is to detect weak emissions, Cr K-alpha, Mn K-alpha, and Fe K-beta lines, which are key to diagnosing the evolution of the Type Ia SN progenitor and the efficiency of collisionless electron heating at the SNR reverse shock. Although the total requested exposure is quite long, the observation is well worth the risk and will certainly provide a heritage dataset prominent in the legacy of Suzaku. This proposal consists of the two steps. The first science goal requires the 400-ks exposure, while the second goal requires additional 800 ks. Approval of only the first step will be accepted. | GALACTIC DIFFUSE EMISSION | 5 | A | YAMAGUCHI | HIROYA | NULL | NULL | USA | 9 | AO9 | THERMAL X-RAYS FROM SN 1006: THE UNIQUE TYPE IA SNR IN THE EXTREMELY LOW-DENSITY AND LOW-METALLICITY ENVIRONMENT | XIS | Y |
| SN1006_BGD3 | 226.4731 | -42.5186 | 327.77356316 | 13.77561257 | 286.5156 | 56888.6466550926 | 56889.2084606482 | 509085010 | 31650 | 30000 | 31650 | 31650 | 0 | 31650 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.5050115741 | 56748 | 56910.6423611111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 096004 | We propose deep XIS observations of SN1006, a Type Ia supernova remnant (SNR) in the Galaxy. Our immediate objective is to detect weak emissions, Cr K-alpha, Mn K-alpha, and Fe K-beta lines, which are key to diagnosing the evolution of the Type Ia SN progenitor and the efficiency of collisionless electron heating at the SNR reverse shock. Although the total requested exposure is quite long, the observation is well worth the risk and will certainly provide a heritage dataset prominent in the legacy of Suzaku. This proposal consists of the two steps. The first science goal requires the 400-ks exposure, while the second goal requires additional 800 ks. Approval of only the first step will be accepted. | GALACTIC DIFFUSE EMISSION | 5 | A | YAMAGUCHI | HIROYA | NULL | NULL | USA | 9 | AO9 | THERMAL X-RAYS FROM SN 1006: THE UNIQUE TYPE IA SNR IN THE EXTREMELY LOW-DENSITY AND LOW-METALLICITY ENVIRONMENT | XIS | Y |
| SN1006_BGD4 | 226.2633 | -42.7499 | 327.5160888 | 13.6541367 | 286.3809 | 56889.2090740741 | 56889.7793865741 | 509086010 | 33511.6 | 30000 | 33515.6 | 33511.6 | 0 | 33519.6 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.5076851852 | 56748 | 56910.6440162037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 096004 | We propose deep XIS observations of SN1006, a Type Ia supernova remnant (SNR) in the Galaxy. Our immediate objective is to detect weak emissions, Cr K-alpha, Mn K-alpha, and Fe K-beta lines, which are key to diagnosing the evolution of the Type Ia SN progenitor and the efficiency of collisionless electron heating at the SNR reverse shock. Although the total requested exposure is quite long, the observation is well worth the risk and will certainly provide a heritage dataset prominent in the legacy of Suzaku. This proposal consists of the two steps. The first science goal requires the 400-ks exposure, while the second goal requires additional 800 ks. Approval of only the first step will be accepted. | GALACTIC DIFFUSE EMISSION | 5 | A | YAMAGUCHI | HIROYA | NULL | NULL | USA | 9 | AO9 | THERMAL X-RAYS FROM SN 1006: THE UNIQUE TYPE IA SNR IN THE EXTREMELY LOW-DENSITY AND LOW-METALLICITY ENVIRONMENT | XIS | Y |
| W63 | 304.8117 | 45.7821 | 82.4091518 | 5.43831098 | 57.9996 | 57171.5134837963 | 57172.616712963 | 510025010 | 42700.3 | 150000 | 44302 | 44606 | 0 | 42700.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13774.7 | 13774.7 | 92773.9 | 0 | PROCESSED | 57618.8028703704 | 57636 | 57260.7216898148 | 3.0.22.44 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 101315 | We propose to conduct a deep Suzaku observation of the X-ray bright central portion of the Galactic supernova remnant (SNR) W63 (G82.2+5.3). This SNR belongs to a class of objects known as mixed-morphology SNRs (MMSNRs) that feature a shell-like radio morphology with a center-filled thermal X-ray morphology: the origin of these contrasting morphologies for these SNRs remains unknown. Our proposed Suzaku observation of this SNR will investigate the putative overabundances of such elements as magnesium, silicon and sulfur (as reported in a previous analysis of an ASCA observation of W63) as well as search for evidence of over-ionization conditions in the X-ray emitting plasma, as has been reported for other MMSNRs. | GALACTIC DIFFUSE EMISSION | 5 | C | PANNUTI | THOMAS | NULL | NULL | USA | 10 | AO10 | A SUZAKU OBSERVATION OF THE GALACTIC SUPERNOVA REMNANT W63 (G82.2+5.3) | XIS | Y |
| 3C120 | 68.2984 | 5.3555 | 190.37315865 | -27.39441526 | 237.4585 | 53775.1527199074 | 53776.2433217593 | 700001010 | 41932.1 | 160000 | 41932.1 | 41932.1 | 41932.1 | 41932.1 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 34094.1 | 34094.1 | 94221.9 | 1 | PROCESSED | 57532.9769791667 | 54247 | 53906.2470601852 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001003 | Broad line radio galaxies (BLRGs) are rare kind of AGNs where the emission from the accretion disc is visible as well as the extended jet emission. Direct comparison of broad-band spectrum in BLRGs to those of Sy-1s provides important clue to understand the formation of relativistic jets. We propose a 160 ksec (40ksec x4) observations of the brightest BLRG 3C120 with Suzaku. Recent XMM and Beppo-SAX observations confirm remarkable spectral features including fluorescent Fe line. Our goals are three folds; (1) Monitoring the variability correlation between Fe line and the Compton reflection hump, (2) Precise measurement of total luminosity as a probe of various accretion states, and (3) Resolving excess soft components, warm absorber, and 6.9 keV line, which are still under debate. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | KATAOKA | JUN | NULL | NULL | JAP | 0 | SWG | BROAD-BAND MONITORING OF 3C120 IN VARIOUS ACCRETING STATES | XIS | N |
| 3C120 | 68.298 | 5.3556 | 190.3728125 | -27.39468757 | 237.4583 | 53782.5602199074 | 53783.5876967593 | 700001020 | 41554.5 | 160000 | 41554.5 | 41554.5 | 41554.5 | 41554.5 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 36846.1 | 36846.1 | 88772 | 2 | PROCESSED | 57533.0172685185 | 54247 | 54041.2956365741 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001003 | Broad line radio galaxies (BLRGs) are rare kind of AGNs where the emission from the accretion disc is visible as well as the extended jet emission. Direct comparison of broad-band spectrum in BLRGs to those of Sy-1s provides important clue to understand the formation of relativistic jets. We propose a 160 ksec (40ksec x4) observations of the brightest BLRG 3C120 with Suzaku. Recent XMM and Beppo-SAX observations confirm remarkable spectral features including fluorescent Fe line. Our goals are three folds; (1) Monitoring the variability correlation between Fe line and the Compton reflection hump, (2) Precise measurement of total luminosity as a probe of various accretion states, and (3) Resolving excess soft components, warm absorber, and 6.9 keV line, which are still under debate. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | KATAOKA | JUN | NULL | NULL | JAP | 0 | SWG | BROAD-BAND MONITORING OF 3C120 IN VARIOUS ACCRETING STATES | XIS | N |
| 3C120 | 68.2993 | 5.3535 | 190.3755878 | -27.39480435 | 262.4873 | 53789.4598726852 | 53790.8748958333 | 700001030 | 40907.3 | 160000 | 40907.3 | 40907.3 | 40907.3 | 40907.3 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 38481.7 | 38481.7 | 77876 | 2 | PROCESSED | 57533.073900463 | 54247 | 54041.5149189815 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001003 | Broad line radio galaxies (BLRGs) are rare kind of AGNs where the emission from the accretion disc is visible as well as the extended jet emission. Direct comparison of broad-band spectrum in BLRGs to those of Sy-1s provides important clue to understand the formation of relativistic jets. We propose a 160 ksec (40ksec x4) observations of the brightest BLRG 3C120 with Suzaku. Recent XMM and Beppo-SAX observations confirm remarkable spectral features including fluorescent Fe line. Our goals are three folds; (1) Monitoring the variability correlation between Fe line and the Compton reflection hump, (2) Precise measurement of total luminosity as a probe of various accretion states, and (3) Resolving excess soft components, warm absorber, and 6.9 keV line, which are still under debate. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | KATAOKA | JUN | NULL | NULL | JAP | 0 | SWG | BROAD-BAND MONITORING OF 3C120 IN VARIOUS ACCRETING STATES | XIS | N |
| 3C120 | 68.2979 | 5.3541 | 190.37414386 | -27.39561637 | 262.5053 | 53796.9456828704 | 53797.8606365741 | 700001040 | 40905.1 | 160000 | 40913.1 | 40921.1 | 40921.1 | 40905.1 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 40311.8 | 40311.8 | 79045.9 | 0 | PROCESSED | 57533.1408912037 | 54247 | 54041.627025463 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001003 | Broad line radio galaxies (BLRGs) are rare kind of AGNs where the emission from the accretion disc is visible as well as the extended jet emission. Direct comparison of broad-band spectrum in BLRGs to those of Sy-1s provides important clue to understand the formation of relativistic jets. We propose a 160 ksec (40ksec x4) observations of the brightest BLRG 3C120 with Suzaku. Recent XMM and Beppo-SAX observations confirm remarkable spectral features including fluorescent Fe line. Our goals are three folds; (1) Monitoring the variability correlation between Fe line and the Compton reflection hump, (2) Precise measurement of total luminosity as a probe of various accretion states, and (3) Resolving excess soft components, warm absorber, and 6.9 keV line, which are still under debate. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | KATAOKA | JUN | NULL | NULL | JAP | 0 | SWG | BROAD-BAND MONITORING OF 3C120 IN VARIOUS ACCRETING STATES | XIS | N |
| MCG -5-23-16 | 146.9445 | -30.9023 | 262.72964912 | 17.28396386 | 118.3849 | 53711.9526388889 | 53714.4939699074 | 700002010 | 95677.4 | 100000 | 95677.4 | 95717.4 | 95717.4 | 95685.4 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 85564.7 | 85564.7 | 219525.1 | 3 | PROCESSED | 57532.4508680556 | 54247 | 54039.1988310185 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001006 | We request a 100ks Suzaku observation of the bright Seyfert galaxy, MCG -5-23-16 simultaneously with approved XMM-Newton and Chandra HETG observations in December 2005. MCG -5-23-16 has one of the best known examples of a relativistically broadened iron K line. With a Swift-BAT flux of 1.6e-10 cgs (15-100 keV), it is one of the brightest AGN above 10 keV. The simultaneous observations will allow us to determine the shape of the broad relativistic Fe line after subtracting the narrow line components measured by HETG. Importantly, Suzaku's wide bandpass will accurately measure the broad-band continuum and reflection component of MCG -5-23-16, essential for constraining the broad iron line. These observations will also allow us to determine the temperature of the high energy cut-off. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | REEVES | JAMES | NULL | NULL | JAP | 0 | SWG | PROBING THE BROAD IRON LINE AND HIGH ENERGY CONTINUUM OF MCG -5-23-16 SIMULTANEOUSLY WITH SUZAKU, XMM-NEWTON AND CHANDRA | HXD | N |
| NGC 4051 | 180.8556 | 44.5807 | 148.68917976 | 70.06918189 | 135.3482 | 53684.8015509259 | 53687.4315277778 | 700004010 | 119578 | 150000 | 119610 | 119610 | 119586 | 119578 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 120004.7 | 120004.7 | 227191.8 | 3 | PROCESSED | 57528.0225810185 | 54247 | 54037.5713078704 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001012 | We propose to obtain a broad band spectrum of the narrow-line Seyfert 1 (NLS1) NGC 4051. NLS1s are often presumed that they host a relatively small black hole with a very high accretion rate. Such a class would have played an important role in the growth of black holes in a cosmological context. We will measure the intrinsic photon index, amount of reflection, and high energy cutoff for the first time to investigate an accretion disk under a high accretion rate and compare them with conventional broad-line Seyferts. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TERASHIMA | YUICHI | NULL | NULL | JAP | 0 | SWG | THE ACCRETION IN THE NARROW-LINE SEYFERT 1 NGC 4051 PROBED BY A BROAD BAND SPECTRUM | HXD | N |
| NGC 2992 | 146.4352 | -14.2714 | 249.66741784 | 28.82528499 | 102.6298 | 53680.5956481482 | 53681.5850925926 | 700005010 | 37502.9 | 120000 | 37502.9 | 38756.8 | 37518 | 37715 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 32073 | 32073 | 85485.9 | 1 | PROCESSED | 57527.9475231482 | 54247 | 54037.5593518518 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001013 | NGC 2992 is a nearby Seyfert 1.9 galaxy showing long-term (20 yrs) large amplitude (factor of 20) variability. This object showed switching between Compton-thick and -thin. Recent RXTE monitoring has shown that this object is highly variable on shorter time scales (2 weeks). We propose three Suzaku observations to monitor the variability of absorption column, broad band continuum shape, and Fe line intensity to understand the cause of the remarkable variability. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TERASHIMA | YUICHI | NULL | NULL | JAP | 0 | SWG | THE SPECTRAL VARIABILITY IN NGC 2992: FE-LINE, REFLECTION, AND COMPTON-THIN/THICK SWITCHING | XIS | N |
| NGC 2992 | 146.4207 | -14.2696 | 249.65504756 | 28.81616071 | 88.7924 | 53693.8781597222 | 53694.9759722222 | 700005020 | 37493.5 | 120000 | 37656.5 | 39691.5 | 37493.5 | 37820.5 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 33899.1 | 33899.1 | 94847.9 | 1 | PROCESSED | 57528.0334490741 | 54247 | 54037.7316087963 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001013 | NGC 2992 is a nearby Seyfert 1.9 galaxy showing long-term (20 yrs) large amplitude (factor of 20) variability. This object showed switching between Compton-thick and -thin. Recent RXTE monitoring has shown that this object is highly variable on shorter time scales (2 weeks). We propose three Suzaku observations to monitor the variability of absorption column, broad band continuum shape, and Fe line intensity to understand the cause of the remarkable variability. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TERASHIMA | YUICHI | NULL | NULL | JAP | 0 | SWG | THE SPECTRAL VARIABILITY IN NGC 2992: FE-LINE, REFLECTION, AND COMPTON-THIN/THICK SWITCHING | HXD | N |
| NGC 2992 | 146.4592 | -14.2821 | 249.69438343 | 28.83515423 | 128.4959 | 53717.4275462963 | 53718.506412037 | 700005030 | 46836.1 | 120000 | 46844.1 | 46868.1 | 46836.1 | 46860.1 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 44298.3 | 44298.3 | 93207.9 | 1 | PROCESSED | 57532.4690046296 | 54247 | 54039.2254861111 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001013 | NGC 2992 is a nearby Seyfert 1.9 galaxy showing long-term (20 yrs) large amplitude (factor of 20) variability. This object showed switching between Compton-thick and -thin. Recent RXTE monitoring has shown that this object is highly variable on shorter time scales (2 weeks). We propose three Suzaku observations to monitor the variability of absorption column, broad band continuum shape, and Fe line intensity to understand the cause of the remarkable variability. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TERASHIMA | YUICHI | NULL | NULL | JAP | 0 | SWG | THE SPECTRAL VARIABILITY IN NGC 2992: FE-LINE, REFLECTION, AND COMPTON-THIN/THICK SWITCHING | HXD | N |
| ARP220 | 233.7664 | 23.5658 | 36.73879852 | 53.01919685 | 114.8377 | 53742.3490856482 | 53744.9654398148 | 700006010 | 98550.6 | 100000 | 98558.6 | 98550.6 | 98558.6 | 98558.6 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 93362.3 | 93362.3 | 226041.9 | 2 | PROCESSED | 57532.6850925926 | 54247 | 54040.0356597222 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001033 | We propose a 100 ks observation of the nearest ultraluminous infrared galaxy (ULIG) Arp220. The major objective is to search for evidence of heavily obscured nuclei. First detection of a Compton-thick source may be possible with the HXD's sensitivity, if a powerful nucleus is present, leading to a major discovery. The good quality XIS spectrum can be decisive for the origin of the strong Fe K line, barely detected with the previous XMM-Newton observation. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | IWASAWA | KAZUSHI | NULL | NULL | JAP | 0 | SWG | HARD X-RAY EMISSION FROM THE NEAREST ULTRALUMINOUS INFRARED GALAXY ARP220 | HXD | N |
| MCG-6-30-15 | 203.9706 | -34.2946 | 313.28931603 | 27.68170589 | 107.0204 | 53744.9738310185 | 53749.1390277778 | 700007010 | 143196.5 | 300000 | 143196.5 | 143316.2 | 143268.5 | 143244.5 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 126290.3 | 126290.3 | 359839.9 | 4 | PROCESSED | 57532.7604398148 | 54247 | 54040.4060416667 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001035 | The broad iron line in the Seyfert 1 galaxy MCG-6-30-15 shows that most of the power is released at 2--4 gravitational radii enabling the strong gravity, accretion flow and energy release in that exciting regime to be studied. The spectral variability of the source decomposes into a highly variable power law and a reflection-dominated component, containing the iron line and Compton hump, which varies significantly but with much less amplitude. This can be explained by the extreme gravitational light bending occuring in this region. We propose to observe MCG--6-30-15 for 4 x 50~ks in order to determine for the first time the variability of the reflection over a wide range of energies from below 1 keV to above 40 keV and timescales . | EXTRAGALACTIC COMPACT SOURCES | 7 | A | FABIAN | ANDREW | NULL | NULL | JAP | 0 | SWG | REFLECTION, ABSORPTION AND STRONG GRAVITY AROUND THE SPINNING BLACK HOLE IN MCG--6-30-15 | XIS | N |
| MCG-6-30-15 | 203.9717 | -34.2976 | 313.28966663 | 27.67858669 | 102.4356 | 53758.5062962963 | 53761.0835648148 | 700007020 | 98483.4 | 300000 | 98483.4 | 98483.4 | 98483.4 | 98483.4 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 81892.2 | 81892.2 | 222649.7 | 3 | PROCESSED | 57532.8430902778 | 54247 | 54059.5463773148 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001035 | The broad iron line in the Seyfert 1 galaxy MCG-6-30-15 shows that most of the power is released at 2--4 gravitational radii enabling the strong gravity, accretion flow and energy release in that exciting regime to be studied. The spectral variability of the source decomposes into a highly variable power law and a reflection-dominated component, containing the iron line and Compton hump, which varies significantly but with much less amplitude. This can be explained by the extreme gravitational light bending occuring in this region. We propose to observe MCG--6-30-15 for 4 x 50~ks in order to determine for the first time the variability of the reflection over a wide range of energies from below 1 keV to above 40 keV and timescales . | EXTRAGALACTIC COMPACT SOURCES | 7 | A | FABIAN | ANDREW | NULL | NULL | JAP | 0 | SWG | REFLECTION, ABSORPTION AND STRONG GRAVITY AROUND THE SPINNING BLACK HOLE IN MCG--6-30-15 | XIS | N |
| MCG-6-30-15 | 203.9713 | -34.2978 | 313.28925681 | 27.67845448 | 102.4359 | 53762.928275463 | 53765.368275463 | 700007030 | 96691.9 | 300000 | 96691.9 | 96691.9 | 96699.9 | 96699.9 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 89819.4 | 89819.4 | 210801.9 | 5 | PROCESSED | 57532.8529861111 | 54247 | 54040.8156828704 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001035 | The broad iron line in the Seyfert 1 galaxy MCG-6-30-15 shows that most of the power is released at 2--4 gravitational radii enabling the strong gravity, accretion flow and energy release in that exciting regime to be studied. The spectral variability of the source decomposes into a highly variable power law and a reflection-dominated component, containing the iron line and Compton hump, which varies significantly but with much less amplitude. This can be explained by the extreme gravitational light bending occuring in this region. We propose to observe MCG--6-30-15 for 4 x 50~ks in order to determine for the first time the variability of the reflection over a wide range of energies from below 1 keV to above 40 keV and timescales . | EXTRAGALACTIC COMPACT SOURCES | 7 | A | FABIAN | ANDREW | NULL | NULL | JAP | 0 | SWG | REFLECTION, ABSORPTION AND STRONG GRAVITY AROUND THE SPINNING BLACK HOLE IN MCG--6-30-15 | XIS | N |
| 1H 0707-495 | 107.1586 | -49.5558 | 260.16951247 | -17.68246857 | 144.7199 | 53707.1759143518 | 53710.0974537037 | 700008010 | 97229.1 | 100000 | 97852.9 | 100389.1 | 97229.1 | 97814.9 | 4 | 2 | 4 | 4 | 1 | 0 | 0 | 91800.8 | 91800.8 | 252368.8 | 4 | PROCESSED | 57532.4288194444 | 54247 | 54059.7078472222 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001040 | We propose a 100 ks observation of the NLS1 1H 0707--495 in order to understand its remarkable and puzzling spectral and variability properties. The Suzaku data will help us to disentangle between the two interpretations adopted so far, namely partial covering and relativistically blurred reflection. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MINIUTTI | GIOVANNI | NULL | NULL | JAP | 0 | SWG | THE EXTREME PROPERTIES OF THE NLS1 GALAXY 1H 0707-495 | XIS | N |
| PG 1211+143 | 183.6045 | 14.1097 | 267.53559231 | 74.37841457 | 120.7913 | 53698.7348263889 | 53701.3397453704 | 700009010 | 96324.1 | 100000 | 96590 | 97580.2 | 96324.1 | 96324.1 | 3 | 2 | 3 | 3 | 1 | 0 | 0 | 84008.7 | 84008.7 | 225043.8 | 2 | PROCESSED | 57528.1616203704 | 54247 | 54038.7422106482 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001041 | A 100ks Suzaku observation of the NLS1, PG 1211+143 is proposed. Previous XMM-Newton and Chandra observation claimed both blue-shifted (0.1c) and redshifted (0.26c-0.40c) iron Kalpha absorption lines. The redshifted iron K lines may originate from matter falling onto the supermassive black hole. The high effective area and low background of Suzaku XIS above 5 keV will enable us to measure these relativistically shifted iron lines in PG 1211+143 with great accuracy. Constraining the time variability of the lines will allow us to determine the physical origins of the absorption, e.g. failed jet/outflow or gravitational redshift from a Kerr black hole. The excellent broadband capabilities of Suzaku will accurately determine the continuum, essential for modeling the iron K band. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | REEVES | JAMES | NULL | NULL | JAP | 0 | SWG | EXPLORING THE RELATIVISTICALLY SHIFTED IRON LINES IN PG 1211+143 | HXD | N |
| 0836+714 | 130.267 | 70.829 | 143.62710847 | 34.4182022 | 294.8268 | 53809.7578125 | 53810.5836111111 | 700010010 | 55626.1 | 50000 | 55634.1 | 55634.1 | 55626.1 | 55634.1 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 47405.8 | 47405.8 | 71341.9 | 1 | PROCESSED | 57533.2238541667 | 54247 | 54041.9651851852 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001061 | We propose two 50 ks observations, one for each of two EGRET blazars, 1510-089 (OR -017) and 0836+710 (4C +71.07). Both objects show extremely hard X-ray spectra, with photon indices about 1.3. The blazar 1510-089 ($z = 0.361$) is among a few OVV quasars showing prominent soft X-ray excess. The blazar 0836+710 ($z = 2.172)$ is the brightest X-ray source among the high redshift ($z>2$) quasars, and its very hard X-ray spectrum extends down to soft X-rays. Studying spectral shape and variability in the soft X-ray band relative to variability in the mid X-ray and optical bands can help to reveal nature of the soft X-ray excess of unknown origin, and multifrequency variability studies can provide constraints on the structure of jets on subparsec scales. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MADEJSKI | GREG | NULL | NULL | JAP | 0 | SWG | TESTING THE SHOCK-IN-JET MODEL FOR NONTHERMAL FLARES IN BLAZARS VIA SUZAKU OBSERVATIONS | HXD | N |
| SWIFT J0746.3+2548 | 116.6142 | 25.8792 | 194.5201067 | 22.91801121 | 97.0095 | 53678.357974537 | 53680.5862847222 | 700011010 | 99428.4 | 100000 | 99523.5 | 100452.4 | 99428.4 | 99723.5 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 87699.5 | 87699.5 | 192472 | 4 | PROCESSED | 57527.9575694445 | 54247 | 54037.5799074074 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001087 | Recently the BAT gamma-ray detector onboard Swift satellite has discovered very flat hard X-ray sources with photon index ~ 1.5 above 100 keV. The x-ray spectrum obtained with the XRT on Swiftis highly variable on time scales < 90 minutes. This variability and flat continuum spectrum suggests that this source is classified as a blazar. If this association is real, we have a precious chance to obtain spectrum upto several hundred keV in the source frame of the source. This wide range is of particularly importanceto study the blazar spectrum, or the electron distribution. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TAKAHASHI | TADAYUKI | NULL | NULL | JAP | 0 | SWG | SUZAKU OBSERVATION OF A HIGH REDSHIFT BLAZAR RECENTLY DISCOVERED BY THE BAT ON SWIFT | NULL | N |
| PKS2155-304 | 329.7191 | -30.2247 | 17.73226544 | -52.24760927 | 254.1358 | 53704.7749884259 | 53706.3613888889 | 700012010 | 63911.4 | 80000 | 63919.4 | 63911.4 | 63919.4 | 63916.6 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 58011.4 | 58011.4 | 137049.8 | 3 | PROCESSED | 57532.3797685185 | 54247 | 54038.8920138889 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001100 | Jets in blazars are believed to be a powerful site of particle acceleration. TeV emitting blazars are very important, because we can study very end of electron distribution near the maximum energy by using X-ray spectrum, because X-ray emission is believed to be due to synchrotron emission from the higher energy electron. Comparison of spectral index between X-ray and TeV gives us a crucial information on these source, because this is very sensitive to the particle injection and rapid cooling. In order to maximize the capability of sensitive hard X-ray observations of Suzaku, we propose reserved TOO observations for the next six months of PV phase from the TeV emitting blazars established by HESS, selected from five candidates. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TAKAHASHI | TADAYUKI | NULL | NULL | JAP | 0 | SWG-TOO | RESERVED TOO OBSERVATIONS OF SELECTED TEV-BRIGHT BLAZARS | XIS | N |
| NGC4418 | 186.7074 | -0.9383 | 290.03230216 | 61.31559989 | 292.8039 | 53929.4791898148 | 53931.280775463 | 701001010 | 68348.5 | 70000 | 68348.5 | 68348.5 | 68348.5 | 68348.5 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 57110.3 | 57110.3 | 155634 | 1 | PROCESSED | 57534.9858564815 | 54408 | 53942.4601388889 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010001 | We propose Suzaku observations at E > 10 keV of nearby ultraluminous infrared galaxies (ULIRGs), for which our infrared spectroscopy has strongly suggested the presence of luminous AGNs deeply buried in gas and dust. However, extreme starbursts are still a possibility. Through the proposed X-ray observations using Suzaku, we aim to distinguish clearly between buried AGNs (strong X-ray emitters) and extreme starbursts (weak X-ray emitters), and to obtain convincing evidence for luminous buried AGNs. Since buried AGNs in these ULIRGs' cores are likely to suffer from Compton-thick X-ray absorption, the high sensitivity at E > 10 keV achieved by Suzaku HXD PIN is crucial for the success of this experiment. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | IMANISHI | MASATOSHI | NULL | NULL | JAP | 1 | AO1 | COMPTON THICK BURIED AGNS IN NEARBY ULTRALUMINOUS INFRARED GALAXIES | HXD | N |
| UGC5101 | 143.841 | 61.3185 | 152.55229096 | 42.85621781 | 331.581 | 53825.1798148148 | 53826.3509722222 | 701002010 | 48990.2 | 70000 | 48990.2 | 48990.2 | 48990.2 | 48990.2 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 43974.8 | 43974.8 | 101177.9 | 0 | PROCESSED | 57533.3610763889 | 54735 | 53905.890625 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010001 | We propose Suzaku observations at E > 10 keV of nearby ultraluminous infrared galaxies (ULIRGs), for which our infrared spectroscopy has strongly suggested the presence of luminous AGNs deeply buried in gas and dust. However, extreme starbursts are still a possibility. Through the proposed X-ray observations using Suzaku, we aim to distinguish clearly between buried AGNs (strong X-ray emitters) and extreme starbursts (weak X-ray emitters), and to obtain convincing evidence for luminous buried AGNs. Since buried AGNs in these ULIRGs' cores are likely to suffer from Compton-thick X-ray absorption, the high sensitivity at E > 10 keV achieved by Suzaku HXD PIN is crucial for the success of this experiment. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | IMANISHI | MASATOSHI | NULL | NULL | JAP | 1 | AO1 | COMPTON THICK BURIED AGNS IN NEARBY ULTRALUMINOUS INFRARED GALAXIES | HXD | N |
| UGC5101 | 144.0189 | 61.4178 | 152.38145034 | 42.89433298 | 112.6892 | 54039.7635300926 | 54040.396087963 | 701002020 | 42166 | 35000 | 42166 | 42174 | 42182 | 42182 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 33558.9 | 33558.9 | 54651.9 | 0 | PROCESSED | 57536.0043518518 | 54735 | 54063.3945949074 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010001 | We propose Suzaku observations at E > 10 keV of nearby ultraluminous infrared galaxies (ULIRGs), for which our infrared spectroscopy has strongly suggested the presence of luminous AGNs deeply buried in gas and dust. However, extreme starbursts are still a possibility. Through the proposed X-ray observations using Suzaku, we aim to distinguish clearly between buried AGNs (strong X-ray emitters) and extreme starbursts (weak X-ray emitters), and to obtain convincing evidence for luminous buried AGNs. Since buried AGNs in these ULIRGs' cores are likely to suffer from Compton-thick X-ray absorption, the high sensitivity at E > 10 keV achieved by Suzaku HXD PIN is crucial for the success of this experiment. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | IMANISHI | MASATOSHI | NULL | NULL | JAP | 1 | AO1 | COMPTON THICK BURIED AGNS IN NEARBY ULTRALUMINOUS INFRARED GALAXIES | HXD | Y |
| IRAS13224-3809 | 201.327 | -38.416 | 310.18598264 | 23.97820794 | 118.5234 | 54126.2420601852 | 54131.0849421296 | 701003010 | 197937.6 | 200000 | 197953.6 | 197937.6 | 0 | 197951.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 169652.6 | 169652.6 | 418397.8 | 4 | PROCESSED | 57537.0458912037 | 54777 | 54139.7293287037 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010028 | We propose a 200 ks continuous observation of the narrow-line Seyfert 1 galaxy IRAS13224-3809 in order to understand its remarkable and puzzling spectral and variability properties. Suzaku data will enable us to disentangle the two interpretations adopted so far, namely partial covering and relativistically blurred reflection. If the latter then the appearance of the source is controlled by general relativistic effects. In addition, the ability for Suzaku to conduct long continuous observations will allow us to monitor IRAS13224-3809 for giant amplitude flaring (as seen with ROSAT); therefore enabling us to enhance our understanding of AGN variability. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | TANAKA | YASUO | NULL | NULL | JAP | 1 | AO1 | THE REMARKABLE NARROW LINE SEYFERT 1 GALAXY IRAS13224-3809 | XIS | Y |
| SDSSJ084234.9+362503 | 130.6534 | 36.3531 | 186.36195466 | 37.19411123 | 266.2333 | 53868.6856018518 | 53871.41625 | 701004010 | 109955.6 | 120000 | 109971.6 | 109963.6 | 109955.6 | 109963.6 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 127230.6 | 127230.6 | 235894.8 | 1 | PROCESSED | 57534.3648032407 | 54400 | 53920.287650463 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010036 | Type 2 QSOs are one of the key class to understand the structure and evolution of AGN, origin of the Cosmic X-ray background, and the history of black hole growth. We propose to measure a hard X-ray spectrum of the most luminous and brightest type 2 QSO candidate in the Sloan Digital Sky Survey. The selection by optical narrow line spectra is not biased toward Compton-thin AGNs and enables us to investigate the true nature of type 2 QSOs. The data will be used to measure the absorption column density, intrinsic luminosity, and to constrain the structure of the absorber. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | TERASHIMA | YUICHI | NULL | NULL | JAP | 1 | AO1 | THE MOST LUMINOUS TYPE 2 QSO IN SDSS | HXD | N |
| NGC 4968 | 196.7464 | -23.7282 | 307.51234678 | 39.00523278 | 298.8345 | 53954.7307523148 | 53955.6822222222 | 701005010 | 39050.8 | 40000 | 39050.8 | 39050.8 | 39050.8 | 39050.8 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 35617 | 35617 | 82197.9 | 1 | PROCESSED | 57535.2527546296 | 54408 | 54020.7898148148 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010037 | We propose to measure broad band X-ray spectra of three Compton-thick Seyfert 2s selected based on large | EXTRAGALACTIC COMPACT SOURCES | 7 | B | TERASHIMA | YUICHI | NULL | NULL | JAP | 1 | AO1 | COMPTON-THICK AGN POPULATION IN THE LOCAL UNIVERSE: HARD X-RAY VIEW OF A COMPLETE | HXD | N |
| NGC 1667 | 72.1445 | -6.2644 | 203.99435404 | -30.10712566 | 81.9813 | 53964.3614814815 | 53965.2536805556 | 701006010 | 39253 | 40000 | 39253 | 39261 | 39261 | 39261 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 35728.1 | 35728.1 | 77075.9 | 0 | PROCESSED | 57535.2875578704 | 54526 | 54020.7803009259 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010037 | We propose to measure broad band X-ray spectra of three Compton-thick Seyfert 2s selected based on large | EXTRAGALACTIC COMPACT SOURCES | 7 | B | TERASHIMA | YUICHI | NULL | NULL | JAP | 1 | AO1 | COMPTON-THICK AGN POPULATION IN THE LOCAL UNIVERSE: HARD X-RAY VIEW OF A COMPLETE | HXD | N |
| MRK 1073 | 48.7401 | 42.0969 | 149.47083071 | -13.26071681 | 81.0781 | 53949.235162037 | 53949.3834722222 | 701007010 | 3474.6 | 40000 | 3474.6 | 3480.6 | 3478.6 | 3476.6 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 4135.8 | 4135.8 | 12806 | 0 | PROCESSED | 57535.0684375 | 54735 | 54132.9684490741 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010037 | We propose to measure broad band X-ray spectra of three Compton-thick Seyfert 2s selected based on large | EXTRAGALACTIC COMPACT SOURCES | 7 | B | TERASHIMA | YUICHI | NULL | NULL | JAP | 1 | AO1 | COMPTON-THICK AGN POPULATION IN THE LOCAL UNIVERSE: HARD X-RAY VIEW OF A COMPLETE | HXD | N |
| MRK 1073 | 48.7759 | 41.9723 | 149.56255257 | -13.3516285 | 258.3737 | 54135.7651851852 | 54136.6641087963 | 701007020 | 39511.1 | 40000 | 39519.1 | 39511.1 | 0 | 39519.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37181.4 | 37181.4 | 77651.9 | 0 | PROCESSED | 57537.3263657407 | 54735 | 54151.4969444445 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010037 | We propose to measure broad band X-ray spectra of three Compton-thick Seyfert 2s selected based on large | EXTRAGALACTIC COMPACT SOURCES | 7 | B | TERASHIMA | YUICHI | NULL | NULL | JAP | 1 | AO1 | COMPTON-THICK AGN POPULATION IN THE LOCAL UNIVERSE: HARD X-RAY VIEW OF A COMPLETE | HXD | Y |
| IRASF11223-1244 | 171.2239 | -12.9662 | 272.54538498 | 44.73919633 | 107.3062 | 54064.7275347222 | 54065.5709953704 | 701008010 | 40941.5 | 40000 | 41101.5 | 40941.5 | 0 | 41109.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 37680.4 | 37680.4 | 72863.9 | 1 | PROCESSED | 57536.1775925926 | 54735 | 54088.8556828704 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010038 | The source of huge energy output from ultraluminous infrared galaxies (ULIRGs) is still under debate. We propose to search for a hidden QSO as the energy source by observing ULIRGs with high luminosity optical emission lines classified as a Seyfert 2. The data will be used to constrain the power of the central AGN and to study the nature of infrared selected type 2 QSOs. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | TERASHIMA | YUICHI | NULL | NULL | JAP | 1 | AO1 | A SEARCH FOR HIDDEN QSO IN ULTRALUMINOUS INFRARED GALAXIES | HXD | Y |
| PKS 0558-504 | 89.9338 | -50.4417 | 257.95388656 | -28.57696937 | 207.8266 | 54117.4686226852 | 54118.1127777778 | 701011010 | 20620.7 | 20000 | 20620.7 | 20620.7 | 0 | 20620.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18914 | 18914 | 55647.9 | 0 | PROCESSED | 57536.8527777778 | 54735 | 54133.0355787037 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010057 | Narrow-line Seyfert 1 Galaxies (NLS1s) must have been crucial key to understand the rapid growth of the central supermassive black hole, which may be related to the evolution of the host galaxy. Hence, we propose 20x5 ksec observations of the luminous NLS1 galaxy PKS 0558-504, which is the candidate having the highest mass-accretion rate among the class. Large effective area and good energy resolution of XISs allow us to strictly constrain the temperature and the luminosity of the accretion flow. In addition, Suzaku HXD will detect the significant fraction of hard power law emission in the 10-60 keV band for the first time. From these observations, we expect to derive the new picture of the high mass-accretion mechanism in NLS1s. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | HABA | YOSHITO | NULL | NULL | JAP | 1 | AO1 | SUZAKU VIEW OF THE SUPER-CRITICAL ACCRETION FLOW IN NARROW-LINE SEYFERT 1 GALAXY PKS 0558-504 | XIS | Y |
| PKS 0558-504 | 89.9338 | -50.4409 | 257.95298672 | -28.57684464 | 209.1054 | 54118.6998032407 | 54119.2654976852 | 701011020 | 18875.3 | 20000 | 18875.3 | 18875.3 | 0 | 18875.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18049.7 | 18049.7 | 48870 | 1 | PROCESSED | 57536.8739814815 | 54735 | 54133.3967361111 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010057 | Narrow-line Seyfert 1 Galaxies (NLS1s) must have been crucial key to understand the rapid growth of the central supermassive black hole, which may be related to the evolution of the host galaxy. Hence, we propose 20x5 ksec observations of the luminous NLS1 galaxy PKS 0558-504, which is the candidate having the highest mass-accretion rate among the class. Large effective area and good energy resolution of XISs allow us to strictly constrain the temperature and the luminosity of the accretion flow. In addition, Suzaku HXD will detect the significant fraction of hard power law emission in the 10-60 keV band for the first time. From these observations, we expect to derive the new picture of the high mass-accretion mechanism in NLS1s. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | HABA | YOSHITO | NULL | NULL | JAP | 1 | AO1 | SUZAKU VIEW OF THE SUPER-CRITICAL ACCRETION FLOW IN NARROW-LINE SEYFERT 1 GALAXY PKS 0558-504 | XIS | Y |
| PKS 0558-504 | 89.9334 | -50.4402 | 257.95215413 | -28.57698713 | 210.2147 | 54119.7661805556 | 54120.3203009259 | 701011030 | 21256.3 | 20000 | 21256.3 | 21256.3 | 0 | 21256.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19114.5 | 19114.5 | 47870 | 0 | PROCESSED | 57536.8847916667 | 54735 | 54133.3934259259 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010057 | Narrow-line Seyfert 1 Galaxies (NLS1s) must have been crucial key to understand the rapid growth of the central supermassive black hole, which may be related to the evolution of the host galaxy. Hence, we propose 20x5 ksec observations of the luminous NLS1 galaxy PKS 0558-504, which is the candidate having the highest mass-accretion rate among the class. Large effective area and good energy resolution of XISs allow us to strictly constrain the temperature and the luminosity of the accretion flow. In addition, Suzaku HXD will detect the significant fraction of hard power law emission in the 10-60 keV band for the first time. From these observations, we expect to derive the new picture of the high mass-accretion mechanism in NLS1s. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | HABA | YOSHITO | NULL | NULL | JAP | 1 | AO1 | SUZAKU VIEW OF THE SUPER-CRITICAL ACCRETION FLOW IN NARROW-LINE SEYFERT 1 GALAXY PKS 0558-504 | XIS | Y |
| PKS 0558-504 | 89.9324 | -50.4401 | 257.95192858 | -28.57760064 | 211.3321 | 54120.8400925926 | 54121.3279976852 | 701011040 | 19738.1 | 20000 | 19754.1 | 19738.1 | 0 | 19754.1 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17175 | 17175 | 42135.9 | 0 | PROCESSED | 57536.8909953704 | 54735 | 54137.1036921296 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010057 | Narrow-line Seyfert 1 Galaxies (NLS1s) must have been crucial key to understand the rapid growth of the central supermassive black hole, which may be related to the evolution of the host galaxy. Hence, we propose 20x5 ksec observations of the luminous NLS1 galaxy PKS 0558-504, which is the candidate having the highest mass-accretion rate among the class. Large effective area and good energy resolution of XISs allow us to strictly constrain the temperature and the luminosity of the accretion flow. In addition, Suzaku HXD will detect the significant fraction of hard power law emission in the 10-60 keV band for the first time. From these observations, we expect to derive the new picture of the high mass-accretion mechanism in NLS1s. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | HABA | YOSHITO | NULL | NULL | JAP | 1 | AO1 | SUZAKU VIEW OF THE SUPER-CRITICAL ACCRETION FLOW IN NARROW-LINE SEYFERT 1 GALAXY PKS 0558-504 | XIS | Y |
| PKS 0558-504 | 89.9335 | -50.4395 | 257.95137808 | -28.57681508 | 212.4401 | 54121.9091203704 | 54122.3529976852 | 701011050 | 19515.4 | 20000 | 19531.4 | 19515.4 | 0 | 19531.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16123.6 | 16123.6 | 38312 | 0 | PROCESSED | 57536.8983217593 | 54735 | 54137.0453240741 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010057 | Narrow-line Seyfert 1 Galaxies (NLS1s) must have been crucial key to understand the rapid growth of the central supermassive black hole, which may be related to the evolution of the host galaxy. Hence, we propose 20x5 ksec observations of the luminous NLS1 galaxy PKS 0558-504, which is the candidate having the highest mass-accretion rate among the class. Large effective area and good energy resolution of XISs allow us to strictly constrain the temperature and the luminosity of the accretion flow. In addition, Suzaku HXD will detect the significant fraction of hard power law emission in the 10-60 keV band for the first time. From these observations, we expect to derive the new picture of the high mass-accretion mechanism in NLS1s. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | HABA | YOSHITO | NULL | NULL | JAP | 1 | AO1 | SUZAKU VIEW OF THE SUPER-CRITICAL ACCRETION FLOW IN NARROW-LINE SEYFERT 1 GALAXY PKS 0558-504 | XIS | Y |
| KAZ 102 | 270.6661 | 67.6374 | 97.62313354 | 29.55178422 | 2.066 | 53895.6833101852 | 53896.5343055556 | 701012010 | 41454 | 40000 | 41454 | 41462 | 41470 | 41470 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 40950.7 | 40950.7 | 73519.9 | 2 | PROCESSED | 57534.6269328704 | 54394 | 53928.2501157407 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010112 | We propose to make a detailed broad-band X-ray spectroscopic study of the radio quiet QSO (RQQ) Kaz 102. This RQQ had a power-law spectrum with a photon index ~ 1 with our ASCA observation. We also found a spectral variability over the time scale of years, from ~ 2.2 during the ROSAT All Sky Survey to ~ 1 during the Einstein / ASCA observations. From our ASCA spectra, we couldn't discriminate whether the apparently unusual hard spectrum was caused by warm absorber, Compton reflection, or a simple featureless power-law continuum. High quality and wide-band spectroscopy with Suzaku is essential to unveil the physical nature of the enigmatic hardness and spectral variability of Kaz 102. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | ISHISAKI | YOSHITAKA | NULL | NULL | JAP | 1 | AO1 | WHAT IS THE PHYSICAL NATURE OF KAZ 102: AN ENIGMATIC X-RAY HARD RADIO QUIET QSO? | HXD | N |
| SWIFT J0255.2-0011 | 43.8161 | -0.2397 | 175.95402612 | -49.91735431 | 256.3177 | 54123.6209490741 | 54126.2294560185 | 701013010 | 101632.1 | 100000 | 101632.1 | 101632.1 | 0 | 101632.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 86282.4 | 86282.4 | 225337.9 | 3 | PROCESSED | 57536.9811342593 | 54735 | 54137.3009027778 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010122 | The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to the latetest population synthesis model, its estimate is strongly coupled with the broad band spectral shape of type-2 AGNs, which is only poorly understood. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many new type-2 AGNs that can be best followed-up with Suzaku. Here we propose to observe two of them to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. This proposal is complementary to our separate proposal entitled "direct determination of the fraction of Compton-thick AGNs in the local universe". | EXTRAGALACTIC COMPACT SOURCES | 7 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 1 | AO1 | BROAD BAND SPECTRA OF NEW SWIFT/BAT AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND | HXD | Y |
| SWIFT J0505.7-2348 | 76.4285 | -23.9055 | 225.00444872 | -33.15769393 | 284.9903 | 53826.9254166667 | 53829.1216898148 | 701014010 | 78554.4 | 80000 | 78554.4 | 78554.4 | 78554.4 | 78554.4 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 53493.7 | 53493.7 | 189697.9 | 1 | PROCESSED | 57533.4023726852 | 54439 | 53945.2822569444 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010122 | The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to the latetest population synthesis model, its estimate is strongly coupled with the broad band spectral shape of type-2 AGNs, which is only poorly understood. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many new type-2 AGNs that can be best followed-up with Suzaku. Here we propose to observe two of them to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. This proposal is complementary to our separate proposal entitled "direct determination of the fraction of Compton-thick AGNs in the local universe". | EXTRAGALACTIC COMPACT SOURCES | 7 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 1 | AO1 | BROAD BAND SPECTRA OF NEW SWIFT/BAT AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND | HXD | N |
| SWIFT J0138.6-4001 | 24.6022 | -39.9757 | 268.75310615 | -73.8819888 | 44.7851 | 53890.7590740741 | 53891.2085532407 | 701015010 | 21197.9 | 20000 | 21213.9 | 21197.9 | 21213.9 | 21213.9 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 17477.1 | 17477.1 | 38831.9 | 1 | PROCESSED | 57534.4839814815 | 54394 | 53926.7722337963 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010133 | Swift/BAT extragalactic survey above E>15 keV has provided us with the first truely unbiased AGN sample in the local universe. The second BAT catalog contains about 80 sources, where a significant fraction is "new" AGNs without measurement of spectra below 15 keV. Here we propose to observe 6 new (non type-1) AGNs with Suzaku to make the BAT sample complete. Many are expected to be Compton-thick AGNs and hence the HXD data are crucial. This will lead us to the first direct measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. This proposal is complementary to our separate proposal tntitled "broad band spectra of new Swift/BAT AGNs and the origin of the X-ray background". | EXTRAGALACTIC COMPACT SOURCES | 7 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 1 | AO1 | DIRECT DETERMINATION OF THE FRACTION OF COMPTON THICK AGNS IN THE LOCAL UNIVERSE | HXD | N |
| SWIFT J1628.1+5145 | 246.9541 | 51.8388 | 79.81767806 | 42.92326404 | 60.2479 | 53840.7843518518 | 53841.3904976852 | 701016010 | 23589 | 20000 | 23605 | 23597 | 23589 | 23597 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 20626.1 | 20626.1 | 52359.9 | 2 | PROCESSED | 57533.4625231482 | 54394 | 53905.7494444444 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010133 | Swift/BAT extragalactic survey above E>15 keV has provided us with the first truely unbiased AGN sample in the local universe. The second BAT catalog contains about 80 sources, where a significant fraction is "new" AGNs without measurement of spectra below 15 keV. Here we propose to observe 6 new (non type-1) AGNs with Suzaku to make the BAT sample complete. Many are expected to be Compton-thick AGNs and hence the HXD data are crucial. This will lead us to the first direct measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. This proposal is complementary to our separate proposal tntitled "broad band spectra of new Swift/BAT AGNs and the origin of the X-ray background". | EXTRAGALACTIC COMPACT SOURCES | 7 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 1 | AO1 | DIRECT DETERMINATION OF THE FRACTION OF COMPTON THICK AGNS IN THE LOCAL UNIVERSE | HXD | N |
| SWIFT J0350.1-5019 | 57.5315 | -50.3337 | 259.74491819 | -49.02538792 | 320.5309 | 53838.5046875 | 53838.6752199074 | 701017010 | 2699.8 | 20000 | 2715.8 | 2715.8 | 2699.8 | 2707.8 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 1177.1 | 1177.1 | 9165 | 0 | PROCESSED | 57533.4464930556 | 54750 | 53905.4679398148 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010133 | Swift/BAT extragalactic survey above E>15 keV has provided us with the first truely unbiased AGN sample in the local universe. The second BAT catalog contains about 80 sources, where a significant fraction is "new" AGNs without measurement of spectra below 15 keV. Here we propose to observe 6 new (non type-1) AGNs with Suzaku to make the BAT sample complete. Many are expected to be Compton-thick AGNs and hence the HXD data are crucial. This will lead us to the first direct measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. This proposal is complementary to our separate proposal tntitled "broad band spectra of new Swift/BAT AGNs and the origin of the X-ray background". | EXTRAGALACTIC COMPACT SOURCES | 7 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 1 | AO1 | DIRECT DETERMINATION OF THE FRACTION OF COMPTON THICK AGNS IN THE LOCAL UNIVERSE | HXD | N |
| SWIFT J0350.1-5019 | 57.6662 | -50.2998 | 259.65657878 | -48.95336771 | 180.7044 | 54062.0888078704 | 54062.5647453704 | 701017020 | 19271 | 23000 | 19271 | 19271 | 0 | 19271 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16740 | 16740 | 41097 | 0 | PROCESSED | 57536.1549768518 | 54750 | 54088.5939583333 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010133 | Swift/BAT extragalactic survey above E>15 keV has provided us with the first truely unbiased AGN sample in the local universe. The second BAT catalog contains about 80 sources, where a significant fraction is "new" AGNs without measurement of spectra below 15 keV. Here we propose to observe 6 new (non type-1) AGNs with Suzaku to make the BAT sample complete. Many are expected to be Compton-thick AGNs and hence the HXD data are crucial. This will lead us to the first direct measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. This proposal is complementary to our separate proposal tntitled "broad band spectra of new Swift/BAT AGNs and the origin of the X-ray background". | EXTRAGALACTIC COMPACT SOURCES | 7 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 1 | AO1 | DIRECT DETERMINATION OF THE FRACTION OF COMPTON THICK AGNS IN THE LOCAL UNIVERSE | HXD | Y |
| SWIFT J0350.1-5019 | 57.5863 | -50.3518 | 259.75531799 | -48.98660415 | 277.9348 | 54162.2927777778 | 54162.5036921296 | 701017030 | 8148.7 | 10000 | 8156.7 | 8148.7 | 0 | 8156.7 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7059.7 | 7059.7 | 18215.9 | 0 | PROCESSED | 57537.5866898148 | 54750 | 54167.6235763889 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010133 | Swift/BAT extragalactic survey above E>15 keV has provided us with the first truely unbiased AGN sample in the local universe. The second BAT catalog contains about 80 sources, where a significant fraction is "new" AGNs without measurement of spectra below 15 keV. Here we propose to observe 6 new (non type-1) AGNs with Suzaku to make the BAT sample complete. Many are expected to be Compton-thick AGNs and hence the HXD data are crucial. This will lead us to the first direct measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. This proposal is complementary to our separate proposal tntitled "broad band spectra of new Swift/BAT AGNs and the origin of the X-ray background". | EXTRAGALACTIC COMPACT SOURCES | 7 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 1 | AO1 | DIRECT DETERMINATION OF THE FRACTION OF COMPTON THICK AGNS IN THE LOCAL UNIVERSE | HXD | Y |
| SWIFT J0601.9-8636 | 91.1523 | -86.6779 | 299.2555588 | -27.75439578 | 292.1727 | 53838.6834259259 | 53839.0779976852 | 701018010 | 19765.7 | 20000 | 19781.7 | 19781.7 | 19765.7 | 19773.7 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 16661.4 | 16661.4 | 34059.9 | 0 | PROCESSED | 57533.4511226852 | 54397 | 53905.4682060185 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010133 | Swift/BAT extragalactic survey above E>15 keV has provided us with the first truely unbiased AGN sample in the local universe. The second BAT catalog contains about 80 sources, where a significant fraction is "new" AGNs without measurement of spectra below 15 keV. Here we propose to observe 6 new (non type-1) AGNs with Suzaku to make the BAT sample complete. Many are expected to be Compton-thick AGNs and hence the HXD data are crucial. This will lead us to the first direct measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. This proposal is complementary to our separate proposal tntitled "broad band spectra of new Swift/BAT AGNs and the origin of the X-ray background". | EXTRAGALACTIC COMPACT SOURCES | 7 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 1 | AO1 | DIRECT DETERMINATION OF THE FRACTION OF COMPTON THICK AGNS IN THE LOCAL UNIVERSE | HXD | N |
| TON S180 | 14.333 | -22.3803 | 138.98529016 | -85.06726133 | 237.1425 | 54078.5680671296 | 54081.3584953704 | 701021010 | 120660.9 | 120000 | 120684.9 | 120660.9 | 0 | 120676.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 109312.8 | 109312.8 | 241052 | 3 | PROCESSED | 57536.3458680556 | 54735 | 54094.4773958333 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010141 | TON S180 is a luminous Narrow Line Seyfert 1 galaxy, chracterizing enhanced Soft X-ray emission component without complex absorption/emission structures. The source is considered to be at super Eddington accretion rate. We aim to track change (or no change) in soft X-ray spectrum of this source according to factor of two ,rapid flux variation this source show. We partciularly focus on the slim disk model propsed for super Eddington accretion disk. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | HAYASHIDA | KIYOSHI | NULL | NULL | JAP | 1 | AO1 | SOFT X-RAY EMISSION FROM SUPER-EDDINGTON ACCRETION DISK IN TON S180 | XIS | Y |
| M81 | 148.8559 | 68.9951 | 142.17660014 | 40.93097712 | 281.1688 | 53863.0052083333 | 53864.5209953704 | 701022010 | 103518.6 | 100000 | 103526.6 | 103526.6 | 103526.6 | 103518.6 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 70736.9 | 70736.9 | 130942.1 | 0 | PROCESSED | 57534.2973726852 | 54397 | 53913.9816550926 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010151 | We propose observations of the nearby Low Luminosity AGN, M81 and M106, for 100 ks for each target. We aim to detect both targets up to ~200 keV for the first time. We will determine the photon indices of the hard X-ray power-law continuum, with searching for other possible characteristics such as Compton hump around 10-20 keV and cutoff around 100-200 keV which would lead major discoveries. We will study the shape of Fe-K line(s) around 6-7 keV and their time variances. Our goal is to compare their hard X-ray spectra with those of SWG seyfert galaxies, with unprecedented accuracy, to study the accresion mechanism of LLAGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ITOH | TAKESHI | NULL | NULL | JAP | 1 | AO1 | OBSERVATIONS OF HARD X-RAYS FROM LOW LUMINOSITY ACTIVE GALACTIC NUCLEI | HXD | N |
| MRK421 | 166.0521 | 38.1644 | 179.96763761 | 64.99940635 | 318.3733 | 53853.2821412037 | 53854.2711226852 | 701024010 | 41470.9 | 40000 | 41478.9 | 41470.9 | 41478.9 | 41478.9 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 34703.3 | 34703.3 | 85430.1 | 1 | PROCESSED | 57533.6140162037 | 54394 | 53908.0343055556 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010157 | We propose to conduct a series of simultaneous X-ray/VHE (very high energy) gamma-ray observations of northern TeV Blazars (Mkn 421, Mkn 501, 1ES1218+304, and 1ES1426+428) with Suzaku XIS and HXD in conjunction with the HESS (High Energy Stereoscopic System) and MAGIC ground based gamma-ray observatories. The goal of these observations is to study the spectral energy distribution of these highly variable objects for the first time simultaneously in the soft to hard X-ray (0.3 keV-100 keV) | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TAKAHASHI | TADAYUKI | NULL | NULL | JAP | 1 | AO1 | SIMULTANEOUS X-RAY/VHE GAMMA-RAY OBSERVATIONS OF NORTHERN BLAZARS WITH SUZAKU AND HESS/MAGIC | HXD | N |
| 1ES1218+304 | 185.3064 | 30.1169 | 186.88913956 | 82.72978014 | 298.9428 | 53874.8006365741 | 53876.706412037 | 701025010 | 79869.2 | 80000 | 79885.2 | 79869.2 | 79885.2 | 79877.2 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 70511.8 | 70511.8 | 164637.9 | 2 | PROCESSED | 57534.4292013889 | 54398 | 53927.8564930556 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010157 | We propose to conduct a series of simultaneous X-ray/VHE (very high energy) gamma-ray observations of northern TeV Blazars (Mkn 421, Mkn 501, 1ES1218+304, and 1ES1426+428) with Suzaku XIS and HXD in conjunction with the HESS (High Energy Stereoscopic System) and MAGIC ground based gamma-ray observatories. The goal of these observations is to study the spectral energy distribution of these highly variable objects for the first time simultaneously in the soft to hard X-ray (0.3 keV-100 keV) | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TAKAHASHI | TADAYUKI | NULL | NULL | JAP | 1 | AO1 | SIMULTANEOUS X-RAY/VHE GAMMA-RAY OBSERVATIONS OF NORTHERN BLAZARS WITH SUZAKU AND HESS/MAGIC | HXD | N |
| 1ES1426+428 | 217.0716 | 42.6249 | 77.44668506 | 64.96380656 | 316.1862 | 53902.7388310185 | 53904.2225 | 701026010 | 60914.9 | 60000 | 60914.9 | 60914.9 | 60914.9 | 60914.9 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 54091.1 | 54091.1 | 128160 | 1 | PROCESSED | 57534.6747800926 | 54400 | 53928.3009143518 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010157 | We propose to conduct a series of simultaneous X-ray/VHE (very high energy) gamma-ray observations of northern TeV Blazars (Mkn 421, Mkn 501, 1ES1218+304, and 1ES1426+428) with Suzaku XIS and HXD in conjunction with the HESS (High Energy Stereoscopic System) and MAGIC ground based gamma-ray observatories. The goal of these observations is to study the spectral energy distribution of these highly variable objects for the first time simultaneously in the soft to hard X-ray (0.3 keV-100 keV) | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TAKAHASHI | TADAYUKI | NULL | NULL | JAP | 1 | AO1 | SIMULTANEOUS X-RAY/VHE GAMMA-RAY OBSERVATIONS OF NORTHERN BLAZARS WITH SUZAKU AND HESS/MAGIC | HXD | N |
| MRK 501 | 253.4 | 39.7089 | 63.52834502 | 38.90621529 | 316.9908 | 53934.7872569444 | 53935.7272916667 | 701027010 | 42427.1 | 40000 | 42438.9 | 42438.9 | 42427.1 | 42435.1 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 39971.1 | 39971.1 | 81209.9 | 0 | PROCESSED | 57534.9978587963 | 54408 | 53971.6784259259 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010157 | We propose to conduct a series of simultaneous X-ray/VHE (very high energy) gamma-ray observations of northern TeV Blazars (Mkn 421, Mkn 501, 1ES1218+304, and 1ES1426+428) with Suzaku XIS and HXD in conjunction with the HESS (High Energy Stereoscopic System) and MAGIC ground based gamma-ray observatories. The goal of these observations is to study the spectral energy distribution of these highly variable objects for the first time simultaneously in the soft to hard X-ray (0.3 keV-100 keV) | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TAKAHASHI | TADAYUKI | NULL | NULL | JAP | 1 | AO1 | SIMULTANEOUS X-RAY/VHE GAMMA-RAY OBSERVATIONS OF NORTHERN BLAZARS WITH SUZAKU AND HESS/MAGIC | HXD | N |
| BO 375 | 11.4476 | 41.6573 | 121.80050832 | -21.20204189 | 232.9596 | 54135.3691666667 | 54135.7592476852 | 701028010 | 12779.8 | 13000 | 12779.8 | 12779.8 | 0 | 12779.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12838.6 | 12838.6 | 33664 | 1 | PROCESSED | 57536.9599189815 | 54695 | 54151.4930324074 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011120 | There are over 400 very luminous (Lx > 1e38-1e40 erg/s) globular cluster X-ray sources in nearby galaxies. None are present in our Galaxy, and their nature is unknown. They may be accreting black holes, however, this is quite controversial and it is contrary to theoretical expectations. The distance is too large to make accurate studies of any of them that could reveal their nature. Luckily, there is one such very luminous source, Bo 375, in a globular cluster in M31. We propose to perform ten 10 ksec Suzaku observations of Bo 375. We expect that from the long-term lightcurve, broad-band energy spectra, and power spectra, we will be able to determine the nature of this object and thereby possibly the nature of the many very luminous globular cluster X-ray sources in nearby galaxies. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | KONG | ALBERT | NULL | NULL | USA | 1 | AO1 | PROBING THE NATURE OF A VERY LUMINOUS GLOBULAR CLUSTER X-RAY SOURCE IN M31 | XIS | Y |
| BO 375 | 11.4497 | 41.6556 | 121.80214792 | -21.2037783 | 231.6187 | 54137.6100810185 | 54137.9737731482 | 701028020 | 15537.1 | 13000 | 15537.1 | 15537.1 | 0 | 15537.1 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 14942 | 14942 | 31415.9 | 0 | PROCESSED | 57537.3176967593 | 54695 | 54151.4987731482 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011120 | There are over 400 very luminous (Lx > 1e38-1e40 erg/s) globular cluster X-ray sources in nearby galaxies. None are present in our Galaxy, and their nature is unknown. They may be accreting black holes, however, this is quite controversial and it is contrary to theoretical expectations. The distance is too large to make accurate studies of any of them that could reveal their nature. Luckily, there is one such very luminous source, Bo 375, in a globular cluster in M31. We propose to perform ten 10 ksec Suzaku observations of Bo 375. We expect that from the long-term lightcurve, broad-band energy spectra, and power spectra, we will be able to determine the nature of this object and thereby possibly the nature of the many very luminous globular cluster X-ray sources in nearby galaxies. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | KONG | ALBERT | NULL | NULL | USA | 1 | AO1 | PROBING THE NATURE OF A VERY LUMINOUS GLOBULAR CLUSTER X-RAY SOURCE IN M31 | XIS | Y |
| BO 375 | 11.4497 | 41.6556 | 121.80214792 | -21.2037783 | 231.4176 | 54142.8248032407 | 54143.2167824074 | 701028030 | 15087.8 | 13000 | 15087.8 | 15087.8 | 0 | 15087.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15716.4 | 15716.4 | 33837.9 | 1 | PROCESSED | 57537.3535069444 | 54695 | 54153.1806828704 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011120 | There are over 400 very luminous (Lx > 1e38-1e40 erg/s) globular cluster X-ray sources in nearby galaxies. None are present in our Galaxy, and their nature is unknown. They may be accreting black holes, however, this is quite controversial and it is contrary to theoretical expectations. The distance is too large to make accurate studies of any of them that could reveal their nature. Luckily, there is one such very luminous source, Bo 375, in a globular cluster in M31. We propose to perform ten 10 ksec Suzaku observations of Bo 375. We expect that from the long-term lightcurve, broad-band energy spectra, and power spectra, we will be able to determine the nature of this object and thereby possibly the nature of the many very luminous globular cluster X-ray sources in nearby galaxies. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | KONG | ALBERT | NULL | NULL | USA | 1 | AO1 | PROBING THE NATURE OF A VERY LUMINOUS GLOBULAR CLUSTER X-RAY SOURCE IN M31 | XIS | Y |
| NGC 7213 | 332.316 | -47.1629 | 349.59497628 | -52.58020545 | 231.3714 | 54030.2323611111 | 54032.2759722222 | 701029010 | 90736 | 100000 | 90760 | 90744 | 90736 | 90752 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 90341.8 | 90341.8 | 176535.8 | 0 | PROCESSED | 57535.9564814815 | 54695 | 54056.3665162037 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011305 | We propose a 100ks Suzaku observation of the low luminosity AGN, NGC 7213. Previous observations show a complex iron line and weak or no Compton reflection. However the iron line and reflection hump are poorly constrained, so the line emitting matter could arise from a truncated disk, BLR or a Compton-thin torus. A high quality Suzaku observation will constrain the iron line profile, resolve the ionized emission and unambiguously determine its origin. Using the unique broad bandpass of Suzaku above 10 keV we will place tight constraints on any reflection hump, enabling us to determine if the iron line originates from a truncated disk. This could provide a direct test of the paradigm that the X-ray emission in low accretion rate AGN occurs in a truncated disk system such as an ADAF. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | REEVES | JAMES | NULL | NULL | USA | 1 | AO1 | DOES THE LOW LUMINOSITY AGN NGC7213 CONTAIN A TRUNCATED ACCRETION DISK? | XIS | Y |
| NGC 5506 | 213.312 | -3.2124 | 339.14600253 | 53.80603682 | 287.3743 | 53955.6875578704 | 53957.003900463 | 701030010 | 47753.1 | 150000 | 47753.1 | 47753.1 | 47753.1 | 47753.1 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 41097.3 | 41097.3 | 113725.9 | 2 | PROCESSED | 57535.2578587963 | 54695 | 54116.2715740741 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011312 | NGC 5506 is one of the brightest Seyferts in the X-ray sky, the second brightest in the PIN bandpass. Obscuring gas has kept the true nature of this AGN secret until recent optical and infrared studies have unmasked the narrow-line-seyfert 1 nucleus. With this knowledge, NGC 5506 is the perfect candidate for confirming the generality of a new result based on a recent XMM observation of Mkn 766, ie that the ionized component of Fe K emission originates from the inner accretion disk and closely tracks the hard X-ray continuum flux. This immediately gives us the ionization-state and size-scale of the inner disk. We request a 150 ks Suzaku observation to see whether a similar result holds for NGC 5506 and, by extension, may be a property of NLS1s. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TURNER | TRACEY | NULL | NULL | USA | 1 | AO1 | SUZAKU STUDY OF THE BRIGHTEST NARROW LINE SEYFERT 1: NGC 5506 | XIS | N |
| NGC 5506 | 213.3121 | -3.2119 | 339.14659218 | 53.80640928 | 287.3747 | 53958.1015972222 | 53959.4488425926 | 701030020 | 53296.2 | 63000 | 53304.2 | 53296.2 | 53304.2 | 53304.2 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 47983.2 | 47983.2 | 116386 | 1 | PROCESSED | 57535.2817476852 | 54695 | 54116.3307291667 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011312 | NGC 5506 is one of the brightest Seyferts in the X-ray sky, the second brightest in the PIN bandpass. Obscuring gas has kept the true nature of this AGN secret until recent optical and infrared studies have unmasked the narrow-line-seyfert 1 nucleus. With this knowledge, NGC 5506 is the perfect candidate for confirming the generality of a new result based on a recent XMM observation of Mkn 766, ie that the ionized component of Fe K emission originates from the inner accretion disk and closely tracks the hard X-ray continuum flux. This immediately gives us the ionization-state and size-scale of the inner disk. We request a 150 ks Suzaku observation to see whether a similar result holds for NGC 5506 and, by extension, may be a property of NLS1s. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TURNER | TRACEY | NULL | NULL | USA | 1 | AO1 | SUZAKU STUDY OF THE BRIGHTEST NARROW LINE SEYFERT 1: NGC 5506 | XIS | N |
| NGC 5506 | 213.3095 | -3.2029 | 339.1508826 | 53.81542712 | 91.2728 | 54131.0918055556 | 54132.6279513889 | 701030030 | 57406.3 | 150000 | 57414.3 | 57406.3 | 0 | 57414.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47702.7 | 47702.7 | 132685.8 | 0 | PROCESSED | 57536.9491666667 | 54695 | 54139.3642361111 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011312 | NGC 5506 is one of the brightest Seyferts in the X-ray sky, the second brightest in the PIN bandpass. Obscuring gas has kept the true nature of this AGN secret until recent optical and infrared studies have unmasked the narrow-line-seyfert 1 nucleus. With this knowledge, NGC 5506 is the perfect candidate for confirming the generality of a new result based on a recent XMM observation of Mkn 766, ie that the ionized component of Fe K emission originates from the inner accretion disk and closely tracks the hard X-ray continuum flux. This immediately gives us the ionization-state and size-scale of the inner disk. We request a 150 ks Suzaku observation to see whether a similar result holds for NGC 5506 and, by extension, may be a property of NLS1s. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TURNER | TRACEY | NULL | NULL | USA | 1 | AO1 | SUZAKU STUDY OF THE BRIGHTEST NARROW LINE SEYFERT 1: NGC 5506 | XIS | Y |
| MARKARIAN 335 | 1.5539 | 20.2624 | 108.74842011 | -41.36053721 | 68.4831 | 53907.0624537037 | 53910.7585532407 | 701031010 | 151288.4 | 150000 | 151296.4 | 151288.4 | 151296.4 | 151296.4 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 140981.2 | 140981.2 | 319302.8 | 4 | PROCESSED | 57534.8340046296 | 54401 | 53928.5392361111 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011323 | We propose to observe the two Seyfert 1 galaxies Mrk 335 and ESO198-G024 for a total exposure of 150 ks each with the high sensitivity and broad band coverage of the Suzaku satellite. Both sources show a broad Fe K line and a strong soft excess. One appealing explanation for the nature of the soft excess is reflection. Fundamental to this hypothesis is the assumption that the same self-consistent reflection spectrum explains the Fe K line (including its shape), the soft excess, and also the Compton reflection hump above 20 keV. Suzaku's ability to measure all three reflection components simultaneously enables the different spectral models to be disentangled and reflection to be strongly tested. Understanding black hole accretion is fundamental to NASA's "SEU" theme. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | MILLER | JON | NULL | NULL | USA | 1 | AO1 | REVEALING THE NATURE OF THE SOFT EXCESS IN AGNS WITH SUZAKU | HXD | N |
| NGC 3783 | 174.7611 | -37.7364 | 287.45850943 | 22.95048745 | 293.6402 | 53910.7726388889 | 53912.8571412037 | 701033010 | 75719.3 | 75000 | 75719.3 | 75719.3 | 75719.3 | 75719.3 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 68299.3 | 68299.3 | 180023.7 | 0 | PROCESSED | 57534.7899652778 | 54401 | 53926.8847453704 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011325 | We propose a 75 ksec Suzaku observation of the bright Seyfert 1 NGC 3783. Absorption due to photo-ionized material in the line of sight is well-established in this source, but can lead to degeneracy during modeling: is 3-6 keV continuum curvature due to photo-ionized absorption or a relativistically broad Fe K component? The simultaneous broadband XIS/HXD coverage is needed to define the continuum emission over a wide bandpass and disentangle the various emitting and absorbing components. We can then study the ionized absorber components, establish whether or not broad Fe K emission exists, and constrain reflection components, including the Compton shoulder. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | MARKOWITZ | ALEX | NULL | NULL | USA | 1 | AO1 | PROBING FE K EMISSION AND IONIZED ABSORPTION IN NGC 3783 | XIS | N |
| NGC 4151 | 182.6375 | 39.4139 | 155.05374688 | 75.05753801 | 112.1087 | 54087.8369097222 | 54090.3848726852 | 701034010 | 124979.6 | 125000 | 124979.6 | 124979.6 | 0 | 124979.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 131274.1 | 131274.1 | 220105.9 | 3 | PROCESSED | 57536.4582060185 | 54702 | 54132.849537037 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011327 | We propose a 100 ks Suzaku observation of the brightest Seyfert Galaxy in the sky. Given the broad band-pass, and high sensitivity, the proposed observations will provide a high-quality spectrum which will allow us to search for variability in the high-ionized absorber (compared to previous observations). We will be able to obtain stringent constraints on the "Reflection Hump" and compare it to the strength of the Fe Kalpha emission line - thus providing a direct test of Reflection models. The proposed program will also complement observations of fainter and more exotic Seyferts likely to be observed during AO-1. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GEORGE | IAN | NULL | NULL | USA | 1 | AO1 | DECOUPLING THE COMPONENTS IN THE BRIGHTEST SEYFERT: NGC 4151 | XIS | Y |
| MRK 766 | 184.6154 | 29.8184 | 190.63186084 | 82.27243688 | 133.2599 | 54055.0242361111 | 54057.363900463 | 701035010 | 97869.3 | 150000 | 98175.6 | 97869.3 | 0 | 98167.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 96893.1 | 96893.1 | 202129.9 | 2 | PROCESSED | 57536.189525463 | 54800 | 54132.8396990741 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011328 | X-ray spectroscopy of Mkn 766 has revealed ionised Fe emission that varies with the continuum on 10 ks timescales: direct evidence for ionised reflection from the accretion disk. This bright NLSy1 also shows extreme spectral variability, with the low state being dominated by a hard, constant reflection component, probably from cool distant material. We propose to measure the spectrum above 10 keV; the hot component should vary with the continuum, the cold distant component should be constant, and we can measure their relative contributions to test the predictions of the lower-energy analysis. This source is complex and needs the high-energy spectrum from Suzaku: it seems likely that previous complex behavior of several Seyferts can be described by these components | EXTRAGALACTIC COMPACT SOURCES | 7 | B | TURNER | TRACEY | NULL | NULL | USA | 1 | AO1 | DECOMPOSITION OF SEYFERT SPECTRA: TRACKING THE INNER DISK IN MKN 766 | XIS | N |
| MRK 766 | 184.6147 | 29.8197 | 190.62410896 | 82.27145087 | 134.9989 | 54421.893287037 | 54423.2363310185 | 701035020 | 59363.5 | 50000 | 59363.5 | 59363.5 | 0 | 59363.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 51151.7 | 51151.7 | 116023.8 | 1 | PROCESSED | 57540.5762384259 | 54800 | 54433.2716666667 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011328 | X-ray spectroscopy of Mkn 766 has revealed ionised Fe emission that varies with the continuum on 10 ks timescales: direct evidence for ionised reflection from the accretion disk. This bright NLSy1 also shows extreme spectral variability, with the low state being dominated by a hard, constant reflection component, probably from cool distant material. We propose to measure the spectrum above 10 keV; the hot component should vary with the continuum, the cold distant component should be constant, and we can measure their relative contributions to test the predictions of the lower-energy analysis. This source is complex and needs the high-energy spectrum from Suzaku: it seems likely that previous complex behavior of several Seyferts can be described by these components | EXTRAGALACTIC COMPACT SOURCES | 7 | B | TURNER | TRACEY | NULL | NULL | USA | 1 | AO1 | DECOMPOSITION OF SEYFERT SPECTRA: TRACKING THE INNER DISK IN MKN 766 | XIS | Y |
| CIRCINUS GALAXY | 213.2971 | -65.3336 | 311.32997737 | -3.80345965 | 276.4798 | 53937.5207986111 | 53939.0475 | 701036010 | 108021.7 | 100000 | 108045.7 | 108021.7 | 108045.7 | 108029.7 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 94272 | 94272 | 131887.9 | 1 | PROCESSED | 57535.0550578704 | 54401 | 53943.5986574074 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011331 | The light of AGN dominates the hard cosmic X-ray background. However, the contribution of Compton thick objects is poorly constrained because they emit chiefly above the energy range where Chandra and XMM are sensitive. Here we propose to observe the Circinus galaxy, one of the two brightest AGN reflection sources below 10 keV and with a known high column density. Our observations below 10 keV will provide CCD spectra of the rich emission line and continuum spectra, allowing limited photoionization modelling and searches for variability, possibly seen in Circinus. In the range 10 - 60 keV, we shall obtain a spectrum of the directly viewed continuum with unprecedented S/N in the key band for the HCXB. Above 60 keV, we will detect Circinus and check whether the spectrum has a rollover. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | WILSON | ANDREW | NULL | NULL | USA | 1 | AO1 | THE HARD X-RAY BACKGROUND, COMPTON-THICK AGN AND WATER VAPOR MEGAMASERS | XIS | N |
| NGC 4552 | 188.9456 | 12.612 | 287.9907408 | 75.02773792 | 120.0696 | 54072.312974537 | 54072.8405092593 | 701037010 | 20439.8 | 20000 | 20439.8 | 20439.8 | 0 | 20439.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16553 | 16553 | 45543.9 | 0 | PROCESSED | 57536.226875 | 54455 | 54088.5410069444 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011333 | The majority of accretion onto supermassive black holes in the local Universe occurs in obscured Seyferts. At moderate redshifts, the optical narrow emission-lines used to identify Seyfert 2s become difficult to isolate from the host galaxy's emission, resulting in an underestimate of the numbers of Seyfert 2s. Seyfert 2s are a critical component of AGN synthesis models of the Cosmic X-ray Background (CXB), as these sources are likely responsible for the unresolved component of the 2-8 keV background and may also contribute significantly to the 30 keV background. We propose to use Suzaku observations of ten local Seyfert 2s to measure their ultrahard (>10 keV) emission and examine how Seyfert 2s at moderate redshifts contribute to the CXB. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | STEFFEN | AARON | NULL | NULL | USA | 1 | AO1 | MEASURING THE ULTRAHARD X-RAY EMISSION OF A LOCAL POPULATION OF SEYFERT 2S | HXD | N |
| NGC 1068 | 40.6928 | -0.0667 | 172.18986515 | -51.95763403 | 248.588 | 54141.0038078704 | 54141.9168287037 | 701039010 | 41622.9 | 35000 | 41630.9 | 41630.9 | 0 | 41622.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41802.4 | 41802.4 | 78883.9 | 0 | PROCESSED | 57537.346875 | 54525 | 54151.5012962963 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011333 | The majority of accretion onto supermassive black holes in the local Universe occurs in obscured Seyferts. At moderate redshifts, the optical narrow emission-lines used to identify Seyfert 2s become difficult to isolate from the host galaxy's emission, resulting in an underestimate of the numbers of Seyfert 2s. Seyfert 2s are a critical component of AGN synthesis models of the Cosmic X-ray Background (CXB), as these sources are likely responsible for the unresolved component of the 2-8 keV background and may also contribute significantly to the 30 keV background. We propose to use Suzaku observations of ten local Seyfert 2s to measure their ultrahard (>10 keV) emission and examine how Seyfert 2s at moderate redshifts contribute to the CXB. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | STEFFEN | AARON | NULL | NULL | USA | 1 | AO1 | MEASURING THE ULTRAHARD X-RAY EMISSION OF A LOCAL POPULATION OF SEYFERT 2S | HXD | N |
| MRK 1 | 19.06 | 33.0289 | 128.90716196 | -29.55492804 | 249.7486 | 54111.5318171296 | 54114.5836111111 | 701047010 | 126444.1 | 120000 | 126444.1 | 126444.1 | 0 | 126444.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 126012.2 | 126012.2 | 263623.7 | 2 | PROCESSED | 57637.5831944445 | 54702 | 54133.1552314815 | 3.0.22.44 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011336 | The supermassive black holes of active galactic nuclei (AGN) are fundamentally connected to the stars of their host galaxies, but it is not clear whether this relationship is evident at X-ray energies. We will test the prediction that prolific star formation is responsible for the soft X-ray emission from a Compton thick AGN that also contains a powerful circumnuclear starburst. The AGN's deep obscuration facilitates the soft X-ray measurements, and Compton thick AGN are generally significant, both as a large fraction of the local AGN population and for their contribution to the X-ray background. Furthermore, we will use the direct measurement of the intrinsic AGN luminosity to test unified AGN models and the validity of indirect luminosity indicators. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | LEVENSON | NANCY | NULL | NULL | USA | 1 | AO1 | TESTING THE STARBURST-AGN CONNECTION AND MEASURING DEEPLY OBSCURED AGN | HXD | Y |
| MRK 273 | 206.1319 | 55.8192 | 108.09580624 | 59.75355315 | 290.8776 | 53923.3108333333 | 53925.3356481482 | 701050010 | 79904.6 | 80000 | 79912.6 | 79904.6 | 79920.6 | 79920.6 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 82807.6 | 82807.6 | 174905.9 | 3 | PROCESSED | 57534.931400463 | 54401 | 53930.7076851852 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011341 | We wish to take advantage of the unprecedented sensitivity of Suzaku Observatory to very hard X-rays (> 10 keV) to constrain the energy source -- starburst or black-hole driven activity -- in two of the nearest and brightest ultraluminous infrared galaxies, Mrk 273 and F05189-2524. These objects are arguably the best local laboratories to study the basic physical processes involved in creating massive early type hosts on the one hand, and feeding embedded supermassive black holes on the other hand, in major galaxy mergers. The Suzaku data will be used to search for the high-energy signature of deeply buried active black holes and to look for short timescale variability, another signature of black-hole driven activity. These data will be part of S. Teng's PhD thesis at Maryland. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | VEILLEUX | SYLVAIN | NULL | NULL | USA | 1 | AO1 | THE DOMINANT ENERGY SOURCE OF ULTRALUMINOUS INFRARED GALAXIES | HXD | N |
| IRAS 19254-7245 | 292.8508 | -72.6492 | 322.5078751 | -28.76929596 | 279.8892 | 54041.9830208333 | 54044.5967476852 | 701052010 | 113512.3 | 120000 | 113520.3 | 113520.3 | 113512.3 | 113520.3 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 151977.8 | 151977.8 | 225809.9 | 1 | PROCESSED | 57536.068125 | 54455 | 54088.8285185185 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011342 | We propose a 120 ksec Suzaku exposure of the ULIRG IRAS19254-7245. A previous XMM-Newton observation revealed the presence of a strong iron emission line and a flat continuum, both suggesting that this source hosts a Compton-thick AGN. In this scenario, the 2-10 keV luminosity of IRAS19254-7245 could be greater than 10e44 erg/s. However since no direct continuum is visible in the XMM bandpass, a direct measure of the absorbing column density was not feasible, thus the intrinsic X-ray luminosity of this source was derived only through indirect arguments. The unique bandpass and sensititvity of Suzaku above 10 keV will allow us to confirm the Compton-thick nature of this source and to measure for the first time the intrinsic X-ray luminosity of the AGN hosted in IRAS 19254-7245. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | BRAITO | VALENTINA | NULL | NULL | USA | 1 | AO1 | ASSESSING THE ENERGETIC BUDGET IN THE SUPERANTENNAE | XIS | N |
| IRAS08572+3915 | 135.0664 | 39.0091 | 183.47368885 | 40.96543811 | 300.022 | 53839.0903240741 | 53840.7752199074 | 701053010 | 77197.4 | 75000 | 77221.4 | 77197.4 | 77213.4 | 77221.4 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 62333.9 | 62333.9 | 145499.9 | 9 | PROCESSED | 57533.486875 | 54401 | 53906.2114699074 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011344 | Ultraluminous infrared galaxies (ULIRGs) produce the energy outputs of quasars with nearly all the power emerging in the far-IR via reprocessing of optical, UV, and X-ray radiation by dust. The ultimate nuclear power source, be it AGN or compact starburst, of ULIRGs has been the focus of much debate since their discovery with the IRAS mission. While observations with Spitzer are unlocking the secrets of many nearby ULIRGs, some have nuclei that are apparently so obscured as to be optically thick even in the mid-IR. We have chosen three local ULIRGs, IRAS 08572+3915, IRAS15250+3609, and IRAS20551-4250 that are IR-bright, yet highly obscured for deep Suzaku observations to search for the tell-tale signs of a buried AGN: hard X-ray emission behind significant column densities of HI gas. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GALLAGHER | SARAH | NULL | NULL | USA | 1 | AO1 | ULTRAHARD X-RAY CASE STUDIES OF ULIRGS WITH DEEP SILICATE ABSORPTION | HXD | N |
| PDS 456 | 262.0807 | -14.2604 | 10.39565911 | 11.16772638 | 98.239 | 54155.7486574074 | 54160.0355787037 | 701056010 | 190600.2 | 188000 | 190608.2 | 190600.2 | 0 | 190614.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 176470.8 | 176470.8 | 370342.8 | 4 | PROCESSED | 57537.5850578704 | 54757 | 54168.6244560185 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011351 | A long 150ks Suzaku observation of the most luminous nearby quasar, PDS 456, is proposed. In the X-ray band, PDS 456 shows a deep iron K absorption trough. One possibility is that the absorption arises from a massive 0.1c outflow, of column density 10^24 cm^-2. Such an outflow would represent a significant fraction of the quasar energy budget. A deep Suzaku observation is proposed to test this outflow model, in particular the high energy bandpass of Suzaku is essential for measuring the profile of the absorption feature and determining the kinematics of the outflow. It is also possible to differentiate between competing models for the iron K feature, most notably between an outflow and a strong reflection component from the innermost radii around a Kerr black hole. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | REEVES | JAMES | NULL | NULL | USA | 1 | AO1 | SOLVING THE ORIGIN OF THE DEEP IRON K ABSORPTION IN PDS 456 | XIS | Y |
| APM 08279+5255 | 127.9265 | 52.7635 | 165.74397918 | 36.24189551 | 118.0523 | 54020.1580902778 | 54022.3134143518 | 701057010 | 102332.8 | 100000 | 102340.8 | 102340.8 | 102332.8 | 102340.8 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 96018.7 | 96018.7 | 186185.8 | 3 | PROCESSED | 57535.8953125 | 54702 | 54053.9467013889 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011353 | Motivated by the detection of a relativistic outflow of highly ionized gas in previous XMM-Newton and Chandra observations of the lensed quasar APM08279+5255 we propose to monitor this object with three 100ks observations with the aim of improving our understanding of the significance of such outflows in regulating black hole growth and in influencing structure formation. The main scientific goals are : (a) verify the present interpretations of Fe line features in this quasar, (b) monitor the time variability of the Fe absorption features and thus constrain the acceleration mechanism, (c) constrain the kinematic, ionization and absorbing properties of the outflow, and (d) show whether the low-energy ionized absorber is part of the relativistic outflow. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | CHARTAS | GEORGE | NULL | NULL | USA | 1 | AO1 | VIEWS OF RELATIVISTIC WINDS THROUGH NATURAL LENSES | XIS | Y |
| APM 08279+5255 | 127.9229 | 52.7639 | 165.74356471 | 36.23970609 | 100.0676 | 54040.3996643518 | 54041.9690277778 | 701057020 | 102295 | 100000 | 102303 | 102311 | 102311 | 102295 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 95624 | 95624 | 135577.8 | 1 | PROCESSED | 57536.0492592593 | 54695 | 54088.5241782407 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011353 | Motivated by the detection of a relativistic outflow of highly ionized gas in previous XMM-Newton and Chandra observations of the lensed quasar APM08279+5255 we propose to monitor this object with three 100ks observations with the aim of improving our understanding of the significance of such outflows in regulating black hole growth and in influencing structure formation. The main scientific goals are : (a) verify the present interpretations of Fe line features in this quasar, (b) monitor the time variability of the Fe absorption features and thus constrain the acceleration mechanism, (c) constrain the kinematic, ionization and absorbing properties of the outflow, and (d) show whether the low-energy ionized absorber is part of the relativistic outflow. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | CHARTAS | GEORGE | NULL | NULL | USA | 1 | AO1 | VIEWS OF RELATIVISTIC WINDS THROUGH NATURAL LENSES | XIS | Y |
| APM 08279+5255 | 127.9195 | 52.7471 | 165.76446097 | 36.2381521 | 299.485 | 54183.9301041667 | 54186.4654513889 | 701057030 | 117143.3 | 125000 | 117143.3 | 117151.3 | 0 | 117143.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 110932.4 | 110932.4 | 219041.8 | 3 | PROCESSED | 57538.0464467593 | 54702 | 54209.5933680556 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011353 | Motivated by the detection of a relativistic outflow of highly ionized gas in previous XMM-Newton and Chandra observations of the lensed quasar APM08279+5255 we propose to monitor this object with three 100ks observations with the aim of improving our understanding of the significance of such outflows in regulating black hole growth and in influencing structure formation. The main scientific goals are : (a) verify the present interpretations of Fe line features in this quasar, (b) monitor the time variability of the Fe absorption features and thus constrain the acceleration mechanism, (c) constrain the kinematic, ionization and absorbing properties of the outflow, and (d) show whether the low-energy ionized absorber is part of the relativistic outflow. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | CHARTAS | GEORGE | NULL | NULL | USA | 1 | AO1 | VIEWS OF RELATIVISTIC WINDS THROUGH NATURAL LENSES | XIS | Y |
| 3C 390.3 | 280.629 | 79.7686 | 111.4356997 | 27.05756334 | 197.286 | 54083.1426851852 | 54085.1384722222 | 701060010 | 24 | 100000 | 99367.8 | 99367.8 | 24 | 99367.8 | 2 | 2 | 1 | 2 | 1 | 0 | 0 | 97881.3 | 97881.3 | 172419.9 | 3 | PROCESSED | 57536.3784722222 | 54702 | 54132.9968055556 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011363 | We propose Suzaku observations of the X-ray bright Broad-Line Radio Galaxies 3C382 and 3C390.3 to study their complex broad-band X-ray spectra. The HXD will constrain the continuum above 10 keV, discriminating between competing physically-different models, while at the same time the XIS will determine the parameters of the FeKalpha line and the shape of the soft X-rays. The proposed observations will allow us to shed light on the origin of reflection features in radio-loud AGN, ultimately determining the structure and ionization state of the accretion flow in these objects. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | SAMBRUNA | RITA | NULL | NULL | USA | 1 | AO1 | THE BROAD-BAND X-RAY SPECTRUM OF BROAD-LINE RADIO GALAXIES | XIS | Y |
| 1ES 1553+113 | 238.8999 | 11.1305 | 21.81691499 | 43.96274027 | 296.7536 | 53940.6127777778 | 53941.8036342593 | 701070010 | 55635.5 | 55000 | 55643.5 | 55651.5 | 55651.5 | 55635.5 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 53201.5 | 53201.5 | 102881.9 | 0 | PROCESSED | 57535.0418171296 | 54401 | 53955.6133680556 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011376 | Detecting absorption effects in TeV blazar spectra from TeV photon collisions on the extragalactic IR background (EBL) is a powerful tool to probe the EBL. It requires a thorough understanding of the intrinsic blazar spectra. We propose XIS and HXD observations, with emphasis on the hard X-rays, for the 3 most distant HESS blazars, coordinated with HESS observations. Thanks to Suzaku's sensitivity in a broad energy range, we expect to set tight limits on the models' parameter space, and constrain emission and acceleration scenarios by studying the shape and evolution of the particle distribution, most sensitively conducted in the important hard X-ray energy range. In coordination with TeV observations, it allows us to disentangle EBL absorption effects from the blazar intrinsic spectra. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | REIMER | ANITA | NULL | NULL | USA | 1 | AO1 | CHALLENGING JET MODELS OF THE MOST DISTANT TEV-BLAZARS | HXD | N |
| 1ES 1101-232 | 165.8976 | -23.5471 | 273.21266184 | 33.02701002 | 279.8544 | 53880.6859606482 | 53882.2161921296 | 701071010 | 62432.7 | 55000 | 62440.7 | 62440.7 | 62440.7 | 62432.7 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 50103.3 | 50103.3 | 132193.9 | 0 | PROCESSED | 57534.4584027778 | 54401 | 53927.4165393518 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011376 | Detecting absorption effects in TeV blazar spectra from TeV photon collisions on the extragalactic IR background (EBL) is a powerful tool to probe the EBL. It requires a thorough understanding of the intrinsic blazar spectra. We propose XIS and HXD observations, with emphasis on the hard X-rays, for the 3 most distant HESS blazars, coordinated with HESS observations. Thanks to Suzaku's sensitivity in a broad energy range, we expect to set tight limits on the models' parameter space, and constrain emission and acceleration scenarios by studying the shape and evolution of the particle distribution, most sensitively conducted in the important hard X-ray energy range. In coordination with TeV observations, it allows us to disentangle EBL absorption effects from the blazar intrinsic spectra. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | REIMER | ANITA | NULL | NULL | USA | 1 | AO1 | CHALLENGING JET MODELS OF THE MOST DISTANT TEV-BLAZARS | HXD | N |
| BL LACERTAE | 330.6466 | 42.3471 | 92.61224541 | -10.37092111 | 71.9797 | 53882.2303703704 | 53883.305775463 | 701073010 | 48529.4 | 50000 | 48545.4 | 48545.4 | 48529.4 | 48537.4 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 35544.3 | 35544.3 | 92902 | 1 | PROCESSED | 57534.4514236111 | 54401 | 53926.2373032407 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011377 | We propose two 50 ks Suzaku observations, one for each of gamma-ray bright blazars PKS 1510-089 and BL Lacertae, to be coordinated with optical and radio observations. The goal is to obtain broadband spectra and light-curves. The X-ray fluxes are known to be rapidly variable, but there is no information about the correlation between the spectral shape and flux, which is necessary to establish the origin of previously detected prominent soft X-ray excesses. They are crucial to discriminate between different radiation scenarios responsible for production of hard X-rays and gamma-rays, and to constrain the content and by extension, the acceleration process of the jet. These observations will be ingredients of a "pilot" campaigns for the future joint Suzaku-GLAST investigations. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MADEJSKI | GRZEGORZ | NULL | NULL | USA | 1 | AO1 | SUZAKU OBSERVATIONS OF GAMMA-RAY BRIGHT BLAZARS BL LACERTAE AND PKS 1510-089 | HXD | N |
| 1ES 1959+650 | 299.9645 | 65.1588 | 98.00607393 | 17.68746705 | 45.1602 | 53878.0509606482 | 53880.1718055556 | 701075010 | 98862.2 | 100000 | 98878.2 | 98862.2 | 98870.2 | 98878.2 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 96106 | 96106 | 183202.8 | 2 | PROCESSED | 57534.4674305556 | 54408 | 53928.2478472222 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012002 | We request to observe 1ES1959+650 and 1ES2344+514 for 100 ks each with SUZAKU simultaneously with the Whipple Cherenkov telescope. Whipple will extensively monitor these sources for months in 2006-2007. There are three well defined scientific cases that we would like to address. We want to study 1) the correlation between the soft and hard X-ray and TeV fluxes and spectra, extremely variable in these sources, sometimes showing extreme conditions; 2) the mystery of the ''orphan'' flares; i.e. events observed only in the TeV gamma rays without a counterpart in the X-rays: this is currently not understood in the framework of SSC models; 3) the origin of the lag observed between soft and hard X-ray variability in some blazars and the implications for the TeV emission. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TAGLIAFERRI | GIANPIERO | NULL | NULL | EUR | 1 | AO1 | JETS ON TEST: SIMULTANEOUS X-RAY AND TEV OBSERVATIONS OF 1ES1959+650 AND 1ES2344+514 | XIS | N |
| RBS 315 | 36.2519 | 18.8398 | 151.73247281 | -38.74296898 | 76.7825 | 53941.8167013889 | 53943.0404976852 | 701077010 | 47830.9 | 50000 | 47830.9 | 47830.9 | 47830.9 | 47830.9 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 43425 | 43425 | 105729.9 | 1 | PROCESSED | 57535.0495023148 | 54400 | 53955.7322106482 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012008 | We propose to observe with Suzaku the X-ray bright blazar RBS 315, showing a very hard spectrum (Gamma<1.2) in the 2-10 keV range as determined by XMM. The requested observation will allow us to measure the continuum in the full Suzaku range (0.3-200 keV), fully exploiting the unique capabilities of the satellite. With its wide energy coverage and good response at soft energies, Suzaku will allow to determine with precision the spectral properties of the source in the hard medium and soft X-ray ranges, providing important clues on the physics and the environment of relativistic jets. A good measurement of the continuum will allow us to determine the luminosity emitted via the IC mechanism which usually dominates the radiative output and the total kinetic power carried by the outflow. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | TAVECCHIO | FABRIZIO | NULL | NULL | EUR | 1 | AO1 | SUZAKU OBSERVATION OF THE HARD BROAD BAND CONTINUUM OF THE POWERFUL BLAZAR RBS 315 | HXD | N |
| NGC 5728 | 220.5794 | -17.3095 | 337.26599487 | 38.0606459 | 290.4081 | 53935.7359143518 | 53936.6264930556 | 701079010 | 41307.7 | 40000 | 41307.7 | 41307.7 | 41307.7 | 41307.7 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 39569 | 39569 | 76941.9 | 0 | PROCESSED | 57535.0121064815 | 54400 | 53943.5061111111 | 3.0.22.43 | 6 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012016 | The high-energy detectors onboard Swift and INTEGRAL have started to survey the hard X-ray sky above 10 keV. Although limited to bright X-ray fluxes (~10^-11 cgs), the large area surveyed so far has allowed to build up sizable sa mples of hard X-ray selected AGN almost unbiased against X-ray absorption. The AGN content of these surveys is dominated by obscured AGN. We have identified 3 objects which are most likely obscured by Compton-thick matter and very bright above 10 keV. We propose to observe them with Suzaku for 40 ks each to study their broad-band X-ray spectra and unveil previously unknown nearby heavily obscured AGN, with important consequences for the study of the AGN evolution and the synthesis of the X-ray background. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | COMASTRI | ANDREA | NULL | NULL | EUR | 1 | AO1 | BRIGHT COMPTON THICK GALAXIES IN THE BACKYARD | HXD | N |
| NGC 4992 | 197.2442 | 11.5776 | 318.61367169 | 73.91298788 | 297.9177 | 53904.2287615741 | 53905.2112615741 | 701080010 | 38788.6 | 40000 | 38788.6 | 38788.6 | 38788.6 | 38788.6 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 33617.9 | 33617.9 | 84881.9 | 1 | PROCESSED | 57534.7313657407 | 54422 | 53926.1865856482 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012016 | The high-energy detectors onboard Swift and INTEGRAL have started to survey the hard X-ray sky above 10 keV. Although limited to bright X-ray fluxes (~10^-11 cgs), the large area surveyed so far has allowed to build up sizable sa mples of hard X-ray selected AGN almost unbiased against X-ray absorption. The AGN content of these surveys is dominated by obscured AGN. We have identified 3 objects which are most likely obscured by Compton-thick matter and very bright above 10 keV. We propose to observe them with Suzaku for 40 ks each to study their broad-band X-ray spectra and unveil previously unknown nearby heavily obscured AGN, with important consequences for the study of the AGN evolution and the synthesis of the X-ray background. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | COMASTRI | ANDREA | NULL | NULL | EUR | 1 | AO1 | BRIGHT COMPTON THICK GALAXIES IN THE BACKYARD | HXD | N |
| MRK 0359 | 21.8893 | 19.1757 | 134.6025573 | -42.87605962 | 244.6178 | 54137.9789699074 | 54140.3738078704 | 701082010 | 107507 | 100000 | 107507 | 107507 | 0 | 107507 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 102576.1 | 102576.1 | 206867.8 | 2 | PROCESSED | 57537.3689930556 | 54735 | 54151.5150925926 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012023 | Markarian 359 was the first source to be identified as a Narrow Line Seyfert 1 (NLS1) AGN, and its importance as an unusual source has been recognised for a long time. In the optical, it has unusually narrow lines for a NLS1. X-ray observations of the source are rare, but based on an XMM-Newton observation a strong reflection 'hump' is predicted. The source is therefore a critical one in the investigation of relativistically blurred photoionized disc reflection models. A detailed Suzaku observation will provide improved data quality in the XIS waveband, allow investigation of spectral variability in this waveband, and constrain the amount of reflection independently by using the HXD. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | CRUMMY | JAMIE | NULL | NULL | EUR | 1 | AO1 | NVESTIGATING REFLECTION IN MARKARIAN 359 | XIS | Y |
| MKN 841 | 226.022 | 10.498 | 11.31218444 | 54.65057921 | 105.7688 | 54122.3650925926 | 54123.6063541667 | 701084010 | 51752.8 | 50000 | 51792.8 | 51752.8 | 0 | 51792.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43707.7 | 43707.7 | 107237.9 | 1 | PROCESSED | 57536.9356481482 | 54777 | 54139.3030208333 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012028 | We propose to perform two 50 ks Suzaku observations of Mkn 841, at an interval of a few months, in order to elucidate the origin of its different X-ray components. Strong soft excess and complex iron line profile are known to be present in this source and recent XMM observations reveal their extreme and puzzling spectral and temporal behaviors. Nevertheless, while the XMM observations help to better constrain their natures, their physical interpretation strongly suffer from the lack of data above 10 keV. Two dedicated Suzaku observations will provide crucial information for our understanding of these components, allowing 1) to obtain high S/N and striclty simultaneous broad band X-ray spectra from the soft X-ray up to the reflection bump and 2) to study their spectral variability behaviors | EXTRAGALACTIC COMPACT SOURCES | 7 | B | PETRUCCI | PIERRE-OLIVIER | NULL | NULL | EUR | 1 | AO1 | PROBING THE ORIGIN OF THE STRONG SOFT EXCESS AND PUZZLING REFLECTION COMPONENTS IN MKN 841 | HXD | Y |
| MKN 841 | 225.9811 | 10.3761 | 11.09749436 | 54.61837916 | 292.433 | 54304.6970949074 | 54306.218912037 | 701084020 | 50925.3 | 50000 | 50925.3 | 50933.3 | 0 | 50933.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47655.6 | 47655.6 | 131473.8 | 2 | PROCESSED | 57539.3432060185 | 54800 | 54339.5240277778 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012028 | We propose to perform two 50 ks Suzaku observations of Mkn 841, at an interval of a few months, in order to elucidate the origin of its different X-ray components. Strong soft excess and complex iron line profile are known to be present in this source and recent XMM observations reveal their extreme and puzzling spectral and temporal behaviors. Nevertheless, while the XMM observations help to better constrain their natures, their physical interpretation strongly suffer from the lack of data above 10 keV. Two dedicated Suzaku observations will provide crucial information for our understanding of these components, allowing 1) to obtain high S/N and striclty simultaneous broad band X-ray spectra from the soft X-ray up to the reflection bump and 2) to study their spectral variability behaviors | EXTRAGALACTIC COMPACT SOURCES | 7 | B | PETRUCCI | PIERRE-OLIVIER | NULL | NULL | EUR | 1 | AO1 | PROBING THE ORIGIN OF THE STRONG SOFT EXCESS AND PUZZLING REFLECTION COMPONENTS IN MKN 841 | HXD | Y |
| GB1428+4217 | 217.5879 | 42.0673 | 75.8575282 | 64.90635728 | 315.7011 | 53898.716400463 | 53899.8336111111 | 701092010 | 48695.6 | 50000 | 48695.6 | 48695.6 | 48695.6 | 48695.6 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 43494.3 | 43494.3 | 96515.9 | 1 | PROCESSED | 57534.6334259259 | 54394 | 53926.3635069444 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012043 | We propose to observe GB1428+4217 at z=4.72 for 50ks with Suzaku in order to determine its spectrum up to 45 keV, corresponding to a rest-frame energy of ~250 keV. This will allow to robustly model the spectrum in terms of a hard power-law and a Comptonization component from the scattering of `cold' electrons in the jet onto the soft nuclear photon field, as qualitatively hinted by XMM-Newton available data. This would be the first detection of such a feature in blazars and would directly and uniquely give information on the power of the relativistic jets in this source. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | FABIAN | ANDREW | NULL | NULL | EUR | 1 | AO1 | JET POWER OF THE DISTANT EXTREME LUMINOSITY BLAZAR GB1428+4217 | XIS | N |
| MARKARIAN 509 | 311.0194 | -10.6637 | 36.02321332 | -29.81091499 | 73.1708 | 53850.7831481482 | 53851.5252199074 | 701093010 | 24575.6 | 25000 | 24575.6 | 24575.6 | 24591.6 | 24591.6 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 15407 | 15407 | 64097.9 | 1 | PROCESSED | 57533.5586342593 | 54394 | 53907.6894560185 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012050 | We propose to perform 4 repeated Suzaku observations of 25 ks each of the Seyfert 1 galaxy MKN 509, the brightest Seyfert galaxy of the Piccinotti sample in the 2-100 keV band that is not strongly affected by neutral or ionized absorbing material. The aim of the study is to disentangle the different physical explanations for the origin of the soft excess looking at the long time--scale correlations between the variations of the emission and shape of the soft excess and the emission at high energy (E > 10 keV). | EXTRAGALACTIC COMPACT SOURCES | 7 | A | PONTI | GABRIELE | NULL | NULL | EUR | 1 | AO1 | SOLVING THE NATURE OF THE SOFT EXCESS IN AGNS WITH SUZAKU | HXD | N |
| MARKARIAN 509 | 311.0427 | -10.7271 | 35.96837179 | -29.85867019 | 254.3019 | 54022.3263888889 | 54023.0856365741 | 701093020 | 25929.8 | 25000 | 25961.8 | 25929.8 | 25953.8 | 25961.8 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 23449.7 | 23449.7 | 65589.9 | 1 | PROCESSED | 57535.8399305556 | 54526 | 54053.6032638889 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012050 | We propose to perform 4 repeated Suzaku observations of 25 ks each of the Seyfert 1 galaxy MKN 509, the brightest Seyfert galaxy of the Piccinotti sample in the 2-100 keV band that is not strongly affected by neutral or ionized absorbing material. The aim of the study is to disentangle the different physical explanations for the origin of the soft excess looking at the long time--scale correlations between the variations of the emission and shape of the soft excess and the emission at high energy (E > 10 keV). | EXTRAGALACTIC COMPACT SOURCES | 7 | A | PONTI | GABRIELE | NULL | NULL | EUR | 1 | AO1 | SOLVING THE NATURE OF THE SOFT EXCESS IN AGNS WITH SUZAKU | XIS | N |
| MARKARIAN 509 | 311.0428 | -10.7274 | 35.9681072 | -29.85888698 | 254.2043 | 54054.375150463 | 54055.0113541667 | 701093030 | 24446.6 | 25000 | 24446.6 | 24446.6 | 0 | 24446.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18327 | 18327 | 54967.9 | 1 | PROCESSED | 57536.1015162037 | 54456 | 54088.6171875 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012050 | We propose to perform 4 repeated Suzaku observations of 25 ks each of the Seyfert 1 galaxy MKN 509, the brightest Seyfert galaxy of the Piccinotti sample in the 2-100 keV band that is not strongly affected by neutral or ionized absorbing material. The aim of the study is to disentangle the different physical explanations for the origin of the soft excess looking at the long time--scale correlations between the variations of the emission and shape of the soft excess and the emission at high energy (E > 10 keV). | EXTRAGALACTIC COMPACT SOURCES | 7 | A | PONTI | GABRIELE | NULL | NULL | EUR | 1 | AO1 | SOLVING THE NATURE OF THE SOFT EXCESS IN AGNS WITH SUZAKU | XIS | N |
| MARKARIAN 509 | 311.0451 | -10.7278 | 35.96880101 | -29.86110163 | 254.2048 | 54066.1625810185 | 54067.12875 | 701093040 | 33094.4 | 32000 | 33094.4 | 33094.4 | 0 | 33094.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 29454.4 | 29454.4 | 83465.9 | 1 | PROCESSED | 57536.2044212963 | 54456 | 54088.5895023148 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012050 | We propose to perform 4 repeated Suzaku observations of 25 ks each of the Seyfert 1 galaxy MKN 509, the brightest Seyfert galaxy of the Piccinotti sample in the 2-100 keV band that is not strongly affected by neutral or ionized absorbing material. The aim of the study is to disentangle the different physical explanations for the origin of the soft excess looking at the long time--scale correlations between the variations of the emission and shape of the soft excess and the emission at high energy (E > 10 keV). | EXTRAGALACTIC COMPACT SOURCES | 7 | A | PONTI | GABRIELE | NULL | NULL | EUR | 1 | AO1 | SOLVING THE NATURE OF THE SOFT EXCESS IN AGNS WITH SUZAKU | XIS | N |
| PKS 1510-089 | 228.2108 | -9.1043 | 351.2856545 | 40.1353659 | 286.8003 | 53949.3968634259 | 53952.2544444445 | 701094010 | 119157.7 | 120000 | 119157.7 | 119157.7 | 119165.7 | 119165.7 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 106258.8 | 106258.8 | 246863.8 | 5 | PROCESSED | 57535.1605208333 | 54394 | 54018.7363194444 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 013016 | It has been a long mystery (i) how the relativistic jets are formed, and (ii) what is the composition of a jet. In the theoretical view, strong magnetic field (u_B >> u_e) is necessary to produce such outflows with baryonic matters, but observations favor opposite scenario, namely particle dominated (u_e >> u_B), leptonic jet. Such discrepancies can be resolved if moderate numbers of protons (n_e/n_p > 50) are mixed in the non-tnermal pair populations. This can be easily tested if we can observe characteristic "soft X-ray bump" produced by the bulk-Comptonization of UV photons emitted from an accretion disk. We propose a deep observation (40ksec x3) of an EGRET quasar PKS 1510-089, which shows a clear sign of soft X-ray bump in BeppoSAX, ROSAT and ASCA observations. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | KATAOKA | JUN | MADEJSKI | GRZEGORZ | JUS | 1 | AO1 | DIRECT TESTING THE JET COMPOSITION IN A POWERFUL EGRET QUASAR PKS 1510-089 | XIS | N |
| M106 | 184.7117 | 47.2376 | 138.43381178 | 68.89762168 | 287.1938 | 53896.5413078704 | 53898.7113425926 | 701095010 | 99817.5 | 100000 | 99881.5 | 99817.5 | 99881.5 | 99881.5 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 97522.9 | 97522.9 | 187483.9 | 1 | PROCESSED | 57534.6515393518 | 54401 | 53927.2308449074 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 013151 | We propose observations of the nearby Low Luminosity AGN, M81 and M106, for 100 ks for each target. We aim to detect both targets up to ~200 keV for the first time. We will determine the photon indices of the hard X-ray power-law continuum, with searching for other possible characteristics such as Compton hump around 10-20 keV and cutoff around 100-200 keV which would lead major discoveries. We will study the shape of Fe-K line(s) around 6-7 keV and their time variances. Our goal is to compare their hard X-ray spectra with those of SWG seyfert galaxies, with unprecedented accuracy, to study the accresion mechanism of LLAGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ITOH | TAKESHI | REYNOLDS | CHRISTOPHER | JUS | 1 | AO1 | OBSERVATIONS OF HARD X-RAYS FROM LOW LUMINOSITY ACTIVE GALACTIC NUCLEI | HXD | N |
| F05189-2524 | 80.2383 | -25.4117 | 227.93752087 | -30.32292957 | 290.8212 | 53835.6784259259 | 53837.6467708333 | 701097010 | 78155.5 | 80000 | 78155.5 | 78163.5 | 78155.5 | 78155.5 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 51740.2 | 51740.2 | 169989.9 | 2 | PROCESSED | 57533.4937268518 | 54401 | 53906.8811689815 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 014341 | We wish to take advantage of the unprecedented sensitivity of Suzaku Observatory to very hard X-rays (> 10 keV) to constrain the energy source -- starburst or black-hole driven activity -- in two of the nearest and brightest ultraluminous infrared galaxies, Mrk 273 and F05189-2524. These objects are arguably the best local laboratories to study the basic physical processes involved in creating massive early type hosts on the one hand, and feeding embedded supermassive black holes on the other hand, in major galaxy mergers. The Suzaku data will be used to search for the high-energy signature of deeply buried active black holes and to look for short timescale variability, another signature of black-hole driven activity. These data will be part of S. Teng's PhD thesis at Maryland. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | VEILLEUX | SYLVAIN | ANABUKI | NAOHISA | USJ | 1 | AO1 | THE DOMINANT ENERGY SOURCE OF ULTRALUMINOUS INFRARED GALAXIES | HXD | N |
| NGC 4395 | 186.4111 | 33.4884 | 162.54122992 | 81.55189464 | 303.1476 | 54253.6042013889 | 54256.2981944444 | 702001010 | 101507.5 | 100000 | 101515.5 | 101507.5 | 0 | 101515.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 101929.2 | 101929.2 | 232719.8 | 4 | PROCESSED | 57538.8900694444 | 54745 | 54263.5438194445 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020001 | We propose a 100 ks observation of the intermediate mass black hole (IMBH) active nucleus in the dwarf Seyfert galaxy NGC 4395. Utilising the high-energy sensitivity of Suzaku will enable us to determine the shape of the intrinsic continuum, which is significantly absorbed below 10 keV. Constraining the shape of the continuum will allow us to investigate the more general problem of the relationship between AGN flux and apparent spectral slope. In addition, with a firm grasp of the intrinsic continuum properties, we can accurately determine the physical conditions of the warm absorber in NGC 4395. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TANAKA | YASUO | NULL | NULL | JAP | 2 | AO2 | UNCOVERING THE IMBH ACTIVE NUCLEUS IN THE DWARF SEYFERT GALAXY NGC 4395 | HXD | Y |
| NGC1386 | 54.1629 | -35.9533 | 237.58696036 | -53.99184818 | 64.5172 | 54309.0884259259 | 54310.1668402778 | 702002010 | 55522.6 | 50000 | 55522.6 | 55530.6 | 0 | 55530.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47521.3 | 47521.3 | 93143.9 | 1 | PROCESSED | 57539.3619907407 | 54707 | 54339.0775115741 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020005 | Compton thick Seyfert 2 galaxies may constitute a large fraction of the Seyfert 2 galaxy's population. However, the nature of the Compton-thick objects is still unclear due to the heavy obscuration of the nuclear emission. The wide-band spectroscopy with Suzaku is crucial to expose their nature hidden by thick matter. In order to reveal their nature in the local Universe, we propose Suzaku observations of Risaliti's Compton-thick objects. These observations will also bring us important results to study the structure and evolution of active galactic nuclei. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | AWAKI | HISAMITSU | NULL | NULL | JAP | 2 | AO2 | REVEAL THE NATURE OF COMPTON THICK SEYFERT 2 GALAXIES WITH SUZAKU | HXD | Y |
| NGC2273 | 102.5972 | 60.7838 | 155.04232679 | 23.32753471 | 246.2514 | 54211.2737384259 | 54212.5071643518 | 702003010 | 90012.6 | 50000 | 90028.6 | 90020.6 | 0 | 90012.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 69588.7 | 69588.7 | 106557.9 | 1 | PROCESSED | 57538.4439583333 | 54744 | 54216.1628703704 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020005 | Compton thick Seyfert 2 galaxies may constitute a large fraction of the Seyfert 2 galaxy's population. However, the nature of the Compton-thick objects is still unclear due to the heavy obscuration of the nuclear emission. The wide-band spectroscopy with Suzaku is crucial to expose their nature hidden by thick matter. In order to reveal their nature in the local Universe, we propose Suzaku observations of Risaliti's Compton-thick objects. These observations will also bring us important results to study the structure and evolution of active galactic nuclei. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | AWAKI | HISAMITSU | NULL | NULL | JAP | 2 | AO2 | REVEAL THE NATURE OF COMPTON THICK SEYFERT 2 GALAXIES WITH SUZAKU | HXD | Y |
| NGC3393 | 162.075 | -25.2139 | 270.6699706 | 29.83420275 | 292.9271 | 54243.7827662037 | 54245.1876041667 | 702004010 | 55227 | 50000 | 55227 | 55227 | 0 | 55227 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48255 | 48255 | 121369.9 | 4 | PROCESSED | 57538.7560416667 | 54745 | 54255.6532986111 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020005 | Compton thick Seyfert 2 galaxies may constitute a large fraction of the Seyfert 2 galaxy's population. However, the nature of the Compton-thick objects is still unclear due to the heavy obscuration of the nuclear emission. The wide-band spectroscopy with Suzaku is crucial to expose their nature hidden by thick matter. In order to reveal their nature in the local Universe, we propose Suzaku observations of Risaliti's Compton-thick objects. These observations will also bring us important results to study the structure and evolution of active galactic nuclei. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | AWAKI | HISAMITSU | NULL | NULL | JAP | 2 | AO2 | REVEAL THE NATURE OF COMPTON THICK SEYFERT 2 GALAXIES WITH SUZAKU | HXD | Y |
| NGC5135 | 201.4174 | -29.8897 | 311.72101463 | 32.39717213 | 286.1252 | 54284.2497800926 | 54285.3057175926 | 702005010 | 52496.4 | 50000 | 52496.4 | 52496.4 | 0 | 52496.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 49783.7 | 49783.7 | 91220.9 | 2 | PROCESSED | 57539.1022222222 | 54696 | 54328.4497453704 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020005 | Compton thick Seyfert 2 galaxies may constitute a large fraction of the Seyfert 2 galaxy's population. However, the nature of the Compton-thick objects is still unclear due to the heavy obscuration of the nuclear emission. The wide-band spectroscopy with Suzaku is crucial to expose their nature hidden by thick matter. In order to reveal their nature in the local Universe, we propose Suzaku observations of Risaliti's Compton-thick objects. These observations will also bring us important results to study the structure and evolution of active galactic nuclei. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | AWAKI | HISAMITSU | NULL | NULL | JAP | 2 | AO2 | REVEAL THE NATURE OF COMPTON THICK SEYFERT 2 GALAXIES WITH SUZAKU | HXD | Y |
| 3C 326 | 238.0402 | 20.0989 | 33.27596058 | 48.22956027 | 119.5805 | 54484.6775 | 54486.215462963 | 702006010 | 61738.1 | 60000 | 61738.1 | 61738.1 | 0 | 61738.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 53412.6 | 53412.6 | 132859.8 | 1 | PROCESSED | 57541.3565162037 | 54888 | 54515.0338078704 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020014 | Suzaku observations of two giant radio galaxies, 3C 326 and 3C 35, are proposed. In 60 ks exposure on the individual targets, inverse Component X-ray emission from their lobes is detected with high signal statistics. As a result, the energy densities of electrons and magnetic fields in these lobesare precisely deteremined. The size of these radio galaxies are significantly larger than that of the previous sample. Therefore, the size dependence of energetics in the lobes will be investigated. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | ISOBE | NAOKI | NULL | NULL | JAP | 2 | AO2 | SUZAKU OBSERVATIONS OF LOBES OF GIANT RADIO GALAXIES, 3C 326 AND 3C 35 | XIS | Y |
| OJ 287 FLARE | 133.7115 | 20.1695 | 206.74425687 | 35.84822718 | 98.7868 | 54411.475 | 54413.896099537 | 702008010 | 112044 | 100000 | 112052 | 112060 | 0 | 112044 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 102923.8 | 102923.8 | 209151.9 | 3 | PROCESSED | 57540.5116087963 | 54791 | 54423.3848032407 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020024 | OJ 287 is a promissing candidate of a suppermassive binary black hole, based on its periodic flare with a cycle of about 12 years. The next flare is predicted to take place on the fall, 2007. Therefore, two Suzaku exposures on OJ 287 is proposed, coordinated with radio, optical and very high energy gamma-ray observations. The first observation is on the spring to obtained the multi-wavelength spectrum of the target in its quiescent phase. The second is planned to be in a form of ToO observation on the fall, which will be triggered by an optical flare. The nature of the flare will be extensively investigated in these observatsions. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ISOBE | NAOKI | NULL | NULL | JAP | 2 | AO2-TOO | MULTI-WAVELENGTH OBSERVATION OF PREDICTED FLARE OF SUPERMASSIVE BINARY BLACK HOLE CANDIDATE, OJ 287 | HXD | Y |
| OJ 287 QUIESCENT | 133.689 | 20.0482 | 206.87650629 | 35.78772906 | 283.9125 | 54200.8243055556 | 54203.4654976852 | 702009010 | 102844.1 | 100000 | 102844.1 | 102844.1 | 0 | 102844.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 93624.4 | 93624.4 | 228185.9 | 12 | PROCESSED | 57538.2031018518 | 54744 | 54210.7303587963 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020024 | OJ 287 is a promissing candidate of a suppermassive binary black hole, based on its periodic flare with a cycle of about 12 years. The next flare is predicted to take place on the fall, 2007. Therefore, two Suzaku exposures on OJ 287 is proposed, coordinated with radio, optical and very high energy gamma-ray observations. The first observation is on the spring to obtained the multi-wavelength spectrum of the target in its quiescent phase. The second is planned to be in a form of ToO observation on the fall, which will be triggered by an optical flare. The nature of the flare will be extensively investigated in these observatsions. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ISOBE | NAOKI | NULL | NULL | JAP | 2 | AO2-TOO | MULTI-WAVELENGTH OBSERVATION OF PREDICTED FLARE OF SUPERMASSIVE BINARY BLACK HOLE CANDIDATE, OJ 287 | HXD | Y |
| NGC5643 | 218.1422 | -44.2268 | 321.40267054 | 14.9878026 | 293.4229 | 54331.8795023148 | 54332.9724421296 | 702010010 | 42882.3 | 50000 | 42890.3 | 42890.3 | 0 | 42882.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40868.5 | 40868.5 | 94386 | 2 | PROCESSED | 57539.6330902778 | 54770 | 54402.2016782407 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020034 | Seyfert 2 galaxies often have an nucleus obscured by thick matter. Risaliti et al. found that Compton thick Seyfert 2 galaxies may constitute a large fraction of the Seyfert 2 galaxy s population by studying the distribution of absorbing column densities among Seyfert 2 galaxies. This result is important to discuss on the structure and evolution of active galactic nuclei. However, it is difficult to classify Seyfert 2 galaxies into Compton thick and thin objects only by using their X-ray spectra below 10 keV. Therefore, there may be Compton thin objects among Risaliti s Compton thick sample. In order to make the distribuion of the column density more reliable, we propose the Suzaku observations of heavily obscured AGNs with NH >1E25cm-2. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | AWAKI | HISAMITSU | NULL | NULL | JAP | 2 | AO2 | SUZAKU OBSERVATIONS OF THE HEAVILY OBSCURED AGNS WITH NH>1E25 CM-2 | HXD | Y |
| IC 3639 | 190.1935 | -36.8078 | 300.55692841 | 26.01476797 | 293.9494 | 54293.1966435185 | 54294.4133564815 | 702011010 | 53391.2 | 50000 | 53391.2 | 53391.2 | 0 | 53391.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48485.2 | 48485.2 | 105110 | 1 | PROCESSED | 57539.1904050926 | 54709 | 54339.5331365741 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020034 | Seyfert 2 galaxies often have an nucleus obscured by thick matter. Risaliti et al. found that Compton thick Seyfert 2 galaxies may constitute a large fraction of the Seyfert 2 galaxy s population by studying the distribution of absorbing column densities among Seyfert 2 galaxies. This result is important to discuss on the structure and evolution of active galactic nuclei. However, it is difficult to classify Seyfert 2 galaxies into Compton thick and thin objects only by using their X-ray spectra below 10 keV. Therefore, there may be Compton thin objects among Risaliti s Compton thick sample. In order to make the distribuion of the column density more reliable, we propose the Suzaku observations of heavily obscured AGNs with NH >1E25cm-2. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | AWAKI | HISAMITSU | NULL | NULL | JAP | 2 | AO2 | SUZAKU OBSERVATIONS OF THE HEAVILY OBSCURED AGNS WITH NH>1E25 CM-2 | HXD | Y |
| ARK 120 | 79.0439 | -0.2064 | 201.74563913 | -21.16237248 | 274.9546 | 54191.755162037 | 54193.905150463 | 702014010 | 100863.5 | 100000 | 100863.5 | 100863.5 | 0 | 100863.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 95312.1 | 95312.1 | 185743.9 | 1 | PROCESSED | 57538.0955324074 | 54744 | 54200.5657060185 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020035 | We propose to obtain the broad-band spectra of the bright Seyfert 1 Ark 120 with Suzaku. Since Ark 120 shows no strong absorption features in its X-ray spectrum, we can cleanly measure the shape of the continuum and Fe K line without introducing any ambiguity caused by absorption along the line of sight. The spectrum will be used to test the diskline hypothesis in Seyferts and to study the fundamental processes producing broad band spectra of AGNs. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TERASHIMA | YUICHI | NULL | NULL | JAP | 2 | AO2 | THE ORIGIN OF THE BROAD FE LINE IN THE SEYFERT 1 ARK 120 | HXD | Y |
| NGC 7314 | 338.9055 | -25.9984 | 27.22535085 | -59.7013223 | 59.6979 | 54215.4316319444 | 54217.9516666667 | 702015010 | 109019.8 | 100000 | 109019.8 | 109019.8 | 0 | 109019.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 92240.8 | 92240.8 | 217713.9 | 2 | PROCESSED | 57538.5280439815 | 54744 | 54230.4096527778 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020037 | We propose a Suzaku observation of the highly variable Seyfert 1.9 NGC 7314. The Fe K line in this object varies on a very short time scale (<10 keV) in contrast to Seyferts observed with Suzaku in the SWG time. The data will be used to search for a weak broad Fe K line to constrain the inner radius of an optically thick disk and to study the spectral variation on short time scales to elucidate the fundamental processes producing X-rays in the vicinity of the central black hole. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | TERASHIMA | YUICHI | NULL | NULL | JAP | 2 | AO2 | RAPID SPECTRAL X-RAY VARIABILITY IN THE SEYFERT GALAXY NGC 7314: UNDERSTANDING ENERGY RELEASE PROCESSES IN AGN | HXD | Y |
| M82 X-1 | 149.1432 | 69.7042 | 141.33659361 | 40.60182861 | 163.0524 | 54367.135775463 | 54367.8716898148 | 702026010 | 35599.9 | 40000 | 36031.9 | 35599.9 | 0 | 36023.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30474.9 | 30474.9 | 63569.9 | 1 | PROCESSED | 57540.0638194444 | 54770 | 54402.2563657407 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020092 | We propose Suzaku observations of the intermediate-mass black hole candidate M82 X-1 for spectral study with a wide-band energy range including over 10 keV. In particular, the purpose is to determine a spectral cut-off energy in details in order to improve unified understanding of different mass black holes in comparison with those of stellar-mass black holes and ULXs in nearby galaxies. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | MIYAWAKI | RYOHEI | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY SPECTRAL STUDY OF M82 X-1 WITH SUZAKU | HXD | Y |
| IGR J21247+5058 | 321.1969 | 51.0428 | 93.38215801 | 0.42876214 | 108.8126 | 54206.5871759259 | 54208.4613888889 | 702027010 | 85031.9 | 80000 | 85031.9 | 85039.9 | 0 | 85047.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70970.9 | 70970.9 | 161894.9 | 2 | PROCESSED | 57538.4530671296 | 54744 | 54214.1071412037 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020097 | The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to the latetest population synthesis model, its estimate is strongly coupled with the broad band spectral shape of moderately absorbed AGNs, which is only poorly understood. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many new absorbed AGNs that can be best followed-up with Suzaku. Here we propose to observe two of them to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 2 | AO2 | BROAD BAND SPECTRA OF NEW SWIFT/BAT AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND | HXD | Y |
| SWIFT J1922.7-1716 | 290.6403 | -17.2233 | 20.73500926 | -14.48356253 | 80.064 | 54198.231099537 | 54200.4321643518 | 702028010 | 78638.6 | 80000 | 78638.6 | 78638.6 | 0 | 78638.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 61353.3 | 61353.3 | 190129.8 | 0 | PROCESSED | 57538.1728356482 | 54744 | 54206.3754166667 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020097 | The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to the latetest population synthesis model, its estimate is strongly coupled with the broad band spectral shape of moderately absorbed AGNs, which is only poorly understood. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many new absorbed AGNs that can be best followed-up with Suzaku. Here we propose to observe two of them to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 2 | AO2 | BROAD BAND SPECTRA OF NEW SWIFT/BAT AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND | HXD | Y |
| MRK 1239 | 148.0816 | -1.6118 | 239.27134701 | 38.21950621 | 286.5242 | 54226.0919907407 | 54227.5973726852 | 702031010 | 63128 | 80000 | 63128 | 63128 | 0 | 63128 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 53594.4 | 53594.4 | 130061.9 | 2 | PROCESSED | 57615.5991435185 | 54744 | 54235.4602662037 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020127 | X-ray observations of "Hidden" narrow-line Seyfert 1 galaxies (NLS1s) have never been performed effectively, in spite of the fact that both obscuring material and nucleus of NLS1s are thought to be a crucial key to understand the fueling and accretion mechanisms, which may be directly related to the evolution of supermassive black holes and host galaxies. Hence,we propose 80 ksec observation of the candidates of hidden NLS1s Mrk 1239. Large effective area and unprecedented wide energy band of Suzaku allows us to strictly constrain the column density and covering fraction of obscuring matter, intrinsic power law slope, and its luminosity. From these observations, we expect to derive more complete unified picture of AGNs | EXTRAGALACTIC COMPACT SOURCES | 7 | B | HABA | YOSHITO | NULL | NULL | JAP | 2 | AO2 | SUZAKU VIEW OF "HIDDEN" NARROW-LINE SEYFERT 1 GALAXY MRK 1239 | XIS | Y |
| LMC X-4 | 83.1886 | -66.3594 | 276.32297371 | -32.53740633 | 226.9086 | 54500.7929513889 | 54501.0521875 | 702036010 | 0 | 20000 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1 | 0 | 0 | 5672.9 | 5672.9 | 22377.9 | 1 | PROCESSED | 57541.4899537037 | 54883 | 54515.6401851852 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021127 | We propose for a series of three 20ks observations of the binary X-ray pulsar LMC X-4. This source shows 13.5 s pulsations, a 1.4 d orbital period, and a long-period (~30 d) variability due to a warped, precessing accretion disk. The proposed analysis will use pulse-phase spectroscopy with XIS to explore changes in the X-ray pulses and spectra at three different phases in the disk precession. This work will give us a detailed picture of the accretion flow, particularly for the inner regions of the accretion disk that are illuminated by the X-rays from the neutron star. This project takes advantage of the strengths of the XIS, particularly its excellent spectral resolution, sufficient (1s) time resolution in Window mode, and wide PSF that limits pile-up effects. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | HICKOX | RYAN | NULL | NULL | USA | 2 | AO2 | SUPERORBITAL VARIATION OF LMC X-4: EXPLORING THE ACCRETION FLOW | XIS | Y |
| LMC X-4 | 83.221 | -66.3591 | 276.32094979 | -32.52452295 | 284.2438 | 54561.5523842593 | 54562.3058333333 | 702036020 | 25339.7 | 20000 | 25342.5 | 25342.5 | 0 | 25339.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 24502 | 24502 | 65070 | 0 | PROCESSED | 57542.2490046296 | 54943 | 54574.4237152778 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021127 | We propose for a series of three 20ks observations of the binary X-ray pulsar LMC X-4. This source shows 13.5 s pulsations, a 1.4 d orbital period, and a long-period (~30 d) variability due to a warped, precessing accretion disk. The proposed analysis will use pulse-phase spectroscopy with XIS to explore changes in the X-ray pulses and spectra at three different phases in the disk precession. This work will give us a detailed picture of the accretion flow, particularly for the inner regions of the accretion disk that are illuminated by the X-rays from the neutron star. This project takes advantage of the strengths of the XIS, particularly its excellent spectral resolution, sufficient (1s) time resolution in Window mode, and wide PSF that limits pile-up effects. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | HICKOX | RYAN | NULL | NULL | USA | 2 | AO2 | SUPERORBITAL VARIATION OF LMC X-4: EXPLORING THE ACCRETION FLOW | XIS | Y |
| LMC X-4 | 83.1883 | -66.3595 | 276.32310713 | -32.53751505 | 226.9099 | 54507.0294560185 | 54507.6043287037 | 702037010 | 23381.4 | 20000 | 23389.4 | 23397.4 | 0 | 23381.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 20047 | 20047 | 49662 | 1 | PROCESSED | 57541.5628356482 | 54883 | 54515.5898842593 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021127 | We propose for a series of three 20ks observations of the binary X-ray pulsar LMC X-4. This source shows 13.5 s pulsations, a 1.4 d orbital period, and a long-period (~30 d) variability due to a warped, precessing accretion disk. The proposed analysis will use pulse-phase spectroscopy with XIS to explore changes in the X-ray pulses and spectra at three different phases in the disk precession. This work will give us a detailed picture of the accretion flow, particularly for the inner regions of the accretion disk that are illuminated by the X-rays from the neutron star. This project takes advantage of the strengths of the XIS, particularly its excellent spectral resolution, sufficient (1s) time resolution in Window mode, and wide PSF that limits pile-up effects. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | HICKOX | RYAN | NULL | NULL | USA | 2 | AO2 | SUPERORBITAL VARIATION OF LMC X-4: EXPLORING THE ACCRETION FLOW | XIS | Y |
| LMC X-4 | 83.1804 | -66.3624 | 276.32693529 | -32.54034863 | 209.1491 | 54480.3607175926 | 54480.7919560185 | 702038010 | 21657.9 | 20000 | 21672.6 | 21657.9 | 0 | 21672.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22883.7 | 22883.7 | 37252 | 0 | PROCESSED | 57541.3108796296 | 54860 | 54490.3089236111 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021127 | We propose for a series of three 20ks observations of the binary X-ray pulsar LMC X-4. This source shows 13.5 s pulsations, a 1.4 d orbital period, and a long-period (~30 d) variability due to a warped, precessing accretion disk. The proposed analysis will use pulse-phase spectroscopy with XIS to explore changes in the X-ray pulses and spectra at three different phases in the disk precession. This work will give us a detailed picture of the accretion flow, particularly for the inner regions of the accretion disk that are illuminated by the X-rays from the neutron star. This project takes advantage of the strengths of the XIS, particularly its excellent spectral resolution, sufficient (1s) time resolution in Window mode, and wide PSF that limits pile-up effects. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | HICKOX | RYAN | NULL | NULL | USA | 2 | AO2 | SUPERORBITAL VARIATION OF LMC X-4: EXPLORING THE ACCRETION FLOW | XIS | Y |
| NGC 4593 | 189.9131 | -5.3426 | 297.48049807 | 57.40434975 | 112.24 | 54449.1962384259 | 54451.972349537 | 702040010 | 118841.5 | 107000 | 118841.5 | 118841.5 | 0 | 118841.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 108976 | 108976 | 239789.9 | 6 | PROCESSED | 57540.92 | 54829 | 54462.4425462963 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021302 | We propose a 80 ksec observation of the bright Seyfert 1 NGC 4593 to resolve the moderately relativistic Fe K line, and test for a truncated or ionized accretion disk. To achieve accurate modeling of the broad Fe line, Suzaku's broad bandpass is required to deconvolve the broadband emitting component and accurately constrain the continuum. NGC 4593 is one of the few Seyferts to also show evidence for Fe XXVI emission at 6.9 keV; we will use the XIS to confirm the line and constrain its origin. If the thin accretion disk is truncated or transitions to an ADAF, it would reveal NGC 4593 to be an analogue of low/hard-state X-ray Binaries. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | MARKOWITZ | ALEX | NULL | NULL | USA | 2 | AO2 | DOES THE SEYFERT AGN NGC 4593 HAVE A TRUNCATED OR IONIZED ACCRETION DISK? | XIS | Y |
| 1H0419-577 | 66.5116 | -57.211 | 266.99901337 | -41.98911345 | 55.5914 | 54306.2319328704 | 54309.0835532407 | 702041010 | 205862.8 | 200000 | 205870.8 | 205870.8 | 0 | 205862.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 152831.7 | 152831.7 | 246357.8 | 2 | PROCESSED | 57539.3963888889 | 54706 | 54339.7211111111 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021304 | A hotly debated question is whether Seyfert X-ray spectra are dominated by components that are blurred by strong gravitational effects close (< 20rg) to the central black hole. Models featuring either complex absorption or blurred disk spectra provide equally good parameterizations of the mean X-ray spectrum of many objects. To make progress with current instruments we require observations with a temporal baseline and flux that will allow us to look for key parameter correlations, as the two scenarios predict different time-dependent behavior. To that end, we propose a Suzaku observation of 1H0419-577, a target that exhibits a remarkable degree of spectral variability in the X-ray regime promising some definitive results in this important area. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | TURNER | TRACEY | NULL | NULL | USA | 2 | AO2 | HOW IMPORTANT IS STRONG RELATIVISTIC BLURRING IN SPECTRA OF SEYFERT GALAXIES? | XIS | Y |
| NGC5548 | 214.4931 | 25.1284 | 31.93341942 | 70.49864062 | 309.3821 | 54269.9362847222 | 54270.6389814815 | 702042010 | 31118.8 | 30000 | 31118.8 | 31118.8 | 0 | 31118.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27175.9 | 27175.9 | 60705.9 | 0 | PROCESSED | 57538.9803703704 | 54695 | 54319.4659953704 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021307 | We propose a 2 month Suzaku monitoring program of 7 weekly 30ksec observations of the normal type 1 AGN, NGC5548. NGC5548 is uniquely well studied at all wavelengths, and will vary by a factor of 1.5, or more, at 97% probability. Variations of the Warm Absorber will determine its location in NGC5548, disciminating between models and determining the mass loss rate in the WA wind. This will provide a baseline data point for models of 'cosmological feedback' from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes or lack thereof in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, any broad Fe-K or high ionization edge. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ELVIS | MARTIN | NULL | NULL | USA | 2 | AO2 | NGC5548 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK | XIS | Y |
| NGC5548 | 214.4931 | 25.1252 | 31.92399813 | 70.49805067 | 305.6592 | 54275.9121643518 | 54276.6918055556 | 702042020 | 35915.2 | 30000 | 35915.2 | 35915.2 | 0 | 35915.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 33175 | 33175 | 67341.9 | 3 | PROCESSED | 57539.0421759259 | 54695 | 54322.4919675926 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021307 | We propose a 2 month Suzaku monitoring program of 7 weekly 30ksec observations of the normal type 1 AGN, NGC5548. NGC5548 is uniquely well studied at all wavelengths, and will vary by a factor of 1.5, or more, at 97% probability. Variations of the Warm Absorber will determine its location in NGC5548, disciminating between models and determining the mass loss rate in the WA wind. This will provide a baseline data point for models of 'cosmological feedback' from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes or lack thereof in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, any broad Fe-K or high ionization edge. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ELVIS | MARTIN | NULL | NULL | USA | 2 | AO2 | NGC5548 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK | XIS | Y |
| NGC5548 | 214.4933 | 25.1285 | 31.9338138 | 70.49848107 | 305.6607 | 54289.4186921296 | 54290.1182175926 | 702042040 | 30699.6 | 30000 | 30699.6 | 30699.6 | 0 | 30699.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 28827.9 | 28827.9 | 60431.9 | 1 | PROCESSED | 57539.1330324074 | 54695 | 54328.4843402778 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021307 | We propose a 2 month Suzaku monitoring program of 7 weekly 30ksec observations of the normal type 1 AGN, NGC5548. NGC5548 is uniquely well studied at all wavelengths, and will vary by a factor of 1.5, or more, at 97% probability. Variations of the Warm Absorber will determine its location in NGC5548, disciminating between models and determining the mass loss rate in the WA wind. This will provide a baseline data point for models of 'cosmological feedback' from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes or lack thereof in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, any broad Fe-K or high ionization edge. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ELVIS | MARTIN | NULL | NULL | USA | 2 | AO2 | NGC5548 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK | XIS | Y |
| NGC5548 | 214.4959 | 25.1277 | 31.932758 | 70.49602002 | 293.6791 | 54296.5817013889 | 54297.4168865741 | 702042050 | 30019.7 | 30000 | 30027.7 | 30035.7 | 0 | 30019.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26300.4 | 26300.4 | 58971 | 1 | PROCESSED | 57539.274849537 | 54707 | 54340.3894328704 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021307 | We propose a 2 month Suzaku monitoring program of 7 weekly 30ksec observations of the normal type 1 AGN, NGC5548. NGC5548 is uniquely well studied at all wavelengths, and will vary by a factor of 1.5, or more, at 97% probability. Variations of the Warm Absorber will determine its location in NGC5548, disciminating between models and determining the mass loss rate in the WA wind. This will provide a baseline data point for models of 'cosmological feedback' from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes or lack thereof in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, any broad Fe-K or high ionization edge. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ELVIS | MARTIN | NULL | NULL | USA | 2 | AO2 | NGC5548 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK | XIS | Y |
| NGC5548 | 214.4955 | 25.1272 | 31.93108614 | 70.4962838 | 289.7815 | 54303.4447337963 | 54304.2711111111 | 702042060 | 28917.8 | 30000 | 28925.8 | 28925.8 | 0 | 28917.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 24818.1 | 24818.1 | 71383.9 | 1 | PROCESSED | 57539.29125 | 54706 | 54339.5363310185 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021307 | We propose a 2 month Suzaku monitoring program of 7 weekly 30ksec observations of the normal type 1 AGN, NGC5548. NGC5548 is uniquely well studied at all wavelengths, and will vary by a factor of 1.5, or more, at 97% probability. Variations of the Warm Absorber will determine its location in NGC5548, disciminating between models and determining the mass loss rate in the WA wind. This will provide a baseline data point for models of 'cosmological feedback' from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes or lack thereof in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, any broad Fe-K or high ionization edge. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ELVIS | MARTIN | NULL | NULL | USA | 2 | AO2 | NGC5548 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK | XIS | Y |
| NGC5548 | 214.4969 | 25.1266 | 31.93001973 | 70.4949274 | 285.8791 | 54310.1810648148 | 54311.0209953704 | 702042070 | 31809.9 | 30000 | 31809.9 | 31809.9 | 0 | 31809.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 29503 | 29503 | 72527.9 | 1 | PROCESSED | 57539.3547569444 | 54706 | 54339.4245486111 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021307 | We propose a 2 month Suzaku monitoring program of 7 weekly 30ksec observations of the normal type 1 AGN, NGC5548. NGC5548 is uniquely well studied at all wavelengths, and will vary by a factor of 1.5, or more, at 97% probability. Variations of the Warm Absorber will determine its location in NGC5548, disciminating between models and determining the mass loss rate in the WA wind. This will provide a baseline data point for models of 'cosmological feedback' from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes or lack thereof in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, any broad Fe-K or high ionization edge. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ELVIS | MARTIN | NULL | NULL | USA | 2 | AO2 | NGC5548 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK | XIS | Y |
| NGC5548 | 214.4979 | 25.1264 | 31.92993093 | 70.49400067 | 281.7605 | 54317.0262268518 | 54318.0211111111 | 702042080 | 38775.7 | 210000 | 38783.7 | 38791.7 | 0 | 38775.7 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 32649.7 | 32649.7 | 85951.9 | 0 | PROCESSED | 57539.4187037037 | 54714 | 54347.3528472222 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021307 | We propose a 2 month Suzaku monitoring program of 7 weekly 30ksec observations of the normal type 1 AGN, NGC5548. NGC5548 is uniquely well studied at all wavelengths, and will vary by a factor of 1.5, or more, at 97% probability. Variations of the Warm Absorber will determine its location in NGC5548, disciminating between models and determining the mass loss rate in the WA wind. This will provide a baseline data point for models of 'cosmological feedback' from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes or lack thereof in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, any broad Fe-K or high ionization edge. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ELVIS | MARTIN | NULL | NULL | USA | 2 | AO2 | NGC5548 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK | XIS | Y |
| FAIRALL 9 | 20.9481 | -58.8141 | 295.06951561 | -57.81752905 | 48.1772 | 54258.155462963 | 54260.5766666667 | 702043010 | 167798.3 | 164000 | 167798.3 | 167806.3 | 0 | 167814.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 136483.4 | 136483.4 | 209175.8 | 2 | PROCESSED | 57538.9238425926 | 54773 | 54265.5470717593 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021313 | Recently, deep observations of a number of Seyfert AGN with XMM-Newton and Suzaku have established variable and relativistic iron lines as robust features in roughly half of all deep Seyfert spectra. In these sources, the spin of the black hole can be constrained directly through fits to the relativistic iron line. A sample of excellent spectra from well-chosen AGN will facilitate a better understanding of the innermost regime near to black holes, and make correlations with parameters like radio luminosity, star formation rate, and galaxy and black hole mass possible for the first time. We propose to obtain observations of 4 under-exposed Seyfert AGN with promising evidence for broad lines to robustly constrain their spin parameters. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MILLER | JON | NULL | NULL | USA | 2 | AO2 | REVEALING BLACK HOLE SPIN IN RELATIVISTIC SEYFERT AGN | XIS | Y |
| MARKARIAN 79 | 115.6357 | 49.8015 | 168.6115046 | 28.38007803 | 283.4884 | 54193.9134953704 | 54195.7655439815 | 702044010 | 83703.8 | 82000 | 83711.8 | 83703.8 | 0 | 83711.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 82104.2 | 82104.2 | 160005.9 | 0 | PROCESSED | 57538.0894444444 | 54695 | 54203.4223842593 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021313 | Recently, deep observations of a number of Seyfert AGN with XMM-Newton and Suzaku have established variable and relativistic iron lines as robust features in roughly half of all deep Seyfert spectra. In these sources, the spin of the black hole can be constrained directly through fits to the relativistic iron line. A sample of excellent spectra from well-chosen AGN will facilitate a better understanding of the innermost regime near to black holes, and make correlations with parameters like radio luminosity, star formation rate, and galaxy and black hole mass possible for the first time. We propose to obtain observations of 4 under-exposed Seyfert AGN with promising evidence for broad lines to robustly constrain their spin parameters. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | MILLER | JON | NULL | NULL | USA | 2 | AO2 | REVEALING BLACK HOLE SPIN IN RELATIVISTIC SEYFERT AGN | XIS | Y |
| NGC 1365 | 53.3968 | -36.1347 | 237.94662462 | -54.6022242 | 221.6565 | 54486.2300578704 | 54490.0002083333 | 702047010 | 160505.7 | 150000 | 160505.7 | 160513.7 | 0 | 160513.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 146813.9 | 146813.9 | 325676.8 | 4 | PROCESSED | 57541.4786342593 | 54883 | 54515.5847800926 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021314 | We propose a 150 ksec observation of the Seyfert Galaxy NGC 1365. This galaxy have a unique set of properties: FeXXV and FeXXVI Kalpha and Kbeta absorption lines (the highest S/N detection so far among AGNs), rapidly varying cold absorber (nH variations of ~10^23/cm^2 in a few hours, changes from Compton-thick to Compton-thin in two days), a relativistic iron emission line. This new long observation will use at best the unique capabilities of Suzaku to constrain the dimensions of the absorbers, and, for the first time, will investigate the dynamics and physical conditions of the hot absorber responsible of the iron absorption lines. It is likely that an occultation will occur during the observation. This occultation would directly set the dimension of the X-ray source. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | RISALITI | GUIDO | NULL | NULL | USA | 2 | AO2 | BLACK HOLE OCCULTATION AND OUTFLOW VARIABILITY IN NGC 1365 | XIS | Y |
| NGC 4507 | 188.8987 | -39.9119 | 299.63576127 | 22.85843053 | 109.5879 | 54454.5145717593 | 54456.5835532407 | 702048010 | 103626 | 80000 | 103634 | 103626 | 0 | 103634 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 110902.1 | 110902.1 | 178727.9 | 0 | PROCESSED | 57540.963900463 | 54829 | 54462.288287037 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021331 | Recent X-ray observations of Seyfert 2 galaxies have shown that the distribution and ionization state of the circumnuclear material is more complex than the simple homogeneous torus predicted by AGN Unified Schemes. To investigate the nature of this material, high sensitivity is needed to detect relatively faint emission lines, while broad bandpass is required to constrain the primary X-ray continuum. We propose Suzaku observations (60 ksec each) of four local bright Compton-thin Seyfert2s, selected from the Swift/BAT survey with a hard X-ray flux exceeding 1e-10 cgs to form a flux-limited sample. The unprecedented broad bandpass of Suzaku offers a unique tool to investigate the X-ray emission, placing strong constraints on the geometry and location of the reprocessing matter. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | REEVES | JAMES | NULL | NULL | USA | 2 | AO2 | REVEALING THE REPROCESSING MATTER IN SEYFERT 2 GALAXIES | XIS | Y |
| NGC 6300 | 259.2549 | -62.8185 | 328.49505458 | -14.05378352 | 296.7285 | 54390.5141087963 | 54392.375162037 | 702049010 | 82577 | 80000 | 82577 | 82577 | 0 | 82577 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 105512.7 | 105512.7 | 160779.8 | 1 | PROCESSED | 57540.3276041667 | 54770 | 54403.3802083333 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021331 | Recent X-ray observations of Seyfert 2 galaxies have shown that the distribution and ionization state of the circumnuclear material is more complex than the simple homogeneous torus predicted by AGN Unified Schemes. To investigate the nature of this material, high sensitivity is needed to detect relatively faint emission lines, while broad bandpass is required to constrain the primary X-ray continuum. We propose Suzaku observations (60 ksec each) of four local bright Compton-thin Seyfert2s, selected from the Swift/BAT survey with a hard X-ray flux exceeding 1e-10 cgs to form a flux-limited sample. The unprecedented broad bandpass of Suzaku offers a unique tool to investigate the X-ray emission, placing strong constraints on the geometry and location of the reprocessing matter. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | REEVES | JAMES | NULL | NULL | USA | 2 | AO2 | REVEALING THE REPROCESSING MATTER IN SEYFERT 2 GALAXIES | XIS | Y |
| NGC7582 | 349.5472 | -42.3304 | 348.20905034 | -65.68466064 | 49.5845 | 54221.7937384259 | 54222.3176273148 | 702052010 | 23941.2 | 25000 | 23957.2 | 23941.2 | 0 | 23957.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21581.6 | 21581.6 | 45256 | 0 | PROCESSED | 57538.5368402778 | 54695 | 54228.073275463 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021332 | We propose to perform 4 Suzaku observations of 25 ks each (for a total of 100 ks) of the bright Seyfert 2 galaxy,NGC 7582.The aim of this proposal is to measure the distance of the gas that absorbs the nuclear radiation, by analyzing the pattern of variability of its column density.NGC7582 is the ideal target for this kind of analysis, because it already showed large variations of the column density of the absorber between X-ray observations taken a few years apart.With the present proposal, we intend to probe a wider range of timescales, from a week to about six months, in order to measure the distance of the absorber from the nucleus. This measure is crucial to understand the nature of the absorber in type 2 objects and the validity of the torus paradigm. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | CHIABERGE | MARCO | NULL | NULL | USA | 2 | AO2 | MEASURING THE DISTANCE OF THE ABSORBER IN NGC 7582 | HXD | Y |
| NGC7582 | 349.5634 | -42.322 | 348.21143031 | -65.69925686 | 64.738 | 54248.9237152778 | 54249.7328587963 | 702052020 | 28769 | 25000 | 28769 | 28769 | 0 | 28769 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 24682.4 | 24682.4 | 69905.9 | 0 | PROCESSED | 57538.7538541667 | 54695 | 54255.6928472222 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021332 | We propose to perform 4 Suzaku observations of 25 ks each (for a total of 100 ks) of the bright Seyfert 2 galaxy,NGC 7582.The aim of this proposal is to measure the distance of the gas that absorbs the nuclear radiation, by analyzing the pattern of variability of its column density.NGC7582 is the ideal target for this kind of analysis, because it already showed large variations of the column density of the absorber between X-ray observations taken a few years apart.With the present proposal, we intend to probe a wider range of timescales, from a week to about six months, in order to measure the distance of the absorber from the nucleus. This measure is crucial to understand the nature of the absorber in type 2 objects and the validity of the torus paradigm. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | CHIABERGE | MARCO | NULL | NULL | USA | 2 | AO2 | MEASURING THE DISTANCE OF THE ABSORBER IN NGC 7582 | HXD | Y |
| NGC7582 | 349.6446 | -42.4137 | 347.94526846 | -65.70277041 | 233.1822 | 54413.9093981482 | 54414.6459490741 | 702052030 | 29353.8 | 25000 | 29353.8 | 29353.8 | 0 | 29353.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 24433.1 | 24433.1 | 63631.9 | 1 | PROCESSED | 57540.4723842593 | 54790 | 54423.1929398148 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021332 | We propose to perform 4 Suzaku observations of 25 ks each (for a total of 100 ks) of the bright Seyfert 2 galaxy,NGC 7582.The aim of this proposal is to measure the distance of the gas that absorbs the nuclear radiation, by analyzing the pattern of variability of its column density.NGC7582 is the ideal target for this kind of analysis, because it already showed large variations of the column density of the absorber between X-ray observations taken a few years apart.With the present proposal, we intend to probe a wider range of timescales, from a week to about six months, in order to measure the distance of the absorber from the nucleus. This measure is crucial to understand the nature of the absorber in type 2 objects and the validity of the torus paradigm. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | CHIABERGE | MARCO | NULL | NULL | USA | 2 | AO2 | MEASURING THE DISTANCE OF THE ABSORBER IN NGC 7582 | HXD | Y |
| NGC7582 | 349.6411 | -42.4153 | 347.94523476 | -65.69973119 | 236.7954 | 54420.0722337963 | 54420.8960532407 | 702052040 | 31895.5 | 25000 | 31895.5 | 31895.5 | 0 | 31895.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25780.6 | 25780.6 | 71171.9 | 0 | PROCESSED | 57540.5407060185 | 54797 | 54430.3041203704 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021332 | We propose to perform 4 Suzaku observations of 25 ks each (for a total of 100 ks) of the bright Seyfert 2 galaxy,NGC 7582.The aim of this proposal is to measure the distance of the gas that absorbs the nuclear radiation, by analyzing the pattern of variability of its column density.NGC7582 is the ideal target for this kind of analysis, because it already showed large variations of the column density of the absorber between X-ray observations taken a few years apart.With the present proposal, we intend to probe a wider range of timescales, from a week to about six months, in order to measure the distance of the absorber from the nucleus. This measure is crucial to understand the nature of the absorber in type 2 objects and the validity of the torus paradigm. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | CHIABERGE | MARCO | NULL | NULL | USA | 2 | AO2 | MEASURING THE DISTANCE OF THE ABSORBER IN NGC 7582 | HXD | Y |
| PKS 1345+12 | 206.9131 | 12.3498 | 347.38894416 | 70.20282736 | 113.9421 | 54472.3082407407 | 54473.6799768518 | 702053010 | 52984.4 | 50000 | 52984.4 | 52984.4 | 0 | 52984.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45203.4 | 45203.4 | 118503.8 | 4 | PROCESSED | 57541.3141782407 | 54854 | 54483.4984375 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021341 | We wish to take advantage of the sensitivity of Suzaku above 10 keV to constrain the energy source -- starburst or black-hole driven activity -- in three of the brightest warm transitional ultraluminous infrared galaxies, PKS 1345+12, Mrk 463, and 3C 273. These objects are arguably the best local laboratories to study the basic physical processes involved in creating massive early type hosts on the one hand, and feeding embedded supermassive black holes on the other hand, in major galaxy mergers. The Suzaku data will be used to search for the high-energy signature of deeply buried active black holes and to look for short time scale variability, another signature of black-hole driven activity. These data will be combined with our A01 spectra and be part of S. Teng's PhD thesis at UMD. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | VEILLEUX | SYLVAIN | NULL | NULL | USA | 2 | AO2 | SPECTRA OF THE BRIGHTEST WARM ULTRALUMINOUS INFRARED GALAXIES | HXD | Y |
| 3C 445 | 335.9528 | -2.0995 | 61.86726076 | -46.70852053 | 68.9567 | 54245.2015046296 | 54248.9169444444 | 702056010 | 139769.1 | 125000 | 139769.1 | 139769.1 | 0 | 139769.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 117241.2 | 117241.2 | 320991.8 | 4 | PROCESSED | 57538.8276967593 | 54702 | 54256.717662037 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021352 | It is well known that the circum-black hole environ of Seyferts contain warm, photoionized gas responsible for complex absorption/emission at X-rays. Evidence for such components in radio-loud AGN is, instead, rare. And yet, presence of an ionized, scattering medium is postulated by unification models for these sources, and some models for jet formation. Here we tackle this problem by proposing sensitive Suzaku observations of 3C445, the only Broad-Line Radio Galaxy exhibiting soft X-ray emission lines from 0.4-3 keV in an archival EPIC spectrum. We will: 1) Determine the broad-band continuum; 2) Study the properties of the soft emission lines, determining the gas density and location, and thus its role in jet collimation; and 3) Confirm the strong reflection component suggested by EPIC. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | SAMBRUNA | RITA | NULL | NULL | USA | 2 | AO2 | WARM GAS IN THE INNER REGIONS OF RADIO-LOUD AGN: THE CASE OF 3C445 | XIS | Y |
| 4C+74.26 | 310.5668 | 75.0616 | 108.92036641 | 19.50581044 | 289.6922 | 54401.4314467593 | 54403.2606944444 | 702057010 | 91583 | 100000 | 91583 | 91583 | 0 | 91591 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 94114 | 94114 | 158029.8 | 1 | PROCESSED | 57540.3825925926 | 54776 | 54409.2446064815 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021354 | We propose a 100 ks observation of the bright broad-line radio galaxy 4C+74.26. A previous 35 ks XMM-Newton observation of 4C+74.26 yielded the first indication of a relativistically broadened Fe K line in a radio-loud AGN as well as other typical AGN properties (e.g., a warm absorber). The long observation proposed here will allow a detailed investigation of the Fe K line profile and improve significantly on the previous observation by detecting the associated Compton reflection hump with the HXD/PIN instrument. Modeling of these features will allow the first accurate determination of the geometry and structure of the inner accretion disk in a radio-loud AGN, and hence provide invaluable information for modeling the physics of the disk/jet interaction. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | BALLANTYNE | DAVID | NULL | NULL | USA | 2 | AO2 | A CLOSE LOOK AT 4C+74.26 WITH SUZAKU: FOCUSING IN ON THE DISK/JET INTERACTION | HXD | Y |
| NGC 1052 | 40.2309 | -8.2134 | 181.91154484 | -57.92833515 | 49.7745 | 54297.4313888889 | 54299.87875 | 702058010 | 100669.1 | 100000 | 100669.1 | 100669.1 | 0 | 100669.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 83499.8 | 83499.8 | 211427.8 | 2 | PROCESSED | 57539.327037037 | 54707 | 54339.9136458333 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021355 | Accretion onto supermassive black holes is thought to play a major role in the production of relativistic jets. Our understanding of jet production remains elusive, however, because we cannot image the accretion flow. Fortunately, the Fe K line offers a direct probe of accretion. As part of a multi-mission monitoring program of the radio loud AGN NGC 1052, we propose two 100 ksec Suzaku observations to obtain best-quality X-ray spectra at two epochs to determine the true continuum shape and thus probe the relativistic iron line, determine line and continuum variability patterns and possibly investigate how the structure of the accretion disk changes when there are jet ejection events. Our aim is to determine what leads supermassive black holes to launch powerful jets. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | WEAVER | KIMBERLY | NULL | NULL | USA | 2 | AO2 | PROBING THE DISK-JET CONNECTION IN AGN WITH AN INTENSIVE MULTIWAVELENGTH MONITORING CAMPAIGN OF NGC 1052 | HXD | Y |
| 3C 33 | 17.2445 | 13.2796 | 129.4936436 | -49.368548 | 249.2604 | 54460.3029282407 | 54463.6390509259 | 702059010 | 127367.7 | 100000 | 127375.7 | 127375.7 | 0 | 127367.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 106588.5 | 106588.5 | 288203.6 | 7 | PROCESSED | 57541.0545833333 | 54854 | 54483.4886458333 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021356 | We propose a 100 ks Suzaku observation of the nucleus of the nearby (z=0.0597) FRII radio galaxy 3C 33, to constrain the nature of its Compton reflection component, and make an accurate measurement of its Fe Ka emission line. 3C 33 (awarded category-C time in Suzaku AO-1, not observed) is the only radio-loud AGN with evidence of Compton reflection in its low-energy (< 10 keV) spectrum, and so offers a unique opportunity to study both the soft- and hard-band properties of reflection. The HXD will allow us, for the first time, to constrain the nature of the Compton reflection component in 3C 33 and, when combined with the superb sensitivity of the XIS, will enable us to determine the line-of-sight geometry and structure of the reflecting region. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | EVANS | DANIEL | NULL | NULL | USA | 2 | AO2 | CONSTRAINING THE REFLECTION PROPERTIES OF THE NARROW-LINE RADIO GALAXY 3C 33 | HXD | Y |
| Q1946+7658 | 296.1546 | 77.0965 | 109.22346589 | 23.50098326 | 3.7704 | 54294.4255902778 | 54294.6432175926 | 702060010 | 13163.6 | 13000 | 13163.6 | 13163.6 | 0 | 13163.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13928.2 | 13928.2 | 18775.9 | 0 | PROCESSED | 57539.2591782407 | 54706 | 54339.4067824074 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021361 | The main scientific goals of this Suzaku proposal are to: (a) Initiate an exploratory survey to identify high velocity outflows of X-ray absorbing material in NAL quasars. We will search for possible correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. (b) Test existing models of the nature of NAL quasars. (c) The detected X-ray brightest quasars from the proposed survey will be followed up with deeper Suzaku observations to constrain better the kinematic and ionization properties of the absorbers. Ultimately with these deeper observations we will constrain the mass outflow rates and outflow efficiencies of NAL quasars. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | CHARTAS | GEORGE | NULL | NULL | USA | 2 | AO2 | AN EXPLORATORY SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS | XIS | Y |
| Q0450-1310 | 73.3011 | -13.0912 | 211.74785299 | -32.06702416 | 263.6423 | 54535.8878240741 | 54536.2502314815 | 702062010 | 15510.2 | 13000 | 15510.2 | 15510.2 | 0 | 15510.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14988.7 | 14988.7 | 31305.9 | 0 | PROCESSED | 57541.8181828704 | 54916 | 54550.1640277778 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021361 | The main scientific goals of this Suzaku proposal are to: (a) Initiate an exploratory survey to identify high velocity outflows of X-ray absorbing material in NAL quasars. We will search for possible correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. (b) Test existing models of the nature of NAL quasars. (c) The detected X-ray brightest quasars from the proposed survey will be followed up with deeper Suzaku observations to constrain better the kinematic and ionization properties of the absorbers. Ultimately with these deeper observations we will constrain the mass outflow rates and outflow efficiencies of NAL quasars. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | CHARTAS | GEORGE | NULL | NULL | USA | 2 | AO2 | AN EXPLORATORY SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS | XIS | Y |
| Q1017+1055 | 155.041 | 10.671 | 230.36219873 | 50.83483368 | 121.1263 | 54431.9135185185 | 54432.4376851852 | 702064010 | 18048.6 | 20000 | 18048.6 | 18048.6 | 0 | 18048.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15031.6 | 15031.6 | 45281.9 | 0 | PROCESSED | 57540.6059606482 | 54805 | 54438.285150463 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021361 | The main scientific goals of this Suzaku proposal are to: (a) Initiate an exploratory survey to identify high velocity outflows of X-ray absorbing material in NAL quasars. We will search for possible correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. (b) Test existing models of the nature of NAL quasars. (c) The detected X-ray brightest quasars from the proposed survey will be followed up with deeper Suzaku observations to constrain better the kinematic and ionization properties of the absorbers. Ultimately with these deeper observations we will constrain the mass outflow rates and outflow efficiencies of NAL quasars. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | CHARTAS | GEORGE | NULL | NULL | USA | 2 | AO2 | AN EXPLORATORY SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS | XIS | Y |
| Q1334-0033 | 204.1954 | -0.819 | 326.07775276 | 59.99926461 | 306.9566 | 54295.3551736111 | 54295.7084953704 | 702067010 | 13962.1 | 15000 | 13962.1 | 13962.1 | 0 | 13962.1 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13006.4 | 13006.4 | 30519.9 | 0 | PROCESSED | 57539.262337963 | 54710 | 54340.4777430556 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021361 | The main scientific goals of this Suzaku proposal are to: (a) Initiate an exploratory survey to identify high velocity outflows of X-ray absorbing material in NAL quasars. We will search for possible correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. (b) Test existing models of the nature of NAL quasars. (c) The detected X-ray brightest quasars from the proposed survey will be followed up with deeper Suzaku observations to constrain better the kinematic and ionization properties of the absorbers. Ultimately with these deeper observations we will constrain the mass outflow rates and outflow efficiencies of NAL quasars. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | CHARTAS | GEORGE | NULL | NULL | USA | 2 | AO2 | AN EXPLORATORY SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS | XIS | Y |
| Q1548+0917 | 237.6002 | 9.1581 | 18.5566992 | 44.16075413 | 106.1242 | 54513.4560763889 | 54514.16 | 702068010 | 32113.3 | 23000 | 32121.3 | 32121.3 | 0 | 32113.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 29475.6 | 29475.6 | 60815.9 | 0 | PROCESSED | 57541.5745601852 | 54889 | 54522.1462731482 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021361 | The main scientific goals of this Suzaku proposal are to: (a) Initiate an exploratory survey to identify high velocity outflows of X-ray absorbing material in NAL quasars. We will search for possible correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. (b) Test existing models of the nature of NAL quasars. (c) The detected X-ray brightest quasars from the proposed survey will be followed up with deeper Suzaku observations to constrain better the kinematic and ionization properties of the absorbers. Ultimately with these deeper observations we will constrain the mass outflow rates and outflow efficiencies of NAL quasars. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | CHARTAS | GEORGE | NULL | NULL | USA | 2 | AO2 | AN EXPLORATORY SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS | XIS | Y |
| 3C 273 | 187.2559 | 1.9961 | 289.92713501 | 64.30042167 | 293.1671 | 54281.0022569444 | 54282.2661342593 | 702070010 | 54892.7 | 67000 | 54892.7 | 54892.7 | 0 | 54892.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51259.2 | 51259.2 | 109143.9 | 1 | PROCESSED | 57539.0801388889 | 54695 | 54322.4904166667 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021364 | We propose a Suzaku campaign on the bright z=0.158 quasar 3C 273. The source exhibits a Seyfert-like X-ray spectrum when the luminosity is low but is dominated by emission from the jet in a high state. Suzaku will be able to measure the broadband spectrum, especially X-ray reprocessed features, with greater sensitivity than ever before. Decoupling and monitoring of the disk and jet components will enable detailed spectroscopy to help understand the disk-jet connection and the wider implications for AGN physics in general. The target is bright and well-suited because for most AGN either the disk or jet component dominates. For this pilot study we propose two 50 ks observations, one in each visibility window. The science goals cannot be achieved with existing data or other missions. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | YAQOOB | TAHIR | NULL | NULL | USA | 2 | AO2 | EXPLORING THE ACCRETION DISK AND JET CONNECTION IN 3C 273 WITH SUZAKU | HXD | Y |
| 3C 452 | 341.4131 | 39.7498 | 98.13461856 | -16.98917572 | 65.3539 | 54267.3964351852 | 54268.8294444444 | 702073010 | 66680 | 53000 | 66696 | 66680 | 0 | 66696 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 61448.7 | 61448.7 | 123801.8 | 3 | PROCESSED | 57538.9941550926 | 54695 | 54319.4923032407 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021372 | The nature and even the existence of type II quasars is highly controversial. Due to their highly obscured nature, very hard (> 15 keV) observations are needed to probe their properties. With the 9-month SWIFT BAT all-sky AGN survey, detection of heavily obscured sources is now possible. Indeed, 6 type II quasars have been identified. Their properties, however, are a challenge to standard AGN models e.g., all but one of these sources are strong radio sources and several have optical spectra indicative of an un-absorbed source. We propose Suzaku observations of the 5 without broadband high signal to noise x-ray data to perform a detailed analysis of their x-ray properties and to understand their relationship to the lower luminosity well studied Seyfert IIs. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | MUSHOTZKY | RICHARD | NULL | NULL | USA | 2 | AO2 | SUZAKU OBSERVATIONS OF SWIFT BAT TYPE II QUASARS | HXD | Y |
| 3C 105 | 61.8399 | 3.6518 | 187.66746701 | -33.63397375 | 251.3728 | 54501.5363078704 | 54503.0833912037 | 702074010 | 38319 | 53000 | 38319 | 38319 | 0 | 38319 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48881.1 | 48881.1 | 133655.8 | 2 | PROCESSED | 57541.5364351852 | 54883 | 54515.7678819444 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021372 | The nature and even the existence of type II quasars is highly controversial. Due to their highly obscured nature, very hard (> 15 keV) observations are needed to probe their properties. With the 9-month SWIFT BAT all-sky AGN survey, detection of heavily obscured sources is now possible. Indeed, 6 type II quasars have been identified. Their properties, however, are a challenge to standard AGN models e.g., all but one of these sources are strong radio sources and several have optical spectra indicative of an un-absorbed source. We propose Suzaku observations of the 5 without broadband high signal to noise x-ray data to perform a detailed analysis of their x-ray properties and to understand their relationship to the lower luminosity well studied Seyfert IIs. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | MUSHOTZKY | RICHARD | NULL | NULL | USA | 2 | AO2 | SUZAKU OBSERVATIONS OF SWIFT BAT TYPE II QUASARS | HXD | Y |
| SWIFT J0318.7+6828 | 49.4315 | 68.5395 | 135.6962435 | 9.37350025 | 42.3301 | 54365.4488078704 | 54367.125162037 | 702075010 | 77115.6 | 53000 | 77139.6 | 77115.6 | 0 | 77139.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70685.5 | 70685.5 | 144797.8 | 1 | PROCESSED | 57540.0779513889 | 54770 | 54403.1984490741 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021372 | The nature and even the existence of type II quasars is highly controversial. Due to their highly obscured nature, very hard (> 15 keV) observations are needed to probe their properties. With the 9-month SWIFT BAT all-sky AGN survey, detection of heavily obscured sources is now possible. Indeed, 6 type II quasars have been identified. Their properties, however, are a challenge to standard AGN models e.g., all but one of these sources are strong radio sources and several have optical spectra indicative of an un-absorbed source. We propose Suzaku observations of the 5 without broadband high signal to noise x-ray data to perform a detailed analysis of their x-ray properties and to understand their relationship to the lower luminosity well studied Seyfert IIs. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | MUSHOTZKY | RICHARD | NULL | NULL | USA | 2 | AO2 | SUZAKU OBSERVATIONS OF SWIFT BAT TYPE II QUASARS | HXD | Y |
| SWIFT J0918.5+0425 | 139.5114 | 4.476 | 227.10001498 | 34.41934616 | 102.3204 | 54408.8894097222 | 54410.2293981482 | 702076010 | 61018.5 | 53000 | 61018.5 | 61040.1 | 0 | 61018.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 56156.5 | 56156.5 | 115765.9 | 2 | PROCESSED | 57540.4472916667 | 54787 | 54419.0312847222 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021372 | The nature and even the existence of type II quasars is highly controversial. Due to their highly obscured nature, very hard (> 15 keV) observations are needed to probe their properties. With the 9-month SWIFT BAT all-sky AGN survey, detection of heavily obscured sources is now possible. Indeed, 6 type II quasars have been identified. Their properties, however, are a challenge to standard AGN models e.g., all but one of these sources are strong radio sources and several have optical spectra indicative of an un-absorbed source. We propose Suzaku observations of the 5 without broadband high signal to noise x-ray data to perform a detailed analysis of their x-ray properties and to understand their relationship to the lower luminosity well studied Seyfert IIs. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | MUSHOTZKY | RICHARD | NULL | NULL | USA | 2 | AO2 | SUZAKU OBSERVATIONS OF SWIFT BAT TYPE II QUASARS | HXD | Y |
| MRK 417 | 162.3659 | 22.9016 | 214.84390845 | 62.11471123 | 281.9359 | 54238.6593402778 | 54239.5730555556 | 702078010 | 41506.6 | 40000 | 41506.6 | 41506.6 | 0 | 41506.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39338.5 | 39338.5 | 78923.9 | 0 | PROCESSED | 57538.6952662037 | 54695 | 54245.0002430556 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021374 | Though Compton thick AGN are expected to constitute a sizable fraction of the Seyfert population (Maiolino et al 1998 and Risaliti et al 1999), the fraction and the signatures of Compton thick AGN is unknown. The SWIFT BAT all-sky AGN survey has detected a complete sample of AGN with flux > 1-3e-11 erg/cm^2/s in the 15-200 keV band. At this energy range, the effects of heavy obscuration are minimal and thus BAT will allow us to determine the true fraction of Compton-thick sources. However, the BAT spectra are not simultaneous with XRT and XRT does not have the spectral resolution (with 10 ks) necessary to characterize a heavily absorbed 0.3-10 keV spectrum. We propose HXD nominal Suzaku observations of 4 possible Compton thick sources for which we recently obtained XMM 10 ks follow-ups. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | MUSHOTZKY | RICHARD | NULL | NULL | USA | 2 | AO2 | SUZAKU OBSERVATIONS OF POSSIBLY COMPTON THICK AGN FROM THE SWIFT BAT SURVEY | HXD | Y |
| NGC 1142 | 43.7827 | -0.1295 | 175.79604248 | -49.86350093 | 73.9096 | 54302.4506481482 | 54303.4308333333 | 702079010 | 40569.7 | 40000 | 40569.7 | 40569.7 | 0 | 40569.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36540.4 | 36540.4 | 84679.9 | 1 | PROCESSED | 57539.2980902778 | 54706 | 54339.1106828704 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021374 | Though Compton thick AGN are expected to constitute a sizable fraction of the Seyfert population (Maiolino et al 1998 and Risaliti et al 1999), the fraction and the signatures of Compton thick AGN is unknown. The SWIFT BAT all-sky AGN survey has detected a complete sample of AGN with flux > 1-3e-11 erg/cm^2/s in the 15-200 keV band. At this energy range, the effects of heavy obscuration are minimal and thus BAT will allow us to determine the true fraction of Compton-thick sources. However, the BAT spectra are not simultaneous with XRT and XRT does not have the spectral resolution (with 10 ks) necessary to characterize a heavily absorbed 0.3-10 keV spectrum. We propose HXD nominal Suzaku observations of 4 possible Compton thick sources for which we recently obtained XMM 10 ks follow-ups. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | MUSHOTZKY | RICHARD | NULL | NULL | USA | 2 | AO2 | SUZAKU OBSERVATIONS OF POSSIBLY COMPTON THICK AGN FROM THE SWIFT BAT SURVEY | HXD | Y |
| ESO 506-G027 | 189.6943 | -27.3584 | 299.48164005 | 35.42851647 | 302.0467 | 54314.0460300926 | 54315.2572222222 | 702080010 | 41745.3 | 40000 | 41753.3 | 41761.3 | 0 | 41745.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 38282.8 | 38282.8 | 104639.9 | 2 | PROCESSED | 57539.3906134259 | 54710 | 54340.5553125 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021374 | Though Compton thick AGN are expected to constitute a sizable fraction of the Seyfert population (Maiolino et al 1998 and Risaliti et al 1999), the fraction and the signatures of Compton thick AGN is unknown. The SWIFT BAT all-sky AGN survey has detected a complete sample of AGN with flux > 1-3e-11 erg/cm^2/s in the 15-200 keV band. At this energy range, the effects of heavy obscuration are minimal and thus BAT will allow us to determine the true fraction of Compton-thick sources. However, the BAT spectra are not simultaneous with XRT and XRT does not have the spectral resolution (with 10 ks) necessary to characterize a heavily absorbed 0.3-10 keV spectrum. We propose HXD nominal Suzaku observations of 4 possible Compton thick sources for which we recently obtained XMM 10 ks follow-ups. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | MUSHOTZKY | RICHARD | NULL | NULL | USA | 2 | AO2 | SUZAKU OBSERVATIONS OF POSSIBLY COMPTON THICK AGN FROM THE SWIFT BAT SURVEY | HXD | Y |
| MCG +04-48-002 | 307.1488 | 25.8021 | 67.06317106 | -7.53431612 | 93.9583 | 54208.4668634259 | 54209.4134143518 | 702081010 | 41298.8 | 40000 | 41306.8 | 41298.8 | 0 | 41306.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37746.6 | 37746.6 | 81769.9 | 2 | PROCESSED | 57538.398275463 | 54695 | 54217.0231712963 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021374 | Though Compton thick AGN are expected to constitute a sizable fraction of the Seyfert population (Maiolino et al 1998 and Risaliti et al 1999), the fraction and the signatures of Compton thick AGN is unknown. The SWIFT BAT all-sky AGN survey has detected a complete sample of AGN with flux > 1-3e-11 erg/cm^2/s in the 15-200 keV band. At this energy range, the effects of heavy obscuration are minimal and thus BAT will allow us to determine the true fraction of Compton-thick sources. However, the BAT spectra are not simultaneous with XRT and XRT does not have the spectral resolution (with 10 ks) necessary to characterize a heavily absorbed 0.3-10 keV spectrum. We propose HXD nominal Suzaku observations of 4 possible Compton thick sources for which we recently obtained XMM 10 ks follow-ups. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | MUSHOTZKY | RICHARD | NULL | NULL | USA | 2 | AO2 | SUZAKU OBSERVATIONS OF POSSIBLY COMPTON THICK AGN FROM THE SWIFT BAT SURVEY | HXD | Y |
| XBONGBLUE1 | 217.1061 | 32.8569 | 54.10325006 | 68.28811801 | 132.8525 | 54453.8528587963 | 54454.166875 | 702082010 | 15172.5 | 13000 | 15172.5 | 15172.5 | 0 | 15172.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15699.6 | 15699.6 | 27125.9 | 0 | PROCESSED | 57540.9008217593 | 54828 | 54461.0450231482 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021376 | We propose to use Suzaku's large collecting area and excellent energy response to measure accurate X-ray spectra for 9 XBONGs and 8 luminous Type 2 AGN selected from very large samples of identified XBONGs and Type 2 AGN found in our Chandra XBootes survey. We have obtained optical spectra for 258 XBONGs and identified ~700 X-ray luminous Type 2 AGN at z>0.7. With known source positions and X-ray fluxes, we select sources that are relatively bright with little or no contamination from other X-ray sources. Thus we will measure individual spectra for these bright sources. We propose eight 15 ksec Suzaku XIS observations to measure the absorption in 8 luminous z > 0.8 Type 2 AGN and eight 10 ksec observations to measure the absorption and iron emission for nine XBONGs. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | JONES | CHRISTINE | NULL | NULL | USA | 2 | AO2 | OBSCURED AGN AND XBONGS IN BOOTES | XIS | Y |
| XBONGBLUE2 | 217.7653 | 34.3413 | 57.71878971 | 67.47993323 | 130.3787 | 54454.1686921296 | 54454.5050694445 | 702084010 | 14816.2 | 13000 | 14816.2 | 14816.2 | 0 | 14816.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 14579.4 | 14579.4 | 29055.9 | 0 | PROCESSED | 57540.9126851852 | 54828 | 54460.6654398148 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021376 | We propose to use Suzaku's large collecting area and excellent energy response to measure accurate X-ray spectra for 9 XBONGs and 8 luminous Type 2 AGN selected from very large samples of identified XBONGs and Type 2 AGN found in our Chandra XBootes survey. We have obtained optical spectra for 258 XBONGs and identified ~700 X-ray luminous Type 2 AGN at z>0.7. With known source positions and X-ray fluxes, we select sources that are relatively bright with little or no contamination from other X-ray sources. Thus we will measure individual spectra for these bright sources. We propose eight 15 ksec Suzaku XIS observations to measure the absorption in 8 luminous z > 0.8 Type 2 AGN and eight 10 ksec observations to measure the absorption and iron emission for nine XBONGs. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | JONES | CHRISTINE | NULL | NULL | USA | 2 | AO2 | OBSCURED AGN AND XBONGS IN BOOTES | XIS | Y |
| TYPE2AGN | 216.4026 | 35.2819 | 60.85487771 | 68.34395808 | 307.3753 | 54292.1781712963 | 54292.6183333333 | 702090010 | 19838.7 | 19000 | 19846.7 | 19854.7 | 0 | 19838.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20870 | 20870 | 38015.9 | 0 | PROCESSED | 57539.1533912037 | 54706 | 54339.0120833333 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021376 | We propose to use Suzaku's large collecting area and excellent energy response to measure accurate X-ray spectra for 9 XBONGs and 8 luminous Type 2 AGN selected from very large samples of identified XBONGs and Type 2 AGN found in our Chandra XBootes survey. We have obtained optical spectra for 258 XBONGs and identified ~700 X-ray luminous Type 2 AGN at z>0.7. With known source positions and X-ray fluxes, we select sources that are relatively bright with little or no contamination from other X-ray sources. Thus we will measure individual spectra for these bright sources. We propose eight 15 ksec Suzaku XIS observations to measure the absorption in 8 luminous z > 0.8 Type 2 AGN and eight 10 ksec observations to measure the absorption and iron emission for nine XBONGs. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | JONES | CHRISTINE | NULL | NULL | USA | 2 | AO2 | OBSCURED AGN AND XBONGS IN BOOTES | XIS | Y |
| PHOENIX GALAXY | 120.9921 | 5.0644 | 216.72692126 | 18.43029643 | 304.6737 | 54222.3296296296 | 54223.9585069445 | 702111010 | 58867.7 | 50000 | 58867.7 | 58867.7 | 0 | 58867.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 49697.8 | 49697.8 | 140723.9 | 5 | PROCESSED | 57538.5788078704 | 54744 | 54230.3771527778 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 022002 | We propose a 50 ks Suzaku observation of the Seyfert galaxy UGC4203 (a.k.a. Mrk 1210), the ``Phoenix Galaxy''. It is one of the sources which have been discovered to change from Compton-thin to reflection-dominated states. The aim of the proposal is to understand the origin of this variation (i.e. as either due to flux or to NH variations) by measuring its column density and compare it to previous observations. Suzaku is unique for this task, because thanks to its broad band it may probe column densities up to several times 10^24 cm^-2 in this source, which has never been observed above 10 keV. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | MATT | GIORGIO | NULL | NULL | EUR | 2 | AO2 | THE NATURE OF THE VARIATIONS OF STATE IN THE PHOENIX GALAXY | HXD | Y |
| MCG+8-11-11 | 88.7233 | 46.5039 | 165.67352488 | 10.43795472 | 91.6485 | 54360.0736342593 | 54362.2640509259 | 702112010 | 98748.1 | 100000 | 98748.1 | 98756.1 | 0 | 98764.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 89213.8 | 89213.8 | 186438.7 | 1 | PROCESSED | 57540.0368055556 | 54751 | 54371.4963078704 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 022004 | We propose to observe with Suzaku for 100 ks one of the X-ray brightest AGN, the Seyfert 1 galaxy MCG+8-11-11, with the aim to measure the fraction of the reflection component and the iron abundance. Suzaku provides a unique opportunity to perform this kind of analysis, thanks to its broadband coverage. Moreover, the proposed observation will provide an extremely good spectrum, which will allow us to measure the iron line width, its Compton Shoulder and the ionization stage of iron. These three measurements will contribute to provide useful information on the nature of the iron line emitting material, its distance from the central Black Hole and the mass of the latter. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | BIANCHI | STEFANO | NULL | NULL | EUR | 2 | AO2 | MCG+8-11-11: A BROADBAND SPECTRUM OF ONE OF THE X-RAY BRIGHTEST AGN | HXD | Y |
| IC4329A | 207.3319 | -30.3107 | 317.49747069 | 30.91844112 | 292.4395 | 54313.2280092593 | 54314.0419444444 | 702113010 | 25453.4 | 25000 | 25453.4 | 25453.4 | 0 | 25453.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21442.2 | 21442.2 | 70292 | 1 | PROCESSED | 57539.3768287037 | 54710 | 54340.5826273148 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 022009 | IC 4329A is the brightest known Seyfert 1 galaxy between ~2-30 keV (F(2-10 keV)~1-2e-10 erg/cm2s). With its clear warm absorber and reflection component, it is often taken as the prototypical Sey 1 galaxy. Its X-ray variability is strong enough (and on a sufficiently long time scale, ideal for Suzaku) to make multiple observations critical for probing the origin of the Compton reflection component, and to attempt measuring variations of the high energy cut-off. We thus propose 5x20 ks observations to monitor i) the correlated variability of the reflection continuum plus FeK line to primary continuum variations, and ii) the variations in the high-E cut-off, and their relation with the power-law, and iii) check the evidence for a blueshifted (v~0.1c) FeK absorption line at ~7.7 keV. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | CAPPI | MASSIMO | NULL | NULL | EUR | 2 | AO2 | SUZAKU MULTIPLE OBSERVATIONS OF IC4329A TO PROBE THE ORIGIN OF THE COMPTON REFLECTION COMPONENT AND HIGH-ENERGY CUT-OFF | XIS | Y |
| IC4329A | 207.3329 | -30.3099 | 317.49868436 | 30.91898994 | 293.8517 | 54318.0289930556 | 54318.8786226852 | 702113020 | 30623.3 | 25000 | 30623.3 | 30623.3 | 0 | 30623.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25746.1 | 25746.1 | 73384 | 3 | PROCESSED | 57539.4343287037 | 54730 | 54347.5971180556 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 022009 | IC 4329A is the brightest known Seyfert 1 galaxy between ~2-30 keV (F(2-10 keV)~1-2e-10 erg/cm2s). With its clear warm absorber and reflection component, it is often taken as the prototypical Sey 1 galaxy. Its X-ray variability is strong enough (and on a sufficiently long time scale, ideal for Suzaku) to make multiple observations critical for probing the origin of the Compton reflection component, and to attempt measuring variations of the high energy cut-off. We thus propose 5x20 ks observations to monitor i) the correlated variability of the reflection continuum plus FeK line to primary continuum variations, and ii) the variations in the high-E cut-off, and their relation with the power-law, and iii) check the evidence for a blueshifted (v~0.1c) FeK absorption line at ~7.7 keV. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | CAPPI | MASSIMO | NULL | NULL | EUR | 2 | AO2 | SUZAKU MULTIPLE OBSERVATIONS OF IC4329A TO PROBE THE ORIGIN OF THE COMPTON REFLECTION COMPONENT AND HIGH-ENERGY CUT-OFF | XIS | Y |
| IC4329A | 207.3319 | -30.3116 | 317.49719871 | 30.9175719 | 295.4804 | 54323.458599537 | 54324.2127777778 | 702113030 | 26895.9 | 25000 | 26895.9 | 26895.9 | 0 | 26895.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 23872.3 | 23872.3 | 65130.9 | 0 | PROCESSED | 57539.4615972222 | 54730 | 54347.7226041667 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 022009 | IC 4329A is the brightest known Seyfert 1 galaxy between ~2-30 keV (F(2-10 keV)~1-2e-10 erg/cm2s). With its clear warm absorber and reflection component, it is often taken as the prototypical Sey 1 galaxy. Its X-ray variability is strong enough (and on a sufficiently long time scale, ideal for Suzaku) to make multiple observations critical for probing the origin of the Compton reflection component, and to attempt measuring variations of the high energy cut-off. We thus propose 5x20 ks observations to monitor i) the correlated variability of the reflection continuum plus FeK line to primary continuum variations, and ii) the variations in the high-E cut-off, and their relation with the power-law, and iii) check the evidence for a blueshifted (v~0.1c) FeK absorption line at ~7.7 keV. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | CAPPI | MASSIMO | NULL | NULL | EUR | 2 | AO2 | SUZAKU MULTIPLE OBSERVATIONS OF IC4329A TO PROBE THE ORIGIN OF THE COMPTON REFLECTION COMPONENT AND HIGH-ENERGY CUT-OFF | XIS | Y |
| IC4329A | 207.3317 | -30.3084 | 317.49797139 | 30.92070724 | 297.0437 | 54328.4922106482 | 54329.1612731482 | 702113040 | 24219.4 | 25000 | 24219.4 | 24219.4 | 0 | 24219.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20203.1 | 20203.1 | 57800 | 1 | PROCESSED | 57539.604537037 | 54730 | 54351.1843171296 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 022009 | IC 4329A is the brightest known Seyfert 1 galaxy between ~2-30 keV (F(2-10 keV)~1-2e-10 erg/cm2s). With its clear warm absorber and reflection component, it is often taken as the prototypical Sey 1 galaxy. Its X-ray variability is strong enough (and on a sufficiently long time scale, ideal for Suzaku) to make multiple observations critical for probing the origin of the Compton reflection component, and to attempt measuring variations of the high energy cut-off. We thus propose 5x20 ks observations to monitor i) the correlated variability of the reflection continuum plus FeK line to primary continuum variations, and ii) the variations in the high-E cut-off, and their relation with the power-law, and iii) check the evidence for a blueshifted (v~0.1c) FeK absorption line at ~7.7 keV. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | CAPPI | MASSIMO | NULL | NULL | EUR | 2 | AO2 | SUZAKU MULTIPLE OBSERVATIONS OF IC4329A TO PROBE THE ORIGIN OF THE COMPTON REFLECTION COMPONENT AND HIGH-ENERGY CUT-OFF | XIS | Y |
| IC4329A | 207.3321 | -30.3098 | 317.49793706 | 30.91926559 | 298.5047 | 54332.9765740741 | 54333.5558333333 | 702113050 | 24026.2 | 25000 | 24026.2 | 24026.2 | 0 | 24026.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18825.6 | 18825.6 | 50043.9 | 1 | PROCESSED | 57539.6252083333 | 54730 | 54350.649375 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 022009 | IC 4329A is the brightest known Seyfert 1 galaxy between ~2-30 keV (F(2-10 keV)~1-2e-10 erg/cm2s). With its clear warm absorber and reflection component, it is often taken as the prototypical Sey 1 galaxy. Its X-ray variability is strong enough (and on a sufficiently long time scale, ideal for Suzaku) to make multiple observations critical for probing the origin of the Compton reflection component, and to attempt measuring variations of the high energy cut-off. We thus propose 5x20 ks observations to monitor i) the correlated variability of the reflection continuum plus FeK line to primary continuum variations, and ii) the variations in the high-E cut-off, and their relation with the power-law, and iii) check the evidence for a blueshifted (v~0.1c) FeK absorption line at ~7.7 keV. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | CAPPI | MASSIMO | NULL | NULL | EUR | 2 | AO2 | SUZAKU MULTIPLE OBSERVATIONS OF IC4329A TO PROBE THE ORIGIN OF THE COMPTON REFLECTION COMPONENT AND HIGH-ENERGY CUT-OFF | XIS | Y |
| RBS 1124 | 187.6975 | 70.7093 | 125.39855918 | 46.31993489 | 339.073 | 54204.9538078704 | 54206.5786921296 | 702114010 | 86228.4 | 88000 | 86228.4 | 86228.4 | 0 | 86228.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 88855.5 | 88855.5 | 140384 | 3 | PROCESSED | 57538.4340740741 | 54744 | 54210.6501851852 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 022019 | We propose a 70 ks observation of RBS 1124 (z=0.208). This is the X--ray brightest radio--quiet quasar (> 4e45 erg/s in the 2-10 keV band) from the ROSAT bright source catalogue. The expected number of counts (e.g. about 120,000 in just one FI XIS unit and about 11,000 in the HXD/PIN) will provide the best quality X-ray spectrum so far for such a high luminosity AGN. We will investigate the main X-ray spectral components shedding light on this extreme class of objects with unprecedented accuracy making full use of the Suzaku sensitivity across the whole band (XIS and HXD). | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MINIUTTI | GIOVANNI | NULL | NULL | EUR | 2 | AO2 | REVEALING THE X-RAY EMISSION/ACCRETION PROCESSES IN THE VERY LUMINOUS RADIO-QUIET AND X-RAY BRIGHT QUASAR RBS 1124 | HXD | Y |
| IRAS 10565+2448 | 164.8573 | 24.5988 | 212.34078465 | 64.72788111 | 119.4619 | 54410.6325 | 54411.4675347222 | 702115010 | 39423.2 | 30000 | 39423.2 | 39423.2 | 0 | 39423.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35738.8 | 35738.8 | 72145.9 | 0 | PROCESSED | 57540.4702893518 | 54791 | 54423.1618518518 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 022023 | We propose for 30ks Suzaku observations of two ultra-luminous infrared galaxies that lack sensitive 2keV constraints to provide a complete census of Active Galactic Nuclei (AGN) activity in ULIRGs out to 200Mpc. Six (~75%) of the eight ULIRGs in our sample for which we already have sensitive >2keV constraints host AGN activity, indicating that black-hole growth is ubiqitious in the most luminous local galaxies. Our proposed observations are sensitive enough to identify luminous AGN activity (L_X=3x10^{43} erg/s) out to ~40keV, to accurately quantify the properties of less luminous AGN activity, and to identify and quantify the star-formation activity. In addition the results will be used to better understand the z~2 ULIRG population, the likely progenitors of todays massive galaxies. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | ALEXANDER | DAVID | NULL | NULL | EUR | 2 | AO2 | A COMPLETE CENSUS OF AGN ACTIVITY IN ULTRA-LUMINOUS GALAXIES OUT TO 200 MPC | HXD | Y |
| AKN 564 | 340.6246 | 29.7785 | 92.13720271 | -25.27363853 | 56.6178 | 54277.5375694444 | 54279.8002199074 | 702117010 | 99978.1 | 100000 | 99986.1 | 99986.1 | 0 | 99978.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 87225.3 | 87225.3 | 195473.9 | 1 | PROCESSED | 57539.0843518518 | 54703 | 54333.5152199074 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 022024 | Narrow Line Seyfert 1 galaxies show complex X-ray behaviour. At low flux levels their 2-10~keV spectra are hard, with a huge excess at lower energies. Conversely, at high fluxes, the same objects show a soft 2-10 keV spectrum, with moderate soft excess. This behaviour can be explained either by reflection or absorption models. It is important to distinguish between these scenarios as they imply critical differences in the inferred physics of the accretion flow. There is already good Suzaku data on the hard 2-10 keV spectra from a GT observation of NGC4051. We propose to compare this with 100ks of data from Akn564, the brightest NLS1 at 10keV having a soft 2-10keV spectrum, so as to use the full range of spectral behaviour seen in NLS1's to determine the origin of the soft excess. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | DONE | CHRIS | NULL | NULL | EUR | 2 | AO2 | UNDERSTANDING THE ORIGIN OF SPECTRAL COMPLEXITY IN NLS1: AKN564 | HXD | Y |
| IRAS18325-5926 | 279.2243 | -59.4565 | 335.92469241 | -21.3483138 | 281.9669 | 54399.3814699074 | 54401.4169444444 | 702118010 | 78434.8 | 80000 | 78434.8 | 78442.8 | 0 | 78442.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 74291.7 | 74291.7 | 175835.7 | 0 | PROCESSED | 57540.4011458333 | 54777 | 54409.305474537 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 022025 | We propose a 80 ks observation of the Seyfert galaxy IRAS 18325-5926. Previous observations show evidence for reflection from highly ionized matter, absorption features in the 8-10 keV band, and a possible roll-over of the continuum spectrum at around 30 keV. The observation goal is to elucidate the continuum roll-over and to investigate variability of the spectral features, which would have many important implications for the physical condition and the geometry of the accretion disc and the illuminating source. This study will provide crucial keys to understand the geometry of primary X-ray source and immediate surroundings. The broad-band coverage and the high sensitivity at the hard X-ray band provided by Suzaku are ideally suited to study this unique AGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | MISAKI | KAZUTAMI | NULL | NULL | EUR | 2 | AO2 | HARD X-RAY SPECTRUM OF IRAS 18325-5926: REFLECTION FROM AN IONIZED DISC AND CONTINUUM ROLL-OVER | HXD | Y |
| ESO 323-G032 | 193.3499 | -41.5832 | 303.32560645 | 21.28704922 | 104.5857 | 54456.5856481482 | 54458.1459953704 | 702119010 | 79249.4 | 80000 | 80817.8 | 79249.4 | 0 | 80801.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 86896.7 | 86896.7 | 134777.8 | 1 | PROCESSED | 57540.9568055556 | 54854 | 54483.1116203704 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 022033 | The high-energy detectors onboard Swift and INTEGRAL are mapping the hard (>10 keV) X-ray sky. Although limited to bright X-ray fluxes (~1e-11 erg/cm2/s), the large area surveyed so far has allowed to build up sizable samples of hard X-ray selected AGN almost unbiased against X-ray absorption. On the basis of a careful analysis of the available X-ray observations below 10 keV, we identified a sample of relatively bright AGN which are likely to be obscured by Compton-thick (logN_H >24) cold gas. Two of them were observed in EAO-1 and the results confirmed our predictions. We propose further Suzaku observations of 3 bright objects (F(20-40 keV) ~ 0.7-1.4 x 1e-11 erg/cm2/s) which will allow us to unveil previously unknown nearby heavily obscured AGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | COMASTRI | ANDREA | NULL | NULL | EUR | 2 | AO2 | BRIGHT COMPTON-THICK GALAXIES IN THE BACKYARD - PART II | HXD | Y |
| ESO 263-G013 | 152.4256 | -42.8603 | 273.99206854 | 10.74227458 | 292.0779 | 54252.4568287037 | 54253.5946064815 | 702120010 | 45294.7 | 40000 | 45302.7 | 45302.7 | 0 | 45294.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40103.5 | 40103.5 | 98299.9 | 2 | PROCESSED | 57538.8009143518 | 54745 | 54258.5006134259 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 022033 | The high-energy detectors onboard Swift and INTEGRAL are mapping the hard (>10 keV) X-ray sky. Although limited to bright X-ray fluxes (~1e-11 erg/cm2/s), the large area surveyed so far has allowed to build up sizable samples of hard X-ray selected AGN almost unbiased against X-ray absorption. On the basis of a careful analysis of the available X-ray observations below 10 keV, we identified a sample of relatively bright AGN which are likely to be obscured by Compton-thick (logN_H >24) cold gas. Two of them were observed in EAO-1 and the results confirmed our predictions. We propose further Suzaku observations of 3 bright objects (F(20-40 keV) ~ 0.7-1.4 x 1e-11 erg/cm2/s) which will allow us to unveil previously unknown nearby heavily obscured AGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | COMASTRI | ANDREA | NULL | NULL | EUR | 2 | AO2 | BRIGHT COMPTON-THICK GALAXIES IN THE BACKYARD - PART II | HXD | Y |
| SWIFT J2127.4+5654 | 322.001 | 56.878 | 97.78160785 | 4.29621592 | 243.6186 | 54443.0645023148 | 54445.0487962963 | 702122010 | 91730.4 | 88000 | 0 | 91730.4 | 0 | 91730.4 | 0 | 2 | 0 | 2 | 1 | 0 | 0 | 89348.5 | 89348.5 | 171379.9 | 2 | PROCESSED | 57540.867974537 | 55000 | 54633.7130439815 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 022034 | We propose to observe with Suzaku two Narrow Line Seyfert 1 galaxies detected by SWIFT/BAT and INTEGRAL with a flux in excess of $10^{-11}$~erg~s$^{-1}$~cm$^{-2}$ in the HXD/PIN band for 70~ks each. These proposed observations provide rare high quality spectra of NLS1s above 10~keV. This will remove the spectral degeneracies inherent to limited bandpass analysis (such as that with XMM--Newton and Chandra) and the ambiguities between the different proposed models invoked to explain the unique spectral and variability properties of these most extreme class of high accretion rate sources (namely absorption, reflection, nature of the soft excess...). | EXTRAGALACTIC COMPACT SOURCES | 7 | C | MINIUTTI | GIOVANNI | NULL | NULL | EUR | 2 | AO2 | HUNTING HARD-X-RAY-BRIGHT NLS1 GALAXIES FROM THE INTEGRAL CATALOGUE WITH SUZAKU | HXD | Y |
| IGR J16185-5928 | 244.6464 | -59.4001 | 326.66672881 | -6.44446627 | 90.0003 | 54505.6700115741 | 54507.0211111111 | 702123010 | 76607.6 | 88000 | 76631 | 76623.6 | 0 | 76607.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 75255.3 | 75255.3 | 116725.9 | 0 | PROCESSED | 57541.5586226852 | 54888 | 54515.6564699074 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 022034 | We propose to observe with Suzaku two Narrow Line Seyfert 1 galaxies detected by SWIFT/BAT and INTEGRAL with a flux in excess of $10^{-11}$~erg~s$^{-1}$~cm$^{-2}$ in the HXD/PIN band for 70~ks each. These proposed observations provide rare high quality spectra of NLS1s above 10~keV. This will remove the spectral degeneracies inherent to limited bandpass analysis (such as that with XMM--Newton and Chandra) and the ambiguities between the different proposed models invoked to explain the unique spectral and variability properties of these most extreme class of high accretion rate sources (namely absorption, reflection, nature of the soft excess...). | EXTRAGALACTIC COMPACT SOURCES | 7 | B | MINIUTTI | GIOVANNI | NULL | NULL | EUR | 2 | AO2 | HUNTING HARD-X-RAY-BRIGHT NLS1 GALAXIES FROM THE INTEGRAL CATALOGUE WITH SUZAKU | HXD | Y |
| MRK 110 | 141.3383 | 52.3497 | 164.91808924 | 44.3703784 | 110.1475 | 54406.3443055556 | 54408.31625 | 702124010 | 90871.2 | 100000 | 90871.2 | 90879.2 | 0 | 90879.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 86523.1 | 86523.1 | 170355.8 | 2 | PROCESSED | 57540.442037037 | 54786 | 54417.3880092593 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 023012 | We request a 100 ks SUZAKU observation of Mrk 110 to quantify the accretion disk geometry in this high luminosity narrow line Seyfert 1 galaxy. This is an unique low mass AGN which shows an almost featureless X-ray continuum described by a two component Comptonization model. It has shown, based on an XMM-Newton data, energy dependent delays which are consistent with the idea of a Comptonized plasma confined within 10 Schwartzschild radius of the central black hole. The proposed long observation will provide high signal-to-noise hard X-ray data, thus allowing us to extend the observed delay to higher energies and also to quantify the high energy spectral parameters like cut-off energy and reflection parameters. This will help us to identify the accretion disk geometry in this source. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | RAO | ARIKKALA | Dewangan | Gulab | EUS | 2 | AO2 | PROBING THE ACCRETION DISK GEOMETRY IN THE TYPE I SEYFERT GALAXY MRK 110 | HXD | Y |
| 3C382 | 278.7516 | 32.7087 | 61.3132426 | 17.46021716 | 69.589 | 54217.9621412037 | 54220.8119097222 | 702125010 | 130580 | 120000 | 130588 | 130580 | 0 | 130588 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 122470.7 | 122470.7 | 246195.8 | 2 | PROCESSED | 57538.5400694444 | 54777 | 54228.2765740741 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 024353 | We propose Suzaku observations of the X-ray bright Broad-Line Radio Galaxy 3C382 to study its complex broad-band X-ray spectrum and its variability on longer timescales. To this end, we ask for 3 separate observations of 40 ks each, to be scheduled randomly but not less than a couple of days apart. We aim at probing the origin of the reflection features and strong soft excess in 3C382, ultimately determining the structure and ionization state of the accretion flow. The addition of 3C382 to the Suzaku program (already including 3C120 and 3C390.3) will allow us to explore BLRGs central engines over a wide range of accretion/jet parameters. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | SAMBRUNA | RITA | Kataoka | Jun | USJ | 2 | AO2 | THE HIGH-ENERGY SPECTRA OF BROAD-LINE RADIO GALAXIES | XIS | Y |
| PKS2126-15 | 322.2988 | -15.6437 | 35.92993079 | -41.86589251 | 72.3882 | 54576.0912384259 | 54578.4238310185 | 703001010 | 81921.4 | 80000 | 81921.4 | 81936.4 | 0 | 81945.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 71541.4 | 71541.4 | 201527.9 | 3 | PROCESSED | 57542.3941087963 | 54961 | 54594.3427777778 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030003 | We propose intensive Suzaku observations (80ksec each) of two "primitive" blazars at z > 3.3, with a highly unusual SED. ROXA J081009.9 (z=4.0) was recently found by a short Swift/XRT exposure (6 ksec) with a luminosity well in excess of 10^47 ergs/s, but its synchrotron power peaking above 10 keV. This may suggest the bulk Lorentz factor of the jet could reach ~1000 like GRBs, though quite conspicuous among the AGN jets. Meanwhile, unusual SED of PKS2126-15 (z=3.3) , where the synchrotron peaking at GHz and the inverse Compton peaks at ~10 keV, is most likely due to the presence of ultra-massive black hole with 2x10^10 Ms. These new-types are only found in highly distant universe, and maybe categorized as primitive blazars. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | KATAOKA | JUN | NULL | NULL | JAP | 3 | AO3 | UNVEILING NEW-TYPE "PRIMITIVE" BLAZARS WITH SUZAKU | XIS | Y |
| PKS0208-512 | 32.6864 | -51.0102 | 276.09849974 | -61.78596913 | 230.2146 | 54814.3149074074 | 54815.4793171296 | 703002010 | 51959.4 | 40000 | 51983.4 | 51959.4 | 0 | 51983.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42559 | 42559 | 100599.9 | 0 | PROCESSED | 57544.9648032407 | 54557 | 54826.3087268518 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030004 | We propose intensive Suzaku observations of 11 "VIP" blazars with 40ksec each, as a long-category project. We stress that all of the sources will be monitored simultaneously by GLAST (GeV), Swift XRT/UVOT (UV to X-ray), as well as ground-based radio-to-optical telescopes. We will obtain the broadband spectra and light-curves from 10^9 Hz to 10^25 Hz, which reveals for the first time the nature of gamma-loud blazars in their quiescent states. The proposed 40ksec x 11 Suzaku observations will allow us to investigate | EXTRAGALACTIC COMPACT SOURCES | 7 | A | KATAOKA | JUN | NULL | NULL | JAP | 3 | AO3 | REVEALING THE NATURE OF GAMMA-LOUD BLAZARS VIA SUZAKU/GLAST AND WORLD-WIDE GROUND-BASED OBSERVATIONS | XIS | Y |
| Q0827+243 | 127.7159 | 24.1868 | 200.01721235 | 31.87611482 | 114.1438 | 54766.2156828704 | 54767.3363310185 | 703003010 | 48227.7 | 40000 | 48227.7 | 48227.7 | 0 | 48227.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39303.1 | 39303.1 | 96800.1 | 0 | PROCESSED | 57544.2665625 | 54557 | 54788.24125 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030004 | We propose intensive Suzaku observations of 11 "VIP" blazars with 40ksec each, as a long-category project. We stress that all of the sources will be monitored simultaneously by GLAST (GeV), Swift XRT/UVOT (UV to X-ray), as well as ground-based radio-to-optical telescopes. We will obtain the broadband spectra and light-curves from 10^9 Hz to 10^25 Hz, which reveals for the first time the nature of gamma-loud blazars in their quiescent states. The proposed 40ksec x 11 Suzaku observations will allow us to investigate | EXTRAGALACTIC COMPACT SOURCES | 7 | A | KATAOKA | JUN | NULL | NULL | JAP | 3 | AO3 | REVEALING THE NATURE OF GAMMA-LOUD BLAZARS VIA SUZAKU/GLAST AND WORLD-WIDE GROUND-BASED OBSERVATIONS | XIS | Y |
| PKS1127-145 | 172.5274 | -14.8245 | 275.2785401 | 43.63731171 | 115.9184 | 54799.7571180556 | 54800.9523611111 | 703004010 | 55545.1 | 40000 | 55551.1 | 55545.1 | 0 | 55551.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 31012.3 | 31012.3 | 103248.8 | 0 | PROCESSED | 57544.5555208333 | 54557 | 54809.1987152778 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030004 | We propose intensive Suzaku observations of 11 "VIP" blazars with 40ksec each, as a long-category project. We stress that all of the sources will be monitored simultaneously by GLAST (GeV), Swift XRT/UVOT (UV to X-ray), as well as ground-based radio-to-optical telescopes. We will obtain the broadband spectra and light-curves from 10^9 Hz to 10^25 Hz, which reveals for the first time the nature of gamma-loud blazars in their quiescent states. The proposed 40ksec x 11 Suzaku observations will allow us to investigate | EXTRAGALACTIC COMPACT SOURCES | 7 | A | KATAOKA | JUN | NULL | NULL | JAP | 3 | AO3 | REVEALING THE NATURE OF GAMMA-LOUD BLAZARS VIA SUZAKU/GLAST AND WORLD-WIDE GROUND-BASED OBSERVATIONS | XIS | Y |
| PKS1510-089 | 228.2094 | -9.0956 | 351.2919833 | 40.14272744 | 102.2005 | 54858.1887615741 | 54859.2258564815 | 703005010 | 44305.4 | 40000 | 44305.4 | 44305.4 | 0 | 44305.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16653.7 | 16653.7 | 89597.9 | 0 | PROCESSED | 57545.3861342593 | 54557 | 54880.5404282407 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030004 | We propose intensive Suzaku observations of 11 "VIP" blazars with 40ksec each, as a long-category project. We stress that all of the sources will be monitored simultaneously by GLAST (GeV), Swift XRT/UVOT (UV to X-ray), as well as ground-based radio-to-optical telescopes. We will obtain the broadband spectra and light-curves from 10^9 Hz to 10^25 Hz, which reveals for the first time the nature of gamma-loud blazars in their quiescent states. The proposed 40ksec x 11 Suzaku observations will allow us to investigate | EXTRAGALACTIC COMPACT SOURCES | 7 | A | KATAOKA | JUN | NULL | NULL | JAP | 3 | AO3 | REVEALING THE NATURE OF GAMMA-LOUD BLAZARS VIA SUZAKU/GLAST AND WORLD-WIDE GROUND-BASED OBSERVATIONS | XIS | Y |
| 3C454.3 | 343.4943 | 16.1419 | 86.11034311 | -38.19103065 | 250.8076 | 54792.3878703704 | 54793.6884143518 | 703006010 | 46923.9 | 40000 | 46923.9 | 46923.9 | 0 | 46923.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43344 | 43344 | 112313.9 | 2 | PROCESSED | 57544.5029976852 | 54557 | 54811.7229050926 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030004 | We propose intensive Suzaku observations of 11 "VIP" blazars with 40ksec each, as a long-category project. We stress that all of the sources will be monitored simultaneously by GLAST (GeV), Swift XRT/UVOT (UV to X-ray), as well as ground-based radio-to-optical telescopes. We will obtain the broadband spectra and light-curves from 10^9 Hz to 10^25 Hz, which reveals for the first time the nature of gamma-loud blazars in their quiescent states. The proposed 40ksec x 11 Suzaku observations will allow us to investigate | EXTRAGALACTIC COMPACT SOURCES | 7 | A | KATAOKA | JUN | NULL | NULL | JAP | 3 | AO3 | REVEALING THE NATURE OF GAMMA-LOUD BLAZARS VIA SUZAKU/GLAST AND WORLD-WIDE GROUND-BASED OBSERVATIONS | XIS | Y |
| IGR J12391-1612 | 189.807 | -16.1292 | 298.65896251 | 46.64122293 | 122.9437 | 54818.9051273148 | 54822.2910648148 | 703007010 | 130274 | 120000 | 130274 | 130274 | 0 | 130274 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 111089.3 | 111089.3 | 292483.8 | 2 | PROCESSED | 57545.0634953704 | 55206 | 54840.5288425926 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030012 | We propose a Suzaku observation of a Compton thick candidate, IGR J12391-1612. This source is a bright Seyfert 2 galaxy in the INTEGRAL AGN catalog by Beckman et al. 2006. By a follow-up observation in the optical band, this source was classified as an X-ray luminous type 2 Seyfert galaxy. A Chandra follow-up observation was also performed, but the shape of the X-ray spectrum was not well determined due to a short exposure of 3.5ks. Thank to the wide-band spectroscopy of Suzaku, we can obtain an X-ray spectrum in the 0.5-100 keV band. We will reveal the nature of this Compton thick Seyfert in a spectral analysis. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | AWAKI | HISAMITSU | NULL | NULL | JAP | 3 | AO3 | X-RAY OBSERVATION OF A COMPTON THICK CANDIDATE, IGR J12391-1612 | HXD | Y |
| SWIFT J0911.2+4533 | 137.9062 | 45.5305 | 174.70874001 | 43.11152809 | 111.3983 | 54764.185787037 | 54766.2105787037 | 703008010 | 93879 | 80000 | 93879 | 93879 | 0 | 93895 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 80225.6 | 80225.6 | 174929.8 | 4 | PROCESSED | 57544.2883564815 | 55148 | 54782.4040625 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030034 | The hard X-ray survey with Swift BAT have been finding various types of AGNs. Many buried AGNs with very low scattered X-rays have been discovered, for example. We propose to obtain broad band spectra of Compton-thin buried AGNs in the Swift sample. The data will be used to measure the amount of absoption in the direct and reflected emission and to constrain the structure of the obscuring matter around the AGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TERASHIMA | YUICHI | NULL | NULL | JAP | 3 | AO3 | THE STRUCTURE OF BURIED COMPTON-THIN AGNS DISCOVERED BY SWIFT | HXD | Y |
| SWIFT J1200.8+0650 | 180.2185 | 6.7488 | 270.13481807 | 66.34579154 | 293.0035 | 54617.9027662037 | 54619.9280555556 | 703009010 | 84486.6 | 80000 | 84510.6 | 84486.6 | 0 | 84510.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 71110.9 | 71110.9 | 174963.8 | 3 | PROCESSED | 57542.752037037 | 55003 | 54634.1479282407 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030034 | The hard X-ray survey with Swift BAT have been finding various types of AGNs. Many buried AGNs with very low scattered X-rays have been discovered, for example. We propose to obtain broad band spectra of Compton-thin buried AGNs in the Swift sample. The data will be used to measure the amount of absoption in the direct and reflected emission and to constrain the structure of the obscuring matter around the AGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TERASHIMA | YUICHI | NULL | NULL | JAP | 3 | AO3 | THE STRUCTURE OF BURIED COMPTON-THIN AGNS DISCOVERED BY SWIFT | HXD | Y |
| NGC 1313 | 49.5565 | -66.5364 | 283.40259478 | -44.62074971 | 201.281 | 54805.9606828704 | 54808.2814699074 | 703010010 | 91466.1 | 100000 | 91498.1 | 91466.1 | 0 | 91498.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 78759.3 | 78759.3 | 200493.7 | 1 | PROCESSED | 57544.7004861111 | 55188 | 54822.6519328704 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030038 | The nature of ultra luminous X-ray sources (ULX) is one of the most important unresolved issue in the modern astrophysics. We propose a 100 ks observation of an famous ULX, NGC 1313 X1, in order to search for Fe-K absorption lines, which are important spectral feature of Galactic black holes. Through the absorption feature, we will examine the nature of the ULX. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | OHSUGA | KEN | NULL | NULL | JAP | 3 | AO3 | EXPLORING FE K-LINE ABSORPTION FEATURES FROM AN ULTRALUMINOUS X-RAY SOURCE, NGC 1313 X1 | XIS | Y |
| NGC 5347 | 208.2716 | 33.4399 | 62.06849004 | 75.29189994 | 312.225 | 54627.6603703704 | 54628.6064699074 | 703011010 | 42161.1 | 40000 | 42161.1 | 42161.1 | 0 | 42161.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37130.2 | 37130.2 | 81734 | 1 | PROCESSED | 57542.8072569444 | 55008 | 54637.3250810185 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030040 | We propose to measure broad band X-ray spectra of three Compton-thick Seyfert 2s selected based on large | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TERASHIMA | YUICHI | NULL | NULL | JAP | 3 | AO3 | COMPTON-THICK AGN POPULATION IN THE LOCAL UNIVERSE: HARD X-RAY VIEW OF A COMPLETE | HXD | Y |
| NGC 7130 | 327.065 | -34.8962 | 10.02903365 | -50.33744977 | 78.4767 | 54597.5198726852 | 54598.56625 | 703012010 | 44493.1 | 40000 | 44493.1 | 44493.1 | 0 | 44493.1 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 36767.7 | 36767.7 | 90375.9 | 1 | PROCESSED | 57542.510474537 | 54975 | 54609.0170949074 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030040 | We propose to measure broad band X-ray spectra of three Compton-thick Seyfert 2s selected based on large | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TERASHIMA | YUICHI | NULL | NULL | JAP | 3 | AO3 | COMPTON-THICK AGN POPULATION IN THE LOCAL UNIVERSE: HARD X-RAY VIEW OF A COMPLETE | HXD | Y |
| SWIFT J0959.5-2258 | 149.843 | -22.8716 | 259.02796733 | 24.98206567 | 303.2834 | 54635.9091087963 | 54636.8148611111 | 703013010 | 43663.4 | 40000 | 43671.4 | 43679.4 | 0 | 43663.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42406.1 | 42406.1 | 78237.9 | 0 | PROCESSED | 57542.8554861111 | 55016 | 54650.0591782407 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030045 | Swift/BAT extragalactic survey above E>15 keV has provided us with the first unbiased AGN sample in the local universe. Here we propose to observe the remaining four Compton thick AGN candidates in the 2nd BAT catalog with Suzaku to make it complete. To resolve the degeneracy of spectral modeling to the XMM spectra of these sources, the simultaneous wide-band coverage with the XIS and the HXD is crucial. This will lead us to the first reliable measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. We also aim to construct the template spectra of Compton thick AGNs, applicable to buried AGNs at high redshifts detected in deep surveys. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 3 | AO3 | DETERMINATION OF THE NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS | HXD | Y |
| SWIFT J0501.9-3239 | 79.8743 | -32.7041 | 236.069923 | -32.60257079 | 297.9191 | 54567.6584259259 | 54568.8788194444 | 703014010 | 41298.5 | 40000 | 41298.5 | 41298.5 | 0 | 41298.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36434.2 | 36434.2 | 105425.9 | 0 | PROCESSED | 57542.3107291667 | 54953 | 54580.5155208333 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030045 | Swift/BAT extragalactic survey above E>15 keV has provided us with the first unbiased AGN sample in the local universe. Here we propose to observe the remaining four Compton thick AGN candidates in the 2nd BAT catalog with Suzaku to make it complete. To resolve the degeneracy of spectral modeling to the XMM spectra of these sources, the simultaneous wide-band coverage with the XIS and the HXD is crucial. This will lead us to the first reliable measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. We also aim to construct the template spectra of Compton thick AGNs, applicable to buried AGNs at high redshifts detected in deep surveys. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 3 | AO3 | DETERMINATION OF THE NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS | HXD | Y |
| SWIFT J2009.0-6103 | 302.158 | -61.0495 | 335.84532046 | -32.77756596 | 73.0628 | 54563.6948148148 | 54564.600775463 | 703015010 | 43726.8 | 40000 | 43726.8 | 43726.8 | 0 | 43726.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36199.6 | 36199.6 | 78268 | 1 | PROCESSED | 57542.2661342593 | 54953 | 54580.2454976852 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030045 | Swift/BAT extragalactic survey above E>15 keV has provided us with the first unbiased AGN sample in the local universe. Here we propose to observe the remaining four Compton thick AGN candidates in the 2nd BAT catalog with Suzaku to make it complete. To resolve the degeneracy of spectral modeling to the XMM spectra of these sources, the simultaneous wide-band coverage with the XIS and the HXD is crucial. This will lead us to the first reliable measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. We also aim to construct the template spectra of Compton thick AGNs, applicable to buried AGNs at high redshifts detected in deep surveys. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 3 | AO3 | DETERMINATION OF THE NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS | HXD | Y |
| SWIFT J0134.1-3625 | 23.4345 | -36.4661 | 261.71382804 | -77.05672525 | 34.1001 | 54606.6796180556 | 54607.8390277778 | 703016010 | 48511.6 | 40000 | 48519.6 | 48511.6 | 0 | 48527.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41292.7 | 41292.7 | 100149.8 | 0 | PROCESSED | 57542.6141898148 | 54985 | 54616.4068402778 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030045 | Swift/BAT extragalactic survey above E>15 keV has provided us with the first unbiased AGN sample in the local universe. Here we propose to observe the remaining four Compton thick AGN candidates in the 2nd BAT catalog with Suzaku to make it complete. To resolve the degeneracy of spectral modeling to the XMM spectra of these sources, the simultaneous wide-band coverage with the XIS and the HXD is crucial. This will lead us to the first reliable measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. We also aim to construct the template spectra of Compton thick AGNs, applicable to buried AGNs at high redshifts detected in deep surveys. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 3 | AO3 | DETERMINATION OF THE NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS | HXD | Y |
| 4C73.08 | 147.4414 | 73.2521 | 138.04435007 | 38.07252036 | 100.3847 | 54786.9238888889 | 54788.4946643518 | 703018010 | 81375.2 | 80000 | 81375.2 | 81375.2 | 0 | 81375.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 72453.3 | 72453.3 | 135692 | 0 | PROCESSED | 57544.4300694444 | 55164 | 54798.0487152778 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030063 | Suzaku observation of two giant radio galaxies, 4C 73.08 and 3C 35, are proposed. In 80 ks exposure on the individual target, inverse Compton X-ray emission from their lobes is detected with high signal statistics. As a result, the energy densities of electrons and magnetic field in these lobesare precisely determined. The size of these radio galaxies are significantly lager than that of the previous sample. Therefore, the size dependence of energetics in the lobes will be investigated | EXTRAGALACTIC COMPACT SOURCES | 7 | C | YAJI | YUICHI | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF LOBES OF GIANT RADIO GALAXIES | XIS | Y |
| IRAS 05262+4432 | 82.4599 | 44.6406 | 165.01766257 | 5.72021917 | 78.2999 | 54721.6357523148 | 54723.406412037 | 703019010 | 82086 | 80000 | 82097.5 | 82094 | 0 | 82086 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70907.5 | 70907.5 | 152954.1 | 0 | PROCESSED | 57543.8409490741 | 55148 | 54780.4562037037 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030085 | X-ray observations of obscured narrow-line Seyfert 1 galaxies (NLS1s) have never been performed effectively, in spite of the fact that absorbing material and nuclear emission of NLS1s are thought to be a crucial key to understand the fueling and accretion mechanisms, which may be directly related to the rapid evolution of supermassive black holes. We, therefore, propose 80 ksec observation of the candidate of an obscured NLS1 IRAS 05262+4432. High sensitivity throughout the 0.3-70 keV wide energy band of Suzaku allows us to strictly constrain the X-ray luminosity of primary emission and the geometry of the surrounding matter. From our observation, we expect to derive more complete unified picture of AGNs | EXTRAGALACTIC COMPACT SOURCES | 7 | A | HABA | YOSHITO | NULL | NULL | JAP | 3 | AO3 | SUZAKU VIEW OF OBSCURED NARROW-LINE SEYFERT 1 GALAXY IRAS 05262+4432 | HXD | Y |
| MRK421 | 166.1418 | 38.2711 | 179.67525089 | 65.03258412 | 111.0988 | 54803.7278240741 | 54805.9480324074 | 703020010 | 101307.5 | 100000 | 101331.5 | 101307.5 | 0 | 101331.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 65514.8 | 65514.8 | 191787.7 | 3 | PROCESSED | 57544.7029398148 | 55188 | 54818.7659837963 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030119 | Mrk421 provides our best opportunity to understand the high-energy emission of blazar jets, because it has produced the largest observed flux. Suzaku HXD has proved that spectum upto 40 keV can be measured only with an exposure of 1 ks from Mrk 421. Hard X-ray region is very crucial to study particle acceleration in the jet, since it corresponds to high energy end of electron distribution. Cooling and Acceleration phenomena will appear in this energy band. Here we will propose to monitor Mrk 421 for 200 ks, in which we can expect at least four or five flares. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | TAKAHASHI | TADAYUKI | NULL | NULL | JAP | 3 | AO3 | STUDY OF HARD X-RAY EVOLUTION FROM THE BRIGHTEST BLAZAR JET. | HXD | Y |
| SWIFT J0444.1+2813 | 71.029 | 28.2793 | 172.68057795 | -11.38105828 | 85.0234 | 54719.7173958333 | 54721.6306944445 | 703021010 | 81298.6 | 80000 | 81298.6 | 81298.6 | 0 | 81298.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 67765.4 | 67765.4 | 165303.9 | 0 | PROCESSED | 57543.831087963 | 55148 | 54780.4776736111 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030124 | The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to the latetest population synthesis model, its estimate is strongly coupled with the broad band spectral shape of moderately absorbed AGNs, which is only poorly understood. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright, absorbed AGNs that can be best followed-up with Suzaku. Here we propose to observe two of them to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 3 | AO3 | BROAD BAND SPECTRA OF SWIFT/BAT SELECTED AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND | HXD | Y |
| NGC3227 | 155.8766 | 19.8689 | 216.98457422 | 55.44588075 | 115.8562 | 54767.3422685185 | 54768.8487731482 | 703022010 | 58917.2 | 50000 | 58917.2 | 58917.2 | 0 | 58917.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 52033.7 | 52033.7 | 130147.8 | 1 | PROCESSED | 57544.2886689815 | 54557 | 54788.4566203704 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031013 | We propose a 2 month Suzaku monitoring program of 7 weekly 50ksec observations of the normal type 1 AGN, NGC3227. Variations of the Warm Absorber will determine its location in NGC5548, discriminating between models and determining the mass loss rate in the WA wind. This mdot will provide a calibration at low M_BH/Mdot(Edd) compared with our Cycle 2 NGC5548 measurement 'cosmological feedback' models from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes, or lack thereof, in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, and any broad Fe-K or high ionization edge. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ELVIS | MARTIN | NULL | NULL | USA | 3 | AO3 | NGC3227 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK | XIS | Y |
| NGC3227 | 155.8772 | 19.8688 | 216.98506904 | 55.4463804 | 114.6051 | 54774.1503587963 | 54775.6780555556 | 703022020 | 53699.5 | 50000 | 53699.5 | 53699.5 | 0 | 53699.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 50289.1 | 50289.1 | 131971.8 | 3 | PROCESSED | 57544.3625810185 | 54557 | 54788.4371643518 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031013 | We propose a 2 month Suzaku monitoring program of 7 weekly 50ksec observations of the normal type 1 AGN, NGC3227. Variations of the Warm Absorber will determine its location in NGC5548, discriminating between models and determining the mass loss rate in the WA wind. This mdot will provide a calibration at low M_BH/Mdot(Edd) compared with our Cycle 2 NGC5548 measurement 'cosmological feedback' models from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes, or lack thereof, in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, and any broad Fe-K or high ionization edge. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ELVIS | MARTIN | NULL | NULL | USA | 3 | AO3 | NGC3227 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK | XIS | Y |
| NGC3227 | 155.8768 | 19.8689 | 216.98468368 | 55.44605831 | 113.2489 | 54782.1173032407 | 54783.7293865741 | 703022030 | 56571.5 | 50000 | 56577.2 | 56585.2 | 0 | 56571.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 50223.1 | 50223.1 | 139269.8 | 1 | PROCESSED | 57544.401724537 | 54557 | 54797.3603356482 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031013 | We propose a 2 month Suzaku monitoring program of 7 weekly 50ksec observations of the normal type 1 AGN, NGC3227. Variations of the Warm Absorber will determine its location in NGC5548, discriminating between models and determining the mass loss rate in the WA wind. This mdot will provide a calibration at low M_BH/Mdot(Edd) compared with our Cycle 2 NGC5548 measurement 'cosmological feedback' models from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes, or lack thereof, in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, and any broad Fe-K or high ionization edge. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ELVIS | MARTIN | NULL | NULL | USA | 3 | AO3 | NGC3227 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK | XIS | Y |
| NGC3227 | 155.8768 | 19.8688 | 216.98485011 | 55.4460253 | 111.8565 | 54790.7083333333 | 54792.374525463 | 703022040 | 64567.9 | 50000 | 64575.9 | 64567.9 | 0 | 64575.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46622 | 46622 | 143947.8 | 1 | PROCESSED | 57544.506412037 | 54557 | 54812.4380324074 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031013 | We propose a 2 month Suzaku monitoring program of 7 weekly 50ksec observations of the normal type 1 AGN, NGC3227. Variations of the Warm Absorber will determine its location in NGC5548, discriminating between models and determining the mass loss rate in the WA wind. This mdot will provide a calibration at low M_BH/Mdot(Edd) compared with our Cycle 2 NGC5548 measurement 'cosmological feedback' models from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes, or lack thereof, in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, and any broad Fe-K or high ionization edge. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ELVIS | MARTIN | NULL | NULL | USA | 3 | AO3 | NGC3227 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK | XIS | Y |
| NGC3227 | 155.8772 | 19.8684 | 216.98573476 | 55.44624837 | 110.6974 | 54797.8953703704 | 54799.750162037 | 703022050 | 79429.8 | 50000 | 79429.8 | 79433.9 | 0 | 79437.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39843.9 | 39843.9 | 160241.8 | 1 | PROCESSED | 57544.6203819444 | 54557 | 54809.8059490741 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031013 | We propose a 2 month Suzaku monitoring program of 7 weekly 50ksec observations of the normal type 1 AGN, NGC3227. Variations of the Warm Absorber will determine its location in NGC5548, discriminating between models and determining the mass loss rate in the WA wind. This mdot will provide a calibration at low M_BH/Mdot(Edd) compared with our Cycle 2 NGC5548 measurement 'cosmological feedback' models from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes, or lack thereof, in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, and any broad Fe-K or high ionization edge. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ELVIS | MARTIN | NULL | NULL | USA | 3 | AO3 | NGC3227 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK | XIS | Y |
| NGC3227 | 155.8768 | 19.8687 | 216.98501654 | 55.44599229 | 109.926 | 54802.6028125 | 54803.7231365741 | 703022060 | 51410.5 | 50000 | 51410.5 | 51410.5 | 0 | 51410.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39683.6 | 39683.6 | 96781.8 | 1 | PROCESSED | 57544.6321875 | 54557 | 54812.4432407407 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031013 | We propose a 2 month Suzaku monitoring program of 7 weekly 50ksec observations of the normal type 1 AGN, NGC3227. Variations of the Warm Absorber will determine its location in NGC5548, discriminating between models and determining the mass loss rate in the WA wind. This mdot will provide a calibration at low M_BH/Mdot(Edd) compared with our Cycle 2 NGC5548 measurement 'cosmological feedback' models from AGN to galaxy formation. Simultaneously, the XIS and HXD spectra will study changes, or lack thereof, in the reflection components (narrow Fe-K, Compton Hump), again delimiting their location and choosing among models. The summed spectrum will determine the high energy continuum break, and any broad Fe-K or high ionization edge. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ELVIS | MARTIN | NULL | NULL | USA | 3 | AO3 | NGC3227 MONITORING: KEY TO AGN STRUCTURE AND COSMIC FEEDBACK | XIS | Y |
| NGC 4051 | 180.7984 | 44.5394 | 148.85547697 | 70.08163582 | 138.344 | 54776.3187847222 | 54782.1112731482 | 703023010 | 274530.5 | 340000 | 274530.5 | 274530.5 | 0 | 274530.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 220199.3 | 220199.3 | 441448.8 | 3 | PROCESSED | 57544.5089930556 | 54557 | 54795.7746527778 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031014 | The powerful combination of Principal Components Analysis with time-resolved X-ray spectroscopy of Seyfert AGN has shown strong evidence that changes in a complex absorber are the origin of much of observed AGN spectral and flux variability. Large column, high ionization layers of gas may arise in a disk wind, representing a significant new, and possibly dominant, component, responsible for shaping the X-ray spectrum of AGN. The broad bandpass of Suzaku gives us a unique opportunity to model primary and reflected continua and the effects of variable absorbing zones, and test wind and other models. We propose a long 340 ks exposure on the NLSy1 NGC 4051 whose large amplitude of variability and well-studied complex absorption will test those models to the limit | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TURNER | TRACEY | NULL | NULL | USA | 3 | AO3 | DECONSTRUCTING SEYFERT SPECTRA - TIME FOR A PARADIGM SHIFT? | XIS | Y |
| NGC 4051 | 180.7952 | 44.5393 | 148.86124636 | 70.08047443 | 126.4079 | 54793.7 | 54795.572025463 | 703023020 | 78385.5 | 70000 | 78393.5 | 78385.5 | 0 | 78393.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 62760.4 | 62760.4 | 161735.8 | 0 | PROCESSED | 57544.5729513889 | 54557 | 54811.74875 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031014 | The powerful combination of Principal Components Analysis with time-resolved X-ray spectroscopy of Seyfert AGN has shown strong evidence that changes in a complex absorber are the origin of much of observed AGN spectral and flux variability. Large column, high ionization layers of gas may arise in a disk wind, representing a significant new, and possibly dominant, component, responsible for shaping the X-ray spectrum of AGN. The broad bandpass of Suzaku gives us a unique opportunity to model primary and reflected continua and the effects of variable absorbing zones, and test wind and other models. We propose a long 340 ks exposure on the NLSy1 NGC 4051 whose large amplitude of variability and well-studied complex absorption will test those models to the limit | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TURNER | TRACEY | NULL | NULL | USA | 3 | AO3 | DECONSTRUCTING SEYFERT SPECTRA - TIME FOR A PARADIGM SHIFT? | XIS | Y |
| SN 2005KD | 60.8552 | 71.7156 | 136.84988934 | 14.24754739 | 218.8053 | 54568.8904976852 | 54570.0348842593 | 703025010 | 51628.9 | 50000 | 51628.9 | 51636.9 | 0 | 51644.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 63572.6 | 63572.6 | 98863.9 | 1 | PROCESSED | 57542.2950694444 | 54947 | 54581.1998842593 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031241 | Supernovae (SNe) 2005kd and 2006jd are some of the brightest SNe ever detected in X-rays. The high X-ray luminosities (>E41 erg/s) are the results of the SN shock interacting with dense material in the environment of the SNe. We propose one Suzaku observation of each SN to obtain high-quality spectra that will be used to measure the temperature of the forward and reverse shock and to establish the rate of decline in comparison with existing Swift, Chandra and XMM-Newton data. The data will further be used to measure the circumstellar matter density and mass-loss rate of the progenitors to probe the nature of the SN progenitors. Our science objectives rely on Suzaku's uniqueness, i.e. the large collecting area, good spectral resolution, and the high sensitivity in the hard X-ray band. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | IMMLER | STEFAN | NULL | NULL | USA | 3 | AO3 | SUZAKU OBSERVATIONS OF X-RAY BRIGHT SUPERNOVAE | XIS | Y |
| SN 2006JD | 120.5331 | 0.8102 | 220.45612728 | 16.05834455 | 284.354 | 54578.4377777778 | 54579.6807175926 | 703026010 | 54196.8 | 50000 | 54204.8 | 54196.8 | 0 | 54204.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 52048.8 | 52048.8 | 107339.8 | 1 | PROCESSED | 57542.379837963 | 54957 | 54588.1523611111 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031241 | Supernovae (SNe) 2005kd and 2006jd are some of the brightest SNe ever detected in X-rays. The high X-ray luminosities (>E41 erg/s) are the results of the SN shock interacting with dense material in the environment of the SNe. We propose one Suzaku observation of each SN to obtain high-quality spectra that will be used to measure the temperature of the forward and reverse shock and to establish the rate of decline in comparison with existing Swift, Chandra and XMM-Newton data. The data will further be used to measure the circumstellar matter density and mass-loss rate of the progenitors to probe the nature of the SN progenitors. Our science objectives rely on Suzaku's uniqueness, i.e. the large collecting area, good spectral resolution, and the high sensitivity in the hard X-ray band. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | IMMLER | STEFAN | NULL | NULL | USA | 3 | AO3 | SUZAKU OBSERVATIONS OF X-RAY BRIGHT SUPERNOVAE | XIS | Y |
| NGC 7469 | 345.7842 | 8.9301 | 83.10914575 | -45.403242 | 63.4793 | 54641.7015856482 | 54644.683599537 | 703028010 | 112112.8 | 100000 | 112125.1 | 112133.1 | 0 | 112112.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 91557.1 | 91557.1 | 257612.6 | 2 | PROCESSED | 57542.968125 | 55027 | 54658.7891319444 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031311 | We propose a 100 ksec observation of the X-ray bright Seyfert 1 AGN NGC 7469, a strong candidate for having ionized reflection from the accretion disk. Only the broad bandpass provided by Suzaku, including >12 keV coverage via the HXD, will allow us to deconvolve the broadband emitting components, including the strong Compton reflection hump, broad Fe K line, and soft excess. With the XIS, we will study in detail the Fe K emission complex, including the narrow 6.4 keV Fe K core and in particular the prominent ``blue wing'' near 6.9 keV. Our proposed observation will thus be an example of how broad bandpass X-ray observations can critically test blurred, ionized disk reflection model in Seyfert 1s. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | MARKOWITZ | ALEX | NULL | NULL | USA | 3 | AO3 | IONIZED DISK REFLECTION IN THE SEYFERT AGN NGC 7469 | HXD | Y |
| MRK 348 | 12.1911 | 31.9636 | 122.27104531 | -30.90471809 | 71.8836 | 54645.9325694444 | 54648.0591203704 | 703029010 | 87461.4 | 80000 | 88533.4 | 87461.4 | 0 | 88533.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 78550.4 | 78550.4 | 183723.9 | 0 | PROCESSED | 57542.9708333333 | 55031 | 54664.7845601852 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031322 | X-ray observations of Seyfert 2 have shown that the distribution and ionization state of the circumnuclear material is more complex than the simple homogeneous torus predicted by the AGN Unification Scheme. To investigate the nature of this material, high sensitivity is needed to detect relatively faint emission lines, while broad bandpass is required to constrain the primary X-ray continuum. We propose Suzaku observations (80 ksec each) of three bright Compton-thin Seyfert 2 galaxies, selected from the Swift/BAT survey, with a hard X-ray flux exceeding 9e-11cgs, to form a flux-limited sample. The unprecedented bandpass of Suzaku offers a unique tool to investigate the X-ray emission of these sources, allowing us to put strong constraints on the reprocessing matter in Seyfert 2s. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | BRAITO | VALENTINA | NULL | NULL | USA | 3 | AO3 | THE NATURE OF THE X-RAY ABSORBER IN SEYFERT 2 GALAXIES | XIS | Y |
| NGC 7172 | 330.5062 | -31.8708 | 15.12698367 | -53.06449716 | 59.7356 | 54611.0658680556 | 54612.8558217593 | 703030010 | 82279.7 | 80000 | 82279.7 | 82287.7 | 0 | 82287.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 71746.5 | 71746.5 | 154633.8 | 0 | PROCESSED | 57542.6661805556 | 54999 | 54633.7016203704 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031322 | X-ray observations of Seyfert 2 have shown that the distribution and ionization state of the circumnuclear material is more complex than the simple homogeneous torus predicted by the AGN Unification Scheme. To investigate the nature of this material, high sensitivity is needed to detect relatively faint emission lines, while broad bandpass is required to constrain the primary X-ray continuum. We propose Suzaku observations (80 ksec each) of three bright Compton-thin Seyfert 2 galaxies, selected from the Swift/BAT survey, with a hard X-ray flux exceeding 9e-11cgs, to form a flux-limited sample. The unprecedented bandpass of Suzaku offers a unique tool to investigate the X-ray emission of these sources, allowing us to put strong constraints on the reprocessing matter in Seyfert 2s. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | BRAITO | VALENTINA | NULL | NULL | USA | 3 | AO3 | THE NATURE OF THE X-RAY ABSORBER IN SEYFERT 2 GALAXIES | XIS | Y |
| ESO 103- G 035 | 279.5941 | -65.4238 | 329.78379096 | -23.17817546 | 291.5832 | 54761.6331597222 | 54764.1717476852 | 703031010 | 91442 | 80000 | 91442 | 91450 | 0 | 91450 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 81009.6 | 81009.6 | 219282 | 2 | PROCESSED | 57544.3339467593 | 55148 | 54782.4220023148 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031322 | X-ray observations of Seyfert 2 have shown that the distribution and ionization state of the circumnuclear material is more complex than the simple homogeneous torus predicted by the AGN Unification Scheme. To investigate the nature of this material, high sensitivity is needed to detect relatively faint emission lines, while broad bandpass is required to constrain the primary X-ray continuum. We propose Suzaku observations (80 ksec each) of three bright Compton-thin Seyfert 2 galaxies, selected from the Swift/BAT survey, with a hard X-ray flux exceeding 9e-11cgs, to form a flux-limited sample. The unprecedented bandpass of Suzaku offers a unique tool to investigate the X-ray emission of these sources, allowing us to put strong constraints on the reprocessing matter in Seyfert 2s. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | BRAITO | VALENTINA | NULL | NULL | USA | 3 | AO3 | THE NATURE OF THE X-RAY ABSORBER IN SEYFERT 2 GALAXIES | XIS | Y |
| NGC 788 | 30.262 | -6.7593 | 165.15039638 | -63.76864601 | 77.358 | 54660.0353819444 | 54661.0516666667 | 703032010 | 45907.3 | 40000 | 45915.3 | 45907.3 | 0 | 45915.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 39594 | 39594 | 87799.9 | 0 | PROCESSED | 57543.0405902778 | 55048 | 54682.1458564815 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031323 | The classical unified model predicts only one type of Seyfert II (Sy2). Recent observations of SWIFT BAT-detected AGN found at least 4 classes of Sy2s: (1) objects with high column density and scattered soft x-rays, (2) Compton thick objects, (3) `hidden' AGN (Ueda et al. 2007), and (4) the `changing look' objects (Risaliti et al. 2006). The nature of these sources can only be revealed with high quality broad-band X-ray spectra from Suzaku. Thus, we are proposing 40ks observations for 2 of the brightest BAT AGN without high quality data, NGC 788, a type (3) object showing polarized optical broad lines, and NGC 3281, a classified (2) object. Such observations are necessary to build a reasonably large sample of high-quality, broad-band Sy2 spectra covering the range of X-ray/optical types. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MUSHOTZKY | RICHARD | NULL | NULL | USA | 3 | AO3 | SUZAKU OBSERVATIONS OF X-RAY BRIGHT TYPE II AGN | HXD | Y |
| NGC 3281 | 157.9591 | -34.9074 | 273.03211125 | 19.73409342 | 278.2413 | 54607.8508449074 | 54609.2287615741 | 703033010 | 46234 | 40000 | 46242 | 46250 | 0 | 46234 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41454.9 | 41454.9 | 119038 | 0 | PROCESSED | 57542.6257175926 | 54988 | 54620.2890162037 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031323 | The classical unified model predicts only one type of Seyfert II (Sy2). Recent observations of SWIFT BAT-detected AGN found at least 4 classes of Sy2s: (1) objects with high column density and scattered soft x-rays, (2) Compton thick objects, (3) `hidden' AGN (Ueda et al. 2007), and (4) the `changing look' objects (Risaliti et al. 2006). The nature of these sources can only be revealed with high quality broad-band X-ray spectra from Suzaku. Thus, we are proposing 40ks observations for 2 of the brightest BAT AGN without high quality data, NGC 788, a type (3) object showing polarized optical broad lines, and NGC 3281, a classified (2) object. Such observations are necessary to build a reasonably large sample of high-quality, broad-band Sy2 spectra covering the range of X-ray/optical types. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MUSHOTZKY | RICHARD | NULL | NULL | USA | 3 | AO3 | SUZAKU OBSERVATIONS OF X-RAY BRIGHT TYPE II AGN | HXD | Y |
| 3C 111 | 64.5741 | 38.0889 | 161.62276278 | -8.7838332 | 81.5451 | 54700.4141898148 | 54703.1836111111 | 703034010 | 122378 | 120000 | 122386 | 122378 | 0 | 122378 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 109706.7 | 109706.7 | 239251.7 | 1 | PROCESSED | 57543.4018287037 | 55084 | 54713.6361226852 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031332 | The origin of the high-energy emission from Broad-Line Radio Galaxies is still an open issue. A plausible scenario is reprocessed emission from a cold medium (disk) diluted by variable, non-thermal jet flux. To test this scenario we propose Suzaku observations of the BLRG 3C 111, which exhibits flux variability above 10 keV from available data, suggesting a jet contribution. Moreover, 3C 111 was previously detected with EGRET at GeV energies, and synergy with GLAST will thus be exploited in the proposed program. The coupled timing and spectral information provided by Suzaku are key to disentangle the disk and jet contributions, and determine their respective role for the source energy budget. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | SAMBRUNA | RITA | NULL | NULL | USA | 3 | AO3 | SUZAKU OBSERVATIONS OF 3C 111: UNCOVERING THE JET WITHIN | HXD | Y |
| Q0122-380 | 21.0759 | -37.7461 | 271.91657466 | -77.33125236 | 48.7944 | 54615.4511921296 | 54616.2009722222 | 703035010 | 28481 | 25000 | 28481 | 28489 | 0 | 28497 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26810.7 | 26810.7 | 64769.9 | 1 | PROCESSED | 57542.6524421296 | 54999 | 54633.6971759259 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031334 | Recent spectroscopic observations in the UV band have revealed high velocity outflows in Narrow Absorption Line (NAL) quasars. Our analysis of exploratory Suzaku and XMM-Newton observations of NAL quasars indicates that their UV and X-ray properties connect smoothly to those of BAL quasars. The proposed expansion of our sample will allow us to place constraints on correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. We will test existing models of the nature of NAL quasars. The detected X-ray brightest objects from the proposed survey will be followed up with deeper observations to constrain the kinematic and ionization properties of the absorbers and ultimately constrain their mass outflow rates. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | CHARTAS | GEORGE | NULL | NULL | USA | 3 | AO3 | A SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS | XIS | Y |
| Q0551-3637 | 88.2026 | -36.6158 | 242.36930247 | -26.91846995 | 296.4731 | 54575.4385763889 | 54575.6251041667 | 703036010 | 3895.4 | 22000 | 3895.4 | 3895.4 | 0 | 3895.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3773 | 3773 | 16095.9 | 0 | PROCESSED | 57542.3345601852 | 54979 | 54588.1227314815 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031334 | Recent spectroscopic observations in the UV band have revealed high velocity outflows in Narrow Absorption Line (NAL) quasars. Our analysis of exploratory Suzaku and XMM-Newton observations of NAL quasars indicates that their UV and X-ray properties connect smoothly to those of BAL quasars. The proposed expansion of our sample will allow us to place constraints on correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. We will test existing models of the nature of NAL quasars. The detected X-ray brightest objects from the proposed survey will be followed up with deeper observations to constrain the kinematic and ionization properties of the absorbers and ultimately constrain their mass outflow rates. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | CHARTAS | GEORGE | NULL | NULL | USA | 3 | AO3 | A SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS | XIS | Y |
| Q0551-3637 | 88.2027 | -36.6207 | 242.37463259 | -26.91966553 | 321.5977 | 54600.5596643518 | 54601.2044444444 | 703036020 | 21614.3 | 22000 | 21614.3 | 21614.3 | 0 | 21618.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18283.1 | 18283.1 | 55684 | 1 | PROCESSED | 57542.5389236111 | 54979 | 54613.0157060185 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031334 | Recent spectroscopic observations in the UV band have revealed high velocity outflows in Narrow Absorption Line (NAL) quasars. Our analysis of exploratory Suzaku and XMM-Newton observations of NAL quasars indicates that their UV and X-ray properties connect smoothly to those of BAL quasars. The proposed expansion of our sample will allow us to place constraints on correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. We will test existing models of the nature of NAL quasars. The detected X-ray brightest objects from the proposed survey will be followed up with deeper observations to constrain the kinematic and ionization properties of the absorbers and ultimately constrain their mass outflow rates. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | CHARTAS | GEORGE | NULL | NULL | USA | 3 | AO3 | A SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS | XIS | Y |
| Q0109-3518 | 17.9376 | -35.0527 | 275.45528409 | -80.96443984 | 40.3411 | 54606.0677199074 | 54606.6772453704 | 703037010 | 29958.5 | 18000 | 29966.5 | 29958.5 | 0 | 29966.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 22833.9 | 22833.9 | 52655.9 | 1 | PROCESSED | 57542.5808101852 | 54982 | 54616.3810300926 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031334 | Recent spectroscopic observations in the UV band have revealed high velocity outflows in Narrow Absorption Line (NAL) quasars. Our analysis of exploratory Suzaku and XMM-Newton observations of NAL quasars indicates that their UV and X-ray properties connect smoothly to those of BAL quasars. The proposed expansion of our sample will allow us to place constraints on correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. We will test existing models of the nature of NAL quasars. The detected X-ray brightest objects from the proposed survey will be followed up with deeper observations to constrain the kinematic and ionization properties of the absorbers and ultimately constrain their mass outflow rates. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | CHARTAS | GEORGE | NULL | NULL | USA | 3 | AO3 | A SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS | XIS | Y |
| Q0329-385 | 52.7815 | -38.4067 | 241.941352 | -54.89845774 | 23.7676 | 54633.4249421296 | 54634.1898611111 | 703038010 | 30203 | 29000 | 30219 | 30203 | 0 | 30219 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25292.5 | 25292.5 | 66082 | 1 | PROCESSED | 57542.8370601852 | 55010 | 54644.1762615741 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031334 | Recent spectroscopic observations in the UV band have revealed high velocity outflows in Narrow Absorption Line (NAL) quasars. Our analysis of exploratory Suzaku and XMM-Newton observations of NAL quasars indicates that their UV and X-ray properties connect smoothly to those of BAL quasars. The proposed expansion of our sample will allow us to place constraints on correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. We will test existing models of the nature of NAL quasars. The detected X-ray brightest objects from the proposed survey will be followed up with deeper observations to constrain the kinematic and ionization properties of the absorbers and ultimately constrain their mass outflow rates. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | CHARTAS | GEORGE | NULL | NULL | USA | 3 | AO3 | A SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS | XIS | Y |
| Q1158-1843 | 180.1895 | -18.9957 | 286.65628264 | 42.26876142 | 291.8577 | 54636.8208912037 | 54637.4202314815 | 703039010 | 24085 | 22000 | 24101 | 24085 | 0 | 24101 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22430.9 | 22430.9 | 51781.9 | 1 | PROCESSED | 57542.8567361111 | 55014 | 54648.3349305556 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031334 | Recent spectroscopic observations in the UV band have revealed high velocity outflows in Narrow Absorption Line (NAL) quasars. Our analysis of exploratory Suzaku and XMM-Newton observations of NAL quasars indicates that their UV and X-ray properties connect smoothly to those of BAL quasars. The proposed expansion of our sample will allow us to place constraints on correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. We will test existing models of the nature of NAL quasars. The detected X-ray brightest objects from the proposed survey will be followed up with deeper observations to constrain the kinematic and ionization properties of the absorbers and ultimately constrain their mass outflow rates. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | CHARTAS | GEORGE | NULL | NULL | USA | 3 | AO3 | A SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS | XIS | Y |
| Q0940-1050 | 145.7249 | -11.0726 | 246.39011763 | 30.43738638 | 275.7617 | 54616.2125578704 | 54617.1321064815 | 703040010 | 32362.3 | 28000 | 32362.3 | 32362.3 | 0 | 32362.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26777.6 | 26777.6 | 79437.8 | 1 | PROCESSED | 57542.689212963 | 54999 | 54633.6981828704 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031334 | Recent spectroscopic observations in the UV band have revealed high velocity outflows in Narrow Absorption Line (NAL) quasars. Our analysis of exploratory Suzaku and XMM-Newton observations of NAL quasars indicates that their UV and X-ray properties connect smoothly to those of BAL quasars. The proposed expansion of our sample will allow us to place constraints on correlations between the amount of X-ray absorption and UV properties of the wind to better understand the acceleration mechanism of quasar winds. We will test existing models of the nature of NAL quasars. The detected X-ray brightest objects from the proposed survey will be followed up with deeper observations to constrain the kinematic and ionization properties of the absorbers and ultimately constrain their mass outflow rates. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | CHARTAS | GEORGE | NULL | NULL | USA | 3 | AO3 | A SURVEY OF NAL QUASARS WITH HIGH VELOCITY OUTFLOWS | XIS | Y |
| J081618.99+482328.4 | 124.0768 | 48.3841 | 171.01809871 | 33.69777889 | 298.4793 | 54917.0925462963 | 54919.0946643518 | 703042010 | 90922.4 | 90000 | 90922.4 | 90922.4 | 0 | 90922.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 81073.9 | 81073.9 | 172963.7 | 2 | PROCESSED | 57545.9726736111 | 55329 | 54930.3718055556 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031337 | We have discovered polar broad absorption-line quasars (BALQSOs) from their radio variabilities. We know their inclination angles. Our results derived from the archival Chandra data of one polar BALQSO indicate that the X-ray emissions are from the jet and the X-ray absorbing gas is located at tens of parsecs above the accretion disk corona. We want to confirm these results at high confidence level using better signal to noise ratio data from a big observatory, like SUZAKU. In addition, we propose to observe three more polar BALQSOs, which have wide range of radio/UV/X-ray properties. Our primary science goal of this proposal is to determine the radial distribution of the X-ray absorbing gas in 4 polar BALQSOs. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | GHOSH | KAJAL | NULL | NULL | USA | 3 | AO3 | PROBING THE INNER STRUCTURE OF AGNS USING THE POLAR BALQSOS | XIS | Y |
| MRK 421 | 166.1081 | 38.2021 | 179.85015534 | 65.02934628 | 313.5582 | 54591.1196527778 | 54595.3502199074 | 703043010 | 180785.1 | 150000 | 180793.1 | 180785.1 | 0 | 180793.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 163550.7 | 163550.7 | 343651.7 | 9 | PROCESSED | 57542.5998842593 | 54972 | 54606.5618287037 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031341 | We propose one 150 ksec Suzaku ToO observations of one of the three strong GeV-TeV gamma-ray blazars Mrk 421, Mrk 501, or 1ES 1959+650 during a 10 day multiwavelength campaign with coverage from radio to gamma-rays. The proposal is submitted by the VERITAS collaboration, assuring excellent TeV gamma-ray coverage. The Suzaku observations will play a key-role in interpreting the multiwavelength data set, allowing us to measure the time lag between the X-ray and gamma-ray flux variability and to scrutinize the correlation of the X-ray and gamma-ray spectral indices. The Suzaku and gamma-ray energy spectra will allow us to constrain the intensity of the IR Diffuse Extragalactic Background Radiation which absorbs TeV gamma-rays in extragalactic pairproduction processes. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | KRAWCZYNSKI | HENRIC | NULL | NULL | USA | 3 | AO3-TOO | TARGET OF OPPORTUNITY OBSERVATIONS OF THE BLAZARS MRK 421, MRK 501, AND 1ES 1959+650 | HXD | Y |
| MRK 501 | 253.4335 | 39.8281 | 63.68387876 | 38.89139128 | 70.9919 | 54913.7775347222 | 54915.3328587963 | 703046010 | 72334.2 | 65000 | 72334.2 | 72334.2 | 0 | 72334.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 64836.5 | 64836.5 | 134358.1 | 1 | PROCESSED | 57545.930462963 | 55329 | 54924.366724537 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031343 | We propose to observe two bright TeV blazars with Suzaku, in coordination with VERITAS and MAGIC at TeV energies. The primary objective is to make use of the recently available observational capabilities in collecting the much needed simultaneous X-ray and TeV data on these intriguing sources. The data will be essential for addressing a number of unresolved issues in the study of TeV blazars, such as spectral variability, X-ray/TeV correlation and associated time lags, spectral hysteresis, etc. The results will likely provide insights into the properties of the emitting particles, as well as those of the emitting regions, emission mechanism, composition of the jets, and acceleration energetics. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | CUI | WEI | NULL | NULL | USA | 3 | AO3 | COORDINATED X-RAY/TEV OBSERVATIONS OF TEV BLAZARS | HXD | Y |
| PKS 0528+134 | 82.7307 | 13.5905 | 191.31463869 | -10.98486414 | 89.0231 | 54736.1098611111 | 54741.6752777778 | 703048010 | 203457.4 | 200000 | 203465.4 | 203465.4 | 0 | 203457.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 135362.9 | 135362.9 | 443861.9 | 4 | PROCESSED | 57544.2063888889 | 55148 | 54780.7843287037 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031345 | We propose a Suzaku observation of bright gamma-ray blazar PKS 0528+134, to be conducted jointly with GLAST, radio, and optical telescopes. This observation was accepted in the previous AO, but was not conducted due to GLAST launch delays. The goal is to obtain time-resolved broadband spectra. The X-ray and gamma-ray fluxes are known to be rapidly variable, but the information regarding the correlation between the X-ray and gamma-ray flux is limited. Such detailed spectral and variability studies are crucial to discriminate between different radiation scenarios responsible for production of X-rays and gamma-rays, and to constrain the matter content and by extension, the formation process of the jet, dissipation of the jet energy, and energization of the radiating particles. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MADEJSKI | GRZEGORZ | NULL | NULL | USA | 3 | AO3 | SUZAKU AND GLAST OBSERVATIONS OF PKS 0528+134 | HXD | Y |
| 3C279 | 194.0685 | -5.7338 | 305.14803375 | 57.11713803 | 113.6423 | 54850.9795833333 | 54853.9391203704 | 703049010 | 134110.6 | 200000 | 134110.6 | 134110.6 | 0 | 134110.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 82856.3 | 82856.3 | 255689 | 7 | PROCESSED | 57545.3939351852 | 55328 | 54880.5781365741 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031346 | We propose a 200 ks observation of 3C279, the archetypal EGRET blazar to be conducted simultaneously with GLAST as well as many other facilities, with the goal of obtaining broadband spectra and light-curves. The flux in all observable bands is known to be rapidly variable, but the information regarding the correlation between the time history of flux in various bands is limited, and the proposed observations are designed to remedy this shortcoming. Such detailed spectral and variability studies are crucial to discriminate between different radiation scenarios responsible for production of X-rays and gamma-rays, and to constrain the matter content and by extension, the formation process of the jet, dissipation of the jet energy, and energization of the radiating particles. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MADEJSKI | GRZEGORZ | NULL | NULL | USA | 3 | AO3 | SUZAKU AND GLAST OBSERVATIONS OF 3C279 | HXD | Y |
| 3C279 | 194.0699 | -5.7328 | 305.15066173 | 57.11808922 | 113.6425 | 54854.8772222222 | 54856.125162037 | 703049020 | 56937 | 200000 | 56937 | 56937 | 0 | 56937 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12626.3 | 12626.3 | 107779.9 | 2 | PROCESSED | 57545.3327777778 | 55328 | 54880.5584259259 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031346 | We propose a 200 ks observation of 3C279, the archetypal EGRET blazar to be conducted simultaneously with GLAST as well as many other facilities, with the goal of obtaining broadband spectra and light-curves. The flux in all observable bands is known to be rapidly variable, but the information regarding the correlation between the time history of flux in various bands is limited, and the proposed observations are designed to remedy this shortcoming. Such detailed spectral and variability studies are crucial to discriminate between different radiation scenarios responsible for production of X-rays and gamma-rays, and to constrain the matter content and by extension, the formation process of the jet, dissipation of the jet energy, and energization of the radiating particles. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MADEJSKI | GRZEGORZ | NULL | NULL | USA | 3 | AO3 | SUZAKU AND GLAST OBSERVATIONS OF 3C279 | HXD | Y |
| PKS1549-79 | 239.2836 | -79.2302 | 311.18735019 | -19.47008602 | 310.7048 | 54752.6495833333 | 54754.9009375 | 703059010 | 82175.5 | 80000 | 82197 | 82183.5 | 0 | 82175.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 79973.6 | 79973.6 | 194497.7 | 2 | PROCESSED | 57544.1654398148 | 55148 | 54780.6256597222 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 032005 | Galaxy merger models predict rapid black hole growth and strong outflows late in the merger as the accretion rate increases. PKS1549-79 is a powerful, low redshift, high accretion rate active galaxy which has undergone a recent merger. It is therefore an ideal object to test our understanding of galaxy activity and mergers and for studying feedback between AGN and their host galaxies. We propose an 80 ksec Suzaku observation to: (i) determine the amount and ionisation state of the nuclear obscuring material in PKS1549-79 and hence confirm its status as a local proto-quasar; (ii) search for the massive, probably highly ionised, outflowing wind predicted by galaxy evolution models and hence complete a census of outflow components in this object; and (iii) quantify the high energy spectrum. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | O'BRIEN | PAUL | NULL | NULL | EUR | 3 | AO3 | UNVEILING PKS 1549-79 WITH SUZAKU | XIS | Y |
| MCG-02-14-009 | 79.0657 | -10.5106 | 211.75204832 | -25.86275025 | 68.0451 | 54706.9410069444 | 54710.0308333333 | 703060010 | 142152.2 | 125000 | 142152.2 | 142152.2 | 0 | 142152.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 129587.9 | 129587.9 | 266919.9 | 1 | PROCESSED | 57543.5182986111 | 55100 | 54731.4652430556 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 032009 | MCG--02-14-009 appears to have the strongest relativistic iron line of all the Seyfert 1s: a short 5 ks XMM-Newton observation found the line to have an EW 530-770 eV, two times larger than for MCG-6-30-15. We propose a 125 ks Suzaku observation of this AGN, which provides a unique opportunity to probe the innermost accretion disk in the region of strong gravity. The main goals are: (a) utilise the unique broad bandpass of Suzaku to detect the expected strong reflection hump and determine the form of the X-ray continuum; (b) accurately measure the relativistic iron K line profile and thereby the geometry of the X-ray emitting region and (c) determine whether the iron line responds to the continuum down to the orbital timescales of the inner disk. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | REEVES | JAMES | NULL | NULL | EUR | 3 | AO3 | MCG-02-14-009: PROBING THE PHYSICAL PROPERTIES OF THE STRONGEST IRON K LINE | HXD | Y |
| NGC 1448 | 56.1426 | -44.6942 | 251.59735556 | -51.37690943 | 264.6522 | 54879.3481828704 | 54880.4501041667 | 703062010 | 52965.3 | 50000 | 52965.3 | 52965.3 | 0 | 52965.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 55086.9 | 55086.9 | 95202 | 1 | PROCESSED | 57545.5960763889 | 55330 | 54893.4451041667 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 032018 | We propose for a 50 ks Suzaku observation of NGC 1448, a nearby (15 Mpc) gas-rich and dust-obscured Scd galaxy that is optically classified as an HII galaxy. From our Spitzer-IRS mid-IR spectroscopy, we have found the first evidence for an obscured AGN in NGC 1448. On the basis of this data, NGC 1448 appears to be harboring a rapidly growing small obscured black hole (M_BH ~ 6x10^5 M_Sun; Eddington ratio of >0.1), and therefore appears to be an analog of the nearby Compton-thick AGN NGC 4945. To date, no sensitive hard X-ray constraints exist for NGC 1448, which are required to provide a direct measurement of the absorption and mass accretion rate, and thus to test if NGC 1448 is also a Compton-thick AGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | ALEXANDER | DAVID | NULL | NULL | EUR | 3 | AO3 | NGC 1448: A MISSING COMPTON-THICK AGN IN OUR BACKYARD? | HXD | Y |
| 1ES1426+428 | 217.0602 | 42.6327 | 77.47261603 | 64.96709047 | 324.5702 | 54622.8702662037 | 54625.0856944444 | 703063010 | 101166.2 | 100000 | 101166.2 | 101174.2 | 0 | 101174.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 92145.6 | 92145.6 | 191393.7 | 3 | PROCESSED | 57542.7937731482 | 55003 | 54636.5084953704 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 032021 | Simultaneous optical/UV, X-ray and TeV observations are a powerful tool to study the innermost regions of blazar jets, probing the physical state of the jet close to its base. We propose to perform a long SUZAKU observation of the extreme hard-X-ray blazar 1ES 1426+428, simultaneously with MAGIC TeV observations, combined with a series of short Swift observations. With SUZAKU we will study the evolution of the X-ray emission over timescales of minutes-hours, providing important insight into the structure of the emission region and the physical process producing the radiation. We will characterize the synchrotron part of the SED and see how it correlates with the TeV spectrum, disentangling the main physical parameters and probing the still poorly known cosmic IR background. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TAGLIAFERRI | GIANPIERO | NULL | NULL | EUR | 3 | AO3 | THE EXTREME BLAZAR 1ES 1426+428: TESTING THE JET | HXD | Y |
| IRASF01475-0740 | 27.4875 | -7.3766 | 160.69718538 | -65.86110455 | 68.025 | 54661.0549652778 | 54662.3023032407 | 703065010 | 57914.7 | 50000 | 57914.7 | 57918.3 | 0 | 57926.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51125.7 | 51125.7 | 107698.8 | 0 | PROCESSED | 57543.0527546296 | 55051 | 54683.4056712963 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 032030 | We propose 50ks observations of IRASF01475-0740 and NGC 3147, both of which are Seyfert 2s apparently unobscured in X-rays. Unsatisfied with this apparent contradiction, we seek Suzaku observations with two main aims. First, high energy observations with the HXD can reveal whether a deeply buried AGN is present above 10 keV. Second, the XIS observations will probe sensitively for short time-scale variability below 10 keV, the detection of which would establish unambiguously that the objects have genuinely unobscured nuclei and rule out the alternatives of scattered light or X-ray binaries. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | NANDRA | KIRPAL | NULL | NULL | EUR | 3 | AO3 | SOLVING THE MYSTERY OF UNOBSCURED SEYFERT 2 GALAXIES | HXD | Y |
| MRK 573 | 26.0161 | 2.2904 | 148.3199793 | -57.9636564 | 249.71 | 55217.5861226852 | 55219.0328587963 | 704002010 | 64311.8 | 60000 | 64311.8 | 64311.8 | 0 | 64311.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 53747.1 | 53747.1 | 124992 | 0 | PROCESSED | 57550.3256944445 | 55612 | 55245.753599537 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040017 | Monte Carlo simulation is one of the best tools to study the complex spectra of Compton-thick AGNs and to figure out the relation between their nuclear structures and X-ray spectra. We have simulated X-ray spectra of Compton-thick AGNs obscured by an accretion torus, and found that observed spectra of Compton thick objects, Mrk 3 and NGC 2273 are well reproduced by the simulated X-ray spectra. Furthermore, our simulation predicts that there are many obscured AGNs with a heavily absorbed reflection component. Their spectra are similar to that predicted from synthesis modeling of the Cosmic X-ray Background. We propose Suzaku observations of candidates of the Compton thick AGNs, Mrk 573 and Mrk 78. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | AWAKI | HISAMITSU | NULL | NULL | JAP | 4 | AO4 | SEARCH FOR COMPTON THICK AGNS WITH A HEAVILY ABSORBED REFLECTION COMPONENT | HXD | Y |
| IC1586 | 11.9805 | 22.3783 | 121.86323541 | -40.48615304 | 70.9045 | 55006.4686458333 | 55007.0280555556 | 704005010 | 23530.6 | 20000 | 23530.6 | 24346.6 | 0 | 24354.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22277.8 | 22277.8 | 48325.9 | 0 | PROCESSED | 57547.6510648148 | 55385 | 55019.1259259259 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040049 | We propose the first X-ray follow-up observations of 4 gamma-ray bright Seyferts and starburst galaxy, recently discovered by Fermi gamma-ray space telescope. The detection of GeV emission provides new evidence for relativistic jets in radio-quiet AGNs, but steep gamma-ray spectrum as well as an exotic spectral energy distribution (where GeV flux is 2-4 orders of magnitude brighter than radio) indicates that non-thermal emission is relatively weak, and less enhanced compared to radio-loud AGNs. Throughout multiwavelength observations including Suzaku and Fermi satellites, we will investigate the jet power, accretion rate and line intensity of these new comers (i.e., gamma-loud Seyferts) towards the unification scheme of radio-loud and radio-quiet AGNs. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | KATAOKA | JUN | NULL | NULL | JAP | 4 | AO4 | SUZAKU OBSERVATIONS OF GAMMA-LOUD SEYFERTS AND STARBURST GALAXY | XIS | Y |
| 1216-015 | 184.787 | -1.8118 | 286.61259693 | 60.03288042 | 293.8466 | 55010.1063773148 | 55010.6043287037 | 704006010 | 20777.9 | 20000 | 20777.9 | 20785.9 | 0 | 20785.9 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57547.6897337963 | 55388 | 55020.3653009259 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040049 | We propose the first X-ray follow-up observations of 4 gamma-ray bright Seyferts and starburst galaxy, recently discovered by Fermi gamma-ray space telescope. The detection of GeV emission provides new evidence for relativistic jets in radio-quiet AGNs, but steep gamma-ray spectrum as well as an exotic spectral energy distribution (where GeV flux is 2-4 orders of magnitude brighter than radio) indicates that non-thermal emission is relatively weak, and less enhanced compared to radio-loud AGNs. Throughout multiwavelength observations including Suzaku and Fermi satellites, we will investigate the jet power, accretion rate and line intensity of these new comers (i.e., gamma-loud Seyferts) towards the unification scheme of radio-loud and radio-quiet AGNs. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | KATAOKA | JUN | NULL | NULL | JAP | 4 | AO4 | SUZAKU OBSERVATIONS OF GAMMA-LOUD SEYFERTS AND STARBURST GALAXY | XIS | Y |
| PKS1258-321 | 195.0396 | -32.3625 | 305.06853624 | 30.47306853 | 293.0551 | 55027.0059259259 | 55027.6050231482 | 704007010 | 28460.7 | 20000 | 28460.7 | 28732.7 | 0 | 28727.4 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 24027.5 | 24027.5 | 51755.9 | 0 | PROCESSED | 57547.8136921296 | 55406 | 55040.1188657407 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040049 | We propose the first X-ray follow-up observations of 4 gamma-ray bright Seyferts and starburst galaxy, recently discovered by Fermi gamma-ray space telescope. The detection of GeV emission provides new evidence for relativistic jets in radio-quiet AGNs, but steep gamma-ray spectrum as well as an exotic spectral energy distribution (where GeV flux is 2-4 orders of magnitude brighter than radio) indicates that non-thermal emission is relatively weak, and less enhanced compared to radio-loud AGNs. Throughout multiwavelength observations including Suzaku and Fermi satellites, we will investigate the jet power, accretion rate and line intensity of these new comers (i.e., gamma-loud Seyferts) towards the unification scheme of radio-loud and radio-quiet AGNs. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | KATAOKA | JUN | NULL | NULL | JAP | 4 | AO4 | SUZAKU OBSERVATIONS OF GAMMA-LOUD SEYFERTS AND STARBURST GALAXY | XIS | Y |
| 1739+518 | 264.9784 | 52.1719 | 79.52646168 | 31.85370007 | 22.9152 | 54985.7571759259 | 54986.3641087963 | 704008010 | 22486.8 | 20000 | 22494.8 | 22494.8 | 0 | 22486.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28237.8 | 28237.8 | 52431.9 | 0 | PROCESSED | 57547.4536458333 | 55367 | 54998.1968634259 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040049 | We propose the first X-ray follow-up observations of 4 gamma-ray bright Seyferts and starburst galaxy, recently discovered by Fermi gamma-ray space telescope. The detection of GeV emission provides new evidence for relativistic jets in radio-quiet AGNs, but steep gamma-ray spectrum as well as an exotic spectral energy distribution (where GeV flux is 2-4 orders of magnitude brighter than radio) indicates that non-thermal emission is relatively weak, and less enhanced compared to radio-loud AGNs. Throughout multiwavelength observations including Suzaku and Fermi satellites, we will investigate the jet power, accretion rate and line intensity of these new comers (i.e., gamma-loud Seyferts) towards the unification scheme of radio-loud and radio-quiet AGNs. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | KATAOKA | JUN | NULL | NULL | JAP | 4 | AO4 | SUZAKU OBSERVATIONS OF GAMMA-LOUD SEYFERTS AND STARBURST GALAXY | XIS | Y |
| NGC 454 | 18.511 | -55.3853 | 296.21074431 | -61.44696878 | 18.3891 | 54950.2291782407 | 54953.4023032407 | 704009010 | 128956.2 | 120000 | 128956.2 | 128956.2 | 0 | 128956.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 114596.9 | 114596.9 | 274129.6 | 0 | PROCESSED | 57546.5592361111 | 55342 | 54973.5148842593 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040050 | Seyfert galaxies with a low-mass central black hole are a key class of objects to study the growth phase of supermassive black holes. We propose to observe the hard X-ray brightest and low-mass (1.6e6 Msolar) Seyfert 2 galaxy NGC 454 selected from the Swift BAT survey. The data will be used (1) to measure broad-band X-ray spectrum and its variability, (2) to compare them with properties of known Seyferts, and (3) to search for variation of absorption to constrain the structure and origin of obscuring matter. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TERASHIMA | YUICHI | NULL | NULL | JAP | 4 | AO4 | X-RAY SPECTRAL VARIABILITY OF THE HARD X-RAY BRIGHTEST LOW-MASS SEYFERT 2 NGC 454 | HXD | Y |
| SWIFT J2052.0-5704 | 312.9788 | -57.0176 | 340.05945565 | -38.72742848 | 73.9304 | 54945.6280671296 | 54946.6863310185 | 704010010 | 45160 | 40000 | 45160 | 45168 | 0 | 45168 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 57624.2 | 57624.2 | 91409.8 | 1 | PROCESSED | 57546.2560416667 | 55339 | 54973.4487152778 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040059 | The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to the latetest population synthesis model, its estimate is strongly coupled with the broad band spectral shape of moderately absorbed AGNs, which is only poorly understood. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright, absorbed AGNs that can be best followed-up with Suzaku. Here we propose to observe three of them to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. With these observations we can make the spectral survey of bright absorbed Swift/BAT AGNs complete. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 4 | AO4 | SPECTRAL SURVEY OF A COMPLETE SAMPLE OF SWIFT/BAT SELECTED AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND | HXD | Y |
| SWIFT J1952.4+0237 | 298.0556 | 2.5705 | 42.31566647 | -12.27488447 | 82.9116 | 54929.8284722222 | 54931.1079166667 | 704011010 | 47921.1 | 40000 | 47925.9 | 47921.1 | 0 | 47925.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39304.4 | 39304.4 | 110525.8 | 2 | PROCESSED | 57546.1208680556 | 55324 | 54949.4878356482 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040059 | The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to the latetest population synthesis model, its estimate is strongly coupled with the broad band spectral shape of moderately absorbed AGNs, which is only poorly understood. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright, absorbed AGNs that can be best followed-up with Suzaku. Here we propose to observe three of them to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. With these observations we can make the spectral survey of bright absorbed Swift/BAT AGNs complete. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 4 | AO4 | SPECTRAL SURVEY OF A COMPLETE SAMPLE OF SWIFT/BAT SELECTED AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND | HXD | Y |
| 2MASX J02485937+2630 | 42.225 | 26.5707 | 153.13364356 | -29.32417791 | 74.088 | 55030.159224537 | 55031.3766782407 | 704013010 | 42950.1 | 40000 | 42950.1 | 43215.3 | 0 | 43224.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 29540.3 | 29540.3 | 105171.9 | 0 | PROCESSED | 57547.8817013889 | 55415 | 55048.2541435185 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040060 | Swift/BAT extragalactic survey above E>15 keV has provided us with the first unbiased AGN sample in the local universe. Here we propose to observe three Compton thick AGN candidates in the 22 months BAT catalog with Suzaku. To resolve the degeneracy of spectral modeling, the simultaneous wide-band coverage with the XIS and the HXD is crucial. This will lead us to the first reliable measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. We also aim to construct the template spectra of Compton thick AGNs, applicable to buried AGNs at high redshifts detected in deep surveys. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 4 | AO4 | DETERMINATION OF THE NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS | HXD | Y |
| UGC 12741 | 355.4449 | 30.6414 | 105.65559107 | -29.88276227 | 64.429 | 54989.5219560185 | 54990.6711111111 | 704014010 | 47945.8 | 40000 | 47953.8 | 47945.8 | 0 | 47945.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 41524.4 | 41524.4 | 99279.9 | 0 | PROCESSED | 57547.5132060185 | 55367 | 55001.0091435185 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040060 | Swift/BAT extragalactic survey above E>15 keV has provided us with the first unbiased AGN sample in the local universe. Here we propose to observe three Compton thick AGN candidates in the 22 months BAT catalog with Suzaku. To resolve the degeneracy of spectral modeling, the simultaneous wide-band coverage with the XIS and the HXD is crucial. This will lead us to the first reliable measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. We also aim to construct the template spectra of Compton thick AGNs, applicable to buried AGNs at high redshifts detected in deep surveys. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 4 | AO4 | DETERMINATION OF THE NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS | HXD | Y |
| NGC 4686 | 191.5508 | 54.5121 | 124.58283765 | 62.59936814 | 342.6621 | 54946.7002777778 | 54947.7564699074 | 704015010 | 44845.9 | 40000 | 44853.9 | 44845.9 | 0 | 44845.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42327.5 | 42327.5 | 91232 | 0 | PROCESSED | 57546.4795717593 | 55339 | 54973.9296875 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040060 | Swift/BAT extragalactic survey above E>15 keV has provided us with the first unbiased AGN sample in the local universe. Here we propose to observe three Compton thick AGN candidates in the 22 months BAT catalog with Suzaku. To resolve the degeneracy of spectral modeling, the simultaneous wide-band coverage with the XIS and the HXD is crucial. This will lead us to the first reliable measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. We also aim to construct the template spectra of Compton thick AGNs, applicable to buried AGNs at high redshifts detected in deep surveys. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 4 | AO4 | DETERMINATION OF THE NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS | HXD | Y |
| M33 X8 | 23.4834 | 30.5892 | 133.64723816 | -31.39681198 | 258.5185 | 55207.0743865741 | 55209.5626157407 | 704016010 | 106103.6 | 100000 | 106103.6 | 106106.1 | 0 | 106106.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 6105.3 | 6105.3 | 214957.7 | 1 | PROCESSED | 57550.3046412037 | 55587 | 55218.6414930556 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040067 | The nature of ultraluminous X-ray sources (ULXs) is one of the important unresolved issues in the modern astrophysics. In order to solve the problem, it is of crucial importance to observe X-ray spectra above 10 keV from ULXs, which enables us to determine precisely their spectral states. Therefore, Suzaku observations of two bright ULX, M33 X8 and IC 342 X2, are proposed. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | ISOBE | NAOKI | NULL | NULL | JAP | 4 | AO4 | HARD X-RAY STUDY OF ULTRALUMINOUS X-RAY SOURCES | HXD | Y |
| CENTAURUS_A | 201.3411 | -43.072 | 309.48969514 | 19.36734145 | 290.0008 | 55032.3718634259 | 55033.7683333333 | 704018010 | 62432.8 | 50000 | 62432.8 | 62688.8 | 0 | 62707.6 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 55450 | 55450 | 120649.9 | 3 | PROCESSED | 57547.9397569444 | 55415 | 55048.3403356482 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040085 | We propose to observe a nearby radio galaxy Centaurus A (Cen A) in order to search for non-thermal X-ray emission associated with a mis-alighned jet. Recently TeV gamma-ray was detected from M87 and nonthermal X-ray emission was detected from 3C120 with Suzaku, where they are not a blazar and harbor a mis-alighned jet. COMPTEL and EGRET reported a hint of gamma-ray emission from Cen A, but it has not been established. So far, only Seyfert-like thermal-Compoton powerlaw has been detected from Cen A. By taking advantage of Suzaku capability, we study a temporal spectral variation to extract nonthermal emission by considering a different variability time scale of accretion disk component and jet one, as demonstrated for 3C120 with Suzaku. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | FUKAZAWA | YASUSHI | NULL | NULL | JAP | 4 | AO4 | SEARCH FOR NON-THERMAL X-RAY EMISSION FROM A NEARBY RADIO GALAXY CENTAURUS A | HXD | Y |
| CENTAURUS_A | 201.3322 | -43.0688 | 309.48334217 | 19.37141452 | 298.7164 | 55048.3079513889 | 55049.7029398148 | 704018020 | 51278.7 | 50000 | 51278.7 | 51294.7 | 0 | 51286.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43733.2 | 43733.2 | 120505.9 | 1 | PROCESSED | 57548.0839699074 | 55430 | 55062.3520023148 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040085 | We propose to observe a nearby radio galaxy Centaurus A (Cen A) in order to search for non-thermal X-ray emission associated with a mis-alighned jet. Recently TeV gamma-ray was detected from M87 and nonthermal X-ray emission was detected from 3C120 with Suzaku, where they are not a blazar and harbor a mis-alighned jet. COMPTEL and EGRET reported a hint of gamma-ray emission from Cen A, but it has not been established. So far, only Seyfert-like thermal-Compoton powerlaw has been detected from Cen A. By taking advantage of Suzaku capability, we study a temporal spectral variation to extract nonthermal emission by considering a different variability time scale of accretion disk component and jet one, as demonstrated for 3C120 with Suzaku. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | FUKAZAWA | YASUSHI | NULL | NULL | JAP | 4 | AO4 | SEARCH FOR NON-THERMAL X-RAY EMISSION FROM A NEARBY RADIO GALAXY CENTAURUS A | HXD | Y |
| CENTAURUS_A | 201.3281 | -43.0649 | 309.48077241 | 19.37569293 | 303.3465 | 55057.3798148148 | 55059.1051388889 | 704018030 | 55944.2 | 50000 | 55952.2 | 55944.2 | 0 | 55944.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46491.5 | 46491.5 | 149047.8 | 3 | PROCESSED | 57548.1889699074 | 55434 | 55068.1674768518 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040085 | We propose to observe a nearby radio galaxy Centaurus A (Cen A) in order to search for non-thermal X-ray emission associated with a mis-alighned jet. Recently TeV gamma-ray was detected from M87 and nonthermal X-ray emission was detected from 3C120 with Suzaku, where they are not a blazar and harbor a mis-alighned jet. COMPTEL and EGRET reported a hint of gamma-ray emission from Cen A, but it has not been established. So far, only Seyfert-like thermal-Compoton powerlaw has been detected from Cen A. By taking advantage of Suzaku capability, we study a temporal spectral variation to extract nonthermal emission by considering a different variability time scale of accretion disk component and jet one, as demonstrated for 3C120 with Suzaku. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | FUKAZAWA | YASUSHI | NULL | NULL | JAP | 4 | AO4 | SEARCH FOR NON-THERMAL X-RAY EMISSION FROM A NEARBY RADIO GALAXY CENTAURUS A | HXD | Y |
| 3C 35 | 18.0181 | 49.4424 | 126.37585323 | -13.29131796 | 245.0044 | 55200.6165509259 | 55202.466875 | 704019010 | 84756.6 | 80000 | 85028.6 | 84756.6 | 0 | 85020.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 66314.3 | 66314.3 | 147577.8 | 2 | PROCESSED | 57550.0615277778 | 55584 | 55218.1479050926 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040096 | Suzaku observations of two giant radio galaxies, 3C 35 and DA 240, with a total size of about 1 Mpc are proposed, in order to detect diffuse inverse Compton X-ray emission from their radio lobes. The X-ray flux from the lobes, in comparison with the radio one, provides a precise determination of electron and magnetic field energies there. A comparison of them with those in smaller radio galaxies is used to probe into the history of jets and lobes. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | ISOBE | NAOKI | NULL | NULL | JAP | 4 | AO4 | SUZAKU OBSERVATION OF GIANT RADIO GALAXIES AS A PROBE OF JET HISTORY | XIS | Y |
| DA 240 EAST LOBE | 117.3573 | 55.877 | 161.8466677 | 30.16323196 | 293.7777 | 55274.9306134259 | 55276.7238657407 | 704020010 | 81783.4 | 80000 | 81783.4 | 81791.4 | 0 | 81791.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 74303.3 | 74303.3 | 154921.8 | 1 | PROCESSED | 57550.9753587963 | 55654 | 55286.3268518518 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040096 | Suzaku observations of two giant radio galaxies, 3C 35 and DA 240, with a total size of about 1 Mpc are proposed, in order to detect diffuse inverse Compton X-ray emission from their radio lobes. The X-ray flux from the lobes, in comparison with the radio one, provides a precise determination of electron and magnetic field energies there. A comparison of them with those in smaller radio galaxies is used to probe into the history of jets and lobes. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | ISOBE | NAOKI | NULL | NULL | JAP | 4 | AO4 | SUZAKU OBSERVATION OF GIANT RADIO GALAXIES AS A PROBE OF JET HISTORY | XIS | Y |
| SWIFT J1322.2-1641 | 200.5819 | -16.7858 | 313.4989766 | 45.45121448 | 290.037 | 55013.9738310185 | 55014.9981365741 | 704022010 | 41348.7 | 40000 | 41348.7 | 41620.7 | 0 | 41612.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36236.8 | 36236.8 | 88485.8 | 7 | PROCESSED | 57547.7444097222 | 55393 | 55027.0523148148 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 043059 | The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to the latetest population synthesis model, its estimate is strongly coupled with the broad band spectral shape of moderately absorbed AGNs, which is only poorly understood. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright, absorbed AGNs that can be best followed-up with Suzaku. Here we propose to observe three of them to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. With these observations we can make the spectral survey of bright absorbed Swift/BAT AGNs complete. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | UEDA | YOSHIHIRO | DADINA | MAURO | JEU | 4 | AO4 | SPECTRAL SURVEY OF A COMPLETE SAMPLE OF SWIFT/BAT SELECTED AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND | HXD | Y |
| MRK 352 | 14.9991 | 31.7575 | 125.05610732 | -31.07894727 | 255.5628 | 55202.4718402778 | 55203.6009143518 | 704025010 | 45671.7 | 40000 | 45687.7 | 45671.7 | 0 | 45687.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22369.3 | 22369.3 | 97535.8 | 1 | PROCESSED | 57550.0955439815 | 55602 | 55235.27125 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041402 | The Swift BAT survey has identified an unbiased sample of AGN at low z. In the 9-month AGN catalog, a sample of 153 AGN have been identified based on their 14-195 keV flux. Among these, we select a sample of 6 low luminosity Sy 1s for Suzaku follow-ups. All of these sources have low SNR 10 ks XMM-Newton spectra, showing the sources to be unobscured. Analysis of the proposed 40 ks Suzaku follow-ups will fill a gap in our knowledge of AGNs - revealing the 0.3-195 keV (Suzaku + BAT data) variability and spectral properties of this new class of poorly studied low luminosity unobscured AGNs. With Suzaku data available for Swift BAT-detected low luminosity obscured sources and many high luminosity Sy 1s, we will compare the properties of our target sources with both samples. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | WINTER | LISA | NULL | NULL | USA | 4 | AO4 | SUZAKU OBSERVATIONS OF THE LOW LUMINOSITY SEYFERT 1S IN THE SWIFT BAT SURVEY | HXD | Y |
| ESO 548-G081 | 55.4927 | -21.1949 | 213.74761618 | -50.8353425 | 69.3236 | 55046.3350462963 | 55047.1946064815 | 704026010 | 39411.2 | 40000 | 39419.2 | 39419.2 | 0 | 39411.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36142.9 | 36142.9 | 74259.9 | 0 | PROCESSED | 57548.0531481482 | 55427 | 55060.8071875 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041402 | The Swift BAT survey has identified an unbiased sample of AGN at low z. In the 9-month AGN catalog, a sample of 153 AGN have been identified based on their 14-195 keV flux. Among these, we select a sample of 6 low luminosity Sy 1s for Suzaku follow-ups. All of these sources have low SNR 10 ks XMM-Newton spectra, showing the sources to be unobscured. Analysis of the proposed 40 ks Suzaku follow-ups will fill a gap in our knowledge of AGNs - revealing the 0.3-195 keV (Suzaku + BAT data) variability and spectral properties of this new class of poorly studied low luminosity unobscured AGNs. With Suzaku data available for Swift BAT-detected low luminosity obscured sources and many high luminosity Sy 1s, we will compare the properties of our target sources with both samples. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | WINTER | LISA | NULL | NULL | USA | 4 | AO4 | SUZAKU OBSERVATIONS OF THE LOW LUMINOSITY SEYFERT 1S IN THE SWIFT BAT SURVEY | HXD | Y |
| SWIFT J0904.3+5538 | 136.117 | 55.5749 | 161.50516347 | 40.6960792 | 282.0039 | 54949.092025463 | 54949.700162037 | 704027010 | 41943.8 | 40000 | 41943.8 | 41943.8 | 0 | 41943.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 35883.8 | 35883.8 | 52535.9 | 1 | PROCESSED | 57546.4424537037 | 55343 | 54973.440474537 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041402 | The Swift BAT survey has identified an unbiased sample of AGN at low z. In the 9-month AGN catalog, a sample of 153 AGN have been identified based on their 14-195 keV flux. Among these, we select a sample of 6 low luminosity Sy 1s for Suzaku follow-ups. All of these sources have low SNR 10 ks XMM-Newton spectra, showing the sources to be unobscured. Analysis of the proposed 40 ks Suzaku follow-ups will fill a gap in our knowledge of AGNs - revealing the 0.3-195 keV (Suzaku + BAT data) variability and spectral properties of this new class of poorly studied low luminosity unobscured AGNs. With Suzaku data available for Swift BAT-detected low luminosity obscured sources and many high luminosity Sy 1s, we will compare the properties of our target sources with both samples. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | WINTER | LISA | NULL | NULL | USA | 4 | AO4 | SUZAKU OBSERVATIONS OF THE LOW LUMINOSITY SEYFERT 1S IN THE SWIFT BAT SURVEY | HXD | Y |
| MCG +04-22-042 | 140.9461 | 22.9693 | 205.9821846 | 43.11036681 | 106.3587 | 55157.3309259259 | 55158.2634143518 | 704028010 | 40962 | 40000 | 40994 | 40962 | 0 | 40986 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 35896.9 | 35896.9 | 80559.9 | 0 | PROCESSED | 57549.5187384259 | 55542 | 55176.1858101852 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041402 | The Swift BAT survey has identified an unbiased sample of AGN at low z. In the 9-month AGN catalog, a sample of 153 AGN have been identified based on their 14-195 keV flux. Among these, we select a sample of 6 low luminosity Sy 1s for Suzaku follow-ups. All of these sources have low SNR 10 ks XMM-Newton spectra, showing the sources to be unobscured. Analysis of the proposed 40 ks Suzaku follow-ups will fill a gap in our knowledge of AGNs - revealing the 0.3-195 keV (Suzaku + BAT data) variability and spectral properties of this new class of poorly studied low luminosity unobscured AGNs. With Suzaku data available for Swift BAT-detected low luminosity obscured sources and many high luminosity Sy 1s, we will compare the properties of our target sources with both samples. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | WINTER | LISA | NULL | NULL | USA | 4 | AO4 | SUZAKU OBSERVATIONS OF THE LOW LUMINOSITY SEYFERT 1S IN THE SWIFT BAT SURVEY | HXD | Y |
| UGC 6728 | 176.2197 | 79.6106 | 126.64092866 | 37.03371002 | 285.5693 | 54988.5646759259 | 54989.5125925926 | 704029010 | 49003.9 | 40000 | 49003.9 | 49003.9 | 0 | 49003.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41534.7 | 41534.7 | 81883.9 | 0 | PROCESSED | 57547.4998726852 | 55364 | 54998.3390740741 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041402 | The Swift BAT survey has identified an unbiased sample of AGN at low z. In the 9-month AGN catalog, a sample of 153 AGN have been identified based on their 14-195 keV flux. Among these, we select a sample of 6 low luminosity Sy 1s for Suzaku follow-ups. All of these sources have low SNR 10 ks XMM-Newton spectra, showing the sources to be unobscured. Analysis of the proposed 40 ks Suzaku follow-ups will fill a gap in our knowledge of AGNs - revealing the 0.3-195 keV (Suzaku + BAT data) variability and spectral properties of this new class of poorly studied low luminosity unobscured AGNs. With Suzaku data available for Swift BAT-detected low luminosity obscured sources and many high luminosity Sy 1s, we will compare the properties of our target sources with both samples. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | WINTER | LISA | NULL | NULL | USA | 4 | AO4 | SUZAKU OBSERVATIONS OF THE LOW LUMINOSITY SEYFERT 1S IN THE SWIFT BAT SURVEY | HXD | Y |
| MKN 279 | 208.2253 | 69.3021 | 115.05735618 | 46.87522986 | 345.4595 | 54965.2632407407 | 54968.6668287037 | 704031010 | 160351.4 | 150000 | 160359.4 | 160351.4 | 0 | 160359.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 150386 | 150386 | 293997.9 | 3 | PROCESSED | 57546.636099537 | 55345 | 54978.3987152778 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041403 | We aim to test if the high-luminosity Seyfert 1.5 Mkn 279 contains an ionized inner accretion disk by using Suzaku to spectroscopically separate the ionized and neutral reflectors. This source is relatively unobscured, allowing clear modeling of the shape of the strong soft excess; we will also test for a Fe K diskline component, which may be missing if the disk is ionized or truncated. Only a broadband X-ray spectrum, including simultaneous > 10 keV coverage to constrain Compton reflection, will allow us to thoroughly test blurred, ionized disk reflection models and constrain the nature of the reflector(s). | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MARKOWITZ | ALEX | NULL | NULL | USA | 4 | AO4 | DOES THE LOW-OBSCURATION, LOW-REFLECTION, HIGH-LUMINOSITY SEYFERT MKN279 CONTAIN AN IONIZED OR TRUNCATED ACCRETION DISK? | XIS | Y |
| MCG-2-58-22 | 346.1839 | -8.6878 | 64.09176202 | -58.7610593 | 247.1128 | 55167.9420486111 | 55170.9356365741 | 704032010 | 138968.8 | 130000 | 139008.8 | 138968.8 | 0 | 139008.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 105495.7 | 105495.7 | 258627.7 | 2 | PROCESSED | 57549.8017361111 | 55553 | 55187.5510763889 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041404 | We propose a 130 ks Suzaku long-look to study the Fe K emission complex of the Seyfert 1.5 AGN MCG--2-58-22, which has the unique combination of being X-ray bright, ``bare'' (i.e., lacking a strong ionized absorber), and possibly hosting both a truncated accretion disk and ionized circumnuclear material. We aim to accurately constrain the geometry and ionization state of the accreting circumnuclear material of this likely low-Compton reflection source by resolving the Fe K alpha line and constraining its origin, which may likely be a truncated thin disk, and verifying a previous claim of emission from H-like Fe. We will also determine the origin of this object's soft excess. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | MARKOWITZ | ALEX | NULL | NULL | USA | 4 | AO4 | A SUZAKU OBSERVATION OF MCG--2-58-22: A TRUNCATED OR IONIZED ACCRETION DISK? | XIS | Y |
| 1H0323+342 | 51.1507 | 34.2411 | 155.67406743 | -18.71640786 | 76.7168 | 55038.1604513889 | 55040.2084722222 | 704034010 | 84088.4 | 80000 | 84088.4 | 84240.4 | 0 | 84352.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 74297.9 | 74297.9 | 176937.9 | 0 | PROCESSED | 57548.0010532407 | 55419 | 55050.8162847222 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041408 | Recent radio observations reveal blazar-like properties in some radio-loud narrow line Seyfert-1 AGNs. 1H0323+342, classified as this class of AGNs, shows prominent hard X-ray emission with a hard photon index. Since the spectrum in hard X-ray is reminiscent of blazar, its X-ray spectrum seems to have different components originated from disk and jet. Thanks to sensitive X-ray detectors extending to the hard X-ray band, Suzaku observation is expected to resolve a possible multi-component structure in the spectrum. Since beamed radiation from jet is highly variable, spectral temporal behavior is also vital information to distinguish the emission origin. As this source is located relatively nearby (z=0.061), the source is an excellent target to investigate the emission from disk and jet. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | HAYASHIDA | MASAAKI | NULL | NULL | USA | 4 | AO4 | SUZAKU OBSERVATION OF 1H0323+342: A PECULIAR SEYFERT-1 --PROBING THE DISK AND JET CONNECTION IN AGN-- | HXD | Y |
| 3C 332 | 244.4239 | 32.3632 | 52.6372471 | 45.34839384 | 292.5008 | 55051.0341782407 | 55052.4655092593 | 704038010 | 59833.9 | 60000 | 59833.9 | 59833.9 | 0 | 59833.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46049.1 | 46049.1 | 123652 | 0 | PROCESSED | 57548.1132407407 | 55437 | 55067.2557986111 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041413 | We propose to observe the five most luminous type II AGN detected in the Swift BAT all sky hard X-ray survey (14-195~keV). Because BAT's detection efficiency for absorbed sources in the high energy band is very high, these sources are the most luminous (log($L_x$) $> 45.5$~ergs~sec$^{-1}$) absorbed tyoe II QSOs in the local universe and the most ripe for study with suzaku. 3C~332 is believed to be Compton-thick as suggested by chandra observations, and the newly discovered source SWIFT~J2344.6-4233 at a redshift of $z=0.6$ is the most luminous object in the BAT sample with log($L_x$) $=46.5$~ergs~sec$^{-1}$. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | BAUMGARTNER | WAYNE | NULL | NULL | USA | 4 | AO4 | SUZAKU OBSERVATIONS OF THE MOST LUMINOUS ABSORBED TYPE II QSOS | XIS | Y |
| PKS 0326-288 | 52.1551 | -28.6965 | 224.90475513 | -55.39691379 | 250.3682 | 55226.8889699074 | 55228.3266087963 | 704039010 | 58023.7 | 60000 | 58023.8 | 58023.7 | 0 | 58023.7 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 49624.7 | 49624.7 | 124185.9 | 3 | PROCESSED | 57550.4794560185 | 55616 | 55249.7586805556 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041413 | We propose to observe the five most luminous type II AGN detected in the Swift BAT all sky hard X-ray survey (14-195~keV). Because BAT's detection efficiency for absorbed sources in the high energy band is very high, these sources are the most luminous (log($L_x$) $> 45.5$~ergs~sec$^{-1}$) absorbed tyoe II QSOs in the local universe and the most ripe for study with suzaku. 3C~332 is believed to be Compton-thick as suggested by chandra observations, and the newly discovered source SWIFT~J2344.6-4233 at a redshift of $z=0.6$ is the most luminous object in the BAT sample with log($L_x$) $=46.5$~ergs~sec$^{-1}$. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | BAUMGARTNER | WAYNE | NULL | NULL | USA | 4 | AO4 | SUZAKU OBSERVATIONS OF THE MOST LUMINOUS ABSORBED TYPE II QSOS | XIS | Y |
| NGC985 | 38.6279 | -8.738 | 180.72422437 | -59.4803664 | 62.3866 | 55027.6174884259 | 55028.5925231482 | 704042010 | 31996.9 | 30000 | 31996.9 | 32006.3 | 0 | 32006.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25724.1 | 25724.1 | 84237.9 | 1 | PROCESSED | 57547.8515856482 | 55406 | 55040.2752430556 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041414 | We propose to use Suzaku to measure the amount of absorption, the intensity of Compton reflection component and other spectral components for a sample of 5 AGN selected from our ultra-deep, 3 Msec, INTEGRAL survey. These observations are ~3x deeper than the INTEGRAL and Swift/BAT all-sky surveys. Both the absorption distribution and the intensity of the Compton reflection component are fundamental parameters in understanding the AGN population. In fact, the uncertainty in the latter quantity is the main reason why the X-ray background can not be used to constrain the number of Compton Thick AGN. We have supporting multi-wavelength observations for all sources, critical to measure other source parameters like bolometric luminosity, re-radiated emission, black hole mass, etc. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | TREISTER | EZEQUIEL | NULL | NULL | USA | 4 | AO4 | THE NATURE OF THE FAINTEST HARD X-RAY SELECTED AGN | HXD | Y |
| IGRJ01528 | 28.2011 | -3.4464 | 157.35013019 | -62.14500791 | 77.3667 | 55007.0338078704 | 55008.1426388889 | 704043010 | 46915.9 | 40000 | 46915.9 | 47611.9 | 0 | 47624.8 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 42104.3 | 42104.3 | 95791.8 | 0 | PROCESSED | 57547.6882407407 | 55386 | 55019.1922337963 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041414 | We propose to use Suzaku to measure the amount of absorption, the intensity of Compton reflection component and other spectral components for a sample of 5 AGN selected from our ultra-deep, 3 Msec, INTEGRAL survey. These observations are ~3x deeper than the INTEGRAL and Swift/BAT all-sky surveys. Both the absorption distribution and the intensity of the Compton reflection component are fundamental parameters in understanding the AGN population. In fact, the uncertainty in the latter quantity is the main reason why the X-ray background can not be used to constrain the number of Compton Thick AGN. We have supporting multi-wavelength observations for all sources, critical to measure other source parameters like bolometric luminosity, re-radiated emission, black hole mass, etc. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TREISTER | EZEQUIEL | NULL | NULL | USA | 4 | AO4 | THE NATURE OF THE FAINTEST HARD X-RAY SELECTED AGN | XIS | Y |
| MRK1018 | 31.5471 | -0.2351 | 159.73232745 | -57.66458833 | 73.6945 | 55015.0121759259 | 55016.0939699074 | 704044010 | 43901.4 | 40000 | 43909.4 | 43901.4 | 0 | 43909.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37688.4 | 37688.4 | 93457.8 | 5 | PROCESSED | 57547.7689467593 | 55395 | 55027.1070023148 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041414 | We propose to use Suzaku to measure the amount of absorption, the intensity of Compton reflection component and other spectral components for a sample of 5 AGN selected from our ultra-deep, 3 Msec, INTEGRAL survey. These observations are ~3x deeper than the INTEGRAL and Swift/BAT all-sky surveys. Both the absorption distribution and the intensity of the Compton reflection component are fundamental parameters in understanding the AGN population. In fact, the uncertainty in the latter quantity is the main reason why the X-ray background can not be used to constrain the number of Compton Thick AGN. We have supporting multi-wavelength observations for all sources, critical to measure other source parameters like bolometric luminosity, re-radiated emission, black hole mass, etc. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TREISTER | EZEQUIEL | NULL | NULL | USA | 4 | AO4 | THE NATURE OF THE FAINTEST HARD X-RAY SELECTED AGN | HXD | Y |
| MCG0208 | 43.0963 | -8.5129 | 185.55840319 | -55.88722126 | 57.4541 | 55016.0987037037 | 55017.2134722222 | 704045010 | 42911.5 | 40000 | 42943.5 | 42911.5 | 0 | 42919.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36787.8 | 36787.8 | 96286 | 5 | PROCESSED | 57547.7724768518 | 55395 | 55027.1160532407 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041414 | We propose to use Suzaku to measure the amount of absorption, the intensity of Compton reflection component and other spectral components for a sample of 5 AGN selected from our ultra-deep, 3 Msec, INTEGRAL survey. These observations are ~3x deeper than the INTEGRAL and Swift/BAT all-sky surveys. Both the absorption distribution and the intensity of the Compton reflection component are fundamental parameters in understanding the AGN population. In fact, the uncertainty in the latter quantity is the main reason why the X-ray background can not be used to constrain the number of Compton Thick AGN. We have supporting multi-wavelength observations for all sources, critical to measure other source parameters like bolometric luminosity, re-radiated emission, black hole mass, etc. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TREISTER | EZEQUIEL | NULL | NULL | USA | 4 | AO4 | THE NATURE OF THE FAINTEST HARD X-RAY SELECTED AGN | XIS | Y |
| NGC1194 | 45.9522 | -1.1044 | 179.17914291 | -48.96176874 | 76.9913 | 55044.6911689815 | 55045.8141087963 | 704046010 | 50316.1 | 50000 | 50316.1 | 50596.1 | 0 | 50596.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48426.8 | 48426.8 | 97003.8 | 1 | PROCESSED | 57548.0499074074 | 55427 | 55061.5275115741 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041414 | We propose to use Suzaku to measure the amount of absorption, the intensity of Compton reflection component and other spectral components for a sample of 5 AGN selected from our ultra-deep, 3 Msec, INTEGRAL survey. These observations are ~3x deeper than the INTEGRAL and Swift/BAT all-sky surveys. Both the absorption distribution and the intensity of the Compton reflection component are fundamental parameters in understanding the AGN population. In fact, the uncertainty in the latter quantity is the main reason why the X-ray background can not be used to constrain the number of Compton Thick AGN. We have supporting multi-wavelength observations for all sources, critical to measure other source parameters like bolometric luminosity, re-radiated emission, black hole mass, etc. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | TREISTER | EZEQUIEL | NULL | NULL | USA | 4 | AO4 | THE NATURE OF THE FAINTEST HARD X-RAY SELECTED AGN | XIS | Y |
| NGC 4138 | 182.4434 | 43.7345 | 147.09151655 | 71.38668226 | 137.6226 | 55137.5331365741 | 55138.8849305556 | 704047010 | 60771.6 | 60000 | 60843.6 | 60771.6 | 0 | 60843.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35872.4 | 35872.4 | 116781.8 | 2 | PROCESSED | 57549.0852893518 | 55517 | 55151.1923263889 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041415 | The SWIFT BAT hard (14-195 KeV) survey is performing the first unbiased hard X-ray survey of the entire sky with follow-up observations with the Swift XRT to fully identify the sample. In this survey we have found two very low luminosity nearby hard X-ray sources which show little, if any, evidence for nuclear activity in the optical or UV band, and have very low apparent Eddington ratios. We propose Suzaku observations of these objects to determine whether there is an X-ray spectral signature of a low Eddington ratio, as predicted if these objects are indeed in a radiatively inefficient accretion flow. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | MUSHOTZKY | RICHARD | NULL | NULL | USA | 4 | AO4 | SUZAKU OBSERVATIONS OF NGC4138 AND NGC3718 | HXD | Y |
| NGC 3718 | 173.2341 | 53.1118 | 146.87581124 | 60.21394242 | 142.7392 | 55128.8497800926 | 55130.255775463 | 704048010 | 59888.2 | 60000 | 59920.2 | 59888.2 | 0 | 59920.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 52439.2 | 52439.2 | 121459.9 | 0 | PROCESSED | 57548.9845138889 | 55507 | 55141.3212384259 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041415 | The SWIFT BAT hard (14-195 KeV) survey is performing the first unbiased hard X-ray survey of the entire sky with follow-up observations with the Swift XRT to fully identify the sample. In this survey we have found two very low luminosity nearby hard X-ray sources which show little, if any, evidence for nuclear activity in the optical or UV band, and have very low apparent Eddington ratios. We propose Suzaku observations of these objects to determine whether there is an X-ray spectral signature of a low Eddington ratio, as predicted if these objects are indeed in a radiatively inefficient accretion flow. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | MUSHOTZKY | RICHARD | NULL | NULL | USA | 4 | AO4 | SUZAKU OBSERVATIONS OF NGC4138 AND NGC3718 | HXD | Y |
| SDSS J1352+4239 | 208.1832 | 42.6476 | 88.11360974 | 70.09649039 | 316.6443 | 54984.9959375 | 54985.7502199074 | 704050010 | 32074.5 | 30000 | 32082.5 | 32074.5 | 0 | 32082.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 29502.1 | 29502.1 | 65163.9 | 0 | PROCESSED | 57547.4324652778 | 55364 | 54994.4273032407 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041422 | BALQSOs can be used to probe geometric and evolutionary models of quasars and AGN feedback. Recent studies have found larger (~2X) BALQSO fractions in NIR selected samples compared to those in optical samples and have suggested that the NIR samples of BALQSOs better represent the general population of BALQSOs. We propose to observe three bright, red 2MASS selected BALQSOs with Suzaku, to complement archival X-ray observations of BALQSOs that may have been biased by their selection on optical properties only. Combined with the archival sample, we will measure the average X-ray properties of BALQSOs. By comparing the hard X-ray to K_s band flux ratios at a range of optical to infrared colors, we will test the robustness of NIR selection and the origin of the large NIR BALQSO fraction. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | DAI | XINYU | NULL | NULL | USA | 4 | AO4 | X-RAY PROPERTIES OF 2MASS SELECTED BALQSOS | XIS | Y |
| SDSS J1723+5553 | 260.8912 | 55.8942 | 83.89291292 | 34.34970174 | 8.0654 | 54986.3677777778 | 54986.8148032407 | 704051010 | 35936.8 | 30000 | 35944.8 | 35936.8 | 0 | 35952.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 29039.3 | 29039.3 | 38615.9 | 0 | PROCESSED | 57547.4618865741 | 55364 | 54998.1759722222 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041422 | BALQSOs can be used to probe geometric and evolutionary models of quasars and AGN feedback. Recent studies have found larger (~2X) BALQSO fractions in NIR selected samples compared to those in optical samples and have suggested that the NIR samples of BALQSOs better represent the general population of BALQSOs. We propose to observe three bright, red 2MASS selected BALQSOs with Suzaku, to complement archival X-ray observations of BALQSOs that may have been biased by their selection on optical properties only. Combined with the archival sample, we will measure the average X-ray properties of BALQSOs. By comparing the hard X-ray to K_s band flux ratios at a range of optical to infrared colors, we will test the robustness of NIR selection and the origin of the large NIR BALQSO fraction. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | DAI | XINYU | NULL | NULL | USA | 4 | AO4 | X-RAY PROPERTIES OF 2MASS SELECTED BALQSOS | XIS | Y |
| SDSS J0943+5417 | 145.8252 | 54.2751 | 161.23003018 | 46.41565232 | 274.2141 | 54975.5889236111 | 54976.3473611111 | 704052010 | 34226.4 | 30000 | 34226.4 | 34226.4 | 0 | 34226.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32059.1 | 32059.1 | 65517.9 | 2 | PROCESSED | 57546.6638773148 | 55358 | 54992.6588888889 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041422 | BALQSOs can be used to probe geometric and evolutionary models of quasars and AGN feedback. Recent studies have found larger (~2X) BALQSO fractions in NIR selected samples compared to those in optical samples and have suggested that the NIR samples of BALQSOs better represent the general population of BALQSOs. We propose to observe three bright, red 2MASS selected BALQSOs with Suzaku, to complement archival X-ray observations of BALQSOs that may have been biased by their selection on optical properties only. Combined with the archival sample, we will measure the average X-ray properties of BALQSOs. By comparing the hard X-ray to K_s band flux ratios at a range of optical to infrared colors, we will test the robustness of NIR selection and the origin of the large NIR BALQSO fraction. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | DAI | XINYU | NULL | NULL | USA | 4 | AO4 | X-RAY PROPERTIES OF 2MASS SELECTED BALQSOS | XIS | Y |
| IC 2497 | 145.222 | 34.6799 | 190.267728 | 48.8163504 | 306.2341 | 54939.6906365741 | 54941.5550810185 | 704053010 | 76483.7 | 75000 | 76483.7 | 76483.7 | 0 | 76483.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 63948 | 63948 | 161047.8 | 2 | PROCESSED | 57546.2140046296 | 55318 | 54952.1320717593 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041432 | The discovery of `Hanny's Voorwerp' near IC 2497 opens an unprecedented window into the time evolution of a single AGN on timescales up to 100,000 years. Based on its properties, the Voorwerp was illuminated by a luminous AGN ~100,000 years ago, but the AGN host galaxy - IC 2497 - does not seem to host a sufficiently luminous AGN. Thus, IC 2497 either hosts a highly obscured AGN only detectable in hard X-rays, or it has dropped in luminosity by a factor of 10-1000. We propose to observe IC 2497 with Suzaku for 75 ksec to determine the hard X-ray luminosity and spectrum to measure the amount of obscuration and the current intrinsic luminosity of its AGN. Only with hard X-ray observations can we break the degeneracy between obscuration and decrease in luminosity. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | SCHAWINSKI | KEVIN | NULL | NULL | USA | 4 | AO4 | HOW FAST CAN AN AGN SHUT DOWN? - SUZAKU OBSERVATION OF IC 2497 AND `HANNY'S VOORWERP' | HXD | Y |
| MR 2251-178 | 343.5217 | -17.5814 | 46.19628588 | -61.32288878 | 63.4108 | 54958.1447222222 | 54961.4675231482 | 704055010 | 136924 | 130000 | 136932 | 136924 | 0 | 136939.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 112163.7 | 112163.7 | 287057.6 | 2 | PROCESSED | 57546.6278009259 | 55343 | 54976.3091782407 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 042002 | The bright, nearby (z=0.06398) QSO MR 2251-178 was the first AGN where a warm absorber was detected. There are now thought to be at least two warm absorber components in MR 2251-178; a low ionisation soft X-ray absorber and a putative high velocity (13000 km/s) high ionisation wind, which exhibits absorption lines in the iron K-shell band. We propose a 130 ks observation with Suzaku of MR 2251-178 with the primary goals; (i) to establish the nature of the high ionisation absorber, e.g. an accretion disk wind, through unprecedented high S/N observations in the iron K band with XIS; (ii) to determine the physical parameters of the soft X-ray warm absorber and (iii) to characterise the ionised reflection component and high-energy cut-off thanks to the high energy sensitivity of the HXD. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | REEVES | JAMES | FUKAZAWA | YASUSHI | EUR | 4 | AO4 | PROBING THE OUTFLOWING WIND IN MR 2251-178 | XIS | Y |
| NGC4102 | 181.5322 | 52.6534 | 138.20676485 | 63.11040703 | 305.2196 | 54981.0678009259 | 54983.4203009259 | 704057010 | 105557.9 | 100000 | 105581.9 | 105557.9 | 0 | 105565.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 97280.2 | 97280.2 | 203213.9 | 2 | PROCESSED | 57547.4983912037 | 55363 | 54994.4413541667 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 042014 | The nature of Low Ionization Nuclear Emission-line Region (LINER) galaxies has been the subject of a strong controversy. The distinction between LINER nuclei and other families of Active Galactic Nuclei (AGN) can be due to different amounts and/or properties of the obscuring material. A high population of LINERs are Compton-thick candidates. However the Equivalent Width (EW) of the FeKa emission line are lower than those measured for Compton-thick AGN. We propose to use the unprecedented sensitivity of HXD and XIS on board Suzaku to study NGC4102, one of the brightest LINER in the 36-month Swift/BAT survey. NGC4102 is a Compton-thick LINER candidate with EW(FeKa)<500keV, it is therefore an ideal case to investigate the properties of absorption and the FeKa emission line. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | GONZALEZ-MARTIN | OMAIRA | NULL | NULL | EUR | 4 | AO4 | PROBING COMPTON-THICK OBSCURATION AND LOW EW(FEKA) OF LINERS: THE CASE OF NGC4102 | HXD | Y |
| IRAS 04507+0358 | 73.3635 | 4.1233 | 194.58361833 | -23.84576016 | 98.871 | 55075.0228356482 | 55078.1356481482 | 704058010 | 109052.4 | 100000 | 109052.4 | 109052.4 | 0 | 109052.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 84109.8 | 84109.8 | 268911.8 | 3 | PROCESSED | 57548.5242939815 | 55476 | 55109.5623842593 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 042022 | According to X-ray synthesis models, Compton-thick AGN (NH>1e24 cm-2) should represent 50% of the total absorbed AGN population. Despite their importance in the cosmological context, only a few of them have been found so far. We have selected a well-defined sample of 31 Compton-thick candidates on the basis on their FX/FIR and X-ray colors. Due to the heavy obscuration, data above 10 keV are fundamental to unveil these sources. We ask here deep Suzaku observations (100 ks on each source) for 2 sources of our sample for which data at energy >10keV are not available yet. These observations will allow to complete the physical characterization (NH and LX) of the bright tail (F(2-10 keV)>5e-12 cgs) of our sample and to add more information to test the prediction of the AGN synthesis model. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | SEVERGNINI | PAOLA | NULL | NULL | EUR | 4 | AO4 | SUZAKU OBSERVATIONS OF COMPTON-THICK CANDIDATES | HXD | Y |
| IGR J22517+2218 | 342.9769 | 22.2871 | 89.68946946 | -32.75751552 | 253.7359 | 55161.7610648148 | 55163.0086111111 | 704060010 | 52726.5 | 50000 | 52726.5 | 52726.5 | 0 | 52726.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40116.4 | 40116.4 | 107777.9 | 0 | PROCESSED | 57549.6312152778 | 55545 | 55179.2471527778 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 042027 | We propose to observe 4 high-z QSOs observed by INTEGRAL, two of which are newly discovered in hard X-rays. The broadband and the good energy resolution will allow to investigate the spectral behaviour at low energies, and in particular to constraint true absorption $vs$ continuum features scenario. Particularly intriguing is the possible presence of a bulk Compton motion component. A self consistent test of this model could be derived by measuring the peak energy of the Inverse Compton component in the SED, a requirement that further strenghtens the need of a broadband observation with Suzaku. Simultaneous optical, hard X and gamma-ray observations available through WEBT, INTEGRAL and AGILE will also improve the feasibility of the proposed program. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | DE ROSA | ALESSANDRA | NULL | NULL | EUR | 4 | AO4 | SUZAKU OBSERVATION A SAMPLE OF FOUR RADIO-LOUD/HIGH REDSHIFT QSOS OBSERVED BY INTEGRAL | XIS | Y |
| NGC3516 | 166.8656 | 72.6213 | 133.14023939 | 42.38468378 | 135.8338 | 55132.2328125 | 55137.5272453704 | 704062010 | 251355.5 | 250000 | 251379.5 | 251371.5 | 0 | 251355.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 190837.2 | 190837.2 | 333010 | 5 | PROCESSED | 57549.2037268518 | 54922 | 55152.2729398148 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 046003 | We propose deep Suzaku observations of 6 well-known AGN with the primary aim of studying strong-gravitational physics close to these supermassive black holes (SMBH). We will conduct the first ever census of local SMBH spin, providing a new window on the growth-history of SMBHs. Suzaku's unique combination of high-throughput in the iron-K band and hard-band (>10keV) sensitivity is crucial, permitting a separation of the disk-reflection spectrum (which encodes the relativistic physics) from the effects of the warm absorber and low-velocity emission/reflection. These six datasets will be an important legacy of Suzaku, providing an important resource for AGN researchers for at least the next decade. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | REYNOLDS | CHRISTOPHER | NULL | NULL | USA | 4 | AO4 | A SURVEY OF BLACK HOLE SPIN AND RELATIVISTIC PHYSICS IN AGN | HXD | Y |
| NGC3783 | 174.7201 | -37.7846 | 287.44066962 | 22.89477473 | 305.9228 | 55022.9100115741 | 55027.0016087963 | 704063010 | 209503.4 | 200000 | 209503.4 | 210311.4 | 0 | 210319.4 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 174040.4 | 174040.4 | 353453.5 | 2 | PROCESSED | 57547.9411342593 | 54922 | 55040.5612615741 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 046003 | We propose deep Suzaku observations of 6 well-known AGN with the primary aim of studying strong-gravitational physics close to these supermassive black holes (SMBH). We will conduct the first ever census of local SMBH spin, providing a new window on the growth-history of SMBHs. Suzaku's unique combination of high-throughput in the iron-K band and hard-band (>10keV) sensitivity is crucial, permitting a separation of the disk-reflection spectrum (which encodes the relativistic physics) from the effects of the warm absorber and low-velocity emission/reflection. These six datasets will be an important legacy of Suzaku, providing an important resource for AGN researchers for at least the next decade. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | REYNOLDS | CHRISTOPHER | NULL | NULL | USA | 4 | AO4 | A SURVEY OF BLACK HOLE SPIN AND RELATIVISTIC PHYSICS IN AGN | HXD | Y |
| 1H 0419-577 | 66.5658 | -57.2343 | 267.01881665 | -41.95465908 | 226.9739 | 55212.4834259259 | 55214.8224421296 | 704064010 | 122835.4 | 140000 | 123115.4 | 122835.4 | 0 | 123115.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 113439.2 | 113439.2 | 202066.8 | 4 | PROCESSED | 57550.2328472222 | 55594 | 55228.2152893518 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041417 | A 'hard excess' has been detected in 2007 Suzaku PIN data for the nearby quasar 1H 0419-577 relative to models fitting below 10 keV. The excess can be accounted for with Compton-thick partial-covering gas probably part of a clumpy disk wind originating inside of the BLR. The observed Fe Ka line luminosity is consistent with an origin in an equatorial wind. Blurred reflection models cannot satisfactorily fit the source and so 1H0419-577 provides a rare distinction between two observationally-similar classes of model. We propose two 140 ks follow-up Suzaku observations separated by months to probe the properties of the Compton-thick gas via variability measurements: this is an important new science area that can only be studied using the broad bandpass available from Suzaku. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | TURNER | TRACEY | NULL | NULL | USA | 4 | AO4 | STUDYING THE COMPTON-THICK PARTIAL-COVERING ABSORPTION IN 1H 0419-577 | HXD | Y |
| MRK 18 | 135.5092 | 60.0703 | 155.86471567 | 39.40052697 | 266.8203 | 55330.5025810185 | 55331.3772106482 | 705001010 | 37966.7 | 40000 | 37974.7 | 37974.7 | 0 | 37966.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34667 | 34667 | 75553.9 | 1 | PROCESSED | 57551.5224074074 | 55769 | 55403.0749768518 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050003 | We propose to observe two Swift/BAT selected obscured AGNs with significant scattered emission, Mrk 18 and Ark 347. Hard X-ray selected AGNs show some peculiar characteristics compared to optically selected ones such as weak scattering emission from the opening part of the putative torus and weak plasma emission in the soft X-ray band. The targets are Swift/BAT selected AND show significant scattered emission, which are poorly explored with Suzaku so far. Our aims are to constrain the geometrical structure of the obscuring matter based on broad-band X-ray spectra and compare them with other hard X-ray or optically selected obscured AGNs. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | TERASHIMA | YUICHI | NULL | NULL | JAP | 5 | AO5 | THE STRUCTURE OF COMPTON-THIN AGNS WITH SIGNIFICANT SCATTERED EMISSION SELECTED BY SWIFT/BAT | HXD | Y |
| ARK 347 | 181.0952 | 20.2476 | 243.01628342 | 77.22827936 | 294.4295 | 55377.99625 | 55378.8668171296 | 705002010 | 38972.6 | 40000 | 38988.6 | 38972.6 | 0 | 38988.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35987.6 | 35987.6 | 75209.9 | 0 | PROCESSED | 57552.4401851852 | 55772 | 55404.2387268518 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050003 | We propose to observe two Swift/BAT selected obscured AGNs with significant scattered emission, Mrk 18 and Ark 347. Hard X-ray selected AGNs show some peculiar characteristics compared to optically selected ones such as weak scattering emission from the opening part of the putative torus and weak plasma emission in the soft X-ray band. The targets are Swift/BAT selected AND show significant scattered emission, which are poorly explored with Suzaku so far. Our aims are to constrain the geometrical structure of the obscuring matter based on broad-band X-ray spectra and compare them with other hard X-ray or optically selected obscured AGNs. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | TERASHIMA | YUICHI | NULL | NULL | JAP | 5 | AO5 | THE STRUCTURE OF COMPTON-THIN AGNS WITH SIGNIFICANT SCATTERED EMISSION SELECTED BY SWIFT/BAT | HXD | Y |
| 1150+497 | 178.3624 | 49.5318 | 145.51949415 | 64.97605225 | 131.4133 | 55512.7136805556 | 55514.1042824074 | 705003010 | 105655.8 | 100000 | 105711.8 | 105655.8 | 0 | 105719.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 84643.8 | 84643.8 | 120128 | 1 | PROCESSED | 57554.1053356482 | 55892 | 55524.2197337963 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050007 | A Suzaku observation of the iron line emitting blazar 1150+497 is proposed. The object is reported to exhibit a signature iron line. By measuring the equivalent width and line width, Suzaku will reveal the state of the accretion disc with the jet activity. It is notable that the blazar, aligning the jet with the line of sight, allow us to observe the jet and the accretion disc with a sufficient isochronism even with the violently variable sources. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | SETA | HIROMI | NULL | NULL | JAP | 5 | AO5 | SUZAKU OBSERVATION OF AN FE-LINE BLAZAR 1150+497 | XIS | Y |
| PBC J0216.1+5124 | 34.0954 | 51.5104 | 136.13174863 | -9.17115539 | 78.3815 | 55421.9728356482 | 55423.4168171296 | 705006010 | 72773.3 | 80000 | 72796.4 | 72773.3 | 0 | 72796.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 73558.2 | 73558.2 | 124725.8 | 3 | PROCESSED | 57553.114375 | 55804 | 55435.2980092593 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050024 | The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to population synthesis models, its estimate is strongly coupled with the broad band spectral shape of Compton thin AGNs. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright AGNs that can be best followed-up with Suzaku. Previously, such studies have been limited to AGNs with low to intermediate luminosities. Here we propose to observe two of the most luminous AGNs in the latest BAT catalog to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 5 | AO5 | BROAD BAND SPECTRA OF SWIFT/BAT SELECTED ULTRALUMINOUS AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND | HXD | Y |
| PBC J0839.7-1214 | 129.9392 | -12.3029 | 237.21342575 | 17.37856511 | 291.8979 | 55324.6892824074 | 55326.4896990741 | 705007010 | 80564.3 | 80000 | 80564.3 | 80564.3 | 0 | 80564.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70741.8 | 70741.8 | 155535.8 | 1 | PROCESSED | 57551.4721759259 | 55707 | 55341.5690856482 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050024 | The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to population synthesis models, its estimate is strongly coupled with the broad band spectral shape of Compton thin AGNs. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright AGNs that can be best followed-up with Suzaku. Previously, such studies have been limited to AGNs with low to intermediate luminosities. Here we propose to observe two of the most luminous AGNs in the latest BAT catalog to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 5 | AO5 | BROAD BAND SPECTRA OF SWIFT/BAT SELECTED ULTRALUMINOUS AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND | HXD | Y |
| ESO 428-G014 | 109.1256 | -29.3248 | 241.87528565 | -7.96864273 | 123.1273 | 55516.1372569445 | 55518.5508680556 | 705008010 | 82887.3 | 80000 | 82903.3 | 82887.3 | 0 | 82903.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 68451.8 | 68451.8 | 208501.6 | 2 | PROCESSED | 57554.1967361111 | 55898 | 55530.4256597222 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050031 | Non-Hidden Broad Line Region Seyfert 2 galaxies (NHBLR Sey2s) are classified as Seyfert 2 galaxies without broad Balmer lines even in the polarized light. One possible interpretation for the absence of broad lines is that NHBLR Sey2s are viewed from an extreme edge-on direction, so that the scattered light is obscured by the accretion torus. Hence observation of NHBLR Sey2s provides us the unique opportunity to investigate the densest region of the torus. We, therefore, propose 80 ksec observation of NHBLR Sey2 ESO 428-G014. High sensitivity throughout the 0.5-70 keV wide energy band of Suzaku allows us to strictly constrain the intrinsic X-ray luminosity and column density of the obscuring material. From our observation, we expect to derive more complete unified picture of AGNs. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | HABA | YOSHITO | NULL | NULL | JAP | 5 | AO5 | SUZAKU VIEW OF NON-HIDDEN BROAD LINE REGION SEYFERT 2 GALAXY ESO 428-G014 | XIS | Y |
| IC 342 X2 | 56.516 | 68.1498 | 138.08335694 | 10.57829767 | 91.9969 | 55415.9786689815 | 55417.3765625 | 705009010 | 74379 | 80000 | 74379 | 74379 | 0 | 74379 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 64131.6 | 64131.6 | 120767.9 | 0 | PROCESSED | 57552.9205671296 | 55794 | 55428.1624537037 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050041 | The nature of ultraluminous X-ray sources (ULXs) is one of the important unresolved issues in the modern astrophysics. A Suzaku HXD spectrum above 10 keV and its variation, in combination with those with XIS, provide us with an unique opportunity to determine unambiguously the physical state of ULXs, which is a key information to solve their nature. Here, two 80 ks Suzaku exposures are proposed on a bright ULX IC 342 X2, one of the most promising candidates for hard X-ray detection. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ISOBE | NAOKI | NULL | NULL | JAP | 5 | AO5 | HARD X-RAY STUDY OF ULTRALUMINOUS X-RAY SOURCES WITH SUZAKU | XIS | Y |
| IC 342 X2 | 56.548 | 68.1243 | 138.10903546 | 10.56584534 | 237.0509 | 55640.3693981482 | 55641.8058101852 | 705009020 | 75446.7 | 80000 | 75470.7 | 75446.7 | 0 | 75478.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 74257.7 | 74257.7 | 124089.8 | 1 | PROCESSED | 57601.2497800926 | 56019 | 55652.0183680556 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050041 | The nature of ultraluminous X-ray sources (ULXs) is one of the important unresolved issues in the modern astrophysics. A Suzaku HXD spectrum above 10 keV and its variation, in combination with those with XIS, provide us with an unique opportunity to determine unambiguously the physical state of ULXs, which is a key information to solve their nature. Here, two 80 ks Suzaku exposures are proposed on a bright ULX IC 342 X2, one of the most promising candidates for hard X-ray detection. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ISOBE | NAOKI | NULL | NULL | JAP | 5 | AO5 | HARD X-RAY STUDY OF ULTRALUMINOUS X-RAY SOURCES WITH SUZAKU | XIS | Y |
| EMS0071 | 16.6433 | 48.9425 | 125.49064727 | -13.85403968 | 69.9406 | 55392.4123148148 | 55392.8855092593 | 705010010 | 23010.2 | 20000 | 23010.2 | 23010.2 | 0 | 23010.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19568 | 19568 | 40881.9 | 0 | PROCESSED | 57552.6419560185 | 55779 | 55411.2637384259 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050050 | We propose to observe with Suzaku a selected set of 7 Fermi-LAT observed high galactic latitude gamma-ray sources that have no identified counterpart in any other energy range. These sources have been detected by the Fermi-LAT with high confidence and are either active galactic nuclei, galactic pulsars, or an as-yet unidentified new class of gamma-ray sources. The proposed observations are for 40 ks or 20 ks per source covering the Fermi-LAT source error region allowing us to detect sources to a flux level several times 10^(-14) erg/cm^2/s. We will determine the X-ray counterpart within the Fermi-LAT error circle, and characterize its variability and spectral properties to reveal the nature of "GeV dark accelerators". | EXTRAGALACTIC COMPACT SOURCES | 7 | A | KATAOKA | JUN | NULL | NULL | JAP | 5 | AO5 | SUZAKU FOLLOW-UP OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE | XIS | Y |
| EMS0857 | 198.1882 | 0.8497 | 314.828891 | 63.22804034 | 111.0249 | 55578.1935532407 | 55578.746087963 | 705011010 | 22070 | 20000 | 22078 | 22070 | 0 | 22085 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15326.7 | 15326.7 | 47727.9 | 0 | PROCESSED | 57600.6315046296 | 55962 | 55595.4732986111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050050 | We propose to observe with Suzaku a selected set of 7 Fermi-LAT observed high galactic latitude gamma-ray sources that have no identified counterpart in any other energy range. These sources have been detected by the Fermi-LAT with high confidence and are either active galactic nuclei, galactic pulsars, or an as-yet unidentified new class of gamma-ray sources. The proposed observations are for 40 ks or 20 ks per source covering the Fermi-LAT source error region allowing us to detect sources to a flux level several times 10^(-14) erg/cm^2/s. We will determine the X-ray counterpart within the Fermi-LAT error circle, and characterize its variability and spectral properties to reveal the nature of "GeV dark accelerators". | EXTRAGALACTIC COMPACT SOURCES | 7 | A | KATAOKA | JUN | NULL | NULL | JAP | 5 | AO5 | SUZAKU FOLLOW-UP OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE | XIS | Y |
| EMS1160 | 264.608 | 87.3047 | 120.03425165 | 27.94259409 | 59.9344 | 55312.9874537037 | 55313.4279513889 | 705012010 | 20279.6 | 20000 | 20279.6 | 20279.6 | 0 | 20279.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19800.4 | 19800.4 | 38053.9 | 1 | PROCESSED | 57551.2894097222 | 55693 | 55327.1544791667 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050050 | We propose to observe with Suzaku a selected set of 7 Fermi-LAT observed high galactic latitude gamma-ray sources that have no identified counterpart in any other energy range. These sources have been detected by the Fermi-LAT with high confidence and are either active galactic nuclei, galactic pulsars, or an as-yet unidentified new class of gamma-ray sources. The proposed observations are for 40 ks or 20 ks per source covering the Fermi-LAT source error region allowing us to detect sources to a flux level several times 10^(-14) erg/cm^2/s. We will determine the X-ray counterpart within the Fermi-LAT error circle, and characterize its variability and spectral properties to reveal the nature of "GeV dark accelerators". | EXTRAGALACTIC COMPACT SOURCES | 7 | A | KATAOKA | JUN | NULL | NULL | JAP | 5 | AO5 | SUZAKU FOLLOW-UP OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE | XIS | Y |
| EMS1164 | 265.9438 | -76.3446 | 317.07818058 | -22.45515073 | 114.3984 | 55300.0111689815 | 55300.6980439815 | 705013010 | 42378.3 | 40000 | 42383.6 | 42378.3 | 0 | 42389 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39048.7 | 39048.7 | 59343.9 | 1 | PROCESSED | 57551.2223958333 | 55675 | 55309.1947453704 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050050 | We propose to observe with Suzaku a selected set of 7 Fermi-LAT observed high galactic latitude gamma-ray sources that have no identified counterpart in any other energy range. These sources have been detected by the Fermi-LAT with high confidence and are either active galactic nuclei, galactic pulsars, or an as-yet unidentified new class of gamma-ray sources. The proposed observations are for 40 ks or 20 ks per source covering the Fermi-LAT source error region allowing us to detect sources to a flux level several times 10^(-14) erg/cm^2/s. We will determine the X-ray counterpart within the Fermi-LAT error circle, and characterize its variability and spectral properties to reveal the nature of "GeV dark accelerators". | EXTRAGALACTIC COMPACT SOURCES | 7 | A | KATAOKA | JUN | NULL | NULL | JAP | 5 | AO5 | SUZAKU FOLLOW-UP OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE | XIS | Y |
| EMS1274 | 285.5178 | -51.1684 | 345.57919311 | -22.40122796 | 103.8598 | 55299.2761921296 | 55300.0056944445 | 705014010 | 43925.3 | 40000 | 43925.3 | 43933.3 | 0 | 43933.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34958.1 | 34958.1 | 63015.9 | 0 | PROCESSED | 57551.1958333333 | 55675 | 55309.2111458333 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050050 | We propose to observe with Suzaku a selected set of 7 Fermi-LAT observed high galactic latitude gamma-ray sources that have no identified counterpart in any other energy range. These sources have been detected by the Fermi-LAT with high confidence and are either active galactic nuclei, galactic pulsars, or an as-yet unidentified new class of gamma-ray sources. The proposed observations are for 40 ks or 20 ks per source covering the Fermi-LAT source error region allowing us to detect sources to a flux level several times 10^(-14) erg/cm^2/s. We will determine the X-ray counterpart within the Fermi-LAT error circle, and characterize its variability and spectral properties to reveal the nature of "GeV dark accelerators". | EXTRAGALACTIC COMPACT SOURCES | 7 | A | KATAOKA | JUN | NULL | NULL | JAP | 5 | AO5 | SUZAKU FOLLOW-UP OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE | XIS | Y |
| EMS1395 | 310.8148 | 17.1786 | 61.89528011 | -15.30299533 | 74.9546 | 55319.8076736111 | 55320.4342476852 | 705015010 | 23300.2 | 20000 | 23300.2 | 23300.2 | 0 | 23300.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19494.4 | 19494.4 | 54129.9 | 0 | PROCESSED | 57551.3813773148 | 55696 | 55330.2005208333 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050050 | We propose to observe with Suzaku a selected set of 7 Fermi-LAT observed high galactic latitude gamma-ray sources that have no identified counterpart in any other energy range. These sources have been detected by the Fermi-LAT with high confidence and are either active galactic nuclei, galactic pulsars, or an as-yet unidentified new class of gamma-ray sources. The proposed observations are for 40 ks or 20 ks per source covering the Fermi-LAT source error region allowing us to detect sources to a flux level several times 10^(-14) erg/cm^2/s. We will determine the X-ray counterpart within the Fermi-LAT error circle, and characterize its variability and spectral properties to reveal the nature of "GeV dark accelerators". | EXTRAGALACTIC COMPACT SOURCES | 7 | A | KATAOKA | JUN | NULL | NULL | JAP | 5 | AO5 | SUZAKU FOLLOW-UP OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE | XIS | Y |
| EMS1535 | 345.6918 | 44.7374 | 103.4061071 | -13.97501662 | 63.3944 | 55373.2448611111 | 55374.0174768518 | 705016010 | 42395.5 | 40000 | 42403.5 | 42395.5 | 0 | 42403.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 42754.5 | 42754.5 | 66753.9 | 0 | PROCESSED | 57552.4062268518 | 55772 | 55404.2240625 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050050 | We propose to observe with Suzaku a selected set of 7 Fermi-LAT observed high galactic latitude gamma-ray sources that have no identified counterpart in any other energy range. These sources have been detected by the Fermi-LAT with high confidence and are either active galactic nuclei, galactic pulsars, or an as-yet unidentified new class of gamma-ray sources. The proposed observations are for 40 ks or 20 ks per source covering the Fermi-LAT source error region allowing us to detect sources to a flux level several times 10^(-14) erg/cm^2/s. We will determine the X-ray counterpart within the Fermi-LAT error circle, and characterize its variability and spectral properties to reveal the nature of "GeV dark accelerators". | EXTRAGALACTIC COMPACT SOURCES | 7 | A | KATAOKA | JUN | NULL | NULL | JAP | 5 | AO5 | SUZAKU FOLLOW-UP OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE | XIS | Y |
| 3C454.3 | 343.4951 | 16.1379 | 86.10833014 | -38.194784 | 252.9263 | 55525.0494675926 | 55526.0141087963 | 705021010 | 41025.2 | 40000 | 41033.2 | 41033.2 | 0 | 41025.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37141.2 | 37141.2 | 83327.8 | 0 | PROCESSED | 57554.2391319445 | 55916 | 55550.1355439815 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050052 | We propose 40 ksec x 2 (at most) Suzaku ToO observations - from a list of five -of GeV-bright flat spectrum radio quasars (FSRQs) that would be triggered by significant flaring (with E>100 MeV flux of 2x10^(-6) photons/cm^2/s or greater) in the Fermi all-sky monitoring. Those observations will be coordinated with optical and Swift XRT observations, with the goal of obtaining broadband spectra and light-curves during a flare gamma-ray activity. Such detailed spectral and variability studies are crucial to discriminate between different radiation scenarios responsible for production of X-rays and gamma-rays, and to constrain the content and by extension, the accelertation process of the jet and energization of the radiating particles. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | KATAOKA | JUN | NULL | NULL | JAP | 5 | AO5-TOO | SUZAKU TOO OBSERVATION OF GIANT FLARE IN FRSQS TRIGGERED BY FERMI-LAT | XIS | Y |
| LEDA 84274 | 220.5853 | 66.0952 | 106.75984756 | 47.40039166 | 359.2838 | 55331.3858333333 | 55332.0542824074 | 705023010 | 49465 | 50000 | 49465 | 49465 | 0 | 49465 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40838.5 | 40838.5 | 57751.9 | 1 | PROCESSED | 57551.5334143518 | 55769 | 55403.1228125 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050074 | We propose Suzaku XIS and HXD/PIN observations of two buried Active Galactic Nuclei(AGNs) at z=0.04 which are discovered by the AKARI mid-infrared all-sky survey. Both objects only show AGN features in AKARI near- and mid-infrared obsevations, while there are no clues of AGN presence in previous X-ray survey of ROSAT, radio 20cm, near-infrared photometries of 2MASS and detail optical spectroscopic data. These results indicate that a central engine of the AGN is completely buried and the nature of this population of AGNs is only poorly understood. Therefore, the hard X-ray observations is needed in order to confirm the AGN presence as well as to estimate the amount of absorption component and the AGN energy. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | OYABU | SHINKI | NULL | NULL | JAP | 5 | AO5 | SUZAKU SEARCH FOR DIRECT EVIDENCE OF SUPER MASSIVE BLACK HOLES IN BURIED ACTIVE GALACTIC NUCLEI DISCOVERED BY AKARI | XIS | Y |
| IRAS 01250+2832 | 21.9819 | 28.787 | 132.5132824 | -33.40495941 | 250.843 | 55571.3211805556 | 55572.5926388889 | 705024010 | 57582.9 | 50000 | 57582.9 | 57582.9 | 0 | 57582.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 54808.2 | 54808.2 | 109829.9 | 1 | PROCESSED | 57600.6088194444 | 55962 | 55595.2272569444 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050074 | We propose Suzaku XIS and HXD/PIN observations of two buried Active Galactic Nuclei(AGNs) at z=0.04 which are discovered by the AKARI mid-infrared all-sky survey. Both objects only show AGN features in AKARI near- and mid-infrared obsevations, while there are no clues of AGN presence in previous X-ray survey of ROSAT, radio 20cm, near-infrared photometries of 2MASS and detail optical spectroscopic data. These results indicate that a central engine of the AGN is completely buried and the nature of this population of AGNs is only poorly understood. Therefore, the hard X-ray observations is needed in order to confirm the AGN presence as well as to estimate the amount of absorption component and the AGN energy. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | OYABU | SHINKI | NULL | NULL | JAP | 5 | AO5 | SUZAKU SEARCH FOR DIRECT EVIDENCE OF SUPER MASSIVE BLACK HOLES IN BURIED ACTIVE GALACTIC NUCLEI DISCOVERED BY AKARI | XIS | Y |
| MRK 509 | 311.0469 | -10.7401 | 35.95684044 | -29.86794514 | 252.3716 | 55521.595625 | 55523.8155092593 | 705025010 | 102120.5 | 100000 | 102128.5 | 102128.5 | 0 | 102120.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 92062.5 | 92062.5 | 191769.7 | 0 | PROCESSED | 57554.2039930556 | 55916 | 55550.2628356482 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050113 | We propose the observation of one of the typical Seyferts I Mrk 509 for 100 ksec to understand how a vry hard component component that varies independently of power-law is created and how the physical structure near SMBH in Seyferts is. The hard component has been found by carrying out timing analysis of hard X-ray band to explain the extremely broad iron line feature of several Seyferts. Taking this component into account, we succeeded to explain the data of MCG 6-30-15 without the extremely broad iron line, though the origin of this component has not been identified yet. Because Mrk 509 has strong flux and large amplitude of hard X-ray variation, we found it is the most suitable object to verify this component and to get alternative interpretation to the extremely broad iron line. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | NODA | HIROFUMI | NULL | NULL | JAP | 5 | AO5 | VERIFICATION OF A HARD COMPONENT THAT VARIES INDEPENDENTLY OF POWER-LAW IN TYPE I SEYFERT MRK 509 | XIS | Y |
| EMS0992 | 230.2572 | -3.8213 | 358.15856297 | 42.46037658 | 113.2867 | 55593.7858564815 | 55594.1841898148 | 705026010 | 18979 | 20000 | 18979 | 18979 | 0 | 18979 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 14832 | 14832 | 34393.9 | 0 | PROCESSED | 57600.8001388889 | 55973 | 55607.0454976852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050126 | Fermi Gamma-ray Space Telescope has detected a lot of unidentified GeV sources in high latitude. Among these, we focus on five Fermi unIDs whose error circles contain ROSAT faint X-ray sources and propose an X-ray follow-up observation with Suzaku. From an X-ray spectral and variability information, we identify these objects, as well as find new class of GeV emitters. We also aim to study emission and particle acceleration mechanism of these objects. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | TANAKA | YASUYUKI | NULL | NULL | JAP | 5 | AO5 | SEARCH FOR X-RAY COUNTERPARTS OF FERMI HIGH-LATITUDE UNIDENTIFIED GEV SOURCES | XIS | Y |
| EMS1341 | 301.2467 | 70.0571 | 102.85714193 | 19.4440121 | 233.7732 | 55527.303275463 | 55527.7619675926 | 705027010 | 23066.8 | 20000 | 23066.8 | 23066.8 | 0 | 23066.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 21505.5 | 21505.5 | 39623.9 | 0 | PROCESSED | 57554.2240856482 | 55903 | 55537.0214814815 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050126 | Fermi Gamma-ray Space Telescope has detected a lot of unidentified GeV sources in high latitude. Among these, we focus on five Fermi unIDs whose error circles contain ROSAT faint X-ray sources and propose an X-ray follow-up observation with Suzaku. From an X-ray spectral and variability information, we identify these objects, as well as find new class of GeV emitters. We also aim to study emission and particle acceleration mechanism of these objects. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | TANAKA | YASUYUKI | NULL | NULL | JAP | 5 | AO5 | SEARCH FOR X-RAY COUNTERPARTS OF FERMI HIGH-LATITUDE UNIDENTIFIED GEV SOURCES | XIS | Y |
| EMS1388 | 309.878 | -56.3562 | 341.17879119 | -37.12820094 | 256.6037 | 55497.456400463 | 55498.1383912037 | 705028010 | 21533.6 | 20000 | 21541.6 | 21541.6 | 0 | 21533.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18373.5 | 18373.5 | 58909.9 | 0 | PROCESSED | 57553.876724537 | 55875 | 55508.9886342593 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050126 | Fermi Gamma-ray Space Telescope has detected a lot of unidentified GeV sources in high latitude. Among these, we focus on five Fermi unIDs whose error circles contain ROSAT faint X-ray sources and propose an X-ray follow-up observation with Suzaku. From an X-ray spectral and variability information, we identify these objects, as well as find new class of GeV emitters. We also aim to study emission and particle acceleration mechanism of these objects. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | TANAKA | YASUYUKI | NULL | NULL | JAP | 5 | AO5 | SEARCH FOR X-RAY COUNTERPARTS OF FERMI HIGH-LATITUDE UNIDENTIFIED GEV SOURCES | XIS | Y |
| EMS0873 | 200.796 | 29.7234 | 55.1881509 | 82.55574598 | 136.0743 | 55527.7704976852 | 55528.2800231482 | 705029010 | 22784.9 | 20000 | 22784.9 | 22784.9 | 0 | 22784.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 20810.6 | 20810.6 | 44007.9 | 2 | PROCESSED | 57554.227974537 | 55903 | 55536.9832523148 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050126 | Fermi Gamma-ray Space Telescope has detected a lot of unidentified GeV sources in high latitude. Among these, we focus on five Fermi unIDs whose error circles contain ROSAT faint X-ray sources and propose an X-ray follow-up observation with Suzaku. From an X-ray spectral and variability information, we identify these objects, as well as find new class of GeV emitters. We also aim to study emission and particle acceleration mechanism of these objects. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | TANAKA | YASUYUKI | NULL | NULL | JAP | 5 | AO5 | SEARCH FOR X-RAY COUNTERPARTS OF FERMI HIGH-LATITUDE UNIDENTIFIED GEV SOURCES | XIS | Y |
| NGC 1365 | 53.3909 | -36.1409 | 237.95774893 | -54.60665436 | 30.5416 | 55374.0284143518 | 55377.9834606482 | 705031010 | 151613.4 | 450000 | 151629.4 | 151613.4 | 0 | 151621.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 123242.2 | 123242.2 | 341657.7 | 2 | PROCESSED | 57552.5171064815 | 55287 | 55434.2469444445 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051112 | We propose 3 observations (~4 days each) of the Seyfert galaxy NGC 1365, at 2-week intervals. We aim to use eclipses to unambiguously identify the broad Fe K line, examine variability of the HXD/PIN excess, and to search for changes in the physical properties of the ionized absorber in this bright, nearby AGN. Shorter observations of this galaxy with XMM-Newton, Chandra and Suzaku showcase several remarkable physical traits: (1) FeXXV and FeXXVI K-shell absorption lines (the highest s/n detection so far among AGN), (2) rapidly varying cold absorption, (3) a highly significant relativistic Fe K emission line, and (4) a factor ~4 excess flux at high energies. The proposed observations will provide legacy spectra for what is arguably the single most physically-revealing obscured AGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | BRENNEMAN | LAURA | NULL | NULL | USA | 5 | AO5 | A LONG LOOK AT NGC 1365: DISC TOMOGRAPHY, IONIZED ABSORPTION AND HIGH ENERGY EXCESS | XIS | Y |
| NGC 1365 | 53.3976 | -36.1412 | 237.95777124 | -54.60123537 | 60.7695 | 55392.8956597222 | 55399.3676273148 | 705031020 | 302175.3 | 450000 | 302175.3 | 302183.3 | 0 | 302183.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 251061.2 | 251061.2 | 425533.9 | 2 | PROCESSED | 57552.8844791667 | 55287 | 55413.8216435185 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051112 | We propose 3 observations (~4 days each) of the Seyfert galaxy NGC 1365, at 2-week intervals. We aim to use eclipses to unambiguously identify the broad Fe K line, examine variability of the HXD/PIN excess, and to search for changes in the physical properties of the ionized absorber in this bright, nearby AGN. Shorter observations of this galaxy with XMM-Newton, Chandra and Suzaku showcase several remarkable physical traits: (1) FeXXV and FeXXVI K-shell absorption lines (the highest s/n detection so far among AGN), (2) rapidly varying cold absorption, (3) a highly significant relativistic Fe K emission line, and (4) a factor ~4 excess flux at high energies. The proposed observations will provide legacy spectra for what is arguably the single most physically-revealing obscured AGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | BRENNEMAN | LAURA | NULL | NULL | USA | 5 | AO5 | A LONG LOOK AT NGC 1365: DISC TOMOGRAPHY, IONIZED ABSORPTION AND HIGH ENERGY EXCESS | XIS | Y |
| CEN A S LOBE NO. 1 | 200.8664 | -45.1602 | 308.83796576 | 17.34395301 | 288.0039 | 55418.6612962963 | 55419.7758101852 | 705032010 | 75165.4 | 80000 | 75165.4 | 75165.4 | 0 | 75165.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 64272.8 | 64272.8 | 96281.8 | 0 | PROCESSED | 57552.9742476852 | 55803 | 55428.1537152778 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051401 | We propose a set of four pointings (200 ks), to study the X-ray emission from the Southern giant lobe of the radio galaxy Cen A. Those lobes clearly separated from the central source, have been detected as a source of diffuse gamma-ray emission by the Fermi Telescope. The goal of the Suzaku observations is two-fold: first, to measure the diffuse component of the non-thermal X-ray emission with both the XIS and the HXD in order to determine the details of the distribution of the radiating relativistic particles (and B field), and second, to measure the thermal emission from the lobes (using primarily the XIS), to determine temperature and density of the X-ray emitting plasma, which, via consideration of pressure balance, will determine the content of energetic protons (cosmic rays). | EXTRAGALACTIC COMPACT SOURCES | 7 | B | MADEJSKI | GRZEGORZ | NULL | NULL | USA | 5 | AO5 | SUZAKU OBSERVATIONS OF THE SOUTHERN LOBE OF CEN A | XIS | Y |
| CEN A S LOBE NO. 2 | 200.3949 | -45.1401 | 308.49497877 | 17.40582221 | 289.0008 | 55419.7766087963 | 55420.9641087963 | 705033010 | 81387.8 | 80000 | 81395.8 | 81387.8 | 0 | 81403.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 68108.5 | 68108.5 | 102585.8 | 0 | PROCESSED | 57552.9708564815 | 55812 | 55445.267662037 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051401 | We propose a set of four pointings (200 ks), to study the X-ray emission from the Southern giant lobe of the radio galaxy Cen A. Those lobes clearly separated from the central source, have been detected as a source of diffuse gamma-ray emission by the Fermi Telescope. The goal of the Suzaku observations is two-fold: first, to measure the diffuse component of the non-thermal X-ray emission with both the XIS and the HXD in order to determine the details of the distribution of the radiating relativistic particles (and B field), and second, to measure the thermal emission from the lobes (using primarily the XIS), to determine temperature and density of the X-ray emitting plasma, which, via consideration of pressure balance, will determine the content of energetic protons (cosmic rays). | EXTRAGALACTIC COMPACT SOURCES | 7 | B | MADEJSKI | GRZEGORZ | NULL | NULL | USA | 5 | AO5 | SUZAKU OBSERVATIONS OF THE SOUTHERN LOBE OF CEN A | XIS | Y |
| CEN A S LOBE NO. 3 | 205.7514 | -45.1409 | 312.39292182 | 16.78143613 | 279.0007 | 55420.9668981482 | 55421.3452777778 | 705034010 | 20057.5 | 20000 | 20081.5 | 20073.5 | 0 | 20057.5 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 18943.6 | 18943.6 | 32687.9 | 1 | PROCESSED | 57552.9389467593 | 55803 | 55435.169537037 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051401 | We propose a set of four pointings (200 ks), to study the X-ray emission from the Southern giant lobe of the radio galaxy Cen A. Those lobes clearly separated from the central source, have been detected as a source of diffuse gamma-ray emission by the Fermi Telescope. The goal of the Suzaku observations is two-fold: first, to measure the diffuse component of the non-thermal X-ray emission with both the XIS and the HXD in order to determine the details of the distribution of the radiating relativistic particles (and B field), and second, to measure the thermal emission from the lobes (using primarily the XIS), to determine temperature and density of the X-ray emitting plasma, which, via consideration of pressure balance, will determine the content of energetic protons (cosmic rays). | EXTRAGALACTIC COMPACT SOURCES | 7 | B | MADEJSKI | GRZEGORZ | NULL | NULL | USA | 5 | AO5 | SUZAKU OBSERVATIONS OF THE SOUTHERN LOBE OF CEN A | XIS | Y |
| CEN A S LOBE NO. 4 | 196.751 | -45.1436 | 305.81117883 | 17.64110832 | 288.0039 | 55421.3479282407 | 55421.67375 | 705035010 | 20642 | 20000 | 20642 | 20650 | 0 | 20658 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 18964.3 | 18964.3 | 28143.9 | 0 | PROCESSED | 57552.9465277778 | 55803 | 55435.1577314815 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051401 | We propose a set of four pointings (200 ks), to study the X-ray emission from the Southern giant lobe of the radio galaxy Cen A. Those lobes clearly separated from the central source, have been detected as a source of diffuse gamma-ray emission by the Fermi Telescope. The goal of the Suzaku observations is two-fold: first, to measure the diffuse component of the non-thermal X-ray emission with both the XIS and the HXD in order to determine the details of the distribution of the radiating relativistic particles (and B field), and second, to measure the thermal emission from the lobes (using primarily the XIS), to determine temperature and density of the X-ray emitting plasma, which, via consideration of pressure balance, will determine the content of energetic protons (cosmic rays). | EXTRAGALACTIC COMPACT SOURCES | 7 | B | MADEJSKI | GRZEGORZ | NULL | NULL | USA | 5 | AO5 | SUZAKU OBSERVATIONS OF THE SOUTHERN LOBE OF CEN A | XIS | Y |
| 1RXS J111706.3+20141 | 169.2749 | 20.2432 | 225.56577108 | 67.37465885 | 120.2309 | 55510.3081944444 | 55511.1543402778 | 705036010 | 34212.5 | 32000 | 34212.5 | 34212.5 | 0 | 34212.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 31536.6 | 31536.6 | 73097.9 | 0 | PROCESSED | 57554.0402199074 | 55903 | 55537.0979050926 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051402 | High frequency peaked BL Lacs are a peculiar subclass of Blazars characterized by non-thermal emission across the whole electromagnetic spectrum. Their spectral energy distributions (SEDs) include two main components: a low-energy component with power peaking in the range from the UV to the X-ray band, and a substantial high-energy component often dominated by gamma-rays. We propose 3 observations (32 ks each) of a selected sample of HBLs to study the behavior of the first component, widely interpreted as synchrotron radiation. First, we will be able to disentangle between different spectral shapes of the synchrotron SED of HBLs. Second, we will use the proposed observations to investigate the properties of the most representative sample of TeV candidate HBLs. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | MASSARO | FRANCESCO | NULL | NULL | USA | 5 | AO5 | X-RAY CURVED SPECTRA IN HIGH FREQUENCY PEAKED BL LACS | XIS | Y |
| 1RXS J032613.6+02252 | 51.5615 | 2.4213 | 180.7494445 | -42.4285339 | 253.9336 | 55596.8403356482 | 55597.6203125 | 705038010 | 32197.1 | 32000 | 32197.1 | 32197.1 | 0 | 32197.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22644.1 | 22644.1 | 67387.9 | 1 | PROCESSED | 57600.8622106482 | 55983 | 55614.1886342593 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051402 | High frequency peaked BL Lacs are a peculiar subclass of Blazars characterized by non-thermal emission across the whole electromagnetic spectrum. Their spectral energy distributions (SEDs) include two main components: a low-energy component with power peaking in the range from the UV to the X-ray band, and a substantial high-energy component often dominated by gamma-rays. We propose 3 observations (32 ks each) of a selected sample of HBLs to study the behavior of the first component, widely interpreted as synchrotron radiation. First, we will be able to disentangle between different spectral shapes of the synchrotron SED of HBLs. Second, we will use the proposed observations to investigate the properties of the most representative sample of TeV candidate HBLs. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | MASSARO | FRANCESCO | NULL | NULL | USA | 5 | AO5 | X-RAY CURVED SPECTRA IN HIGH FREQUENCY PEAKED BL LACS | XIS | Y |
| NGC 6251 | 248.2903 | 82.5391 | 115.75265542 | 31.17774629 | 182.5432 | 55532.2390625 | 55534.0341898148 | 705039010 | 87070.6 | 85000 | 87070.6 | 87070.6 | 0 | 87070.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 75807.4 | 75807.4 | 155087.9 | 1 | PROCESSED | 57554.3327546296 | 55931 | 55565.375162037 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051411 | We propose an 85-ks Suzaku observation of NGC 6251, the brightest example of a low-excitation radio galaxy (LERG). We have previously suggested that LERGs violate conventional AGN unification schemes: they may lack an obscuring torus and are likely to accrete in a radiatively inefficient manner, with almost all of the energy released by the accretion process being channeled into powerful jets. However, Suzaku observations at low and high energies are needed to test this model directly. We will use the XIS and HXD to search for the signatures of accretion-related X-ray emission: (1) the 6.4 keV Fe Ka line, (2) heavily absorbed X-ray emission, and (3) the >10 keV Compton reflection bump. These results will have important implications for models of accretion and feedback in radio-loud AGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | EVANS | DANIEL | NULL | NULL | USA | 5 | AO5 | A DIRECT TEST OF THE NUCLEAR X-RAY DICHOTOMY IN RADIO-LOUD AGN | XIS | Y |
| 3C111 | 64.5838 | 38.0364 | 161.66578558 | -8.81556542 | 79.7358 | 55441.1593055556 | 55442.8995138889 | 705040010 | 80683 | 80000 | 80691 | 80683 | 0 | 80691 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 73370.7 | 73370.7 | 150307.9 | 1 | PROCESSED | 57553.2986458333 | 55822 | 55456.2202430556 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051412 | Using our Suzaku observations we discovered ultra-fast outflows (UFOs) in radio-loud Broad-Line Radio Galaxies, with velocities v/c~0.04--0.15 and carrying a mass of the same order as the accretion mass. The bright BLRG 3C~111 was selected for an in-depth study of its UFO through its predicted variability on timescales of approximately one week. We propose 3 Suzaku pointings of 80~ks each separated by one week to determine the gas geometrical, physical, and dynamical characteristics and start addressing its role for the jet-disk connection in radio-loud AGN. Additionally, we will obtain a simultaneous radio-to-GeV Spectral Energy Distribution and model the relative contributions of the accretion and non-thermal components. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | SAMBRUNA | RITA | NULL | NULL | USA | 5 | AO5 | PROBING THE ULTRA-FAST OUTFLOW IN 3C 111 WITH SUZAKU | XIS | Y |
| 3C111 | 64.5838 | 38.0341 | 161.66743119 | -8.81719194 | 77.8463 | 55448.0268865741 | 55449.7585416667 | 705040020 | 79419.8 | 80000 | 79419.8 | 79419.8 | 0 | 79419.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 71809 | 71809 | 149605.8 | 0 | PROCESSED | 57553.3942592593 | 55827 | 55461.3122106482 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051412 | Using our Suzaku observations we discovered ultra-fast outflows (UFOs) in radio-loud Broad-Line Radio Galaxies, with velocities v/c~0.04--0.15 and carrying a mass of the same order as the accretion mass. The bright BLRG 3C~111 was selected for an in-depth study of its UFO through its predicted variability on timescales of approximately one week. We propose 3 Suzaku pointings of 80~ks each separated by one week to determine the gas geometrical, physical, and dynamical characteristics and start addressing its role for the jet-disk connection in radio-loud AGN. Additionally, we will obtain a simultaneous radio-to-GeV Spectral Energy Distribution and model the relative contributions of the accretion and non-thermal components. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | SAMBRUNA | RITA | NULL | NULL | USA | 5 | AO5 | PROBING THE ULTRA-FAST OUTFLOW IN 3C 111 WITH SUZAKU | XIS | Y |
| 3C111 | 64.5838 | 38.0329 | 161.66828978 | -8.81804056 | 76.1726 | 55453.9599768518 | 55455.7432986111 | 705040030 | 80365.9 | 80000 | 80381.9 | 80365.9 | 0 | 80381.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70953.3 | 70953.3 | 154063.9 | 2 | PROCESSED | 57553.468599537 | 55835 | 55469.3718287037 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051412 | Using our Suzaku observations we discovered ultra-fast outflows (UFOs) in radio-loud Broad-Line Radio Galaxies, with velocities v/c~0.04--0.15 and carrying a mass of the same order as the accretion mass. The bright BLRG 3C~111 was selected for an in-depth study of its UFO through its predicted variability on timescales of approximately one week. We propose 3 Suzaku pointings of 80~ks each separated by one week to determine the gas geometrical, physical, and dynamical characteristics and start addressing its role for the jet-disk connection in radio-loud AGN. Additionally, we will obtain a simultaneous radio-to-GeV Spectral Energy Distribution and model the relative contributions of the accretion and non-thermal components. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | SAMBRUNA | RITA | NULL | NULL | USA | 5 | AO5 | PROBING THE ULTRA-FAST OUTFLOW IN 3C 111 WITH SUZAKU | XIS | Y |
| PDS 456 | 262.0809 | -14.2537 | 10.4015562 | 11.17111116 | 96.1694 | 55636.625462963 | 55639.3564930556 | 705041010 | 125527.2 | 130000 | 125535.2 | 125527.2 | 0 | 125532.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 100875 | 100875 | 235927.6 | 2 | PROCESSED | 57601.2862615741 | 56050 | 55677.3183564815 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051421 | PDS 456 is the most luminous nearby AGN and a recent Suzaku observation revealed a powerful ionized outflow moving at 0.25c with kinetic output matching the quasar bolometric luminosity. Above 10 keV the HXD appears to show a factor 3 rise in flux over the XIS, implying that a high column density absorber (>10^24 cm^-2) is located close to the X-ray source in order to partially covers its emission. We propose to study the remarkable X-ray absorption towards PDS 456 through two further 130 ks Suzaku observations. This will:-i) confirm the nature of the hard excess, ii) determine whether spectral variability can be explained by variable partial covering and iii) enable us to measure the imprint of the ionized outflow at Fe K with unprecedented accuracy. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | TURNER | TRACEY | NULL | NULL | USA | 5 | AO5 | THE COMPTON-THICK OUTFLOW IN THE TYPE I QSO PDS 456 | XIS | Y |
| CBS 126 | 153.2712 | 35.8701 | 188.30426979 | 55.38335717 | 124.145 | 55487.3144907407 | 55489.5529861111 | 705042010 | 101542 | 100000 | 101566 | 101542 | 0 | 101566 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 90743.8 | 90743.8 | 193389.7 | 2 | PROCESSED | 57553.8238541667 | 55867 | 55498.3270949074 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051432 | We propose to carry out a 100 ks Suzaku observation of Broad Line Seyfert 1 (BLS1) galaxy CBS 126. This source exhibits many properties which are thought to be typical of a Narrow Line Seyfert 1 (NLS1), such as a large soft X-ray excess and strong spectral variability, but unusual for a BLS1. Taking advantage of Suzaku's unique broad band X-ray energy window, our main goal is to clarify the nature of the unusual, variable, optically polarized spectrum of CBS 126. These interesting spectral features cover a wide energy range where Suzaku is ideal. With these proposed studies we will gain better understanding of accretion-powered AGN in general. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | TSURUTA | SACHIKO | NULL | NULL | USA | 5 | AO5 | SPECTRAL AND TEMPORAL STUDIES OF THE SEYFERT 1 GALAXY CBS 126 | XIS | Y |
| MKN 590 | 33.6446 | -0.7698 | 163.50990373 | -56.94179664 | 250.4206 | 55584.0937615741 | 55585.6252083333 | 705043010 | 61554.7 | 150000 | 61586.7 | 61554.7 | 0 | 61570.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 55159.9 | 55159.9 | 132275.8 | 0 | PROCESSED | 57600.7325 | 55965 | 55599.1867824074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051433 | We propose a 150 ks Suzaku long-look to study the Compton reflection component, soft excess, ionized emission and possible ionized reflection of the Seyfert 1.2 AGN Mkn 590, which has an unobscured line of sight or "bare nucleus" and as of yet unquantified reflection. We aim to accurately constrain the geometry of the circumnuclear material and determine the ionization states of both the Compton-thin and Compton-thick material surrounding the black hole by studying the origin of the soft excess, determining the likelihood of ionized reflection and accurately measuring the intensity of neutral, H-like and He-like Fe emission lines. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | RIVERS | ELIZABETH | NULL | NULL | USA | 5 | AO5 | QUANTIFYING THE COMPTON REFLECTION AND IONIZED EMISSION IN MKN 590 | XIS | Y |
| MKN 590 | 33.6477 | -0.7713 | 163.51612886 | -56.94122484 | 251.1273 | 55587.0949652778 | 55588.2146990741 | 705043020 | 40913.9 | 150000 | 40921.9 | 40921.9 | 0 | 40913.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37869.9 | 37869.9 | 96733.9 | 1 | PROCESSED | 57600.7810763889 | 55988 | 55621.2137731482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051433 | We propose a 150 ks Suzaku long-look to study the Compton reflection component, soft excess, ionized emission and possible ionized reflection of the Seyfert 1.2 AGN Mkn 590, which has an unobscured line of sight or "bare nucleus" and as of yet unquantified reflection. We aim to accurately constrain the geometry of the circumnuclear material and determine the ionization states of both the Compton-thin and Compton-thick material surrounding the black hole by studying the origin of the soft excess, determining the likelihood of ionized reflection and accurately measuring the intensity of neutral, H-like and He-like Fe emission lines. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | RIVERS | ELIZABETH | NULL | NULL | USA | 5 | AO5 | QUANTIFYING THE COMPTON REFLECTION AND IONIZED EMISSION IN MKN 590 | XIS | Y |
| NGC 526A | 20.9794 | -35.0729 | 263.77547728 | -79.45131683 | 257.0195 | 55578.7592939815 | 55580.6404050926 | 705044010 | 72934.6 | 70000 | 72934.6 | 72934.6 | 0 | 72934.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 63137.2 | 63137.2 | 162497.7 | 2 | PROCESSED | 57600.6980324074 | 55961 | 55595.4905671296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051434 | The Compton-thin NELG NGC 526a has large hard X-ray variability and likely an abnormally flat photon index, Gamma near 1.6. We request two observations of 70 ks each, spaced six months apart, to accurately constrain Compton reflection and obtain geometrical constraints on the accreting material to test Seyfert unification schemes, as well as constrain coronal power law parameters. Importantly, we will track long-term spectral variability to constrain the location and nature of the reflecting material. We also will resolve the moderately broad Fe K alpha line, which may indicate the presence of a truncated accretion disk, and thus constrain the amount of reflection off an accretion disk versus that from a torus. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | MARKOWITZ | ALEX | NULL | NULL | USA | 5 | AO5 | COMPTON REFLECTION AND LONG-TERM SPECTRAL VARIABILITY IN THE SEYFERT AGN NGC 526A | XIS | Y |
| IRAS 12072-0444 | 182.4393 | -5.0116 | 283.97337665 | 56.31820605 | 111.9489 | 55534.0444328704 | 55535.5169328704 | 705045010 | 61933.9 | 60000 | 61941.9 | 61941.9 | 0 | 61933.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28159.6 | 28159.6 | 127206 | 0 | PROCESSED | 57554.3475810185 | 55910 | 55544.3011226852 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051441 | We propose two Suzaku-HXD observations of two ULIRGs hosting a deeply buried AGN. These two objects are expected to host a powerful AGN in the luminosity range of quasars, based on solid evidence from mid-IR Spitzer spectroscopy. However, these sources are completely buried behind a screen of dust with column density in excess of 10^24 cm^-2, so not only the primary emission below 10 keV is obscured, but the reflected emission, usually ascribed to a circumnuclear "torus", is also absent. This suggests a complete spherical coverage of the X-ray source along all directions. The unique capabilities of Suzaku at high energies will allow to confirm the existence of these objects, representing the most extreme examples of buried AGNs, both in terms of obscuration and of intrinsic luminosity. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | RISALITI | GUIDO | NULL | NULL | USA | 5 | AO5 | BURIED QUASAR 2S INSIDE ULIRGS | XIS | Y |
| IRAS 00397-1312 | 10.5707 | -12.9503 | 113.89016485 | -75.66108211 | 246.4295 | 55558.1361342593 | 55560.2501388889 | 705046010 | 83792.8 | 90000 | 83792.8 | 83792.8 | 0 | 83792.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 71931.4 | 71931.4 | 182631.7 | 1 | PROCESSED | 57632.5965856482 | 56040 | 55670.3615046296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051441 | We propose two Suzaku-HXD observations of two ULIRGs hosting a deeply buried AGN. These two objects are expected to host a powerful AGN in the luminosity range of quasars, based on solid evidence from mid-IR Spitzer spectroscopy. However, these sources are completely buried behind a screen of dust with column density in excess of 10^24 cm^-2, so not only the primary emission below 10 keV is obscured, but the reflected emission, usually ascribed to a circumnuclear "torus", is also absent. This suggests a complete spherical coverage of the X-ray source along all directions. The unique capabilities of Suzaku at high energies will allow to confirm the existence of these objects, representing the most extreme examples of buried AGNs, both in terms of obscuration and of intrinsic luminosity. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | RISALITI | GUIDO | NULL | NULL | USA | 5 | AO5 | BURIED QUASAR 2S INSIDE ULIRGS | XIS | Y |
| NGC 4945 | 196.3459 | -49.5284 | 305.256234 | 13.28040137 | 283.285 | 55381.636087963 | 55382.6765856482 | 705047010 | 39073.7 | 40000 | 39081.7 | 39081.7 | 0 | 39073.7 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 34075.1 | 34075.1 | 89871.9 | 1 | PROCESSED | 57552.4706481482 | 55770 | 55404.2681134259 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051442 | We propose five 40 ks observations of the Compton-thick AGN in NGC 4945, with the aim of monitoring possible variations of the X-ray source, and correlate the intrinsic variations seen above 10~keV with the variations in the reflected spectrum below 10~keV. This campaign is unique in two respects: NGC 4945 is the only object suitable for an investigation of possible variations of a Compton-thick AGN, which would set the first constraints on the structure and dimensions of the absorber/reflector in these objects, and the proposed observations are a clear "ideal case" for Suzaku, making full use of its unique properties, i.e. the high-energy spectral capabilities and the simultaneous availability of the full 1-100~keV spectral interval. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | RISALITI | GUIDO | NULL | NULL | USA | 5 | AO5 | HARD X-RAY MONITORING OF THE COMPTON-THICK AGN IN NGC 4945 | HXD | Y |
| NGC 4945 | 196.3415 | -49.5274 | 305.25336122 | 13.28155854 | 286.7821 | 55386.9936226852 | 55388.2626388889 | 705047020 | 44151.7 | 40000 | 44151.7 | 44159.7 | 0 | 44151.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40161.2 | 40161.2 | 109434 | 0 | PROCESSED | 57552.6167824074 | 55777 | 55411.4916898148 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051442 | We propose five 40 ks observations of the Compton-thick AGN in NGC 4945, with the aim of monitoring possible variations of the X-ray source, and correlate the intrinsic variations seen above 10~keV with the variations in the reflected spectrum below 10~keV. This campaign is unique in two respects: NGC 4945 is the only object suitable for an investigation of possible variations of a Compton-thick AGN, which would set the first constraints on the structure and dimensions of the absorber/reflector in these objects, and the proposed observations are a clear "ideal case" for Suzaku, making full use of its unique properties, i.e. the high-energy spectral capabilities and the simultaneous availability of the full 1-100~keV spectral interval. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | RISALITI | GUIDO | NULL | NULL | USA | 5 | AO5 | HARD X-RAY MONITORING OF THE COMPTON-THICK AGN IN NGC 4945 | HXD | Y |
| NGC 4945 | 196.3265 | -49.5207 | 305.24375345 | 13.28878787 | 296.6587 | 55403.0670717593 | 55404.1745717593 | 705047030 | 40326.6 | 40000 | 40342.6 | 40326.6 | 0 | 40342.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34618.2 | 34618.2 | 95635.8 | 0 | PROCESSED | 57552.7156134259 | 55780 | 55414.0832407407 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051442 | We propose five 40 ks observations of the Compton-thick AGN in NGC 4945, with the aim of monitoring possible variations of the X-ray source, and correlate the intrinsic variations seen above 10~keV with the variations in the reflected spectrum below 10~keV. This campaign is unique in two respects: NGC 4945 is the only object suitable for an investigation of possible variations of a Compton-thick AGN, which would set the first constraints on the structure and dimensions of the absorber/reflector in these objects, and the proposed observations are a clear "ideal case" for Suzaku, making full use of its unique properties, i.e. the high-energy spectral capabilities and the simultaneous availability of the full 1-100~keV spectral interval. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | RISALITI | GUIDO | NULL | NULL | USA | 5 | AO5 | HARD X-RAY MONITORING OF THE COMPTON-THICK AGN IN NGC 4945 | HXD | Y |
| NGC 4945 | 196.2918 | -49.5144 | 305.2209968 | 13.29631795 | 319.7988 | 55438.8990277778 | 55439.9896990741 | 705047040 | 39385.9 | 40000 | 39385.9 | 39385.9 | 0 | 39385.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35782.3 | 35782.3 | 94223.9 | 0 | PROCESSED | 57553.267962963 | 55815 | 55449.2596296296 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051442 | We propose five 40 ks observations of the Compton-thick AGN in NGC 4945, with the aim of monitoring possible variations of the X-ray source, and correlate the intrinsic variations seen above 10~keV with the variations in the reflected spectrum below 10~keV. This campaign is unique in two respects: NGC 4945 is the only object suitable for an investigation of possible variations of a Compton-thick AGN, which would set the first constraints on the structure and dimensions of the absorber/reflector in these objects, and the proposed observations are a clear "ideal case" for Suzaku, making full use of its unique properties, i.e. the high-energy spectral capabilities and the simultaneous availability of the full 1-100~keV spectral interval. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | RISALITI | GUIDO | NULL | NULL | USA | 5 | AO5 | HARD X-RAY MONITORING OF THE COMPTON-THICK AGN IN NGC 4945 | HXD | Y |
| NGC 4945 | 196.3636 | -49.4659 | 305.27160994 | 13.34216317 | 120.2557 | 55590.0873842593 | 55591.1182175926 | 705047050 | 46107.6 | 40000 | 46107.6 | 46107.6 | 0 | 46107.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 54090.7 | 54090.7 | 89051.8 | 0 | PROCESSED | 57600.8100810185 | 55969 | 55602.2238194445 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051442 | We propose five 40 ks observations of the Compton-thick AGN in NGC 4945, with the aim of monitoring possible variations of the X-ray source, and correlate the intrinsic variations seen above 10~keV with the variations in the reflected spectrum below 10~keV. This campaign is unique in two respects: NGC 4945 is the only object suitable for an investigation of possible variations of a Compton-thick AGN, which would set the first constraints on the structure and dimensions of the absorber/reflector in these objects, and the proposed observations are a clear "ideal case" for Suzaku, making full use of its unique properties, i.e. the high-energy spectral capabilities and the simultaneous availability of the full 1-100~keV spectral interval. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | RISALITI | GUIDO | NULL | NULL | USA | 5 | AO5 | HARD X-RAY MONITORING OF THE COMPTON-THICK AGN IN NGC 4945 | XIS | Y |
| ESP 39607 | 11.5922 | -40.0968 | 307.24150307 | -76.98900447 | 243.1952 | 55549.7680208333 | 55551.3175810185 | 705048010 | 60668.7 | 60000 | 60692.7 | 60668.7 | 0 | 60684.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48955.5 | 48955.5 | 133839.9 | 3 | PROCESSED | 57554.5018402778 | 55960 | 55593.2278472222 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051443 | We propose to observe the five most luminous type II AGN detected in the Swift BAT all sky hard X-ray survey (14-195 keV). Because BAT's detection efficiency for absorbed sources in the high energy band is very high, these sources are the most luminous (log(L_x) > 45.5 erg/sec) absorbed type II QSOs in the local universe and the most ripe for study with Suzaku. The newly discovered source SWIFT J2344.6-4233 at a redshift of z=0.6 is the most luminous object in the BAT sample with log(L_x) = 46.5 erg/sec. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | BAUMGARTNER | WAYNE | NULL | NULL | USA | 5 | AO5 | SUZAKU OBSERVATIONS OF THE MOST LUMINOUS ABSORBED TYPE II QSOS | XIS | Y |
| SWIFTJ2344.6-424322 | 356.1059 | -42.7624 | 339.65324523 | -69.27134863 | 225.0657 | 55505.2812731482 | 55506.5570601852 | 705049010 | 61741.6 | 60000 | 61741.6 | 61741.6 | 0 | 61741.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 50394.1 | 50394.1 | 110211.8 | 1 | PROCESSED | 57553.9985532407 | 55885 | 55518.3162847222 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051443 | We propose to observe the five most luminous type II AGN detected in the Swift BAT all sky hard X-ray survey (14-195 keV). Because BAT's detection efficiency for absorbed sources in the high energy band is very high, these sources are the most luminous (log(L_x) > 45.5 erg/sec) absorbed type II QSOs in the local universe and the most ripe for study with Suzaku. The newly discovered source SWIFT J2344.6-4233 at a redshift of z=0.6 is the most luminous object in the BAT sample with log(L_x) = 46.5 erg/sec. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | BAUMGARTNER | WAYNE | NULL | NULL | USA | 5 | AO5 | SUZAKU OBSERVATIONS OF THE MOST LUMINOUS ABSORBED TYPE II QSOS | XIS | Y |
| 3C 433 | 320.9422 | 25.055 | 74.46917661 | -17.70913692 | 252.1178 | 55506.5663310185 | 55508.0953472222 | 705050010 | 62500.9 | 60000 | 62540 | 62500.9 | 0 | 62540 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44427.1 | 44427.1 | 132069.8 | 0 | PROCESSED | 57554.0198958333 | 55890 | 55524.1485416667 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051443 | We propose to observe the five most luminous type II AGN detected in the Swift BAT all sky hard X-ray survey (14-195 keV). Because BAT's detection efficiency for absorbed sources in the high energy band is very high, these sources are the most luminous (log(L_x) > 45.5 erg/sec) absorbed type II QSOs in the local universe and the most ripe for study with Suzaku. The newly discovered source SWIFT J2344.6-4233 at a redshift of z=0.6 is the most luminous object in the BAT sample with log(L_x) = 46.5 erg/sec. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | BAUMGARTNER | WAYNE | NULL | NULL | USA | 5 | AO5 | SUZAKU OBSERVATIONS OF THE MOST LUMINOUS ABSORBED TYPE II QSOS | XIS | Y |
| NGC 4258 | 184.7518 | 47.3153 | 138.28789039 | 68.83430148 | 139.1798 | 55511.1601388889 | 55512.7112615741 | 705051010 | 103833.2 | 100000 | 103833.2 | 103841.2 | 0 | 103837 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 86225.7 | 86225.7 | 133968.8 | 1 | PROCESSED | 57554.0812384259 | 55903 | 55537.1754398148 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051451 | We request a 100 ksec observation of the Low Luminosity AGN NGC 4258. This observation is meant to complement our existing 100 ksec Suzaku observation (Reynolds et al. 2009), and our 320 ksec Chandra-HETG observation (Murphy et al., in prep.). The goal is to further characterize the observed variability of the Fe Kalpha line and any associated changes in the continuum and/or absorption of NGC 4258. Given the unique constraints that we have on the mass, distance and accretion flow geometry in NGC 4258, as well as its role as a bridge between the most quiescent nuclei and powerful AGN, further Suzaku studies of NGC 4258 are clearly warranted. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | NOWAK | MICHAEL | NULL | NULL | USA | 5 | AO5 | HUNTING FOR THE VARIABLE IRON LINE IN NGC 4258 | XIS | Y |
| MCG-03-58-007 | 342.3795 | -19.2152 | 42.20057234 | -60.96689333 | 68.5139 | 55350.7016203704 | 55352.8940046296 | 705052010 | 99087.3 | 100000 | 99087.3 | 99087.3 | 0 | 99087.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 81420 | 81420 | 189406 | 1 | PROCESSED | 57551.8454513889 | 55734 | 55365.563912037 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 052011 | Despite their relevance, less than two dozens of confirmed Compton-thick (CT) AGN have been found so far. We have recently selected a well defined sample of CT AGN candidates using FX/Fir ratios and X-ray colors. Due to their heavy obscuration, good statistics at 6.4 keV and data above 10 keV are needed to assess the real nature of these sources. We propose deep Suzaku observations (100 and 150 ks) for two sources for which data above 10 keV are not available and the quality of XMM data is poor. This request is a continuation of an approved AO4 proposal. These observations will allow us to possibly unveil two more examples of CT AGN, provide a physical characterization of the relatively bright tail of our sample, and estimate the efficiency of our method in selecting CT AGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | SEVERGNINI | PAOLA | NULL | NULL | EUR | 5 | AO5 | SUZAKU OBSERVATIONS OF TWO COMPTON-THICK CANDIDATES | HXD | Y |
| NGC 3147 | 154.2433 | 73.3869 | 136.29780832 | 39.47682975 | 262.9224 | 55340.8248611111 | 55343.2925231482 | 705054010 | 150047.6 | 150000 | 150047.6 | 150055.6 | 0 | 150055.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 132913.6 | 132913.6 | 213181.8 | 2 | PROCESSED | 57553.0649074074 | 55765 | 55393.4710648148 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 052013 | NGC3147 is the best candidate to be a true Seyfert 2, i.e., with no BLR. We propose a 150 ks observation with Suzaku to study the Fe line profile which in the short XMM-Newton observation shows some structure. If the iron line will turn out to be originated from the accretion disc, the lack of the BLR cannot be attributed to the lack of ionizing photons; if originated from the torus, this would put constraints on models assuming a common origin for the torus and the BLR; if the presence of an ionized iron line is confirmed, a BLR might exist but so highly ionized to be invisible at optical/UV wavelengths. An important added value of this observation is to confirm NGC3147 as a true Seyfert 2 by ruling out a Compton-thick nature, which only Suzaku can do thanks to its hard X-ray coverage. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | MATT | GIORGIO | NULL | NULL | EUR | 5 | AO5 | SUZAKU OBSERVATION OF THE BEST ``TRUE SEYFERT 2'' GALAXY CANDIDATE, NGC 3147 | XIS | Y |
| IGR J19378-0617 | 294.4023 | -6.2869 | 32.53385066 | -13.11752642 | 260.9167 | 55485.0705324074 | 55487.3016087963 | 705055010 | 77801.4 | 80000 | 77817.4 | 77801.4 | 0 | 77817.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70571.2 | 70571.2 | 192743.9 | 1 | PROCESSED | 57553.8036226852 | 55867 | 55498.2386805556 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 052014 | We propose to observe with Suzaku three Narrow Line Seyfert 1 galaxies detected by INTEGRAL/IBIS and/or Swift/BAT with a flux in excess of 1.5e-11 cgs in the 15-50keV band (corresponding to the HXD/PIN band). The proposed observations will provide rare high quality spectra of NLS1s in the 0.5-50keV band. The good quality data above 10keV will dramatically help us removing the spectral degeneracies inherent to limited bandpass analysis (such as that with XMM-Newton and Chandra) and the ambiguities between the different proposed models invoked to explain the unique spectral and variability properties of these most extreme class of high accretion rate sources. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MINIUTTI | GIOVANNI | NULL | NULL | EUR | 5 | AO5 | BROADBAND X-RAY PROPERTIES OF HARD-X-RAY-BRIGHT NLS1 GALAXIES | HXD | Y |
| 4U 1344-60 | 206.8966 | -60.619 | 309.76861534 | 1.50528265 | 97.6008 | 55572.7924189815 | 55575.4751273148 | 705058010 | 93877.3 | 100000 | 93901.3 | 93893.3 | 0 | 93877.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 79561.7 | 79561.7 | 231753.7 | 3 | PROCESSED | 57600.6768865741 | 55975 | 55607.6933333333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 052018 | We propose a 100 ks Suzaku observation of 4U 1344-60, a poorly studied (because at low Galactic latitude) but bright (about 2 millicrabs) AGN which showed, in an XMM-Newton observation, a strong relativistic disk iron line. The main aim of the proposal is to determine in detail the parameters of the disk, which is possible only with a high quality broad band observation which permits to control the continuum beneath the line. Presently, only Suzaku has the right combination of sensitivity, energy resolution and broad band coverage to achieve this objective. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | SVOBODA | JIRI | NULL | NULL | EUR | 5 | AO5 | 4U 1344-60: A BRIGHT AGN WITH A STRONG RELATIVISTIC IRON LINE | XIS | Y |
| CENTAURUS B | 206.7018 | -60.4061 | 309.72060452 | 1.73379394 | 97.6796 | 55572.6060763889 | 55572.7919444444 | 705059010 | 8761.1 | 10000 | 8769.1 | 8769.1 | 0 | 8761.1 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 6452.6 | 6452.6 | 16055.9 | 0 | PROCESSED | 57600.577650463 | 55962 | 55595.2069675926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 052018 | We propose a 100 ks Suzaku observation of 4U 1344-60, a poorly studied (because at low Galactic latitude) but bright (about 2 millicrabs) AGN which showed, in an XMM-Newton observation, a strong relativistic disk iron line. The main aim of the proposal is to determine in detail the parameters of the disk, which is possible only with a high quality broad band observation which permits to control the continuum beneath the line. Presently, only Suzaku has the right combination of sensitivity, energy resolution and broad band coverage to achieve this objective. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | SVOBODA | JIRI | NULL | NULL | EUR | 5 | AO5 | 4U 1344-60: A BRIGHT AGN WITH A STRONG RELATIVISTIC IRON LINE | XIS | Y |
| MRK 205 | 185.2459 | 75.2485 | 125.52269394 | 41.72619699 | 309.3435 | 55338.764849537 | 55340.8203125 | 705062010 | 100960.5 | 126000 | 100968.5 | 100960.5 | 0 | 100968.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 91952.5 | 91952.5 | 177577.8 | 0 | PROCESSED | 57551.6334606482 | 55723 | 55355.4313773148 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 052026 | Mrk 205 (z=0.071) is a ``bare'' radio-quiet quasar, showing a peculiar continuum and FeK complex. From our analysis of past XMM-Newton observations, it shows a prominent and variable soft excess down to a two-day timescale. In 2000, an unusual FeK profile was found with an unresolved narrow line at 6.4keV and a broadened line centered at 6.7keV; while in 2006 a broad line has been observed near 6.4keV with a visible energy shift to 6.5keV occurring when the source flux increased. Our aims are to: (i) determine the FeK origin from its profile, and its possible variability on sub-orbital time-scales, (ii) to obtain an unprecedented simultaneous measurement of the Compton hump which is critical for modelling the true FeK profile (iii) and hence to infer a global picture of this object. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | PORQUET | DELPHINE | NULL | NULL | EUR | 5 | AO5 | PROBING THE ORIGIN OF THE FEK COMPLEX IN THE ``BARE'' NUCLEUS OF MRK205. | HXD | Y |
| FAIRALL 9 | 20.848 | -58.7784 | 295.14856402 | -57.86436534 | 32.7271 | 55335.1255671296 | 55338.764837963 | 705063010 | 229296.3 | 250000 | 229302 | 229302 | 0 | 229296.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 174941.2 | 174941.2 | 288656 | 1 | PROCESSED | 57551.9874074074 | 55287 | 55434.4437615741 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056003 | We propose deep Suzaku observations of 6 well-known AGN with the primary aim of studying strong-gravitational physics close to these supermassive black holes (SMBH). We will conduct the first ever census of local SMBH spin, providing a new window on the growth-history of SMBHs. Suzaku's unique combination of high-throughput in the iron-K band and hard-band (>10keV) sensitivity is crucial, permitting a separation of the disk-reflection spectrum (which encodes the relativistic physics) from the effects of the warm absorber and low-velocity emission/reflection. These six datasets will be an important legacy of Suzaku, providing an important resource for AGN researchers for at least the next decade. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | REYNOLDS | CHRISTOPHER | NULL | NULL | USA | 5 | AO5 | A SURVEY OF BLACK HOLE SPIN AND RELATIVISTIC PHYSICS IN AGN | HXD | Y |
| 1FGL J1311.7-3429 | 197.9423 | -34.512 | 307.68226276 | 28.17214982 | 298.263 | 55774.7002314815 | 55776.7362847222 | 706001010 | 82477.1 | 80000 | 82477.1 | 82477.1 | 0 | 82477.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70373.7 | 70373.7 | 175863.8 | 2 | PROCESSED | 57602.7690046296 | 56219 | 55851.4595601852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060003 | We propose Suzaku observations of "unusual" Fermi-LAT sources 1FGL J1311.7 and 1FGL J2339.7, which are extremely bright in gamma-ray (> 30 sigma detection), but are as-yet unidentified even after two-year accumulation of Fermi-LAT data. Previous Suzaku observation revealed a highly variable X-ray source at the position of 1FGL J1311.7, but both spectral and temporal features do not resemble that of blazars or the gamma-ray pulsars. Meanwhile, an X-ray counterpart of 1FGL J2339.7 shows extremely hard spectrum with its photon index 1.1, which seems to connect smoothly with a bump feature around 2GeV. We will characterize variability and spectral properties of these peculiar X-ray counterparts and firmly understand the nature/origin of "new-type" GeV gamma-ray sources. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | KATAOKA | JUN | NULL | NULL | JAP | 6 | AO6 | SUZAKU OBSERVATIONS OF "NEW-TYPE'' GAMMA-RAY SOURCES DETECTED WITH FERMI-LAT | XIS | Y |
| NGC6251_LOBE | 246.4248 | 82.6439 | 116.00587189 | 31.32598662 | 26.9674 | 55666.2760069444 | 55667.0258564815 | 706003010 | 38077.9 | 40000 | 38077.9 | 38077.9 | 0 | 38077.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37527.6 | 37527.6 | 64784 | 0 | PROCESSED | 57601.5103356482 | 56058 | 55690.9897685185 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060004 | We propose a Suzaku observation of "Gamma-ray lobe" accociated with a FR-I/II radio galaxy NGC6251. This is the second discovery next to Cen-A lobe with Fermi-LAT above 100 MeV. Compared to huge angular extent of Cen-A (~10 degree), the lobe of NGC 6251 is comfortably fit within an XIS-FOV, but its physical size is almost the same as Cen-A(~Mpc). We can therefore estimate the total power accumulated in lobe with much less uncertainties, and pressure balance between non-thermal electrons and external thermal cluster medium, that may reveal possible contributions of hidden protons in the lobe. We propose a 40 ksec observation of NGC 6251 centered on the NW-lobe, with additional 20 ksec x 2 observations at "OFF-src" positions to improve the background estimate. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | KATAOKA | JUN | NULL | NULL | JAP | 6 | AO6 | SUZAKU OBSERVATION OF "GAMMA-RAY LOBE'' IN A RADIO GALAXY NGC6251 | XIS | Y |
| NGC6251_LOBE_BGD1 | 247.6537 | 82.9256 | 116.18672095 | 31.0445068 | 26.9624 | 55667.0269328704 | 55667.4328125 | 706004010 | 18822 | 20000 | 18835.7 | 18822 | 0 | 18835.6 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 18957.2 | 18957.2 | 35065.9 | 1 | PROCESSED | 57601.5125694445 | 56058 | 55691.0888194444 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060004 | We propose a Suzaku observation of "Gamma-ray lobe" accociated with a FR-I/II radio galaxy NGC6251. This is the second discovery next to Cen-A lobe with Fermi-LAT above 100 MeV. Compared to huge angular extent of Cen-A (~10 degree), the lobe of NGC 6251 is comfortably fit within an XIS-FOV, but its physical size is almost the same as Cen-A(~Mpc). We can therefore estimate the total power accumulated in lobe with much less uncertainties, and pressure balance between non-thermal electrons and external thermal cluster medium, that may reveal possible contributions of hidden protons in the lobe. We propose a 40 ksec observation of NGC 6251 centered on the NW-lobe, with additional 20 ksec x 2 observations at "OFF-src" positions to improve the background estimate. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | KATAOKA | JUN | NULL | NULL | JAP | 6 | AO6 | SUZAKU OBSERVATION OF "GAMMA-RAY LOBE'' IN A RADIO GALAXY NGC6251 | XIS | Y |
| NGC6251_LOBE_BGD2 | 245.2973 | 82.3586 | 115.82251183 | 31.60630628 | 26.9772 | 55667.4343981482 | 55667.8230902778 | 706005010 | 12010.3 | 20000 | 12018.3 | 12010.3 | 0 | 12026.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17585.1 | 17585.1 | 33575.9 | 0 | PROCESSED | 57601.5154976852 | 56058 | 55690.9834490741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060004 | We propose a Suzaku observation of "Gamma-ray lobe" accociated with a FR-I/II radio galaxy NGC6251. This is the second discovery next to Cen-A lobe with Fermi-LAT above 100 MeV. Compared to huge angular extent of Cen-A (~10 degree), the lobe of NGC 6251 is comfortably fit within an XIS-FOV, but its physical size is almost the same as Cen-A(~Mpc). We can therefore estimate the total power accumulated in lobe with much less uncertainties, and pressure balance between non-thermal electrons and external thermal cluster medium, that may reveal possible contributions of hidden protons in the lobe. We propose a 40 ksec observation of NGC 6251 centered on the NW-lobe, with additional 20 ksec x 2 observations at "OFF-src" positions to improve the background estimate. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | KATAOKA | JUN | NULL | NULL | JAP | 6 | AO6 | SUZAKU OBSERVATION OF "GAMMA-RAY LOBE'' IN A RADIO GALAXY NGC6251 | XIS | Y |
| NGC6251_LOBE_BGD2 | 245.3877 | 82.3337 | 115.79036875 | 31.61025625 | 299.99 | 55789.4176967593 | 55789.6225 | 706005020 | 11178 | 10000 | 11178 | 11178 | 0 | 11178 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9788 | 9788 | 17687.9 | 0 | PROCESSED | 57602.7824421296 | 56173 | 55805.1871527778 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060004 | We propose a Suzaku observation of "Gamma-ray lobe" accociated with a FR-I/II radio galaxy NGC6251. This is the second discovery next to Cen-A lobe with Fermi-LAT above 100 MeV. Compared to huge angular extent of Cen-A (~10 degree), the lobe of NGC 6251 is comfortably fit within an XIS-FOV, but its physical size is almost the same as Cen-A(~Mpc). We can therefore estimate the total power accumulated in lobe with much less uncertainties, and pressure balance between non-thermal electrons and external thermal cluster medium, that may reveal possible contributions of hidden protons in the lobe. We propose a 40 ksec observation of NGC 6251 centered on the NW-lobe, with additional 20 ksec x 2 observations at "OFF-src" positions to improve the background estimate. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | KATAOKA | JUN | NULL | NULL | JAP | 6 | AO6 | SUZAKU OBSERVATION OF "GAMMA-RAY LOBE'' IN A RADIO GALAXY NGC6251 | XIS | Y |
| 1ES 1927+654 | 291.8157 | 65.5862 | 97.0030083 | 20.97400385 | 83.4311 | 55667.8280092593 | 55669.2425115741 | 706006010 | 71888.9 | 100000 | 71912.9 | 71888.9 | 0 | 71912.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 79664.7 | 79664.7 | 122191.9 | 0 | PROCESSED | 57601.5407986111 | 56059 | 55691.2683912037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060008 | 1ES 1927+654, an X-ray unabsorbed optically classified type-2 AGN, challenges the standard unified model. What is known about its X-ray characteristics suggest it can provide tremendous insight. It is extremely bright and will render close to 20 ct/s in the combined XIS providing sufficient data to unambiguously detect features in the Fe~K region, distinguish absorption and reflection models, and study its rapid variability. Even in the most conservative estimates a PIN detection is expected. It is persistently variable on short time scales and in combination with the long duration of Suzaku observations, the proposed observationswill yield fruitful variability studies. It has never been observed by Suzaku thus guaranteeing significant opportunity for discovery. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | GALLO | LUIGI | NULL | NULL | JAP | 6 | AO6 | REVEALING THE NATURE OF AN X-RAY ABSORBED SEYFERT 2 | XIS | Y |
| HESS J1943+213 | 295.9916 | 21.301 | 57.76229591 | -1.30331963 | 246.7107 | 55875.6293055556 | 55876.6015393518 | 706007010 | 38881.5 | 40000 | 38881.5 | 38889.5 | 0 | 38889.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35313 | 35313 | 83972 | 1 | PROCESSED | 57603.7570601852 | 56256 | 55890.6970833333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060028 | A new point-like source HESS J1943+213 has been detected at TeV energies at the position coinciding with the unidentified hard X-ray objects IGR J19443+2117. All the available observational constraints favor an identification of HESS J1943+213 as a BL Lac at redshift z>0.14. If correct, this would be the first time an AGN is discovered serendipitously from TeV observations in the Galactic Plane. It would be also the most extreme BL Lac known, with the persistent synchrotron continuum extending up to the observed energies >100 keV. A good quality broad X-ray spectrum is needed to confirm the blazar association and the extreme character of the peculiar object HESS J1943+213. Here we argue that a relatively moderate Suzaku exposure of 40 ksec will enable us to obtain such a spectrum. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | STAWARZ | LUKASZ | NULL | NULL | JAP | 6 | AO6 | PECULIAR UNIDENTIFIED TEV SOURCE HESS J1943+213 IN THE GALACTIC PLANE: EXTREME BLAZAR OR SOMETHING ELSE? | XIS | Y |
| SWIFT J0709.4-3559 | 107.3109 | -36.0226 | 247.327711 | -12.25710974 | 260.0142 | 55653.0945601852 | 55655.0640393518 | 706008010 | 81173.9 | 80000 | 81173.9 | 81173.9 | 0 | 81173.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 61462.1 | 61462.1 | 170123.9 | 2 | PROCESSED | 57601.393287037 | 56037 | 55670.2451967593 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060030 | The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to population synthesis models, its estimate is strongly coupled with the broad band spectral shape of Compton thin AGNs. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright AGNs that can be best followed-up with Suzaku. Previously, such studies have been limited to AGNs with low to intermediate luminosities. Here we propose to observe two of the most luminous AGNs in the latest BAT catalog to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 6 | AO6 | BROAD BAND SPECTRA OF HARD X-RAY SELECTED ULTRALUMINOUS AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND | XIS | Y |
| SWIFT J1310.9-5553 | 197.6868 | -55.8722 | 305.6577855 | 6.89731776 | 290.4478 | 55761.4489467593 | 55762.6432523148 | 706009010 | 82785 | 80000 | 82793 | 82785 | 0 | 82785 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 67508.1 | 67508.1 | 103177.9 | 1 | PROCESSED | 57602.6323263889 | 56213 | 55845.247662037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060030 | The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to population synthesis models, its estimate is strongly coupled with the broad band spectral shape of Compton thin AGNs. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright AGNs that can be best followed-up with Suzaku. Previously, such studies have been limited to AGNs with low to intermediate luminosities. Here we propose to observe two of the most luminous AGNs in the latest BAT catalog to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 6 | AO6 | BROAD BAND SPECTRA OF HARD X-RAY SELECTED ULTRALUMINOUS AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND | XIS | Y |
| 2MASX J15115979-2119 | 227.9997 | -21.3083 | 341.57056512 | 30.81939061 | 105.6253 | 55979.0551388889 | 55980.937650463 | 706010010 | 83816.2 | 80000 | 83816.2 | 83816.2 | 0 | 83816.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 82256.8 | 82256.8 | 162635.9 | 1 | PROCESSED | 57604.7185763889 | 56361 | 55995.1640393518 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060032 | We propose to observe two hard X-ray bright narrow-line Seyfert 1 galaxies, which are an important class of objects in studying accretion processes under a large mass accretion rate and therefore mass growth of black holes. Our aims are (1) to measure a continuum shape such as spectral slope and high energy cutoff, (2) to compare them with other classes of AGNs, and (3) to search for highly ionized outflows with a large column density. All of these will be a fundamental piece of information to better understand accretion physics and ``feedback'' processes in galaxies. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | TERASHIMA | YUICHI | NULL | NULL | JAP | 6 | AO6 | ACCRETION AND OUTFLOW IN THE HARD X-RAY SELECTED NARROW-LINE SEYFERT 1S | XIS | Y |
| WKK 4438 | 223.8214 | -51.5512 | 321.7239088 | 6.74451921 | 87.8973 | 55948.1066319445 | 55950.0610069444 | 706011010 | 70308.8 | 100000 | 70316.8 | 70308.8 | 0 | 70324.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 61486 | 61486 | 168825.9 | 3 | PROCESSED | 57604.5330324074 | 56469 | 56103.2331597222 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060032 | We propose to observe two hard X-ray bright narrow-line Seyfert 1 galaxies, which are an important class of objects in studying accretion processes under a large mass accretion rate and therefore mass growth of black holes. Our aims are (1) to measure a continuum shape such as spectral slope and high energy cutoff, (2) to compare them with other classes of AGNs, and (3) to search for highly ionized outflows with a large column density. All of these will be a fundamental piece of information to better understand accretion physics and ``feedback'' processes in galaxies. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | TERASHIMA | YUICHI | NULL | NULL | JAP | 6 | AO6 | ACCRETION AND OUTFLOW IN THE HARD X-RAY SELECTED NARROW-LINE SEYFERT 1S | XIS | Y |
| IC 4518A | 224.419 | -43.1269 | 326.11466585 | 13.99053707 | 102.9822 | 55959.1723263889 | 55961.0002777778 | 706012010 | 64398.6 | 60000 | 64398.6 | 64398.6 | 0 | 64398.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 57238.1 | 57238.1 | 157905.8 | 1 | PROCESSED | 57604.5692708333 | 56434 | 56068.6321064815 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060040 | We propose to observe the Compton-thin AGN IC 4518A with a very small L_X/L_IR ratio, which has often been employed as an indicator of the presence of a Compton-thick AGN. Our aim is to examine the recent argument that L_X/L_IR is not a good measure of absorption column densities and that this ratio is more dependent on the covering fraction of absorber and intrinsic spectral shape. We measure the spectral slope, covering fraction, and NH, and compare them with the prediction of Monte-Carlo simulations to test the validity of L_X/L_IR as a measure of Compton thickness. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | HIRATA | YOSHITAKA | NULL | NULL | JAP | 6 | AO6 | BROAD-BAND SPECTRA OF THE COMPTON-THIN AGN IC 4518A WITH A SMALL L_X/L_IR: TESTING VALIDITY OF A COMPTON-THICK INDICATOR | XIS | Y |
| 3C78 | 47.1071 | 4.1138 | 174.85308943 | -44.51284685 | 84.4195 | 55793.5846990741 | 55795.7502430556 | 706013010 | 97012.2 | 100000 | 97012.2 | 97012.2 | 0 | 97012.2 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 85907.5 | 85907.5 | 187087.8 | 0 | PROCESSED | 57602.928275463 | 56176 | 55806.3891435185 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060046 | We propose to observe two radio galaxies 3C78 and PKS0625-354 which were detected by the Fermi gamma-ray satellte survey during the 1st year, in order to investigate the X-ray emission more precisely than ever. In the case of jet emission, we can constrain the jet parameter well from the multi-wavelength spectrum and obtain the jet kinetic energy. In the case of disk emission, we can obtain the jet to disk energy ratio. This observation will enable us to obtain the jet parameters of these galaxies and compare them with others. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | FUKAZAWA | YASUSHI | NULL | NULL | JAP | 6 | AO6 | ORIGIN OF THE X-RAY EMISSION OF GAMAM-RAY RADIO GALAXIES 3C78 AND PKS0625-354 | XIS | Y |
| PKS0625-354 | 96.7724 | -35.4904 | 243.45420005 | -19.97253333 | 121.4596 | 55868.6502199074 | 55871.6231597222 | 706014010 | 100719.8 | 100000 | 100727.8 | 100727.8 | 0 | 100719.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 86434.2 | 86434.2 | 256813.8 | 4 | PROCESSED | 57603.7550231482 | 56250 | 55881.2887731482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060046 | We propose to observe two radio galaxies 3C78 and PKS0625-354 which were detected by the Fermi gamma-ray satellte survey during the 1st year, in order to investigate the X-ray emission more precisely than ever. In the case of jet emission, we can constrain the jet parameter well from the multi-wavelength spectrum and obtain the jet kinetic energy. In the case of disk emission, we can obtain the jet to disk energy ratio. This observation will enable us to obtain the jet parameters of these galaxies and compare them with others. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | FUKAZAWA | YASUSHI | NULL | NULL | JAP | 6 | AO6 | ORIGIN OF THE X-RAY EMISSION OF GAMAM-RAY RADIO GALAXIES 3C78 AND PKS0625-354 | XIS | Y |
| 3C 98 | 59.723 | 10.4395 | 179.82925767 | -31.05249617 | 81.003 | 55812.5811342593 | 55815.280787037 | 706015010 | 101144 | 100000 | 101144 | 101144 | 0 | 101144 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 89838.9 | 89838.9 | 233214 | 3 | PROCESSED | 57603.1723611111 | 56218 | 55851.4528356482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060055 | Whether radio-loud and radio-quiet AGN may be unified under one model is still open to debate. The most important limitation in such work is that jet beaming swamps nuclear emission, so we must study powerful radio sources which are not affected by this bias. These are the Narrow Line Radio Galaxies (NLRGs). Heavy obscuration means that their primary emission is visible only above 10 keV. 3C 98 is an important member of the NLRG class because its hard band power dominates the full radio to X-ray core luminosity. We propose a 100 ks observation of this source with Suzaku to detect the core continuum emission and reflection above 10 keV. 3C~98 is one of few NLRGs for which we can expect to model (rather than just detect) the hard X-ray flux, and hence use it for testing unification schemes. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | GANDHI | POSHAK | NULL | NULL | JAP | 6 | AO6 | HARD X-RAY EMISSION AND REFLECTION IN RADIO GALAXIES: 3C 98 | XIS | Y |
| PG 1626+554 | 247.0224 | 55.3701 | 84.50112094 | 42.16849703 | 200.5289 | 55876.6090046296 | 55877.9341550926 | 706017010 | 60848.8 | 60000 | 60848.8 | 60848.8 | 0 | 60848.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 56132.8 | 56132.8 | 114463.9 | 2 | PROCESSED | 57603.7696412037 | 56256 | 55890.6981828704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060069 | Measurement of iron abundance in active galactic nuclei (AGN) relative to that of alpha-elements possesses potential of elucidating the cosmic chemical evolution, in particular, when the formation of the first stars initiated. However, it has been found that iron abundances estimated from FeII(opt) and FeII(UV) in the broad line region (BLR) do not agree and their ratio is dependent on the BLR cloud column densities. Thus, in order to derive precise AGN iron abundances, independent measurement of the BLR cloud column densities is required. Here we propose to obtain precise X-ray energy spectra of several AGNs, of which FeII(opt)/FeII(UV) values we have already measured. By combining the optical and X-ray spectra, we can estimate iron abundances of these targets more precisely than ever. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | SAMESHIMA | HIROAKI | NULL | NULL | JAP | 6 | AO6 | X-RAY MEASUREMENTS OF COLUMN DENSITIES OF THE BROAD LINE REGION CLOUDS TO CONSTRAIN THE COSMIC CHEMICAL EVOLUTION | XIS | Y |
| PG 1322+659 | 200.9787 | 65.7065 | 117.62442893 | 51.08576313 | 141.5827 | 55892.4154050926 | 55894.0862268518 | 706018010 | 81686.9 | 80000 | 81710.9 | 81686.9 | 0 | 81710.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 78916.8 | 78916.8 | 144343.9 | 2 | PROCESSED | 57603.9954513889 | 56274 | 55907.1929282407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060069 | Measurement of iron abundance in active galactic nuclei (AGN) relative to that of alpha-elements possesses potential of elucidating the cosmic chemical evolution, in particular, when the formation of the first stars initiated. However, it has been found that iron abundances estimated from FeII(opt) and FeII(UV) in the broad line region (BLR) do not agree and their ratio is dependent on the BLR cloud column densities. Thus, in order to derive precise AGN iron abundances, independent measurement of the BLR cloud column densities is required. Here we propose to obtain precise X-ray energy spectra of several AGNs, of which FeII(opt)/FeII(UV) values we have already measured. By combining the optical and X-ray spectra, we can estimate iron abundances of these targets more precisely than ever. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | SAMESHIMA | HIROAKI | NULL | NULL | JAP | 6 | AO6 | X-RAY MEASUREMENTS OF COLUMN DENSITIES OF THE BROAD LINE REGION CLOUDS TO CONSTRAIN THE COSMIC CHEMICAL EVOLUTION | XIS | Y |
| 1FGL J0103.1+4840 | 15.7305 | 48.657 | 124.88749892 | -14.17113818 | 69.2705 | 55753.0127430556 | 55755.0002199074 | 706025010 | 84362.2 | 80000 | 84362.2 | 84362.2 | 0 | 84362.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 79727 | 79727 | 171695.7 | 2 | PROCESSED | 57602.5903935185 | 56148 | 55778.4339814815 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060084 | In this proposal, we'd like to make a suggestion of 2 "steady" unassociated Fermi-LAT gamma-ray sources with Suzaku. 2-year Fermi-LAT observation detected 2412 sources, but 1194 sources are still unassociated. Proposed objects are located at high Galactic latitude, and selected not likely to be associated with blazar(AGN) and pulsar. These lightcurves do not show the significant temporal variability. To confirm their stability, we checked Test Statistic Value of 1FGL and 2-year Fermi observation. Deep Observation with Suzaku (1FGLJ0103: 80ks, 1FGL1946:40ks) is expected to reveal the nature of these unassociated objects, or at least impose strict limits at 2-10keV. Of course, it is necessary that multi-wavelength observation. We'll plan to arrange tie-ups with other wavelength researcher. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | MAEDA | KOTO | NULL | NULL | JAP | 6 | AO6 | SUZAKU OBSERVATION OF "STEADY" UNASSOCIATED FERMI-LAT GAMMA-RAY SOURCES AT HIGH GALACTIC LATITUDE | XIS | Y |
| 1FGL J1946.7-5404 | 296.6052 | -54.0506 | 343.89458124 | -29.55670998 | 268.6577 | 55865.7799074074 | 55866.783599537 | 706026010 | 42395.9 | 40000 | 42395.9 | 42398.8 | 0 | 42398.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 54883.3 | 54883.3 | 86707.9 | 0 | PROCESSED | 57603.6796990741 | 56246 | 55879.1861574074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060084 | In this proposal, we'd like to make a suggestion of 2 "steady" unassociated Fermi-LAT gamma-ray sources with Suzaku. 2-year Fermi-LAT observation detected 2412 sources, but 1194 sources are still unassociated. Proposed objects are located at high Galactic latitude, and selected not likely to be associated with blazar(AGN) and pulsar. These lightcurves do not show the significant temporal variability. To confirm their stability, we checked Test Statistic Value of 1FGL and 2-year Fermi observation. Deep Observation with Suzaku (1FGLJ0103: 80ks, 1FGL1946:40ks) is expected to reveal the nature of these unassociated objects, or at least impose strict limits at 2-10keV. Of course, it is necessary that multi-wavelength observation. We'll plan to arrange tie-ups with other wavelength researcher. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | MAEDA | KOTO | NULL | NULL | JAP | 6 | AO6 | SUZAKU OBSERVATION OF "STEADY" UNASSOCIATED FERMI-LAT GAMMA-RAY SOURCES AT HIGH GALACTIC LATITUDE | XIS | Y |
| RX J1633+4718 | 248.3303 | 47.3072 | 73.53738657 | 42.62611906 | 329.4078 | 55743.8204050926 | 55744.8460069444 | 706027010 | 39991.6 | 40000 | 39991.6 | 39991.6 | 0 | 39991.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39653.1 | 39653.1 | 88605.9 | 1 | PROCESSED | 57602.4692013889 | 56144 | 55775.3057407407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060089 | RX J1633+4718 was detected in the ROSAT all sky survey, later identified as a radio loud narrow line Seyfert 1 (NLS1) galaxy. The soft X-ray spectrum of this source was fitted with a blackbody with temperature of 32eV plus a flat power law component. The blackbody temperature is much lower than 100-200eV, typical soft X-ray excess commonly observed in NLS1. Since radio to UV continuum spectrum of this souce resembles those of blazars, the flat power law X-ray component is likely to be a jet origin. The jet might supress accretion corona, and thus the emission from the accretion disk might visible in its bare form. Suzaku observation of this source will give us X-ray spectrum above 2keV and CCD resolution spectrum below 2keV for the 1st time. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | HAYASHIDA | KIYOSHI | NULL | NULL | JAP | 6 | AO6 | X-RAY EMISSION FROM DISK AND JET AROUND A SMBH IN RX J1633+4718 | XIS | Y |
| RX J1633+4718 | 248.3342 | 47.2989 | 73.52584527 | 42.62417772 | 308.6809 | 55760.5047916667 | 55761.4376388889 | 706027020 | 37510 | 40000 | 37510 | 37510 | 0 | 37510 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57602.5962847222 | 56152 | 55830.7262268518 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060089 | RX J1633+4718 was detected in the ROSAT all sky survey, later identified as a radio loud narrow line Seyfert 1 (NLS1) galaxy. The soft X-ray spectrum of this source was fitted with a blackbody with temperature of 32eV plus a flat power law component. The blackbody temperature is much lower than 100-200eV, typical soft X-ray excess commonly observed in NLS1. Since radio to UV continuum spectrum of this souce resembles those of blazars, the flat power law X-ray component is likely to be a jet origin. The jet might supress accretion corona, and thus the emission from the accretion disk might visible in its bare form. Suzaku observation of this source will give us X-ray spectrum above 2keV and CCD resolution spectrum below 2keV for the 1st time. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | HAYASHIDA | KIYOSHI | NULL | NULL | JAP | 6 | AO6 | X-RAY EMISSION FROM DISK AND JET AROUND A SMBH IN RX J1633+4718 | XIS | Y |
| RX J1633+4718 | 248.3661 | 47.3315 | 73.56753068 | 42.5999019 | 136.9343 | 55939.8747337963 | 55940.8307407407 | 706027030 | 44127.1 | 40000 | 44127.1 | 44127.1 | 0 | 44127.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38957.8 | 38957.8 | 82592 | 0 | PROCESSED | 57604.3578703704 | 56331 | 55960.228587963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060089 | RX J1633+4718 was detected in the ROSAT all sky survey, later identified as a radio loud narrow line Seyfert 1 (NLS1) galaxy. The soft X-ray spectrum of this source was fitted with a blackbody with temperature of 32eV plus a flat power law component. The blackbody temperature is much lower than 100-200eV, typical soft X-ray excess commonly observed in NLS1. Since radio to UV continuum spectrum of this souce resembles those of blazars, the flat power law X-ray component is likely to be a jet origin. The jet might supress accretion corona, and thus the emission from the accretion disk might visible in its bare form. Suzaku observation of this source will give us X-ray spectrum above 2keV and CCD resolution spectrum below 2keV for the 1st time. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | HAYASHIDA | KIYOSHI | NULL | NULL | JAP | 6 | AO6 | X-RAY EMISSION FROM DISK AND JET AROUND A SMBH IN RX J1633+4718 | XIS | Y |
| RX J1633+4718 | 248.3647 | 47.3332 | 73.56993988 | 42.60070523 | 133.9355 | 55962.6778240741 | 55963.7502430556 | 706027040 | 45483.4 | 40000 | 45483.4 | 45483.4 | 0 | 45483.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40311.3 | 40311.3 | 92645.9 | 0 | PROCESSED | 57604.5712152778 | 56345 | 55978.5479282407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060089 | RX J1633+4718 was detected in the ROSAT all sky survey, later identified as a radio loud narrow line Seyfert 1 (NLS1) galaxy. The soft X-ray spectrum of this source was fitted with a blackbody with temperature of 32eV plus a flat power law component. The blackbody temperature is much lower than 100-200eV, typical soft X-ray excess commonly observed in NLS1. Since radio to UV continuum spectrum of this souce resembles those of blazars, the flat power law X-ray component is likely to be a jet origin. The jet might supress accretion corona, and thus the emission from the accretion disk might visible in its bare form. Suzaku observation of this source will give us X-ray spectrum above 2keV and CCD resolution spectrum below 2keV for the 1st time. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | HAYASHIDA | KIYOSHI | NULL | NULL | JAP | 6 | AO6 | X-RAY EMISSION FROM DISK AND JET AROUND A SMBH IN RX J1633+4718 | XIS | Y |
| 4C+74.26 | 310.7114 | 75.111 | 108.98584774 | 19.50187948 | 247.6342 | 55888.5409027778 | 55890.613275463 | 706028010 | 101412.5 | 100000 | 101412.5 | 101412.5 | 0 | 101412.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 117882.7 | 117882.7 | 179029.7 | 2 | PROCESSED | 57603.9949074074 | 56269 | 55901.2441203704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060101 | We propose the 120 ks observation of Broad Line Radio Galaxy 4C+74.26. The purpose is to estimate the angular momentum of the central super massive black hole from the broadness of Fe-K line. We study the spectral changes on spectra in details on the Fe-K lines and reflection hump in HXD-PIN band. We try to study the correlation between the radio intensity and black hole spins. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | NODA | HIROFUMI | NULL | NULL | JAP | 6 | AO6 | STUSY OF BROAD IRON LINE OF 4C+74.26 TO ESTIMATE THE SPIN OF CENTRAL SUPER MASSIVE BLACK HOLE | XIS | Y |
| MRK 841 | 226.0091 | 10.4587 | 11.24319757 | 54.63999984 | 112.9994 | 55931.8646180556 | 55937.1896990741 | 706029010 | 244351.8 | 350000 | 244351.8 | 244351.8 | 0 | 244359.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 229726 | 229726 | 419686 | 4 | PROCESSED | 57604.4310648148 | 55652 | 55946.5082407407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061119 | We propose deep Suzaku observations of 6 well-known AGN with the primary aim of studying strong-gravitational physics close to these supermassive black holes (SMBH). We will conduct the first ever census of local SMBH spin, providing a new window on the growth-history of SMBHs. Suzaku's unique combination of high-throughput in the iron-K band and hard-band (>10keV) sensitivity is crucial, permitting a separation of the disk-reflection spectrum (which encodes the relativistic physics) from the effects of the warm absorber and low-velocity emission/reflection. These six datasets will be an important legacy of Suzaku, providing an important resource for AGN researchers for at least the next decade. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | REYNOLDS | CHRISTOPHER | NULL | NULL | USA | 6 | AO6-LP | A SURVEY OF BLACK HOLE SPIN AND RELATIVISTIC PHYSICS IN AGN | XIS | Y |
| MRK 841 | 226.0057 | 10.444 | 11.21871304 | 54.63485497 | 108.0015 | 55944.7625347222 | 55947.3599305556 | 706029020 | 110289 | 350000 | 110291.5 | 110289 | 0 | 110291.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 92218.2 | 92218.2 | 224404 | 1 | PROCESSED | 57604.469224537 | 55652 | 55985.3097337963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061119 | We propose deep Suzaku observations of 6 well-known AGN with the primary aim of studying strong-gravitational physics close to these supermassive black holes (SMBH). We will conduct the first ever census of local SMBH spin, providing a new window on the growth-history of SMBHs. Suzaku's unique combination of high-throughput in the iron-K band and hard-band (>10keV) sensitivity is crucial, permitting a separation of the disk-reflection spectrum (which encodes the relativistic physics) from the effects of the warm absorber and low-velocity emission/reflection. These six datasets will be an important legacy of Suzaku, providing an important resource for AGN researchers for at least the next decade. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | REYNOLDS | CHRISTOPHER | NULL | NULL | USA | 6 | AO6-LP | A SURVEY OF BLACK HOLE SPIN AND RELATIVISTIC PHYSICS IN AGN | XIS | Y |
| SMC X-1 | 19.2829 | -73.4465 | 300.41108523 | -43.55576838 | 356.8796 | 55658.8646759259 | 55659.2447106482 | 706030010 | 18466.2 | 18000 | 18466.2 | 18550 | 0 | 18544.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15557.7 | 15557.7 | 32823.9 | 0 | PROCESSED | 57601.4235185185 | 56040 | 55673.2343055556 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061236 | We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | NEILSEN | JOSEPH | NULL | NULL | USA | 6 | AO6 | THE WANDERING WARP OF SMC X-1 | XIS | N |
| SMC X-1 | 19.2476 | -73.446 | 300.42473809 | -43.55764171 | 6.4299 | 55669.2561805556 | 55669.705775463 | 706030020 | 17276.9 | 18000 | 17276.9 | 17284.9 | 0 | 17484.4 | 2 | 2 | 0 | 1 | 1 | 0 | 0 | 17664.6 | 17664.6 | 38815.9 | 0 | PROCESSED | 57601.5313657407 | 56058 | 55691.1543171296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061236 | We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | NEILSEN | JOSEPH | NULL | NULL | USA | 6 | AO6 | THE WANDERING WARP OF SMC X-1 | XIS | N |
| SMC X-1 | 19.2337 | -73.4445 | 300.42986971 | -43.55966827 | 9.1005 | 55673.6490625 | 55674.1112037037 | 706030030 | 15652.6 | 18000 | 15652.6 | 15652.6 | 0 | 15871 | 2 | 2 | 0 | 1 | 1 | 0 | 0 | 21261.4 | 21261.4 | 39919.9 | 1 | PROCESSED | 57601.5606597222 | 56067 | 55692.2968634259 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061236 | We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | NEILSEN | JOSEPH | NULL | NULL | USA | 6 | AO6 | THE WANDERING WARP OF SMC X-1 | XIS | N |
| SMC X-1 | 19.2724 | -73.4484 | 300.41553375 | -43.55429702 | 25.8573 | 55691.0197337963 | 55691.4064814815 | 706030040 | 17905.4 | 18000 | 17921.4 | 17921.4 | 0 | 17905.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16814.3 | 16814.3 | 33407.9 | 0 | PROCESSED | 57601.9922222222 | 56068 | 55701.1543981482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061236 | We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | NEILSEN | JOSEPH | NULL | NULL | USA | 6 | AO6 | THE WANDERING WARP OF SMC X-1 | XIS | N |
| SMC X-1 | 19.2828 | -73.4495 | 300.41169288 | -43.55280074 | 39.2778 | 55706.0851851852 | 55706.6745833333 | 706030050 | 17846.3 | 18000 | 17846.3 | 18182.3 | 0 | 18100.1 | 2 | 2 | 0 | 1 | 1 | 0 | 0 | 16682.9 | 16682.9 | 50913.9 | 0 | PROCESSED | 57602.111099537 | 56092 | 55725.1651736111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061236 | We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | NEILSEN | JOSEPH | NULL | NULL | USA | 6 | AO6 | THE WANDERING WARP OF SMC X-1 | XIS | N |
| SMC X-1 | 19.2661 | -73.446 | 300.41753301 | -43.55692043 | 64.0051 | 55740.5953819444 | 55741.0960069444 | 706030060 | 18668.2 | 18000 | 18712.9 | 18704.9 | 0 | 18668.2 | 2 | 2 | 0 | 1 | 1 | 0 | 0 | 20676.4 | 20676.4 | 43247.9 | 0 | PROCESSED | 57602.4222800926 | 56163 | 55775.167974537 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061236 | We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | NEILSEN | JOSEPH | NULL | NULL | USA | 6 | AO6 | THE WANDERING WARP OF SMC X-1 | XIS | N |
| SMC X-1 | 19.2772 | -73.44 | 300.41207357 | -43.56242986 | 167.9636 | 55825.1720949074 | 55825.6536805556 | 706030070 | 18123.9 | 18000 | 18277.2 | 18285.2 | 0 | 18123.9 | 2 | 2 | 0 | 1 | 1 | 0 | 0 | 18368.7 | 18368.7 | 41595.9 | 0 | PROCESSED | 57603.2202662037 | 56218 | 55851.4509027778 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061236 | We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | NEILSEN | JOSEPH | NULL | NULL | USA | 6 | AO6 | THE WANDERING WARP OF SMC X-1 | XIS | N |
| SMC X-1 | 19.2675 | -73.4407 | 300.41598527 | -43.56211574 | 204.2035 | 55875.0768055556 | 55875.6182291667 | 706030080 | 19859.8 | 18000 | 19888.1 | 19896.1 | 0 | 19859.8 | 2 | 2 | 0 | 1 | 1 | 0 | 0 | 19250.8 | 19250.8 | 46772 | 0 | PROCESSED | 57603.7203587963 | 56260 | 55890.6941203704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061236 | We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | NEILSEN | JOSEPH | NULL | NULL | USA | 6 | AO6 | THE WANDERING WARP OF SMC X-1 | XIS | N |
| SMC X-1 | 19.2766 | -73.4376 | 300.41185267 | -43.56483062 | 244.987 | 55907.8985069444 | 55908.2709722222 | 706030090 | 17305.5 | 18000 | 17407.9 | 17407.9 | 0 | 17305.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 18413 | 18413 | 32171.9 | 0 | PROCESSED | 57604.1197685185 | 56289 | 55920.9743981482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061236 | We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | NEILSEN | JOSEPH | NULL | NULL | USA | 6 | AO6 | THE WANDERING WARP OF SMC X-1 | XIS | N |
| SMC X-1 | 19.2681 | -73.4483 | 300.41718915 | -43.55456404 | 342.3682 | 56005.2598611111 | 56005.8452546296 | 706030100 | 18582.1 | 18000 | 18626.3 | 18634.3 | 0 | 18582.1 | 2 | 2 | 0 | 1 | 1 | 0 | 0 | 20306.1 | 20306.1 | 50571.9 | 0 | PROCESSED | 57604.9618055556 | 56399 | 56022.2021296296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061236 | We propose a sequence of 10 18-ks observations of the wind-fed accreting X-ray pulsar SMC X-1. Distributed throughout the orbital and super-orbital period of this high-mass X-ray binary, our proposed observations will reveal the influence of wind accretion on the structure and evolution of accretion disks via three independent methods: (1) mapping the geometry of the accretion flow through soft X-ray emission line variability and ionization studies, (2) tracing the structure of the accretion disk corona with hard X-ray scattering studies, and (3) tracking the evolution of the neutron star spin period and pulse profile for comparison to changes in the warped, precessing accretion disk. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | NEILSEN | JOSEPH | NULL | NULL | USA | 6 | AO6 | THE WANDERING WARP OF SMC X-1 | XIS | N |
| III ZW 2 | 2.6244 | 10.9839 | 106.97577765 | -50.61513425 | 67.4163 | 55726.9877893518 | 55728.9792708333 | 706031010 | 81466 | 80000 | 81466 | 81466 | 0 | 81466 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 74362.9 | 74362.9 | 172039.7 | 3 | PROCESSED | 57602.3450925926 | 56127 | 55757.7040046296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061411 | Fermi-LAT has revealed gamma-ray emission from Seyfert galaxies in its 1st catalog. Optical and X-ray spectra of Seyferts generally provide important clues to the nature of the accretion process, and thus those objects are promising targets to investigate the connection of the jet to the central source. Here, we propose Suzaku observations of three Seyfert-type AGNs from our gamma-ray candidate list: those objects are also present in the Swift-BAT catalog. Those are III Zw 2, NGC 6814 and ESO 323-G077 and we request pointings of 80 ks, 40 ks and 40 ks respectively. All three candidates appear to be associated with AGN, but show different radio or IR properties. Suzaku data will give us crucial information to investigate the origin of high-energy emission from those Seyfert objects. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | HAYASHIDA | MASAAKI | NULL | NULL | USA | 6 | AO6 | SUZAKU OBSERVATIONS OF SEYFERT GALAXIES AS GAMMA-RAY SOURCE CANDIDATES SELECTED FROM THE SWIFT-BAT CATALOG | XIS | Y |
| NGC 6814 | 295.6733 | -10.3371 | 29.34034439 | -16.02176478 | 260.0004 | 55867.6992013889 | 55868.637662037 | 706032010 | 42120 | 40000 | 42143.5 | 42136 | 0 | 42120 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40091.8 | 40091.8 | 81069.8 | 1 | PROCESSED | 57603.6893518518 | 56248 | 55881.0746527778 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061411 | Fermi-LAT has revealed gamma-ray emission from Seyfert galaxies in its 1st catalog. Optical and X-ray spectra of Seyferts generally provide important clues to the nature of the accretion process, and thus those objects are promising targets to investigate the connection of the jet to the central source. Here, we propose Suzaku observations of three Seyfert-type AGNs from our gamma-ray candidate list: those objects are also present in the Swift-BAT catalog. Those are III Zw 2, NGC 6814 and ESO 323-G077 and we request pointings of 80 ks, 40 ks and 40 ks respectively. All three candidates appear to be associated with AGN, but show different radio or IR properties. Suzaku data will give us crucial information to investigate the origin of high-energy emission from those Seyfert objects. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | HAYASHIDA | MASAAKI | NULL | NULL | USA | 6 | AO6 | SUZAKU OBSERVATIONS OF SEYFERT GALAXIES AS GAMMA-RAY SOURCE CANDIDATES SELECTED FROM THE SWIFT-BAT CATALOG | XIS | Y |
| ESO 323-G077 | 196.6073 | -40.4236 | 306.0162391 | 22.35835315 | 295.8925 | 55762.647337963 | 55763.4168287037 | 706033010 | 44122.2 | 40000 | 44122.2 | 44122.2 | 0 | 44122.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40925.8 | 40925.8 | 66481.9 | 0 | PROCESSED | 57602.6188310185 | 56212 | 55845.2395949074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061411 | Fermi-LAT has revealed gamma-ray emission from Seyfert galaxies in its 1st catalog. Optical and X-ray spectra of Seyferts generally provide important clues to the nature of the accretion process, and thus those objects are promising targets to investigate the connection of the jet to the central source. Here, we propose Suzaku observations of three Seyfert-type AGNs from our gamma-ray candidate list: those objects are also present in the Swift-BAT catalog. Those are III Zw 2, NGC 6814 and ESO 323-G077 and we request pointings of 80 ks, 40 ks and 40 ks respectively. All three candidates appear to be associated with AGN, but show different radio or IR properties. Suzaku data will give us crucial information to investigate the origin of high-energy emission from those Seyfert objects. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | HAYASHIDA | MASAAKI | NULL | NULL | USA | 6 | AO6 | SUZAKU OBSERVATIONS OF SEYFERT GALAXIES AS GAMMA-RAY SOURCE CANDIDATES SELECTED FROM THE SWIFT-BAT CATALOG | XIS | Y |
| ZW229-15 | 286.3333 | 42.4706 | 73.09172558 | 15.5517204 | 34.6696 | 55715.0128356482 | 55719.6251736111 | 706035010 | 167083.8 | 165000 | 168676.6 | 167083.8 | 0 | 168684.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 218183.2 | 218183.2 | 398435.7 | 2 | PROCESSED | 57602.3250694445 | 56127 | 55757.7055671296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061414 | The optical emission from AGN is though to be a combination of direct radiation from an accretion disk and reprocessed x-ray emission. Separating these components requires simultaneous high-precision x-ray/optical monitoring, which has heretofore not been achieved. We propose to gather this necessary data via simultaneous optical and x-ray monitoring of the Sy 1 galaxy Zw 229-15. Kepler is monitoring Zw 229-15 every 30 minutes with unprecedented 99% duty cycle and 0.1% repeatability. The key missing data is an appropriate x-ray campaign. We propose a 64-orbit (165 ks) Suzaku long-look combined with a series of 48 Swift visits to probe lags of 0.1-10 days. This will be the first experiment sensitive to such short lags and thus will critically test the present disc/reprocessing paradigm | EXTRAGALACTIC COMPACT SOURCES | 7 | B | MUSHOTZKY | RICHARD | NULL | NULL | USA | 6 | AO6 | SIMULTANEOUS SUZAKU/SWIFT/ KEPLER MONITORING OF ZW 229-15 | XIS | Y |
| B3 0309+411 | 48.2809 | 41.3324 | 149.59257755 | -14.09014879 | 253.0016 | 55976.5100462963 | 55979.0410532407 | 706036010 | 104624.5 | 100000 | 104624.5 | 104629.6 | 0 | 104624.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 95453 | 95453 | 218671.9 | 2 | PROCESSED | 57604.7018981482 | 56360 | 55992.2317824074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 062007 | We propose to observe B3 0309+411, an X--ray bright FRII BLRG detected by INTEGRAL for 100 ks. BRLGs have been poorly studied in X-rays and usually show weak reprocessing spectral features with respect to their radio-quiet counterparts. B3 0309+411 has been already followed-up with XMM-Newton and, the XMM-Newton and INTEGRAL data suggests that the source could 1) be strongly reflection-dominated; 2) exhibit extreme flux/spectral variability; 3) be severely affected by absorption. The Suzaku observation will unveil the puzzling spectral shape of this peculiar BLRG, allowing to determine with accuracy the reflection properties which would have a large impact on our understanding of the disk/jet contribution in BLRG. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | PANESSA | FRANCESCA | NULL | NULL | EUR | 6 | AO6 | B3 0309+411: A REFLECTION--DOMINATED BROAD LINE RADIO GALAXY? | XIS | Y |
| MRK 231 | 193.9205 | 56.8603 | 121.76268106 | 60.25831511 | 352.6128 | 55678.6054282407 | 55682.3543402778 | 706037010 | 197511.3 | 200000 | 197511.3 | 197511.3 | 0 | 197511.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 191743.4 | 191743.4 | 323875.6 | 2 | PROCESSED | 57602.0326851852 | 56065 | 55697.4231597222 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 062008 | We propose the first Suzaku observation of the nearest low-ionization BAL quasar/ULIRG, i.e. MRK 231, for which we have recently reported the most clear-cut evidence for AGN-driven feedback onto the host galaxy cold molecular gas component. Our target exhibits an hard X-ray (> 15 keV) excess in a previous BeppoSAX/PDS spectrum, suggesting the presence of a heavily obscured quasar at the heart of this peculiar system. By exploiting the Suzaku unique broad-band spectral coverage, we aim at deriving the column density of the nuclear absorber and, in turn, the intrinsic luminosity of the quasar with unprecedented accuracy. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | PICONCELLI | ENRICO | NULL | NULL | EUR | 6 | AO6 | BROAD-BAND X-RAY SPECTROSCOPY OF THE NEAREST BAL QUASAR/ULIRG MARKARIAN 231 | HXD | Y |
| IRAS 09104+4109 | 138.3378 | 40.9513 | 180.99146588 | 43.55010524 | 90.0004 | 55883.9878356482 | 55885.7675694444 | 706038010 | 81327.6 | 80000 | 81335.6 | 81327.6 | 0 | 81335.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 76588.3 | 76588.3 | 153730 | 2 | PROCESSED | 57603.9341203704 | 56264 | 55895.209849537 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 062009 | We propose to observe IRAS 09104+4109 for 80 ks with Suzaku in order to confirm the ~3 sigma BeppoSAX PDS detection of the source and increase the detection significance with the HXD/PIN to 10 sigma in the 10--80 keV band, allowing the detailed spectral shape to be determined. IRAS 09104+4109 is a hyperluminous Type 2 quasar embedded in a central cluster galaxy at redshift 0.442. It is likely to be the hard-X-ray-brightest such object observed with Suzaku and could well be the prototype Compton-thick Type 2 quasar. The Suzaku observation, especially above 10 keV will most likely reveal one of the most luminous Compton--thick Type 2 QSO to date. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | CHIANG | CHIA-YING | NULL | NULL | EUR | 6 | AO6 | THE TYPE 2 HYPERLUMINOUS QUASAR IRAS 09104+4109 | XIS | Y |
| MRK 478 | 220.4959 | 35.3708 | 59.0913373 | 65.0766343 | 294.6097 | 55756.9652777778 | 55758.8334837963 | 706041010 | 85323.6 | 80000 | 85331.6 | 85339.6 | 0 | 85323.6 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 77636.6 | 77636.6 | 161389.7 | 1 | PROCESSED | 57602.6370601852 | 56151 | 55783.7198842593 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 062028 | The NLS1 galaxy Mrk 478 has exceptionally unusual properties. It shows up to a factor of five variability while keeping its spectral shape constant. Previous short XMM-Newton observations show that it is probably reflection-dominated, where light-bending effects are at their extreme. This is the only known object that shows such high variability while remaining in a reflection-dominated state. All other known objects show reflection-dominated spectra only when in a faint state, making their study very difficult. This object is reflection-dominated yet bright enough to study with relatively short exposures.Here we propose to observe this object for 80 ks. The goal is to detect the reflection hump using Suzaku capabilities above 10 keV and probe light-bending around this black hole. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ZOGHBI | ABDERAHMEN | NULL | NULL | EUR | 6 | AO6 | PROBING EXTREME RELATIVISITC LIGHT-BENDING IN MRK 478 | HXD | Y |
| 3C120 | 68.2984 | 5.3496 | 190.37864439 | -27.39774516 | 260.9996 | 55966.4234143518 | 55970.8752083333 | 706042010 | 183001.5 | 300000 | 183025.5 | 183001.5 | 0 | 183025.5 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 158030.6 | 158030.6 | 384595.7 | 3 | PROCESSED | 57604.7163310185 | 55652 | 55992.4178819444 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066003 | We propose deep Suzaku observations of 6 well-known AGN with the primary aim of studying strong-gravitational physics close to these supermassive black holes (SMBH). We will conduct the first ever census of local SMBH spin, providing a new window on the growth-history of SMBHs. Suzaku's unique combination of high-throughput in the iron-K band and hard-band (>10keV) sensitivity is crucial, permitting a separation of the disk-reflection spectrum (which encodes the relativistic physics) from the effects of the warm absorber and low-velocity emission/reflection. These six datasets will be an important legacy of Suzaku, providing an important resource for AGN researchers for at least the next decade. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | REYNOLDS | CHRISTOPHER | NULL | NULL | USA | 6 | AO6-KP | A SURVEY OF BLACK HOLE SPIN AND RELATIVISTIC PHYSICS IN AGN | XIS | Y |
| 3C120 | 68.2996 | 5.3511 | 190.37800916 | -27.39591229 | 261.0003 | 55971.7483564815 | 55974.8819907407 | 706042020 | 118068.9 | 120000 | 118068.9 | 118068.9 | 0 | 118068.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 103536.5 | 103536.5 | 270735.9 | 2 | PROCESSED | 57604.7019791667 | 55652 | 55992.3150694444 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066003 | We propose deep Suzaku observations of 6 well-known AGN with the primary aim of studying strong-gravitational physics close to these supermassive black holes (SMBH). We will conduct the first ever census of local SMBH spin, providing a new window on the growth-history of SMBHs. Suzaku's unique combination of high-throughput in the iron-K band and hard-band (>10keV) sensitivity is crucial, permitting a separation of the disk-reflection spectrum (which encodes the relativistic physics) from the effects of the warm absorber and low-velocity emission/reflection. These six datasets will be an important legacy of Suzaku, providing an important resource for AGN researchers for at least the next decade. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | REYNOLDS | CHRISTOPHER | NULL | NULL | USA | 6 | AO6-KP | A SURVEY OF BLACK HOLE SPIN AND RELATIVISTIC PHYSICS IN AGN | XIS | Y |
| 0528+134 | 82.7323 | 13.541 | 191.35839601 | -11.00951452 | 89.1633 | 55832.6802314815 | 55833.0119444444 | 706043010 | 14789.2 | 10000 | 14789.2 | 14789.2 | 0 | 14789.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15865.9 | 15865.9 | 28635.9 | 0 | PROCESSED | 57603.2623032407 | 56225 | 55875.6223958333 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061601 | We propose to perform four 2-week campaigns over period Autumn 2011 - Spring 2013 of multiwaveband observations of a sample of gamma-ray blazars. The campaigns will involve: (1) gamma-ray light curves constructed using the Fermi LAT data, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B,V,R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku, Swift, and RXTE; (6) mid-IR (8-26 microns) bands measurements with IRTF. The research aims to study variability of flux, polarization, and spectral index at different wavelengths and at different states of gamma-ray and radio jet activity to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars. | EXTRAGALACTIC COMPACT SOURCES | 7 | S | JORSTAD | SVETLANA | NULL | NULL | USA | 6 | AO6 | EXPLORATION OF GAMMA-RAY BLAZARS ACROSS THE ELECTROMAGNETIC SPECTRUM | XIS | Y |
| 1622-297 | 246.5282 | -29.8629 | 348.81494865 | 13.309894 | 287.0011 | 55828.8879166667 | 55829.1800810185 | 706044010 | 8778.1 | 10000 | 8778.1 | 8778.1 | 0 | 8778.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 8751.3 | 8751.3 | 25198 | 0 | PROCESSED | 57603.2321064815 | 56236 | 55868.9351851852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061601 | We propose to perform four 2-week campaigns over period Autumn 2011 - Spring 2013 of multiwaveband observations of a sample of gamma-ray blazars. The campaigns will involve: (1) gamma-ray light curves constructed using the Fermi LAT data, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B,V,R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku, Swift, and RXTE; (6) mid-IR (8-26 microns) bands measurements with IRTF. The research aims to study variability of flux, polarization, and spectral index at different wavelengths and at different states of gamma-ray and radio jet activity to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars. | EXTRAGALACTIC COMPACT SOURCES | 7 | S | JORSTAD | SVETLANA | NULL | NULL | USA | 6 | AO6 | EXPLORATION OF GAMMA-RAY BLAZARS ACROSS THE ELECTROMAGNETIC SPECTRUM | XIS | Y |
| 4C38.41 | 248.824 | 38.1186 | 61.06470824 | 42.32788618 | 255.0463 | 55829.1891666667 | 55829.4148032407 | 706045010 | 8923.9 | 10000 | 8931.9 | 8931.9 | 0 | 8923.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9535.3 | 9535.3 | 19471.9 | 0 | PROCESSED | 57603.2349305556 | 56225 | 55875.6235185185 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061601 | We propose to perform four 2-week campaigns over period Autumn 2011 - Spring 2013 of multiwaveband observations of a sample of gamma-ray blazars. The campaigns will involve: (1) gamma-ray light curves constructed using the Fermi LAT data, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B,V,R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku, Swift, and RXTE; (6) mid-IR (8-26 microns) bands measurements with IRTF. The research aims to study variability of flux, polarization, and spectral index at different wavelengths and at different states of gamma-ray and radio jet activity to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars. | EXTRAGALACTIC COMPACT SOURCES | 7 | S | JORSTAD | SVETLANA | NULL | NULL | USA | 6 | AO6 | EXPLORATION OF GAMMA-RAY BLAZARS ACROSS THE ELECTROMAGNETIC SPECTRUM | XIS | Y |
| 1730-130 | 263.2641 | -13.0933 | 12.02258907 | 10.80244107 | 271.1606 | 55829.6599537037 | 55830.0946643518 | 706046010 | 11085.8 | 10000 | 11093.8 | 11093.8 | 0 | 11085.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9881.1 | 9881.1 | 37535.9 | 1 | PROCESSED | 57603.2457407407 | 56225 | 55875.6203703704 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061601 | We propose to perform four 2-week campaigns over period Autumn 2011 - Spring 2013 of multiwaveband observations of a sample of gamma-ray blazars. The campaigns will involve: (1) gamma-ray light curves constructed using the Fermi LAT data, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B,V,R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku, Swift, and RXTE; (6) mid-IR (8-26 microns) bands measurements with IRTF. The research aims to study variability of flux, polarization, and spectral index at different wavelengths and at different states of gamma-ray and radio jet activity to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars. | EXTRAGALACTIC COMPACT SOURCES | 7 | S | JORSTAD | SVETLANA | NULL | NULL | USA | 6 | AO6 | EXPLORATION OF GAMMA-RAY BLAZARS ACROSS THE ELECTROMAGNETIC SPECTRUM | XIS | Y |
| OT+081 | 267.8906 | 9.6366 | 34.9082961 | 17.63584745 | 268.2827 | 55830.0996759259 | 55830.3911921296 | 706047010 | 10774 | 10000 | 10774 | 10774 | 0 | 10774 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11036 | 11036 | 25151.9 | 1 | PROCESSED | 57603.2492708333 | 56225 | 55875.6247569444 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061601 | We propose to perform four 2-week campaigns over period Autumn 2011 - Spring 2013 of multiwaveband observations of a sample of gamma-ray blazars. The campaigns will involve: (1) gamma-ray light curves constructed using the Fermi LAT data, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B,V,R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku, Swift, and RXTE; (6) mid-IR (8-26 microns) bands measurements with IRTF. The research aims to study variability of flux, polarization, and spectral index at different wavelengths and at different states of gamma-ray and radio jet activity to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars. | EXTRAGALACTIC COMPACT SOURCES | 7 | S | JORSTAD | SVETLANA | NULL | NULL | USA | 6 | AO6 | EXPLORATION OF GAMMA-RAY BLAZARS ACROSS THE ELECTROMAGNETIC SPECTRUM | XIS | Y |
| NGC 4941 | 196.0528 | -5.5595 | 308.80102111 | 57.16661738 | 292.811 | 56100.4695833333 | 56102.2446643518 | 707001010 | 80859.3 | 80000 | 80859.3 | 80859.3 | 0 | 80859.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 76748.6 | 76748.6 | 153320 | 1 | PROCESSED | 57605.7725115741 | 56480 | 56113.2872800926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070003 | The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to population synthesis models, its estimate is strongly coupled with the broad band spectral shape of Compton thin AGNs. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright AGNs that can be best followed-up with Suzaku. Previously, such studies have been limited to AGNs with intermediate to high luminosities. Here we propose to observe two of the lowest luminosity AGNs in the latest BAT catalog to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 7 | AO7 | BROAD BAND SPECTRA OF HARD X-RAY SELECTED LOW LUMINOSITY AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND | XIS | Y |
| NGC 1566 | 65.0038 | -54.9403 | 264.31301386 | -43.39149342 | 351.3031 | 56066.0671759259 | 56067.2738310185 | 707002010 | 72791 | 80000 | 72791 | 72791 | 0 | 72791 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 71958.1 | 71958.1 | 104223.9 | 2 | PROCESSED | 57605.4671875 | 56442 | 56076.0434606482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070003 | The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to population synthesis models, its estimate is strongly coupled with the broad band spectral shape of Compton thin AGNs. Recently, Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright AGNs that can be best followed-up with Suzaku. Previously, such studies have been limited to AGNs with intermediate to high luminosities. Here we propose to observe two of the lowest luminosity AGNs in the latest BAT catalog to measure the amount of reflection component with unpreceded accuracy, a key parameter to determine the total contribution of Compton thick AGNs to the X-ray background. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 7 | AO7 | BROAD BAND SPECTRA OF HARD X-RAY SELECTED LOW LUMINOSITY AGNS AND THE ORIGIN OF THE X-RAY BACKGROUND | XIS | Y |
| NGC 7603 | 349.73 | 0.2557 | 80.07171077 | -54.72674929 | 67.5296 | 56080.5080208333 | 56082.6598726852 | 707003010 | 101256.7 | 100000 | 101260.2 | 101265.7 | 0 | 101256.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 96002.3 | 96002.3 | 185903.7 | 2 | PROCESSED | 57605.6196875 | 56464 | 56096.2688541667 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070010 | X-ray spectra from Seyfert galaxies often consist of various emission components such as from an accretion disk and dusty torus. Because of this complexity, interpretation of reprocessed feature (Fe lines and reflection continuum) in X-ray spectra is often ambiguous. We selected a Seyfert 1 with very weak mid infrared emission from the putative torus relative to X-rays from an accretin disk bu using AKARI IR and XMM X-ray catalogs. We will measure a ``pure'' accretion disk spectrum without contamination of reprocessed emission from the torus, and castrain extent of an accretion disk, which is expected to depend on an Eddington ratio, from the reprocessed X-ray emission. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | TERASHIMA | YUICHI | NULL | NULL | JAP | 7 | AO7 | PURE ACCRETION DISK SPECTRUM OF THE SEYFERT 1 NGC 7603 | XIS | Y |
| 3C 227 | 146.9365 | 7.4245 | 228.57888407 | 42.2858038 | 108.3139 | 56237.0794675926 | 56239.0279513889 | 707004010 | 82532.5 | 80000 | 82540.5 | 82532.5 | 0 | 82540.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 71429.9 | 71429.9 | 168333.8 | 0 | PROCESSED | 57608.0036342593 | 56631 | 56264.6488773148 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070012 | Radio galaxies are a key class to understand the origin and effects of AGN feedback to the surroundings. However, the fundamental question, how the structure of the nucleus is different between AGNs with and without jets, is not resolved yet. A key parameter to understand the accretion flow is the Eddington ratio. BLRGs of 4C 50.55 and 3C 120 are rare objects having high Eddington ratio (L_bol/L_Edd~0.4) compared with Seyferts and typical BLRGs (< 0.1). Though the accretion disks in many BLRGs are known to be truncated and/or inner parts covered by corona, unified picture of accretion flows over a wide range of accretion rate is far from established. Therefore we propose observing a BLRG of 3C 227, which has the highest Eddington ratio in the hard X-ray luminous BLRGs. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | TAZAKI | FUMIE | NULL | NULL | JAP | 7 | AO7 | STUDY OF NUCLEAR STRUCTURE OF BLRGS WITH HIGH ACCRETION RATE | XIS | Y |
| 3C 236 WEST LOBE | 151.329 | 34.9949 | 189.91194492 | 53.83302535 | 299.9981 | 56053.9465740741 | 56055.7862384259 | 707005010 | 83993.5 | 80000 | 83993.5 | 83993.5 | 0 | 83993.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 80424.8 | 80424.8 | 158931.8 | 2 | PROCESSED | 57605.4100925926 | 56436 | 56070.2690856482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070014 | Through the Suzaku observations of giant radio galaxies, of which the size is larger than about 1 Mpc, we are going to reveal a picture that the jets in radio galaxies become inactive as they evolve from 500 kpc to 1 Mpc. However, the current Suzaku sample of the giant radio galaxies is far from being satisfactory to make a definite conclusion. Therefore, we propose a Suzaku observation of 3C 236, one of the most giant radio galaxy in the Universe. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ISOBE | NAOKI | NULL | NULL | JAP | 7 | AO7 | INVESTIGATION INTO EVOLUTION OF THE JET ENERGETICS, THROUGH THE SUZAKU OBSERVATION OF THE GIANT RADIO GALAXY 3C 236 | XIS | Y |
| 3C 236 BACKGROUND | 151.1488 | 34.7362 | 190.35215815 | 53.68789407 | 299.9977 | 56055.786712963 | 56056.7919444444 | 707006010 | 46211.3 | 40000 | 46211.3 | 46211.3 | 0 | 46211.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44109.5 | 44109.5 | 86839.9 | 0 | PROCESSED | 57605.3836574074 | 56436 | 56070.1639930556 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070014 | Through the Suzaku observations of giant radio galaxies, of which the size is larger than about 1 Mpc, we are going to reveal a picture that the jets in radio galaxies become inactive as they evolve from 500 kpc to 1 Mpc. However, the current Suzaku sample of the giant radio galaxies is far from being satisfactory to make a definite conclusion. Therefore, we propose a Suzaku observation of 3C 236, one of the most giant radio galaxy in the Universe. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ISOBE | NAOKI | NULL | NULL | JAP | 7 | AO7 | INVESTIGATION INTO EVOLUTION OF THE JET ENERGETICS, THROUGH THE SUZAKU OBSERVATION OF THE GIANT RADIO GALAXY 3C 236 | XIS | Y |
| 2FGL J0923.5+1508 | 140.9887 | 15.0811 | 215.96780071 | 40.48329137 | 287.9737 | 56046.2642939815 | 56048.4933449074 | 707007010 | 95255.4 | 90000 | 95279.4 | 95255.4 | 0 | 95279.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 89587.8 | 89587.8 | 192568 | 1 | PROCESSED | 57605.3423611111 | 56434 | 56068.6261921296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070024 | We propose X-ray follow up observations of two high redshift blazar candidates in the Fermi/LAT unidentified sources. The aim of this proposal is to detect X-ray emissions from high redshift blazars (z >> 3) buried in unidentified Fermi/LAT sources and to find the most distant LAT detected blazar. Gamma-ray photons above 10 GeV are attenuated by interactions with UV photons which result in creating electron-positron pairs. Therefore, attenuation signatures are predicted to be observed in gamma-ray spectra and such attenuation of high redshift blazars with redshift up to z ~ 6 provide information about UV background out to the epoch of cosmological reionization. By utilizing the attenuation, we can investigate the UV radiation state of the early universe. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | TAKAHASHI | YOSUKE | NULL | NULL | JAP | 7 | AO7 | SUZAKU OBSERVATIONS OF HIGH REDSHIFT BLAZAR CANDIDATES IN THE FERMI UNIDENTIFIED SOURCE SAMPLE | XIS | Y |
| 2FGL J1502.1+5548 | 225.5826 | 55.8575 | 92.73148616 | 52.90392629 | 345.2903 | 56069.912974537 | 56070.8342824074 | 707008010 | 62873.3 | 60000 | 62881.3 | 62881.3 | 0 | 62873.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 56167 | 56167 | 79589.9 | 1 | PROCESSED | 57605.4999652778 | 56449 | 56083.096875 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070024 | We propose X-ray follow up observations of two high redshift blazar candidates in the Fermi/LAT unidentified sources. The aim of this proposal is to detect X-ray emissions from high redshift blazars (z >> 3) buried in unidentified Fermi/LAT sources and to find the most distant LAT detected blazar. Gamma-ray photons above 10 GeV are attenuated by interactions with UV photons which result in creating electron-positron pairs. Therefore, attenuation signatures are predicted to be observed in gamma-ray spectra and such attenuation of high redshift blazars with redshift up to z ~ 6 provide information about UV background out to the epoch of cosmological reionization. By utilizing the attenuation, we can investigate the UV radiation state of the early universe. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | TAKAHASHI | YOSUKE | NULL | NULL | JAP | 7 | AO7 | SUZAKU OBSERVATIONS OF HIGH REDSHIFT BLAZAR CANDIDATES IN THE FERMI UNIDENTIFIED SOURCE SAMPLE | XIS | Y |
| 2FGL J0022.2-1853 | 5.5431 | -18.8956 | 82.15155077 | -79.37005347 | 62.0041 | 56077.5533564815 | 56078.2856944445 | 707009010 | 34867.8 | 30000 | 34867.8 | 34867.8 | 0 | 34867.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35196.4 | 35196.4 | 63263.9 | 1 | PROCESSED | 57605.5769444444 | 56456 | 56090.1516435185 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070034 | We propose Suzaku observations of "unusual" Fermi-LAT sources 2FGL J0022.2, J0037.8 and J0157.2, which are yet unidentified in gamma-ray, but their counterparts have already been detected with snapshot (typically 5ksec) Swift XRT observations. Their positions are determined with an excellent accuracy of several arcseconds. Since all three sources are detected both in radio and X-rays, they could be most likely AGN jet sources but their spectral energy distributions are far from what expected from typical blazars, suggesting "new-type" AGN sources. We propose 30 ksec observations of each to investigate temporal variability, as well as to determine wideband XIS/HXD spectra between 0.5-30 keV (J01572.2 is detectable with HXD/PIN). | EXTRAGALACTIC COMPACT SOURCES | 7 | B | KATAOKA | JUN | NULL | NULL | JAP | 7 | AO7 | FURTHER CHALLENGES TO UNUSUAL FERMI-UNIDS WITH SUZAKU X-RAY OBSERVATORY | XIS | Y |
| 2FGL J0037.8+1238 | 9.4591 | 12.6426 | 117.75617703 | -50.09241086 | 67.2998 | 56108.005787037 | 56108.9432523148 | 707010010 | 28603.9 | 30000 | 28603.9 | 28603.9 | 0 | 28603.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30097.7 | 30097.7 | 80972 | 1 | PROCESSED | 57606.5224768518 | 56493 | 56127.1415625 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070034 | We propose Suzaku observations of "unusual" Fermi-LAT sources 2FGL J0022.2, J0037.8 and J0157.2, which are yet unidentified in gamma-ray, but their counterparts have already been detected with snapshot (typically 5ksec) Swift XRT observations. Their positions are determined with an excellent accuracy of several arcseconds. Since all three sources are detected both in radio and X-rays, they could be most likely AGN jet sources but their spectral energy distributions are far from what expected from typical blazars, suggesting "new-type" AGN sources. We propose 30 ksec observations of each to investigate temporal variability, as well as to determine wideband XIS/HXD spectra between 0.5-30 keV (J01572.2 is detectable with HXD/PIN). | EXTRAGALACTIC COMPACT SOURCES | 7 | B | KATAOKA | JUN | NULL | NULL | JAP | 7 | AO7 | FURTHER CHALLENGES TO UNUSUAL FERMI-UNIDS WITH SUZAKU X-RAY OBSERVATORY | XIS | Y |
| 2FGL J0157.2-5259 | 29.3567 | -53.0295 | 282.0695167 | -61.34394411 | 33.9769 | 56075.6946064815 | 56076.2565162037 | 707011010 | 32075.3 | 30000 | 32075.3 | 32075.3 | 0 | 32075.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 31778.4 | 31778.4 | 48523.9 | 1 | PROCESSED | 57605.5386458333 | 56527 | 56161.0508449074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070034 | We propose Suzaku observations of "unusual" Fermi-LAT sources 2FGL J0022.2, J0037.8 and J0157.2, which are yet unidentified in gamma-ray, but their counterparts have already been detected with snapshot (typically 5ksec) Swift XRT observations. Their positions are determined with an excellent accuracy of several arcseconds. Since all three sources are detected both in radio and X-rays, they could be most likely AGN jet sources but their spectral energy distributions are far from what expected from typical blazars, suggesting "new-type" AGN sources. We propose 30 ksec observations of each to investigate temporal variability, as well as to determine wideband XIS/HXD spectra between 0.5-30 keV (J01572.2 is detectable with HXD/PIN). | EXTRAGALACTIC COMPACT SOURCES | 7 | B | KATAOKA | JUN | NULL | NULL | JAP | 7 | AO7 | FURTHER CHALLENGES TO UNUSUAL FERMI-UNIDS WITH SUZAKU X-RAY OBSERVATORY | XIS | Y |
| NGC 3431 | 162.8114 | -17.015 | 266.03803779 | 37.10135134 | 298.5009 | 56089.5660648148 | 56091.5571412037 | 707012010 | 65675.6 | 70000 | 65675.6 | 65675.6 | 0 | 65675.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 59881.9 | 59881.9 | 171995.9 | 2 | PROCESSED | 57605.6909259259 | 56473 | 56106.3662384259 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070067 | The nature of the hard X-ray emission of many AGN remains ill-understood. Using the latest 70 month Swift/BAT sky survey, we have selected optically-classified Seyfert 2s with a very hard BAT photon index (Gamma<1.4). The BAT energy range is not strongly affected by obscuration unless the column is Compton-thick. The selected sources are radio-quiet, arguing against jet-dominated non-thermal spectra. The cause of a low Gamma is unknown, but may include high or atypical obscuration, non-thermal X-ray emission without associated radio/optical jets or the presence of electron coronae with temperatures or optical depths higher than average. Our aim is to observe two of the hardest Seyfert 2s (neither of which has prior pointed observations below 10 keV) with Suzaku to elucidate their nature. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GANDHI | POSHAK | NULL | NULL | JAP | 7 | AO7 | WHAT IS THE NATURE OF SWIFT/BAT HARD-SPECTRUM SEYFERT 2S? | XIS | Y |
| ESO 565-G019 | 143.6802 | -21.9346 | 253.87283017 | 21.67453181 | 298.0016 | 56067.8709259259 | 56069.9022222222 | 707013010 | 78923.9 | 80000 | 78923.9 | 78931.9 | 0 | 78931.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 71121.1 | 71121.1 | 175487.8 | 2 | PROCESSED | 57605.5328935185 | 56448 | 56079.3396643518 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070067 | The nature of the hard X-ray emission of many AGN remains ill-understood. Using the latest 70 month Swift/BAT sky survey, we have selected optically-classified Seyfert 2s with a very hard BAT photon index (Gamma<1.4). The BAT energy range is not strongly affected by obscuration unless the column is Compton-thick. The selected sources are radio-quiet, arguing against jet-dominated non-thermal spectra. The cause of a low Gamma is unknown, but may include high or atypical obscuration, non-thermal X-ray emission without associated radio/optical jets or the presence of electron coronae with temperatures or optical depths higher than average. Our aim is to observe two of the hardest Seyfert 2s (neither of which has prior pointed observations below 10 keV) with Suzaku to elucidate their nature. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GANDHI | POSHAK | NULL | NULL | JAP | 7 | AO7 | WHAT IS THE NATURE OF SWIFT/BAT HARD-SPECTRUM SEYFERT 2S? | XIS | Y |
| RXJ0134-4258 | 23.5686 | -42.9671 | 276.92816891 | -71.93227434 | 245.0998 | 56290.2726851852 | 56292.2506481482 | 707014010 | 81429 | 50000 | 81448.5 | 81445 | 0 | 81429 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16121.9 | 16121.9 | 37685.9 | 0 | PROCESSED | 57608.396087963 | 56702 | 56336.5473263889 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070081 | RXJ0134.2-4258 was detected in the ROSAT all sky observation (RASS), later identified as a radio loud (RL) narrow line Seyfert 1 galaxy. During the RASS, the soft X-ray spectrum of this source was steep. Following observations with ROSAT, ASCA, Swift, and XMM-Newton (XMM) showed flatter spectra. The XMM spectra are fitted with a power law with an cut-off (EC) at 4 keV, where a blackbody (BB) component was not evident. Either type of spectrum is not common for Seyferts. We consider this peculiarity is related to the RL nature of this object, originated in the jet. We will observe this source with Suzaku, which has higher energy resolution than XMM, to reveal the long term variability of this source. Particular interests go to the EC energy, bb component, and the iron K emission line. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | TAKAHASHI | HIROAKI | NULL | NULL | JAP | 7 | AO7 | X-RAY EMISSION FROM THE BRIGHTEST RADIO LOUD NARROW LINE SEYFERT 1 RXJ0134.2-4258 | XIS | Y |
| 1H0323+342 | 51.1746 | 34.1741 | 155.73224486 | -18.75935356 | 251.4848 | 56352.6173611111 | 56354.8078819444 | 707015010 | 101272 | 100000 | 101288 | 101272 | 0 | 101288 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 97128.3 | 97128.3 | 189251.6 | 0 | PROCESSED | 57610.7547916667 | 56739 | 56372.5724189815 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070088 | We propose to observe a narrow-line radio-loud gamma-ray emitting Seyfert 1 galaxy 1H0323+342, which is the X-ray brightest among a new class of GeV gamma-ray emitting AGNs, first detected by Fermi/LAT. Based on accurate and high-sensitive measurement of X-ray spectra with Suzaku, we study the presence of Fe-K lines and energy-dependence of time variability, in order to constrain the origin of X-ray emission of this object. This leads to understanding the SED of this object and constraining the jet power. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | FUKAZAWA | YASUSHI | NULL | NULL | JAP | 7 | AO7 | STUDY OF X-RAY SPECTRAL VARIABILITY OF A NARROW-LINE RADIO-LOUD GAMAM-RAY EMITTING SEYFERT 1 GALAXY 1H0323+342 | XIS | Y |
| E1821+643 | 275.5207 | 64.3306 | 93.98984501 | 27.40177083 | 228.4067 | 56239.7868981482 | 56241.8217708333 | 707016010 | 100413.2 | 100000 | 100413.2 | 100413.2 | 0 | 100413.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 95541.1 | 95541.1 | 175779.9 | 2 | PROCESSED | 57608.0299421296 | 56631 | 56265.6966319444 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070089 | Central engines of AGN are considered to be generally in Multi-Zone Comptonization (MZC) condition (e.g., Noda et al. 2011a,b). To verify this thing on a high-luminosiy AGN, we suggest to observe Radio-Quiet Quasar E1821+643 By Suzaku. Utilizing a time variability of each Comptonization component, we will resolve spectral variable components, and study whether the central engine of E1821+643 is in MZC condition or not. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | NODA | HIROUMI | NULL | NULL | JAP | 7 | AO7 | SUZAKU STUDY OF MULTI-ZONE COMPTONIZATION PICTURE ON THE CENTRAL ENGINE OF RADIO-QUIET QUASAR E1821+643 | XIS | Y |
| NGC1365 | 53.4052 | -36.1452 | 237.96410536 | -54.59489483 | 47.2005 | 56107.1526041667 | 56107.9972916667 | 707017010 | 30694.9 | 30000 | 30694.9 | 30694.9 | 0 | 30694.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27832.1 | 27832.1 | 72973.8 | 0 | PROCESSED | 57606.5279050926 | 56491 | 56125.2372453704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070095 | NGC1365 is one of AGNs which shows the most highly variable spectral change, and furthermore exhibits strong Fe-K absorption lines blue-shifted by 1000--5000 km/s with EW of about 100eV. These absorption lines indicate a massive outflow and are important to consider the AGN feedback to parent galaxies. Currently, there is no other object by which we can measure the Fe-K absorption lines accurately than NGC 1365. Therefore, we propose to monitor a velocity, depth, and ratio of blue-shifted Fe-K absorption lines, hard X-ray flux above 10 keV of NGC1365 every 10 days, in order to probe the massive outflow dynamically and compare the results with the numerical simulation. } | EXTRAGALACTIC COMPACT SOURCES | 7 | B | FUKAZAWA | YASUSHI | NULL | NULL | JAP | 7 | AO7 | MONITOR OF VELOCITY AND STRENGTH OF BLUE-SHIFTED STRONG FE-K ABSORPTION LINES OF NGC 1365 | XIS | Y |
| NGC1365 | 53.4048 | -36.1458 | 237.96516908 | -54.5951856 | 59.0002 | 56116.8446064815 | 56117.6910763889 | 707017020 | 33585.8 | 30000 | 33593.8 | 33601.8 | 0 | 33585.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32579 | 32579 | 73105.9 | 2 | PROCESSED | 57606.5919791667 | 56508 | 56142.1709606482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070095 | NGC1365 is one of AGNs which shows the most highly variable spectral change, and furthermore exhibits strong Fe-K absorption lines blue-shifted by 1000--5000 km/s with EW of about 100eV. These absorption lines indicate a massive outflow and are important to consider the AGN feedback to parent galaxies. Currently, there is no other object by which we can measure the Fe-K absorption lines accurately than NGC 1365. Therefore, we propose to monitor a velocity, depth, and ratio of blue-shifted Fe-K absorption lines, hard X-ray flux above 10 keV of NGC1365 every 10 days, in order to probe the massive outflow dynamically and compare the results with the numerical simulation. } | EXTRAGALACTIC COMPACT SOURCES | 7 | B | FUKAZAWA | YASUSHI | NULL | NULL | JAP | 7 | AO7 | MONITOR OF VELOCITY AND STRENGTH OF BLUE-SHIFTED STRONG FE-K ABSORPTION LINES OF NGC 1365 | XIS | Y |
| NGC1365 | 53.4072 | -36.1471 | 237.96723255 | -54.59318142 | 57.2979 | 56125.3876273148 | 56125.896087963 | 707017030 | 26767.2 | 30000 | 26767.2 | 26767.2 | 0 | 26767.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25211.2 | 25211.2 | 43923.9 | 1 | PROCESSED | 57606.6299537037 | 56582 | 56212.7663194444 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070095 | NGC1365 is one of AGNs which shows the most highly variable spectral change, and furthermore exhibits strong Fe-K absorption lines blue-shifted by 1000--5000 km/s with EW of about 100eV. These absorption lines indicate a massive outflow and are important to consider the AGN feedback to parent galaxies. Currently, there is no other object by which we can measure the Fe-K absorption lines accurately than NGC 1365. Therefore, we propose to monitor a velocity, depth, and ratio of blue-shifted Fe-K absorption lines, hard X-ray flux above 10 keV of NGC1365 every 10 days, in order to probe the massive outflow dynamically and compare the results with the numerical simulation. } | EXTRAGALACTIC COMPACT SOURCES | 7 | B | FUKAZAWA | YASUSHI | NULL | NULL | JAP | 7 | AO7 | MONITOR OF VELOCITY AND STRENGTH OF BLUE-SHIFTED STRONG FE-K ABSORPTION LINES OF NGC 1365 | XIS | Y |
| NGC1365 | 53.4038 | -36.1454 | 237.96455345 | -54.59601318 | 66.4692 | 56137.3445138889 | 56138.1030208333 | 707017040 | 31360.3 | 30000 | 31368.3 | 31368.3 | 0 | 31360.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 28231.4 | 28231.4 | 65527.9 | 2 | PROCESSED | 57606.7020717593 | 56528 | 56162.0367361111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070095 | NGC1365 is one of AGNs which shows the most highly variable spectral change, and furthermore exhibits strong Fe-K absorption lines blue-shifted by 1000--5000 km/s with EW of about 100eV. These absorption lines indicate a massive outflow and are important to consider the AGN feedback to parent galaxies. Currently, there is no other object by which we can measure the Fe-K absorption lines accurately than NGC 1365. Therefore, we propose to monitor a velocity, depth, and ratio of blue-shifted Fe-K absorption lines, hard X-ray flux above 10 keV of NGC1365 every 10 days, in order to probe the massive outflow dynamically and compare the results with the numerical simulation. } | EXTRAGALACTIC COMPACT SOURCES | 7 | B | FUKAZAWA | YASUSHI | NULL | NULL | JAP | 7 | AO7 | MONITOR OF VELOCITY AND STRENGTH OF BLUE-SHIFTED STRONG FE-K ABSORPTION LINES OF NGC 1365 | XIS | Y |
| SWIFT J164449.3+1573 | 251.1623 | 57.5874 | 86.72267547 | 39.46447046 | 15.8437 | 56064.7296064815 | 56066.0522106482 | 707018010 | 80814.1 | 80000 | 80822.1 | 80814.1 | 0 | 80822.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 74337.9 | 74337.9 | 114269.9 | 0 | PROCESSED | 57605.4610648148 | 56442 | 56076.0214351852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070096 | We propose a 80 ks observation of a tidal disruption event Swift J164449.3+1573451 one year after its onset. In this event, a star was presumably disrupted by a strong tidal force of a massive black hole at the center of a galaxy at z=0.35, releasing a relativistic jet that emitted intense X-rays. In this proposal, we attempt to detect the non-thermal emission from the relativistic jet and the fluorescent Fe K line from its surrounding material. With these results we study the driving mechanism of the jet and to test the tidal disruption model. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | USUI | RYUICHI | NULL | NULL | JAP | 7 | AO7 | ONE YEAR AFTER THE TIDAL DISRUPTION OF SWIFT J164449.3+1573451 | XIS | Y |
| HOLMBERG IX X-1 | 149.4435 | 69.0486 | 141.95726659 | 41.07139178 | 311.5635 | 56030.7575810185 | 56034.6807175926 | 707019010 | 182527.4 | 500000 | 182527.4 | 182527.4 | 0 | 182527.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 208623.6 | 208623.6 | 338933.9 | 3 | PROCESSED | 57605.2861342593 | 56018 | 56044.4614699074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071251 | Recent X-ray observations have found evidence that a subset of the most extreme ultra-luminous X-ray sources (ULXs) are either intermediate-mass black holes or stellar-mass binaries in a super-Eddington state. Current data are unable to deliver a clear answer, but the diagnostics possible in a long observation will be decisive. We request a 500 ks observation of the ULX Holmberg IX X-1 to place crucial constraints on atomic features that would signal a super-Eddington flow. Detecting or ruling out atomic features naturally requires a deep exposure. The strong spectral constraints derived will reveal the nature of the accreting black holes in these systems. A definitive statement on the existence of 100-1000 Msun black holes or extreme accretion states will be an important Suzaku legacy. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MILLER | JON | NULL | NULL | USA | 7 | AO7 | A DECISIVE LEGACY OBSERVATION OF AN ULTRALUMINOUS X-RAY SOURCE | XIS | Y |
| HOLMBERG IX X-1 | 149.4877 | 69.0751 | 141.9165022 | 41.0686989 | 124.501 | 56221.770162037 | 56224.1252083333 | 707019020 | 107495.8 | 320000 | 107495.8 | 107495.8 | 0 | 107495.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 106867.3 | 106867.3 | 203447.9 | 1 | PROCESSED | 57607.8555324074 | 56018 | 56330.5864930556 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071251 | Recent X-ray observations have found evidence that a subset of the most extreme ultra-luminous X-ray sources (ULXs) are either intermediate-mass black holes or stellar-mass binaries in a super-Eddington state. Current data are unable to deliver a clear answer, but the diagnostics possible in a long observation will be decisive. We request a 500 ks observation of the ULX Holmberg IX X-1 to place crucial constraints on atomic features that would signal a super-Eddington flow. Detecting or ruling out atomic features naturally requires a deep exposure. The strong spectral constraints derived will reveal the nature of the accreting black holes in these systems. A definitive statement on the existence of 100-1000 Msun black holes or extreme accretion states will be an important Suzaku legacy. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MILLER | JON | NULL | NULL | USA | 7 | AO7 | A DECISIVE LEGACY OBSERVATION OF AN ULTRALUMINOUS X-RAY SOURCE | XIS | Y |
| HOLMBERG IX X-1 | 149.4869 | 69.0752 | 141.91661656 | 41.06840873 | 124.5 | 56224.1252199074 | 56226.4168981482 | 707019030 | 106945.4 | 500000 | 106945.4 | 106953.4 | 0 | 106961.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 105011.9 | 105011.9 | 197947.8 | 1 | PROCESSED | 57607.8725462963 | 56018 | 56240.5429050926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071251 | Recent X-ray observations have found evidence that a subset of the most extreme ultra-luminous X-ray sources (ULXs) are either intermediate-mass black holes or stellar-mass binaries in a super-Eddington state. Current data are unable to deliver a clear answer, but the diagnostics possible in a long observation will be decisive. We request a 500 ks observation of the ULX Holmberg IX X-1 to place crucial constraints on atomic features that would signal a super-Eddington flow. Detecting or ruling out atomic features naturally requires a deep exposure. The strong spectral constraints derived will reveal the nature of the accreting black holes in these systems. A definitive statement on the existence of 100-1000 Msun black holes or extreme accretion states will be an important Suzaku legacy. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MILLER | JON | NULL | NULL | USA | 7 | AO7 | A DECISIVE LEGACY OBSERVATION OF AN ULTRALUMINOUS X-RAY SOURCE | XIS | Y |
| HOLMBERG IX X-1 | 149.4867 | 69.0744 | 141.91753226 | 41.06881922 | 124.4999 | 56226.4169097222 | 56228.7717708333 | 707019040 | 110017.5 | 500000 | 110038.3 | 110017.5 | 0 | 110017.5 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 105796.1 | 105796.1 | 203426 | 2 | PROCESSED | 57607.8756018518 | 56018 | 56240.5502430556 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071251 | Recent X-ray observations have found evidence that a subset of the most extreme ultra-luminous X-ray sources (ULXs) are either intermediate-mass black holes or stellar-mass binaries in a super-Eddington state. Current data are unable to deliver a clear answer, but the diagnostics possible in a long observation will be decisive. We request a 500 ks observation of the ULX Holmberg IX X-1 to place crucial constraints on atomic features that would signal a super-Eddington flow. Detecting or ruling out atomic features naturally requires a deep exposure. The strong spectral constraints derived will reveal the nature of the accreting black holes in these systems. A definitive statement on the existence of 100-1000 Msun black holes or extreme accretion states will be an important Suzaku legacy. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MILLER | JON | NULL | NULL | USA | 7 | AO7 | A DECISIVE LEGACY OBSERVATION OF AN ULTRALUMINOUS X-RAY SOURCE | XIS | Y |
| SNR 1987A | 83.833 | -69.2775 | 279.71430694 | -31.94790633 | 135.9732 | 56233.5143981482 | 56234.854375 | 707020010 | 81276.4 | 80000 | 81276.4 | 81284.4 | 0 | 81292.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 78584.2 | 78584.2 | 115759.9 | 0 | PROCESSED | 57607.9555439815 | 56611 | 56245.4956365741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071331 | Despite extensive observations of supernova remnant (SNR) 1987A with Chandra and XMM-Newton, the origin of the hard band (3-10 keV) X-ray emission is elusive (thermal vs nonthermal). A straightforward way to discriminate the thermal and nonthermal origins of the hard X-rays is to detect Fe K lines. The Suzaku XIS provides a uniquely efficient opportunity for a sensitive search for the Fe K lines, which is an excellent complement to the existing Chandra and XMM-Newton studies of SNR 1987A. Thus, we propose an 80 ks Suzaku observation of SNR 1987A. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | PARK | SANGWOOK | NULL | NULL | USA | 7 | AO7 | X-RAY EMISSION FROM SUPERNOVA REMNANT 1987A | XIS | Y |
| AO 0235+164 | 39.665 | 16.613 | 156.77598662 | -39.11106084 | 252.4352 | 56310.722337963 | 56311.7418634259 | 707021010 | 43102.8 | 40000 | 43110.8 | 43118.8 | 0 | 43102.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38358.3 | 38358.3 | 88069.8 | 0 | PROCESSED | 57608.5604166667 | 56709 | 56342.5387731482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071402 | We request observations of the variable blazar AO 0235+164, to be conducted simultaneously with Fermi and optical and radio telescopes, towards a multi-band campaign. This object has complex X-ray spectrum due to absorption by an intervening galaxy, and Suzaku will be essential in unraveling the effects and composition of that absorber, and for the first time, provide a robust measurement of the underlying blazar X-ray continuum, which, together with the Swift UVOT spectrum, will allow to verify the signature of the bulk-Compton component, due to cold electrons propagating in the relativistic jet. At the highest priority, we request 40 ks for a precise spectral measurement; at a lower priority, we wish to monitor the source for the total of 5 days, with the request of additional 160 ks. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | MADEJSKI | GRZEGORZ | NULL | NULL | USA | 7 | AO7 | SUZAKU OBSERVATIONS OF THE GAMMA-RAY BLAZAR AO 0235+164 | XIS | Y |
| ESO 511-G030 | 214.8452 | -26.6475 | 326.22882256 | 32.21510552 | 286.6511 | 56128.5082523148 | 56128.7501388889 | 707023010 | 5746.1 | 270000 | 5746.1 | 5754.1 | 0 | 5762.1 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 3988.6 | 3988.6 | 20887.9 | 0 | PROCESSED | 57606.6388194444 | 56646 | 56214.9581944445 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071413 | The study of "bare" Seyfert 1 AGN is essential to measure the true properties of the inner regions of the accretion disk. The nearby Seyfert ESO 511-G30 is a prime candidate for fulfilling this role due to its broad Fe K component and lack of any intrinsic warm absorption. It is also one of the X-ray brightest bare Seyferts featured in the Swift 58 month BAT catalogue as yet unobserved with Suzaku. We propose a 270 ks Suzaku observation of ESO 511-G30 to unambiguously constrain the properties of the accretion disk and subsequently the black hole spin. In addition, the HXD data will allow us to measure the Compton reflection hump, while the excellent soft X-ray spectral resolution of XIS will allow the origin of the soft excess to be determined. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | REEVES | JAMES | NULL | NULL | USA | 7 | AO7 | MEASURING THE ACCRETION DISK AND BLACK HOLE PROPERTIES OF ESO 511-G30 | XIS | Y |
| ESO 511-G030 | 214.8452 | -26.646 | 326.22952078 | 32.2164843 | 286.9689 | 56130.0282407407 | 56136.3340856482 | 707023020 | 224025.5 | 270000 | 224025.5 | 224025.5 | 0 | 224033.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 195633.4 | 195633.4 | 410895.8 | 3 | PROCESSED | 57606.8434606482 | 56646 | 56279.0046064815 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071413 | The study of "bare" Seyfert 1 AGN is essential to measure the true properties of the inner regions of the accretion disk. The nearby Seyfert ESO 511-G30 is a prime candidate for fulfilling this role due to its broad Fe K component and lack of any intrinsic warm absorption. It is also one of the X-ray brightest bare Seyferts featured in the Swift 58 month BAT catalogue as yet unobserved with Suzaku. We propose a 270 ks Suzaku observation of ESO 511-G30 to unambiguously constrain the properties of the accretion disk and subsequently the black hole spin. In addition, the HXD data will allow us to measure the Compton reflection hump, while the excellent soft X-ray spectral resolution of XIS will allow the origin of the soft excess to be determined. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | REEVES | JAMES | NULL | NULL | USA | 7 | AO7 | MEASURING THE ACCRETION DISK AND BLACK HOLE PROPERTIES OF ESO 511-G30 | XIS | Y |
| ESO 511-G030 | 214.8456 | -26.6457 | 326.23004886 | 32.21661925 | 292.391 | 56156.7622337963 | 56157.7960416667 | 707023030 | 51917.2 | 270000 | 51925.2 | 51925.2 | 0 | 51917.2 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 52011 | 52011 | 89315.8 | 3 | PROCESSED | 57606.8813194444 | 56640 | 56272.6998148148 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071413 | The study of "bare" Seyfert 1 AGN is essential to measure the true properties of the inner regions of the accretion disk. The nearby Seyfert ESO 511-G30 is a prime candidate for fulfilling this role due to its broad Fe K component and lack of any intrinsic warm absorption. It is also one of the X-ray brightest bare Seyferts featured in the Swift 58 month BAT catalogue as yet unobserved with Suzaku. We propose a 270 ks Suzaku observation of ESO 511-G30 to unambiguously constrain the properties of the accretion disk and subsequently the black hole spin. In addition, the HXD data will allow us to measure the Compton reflection hump, while the excellent soft X-ray spectral resolution of XIS will allow the origin of the soft excess to be determined. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | REEVES | JAMES | NULL | NULL | USA | 7 | AO7 | MEASURING THE ACCRETION DISK AND BLACK HOLE PROPERTIES OF ESO 511-G30 | XIS | Y |
| NGC 4151 | 182.642 | 39.4132 | 155.04475012 | 75.06022062 | 134.3454 | 56242.8428472222 | 56245.9599537037 | 707024010 | 150266.9 | 150000 | 150282.9 | 150266.9 | 0 | 150282.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 150546.5 | 150546.5 | 269289.7 | 4 | PROCESSED | 57608.0679861111 | 56702 | 56330.6348032407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071417 | We propose simultaneous NuSTAR/Suzaku observations of NGC 4151 and IC 4329A. These pointings will achieve three goals: (1) They will provide the best-ever broad-band X-ray spectra of two of the brightest Seyfert galaxies in the 0.5-80 keV band; (2) They will enable broad-band, time-resolved X-ray spectroscopy of these fascinating and variable sources; (3) They will serve as invaluable calibration targets for the two observatories. The spectral coverage and sensitivity will enable the continuum, absorption and reflection components of each spectrum to be conclusively disentangled, allowing us to determine whether inner disk reflection signatures are present. We will also be able to break the degeneracy between the coronal temperature and optical depth in both AGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | BRENNEMAN | LAURA | NULL | NULL | USA | 7 | AO7 | SHEDDING NEW LIGHT ON THE BROAD-BAND X-RAY SPECTRA OF NGC 4151 AND IC 4329A | XIS | Y |
| IC 4329A | 207.3331 | -30.3096 | 317.49896941 | 30.91923491 | 296.2 | 56152.0924652778 | 56154.6425578704 | 707025010 | 117593.8 | 120000 | 117593.8 | 117593.8 | 0 | 117593.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 112998.6 | 112998.6 | 220263.7 | 2 | PROCESSED | 57606.8955208333 | 56540 | 56170.1592824074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071417 | We propose simultaneous NuSTAR/Suzaku observations of NGC 4151 and IC 4329A. These pointings will achieve three goals: (1) They will provide the best-ever broad-band X-ray spectra of two of the brightest Seyfert galaxies in the 0.5-80 keV band; (2) They will enable broad-band, time-resolved X-ray spectroscopy of these fascinating and variable sources; (3) They will serve as invaluable calibration targets for the two observatories. The spectral coverage and sensitivity will enable the continuum, absorption and reflection components of each spectrum to be conclusively disentangled, allowing us to determine whether inner disk reflection signatures are present. We will also be able to break the degeneracy between the coronal temperature and optical depth in both AGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | BRENNEMAN | LAURA | NULL | NULL | USA | 7 | AO7 | SHEDDING NEW LIGHT ON THE BROAD-BAND X-RAY SPECTRA OF NGC 4151 AND IC 4329A | XIS | Y |
| PG 1404+226 | 211.5943 | 22.4043 | 21.50519934 | 72.36517417 | 124.2434 | 56284.2179398148 | 56286.1272453704 | 707026010 | 80296.9 | 80000 | 80312.9 | 80296.9 | 0 | 80304.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70584.8 | 70584.8 | 164945.7 | 1 | PROCESSED | 57608.3815972222 | 56687 | 56320.7751157407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071419 | We propose a 80 ks observation of a NLS galaxy, PG1404+226, with Suzaku/XIS to investigate the physical conditions of extreme absorbers known as the ultra-fast-outflows (UFOs; v/c~0.1-0.2) of variable resonant absorption features from many ions (e.g. Ne IX, Ne X, Mg XII and S XVI) in the soft X-ray band (~0.5-3.5 keV), and we propose the first Suzaku observation of this object to (i) independently confirm/refute the previous claims of the presence of these UFOs including a potential detection of Fe K-shell absorbers, (ii) examine their variabilities and compare the outflow properties at low and high XIS-flux states, (iii) compare its outflow rate and kinetic power with those in other AGN UFOs, and (iv) utilize a high-quality Suzaku data to improve our MHD disk-wind model. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | FUKUMURA | KEIGO | NULL | NULL | USA | 7 | AO7 | PROBING THE ULTRA-FAST-OUTFLOWS OF PG1404+226 WITH SUZAKU | XIS | Y |
| MCG-03-34-64 | 200.5996 | -16.727 | 313.53711237 | 45.50625694 | 110.133 | 56296.8837384259 | 56301.1737384259 | 707027010 | 155712.7 | 150000 | 155736.7 | 155712.7 | 0 | 155728.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 135051.6 | 135051.6 | 370603.8 | 4 | PROCESSED | 57608.5292824074 | 56018 | 56336.6958680556 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071423 | Analysis of Suzaku observations selected from the BAT 58-month catalog has shown extreme hard X-ray excesses to exist in ~70% of type 1 AGN, and these can be modeled by partial-covering of Compton-thick gas. This new result shows the importance of broad X-ray coverage, currently available only with Suzaku. The most extreme of the sample sources, MCG-03-34-64 and NGC 1194, show significant spectral and flux variability above 10 keV, likely attributable to changes in the Compton-thick absorber. We request new observations of MCG-03-34-64 (150 ks) and NGC 1194 (200 ks) to study the X-ray reprocessor in these extreme systems, confirm the high-energy spectral variability and constrain the nature and location of the Compton-thick absorber. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | TURNER | TRACEY | NULL | NULL | USA | 7 | AO7 | THE CASE FOR VARIATIONS IN COMPTON-THICK ABSORPTION: MCG-03-34-64 AND NGC 1194 | XIS | Y |
| NGC 5252 | 204.5663 | 4.5481 | 331.30380316 | 64.80829028 | 117.6998 | 56287.8794791667 | 56289.0952777778 | 707028010 | 50270.1 | 45000 | 50270.1 | 50292.1 | 0 | 50276.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43336.7 | 43336.7 | 105027.8 | 0 | PROCESSED | 57608.3760300926 | 56687 | 56321.5462268518 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071424 | A hard X-ray-selected (BAT) AGN sample shows a remarkable 70% of the local population of type 1 AGN to have extreme hard excesses above 20 keV, likely caused by Compton-thick gas in the line-of-sight, covering at least 50% of the source. We request six snapshot observations to complete a Suzaku survey of a BAT-flux-limited sample and make a complete and unbiased measurement of the incidence. Analysis of the new sources will be performed in conjunction with existing exposures, providing exciting new insight into the previously unknown structures in hard X-ray selected AGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | TURNER | TRACEY | NULL | NULL | USA | 7 | AO7 | INVESTIGATING COMPTON-THICK ABSORBERS IN TYPE 1 AGN: OVERHAULING THE AGN PARADIGM | XIS | Y |
| IRAS 05078+1626 | 77.6911 | 16.4922 | 186.12002752 | -13.50176431 | 259.3263 | 56351.6301736111 | 56352.6112847222 | 707029010 | 46016.7 | 45000 | 46016.7 | 46016.7 | 0 | 46016.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44110.1 | 44110.1 | 84755.8 | 1 | PROCESSED | 57610.7197916667 | 56749 | 56372.578287037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071424 | A hard X-ray-selected (BAT) AGN sample shows a remarkable 70% of the local population of type 1 AGN to have extreme hard excesses above 20 keV, likely caused by Compton-thick gas in the line-of-sight, covering at least 50% of the source. We request six snapshot observations to complete a Suzaku survey of a BAT-flux-limited sample and make a complete and unbiased measurement of the incidence. Analysis of the new sources will be performed in conjunction with existing exposures, providing exciting new insight into the previously unknown structures in hard X-ray selected AGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | TURNER | TRACEY | NULL | NULL | USA | 7 | AO7 | INVESTIGATING COMPTON-THICK ABSORBERS IN TYPE 1 AGN: OVERHAULING THE AGN PARADIGM | XIS | Y |
| UGC 03142 | 70.9469 | 28.9681 | 172.09277202 | -10.99747628 | 264.8107 | 56335.692349537 | 56336.9946296296 | 707032010 | 51284.7 | 50000 | 51284.7 | 51292.7 | 0 | 51300.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47563.2 | 47563.2 | 112510 | 1 | PROCESSED | 57610.6216898148 | 56721 | 56349.5963541667 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071424 | A hard X-ray-selected (BAT) AGN sample shows a remarkable 70% of the local population of type 1 AGN to have extreme hard excesses above 20 keV, likely caused by Compton-thick gas in the line-of-sight, covering at least 50% of the source. We request six snapshot observations to complete a Suzaku survey of a BAT-flux-limited sample and make a complete and unbiased measurement of the incidence. Analysis of the new sources will be performed in conjunction with existing exposures, providing exciting new insight into the previously unknown structures in hard X-ray selected AGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | TURNER | TRACEY | NULL | NULL | USA | 7 | AO7 | INVESTIGATING COMPTON-THICK ABSORBERS IN TYPE 1 AGN: OVERHAULING THE AGN PARADIGM | XIS | Y |
| NGC 2110 | 88.0457 | -7.4586 | 212.92775975 | -16.54787795 | 79.201 | 56170.1053009259 | 56172.5412268518 | 707034010 | 103259.5 | 100000 | 103259.5 | 103259.5 | 0 | 103259.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 102806.3 | 102806.3 | 210436.1 | 1 | PROCESSED | 57607.0102199074 | 56667 | 56301.6411458333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071426 | We request two 100 ks | EXTRAGALACTIC COMPACT SOURCES | 7 | B | RIVERS | ELIZABETH | NULL | NULL | USA | 7 | AO7 | TRACKING THE PARTIAL COVERING ABSORBERS IN NGC 2110: CONSTRAINTS FOR CLUMPY ABSORBER MODELS | XIS | Y |
| PDS 456 | 262.0802 | -14.261 | 10.39487872 | 11.16781955 | 96.2511 | 56344.8907407407 | 56349.993912037 | 707035010 | 182299 | 450000 | 182299 | 182299 | 0 | 182299 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 160307.1 | 160307.1 | 440875.2 | 4 | PROCESSED | 57610.7549768518 | 56018 | 56363.6993981482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071431 | PDS 456 is the most luminous nearby (z=0.184) AGN, more typical of quasars at high redshift. A 2007 Suzaku observation resolved iron K absorption at 9 keV in the QSO frame, moving at near relativistic velocities (0.25c). A follow-up 2011 observation was highly absorbed and showed a direct response of the iron K absorber to a decrease in the ionizing flux, while the harder photons lag behind the soft, by 10^4 secs. We propose to monitor the remarkable spectral variability and outflow from PDS 456, through a deep 450ks Suzaku observation. We wish to:- (i) quantify the time lags and determine the location of the reprocessor, (ii) determine the origin and timescale of the absorber variability and (iii) measure the hard X-ray variability from a Compton thick absorber in PDS 456. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | REEVES | JAMES | NULL | NULL | USA | 7 | AO7 | VARIABILITY AND REVERBERATION OF THE QUASAR WIND IN PDS 456 | XIS | Y |
| PDS 456 | 262.0805 | -14.2617 | 10.39443055 | 11.16720212 | 96.2512 | 56354.8215972222 | 56359.5001388889 | 707035020 | 164810.7 | 450000 | 164826.7 | 164810.7 | 0 | 164829.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 147449.6 | 147449.6 | 404181.5 | 2 | PROCESSED | 57610.8342824074 | 56018 | 56373.6804166667 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071431 | PDS 456 is the most luminous nearby (z=0.184) AGN, more typical of quasars at high redshift. A 2007 Suzaku observation resolved iron K absorption at 9 keV in the QSO frame, moving at near relativistic velocities (0.25c). A follow-up 2011 observation was highly absorbed and showed a direct response of the iron K absorber to a decrease in the ionizing flux, while the harder photons lag behind the soft, by 10^4 secs. We propose to monitor the remarkable spectral variability and outflow from PDS 456, through a deep 450ks Suzaku observation. We wish to:- (i) quantify the time lags and determine the location of the reprocessor, (ii) determine the origin and timescale of the absorber variability and (iii) measure the hard X-ray variability from a Compton thick absorber in PDS 456. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | REEVES | JAMES | NULL | NULL | USA | 7 | AO7 | VARIABILITY AND REVERBERATION OF THE QUASAR WIND IN PDS 456 | XIS | Y |
| PDS 456 | 262.0806 | -14.2617 | 10.39448289 | 11.16711992 | 96.2509 | 56359.500150463 | 56362.375162037 | 707035030 | 108339.7 | 450000 | 108347.7 | 108347.7 | 0 | 108339.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 94226 | 94226 | 248391.8 | 3 | PROCESSED | 57610.7991435185 | 56018 | 56373.5603125 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071431 | PDS 456 is the most luminous nearby (z=0.184) AGN, more typical of quasars at high redshift. A 2007 Suzaku observation resolved iron K absorption at 9 keV in the QSO frame, moving at near relativistic velocities (0.25c). A follow-up 2011 observation was highly absorbed and showed a direct response of the iron K absorber to a decrease in the ionizing flux, while the harder photons lag behind the soft, by 10^4 secs. We propose to monitor the remarkable spectral variability and outflow from PDS 456, through a deep 450ks Suzaku observation. We wish to:- (i) quantify the time lags and determine the location of the reprocessor, (ii) determine the origin and timescale of the absorber variability and (iii) measure the hard X-ray variability from a Compton thick absorber in PDS 456. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | REEVES | JAMES | NULL | NULL | USA | 7 | AO7 | VARIABILITY AND REVERBERATION OF THE QUASAR WIND IN PDS 456 | XIS | Y |
| IRAS 00182-7112 | 5.1458 | -70.9276 | 306.55074146 | -45.98323945 | 33.8687 | 56050.171087963 | 56052.8759143518 | 707036010 | 93959 | 90000 | 93967 | 93959 | 0 | 93959 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 86576.6 | 86576.6 | 233681.9 | 1 | PROCESSED | 57605.3998263889 | 56435 | 56068.6299537037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071441 | We propose to observe with the Hard X-ray Detector onboard Suzaku the two Ultraluminous Infrared Galaxies IRAS 00182-7112 and IRAS 12127-1412, both of which are known to harbour very luminous and highly obscured active galactic nuclei (AGN). An AGN reflection component arising from ionized gas is clearly identified at 2 10 keV: the detection of the direct AGN emission above 10 keV and the measure of the reflection efficiency would provide fundamental information on both the physical structure of Compton-thick AGN embedded in a nuclear starburst and their feedback on the surrounding environment. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | NARDINI | EMANUELE | NULL | NULL | USA | 7 | AO7 | THE PHYSICAL STRUCTURE OF COMPTON-THICK AGN/ULIRGS | XIS | Y |
| IRAS 12127-1412 | 183.8305 | -14.4966 | 289.94461652 | 47.46236248 | 294.8513 | 56113.7580671296 | 56115.2862615741 | 707037010 | 63609.5 | 60000 | 63609.5 | 63609.5 | 0 | 63609.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 57584 | 57584 | 132012 | 2 | PROCESSED | 57606.6111342593 | 56508 | 56142.1406018518 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071441 | We propose to observe with the Hard X-ray Detector onboard Suzaku the two Ultraluminous Infrared Galaxies IRAS 00182-7112 and IRAS 12127-1412, both of which are known to harbour very luminous and highly obscured active galactic nuclei (AGN). An AGN reflection component arising from ionized gas is clearly identified at 2 10 keV: the detection of the direct AGN emission above 10 keV and the measure of the reflection efficiency would provide fundamental information on both the physical structure of Compton-thick AGN embedded in a nuclear starburst and their feedback on the surrounding environment. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | NARDINI | EMANUELE | NULL | NULL | USA | 7 | AO7 | THE PHYSICAL STRUCTURE OF COMPTON-THICK AGN/ULIRGS | XIS | Y |
| WISE J1819+4532 | 274.9137 | 45.5584 | 73.38480627 | 24.31157427 | 77.6532 | 56020.3333333333 | 56021.0070833333 | 707038010 | 30881.9 | 30000 | 30881.9 | 30881.9 | 0 | 30881.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27564 | 27564 | 58203.9 | 0 | PROCESSED | 57605.0974537037 | 56399 | 56033.2380787037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071443 | We request a 30-ks observation of WISE J1819+4532, an extreme WISE-selected AGN at z=2.031. This source stands out even amongst the rare WISE-selected sources we have been targeting: at mid-IR wavelengths, WISE J1819+4532 is ~10x brighter than similarly selected WISE sources, and more than 50x brighter than extreme Spitzer-selected sources. Assuming the local mid-IR to hard X-ray correlations, the implied intrinsic hard X-ray luminosity is L(2-10)~3e46 erg/s. WISE J1819+4532 is optically faint and the optical spectrum shows a typical obscured AGN with narrow emission lines. However, the object is infrared bright and the near-IR spectrum shows broad H-alpha emission. This implies that WISE J1819+4532 is a rare example of a an extremely luminous, semi-obscured AGN. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | STERN | DANIEL | NULL | NULL | USA | 7 | AO7 | WISE J1819+4532: AN OBSCURED, HYPERLUMINOUS ULIRG/AGN AT Z~2 | XIS | Y |
| RE J1034+396 | 158.663 | 39.6488 | 180.26295059 | 59.06449262 | 115.7032 | 56245.9648726852 | 56248.0689583333 | 707039010 | 99911.3 | 100000 | 99919.3 | 99911.3 | 0 | 99919.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 93446 | 93446 | 181763.9 | 3 | PROCESSED | 57608.0485416667 | 56640 | 56274.6249884259 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 072005 | Understanding the nature of the emission from the extreme active galaxy, RE J1034+396 can help us to unravel the properties of accretion as the Eddington limit is reached. A fleeting glimpse of the unique quasi-periodic oscillation (QPO) in this source has shown a complex timing behaviour with the emission below ~2 keV apparently crucial to its presence. Thus by understanding the origin and properties of the soft emission we can probe the physical mechanism of signals that cannot be resolved in stellar mass X-ray binaries but must be associated with the regions closest to the black hole. A new observation with Suzaku will allow a much deeper analysis of the soft emission and will shed light on how its changing properties can trigger such unique behaviour as the QPO. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | MIDDLETON | MATTHEW | NULL | NULL | EUR | 7 | AO7 | REVEALING THE NATURE OF RE J1034+396 AND THE EXTREME SOFT EXCESS | XIS | Y |
| PKS 0548-322 | 87.6707 | -32.2739 | 237.56869078 | -26.144265 | 287.028 | 56023.6105555556 | 56026.3891435185 | 707040010 | 102656.7 | 100000 | 102656.7 | 102656.7 | 0 | 102656.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 91523.7 | 91523.7 | 240055.8 | 3 | PROCESSED | 57605.1844907407 | 56415 | 56044.314525463 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 072006 | We propose Suzaku observations of the two brightest extreme BL Lac objects, PKS 0548-322 and RGB J0710+591 (100 ksec each), whose synchrotron bump peaks in the medium-hard X-ray band. The requested observations, never performed by Suzaku on this two sources, will permit to measure their continuum in the 0.6-70 keV range, fully exploiting the unique capabilities of the Suzaku satellite. With its wide energy coverage and good response, Suzaku will allow us to determine with unprecedented precision the spectral properties of the sources in the hard, medium and soft X-ray ranges, allowing us to measure the physical properties of the emitting relativistic electrons and, complemented by data at other frequencies, to infer the physical conditions in the emitting region. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TAVECCHIO | FABRIZIO | NULL | NULL | EUR | 7 | AO7 | REVEALING THE HIGH-ENERGY SYNCHROTRON PEAK OF EXTREME BL LACS WITH SUZAKU | XIS | Y |
| 0827+243 | 127.7155 | 24.1863 | 200.01763935 | 31.87561316 | 105.3936 | 56213.3893287037 | 56213.5959837963 | 707041010 | 8039.2 | 10000 | 8047.2 | 8039.2 | 0 | 8047.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7737 | 7737 | 17847.9 | 0 | PROCESSED | 57607.7474652778 | 56598 | 56232.4327199074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071601 | We propose to perform two 2-week multi-frequency campaigns of observations of a sample of gamma-ray blazars during Fermi Cycle 5. The campaigns will involve: (1) gamma-ray monitoring with the Fermi LAT, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B, V, R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku and Swift; (6) mid-IR measurements with IRTF; and (7) near-IR photometric J, H, and K observations. The research aims i) to search for correlated variability on short timescales; ii) to compile SEDs at different states of gamma-ray and radio jet activitiy; and iii) to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars. | EXTRAGALACTIC COMPACT SOURCES | 7 | S | JORSTAD | SVETLANA | NULL | NULL | USA | 7 | AO7 | MULTI-FREQUENCY CAMPAIGNS TO STUDY RAPID VARIABILITY IN GAMMA_RAY BLAZARS | XIS | Y |
| 0836+710 | 130.3582 | 70.9091 | 143.52368034 | 34.42368753 | 111.9979 | 56213.6030787037 | 56213.8223726852 | 707042010 | 10613 | 10000 | 10613 | 10613 | 0 | 10613 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8866 | 8866 | 18927.9 | 0 | PROCESSED | 57607.7537615741 | 56598 | 56232.4320717593 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071601 | We propose to perform two 2-week multi-frequency campaigns of observations of a sample of gamma-ray blazars during Fermi Cycle 5. The campaigns will involve: (1) gamma-ray monitoring with the Fermi LAT, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B, V, R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku and Swift; (6) mid-IR measurements with IRTF; and (7) near-IR photometric J, H, and K observations. The research aims i) to search for correlated variability on short timescales; ii) to compile SEDs at different states of gamma-ray and radio jet activitiy; and iii) to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars. | EXTRAGALACTIC COMPACT SOURCES | 7 | S | JORSTAD | SVETLANA | NULL | NULL | USA | 7 | AO7 | MULTI-FREQUENCY CAMPAIGNS TO STUDY RAPID VARIABILITY IN GAMMA_RAY BLAZARS | XIS | Y |
| 3C345 | 250.7487 | 39.7945 | 63.43440525 | 40.94504508 | 267.732 | 56181.2697453704 | 56181.4772337963 | 707043010 | 12700.8 | 10000 | 12708.8 | 12716.8 | 0 | 12700.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10731.4 | 10731.4 | 17919.9 | 0 | PROCESSED | 57606.986412037 | 56582 | 56212.7656712963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071601 | We propose to perform two 2-week multi-frequency campaigns of observations of a sample of gamma-ray blazars during Fermi Cycle 5. The campaigns will involve: (1) gamma-ray monitoring with the Fermi LAT, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B, V, R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku and Swift; (6) mid-IR measurements with IRTF; and (7) near-IR photometric J, H, and K observations. The research aims i) to search for correlated variability on short timescales; ii) to compile SEDs at different states of gamma-ray and radio jet activitiy; and iii) to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars. | EXTRAGALACTIC COMPACT SOURCES | 7 | S | JORSTAD | SVETLANA | NULL | NULL | USA | 7 | AO7 | MULTI-FREQUENCY CAMPAIGNS TO STUDY RAPID VARIABILITY IN GAMMA_RAY BLAZARS | XIS | Y |
| BL LAC | 330.6707 | 42.2941 | 92.59387966 | -10.42383814 | 77.7587 | 56431.6193981482 | 56431.8724884259 | 707044010 | 12742.6 | 10000 | 12750.6 | 12742.6 | 0 | 12750.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13144 | 13144 | 21831.9 | 0 | PROCESSED | 57611.320625 | 56826 | 56455.7300231482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071601 | We propose to perform two 2-week multi-frequency campaigns of observations of a sample of gamma-ray blazars during Fermi Cycle 5. The campaigns will involve: (1) gamma-ray monitoring with the Fermi LAT, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B, V, R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku and Swift; (6) mid-IR measurements with IRTF; and (7) near-IR photometric J, H, and K observations. The research aims i) to search for correlated variability on short timescales; ii) to compile SEDs at different states of gamma-ray and radio jet activitiy; and iii) to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars. | EXTRAGALACTIC COMPACT SOURCES | 7 | S | JORSTAD | SVETLANA | NULL | NULL | USA | 7 | AO7 | MULTI-FREQUENCY CAMPAIGNS TO STUDY RAPID VARIABILITY IN GAMMA_RAY BLAZARS | XIS | Y |
| CTA102 | 338.1458 | 11.7401 | 77.43997335 | -38.57166798 | 72.4263 | 56431.345462963 | 56431.6134606482 | 707045010 | 9562.6 | 10000 | 9570.6 | 9562.6 | 0 | 9570.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7283 | 7283 | 23143.9 | 0 | PROCESSED | 57611.3187847222 | 56809 | 56443.5010069444 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071601 | We propose to perform two 2-week multi-frequency campaigns of observations of a sample of gamma-ray blazars during Fermi Cycle 5. The campaigns will involve: (1) gamma-ray monitoring with the Fermi LAT, (2) VLBA total and polarized intensity imaging at 43 GHz 3 times per campaign, (3) daily optical photometric B, V, R, and I measurements, (4) R-band polarimetric observations, (5) X-ray observations with Suzaku and Swift; (6) mid-IR measurements with IRTF; and (7) near-IR photometric J, H, and K observations. The research aims i) to search for correlated variability on short timescales; ii) to compile SEDs at different states of gamma-ray and radio jet activitiy; and iii) to explore mechanisms of high energy production and locations of gamma-ray emission regions in blazars. | EXTRAGALACTIC COMPACT SOURCES | 7 | S | JORSTAD | SVETLANA | NULL | NULL | USA | 7 | AO7 | MULTI-FREQUENCY CAMPAIGNS TO STUDY RAPID VARIABILITY IN GAMMA_RAY BLAZARS | XIS | Y |
| MARKARIAN 1040 | 37.056 | 31.3166 | 146.10796909 | -27.16282444 | 69.5695 | 56515.9165740741 | 56519.1681597222 | 707046010 | 137435.3 | 135000 | 137435.3 | 137435.3 | 0 | 137435.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 136328 | 136328 | 280905.3 | 1 | PROCESSED | 57612.3140625 | 56955 | 56587.9502662037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 072025 | Mrk 1040 is a nearby type-1 Seyfert galaxy where a recent XMM observation revealed the presence of a deep soft X-ray warm absorber. However the current data are unable to resolve the components of the absorber so very little is known about its properties. We propose to obtain a 200 ks definitive Chandra HETG observation of Mrk 1040 from 0.5-9.0 keV where we will resolve the lines for the first time enabling a detailed analysis of the kinematics and energetics to be made. We will also obtain the first high-resolution spectrum > 2 keV in this source allowing us to resolve the narrow Fe K alpha core. Furthermore, through a 125 ks Suzaku observation we will also study the Fe K complex in unprecedented detail while simultaneously determining the origin of the hard excess. | EXTRAGALACTIC COMPACT SOURCES | 7 | S | LOBBAN | ANDREW | NULL | NULL | EUR | 7 | AO7 | A HIGH-RESOLUTION VIEW OF THE WARM ABSORBER AND IRON LINE IN MRK 1040 | XIS | Y |
| NGC 5273 | 205.535 | 35.6446 | 74.3162813 | 76.25118024 | 278.9999 | 56489.1929976852 | 56491.0543171296 | 708001010 | 81770.9 | 80000 | 81770.9 | 81794.9 | 0 | 81778.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 79098.1 | 79098.1 | 160801.8 | 3 | PROCESSED | 57612.0002546296 | 56890 | 56523.6749537037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080015 | The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to population synthesis models, its estimate is strongly coupled with the broad band spectral shape of Compton thin AGNs. Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright AGNs that can be best followed-up with Suzaku. Here we propose to observe two of the lowest luminosity BAT AGNs to measure the amount of the reflection component with unpreceded accuracy, a key parameter to determine the contribution of Compton thick AGNs to the X-ray background. We will also study how the torus structure of low luminosity AGNs differs from that of more luminous AGNs. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 8 | AO8 | BROAD BAND SPECTRA OF HARD X-RAY SELECTED VERY LOW LUMINOSITY AGNS AND THEIR TORUS STRUCTURE | XIS | Y |
| NGC 3997 | 179.448 | 25.2646 | 218.72362191 | 77.82883353 | 305.585 | 56439.4793981482 | 56441.452974537 | 708002010 | 87138.3 | 80000 | 87138.3 | 87138.3 | 0 | 87138.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 83050.4 | 83050.4 | 170508 | 2 | PROCESSED | 57611.4399305556 | 56816 | 56450.866724537 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080015 | The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to population synthesis models, its estimate is strongly coupled with the broad band spectral shape of Compton thin AGNs. Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright AGNs that can be best followed-up with Suzaku. Here we propose to observe two of the lowest luminosity BAT AGNs to measure the amount of the reflection component with unpreceded accuracy, a key parameter to determine the contribution of Compton thick AGNs to the X-ray background. We will also study how the torus structure of low luminosity AGNs differs from that of more luminous AGNs. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 8 | AO8 | BROAD BAND SPECTRA OF HARD X-RAY SELECTED VERY LOW LUMINOSITY AGNS AND THEIR TORUS STRUCTURE | XIS | Y |
| NGC 4785 | 193.3693 | -48.746 | 303.27856941 | 14.12437615 | 296.8629 | 56495.4767013889 | 56496.6341782407 | 708003010 | 79388.2 | 70000 | 79388.2 | 79396.2 | 0 | 79388.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70777 | 70777 | 99994 | 0 | PROCESSED | 57611.9465972222 | 56876 | 56509.7469907407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080027 | At faint fluxes, the Swift/BAT AGN survey is uncovering sources with very hard photon indices (Gamma) above 10 keV. The origin of a low Gamma in the hard band is ill-understood, but may include high/atypical obscuration, non-thermal X-rays without radio jets, or electron coronae with high temperatures or optical depths. In AO7, we observed two such Seyfert 2s and discovered Compton-thick obscuration in one source, and a buried AGN spectrum with no reflection or high-energy cutoff in the other. The hard BAT Gamma values thus have a variety of origins, and our strategy is very effective in selecting objects with interesting spectra. Here, we propose to observe two hardest sources (Gamma<~1) with no prior X-ray observations below 10 keV in order to shed light on the nature of this population. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GANDHI | POSHAK | NULL | NULL | JAP | 8 | AO8 | THE VARIED NATURE OF SWIFT/BAT HARD-SPECTRUM SEYFERT 2S | XIS | Y |
| ESO 119-G008 | 72.2547 | -57.6544 | 266.66680471 | -38.87724734 | 324.43 | 56411.0111458333 | 56413.2355787037 | 708004010 | 100587.3 | 100000 | 100595.3 | 100595.3 | 0 | 100587.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 103761.4 | 103761.4 | 192171.9 | 3 | PROCESSED | 57611.2384375 | 56837 | 56475.7648611111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080027 | At faint fluxes, the Swift/BAT AGN survey is uncovering sources with very hard photon indices (Gamma) above 10 keV. The origin of a low Gamma in the hard band is ill-understood, but may include high/atypical obscuration, non-thermal X-rays without radio jets, or electron coronae with high temperatures or optical depths. In AO7, we observed two such Seyfert 2s and discovered Compton-thick obscuration in one source, and a buried AGN spectrum with no reflection or high-energy cutoff in the other. The hard BAT Gamma values thus have a variety of origins, and our strategy is very effective in selecting objects with interesting spectra. Here, we propose to observe two hardest sources (Gamma<~1) with no prior X-ray observations below 10 keV in order to shed light on the nature of this population. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GANDHI | POSHAK | NULL | NULL | JAP | 8 | AO8 | THE VARIED NATURE OF SWIFT/BAT HARD-SPECTRUM SEYFERT 2S | XIS | Y |
| IRAS 00521-7054 | 13.5029 | -70.6421 | 302.62218098 | -46.48460341 | 40.2116 | 56431.8840740741 | 56434.2543287037 | 708005010 | 103045 | 100000 | 103053 | 103045 | 0 | 103053 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 87340.5 | 87340.5 | 204769.7 | 1 | PROCESSED | 57611.3837152778 | 56809 | 56443.6034259259 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080036 | The existence of a broad iron line in AGN is still very debated. Amongst the several claims of detection of broad iron lines performed in the last decade, that of IRAS 00521-7054 is one of the most surprising. This type-2 object appears to show in fact an extremely broadened iron line, which would require a maximally rotating supermassive black hole and the presence of light bending. However, due to the lack of high-quality broadband studies, alternative explanations, as a clumpy-absorbers scenario, cannot be ruled out. The aim of this proposal is to perform a 100ks observation of IRAS 00521-7054. Thanks to its large band coverage and its good sensitivity in the iron-line region, Suzaku will allow us to clearly understand the origin of the intriguing spectral features of IRAS 00521-7054. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | RICCI | CLAUDIO | NULL | NULL | JAP | 8 | AO8 | UNDERSTANDING THE ORIGIN OF THE PECULIAR X-RAY SPECTRAL FEATURES OF THE SEYFERT 2 IRAS 00521-7054 | XIS | Y |
| NGC 3516 | 166.6556 | 72.561 | 133.25565935 | 42.40250412 | 335.7404 | 56391.9675925926 | 56393.0460185185 | 708006010 | 51386 | 50000 | 51402 | 51386 | 0 | 51402 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 49101.5 | 49101.5 | 93163.8 | 1 | PROCESSED | 57611.0515856482 | 56383 | 56421.6947106482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080066 | We propose a series of Suzaku observations of the type I Seyfert galaxy NGC 3516 combined with an optical monitoring campaign. By applying the C3PO method (Noda et al. 2012) to the time variable AGN signals, we can decompose them into individual spectral components, and identify (presumably) primary X-ray emissions in the soft and hard X-ray band distinct from the well-known power law continuum, as well as the reflection component (Noda et al. 2011a, 2011b, 2012). Multiple observations enable us to see the time variability of each primary component, and compare it with an optical variation. From these studies, we can examine where the three primary sources generally exist in AGN central engines. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | NODA | HIROFUMI | NULL | NULL | JAP | 8 | AO8 | THE STUDY OF CENTRAL ENGINE IN NGC 3516 WITH SUZAKU AND OPTICAL SIMULTANEOUS OBSERVATIONS | XIS | Y |
| NGC 3516 | 166.6684 | 72.5566 | 133.25443095 | 42.40827092 | 314.5458 | 56409.0119560185 | 56409.446087963 | 708006020 | 19103 | 50000 | 19119 | 19103 | 0 | 19119 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 20212.1 | 20212.1 | 30723.9 | 0 | PROCESSED | 57611.1744907407 | 56383 | 56457.6034375 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080066 | We propose a series of Suzaku observations of the type I Seyfert galaxy NGC 3516 combined with an optical monitoring campaign. By applying the C3PO method (Noda et al. 2012) to the time variable AGN signals, we can decompose them into individual spectral components, and identify (presumably) primary X-ray emissions in the soft and hard X-ray band distinct from the well-known power law continuum, as well as the reflection component (Noda et al. 2011a, 2011b, 2012). Multiple observations enable us to see the time variability of each primary component, and compare it with an optical variation. From these studies, we can examine where the three primary sources generally exist in AGN central engines. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | NODA | HIROFUMI | NULL | NULL | JAP | 8 | AO8 | THE STUDY OF CENTRAL ENGINE IN NGC 3516 WITH SUZAKU AND OPTICAL SIMULTANEOUS OBSERVATIONS | XIS | Y |
| NGC 3516 | 166.6764 | 72.5574 | 133.25110438 | 42.40886909 | 307.603 | 56424.0155555556 | 56425.1044328704 | 708006030 | 50428.3 | 50000 | 50428.3 | 50428.3 | 0 | 50428.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 57227.5 | 57227.5 | 94076 | 0 | PROCESSED | 57611.3108680556 | 56383 | 56436.6511805556 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080066 | We propose a series of Suzaku observations of the type I Seyfert galaxy NGC 3516 combined with an optical monitoring campaign. By applying the C3PO method (Noda et al. 2012) to the time variable AGN signals, we can decompose them into individual spectral components, and identify (presumably) primary X-ray emissions in the soft and hard X-ray band distinct from the well-known power law continuum, as well as the reflection component (Noda et al. 2011a, 2011b, 2012). Multiple observations enable us to see the time variability of each primary component, and compare it with an optical variation. From these studies, we can examine where the three primary sources generally exist in AGN central engines. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | NODA | HIROFUMI | NULL | NULL | JAP | 8 | AO8 | THE STUDY OF CENTRAL ENGINE IN NGC 3516 WITH SUZAKU AND OPTICAL SIMULTANEOUS OBSERVATIONS | XIS | Y |
| NGC 3516 | 166.6912 | 72.5534 | 133.24889589 | 42.41461595 | 284.0065 | 56441.4603009259 | 56442.6355787037 | 708006040 | 54218 | 50000 | 54218 | 54218 | 0 | 54218 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 53120.7 | 53120.7 | 101540 | 1 | PROCESSED | 57615.5831134259 | 56383 | 56503.6575347222 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080066 | We propose a series of Suzaku observations of the type I Seyfert galaxy NGC 3516 combined with an optical monitoring campaign. By applying the C3PO method (Noda et al. 2012) to the time variable AGN signals, we can decompose them into individual spectral components, and identify (presumably) primary X-ray emissions in the soft and hard X-ray band distinct from the well-known power law continuum, as well as the reflection component (Noda et al. 2011a, 2011b, 2012). Multiple observations enable us to see the time variability of each primary component, and compare it with an optical variation. From these studies, we can examine where the three primary sources generally exist in AGN central engines. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | NODA | HIROFUMI | NULL | NULL | JAP | 8 | AO8 | THE STUDY OF CENTRAL ENGINE IN NGC 3516 WITH SUZAKU AND OPTICAL SIMULTANEOUS OBSERVATIONS | XIS | Y |
| NGC 3516 | 166.74 | 72.5773 | 133.21492543 | 42.40213112 | 153.6201 | 56572.1874537037 | 56573.9780092593 | 708006050 | 0 | 50000 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | 1 | 0 | 0 | 37205.3 | 37205.3 | 154699.8 | 0 | PROCESSED | 57612.8632291667 | 56383 | 56631.766712963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080066 | We propose a series of Suzaku observations of the type I Seyfert galaxy NGC 3516 combined with an optical monitoring campaign. By applying the C3PO method (Noda et al. 2012) to the time variable AGN signals, we can decompose them into individual spectral components, and identify (presumably) primary X-ray emissions in the soft and hard X-ray band distinct from the well-known power law continuum, as well as the reflection component (Noda et al. 2011a, 2011b, 2012). Multiple observations enable us to see the time variability of each primary component, and compare it with an optical variation. From these studies, we can examine where the three primary sources generally exist in AGN central engines. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | NODA | HIROFUMI | NULL | NULL | JAP | 8 | AO8 | THE STUDY OF CENTRAL ENGINE IN NGC 3516 WITH SUZAKU AND OPTICAL SIMULTANEOUS OBSERVATIONS | XIS | Y |
| NGC 3516 | 166.7239 | 72.5839 | 133.21571384 | 42.39397937 | 129.7498 | 56600.2605671296 | 56601.215474537 | 708006060 | 46200 | 50000 | 46200 | 46200 | 0 | 46200 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45176.4 | 45176.4 | 82502 | 1 | PROCESSED | 57613.2009722222 | 56383 | 56646.7076041667 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080066 | We propose a series of Suzaku observations of the type I Seyfert galaxy NGC 3516 combined with an optical monitoring campaign. By applying the C3PO method (Noda et al. 2012) to the time variable AGN signals, we can decompose them into individual spectral components, and identify (presumably) primary X-ray emissions in the soft and hard X-ray band distinct from the well-known power law continuum, as well as the reflection component (Noda et al. 2011a, 2011b, 2012). Multiple observations enable us to see the time variability of each primary component, and compare it with an optical variation. From these studies, we can examine where the three primary sources generally exist in AGN central engines. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | NODA | HIROFUMI | NULL | NULL | JAP | 8 | AO8 | THE STUDY OF CENTRAL ENGINE IN NGC 3516 WITH SUZAKU AND OPTICAL SIMULTANEOUS OBSERVATIONS | XIS | Y |
| NGC 3516 | 166.6957 | 72.5543 | 133.24670004 | 42.41457084 | 283.0856 | 56435.1473148148 | 56436.2952199074 | 708006070 | 51475.2 | 50000 | 51477.2 | 51475.2 | 0 | 51479.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 53720.3 | 53720.3 | 99165.8 | 1 | PROCESSED | 57611.3639351852 | 56383 | 56449.6609027778 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080066 | We propose a series of Suzaku observations of the type I Seyfert galaxy NGC 3516 combined with an optical monitoring campaign. By applying the C3PO method (Noda et al. 2012) to the time variable AGN signals, we can decompose them into individual spectral components, and identify (presumably) primary X-ray emissions in the soft and hard X-ray band distinct from the well-known power law continuum, as well as the reflection component (Noda et al. 2011a, 2011b, 2012). Multiple observations enable us to see the time variability of each primary component, and compare it with an optical variation. From these studies, we can examine where the three primary sources generally exist in AGN central engines. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | NODA | HIROFUMI | NULL | NULL | JAP | 8 | AO8 | THE STUDY OF CENTRAL ENGINE IN NGC 3516 WITH SUZAKU AND OPTICAL SIMULTANEOUS OBSERVATIONS | XIS | Y |
| NGC 3516 | 166.6694 | 72.5588 | 133.25250212 | 42.40656753 | 323.9054 | 56754.7044675926 | 56755.5002777778 | 708006080 | 51539 | 50000 | 51539 | 51547 | 0 | 51555 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46047.2 | 46047.2 | 68752 | 1 | PROCESSED | 57614.1922800926 | 56383 | 56817.774849537 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080066 | We propose a series of Suzaku observations of the type I Seyfert galaxy NGC 3516 combined with an optical monitoring campaign. By applying the C3PO method (Noda et al. 2012) to the time variable AGN signals, we can decompose them into individual spectral components, and identify (presumably) primary X-ray emissions in the soft and hard X-ray band distinct from the well-known power law continuum, as well as the reflection component (Noda et al. 2011a, 2011b, 2012). Multiple observations enable us to see the time variability of each primary component, and compare it with an optical variation. From these studies, we can examine where the three primary sources generally exist in AGN central engines. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | NODA | HIROFUMI | NULL | NULL | JAP | 8 | AO8 | THE STUDY OF CENTRAL ENGINE IN NGC 3516 WITH SUZAKU AND OPTICAL SIMULTANEOUS OBSERVATIONS | XIS | Y |
| SPT-CLJ2344-4243 | 356.1816 | -42.7169 | 339.63806237 | -69.34299043 | 226.1467 | 56605.0105902778 | 56607.4106597222 | 708012010 | 86204.3 | 80000 | 86204.3 | 86204.3 | 0 | 86204.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 80028.9 | 80028.9 | 207347.7 | 3 | PROCESSED | 57613.3115625 | 56383 | 56653.7570949074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080071 | SPT-CLJ2344-4243 is a distant (z=0.596) extremely luminous (Lx=8x10^45erg/s) cluster with a strong cooling flow rate of 3820 Msun/year. The central galaxy of the cluster shows huge star formation activity and has a luminous (Lx=3x10^45 erg/s) AGN. According to the paper by McDonald et al. (2012) and Fe I detection by our analysis of the archived data of Suzaku, this AGN is likely to be a type 2 QSO, for which we don ft know any other example situated at the center of a cluster. We are observing a special phase of co-evolution of a cluster, its central galaxy, and SMBH at its center. We propose to perform 80ks x 4 times observations with Suzaku to estimate SMBH mass in this system through X-ray variability and to get Fe I line detection with higher confidence. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | UEDA | SHUTARO | NULL | NULL | JAP | 8 | AO8 | CO-EVOLUTION IN SMBH, GALAXY AND CLUSTERS; SUZAKU OBSERVATION OF A TYPE 2 QSO AT THE CENTER OF SPT-CLJ2344-4243 | XIS | Y |
| NGC6552 | 270.0757 | 66.6036 | 96.43339546 | 29.78135373 | 217.6129 | 56610.8399884259 | 56613.0126851852 | 708014010 | 105776.7 | 100000 | 105776.7 | 105776.7 | 0 | 105776.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 102279.7 | 102279.7 | 187707.9 | 1 | PROCESSED | 57613.3907060185 | 57019 | 56653.7413078704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080092 | We propose to observe the interesting Seyfert 2 galaxy NGC6552, which has multi fluorescence lines in the X-ray band. There ara only three objects, including NGC6552, which has multi fluorescence lines in the X-ray band. We aim to detect emission lines finely and study the chemical evolution of the galaxy. We also aim measurements of hard X-ray continuum to constrain the reflection component and other nonthermal emission asscciated with jet or starburst activity. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | KAWANO | TAKAFUMI | NULL | NULL | JAP | 8 | AO8 | OBSERVATION OF THE MULTI EMISSION LINES FROM SEYFERT 2 GALAXY: NGC6552 | XIS | Y |
| HOLMBERG II X-1 | 124.8874 | 70.7162 | 144.27230635 | 32.72696637 | 127.9069 | 56552.1954398148 | 56553.2994212963 | 708015010 | 52190 | 50000 | 52190 | 52190 | 0 | 52190 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48985.2 | 48985.2 | 95376 | 0 | PROCESSED | 57612.6731481482 | 56954 | 56588.6670717593 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081251 | Recent X-ray observations have produced evidence that a subset of the most extreme ultra-luminous X-ray sources (ULXs) are either intermediate-mass black holes or stellar-mass binaries in an unusual super-Eddington state. Current data are unable to deliver a clear answer, as attempts to model the 0.5-10keV spectra have been plagued by degeneracies resulting from the limited bandpass, owing to the previous lack of focusing hard X-ray telescopes. Combined, Suzaku and NuSTAR will obtain high-quality spectra covering 0.5-30keV, providing powerful probes for understanding the accretion modes and nature of the central BHs. A definitive statement on the existence of either 100-1000Msun black holes or extreme accretion states will be an important legacy of both missions. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | WALTON | DOMINIC | NULL | NULL | USA | 8 | AO8 | COORDINATED SUZAKU AND NUSTAR OBSERVATIONS OF HOLMBERG II X-1 | XIS | Y |
| HOLMBERG II X-1 | 124.8826 | 70.7169 | 144.27185866 | 32.72527495 | 119.959 | 56562.4955555556 | 56563.5730324074 | 708015020 | 49283 | 50000 | 49283 | 49283 | 0 | 49283 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48206 | 48206 | 93087.9 | 0 | PROCESSED | 57612.7832986111 | 56954 | 56588.5225462963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081251 | Recent X-ray observations have produced evidence that a subset of the most extreme ultra-luminous X-ray sources (ULXs) are either intermediate-mass black holes or stellar-mass binaries in an unusual super-Eddington state. Current data are unable to deliver a clear answer, as attempts to model the 0.5-10keV spectra have been plagued by degeneracies resulting from the limited bandpass, owing to the previous lack of focusing hard X-ray telescopes. Combined, Suzaku and NuSTAR will obtain high-quality spectra covering 0.5-30keV, providing powerful probes for understanding the accretion modes and nature of the central BHs. A definitive statement on the existence of either 100-1000Msun black holes or extreme accretion states will be an important legacy of both missions. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | WALTON | DOMINIC | NULL | NULL | USA | 8 | AO8 | COORDINATED SUZAKU AND NUSTAR OBSERVATIONS OF HOLMBERG II X-1 | XIS | Y |
| MKN 335 | 1.5767 | 20.2085 | 108.75946317 | -41.41793251 | 71.5257 | 56454.1494907407 | 56457.9792824074 | 708016010 | 143995 | 300000 | 144027 | 143995 | 0 | 144027 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 129552.9 | 129552.9 | 330867.4 | 3 | PROCESSED | 57611.6156828704 | 56383 | 56470.7662037037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081411 | The idea of this proposal is trigger a 300ks observation with Suzaku of the Narrow Line Seyfert 1 Galaxy Mkn 335 during one of its low X-ray flux states. The goal here is to measure its underlying broad-band continuum with Suzaku during a low state and compare it with the 2006 high-state observations. Mkn 335 is one of the best examples of an AGN that went into a deep minimum X-ray flux state. Two competing models can explain these extreme low states: reflection models and partial covering absorber models. Both models still require a variable underlying intrinsic continuum. The science driver is to find out what is causing these low X-ray flux states that have been observed in several NLS1s. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GRUPE | DIRK | NULL | NULL | USA | 8 | AO8-TOO | INTRINSIC LOW-STATE X-RAY LUMINOSITY OF THE NLS1 MKN 335 | XIS | Y |
| MKN 335 | 1.5763 | 20.2091 | 108.75916207 | -41.41726175 | 71.5255 | 56457.9792939815 | 56461.868287037 | 708016020 | 154816.8 | 300000 | 154864.8 | 154816.8 | 0 | 154856.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 141590.8 | 141590.8 | 335894.4 | 3 | PROCESSED | 57611.6590162037 | 56383 | 56512.7189467593 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081411 | The idea of this proposal is trigger a 300ks observation with Suzaku of the Narrow Line Seyfert 1 Galaxy Mkn 335 during one of its low X-ray flux states. The goal here is to measure its underlying broad-band continuum with Suzaku during a low state and compare it with the 2006 high-state observations. Mkn 335 is one of the best examples of an AGN that went into a deep minimum X-ray flux state. Two competing models can explain these extreme low states: reflection models and partial covering absorber models. Both models still require a variable underlying intrinsic continuum. The science driver is to find out what is causing these low X-ray flux states that have been observed in several NLS1s. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GRUPE | DIRK | NULL | NULL | USA | 8 | AO8-TOO | INTRINSIC LOW-STATE X-RAY LUMINOSITY OF THE NLS1 MKN 335 | XIS | Y |
| LEDA 168563 | 73.0158 | 49.5506 | 157.24701812 | 3.42018054 | 86.3166 | 56536.8773611111 | 56539.0592708333 | 708017010 | 100011 | 100000 | 100035 | 100011 | 0 | 100035 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 92947 | 92947 | 188501.8 | 1 | PROCESSED | 57612.530162037 | 56383 | 56608.7327893518 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081413 | We propose to carry out Suzaku observations, a 100 ks each, of three Seyfert I nuclei hard X-ray selected by Swift. Our goal is to distinguish between various competing models proposed for the X-ray spectra of Seyfert I nuclei. Especially we will test, by observing these targets, the ionized relativistic reflection (hereafter IRR). We will take advantage of Suzaku s unique capability of detecting hard X-rays beyond 10 keV by its HXD-PIN, simultaneously with X-rays in lower to medium energy bands by its XIS on board. With our proposed studies we will gain deeper understanding of accretion-powered AGN in general. Since the IRR takes place close to the black hole we will test the effects of strong gravity, such as the black hole spin. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | TSURUTA | SACHIKO | NULL | NULL | USA | 8 | AO8 | SPECTRAL STUDIES OF SOME HARD X-RAY SELECTED SEYFERT NUCLEI | XIS | Y |
| MCG-5-23-16 | 146.9232 | -30.945 | 262.74537578 | 17.2400137 | 295.4404 | 56444.9213194444 | 56448.2467361111 | 708021010 | 159526.2 | 300000 | 159558.2 | 159526.2 | 0 | 159558.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 155126.7 | 155126.7 | 287301.8 | 1 | PROCESSED | 57611.525787037 | 56383 | 56461.789537037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081416 | Significant recent developments in probing environments around AGN black holes has been achieved using X-ray reverberation. They were initially detected in the soft excess of several NLS1s, then recently, the first Fe K reverberation was also seen. In addition to measuring x-rays reverberating a few r_g from the event horizon, short/long delays from different radii have been separated for the first time in NGC4151. Here we propose to observe MCG-5-23-1 for 300 ks in order to study its iron K reverberation. It is optimally one of the brightest and most variable AGN in X-rays. Archival data already show very exciting signatures of Fe K reverberation. With new observations we aim to constrain the emitting region size and study the emission originating at different distances from of the hole. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ZOGHBI | ABDERAHMEN | NULL | NULL | USA | 8 | AO8 | IRON K REVERBERATION IN MCG 5-23-16 | XIS | Y |
| MCG-5-23-16 | 146.9228 | -30.9448 | 262.74496877 | 17.23993252 | 295.4404 | 56448.2467476852 | 56450.9584606482 | 708021020 | 138846.6 | 300000 | 138846.6 | 138846.6 | 0 | 138846.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 140491.4 | 140491.4 | 234282 | 2 | PROCESSED | 57611.5159490741 | 56383 | 56461.7776736111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081416 | Significant recent developments in probing environments around AGN black holes has been achieved using X-ray reverberation. They were initially detected in the soft excess of several NLS1s, then recently, the first Fe K reverberation was also seen. In addition to measuring x-rays reverberating a few r_g from the event horizon, short/long delays from different radii have been separated for the first time in NGC4151. Here we propose to observe MCG-5-23-1 for 300 ks in order to study its iron K reverberation. It is optimally one of the brightest and most variable AGN in X-rays. Archival data already show very exciting signatures of Fe K reverberation. With new observations we aim to constrain the emitting region size and study the emission originating at different distances from of the hole. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | ZOGHBI | ABDERAHMEN | NULL | NULL | USA | 8 | AO8 | IRON K REVERBERATION IN MCG 5-23-16 | XIS | Y |
| NGC5929 | 231.5229 | 41.6989 | 67.89643134 | 55.30533508 | 120.4869 | 56651.8033217593 | 56652.6042824074 | 708022010 | 24649 | 30000 | 24649 | 24668.9 | 0 | 24656.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25176.7 | 25176.7 | 69191.9 | 0 | PROCESSED | 57613.6825925926 | 56383 | 56700.6301388889 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081418 | Using Suzaku's sensitivity in the 2-50keV range, we propose to obtain broad-band spectral fits to the X-ray emission from five Seyfert galaxies which have nuclei that are likely to be Compton-thick. We will thereby derive estimates of their absorbing column densities (hitherto unknown), Fe line widths and equivalent widths, absorption-corrected nuclear X-ray emission and the reprocessed components. With these new estimates we will have complete measurements for a rigorously selected sample of 20 Seyferts that are matched in orientation-independent parameters. The sample selection enables us to account for orientation effects which dominate in them, and investigate the AGN evolution, AGN-star burst connection, and host galaxy evolution. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | SHASTRI | PRAJVAL | NULL | NULL | USA | 8 | AO8 | COMPTON-THICK SEYFERT NUCLEI AND SEYFERT UNIFICATION | XIS | Y |
| MRK533 | 351.9889 | 8.7759 | 90.62800693 | -48.78900326 | 248.1747 | 56634.8830671296 | 56636.0847569444 | 708023010 | 52194 | 50000 | 52194 | 52194 | 0 | 52194 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48561.7 | 48561.7 | 103805.9 | 0 | PROCESSED | 57613.5724421296 | 56383 | 56646.7358449074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081418 | Using Suzaku's sensitivity in the 2-50keV range, we propose to obtain broad-band spectral fits to the X-ray emission from five Seyfert galaxies which have nuclei that are likely to be Compton-thick. We will thereby derive estimates of their absorbing column densities (hitherto unknown), Fe line widths and equivalent widths, absorption-corrected nuclear X-ray emission and the reprocessed components. With these new estimates we will have complete measurements for a rigorously selected sample of 20 Seyferts that are matched in orientation-independent parameters. The sample selection enables us to account for orientation effects which dominate in them, and investigate the AGN evolution, AGN-star burst connection, and host galaxy evolution. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | SHASTRI | PRAJVAL | NULL | NULL | USA | 8 | AO8 | COMPTON-THICK SEYFERT NUCLEI AND SEYFERT UNIFICATION | XIS | Y |
| NGC 235A | 10.7176 | -23.5378 | 94.13393297 | -85.9211578 | 213.1719 | 56636.0921759259 | 56636.4792939815 | 708026010 | 19825.1 | 20000 | 19833.1 | 19825.1 | 0 | 19840.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18225.1 | 18225.1 | 33443.9 | 1 | PROCESSED | 57613.5511921296 | 56383 | 56646.6871412037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081419 | The BAT AGN sample constitutes an unprecedented all-sky hard X-ray survey of the local AGN population. However, to properly model the X-ray absorption & reflection, coverage below 10 keV is needed with CCD spectral resolution and adequate signal-to-noise. We propose to observe 11 AGN with Suzaku, which will increase the completeness of a flux-limited sample with such coverage from 85 to 158 sources. The 11 AGN only have severely underexposed Swift XRT coverage below 10 keV whereas the remaining sources have either Suzaku or XMM coverage. The Suzaku data have the additional advantage of sensitivity above 10 keV that helps to mitigate the long time-baseline of the BAT spectra. The new observations will create a significantly enhanced legacy data set that will provide value for years to come. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | YAQOOB | TAHIR | NULL | NULL | USA | 8 | AO8 | ROBUST CHARACTERIZATION OF ABSORPTION AND REFLECTION IN A LOCAL FLUX-LIMITED AGN POPULATION FROM THE SWIFT BAT SURVEY | XIS | Y |
| MKN 915 | 339.1982 | -12.5468 | 51.05925373 | -55.2984956 | 243.0396 | 56622.9636458333 | 56624.1320601852 | 708029010 | 41220 | 40000 | 41220 | 41220 | 0 | 41220 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37389.3 | 37389.3 | 100939.9 | 0 | PROCESSED | 57613.4605787037 | 56383 | 56637.6375347222 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081419 | The BAT AGN sample constitutes an unprecedented all-sky hard X-ray survey of the local AGN population. However, to properly model the X-ray absorption & reflection, coverage below 10 keV is needed with CCD spectral resolution and adequate signal-to-noise. We propose to observe 11 AGN with Suzaku, which will increase the completeness of a flux-limited sample with such coverage from 85 to 158 sources. The 11 AGN only have severely underexposed Swift XRT coverage below 10 keV whereas the remaining sources have either Suzaku or XMM coverage. The Suzaku data have the additional advantage of sensitivity above 10 keV that helps to mitigate the long time-baseline of the BAT spectra. The new observations will create a significantly enhanced legacy data set that will provide value for years to come. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | YAQOOB | TAHIR | NULL | NULL | USA | 8 | AO8 | ROBUST CHARACTERIZATION OF ABSORPTION AND REFLECTION IN A LOCAL FLUX-LIMITED AGN POPULATION FROM THE SWIFT BAT SURVEY | XIS | Y |
| IGR J09026-4812 | 135.6468 | -48.2323 | 268.86967218 | -1.09239209 | 115.8572 | 56622.3203356482 | 56622.9521990741 | 708031010 | 37792.4 | 35000 | 37824.4 | 37816.4 | 0 | 37792.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35202.9 | 35202.9 | 54585.9 | 1 | PROCESSED | 57613.429212963 | 56383 | 56632.5852777778 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081419 | The BAT AGN sample constitutes an unprecedented all-sky hard X-ray survey of the local AGN population. However, to properly model the X-ray absorption & reflection, coverage below 10 keV is needed with CCD spectral resolution and adequate signal-to-noise. We propose to observe 11 AGN with Suzaku, which will increase the completeness of a flux-limited sample with such coverage from 85 to 158 sources. The 11 AGN only have severely underexposed Swift XRT coverage below 10 keV whereas the remaining sources have either Suzaku or XMM coverage. The Suzaku data have the additional advantage of sensitivity above 10 keV that helps to mitigate the long time-baseline of the BAT spectra. The new observations will create a significantly enhanced legacy data set that will provide value for years to come. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | YAQOOB | TAHIR | NULL | NULL | USA | 8 | AO8 | ROBUST CHARACTERIZATION OF ABSORPTION AND REFLECTION IN A LOCAL FLUX-LIMITED AGN POPULATION FROM THE SWIFT BAT SURVEY | XIS | Y |
| MKN 1148 | 12.9805 | 17.4231 | 123.09650608 | -45.44849404 | 266.997 | 56656.2855555556 | 56657.0627662037 | 708033010 | 28318.9 | 30000 | 28318.9 | 28326.9 | 0 | 28326.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 23100.5 | 23100.5 | 67137.9 | 2 | PROCESSED | 57613.7155324074 | 56383 | 56702.7526273148 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081419 | The BAT AGN sample constitutes an unprecedented all-sky hard X-ray survey of the local AGN population. However, to properly model the X-ray absorption & reflection, coverage below 10 keV is needed with CCD spectral resolution and adequate signal-to-noise. We propose to observe 11 AGN with Suzaku, which will increase the completeness of a flux-limited sample with such coverage from 85 to 158 sources. The 11 AGN only have severely underexposed Swift XRT coverage below 10 keV whereas the remaining sources have either Suzaku or XMM coverage. The Suzaku data have the additional advantage of sensitivity above 10 keV that helps to mitigate the long time-baseline of the BAT spectra. The new observations will create a significantly enhanced legacy data set that will provide value for years to come. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | YAQOOB | TAHIR | NULL | NULL | USA | 8 | AO8 | ROBUST CHARACTERIZATION OF ABSORPTION AND REFLECTION IN A LOCAL FLUX-LIMITED AGN POPULATION FROM THE SWIFT BAT SURVEY | XIS | Y |
| 3C 390.3 | 280.4556 | 79.7798 | 111.44649344 | 27.08887917 | 37.561 | 56436.3002777778 | 56438.6036921296 | 708034010 | 100366.8 | 100000 | 100366.8 | 100366.8 | 0 | 100366.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 109326.7 | 109326.7 | 198981.7 | 3 | PROCESSED | 57611.4065740741 | 56816 | 56449.7081365741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081431 | We propose simultaneous Suzaku (100 ks) and NuSTAR observations of the broad-line radio galaxy 3C 390.3, to measure Fe K-alpha emission and Compton reflection from the accretion disk. This is crucial for understanding the geometry of the accretion disk and its relation to the production of a powerful, relativistic radio jet. The combination of accurate Compton reflection parameters measured with NuSTAR and a simultaneous estimate of the accretion disk inner radius from Fe K-alpha with Suzaku will place strong constraints on accretion disk models for radio loud AGNs. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | OGLE | PATRICK | NULL | NULL | USA | 8 | AO8 | ACCRETION AND BLACK HOLE SPIN IN THE POWERFUL, RADIO-LOUD AGN 3C 390.3 | XIS | Y |
| PMN J1603-4904 | 240.9652 | -49.0681 | 332.15292306 | 2.57171396 | 292.7209 | 56547.6621643518 | 56548.4842013889 | 708035010 | 50912.9 | 50000 | 50925.2 | 50912.9 | 0 | 50917.2 | 3 | 2 | 0 | 3 | 1 | 0 | 0 | 49280.3 | 49280.3 | 70990 | 0 | PROCESSED | 57612.626875 | 56956 | 56588.7813657407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081432 | We propose a 50ksec Suzaku observation of the gamma-ray emitting compact symmetric radio source PMN J1603-4904 as a crucial part of the first simultaneous radio to gamma-ray campaign on this object. Constraining the X-ray spectrum of the compact radio source is needed to properly model the broadband spectral energy distribution (SED), which is essential for understanding the physical nature of this unusual object. The Swift detection allows no spectral modeling of its very faint X-ray counterpart, hence, precise spectral investigations with Suzaku are strongly required. PMN J1603-4904 is one of the few young radio galaxy candidates associated with a bright Fermi gamma-ray source, thus it plays a key role in investigating the underlying emission mechanism of newly born active galaxies. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | OJHA | ROOPESH | NULL | NULL | USA | 8 | AO8 | CONSTRAINING THE NATURE OF PMN J1603-4904: IS IT A GAMMA-LOUD YOUNG RADIO GALAXY? | XIS | Y |
| CENTAURUS A | 201.3699 | -43.0194 | 309.51956362 | 19.416494 | 303.7255 | 56519.1824305556 | 56519.4264930556 | 708036010 | 10675.1 | 10000 | 10675.1 | 10675.1 | 0 | 10691.1 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10064.7 | 10064.7 | 21079.9 | 0 | PROCESSED | 57612.2554050926 | 56954 | 56587.7389351852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081433 | We request observations of the nucleus of the radio galaxy Centaurus A to study time variability of its broadband spectral energy distribution (SED) and constrain jet emission models of radio-loud AGN. Due to its proximity, Cen A can be studied in unique detail. Although frequently observed, no time-dependent, simultaneous SEDs covering the spectrum from radio to gamma-rays have been obtained for Cen A so far. Since AGN are highly variable, only quasi-contemporaneous SEDs allow us to constrain parameters of jet emission models. Combining our TANAMI radio Very Long Baseline Interferometry monitoring campaign and Fermi observations with simultaneous Suzaku spectra will fill the gap in energy and address the time-dependent behavior of jet emission and torus absorption with high accuracy. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | OJHA | ROOPESH | NULL | NULL | USA | 8 | AO8 | SIMULTANEOUS SUZAKU AND MULTIWAVELENGTH OBSERVATIONS OF THE NUCLEUS OF CENTAURUS A | XIS | Y |
| CENTAURUS A | 201.3033 | -43.0014 | 309.47108059 | 19.44109405 | 111.5377 | 56663.4710763889 | 56663.6613888889 | 708036020 | 7365.2 | 10000 | 7365.2 | 7373.2 | 0 | 7373.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 6544.4 | 6544.4 | 16439.9 | 0 | PROCESSED | 57613.7500462963 | 57086 | 56719.7206944444 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081433 | We request observations of the nucleus of the radio galaxy Centaurus A to study time variability of its broadband spectral energy distribution (SED) and constrain jet emission models of radio-loud AGN. Due to its proximity, Cen A can be studied in unique detail. Although frequently observed, no time-dependent, simultaneous SEDs covering the spectrum from radio to gamma-rays have been obtained for Cen A so far. Since AGN are highly variable, only quasi-contemporaneous SEDs allow us to constrain parameters of jet emission models. Combining our TANAMI radio Very Long Baseline Interferometry monitoring campaign and Fermi observations with simultaneous Suzaku spectra will fill the gap in energy and address the time-dependent behavior of jet emission and torus absorption with high accuracy. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | OJHA | ROOPESH | NULL | NULL | USA | 8 | AO8 | SIMULTANEOUS SUZAKU AND MULTIWAVELENGTH OBSERVATIONS OF THE NUCLEUS OF CENTAURUS A | XIS | Y |
| H1821+643 | 275.4676 | 64.3592 | 94.01912066 | 27.4276768 | 65.0012 | 56398.4117013889 | 56402.5419328704 | 708037010 | 246583.9 | 400000 | 246583.9 | 246591.9 | 0 | 246599.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 251027.3 | 251027.3 | 356829.9 | 0 | PROCESSED | 57611.1526273148 | 56383 | 56425.7059606482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081436 | H1821+643 (z=0.297) is not "just another quasar". This luminous active galactic nucleus (AGN) is an extremely rare example of a powerful quasar at the center of a rich, cooling-core cluster of galaxies. As such, it may represent a key evolutionary stage in the complex interplay between AGN and the core regions of the intracluster medium (ICM). Our analysis of archival XMM-Newton data has found evidence for a relativistically broad iron line. Here, we build on this request deep (400ks) Suzaku spectroscopy of H1821+643 to (1) measure the spin of this supermassive black hole and (2) search for powerful highly ionized outflows. In addition to measuring spin in the most luminous and distant object yet, this will enable us to test key predictions of recent models for AGN feedback. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | REYNOLDS | CHRISTOPHER | NULL | NULL | USA | 8 | AO8 | THE BLACK HOLE SPIN AND IONIZED OUTFLOWS IN THE COOLING-FLOW QUASAR H1821+643 | XIS | Y |
| H1821+643 | 275.4669 | 64.3595 | 94.01942058 | 27.4280098 | 65.0004 | 56402.5419444444 | 56404.6925462963 | 708037020 | 128248.5 | 400000 | 128270.3 | 128248.5 | 0 | 128248.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 132821.5 | 132821.5 | 185805.8 | 2 | PROCESSED | 57611.1374884259 | 56383 | 56425.6256712963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081436 | H1821+643 (z=0.297) is not "just another quasar". This luminous active galactic nucleus (AGN) is an extremely rare example of a powerful quasar at the center of a rich, cooling-core cluster of galaxies. As such, it may represent a key evolutionary stage in the complex interplay between AGN and the core regions of the intracluster medium (ICM). Our analysis of archival XMM-Newton data has found evidence for a relativistically broad iron line. Here, we build on this request deep (400ks) Suzaku spectroscopy of H1821+643 to (1) measure the spin of this supermassive black hole and (2) search for powerful highly ionized outflows. In addition to measuring spin in the most luminous and distant object yet, this will enable us to test key predictions of recent models for AGN feedback. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | REYNOLDS | CHRISTOPHER | NULL | NULL | USA | 8 | AO8 | THE BLACK HOLE SPIN AND IONIZED OUTFLOWS IN THE COOLING-FLOW QUASAR H1821+643 | XIS | Y |
| IRAS F11119+3257 | 168.6582 | 32.6829 | 192.21056175 | 68.35212615 | 301.5808 | 56425.1110185185 | 56431.3329050926 | 708038010 | 252299.2 | 250000 | 252323.2 | 252299.2 | 0 | 252323.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 220303.6 | 220303.6 | 400859.9 | 10 | PROCESSED | 57611.4720717593 | 56858 | 56491.9181828704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081441 | Recent Herschel observations provided a breakthrough in identifying powerful, large-scale molecular outflows in ULIRGs, indicating that AGN feedback can indeed have a strong impact on star formation and galaxy evolution, in accordance with theoretical models. However, observational evidence for the connection between the putative fast nuclear AGN winds required for the formation of these large-scale outflows is missing. X-ray observations of blue-shifted Fe K absorption lines directly probe ultra-fast outflows (UFOs) ejected from the AGN accretion disk with v>10,000km/s. A 250ks Suzaku exposure of the ULIRG F11119+3257 with observed extreme molecular/neutral/ionized outflows would allow to characterize the expected UFO, providing the "smoking gun" evidence for feedback driven by AGN winds. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | TOMBESI | FRANCESCO | NULL | NULL | USA | 8 | AO8 | IRAS F11119+3257: THE "SMOKING GUN" EVIDENCE FOR AGN FEEDBACK | XIS | Y |
| VII ZW 403 | 172.0164 | 79.0077 | 127.82558857 | 37.31615306 | 108.8488 | 56627.0107638889 | 56628.7884027778 | 708039010 | 88661.6 | 87000 | 88661.6 | 88661.6 | 0 | 88661.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 87397.4 | 87397.4 | 153557.8 | 1 | PROCESSED | 57613.4969328704 | 57008 | 56639.6396990741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081443 | The source of energetic photons that reionized the early universe remains uncertain. Recently, it has been proposed that X-ray binaries in early galaxies made a significant contribution to reionization. Early galaxies had low metallicity and the best local analogs are blue compact dwarf galaxies (BCDs) with low metallicity. We propose to observe two such galaxies known to be luminous in X-rays and accurately measure their spectra with the Suzaku XIS. These observations are important to our understanding of reionization and the formation of early galaxies. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | KAARET | PHILIP | NULL | NULL | USA | 8 | AO8 | X-RAYS FROM LOW-METALLICITY BLUE COMPACT DWARF GALAXIES | XIS | Y |
| ABELL 981 | 156.0884 | 68.0988 | 140.87577234 | 43.55064218 | 119.4308 | 56601.2179398148 | 56601.7917708333 | 708040010 | 27594.5 | 30000 | 27602.5 | 27594.5 | 0 | 27594.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25286 | 25286 | 49574 | 1 | PROCESSED | 57613.2182060185 | 56980 | 56614.6564583333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081533 | We propose to map out the core of the A981 supercluster with three Suzaku observations. The A981 supercluster contains four Abell richness class 2 clusters within a redshift range of 2,000 km/s. All four clusters also overlap within their virial radii, at least in projection. The low and steady background of the Suzaku telescope is ideal for studying the low surface brightness X-ray emission between the clusters. Such observations will determine if the clusters are interacting via the detection of merger-induced shocks or perturbed features in the outskirts of the individual clusters. Our proposed Suzaku observations will help elucidate the fundamental astrophysics that occurs during the formation of very massive clusters. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | DAVID | LAURENCE | NULL | NULL | USA | 8 | AO8 | MAPPING THE ABELL 981 SUPER CLUSTER WITH SUZAKU | XIS | Y |
| ABELL 998 | 156.5862 | 67.9284 | 140.87284378 | 43.80315875 | 119.4303 | 56601.7924768518 | 56602.9584722222 | 708041010 | 60240.2 | 60000 | 60240.2 | 60240.4 | 0 | 60256.2 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 51856 | 51856 | 100731.9 | 2 | PROCESSED | 57613.2563657407 | 56980 | 56614.6831944444 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081533 | We propose to map out the core of the A981 supercluster with three Suzaku observations. The A981 supercluster contains four Abell richness class 2 clusters within a redshift range of 2,000 km/s. All four clusters also overlap within their virial radii, at least in projection. The low and steady background of the Suzaku telescope is ideal for studying the low surface brightness X-ray emission between the clusters. Such observations will determine if the clusters are interacting via the detection of merger-induced shocks or perturbed features in the outskirts of the individual clusters. Our proposed Suzaku observations will help elucidate the fundamental astrophysics that occurs during the formation of very massive clusters. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | DAVID | LAURENCE | NULL | NULL | USA | 8 | AO8 | MAPPING THE ABELL 981 SUPER CLUSTER WITH SUZAKU | XIS | Y |
| ABELL 1005 | 156.925 | 68.2013 | 140.47803773 | 43.70739533 | 119.4313 | 56609.4953819444 | 56610.8334490741 | 708042010 | 61349.6 | 60000 | 61349.6 | 61349.6 | 0 | 61349.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 58964.5 | 58964.5 | 115599.8 | 2 | PROCESSED | 57613.3284722222 | 56994 | 56625.7198611111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081533 | We propose to map out the core of the A981 supercluster with three Suzaku observations. The A981 supercluster contains four Abell richness class 2 clusters within a redshift range of 2,000 km/s. All four clusters also overlap within their virial radii, at least in projection. The low and steady background of the Suzaku telescope is ideal for studying the low surface brightness X-ray emission between the clusters. Such observations will determine if the clusters are interacting via the detection of merger-induced shocks or perturbed features in the outskirts of the individual clusters. Our proposed Suzaku observations will help elucidate the fundamental astrophysics that occurs during the formation of very massive clusters. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | DAVID | LAURENCE | NULL | NULL | USA | 8 | AO8 | MAPPING THE ABELL 981 SUPER CLUSTER WITH SUZAKU | XIS | Y |
| NGC 3660 | 170.883 | -8.6561 | 269.10006798 | 48.35629614 | 109.6283 | 56624.1463773148 | 56627.0001967593 | 708043010 | 124777.4 | 120000 | 124785.4 | 124785.4 | 0 | 124777.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 109769.2 | 109769.2 | 246543.4 | 2 | PROCESSED | 57613.5216550926 | 57058 | 56691.7534953704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 082003 | We propose a 120-ks observation of NGC 3660, which is a strong candidate for a True Seyfert 2, a Seyfert that intrinsically lacks the broad line regions (BLRs), and challenges the AGN unified scheme. However, a puzzling BeppoSAX observation lingers, which shows excess emission above 10 keV indicative of a Compton thick AGN. Nevertheless, rapid variability below 10 keV and meagre iron line emission (EW=60 eV) strongly argue against this conclusion. Data from the HXD will elucidate the situation, and either dispel this evidence, adding weight to the True Seyfert 2 scenario, or confirm the presence of heavily obscured emission, which may be explained by a partial covering scenario. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | BRIGHTMAN | MURRAY | NULL | NULL | EUR | 8 | AO8 | NGC 3660: A TRUE SEYFERT 2? | XIS | Y |
| B2 1023+25 | 156.5986 | 25.7113 | 207.05661505 | 57.60744793 | 288.3095 | 56442.6428125 | 56444.9133449074 | 708044010 | 100887.4 | 100000 | 100895.4 | 100887.4 | 0 | 100895.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 96578.7 | 96578.7 | 196129.8 | 2 | PROCESSED | 57611.461099537 | 56821 | 56455.8205324074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 082005 | We propose a deep (100 ksec) Suzaku observation of the recently discovered high redshift blazar candidate B2 1023+25 (z=5.3). A very hard (Gamma <2) spectrum would confirm its blazar nature, allowing to study the physical properties of the relativistic jet in this extremely powerful and very high redshift source. The proposed observation will yield an X-ray spectrum of sufficient quality to determine the X-ray shape. The confirmation of a second blazar at this redshift has profound cosmological implications, placing stronger constraints on the number density of high mass BH at high z | EXTRAGALACTIC COMPACT SOURCES | 7 | A | BRAITO | VALENTINA | NULL | NULL | EUR | 8 | AO8 | THE HIGH-REDSHIFT BLAZAR CANDIDATE B2 1023+25 | XIS | Y |
| PG 1404+226 | 211.5907 | 22.3868 | 21.44706338 | 72.36251102 | 287.2346 | 56486.8565972222 | 56489.1889583333 | 708045010 | 102332.7 | 100000 | 102370.4 | 102332.7 | 0 | 102362.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 95340.7 | 95340.7 | 201505.9 | 2 | PROCESSED | 57612.0131828704 | 56872 | 56503.7358796296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 082010 | Suzaku observations reveal evidence of relativistically-broadened emission lines from the inner regions of supermassive black holes, providing a unique tool for studying accreting systems. It is understood that the X-ray source is compact at low-fluxes, and increases in size at higher fluxes. Thus variable sources are essential for probing the physics of the innermost regions. Previous studies of the low-flux 'state' have been limited by low count rates. We propose to observe PG 1404+226, which shares many properties of other AGN showing reverberation, but even at low-fluxes, it is a factor of three brighter than similar objects. This source, never before observed with Suzaku, provides a unique opportunity for probing strong-field accretion because of its high luminosity and variability. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | KARA | ERIN | NULL | NULL | EUR | 8 | AO8 | MAPPING THE X-RAY EMISSION IN THE VICINITY OF THE BLACK HOLE PG 1404+226 | XIS | Y |
| FAIRALL 51 | 281.2238 | -62.3567 | 333.20743511 | -23.0882296 | 252.0031 | 56539.073587963 | 56539.5245486111 | 708046010 | 31557.6 | 30000 | 31557.6 | 31567.6 | 0 | 31565.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25654.9 | 25654.9 | 38955.9 | 0 | PROCESSED | 57612.4964236111 | 56956 | 56587.5110763889 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 082016 | Fairall 51 is a variable bright active galaxy (about 1 millicrab), classified as a polar-scattered Seyfert~1 galaxy. It was observed twice with high-quality X-ray spectrometers on-board the XMM-Newton satellite. The two observations are separated by half a year and the spectra significantly differ from each other. The difference can be well explained by a variable covering fraction of a cold (very low-ionised) absorber (Ricci et al., 2010). Two additional Swift data, separated by five days, suggest that the variability may occur at time-scales as short as a few days. The ultimate goal of the proposal is to locate this variable absorber by the determination of the typical time-scale of the variability. We therefore propose a series of observations of Fairall 51 with short exposures. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | SVOBODA | JIRI | NULL | NULL | EUR | 8 | AO8 | STUDY OF THE VARIABLE ABSORBER IN A BRIGHT ACTIVE GALAXY FAIRALL 51 | XIS | Y |
| FAIRALL 51 | 281.2261 | -62.3592 | 333.20510197 | -23.08989761 | 251.799 | 56540.8073958333 | 56541.1744212963 | 708046020 | 30958 | 30000 | 30958 | 30958 | 0 | 30964.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 23217.1 | 23217.1 | 31703.9 | 0 | PROCESSED | 57612.5333333333 | 56956 | 56588.7741319444 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 082016 | Fairall 51 is a variable bright active galaxy (about 1 millicrab), classified as a polar-scattered Seyfert~1 galaxy. It was observed twice with high-quality X-ray spectrometers on-board the XMM-Newton satellite. The two observations are separated by half a year and the spectra significantly differ from each other. The difference can be well explained by a variable covering fraction of a cold (very low-ionised) absorber (Ricci et al., 2010). Two additional Swift data, separated by five days, suggest that the variability may occur at time-scales as short as a few days. The ultimate goal of the proposal is to locate this variable absorber by the determination of the typical time-scale of the variability. We therefore propose a series of observations of Fairall 51 with short exposures. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | SVOBODA | JIRI | NULL | NULL | EUR | 8 | AO8 | STUDY OF THE VARIABLE ABSORBER IN A BRIGHT ACTIVE GALAXY FAIRALL 51 | XIS | Y |
| FAIRALL 51 | 281.2231 | -62.3584 | 333.20555808 | -23.08834808 | 251.8035 | 56542.816087963 | 56543.4286689815 | 708046030 | 23930.1 | 30000 | 23938.1 | 23943.9 | 0 | 23930.1 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 35650.7 | 35650.7 | 52919.9 | 0 | PROCESSED | 57612.5525694445 | 56990 | 56625.6038078704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 082016 | Fairall 51 is a variable bright active galaxy (about 1 millicrab), classified as a polar-scattered Seyfert~1 galaxy. It was observed twice with high-quality X-ray spectrometers on-board the XMM-Newton satellite. The two observations are separated by half a year and the spectra significantly differ from each other. The difference can be well explained by a variable covering fraction of a cold (very low-ionised) absorber (Ricci et al., 2010). Two additional Swift data, separated by five days, suggest that the variability may occur at time-scales as short as a few days. The ultimate goal of the proposal is to locate this variable absorber by the determination of the typical time-scale of the variability. We therefore propose a series of observations of Fairall 51 with short exposures. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | SVOBODA | JIRI | NULL | NULL | EUR | 8 | AO8 | STUDY OF THE VARIABLE ABSORBER IN A BRIGHT ACTIVE GALAXY FAIRALL 51 | XIS | Y |
| FAIRALL 51 | 281.2285 | -62.3615 | 333.20299178 | -23.09155943 | 253.9697 | 56548.4894444445 | 56549.3146990741 | 708046040 | 30192.6 | 30000 | 30200.6 | 30192.6 | 0 | 30192.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37181.2 | 37181.2 | 71267.9 | 1 | PROCESSED | 57612.6129050926 | 56990 | 56625.6172337963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 082016 | Fairall 51 is a variable bright active galaxy (about 1 millicrab), classified as a polar-scattered Seyfert~1 galaxy. It was observed twice with high-quality X-ray spectrometers on-board the XMM-Newton satellite. The two observations are separated by half a year and the spectra significantly differ from each other. The difference can be well explained by a variable covering fraction of a cold (very low-ionised) absorber (Ricci et al., 2010). Two additional Swift data, separated by five days, suggest that the variability may occur at time-scales as short as a few days. The ultimate goal of the proposal is to locate this variable absorber by the determination of the typical time-scale of the variability. We therefore propose a series of observations of Fairall 51 with short exposures. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | SVOBODA | JIRI | NULL | NULL | EUR | 8 | AO8 | STUDY OF THE VARIABLE ABSORBER IN A BRIGHT ACTIVE GALAXY FAIRALL 51 | XIS | Y |
| SN 2006JD | 120.5317 | 0.8109 | 220.45479917 | 16.05743863 | 101.8795 | 56954.8286458333 | 56958.31125 | 709001010 | 144489.4 | 150000 | 144489.4 | 151036.1 | 0 | 151052.1 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7014351852 | 57435 | 57066.4298032407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090005 | We propose a 150 ks observation of a supernova (SN) 2006jd, a bright SN IIn discovered on October 12, 2006. It is a rare SN that remains bright in X-rays over several years, hence provides us with a rare opportunity to study the dense medium that was ejected by the progenitor star before the SN explosion. Our analysis of archival data taken by Suzaku in 2008 and XMM-Newton in 2009 has indicated interesting spectral evolution, i.e., spectral softening and an increasing centroid of Fe-K lines complex. Our proposed observation will show much clearer spectral variation than that seen in the previous Suzaku and XMM-Newton data, allowing us to understand the details of spectral evolution. The dataset will become a reference for the study of late-time X-ray spectroscopy of SN IIn. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | KATSUDA | SATORU | NULL | NULL | JAP | 9 | AO9 | PROBING LATE-TIME X-RAY SPECTRUM OF SN 2006JD | XIS | Y |
| NGC 3998 | 179.4698 | 55.4443 | 138.19460038 | 60.06850959 | 319.2188 | 56780.8797569445 | 56782.5966898148 | 709002010 | 80675.4 | 80000 | 80675.4 | 80675.4 | 0 | 80675.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 76890.1 | 76890.1 | 148285.8 | 0 | PROCESSED | 57615.0693981482 | 57159 | 56793.5775 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090017 | The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to population synthesis models, its estimate is strongly coupled with the broad band spectral shape of Compton thin AGNs. Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright AGNs that can be best followed-up with Suzaku. Here we propose to observe two of the lowest luminosity BAT AGNs to measure the amount of the reflection component with unpreceded accuracy, a key parameter to determine the contribution of Compton thick AGNs to the X-ray background. We will also study how the torus structure of low luminosity AGNs differs from that of more luminous AGNs. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 9 | AO9 | BROAD BAND SPECTRA OF HARD X-RAY SELECTED VERY LOW LUMINOSITY AGNS AND THEIR TORUS STRUCTURE | XIS | Y |
| NGC 2655 | 133.9038 | 78.2094 | 134.93858201 | 32.69360092 | 275.5561 | 56789.4281828704 | 56791.0731712963 | 709003010 | 76837.1 | 80000 | 76837.1 | 76837.1 | 0 | 76837.1 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 2153.9 | 0 | PROCESSED | 57615.0904398148 | 57173 | 56807.6198726852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090017 | The number of Compton thick AGNs is the biggest issue in the origin of the X-ray background and AGN evolution. According to population synthesis models, its estimate is strongly coupled with the broad band spectral shape of Compton thin AGNs. Swift/BAT has provided the first unbiased AGN sample above 15 keV, which includes many hard X-ray bright AGNs that can be best followed-up with Suzaku. Here we propose to observe two of the lowest luminosity BAT AGNs to measure the amount of the reflection component with unpreceded accuracy, a key parameter to determine the contribution of Compton thick AGNs to the X-ray background. We will also study how the torus structure of low luminosity AGNs differs from that of more luminous AGNs. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 9 | AO9 | BROAD BAND SPECTRA OF HARD X-RAY SELECTED VERY LOW LUMINOSITY AGNS AND THEIR TORUS STRUCTURE | XIS | Y |
| SWIFT J2248.8+1725 | 342.1903 | 17.444 | 85.72592105 | -36.41328844 | 248.2402 | 56997.6938888889 | 56999.668287037 | 709004010 | 78093.8 | 80000 | 78093.8 | 78093.8 | 0 | 78093.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 68826.6 | 68826.6 | 170560 | 1 | PROCESSED | 57617.5240046296 | 57460 | 57092.3224652778 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090018 | We propose to observe two hard X-ray bright Seyfert galaxies with a highly accreting small BH. This class of objects is of importance in studying accretion processes under a large mass accretion rate and therefore mass growth of black holes. Our aims are (1) to measure a continuum shape such as spectral slope and high energy cutoff, (2) to compare them with other classes of AGNs, and (3) to search for highly ionized outflows with a large column density. All of these will be fundamental pieces of information to better understand accretion physics and ``feedback'' processes in galaxies. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | TERASHIMA | YUICHI | NULL | NULL | JAP | 9 | AO9 | ACCRETION AND OUTFLOW IN THE HARD X-RAY SELECTED LOW-MASS SEYFERTS | XIS | Y |
| SWIFT J0544.4-4328 | 86.0099 | -43.419 | 249.50201979 | -30.05213281 | 308.9989 | 57140.9252083333 | 57143.359212963 | 709005010 | 84362 | 100000 | 84362 | 92725.1 | 0 | 92717.1 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57618.0749537037 | 57527 | 57160.6331597222 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090018 | We propose to observe two hard X-ray bright Seyfert galaxies with a highly accreting small BH. This class of objects is of importance in studying accretion processes under a large mass accretion rate and therefore mass growth of black holes. Our aims are (1) to measure a continuum shape such as spectral slope and high energy cutoff, (2) to compare them with other classes of AGNs, and (3) to search for highly ionized outflows with a large column density. All of these will be fundamental pieces of information to better understand accretion physics and ``feedback'' processes in galaxies. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | TERASHIMA | YUICHI | NULL | NULL | JAP | 9 | AO9 | ACCRETION AND OUTFLOW IN THE HARD X-RAY SELECTED LOW-MASS SEYFERTS | XIS | Y |
| SWIFT J0250.7+4142 | 42.6629 | 41.6747 | 145.63636615 | -15.88173015 | 76.5152 | 56872.0541898148 | 56873.8814930556 | 709006010 | 82154.9 | 80000 | 82162.9 | 82162.9 | 0 | 82154.9 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.4596527778 | 57267 | 56902.7258564815 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090019 | Swift/BAT extragalactic survey above E >15 keV has provided us with the first unbiased AGN sample in the local universe. Here we propose to observe two Compton thick AGN candidates in the 70 month BAT catalog with Suzaku. To resolve the degeneracy of spectral modeling, the simultaneous wide-band coverage with the XIS and the HXD is crucial. This will lead us to the first reliable measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. We also aim to construct the template spectra of Compton thick AGNs, applicable to buried AGNs at high redshifts detected in deep surveys. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 9 | AO9 | DETERMINATION OF NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS | XIS | Y |
| SWIFT J0714.2+3518 | 108.5168 | 35.2792 | 182.49455345 | 19.57130625 | 283.6115 | 57116.9939814815 | 57118.9043634259 | 709007010 | 79247.1 | 80000 | 79247.1 | 79247.1 | 0 | 79247.1 | 3 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.9309027778 | 57565 | 57198.4724074074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090019 | Swift/BAT extragalactic survey above E >15 keV has provided us with the first unbiased AGN sample in the local universe. Here we propose to observe two Compton thick AGN candidates in the 70 month BAT catalog with Suzaku. To resolve the degeneracy of spectral modeling, the simultaneous wide-band coverage with the XIS and the HXD is crucial. This will lead us to the first reliable measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. We also aim to construct the template spectra of Compton thick AGNs, applicable to buried AGNs at high redshifts detected in deep surveys. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 9 | AO9 | DETERMINATION OF NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS | XIS | Y |
| ARP318 | 32.3792 | -10.1586 | 173.95964772 | -64.97329044 | 75.9989 | 56873.8890509259 | 56875.8252662037 | 709009010 | 80219.5 | 80000 | 80219.5 | 80219.5 | 0 | 80222 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15381.1 | 15381.1 | 43076 | 0 | PROCESSED | 57616.4808217593 | 57267 | 56898.4603703704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090037 | We propose Suzaku/XIS and PIN observations of nearby two radio-quiet AGNs with very weak mid-infrared emission, which might represent a new class of hot dust free AGNs. We found hot dust free AGN candidates by combining the Swift/BAT hard X-ray all-sky AGN catalog with mid-infrared (MIR) all-sky surveys. Three out of 503 sources are not detected in their MIR bands, even in the high sensitivity of WISE. One source is radio-loud AGNs and the other two radio-quiet sources are also observed in 2-10 keV band with Swift/XRT, and no significant Fe Ka line emission is detected. The scientific goal of this proposal is to obtain the first Fe Ka detection or strong constraints of the emission, which will give us a direct evidence that these sources have very small amount or even lack of torus. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | ICHIKAWA | KOHEI | NULL | NULL | JAP | 9 | AO9 | THE FIRST BROADBAND X-RAY OBSERVATIONS OF HOT DUST FREE AGNS IN THE LOCAL UNIVERSE | XIS | Y |
| NGC2110 | 88.0489 | -7.4533 | 212.92425635 | -16.54269345 | 269.0605 | 57101.7987152778 | 57103.3044328704 | 709011010 | 45625.7 | 50000 | 45625.7 | 49493.6 | 0 | 49509.6 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.8483564815 | 57558 | 57190.4658333333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090062 | We propose to observe the Seyfert galaxy NGC2110 twice every half year, which showed a big flare by a factor of around 5 against the normal state around 2012 December. We can observe the echo history following the flare in a time scale of years, and then measure the reflection spectrum very accurately to constrain the geometry of the reflection torus. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | FUKAZAWA | YASUSHI | NULL | NULL | JAP | 9 | AO9 | X-RAY ECHO OF THE BIG FLARE OF SEYFERT GALAXY NGC2110 | XIS | Y |
| KUV 00311-1938 | 8.3907 | -19.361 | 94.15504043 | -81.21658968 | 60.8243 | 56821.2581481482 | 56822.2384606482 | 709013010 | 41892.6 | 40000 | 41892.6 | 41900.6 | 0 | 41900.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35985.3 | 35985.3 | 84685.8 | 0 | PROCESSED | 57615.2401851852 | 57200 | 56833.588900463 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090088 | Extreme HBL objects are BL Lac objects characterized by their hard TeV gamma-ray spectra, by which the sources are considered as excellent targets to study secondary cascade gamma-ray emission induced by very-high-energy photons or protons from the sources. We propose Suzaku observations of 1ES 0347-121 and KUV 00311-1938 for 60 ks and 40 ks, respectively. The observations can reveal detailed spectral structure around synchrotron peak in the extreme HBLs, which are essential to derive physical parameters such as electron spectrum, magnetic filed strength in the jet. The results will help understating gamma-ray components of both intrinsic jet emission and the secondary cascade emission. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | HAYASHIDA | MASAAKI | NULL | NULL | JAP | 9 | AO9 | SUZAKU OBSERVATIONS OF EXTREME HIGH-FREQUENCY PEAKED BL LAC OBJECTS | XIS | Y |
| NGC 4593 | 189.915 | -5.3482 | 297.48487911 | 57.39893055 | 292.7762 | 56824.1040972222 | 56824.8563888889 | 709014010 | 29761.6 | 30000 | 29769.6 | 29761.6 | 0 | 29769.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 24185 | 24185 | 64991.9 | 1 | PROCESSED | 57615.2408449074 | 57204 | 56835.7291435185 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090097 | In the AO-8 cycle, we proposed six X-ray and optical simultaneous observations of type I Seyfert galaxy NGC 3516, and now obtaining a good correlation between those wavelengths. In the observations, we confirmed that a hard X-ray primary component (HXPC) found in Noda et al. (2013) was dominant, and its variation is well correlated with an optical one. To verify the probability that a variation of HXPC in other Seyfert also correlates with that in its optical, we propose six X-ray and optical simultaneous observations of NGC 4593, which has an X-ray spectrum dominated by HXPC as well as NGC 3516 in 2013. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | NODA | HIROFUMI | NULL | NULL | JAP | 9 | AO9 | X-RAY AND OPTICAL SIMULTANEOUS OBSERVATIONS OF TYPICAL TYPE I SEYFERT NGC 4593 | XIS | Y |
| NGC 4593 | 189.9148 | -5.3464 | 297.48422734 | 57.40070716 | 292.7769 | 56830.338275463 | 56831.0988657407 | 709014020 | 30961 | 30000 | 30977 | 30961 | 0 | 30985 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 30408 | 30408 | 65688 | 0 | PROCESSED | 57615.3154976852 | 57212 | 56846.5106365741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090097 | In the AO-8 cycle, we proposed six X-ray and optical simultaneous observations of type I Seyfert galaxy NGC 3516, and now obtaining a good correlation between those wavelengths. In the observations, we confirmed that a hard X-ray primary component (HXPC) found in Noda et al. (2013) was dominant, and its variation is well correlated with an optical one. To verify the probability that a variation of HXPC in other Seyfert also correlates with that in its optical, we propose six X-ray and optical simultaneous observations of NGC 4593, which has an X-ray spectrum dominated by HXPC as well as NGC 3516 in 2013. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | NODA | HIROFUMI | NULL | NULL | JAP | 9 | AO9 | X-RAY AND OPTICAL SIMULTANEOUS OBSERVATIONS OF TYPICAL TYPE I SEYFERT NGC 4593 | XIS | Y |
| NGC 4593 | 189.9131 | -5.3423 | 297.48045078 | 57.40464867 | 113.7512 | 57006.6309375 | 57007.3023263889 | 709014030 | 30531.2 | 30000 | 30531.2 | 30539.2 | 0 | 30539.2 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.5109722222 | 57383 | 57017.413900463 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090097 | In the AO-8 cycle, we proposed six X-ray and optical simultaneous observations of type I Seyfert galaxy NGC 3516, and now obtaining a good correlation between those wavelengths. In the observations, we confirmed that a hard X-ray primary component (HXPC) found in Noda et al. (2013) was dominant, and its variation is well correlated with an optical one. To verify the probability that a variation of HXPC in other Seyfert also correlates with that in its optical, we propose six X-ray and optical simultaneous observations of NGC 4593, which has an X-ray spectrum dominated by HXPC as well as NGC 3516 in 2013. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | NODA | HIROFUMI | NULL | NULL | JAP | 9 | AO9 | X-RAY AND OPTICAL SIMULTANEOUS OBSERVATIONS OF TYPICAL TYPE I SEYFERT NGC 4593 | XIS | Y |
| NGC 4593 | 189.9133 | -5.3412 | 297.4806457 | 57.40576161 | 111.8999 | 57017.6624421296 | 57021.7640740741 | 709014040 | 130358.4 | 30000 | 130390.4 | 130358.4 | 0 | 130382.4 | 3 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.5950810185 | 57415 | 57049.4551851852 | 3.0.22.44 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090097 | In the AO-8 cycle, we proposed six X-ray and optical simultaneous observations of type I Seyfert galaxy NGC 3516, and now obtaining a good correlation between those wavelengths. In the observations, we confirmed that a hard X-ray primary component (HXPC) found in Noda et al. (2013) was dominant, and its variation is well correlated with an optical one. To verify the probability that a variation of HXPC in other Seyfert also correlates with that in its optical, we propose six X-ray and optical simultaneous observations of NGC 4593, which has an X-ray spectrum dominated by HXPC as well as NGC 3516 in 2013. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | NODA | HIROFUMI | NULL | NULL | JAP | 9 | AO9 | X-RAY AND OPTICAL SIMULTANEOUS OBSERVATIONS OF TYPICAL TYPE I SEYFERT NGC 4593 | XIS | Y |
| NGC 4593 | 189.9132 | -5.341 | 297.48043001 | 57.40595243 | 111.8998 | 57021.7640856482 | 57025.333287037 | 709014050 | 145281.9 | 30000 | 145281.9 | 145303.2 | 0 | 145289.9 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.5760069445 | 57415 | 57049.4542939815 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090097 | In the AO-8 cycle, we proposed six X-ray and optical simultaneous observations of type I Seyfert galaxy NGC 3516, and now obtaining a good correlation between those wavelengths. In the observations, we confirmed that a hard X-ray primary component (HXPC) found in Noda et al. (2013) was dominant, and its variation is well correlated with an optical one. To verify the probability that a variation of HXPC in other Seyfert also correlates with that in its optical, we propose six X-ray and optical simultaneous observations of NGC 4593, which has an X-ray spectrum dominated by HXPC as well as NGC 3516 in 2013. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | NODA | HIROFUMI | NULL | NULL | JAP | 9 | AO9 | X-RAY AND OPTICAL SIMULTANEOUS OBSERVATIONS OF TYPICAL TYPE I SEYFERT NGC 4593 | XIS | Y |
| HOLMBERG IX X-1 | 149.4599 | 69.05 | 141.95121201 | 41.07533054 | 294.5528 | 56780.1586111111 | 56780.8752546296 | 709015010 | 31886 | 30000 | 31886 | 31886 | 0 | 31886 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30861.8 | 30861.8 | 61915.9 | 0 | PROCESSED | 57615.0271990741 | 57218 | 56852.5963194444 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091251 | Broadband X-ray spectroscopy of ultraluminous X-ray sources (ULXs) with NuSTAR and Suzaku has begun to provide important information regarding the nature of these enigmatic sources. Recent NuSTAR observations of the extreme ULX Holmberg IX X-1 revealed unusual spectral variability, and different competing evolutionary scenarios can explain the available data. Resolving this degeneracy is critical to determining the nature of the accretion onto this source, and requires multi-epoch broadband spectroscopy probing a more diverse range of fluxes. We propose to undertake 4x30 ks coordinated Suzaku+NuSTAR observations of Holmberg IX X-1 to provide the additional spectra needed to robustly determine the nature of the observed evolution, providing a vital step in our understanding of extreme ULXs. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | WALTON | DOMINIC | NULL | NULL | USA | 9 | AO9 | MULTI-EPOCH BROADBAND X-RAY SPECTROSCOPY OF HOLMBERG IX X-1 WITH SUZAKU AND NUSTAR | XIS | Y |
| HOLMBERG IX X-1 | 149.4756 | 69.0751 | 141.91985765 | 41.06519535 | 104.8942 | 56976.7425347222 | 56977.5230787037 | 709015020 | 34128.1 | 30000 | 34128.1 | 34128.1 | 0 | 34128.1 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7878240741 | 57359 | 56993.4304513889 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091251 | Broadband X-ray spectroscopy of ultraluminous X-ray sources (ULXs) with NuSTAR and Suzaku has begun to provide important information regarding the nature of these enigmatic sources. Recent NuSTAR observations of the extreme ULX Holmberg IX X-1 revealed unusual spectral variability, and different competing evolutionary scenarios can explain the available data. Resolving this degeneracy is critical to determining the nature of the accretion onto this source, and requires multi-epoch broadband spectroscopy probing a more diverse range of fluxes. We propose to undertake 4x30 ks coordinated Suzaku+NuSTAR observations of Holmberg IX X-1 to provide the additional spectra needed to robustly determine the nature of the observed evolution, providing a vital step in our understanding of extreme ULXs. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | WALTON | DOMINIC | NULL | NULL | USA | 9 | AO9 | MULTI-EPOCH BROADBAND X-RAY SPECTROSCOPY OF HOLMBERG IX X-1 WITH SUZAKU AND NUSTAR | XIS | Y |
| HOLMBERG IX X-1 | 149.4572 | 69.0544 | 141.94722641 | 41.07197433 | 311.5038 | 57118.9110416667 | 57119.5667708333 | 709015030 | 31526.3 | 30000 | 31526.3 | 31526.3 | 0 | 31526.3 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.9243402778 | 57513 | 57129.4193171296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091251 | Broadband X-ray spectroscopy of ultraluminous X-ray sources (ULXs) with NuSTAR and Suzaku has begun to provide important information regarding the nature of these enigmatic sources. Recent NuSTAR observations of the extreme ULX Holmberg IX X-1 revealed unusual spectral variability, and different competing evolutionary scenarios can explain the available data. Resolving this degeneracy is critical to determining the nature of the accretion onto this source, and requires multi-epoch broadband spectroscopy probing a more diverse range of fluxes. We propose to undertake 4x30 ks coordinated Suzaku+NuSTAR observations of Holmberg IX X-1 to provide the additional spectra needed to robustly determine the nature of the observed evolution, providing a vital step in our understanding of extreme ULXs. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | WALTON | DOMINIC | NULL | NULL | USA | 9 | AO9 | MULTI-EPOCH BROADBAND X-RAY SPECTROSCOPY OF HOLMBERG IX X-1 WITH SUZAKU AND NUSTAR | XIS | Y |
| HOLMBERG IX X-1 | 149.4663 | 69.0509 | 141.94846823 | 41.07666025 | 284.4995 | 57158.2357291667 | 57159.0827546296 | 709015040 | 34120 | 30000 | 34120 | 34128 | 0 | 34128 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57618.6575347222 | 57536 | 57168.6253935185 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091251 | Broadband X-ray spectroscopy of ultraluminous X-ray sources (ULXs) with NuSTAR and Suzaku has begun to provide important information regarding the nature of these enigmatic sources. Recent NuSTAR observations of the extreme ULX Holmberg IX X-1 revealed unusual spectral variability, and different competing evolutionary scenarios can explain the available data. Resolving this degeneracy is critical to determining the nature of the accretion onto this source, and requires multi-epoch broadband spectroscopy probing a more diverse range of fluxes. We propose to undertake 4x30 ks coordinated Suzaku+NuSTAR observations of Holmberg IX X-1 to provide the additional spectra needed to robustly determine the nature of the observed evolution, providing a vital step in our understanding of extreme ULXs. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | WALTON | DOMINIC | NULL | NULL | USA | 9 | AO9 | MULTI-EPOCH BROADBAND X-RAY SPECTROSCOPY OF HOLMBERG IX X-1 WITH SUZAKU AND NUSTAR | XIS | Y |
| SBS 1301+540 | 196.0153 | 53.8063 | 118.79430047 | 63.22042238 | 133.9261 | 56991.9979976852 | 56994.5141435185 | 709018010 | 94317.6 | 100000 | 94317.6 | 95157.6 | 0 | 95173.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 105464.1 | 105464.1 | 217349.8 | 5 | PROCESSED | 57617.4634143518 | 57451 | 57084.1361574074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091411 | We propose to carry out Suzaku observations, 100 ks each, of two Seyfert I nuclei, IGR J16558-5203 and SBS 1301+540, hard X-ray selected by Swift. Our goal is to distinguish between various competing models proposed for the X-ray spectra of Seyfert I nuclei. Specifically we will explore the effects of strong gravity, by testing the ionized relativistic reflection (hereafter IRR) and by measuring the spin of the black hole. We will take advantage of Suzaku s excellent capability in the broad bands from the soft through medium to hard X-ray bands. With our proposed studies we will gain deeper understanding of accretion-powered AGN in general. | EXTRAGALACTIC COMPACT SOURCES | 7 | C | TSURUTA | SACHIKO | NULL | NULL | USA | 9 | AO9 | SPECTRAL STUDIES OF SOME HARD X RAY SELECTED SEYFERT NUCLEI | XIS | Y |
| Q0142-100 | 26.3171 | -9.7556 | 161.63610788 | -68.48152364 | 68.9469 | 56854.9601041667 | 56856.4794328704 | 709019010 | 60975.1 | 55000 | 60983.1 | 60983.1 | 0 | 60975.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10530 | 10530 | 22736 | 0 | PROCESSED | 57615.4077083333 | 57261 | 56895.341412037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091431 | The origin of AGN iron K alpha emission has been debated for two decades. We propose to constrain iron line emission sizes using quasar X-ray microlensing. Our Chandra Cycle 11 observations have shown that the iron line equivalent widths (EWs) in six lensed systems are significantly higher than those measured in local AGNs. This implies that the iron line emission is microlensed more strongly than the X-ray continuum and originates from very compact regions. We propose to confirm the high iron line EWs in lensed quasars by monitoring two more lenses, Q0142-100 and HE0512+3329 using Suzaku, with a total exposure time 115 kilo-seconds. This will provide independent constraints for settling the debate on the origin of the iron line emission. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | CHEN | BIN | NULL | NULL | USA | 9 | AO9 | CONSTRAINING QUASAR IRON LINE EMISSION USING MICROLENSING | XIS | Y |
| HE0512-3329 | 78.5402 | -33.4449 | 236.63398617 | -33.8579138 | 105.1284 | 56932.4291435185 | 56932.6252083333 | 709020010 | 6864.9 | 60000 | 6873 | 6872.9 | 0 | 6864.9 | 3 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.600474537 | 57345 | 56979.403125 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091431 | The origin of AGN iron K alpha emission has been debated for two decades. We propose to constrain iron line emission sizes using quasar X-ray microlensing. Our Chandra Cycle 11 observations have shown that the iron line equivalent widths (EWs) in six lensed systems are significantly higher than those measured in local AGNs. This implies that the iron line emission is microlensed more strongly than the X-ray continuum and originates from very compact regions. We propose to confirm the high iron line EWs in lensed quasars by monitoring two more lenses, Q0142-100 and HE0512+3329 using Suzaku, with a total exposure time 115 kilo-seconds. This will provide independent constraints for settling the debate on the origin of the iron line emission. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | CHEN | BIN | NULL | NULL | USA | 9 | AO9 | CONSTRAINING QUASAR IRON LINE EMISSION USING MICROLENSING | XIS | Y |
| HE0512-3329 | 78.54 | -33.4465 | 236.6358247 | -33.85842065 | 104.8837 | 56933.2970833333 | 56934.0071180556 | 709020020 | 27508.6 | 60000 | 27508.6 | 27516.6 | 0 | 27516.6 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.6104976852 | 57345 | 56979.4110300926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091431 | The origin of AGN iron K alpha emission has been debated for two decades. We propose to constrain iron line emission sizes using quasar X-ray microlensing. Our Chandra Cycle 11 observations have shown that the iron line equivalent widths (EWs) in six lensed systems are significantly higher than those measured in local AGNs. This implies that the iron line emission is microlensed more strongly than the X-ray continuum and originates from very compact regions. We propose to confirm the high iron line EWs in lensed quasars by monitoring two more lenses, Q0142-100 and HE0512+3329 using Suzaku, with a total exposure time 115 kilo-seconds. This will provide independent constraints for settling the debate on the origin of the iron line emission. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | CHEN | BIN | NULL | NULL | USA | 9 | AO9 | CONSTRAINING QUASAR IRON LINE EMISSION USING MICROLENSING | XIS | Y |
| HE0512-3329 | 78.5445 | -33.4308 | 236.61833373 | -33.85137764 | 251.0519 | 57071.9701388889 | 57072.4937847222 | 709020030 | 25095.5 | 26000 | 25095.5 | 25095.5 | 0 | 25095.5 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.6171296296 | 57457 | 57087.4623726852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091431 | The origin of AGN iron K alpha emission has been debated for two decades. We propose to constrain iron line emission sizes using quasar X-ray microlensing. Our Chandra Cycle 11 observations have shown that the iron line equivalent widths (EWs) in six lensed systems are significantly higher than those measured in local AGNs. This implies that the iron line emission is microlensed more strongly than the X-ray continuum and originates from very compact regions. We propose to confirm the high iron line EWs in lensed quasars by monitoring two more lenses, Q0142-100 and HE0512+3329 using Suzaku, with a total exposure time 115 kilo-seconds. This will provide independent constraints for settling the debate on the origin of the iron line emission. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | CHEN | BIN | NULL | NULL | USA | 9 | AO9 | CONSTRAINING QUASAR IRON LINE EMISSION USING MICROLENSING | XIS | Y |
| I ZW 18 | 143.5064 | 55.23 | 160.54065348 | 44.84408453 | 279.2158 | 56792.4911111111 | 56792.8568402778 | 709021010 | 17261.2 | 100000 | 17261.2 | 17261.2 | 0 | 17261.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16549 | 16549 | 31127.9 | 0 | PROCESSED | 57615.102650463 | 57358 | 56818.6775347222 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091441 | The source of energetic photons that reionized and heated the early universe remains uncertain. Early galaxies had low metallicity and the best local analogs are blue compact dwarf galaxies (BCDs) with low metallicity. We propose to observe two such galaxies known to be luminous in X-rays and accurately measure their spectrum with the Suzaku XIS. These observations are important to our understanding of the heating of the universe during the epoch of reionization. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | KAARET | PHILIP | NULL | NULL | USA | 9 | AO9 | X-RAYS FROM LOW-METALLICITY BLUE COMPACT DWARF GALAXIES | XIS | Y |
| I ZW 18 | 143.5151 | 55.2494 | 160.51246258 | 44.84288886 | 130.2629 | 56934.0191666667 | 56935.6258680556 | 709021020 | 82070.8 | 70000 | 82070.8 | 82086.8 | 0 | 82086.8 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.6143865741 | 57358 | 56989.5111689815 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091441 | The source of energetic photons that reionized and heated the early universe remains uncertain. Early galaxies had low metallicity and the best local analogs are blue compact dwarf galaxies (BCDs) with low metallicity. We propose to observe two such galaxies known to be luminous in X-rays and accurately measure their spectrum with the Suzaku XIS. These observations are important to our understanding of the heating of the universe during the epoch of reionization. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | KAARET | PHILIP | NULL | NULL | USA | 9 | AO9 | X-RAYS FROM LOW-METALLICITY BLUE COMPACT DWARF GALAXIES | XIS | Y |
| MARKARIAN 3 | 93.8921 | 71.0501 | 143.28202475 | 22.71957945 | 87.4437 | 56931.9222337963 | 56932.4181597222 | 709022010 | 23831 | 20000 | 23831 | 23831 | 0 | 23837.6 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.5994328704 | 57345 | 56979.4072569444 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 092008 | We propose to measure size and distance from the black hole of the optically-thick absorbing and reprocessing system(s) in the heavily obscured Seyfert Galaxy Markarian~3 by means of its known X-ray spectral variability. We aim at simultaneously measuring: the variability timescale of the primary emission, seen in transmission through a photoelectric column density of (0.7--1.1)x10^{24} atoms/cm/cm; the variability timescale of its Compton-reflection, dominating the continuum flux in the 3-10 keV energy band; and the variability timescale of the nuclear obscuration. Only the scientific payload on-board Suzaku possesses the required combination of broadband X-ray coverage, sensitivity, and spectroscopic capabilities to perform this experiment. We request 5 observations of 20 ks each. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GUAINAZZI | MATTEO | NULL | NULL | EUR | 9 | AO9 | MEASURING THE TORUS SPATIAL SCALE(S) IN SEYFERT GALAXIES: A SUZAKU MONITORING OF MARKARIAN 3 | XIS | Y |
| MARKARIAN 3 | 93.8907 | 71.0457 | 143.28642165 | 22.71781378 | 80.3638 | 56937.8059953704 | 56938.0751967593 | 709022020 | 17727.7 | 20000 | 17735.7 | 17735.7 | 0 | 17727.7 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.6163078704 | 57358 | 56992.4094560185 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 092008 | We propose to measure size and distance from the black hole of the optically-thick absorbing and reprocessing system(s) in the heavily obscured Seyfert Galaxy Markarian~3 by means of its known X-ray spectral variability. We aim at simultaneously measuring: the variability timescale of the primary emission, seen in transmission through a photoelectric column density of (0.7--1.1)x10^{24} atoms/cm/cm; the variability timescale of its Compton-reflection, dominating the continuum flux in the 3-10 keV energy band; and the variability timescale of the nuclear obscuration. Only the scientific payload on-board Suzaku possesses the required combination of broadband X-ray coverage, sensitivity, and spectroscopic capabilities to perform this experiment. We request 5 observations of 20 ks each. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GUAINAZZI | MATTEO | NULL | NULL | EUR | 9 | AO9 | MEASURING THE TORUS SPATIAL SCALE(S) IN SEYFERT GALAXIES: A SUZAKU MONITORING OF MARKARIAN 3 | XIS | Y |
| MARKARIAN 3 | 93.8812 | 71.0496 | 143.28137914 | 22.71605454 | 71.2169 | 56953.1510532407 | 56953.6731828704 | 709022030 | 22746.1 | 20000 | 22754.1 | 22754.1 | 0 | 22746.1 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.6616087963 | 57376 | 57010.3833217593 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 092008 | We propose to measure size and distance from the black hole of the optically-thick absorbing and reprocessing system(s) in the heavily obscured Seyfert Galaxy Markarian~3 by means of its known X-ray spectral variability. We aim at simultaneously measuring: the variability timescale of the primary emission, seen in transmission through a photoelectric column density of (0.7--1.1)x10^{24} atoms/cm/cm; the variability timescale of its Compton-reflection, dominating the continuum flux in the 3-10 keV energy band; and the variability timescale of the nuclear obscuration. Only the scientific payload on-board Suzaku possesses the required combination of broadband X-ray coverage, sensitivity, and spectroscopic capabilities to perform this experiment. We request 5 observations of 20 ks each. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GUAINAZZI | MATTEO | NULL | NULL | EUR | 9 | AO9 | MEASURING THE TORUS SPATIAL SCALE(S) IN SEYFERT GALAXIES: A SUZAKU MONITORING OF MARKARIAN 3 | XIS | Y |
| MARKARIAN 3 | 93.9187 | 71.0301 | 143.30552616 | 22.72176381 | 268.1895 | 57104.2423148148 | 57104.6266550926 | 709022040 | 23518 | 20000 | 23518 | 23526 | 0 | 23526 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.8399305556 | 57486 | 57119.4206018518 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 092008 | We propose to measure size and distance from the black hole of the optically-thick absorbing and reprocessing system(s) in the heavily obscured Seyfert Galaxy Markarian~3 by means of its known X-ray spectral variability. We aim at simultaneously measuring: the variability timescale of the primary emission, seen in transmission through a photoelectric column density of (0.7--1.1)x10^{24} atoms/cm/cm; the variability timescale of its Compton-reflection, dominating the continuum flux in the 3-10 keV energy band; and the variability timescale of the nuclear obscuration. Only the scientific payload on-board Suzaku possesses the required combination of broadband X-ray coverage, sensitivity, and spectroscopic capabilities to perform this experiment. We request 5 observations of 20 ks each. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GUAINAZZI | MATTEO | NULL | NULL | EUR | 9 | AO9 | MEASURING THE TORUS SPATIAL SCALE(S) IN SEYFERT GALAXIES: A SUZAKU MONITORING OF MARKARIAN 3 | XIS | Y |
| MARKARIAN 3 | 93.9093 | 71.025 | 143.30979342 | 22.71730777 | 267.1766 | 57116.4730902778 | 57116.9877199074 | 709022050 | 21455.6 | 20000 | 21455.6 | 21455.6 | 0 | 21455.6 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.9089814815 | 57550 | 57183.6622916667 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 092008 | We propose to measure size and distance from the black hole of the optically-thick absorbing and reprocessing system(s) in the heavily obscured Seyfert Galaxy Markarian~3 by means of its known X-ray spectral variability. We aim at simultaneously measuring: the variability timescale of the primary emission, seen in transmission through a photoelectric column density of (0.7--1.1)x10^{24} atoms/cm/cm; the variability timescale of its Compton-reflection, dominating the continuum flux in the 3-10 keV energy band; and the variability timescale of the nuclear obscuration. Only the scientific payload on-board Suzaku possesses the required combination of broadband X-ray coverage, sensitivity, and spectroscopic capabilities to perform this experiment. We request 5 observations of 20 ks each. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | GUAINAZZI | MATTEO | NULL | NULL | EUR | 9 | AO9 | MEASURING THE TORUS SPATIAL SCALE(S) IN SEYFERT GALAXIES: A SUZAKU MONITORING OF MARKARIAN 3 | XIS | Y |
| SN 1978K | 49.5382 | -66.5402 | 283.41338803 | -44.62366671 | 13.2585 | 56804.2369097222 | 56806.5279398148 | 709023010 | 107313.6 | 100000 | 107321.6 | 107321.6 | 0 | 107313.6 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.1724074074 | 57234 | 56866.7205092593 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 094341 | SN 1978K is a remarkable Type IIn supernova that remains bright at X-ray through radio wavelengths 35 years after its explosion. Our ongoing multiwavelength observations probe the dense medium that was ejected by the progenitor star, possibly a Luminous Blue Variable. While the radio flux dropped steadily, the X-ray and UV/optical fluxes remained surprisingly constant for a decade. However, our most recent XMM observation in 2013 June reveals a significant fading compared to the 2006 Oct Suzaku observation. Here we request a 100 ksec observation to study the spectral evolution during the decay. This will serve as a pathfinder for younger Type IIn supernovae. As secondary science, we will obtain data on the ULXs X-1 and X-2, and the other luminous sources in NGC 1313. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | SMITH | IAN | KOBAYASHI | SHOGO | USJ | 9 | AO9 | STUDYING THE LATE-TIME DECAY OF SN 1978K | XIS | Y |
| QSO 1222+216 | 186.229 | 21.3887 | 255.03812277 | 81.66761796 | 123.6044 | 56988.9003125 | 56989.2953240741 | 709025010 | 13400.2 | 15000 | 0 | 0 | 0 | 13400.2 | 0 | 0 | 0 | 2 | 1 | 0 | 0 | 12047.4 | 12047.4 | 31435.9 | 0 | PROCESSED | 57617.406099537 | 57368 | 57002.0161111111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 092023 | NULL | EXTRAGALACTIC COMPACT SOURCES | 7 | C | LANGEJAHN | MARCUS | NULL | NULL | EUR | 9 | AO9 | false | XIS | Y |
| QSO 1222+216 | 186.2289 | 21.3877 | 255.04256268 | 81.66684682 | 123.6039 | 56989.2953356482 | 56989.4064583333 | 709025020 | 527.2 | 15000 | 535.2 | 527.2 | 0 | 808.8 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.4022222222 | 57368 | 57002.4417361111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 092023 | NULL | EXTRAGALACTIC COMPACT SOURCES | 7 | C | LANGEJAHN | MARCUS | NULL | NULL | EUR | 9 | AO9 | false | XIS | Y |
| QSO 1828+487 | 277.4042 | 48.7379 | 77.22058509 | 23.48843965 | 218.1356 | 56983.2742592593 | 56983.6771875 | 709026010 | 14176.6 | 15000 | 14176.6 | 14176.6 | 0 | 14176.6 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.8008912037 | 57442 | 57076.4104861111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 092023 | NULL | EXTRAGALACTIC COMPACT SOURCES | 7 | C | LANGEJAHN | MARCUS | NULL | NULL | EUR | 9 | AO9 | false | XIS | Y |
| MKN 6 | 103.0685 | 74.413 | 140.3435691 | 26.1094153 | 254.4482 | 57133.5883333333 | 57134.7015046296 | 710001010 | 50654.1 | 50000 | 50654.1 | 51339.6 | 0 | 51339.6 | 3 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57618.0317476852 | 57548 | 57154.4415162037 | 3.0.22.44 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 101730 | We request two quasi-simultaneous NuSTAR + Suzaku-XIS pointings of the radio-loud Sy 1.5 Mkn 6 to understand the complexity of its accreting circumnuclear gas structures. A series of high-quality, broadband X-ray spectra, including coverage above 10 keV, are needed to properly quantify the variable and complex line of sight absorbers. These new observations, in conjunction with radio and previous X-ray observations, will be a unique opportunity to understand accretion modes in the innermost regions of a radio-loud AGN that has recently undergone a merger. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | MARKOWITZ | ALEX | NULL | NULL | USA | 10 | AO10 | COMPLEX CIRCUMNUCLEAR ABSORPTION IN RADIO-LOUD AGN: VARIABLE ABSORPTION IN MKN 6 | XIS | Y |
| NGC 2788A | 135.6754 | -68.2181 | 284.17134554 | -14.14937336 | 282.2863 | 57157.0478819444 | 57158.2230324074 | 710007010 | 42233.9 | 40000 | 42233.9 | 42233.9 | 0 | 42233.9 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57618.6656828704 | 57591 | 57224.447650463 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 100009 | Swift/BAT extragalactic survey above E >15 keV has provided us with the first unbiased AGN sample in the local universe. Here we propose to observe four Compton thick AGN candidates in the 70 month BAT catalog with Suzaku. Since their spectra below 10 keV are likely reflection dominated, joint analysis of Suzaku/XIS and Swift/BAT can constrain the absorption and intrinsic luminosity without being much affected by time variability. This will lead us to the first reliable measurement of the fraction of Compton thick AGNs and column density distribution, which are key parameters in the population synthesis of the X-ray background. We also aim to construct the template spectra of Compton thick AGNs, applicable to buried AGNs at high redshifts detected in deep survey. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | UEDA | YOSHIHIRO | NULL | NULL | JAP | 10 | AO10 | DETERMINATION OF NUMBER DENSITY AND TEMPLATE SPECTRA OF COMPTON THICK AGNS | XIS | Y |
| NGC 3516 | 166.6817 | 72.5579 | 133.24892211 | 42.40929053 | 306.0068 | 57154.3345023148 | 57157.0348611111 | 710009010 | 117701.2 | 120000 | 117701.2 | 123003.2 | 0 | 124763.2 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57618.6915277778 | 57593 | 57224.4439467593 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 100040 | In the AO-8 cycle, we have proposed several X-ray and optical simultaneous observations of a type I Seyfert galaxy NGC 3516, and obtained a good correlation between those wavelengths in its faint phase. The result suggests that a hard primary X-ray continua found in NGC 3516 by Noda et al. (2013) is generated in a corona formed closely to an accretion disk, which is possibly a radiatively inefficient accretion flow. As a next step, we examine whether or not an X-ray variation is also correlated with that in optical, when NGC 3516 is in the bright phase, and the other primary X-ray continuum, also reported by Noda et al. (2013), is dominant. For it, we propose an X-ray and optical simultaneous observation of NGC 3516 with an exposure of 120 ksec, which is triggered by a Swift monitoring. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | NODA | HIROFUMI | NULL | NULL | JAP | 10 | AO10-TOO | X-RAY AND OPTICAL SIMULTANEOUS OBSERVATIONS OF NGC 3516 IN ITS BRIGHT PHASE | XIS | Y |
| OJ 287 | 133.7046 | 20.1043 | 206.8173824 | 35.82032681 | 285.8742 | 57145.5508449074 | 57148.4467592593 | 710011010 | 111638.8 | 323000 | 111638.8 | 111638.8 | 0 | 111638.8 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57618.1122800926 | 57113 | 57164.5257523148 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 101431 | Kepler will observe OJ 287 with 1 min sampling and >90% duty cycle for ~75 days in 2015, providing an unprecedented opportunity to quantitatively compare optical and X-ray variations in one of the brightest and most active blazars in the sky. We request continuous Suzaku coverage for 128 orbits (323 ks) in a simultaneous campaign including XMM, Swift, radio and multi-color optical monitoring. Suzaku samples key intermediate timescales of hours-days, allowing measurement of CCFs and PSDs spanning a wide range of temporal frequencies. These will be used to test models and determine source parameters e.g. if the X-rays are due to synchrotron-self Compton the optical should lead the X-rays by ~1 day, but if they are "synchrotron flashes" the bands should vary nearly simultaneously. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | EDELSON | RICK | NULL | NULL | USA | 10 | AO10 | SIMULTANEOUS SUZAKU/KEPLER/MULTIWAVELENGTH MONITORING OF OJ 287 | XIS | Y |
| OJ 287 | 133.705 | 20.1043 | 206.81753743 | 35.82068078 | 285.8744 | 57148.4467708333 | 57151.4189351852 | 710011020 | 110281.9 | 323000 | 110281.9 | 112309.9 | 0 | 112309.9 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57618.1271643518 | 57113 | 57164.5272337963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 101431 | Kepler will observe OJ 287 with 1 min sampling and >90% duty cycle for ~75 days in 2015, providing an unprecedented opportunity to quantitatively compare optical and X-ray variations in one of the brightest and most active blazars in the sky. We request continuous Suzaku coverage for 128 orbits (323 ks) in a simultaneous campaign including XMM, Swift, radio and multi-color optical monitoring. Suzaku samples key intermediate timescales of hours-days, allowing measurement of CCFs and PSDs spanning a wide range of temporal frequencies. These will be used to test models and determine source parameters e.g. if the X-rays are due to synchrotron-self Compton the optical should lead the X-rays by ~1 day, but if they are "synchrotron flashes" the bands should vary nearly simultaneously. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | EDELSON | RICK | NULL | NULL | USA | 10 | AO10 | SIMULTANEOUS SUZAKU/KEPLER/MULTIWAVELENGTH MONITORING OF OJ 287 | XIS | Y |
| OJ 287 | 133.7049 | 20.1044 | 206.81738245 | 35.82062575 | 285.8744 | 57151.4189467593 | 57154.3266666667 | 710011030 | 107714.3 | 323000 | 107714.3 | 107714.3 | 0 | 107714.3 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57618.6879166667 | 57113 | 57164.5596527778 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 101431 | Kepler will observe OJ 287 with 1 min sampling and >90% duty cycle for ~75 days in 2015, providing an unprecedented opportunity to quantitatively compare optical and X-ray variations in one of the brightest and most active blazars in the sky. We request continuous Suzaku coverage for 128 orbits (323 ks) in a simultaneous campaign including XMM, Swift, radio and multi-color optical monitoring. Suzaku samples key intermediate timescales of hours-days, allowing measurement of CCFs and PSDs spanning a wide range of temporal frequencies. These will be used to test models and determine source parameters e.g. if the X-rays are due to synchrotron-self Compton the optical should lead the X-rays by ~1 day, but if they are "synchrotron flashes" the bands should vary nearly simultaneously. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | EDELSON | RICK | NULL | NULL | USA | 10 | AO10 | SIMULTANEOUS SUZAKU/KEPLER/MULTIWAVELENGTH MONITORING OF OJ 287 | XIS | Y |
| M81 | 148.8829 | 69.0533 | 142.10623941 | 40.90540672 | 287.1391 | 57160.4721180556 | 57162.9807523148 | 710017010 | 97702.2 | 100000 | 97702.2 | 99738 | 0 | 99744.4 | 3 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 300 | 0 | PROCESSED | 57618.7210532407 | 57543 | 57177.3710300926 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 102700 | We propose to observe the Low-Luminosity Active Galactic Nucleus of M81 for 200 ksec with NuSTAR and for 100 ksec with Suzaku. In low accretion rate AGN, where does the optically thick part of the accretion disk stop? Does it go in to within a few gravitational radii of the black hole, as in higher accretion rate Seyfert galaxies, or does it stop hundreds of gravitational radii from the black hole? Using NuSTAR and Suzaku spectra we will measure the strengths of the Compton reflection hump, Fe K alpha, Fe XXV and Fe XXVI lines. This will determine whether the Fe K alpha line is produced by reflection off the optically thick outer disk, or is produced in the optically thin inner flow. We will measure the reflection fraction and constrain the source geometry and disk transition radius. | EXTRAGALACTIC COMPACT SOURCES | 7 | A | YOUNG | ANDREW | NULL | NULL | EUR | 10 | AO10 | M81: ACCRETION GEOMETRY AT LOW EDDINGTON RATES | XIS | Y |
| ARK 564 | 340.6583 | 29.7351 | 92.13955378 | -25.32593551 | 75.7895 | 57167.0898842593 | 57168.4029282407 | 710018010 | 52510.4 | 50000 | 52510.4 | 53934.4 | 0 | 53934.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27980.2 | 27980.2 | 100947.7 | 2 | PROCESSED | 57618.7636921296 | 57548 | 57178.248587963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 102721 | A NuSTAR legacy is emerging through long observations of bare Seyfert galaxies that reveal an unprecedented look at relativistic reflection off an ionized accretion disc. We propose now to look at the Seyfert galaxy Ark 564 for 200 ks with NuSTAR and 50 ks with Suzaku in order to understand the reflection in this bright source. Ark 564 has been well-studied in the soft band, revealing a steep spectrum, strong soft excess, broad iron K emission line and dramatic variability on the order of hours. It is very akin to two other well-known bare Seyferts, 1H0707-405 and IRAS 13224-3809, except it is an order of magnitude brighter. With this 200 ks observation, we will probe the geometry of the corona, through a complete spectral and timing analysis. | EXTRAGALACTIC COMPACT SOURCES | 7 | B | KARA | ERIN | NULL | NULL | EUR | 10 | AO10 | UNDERSTANDING REFLECTION IN THE BARE SEYFERT I ARK 564 | XIS | Y |
| A1413 | 178.8303 | 23.6485 | 225.18767075 | 76.86550896 | 123.0348 | 53689.8362847222 | 53692.5939699074 | 800001010 | 107867.2 | 100000 | 107867.2 | 108003.2 | 107947.2 | 107910.3 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 102431.5 | 102431.5 | 238239.7 | 7 | PROCESSED | 57528.0427546296 | 54247 | 54038.1136689815 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001010 | No cluster has had its X-ray temperature measured out to the virial radius. Hence no cluster has had it total mass measured using X-ray methods. Typically these measurements extend only to 60% of the virial radius. We propose to perform these measurements for the first time and with high accuracy for the relaxed cluster A1413. The low Suzaku background permits us to make this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | HENRY | J. | NULL | NULL | JAP | 0 | SWG | CLUSTER TEMPERATURE AND MASS MEASUREMENT TO THE VIRIAL RADIUS | XIS | N |
| FORNAX CLUSTER NORTH | 54.7022 | -35.2276 | 236.33819165 | -53.57399329 | 245.0013 | 53740.3046990741 | 53740.493275463 | 800002010 | 7763.5 | 80000 | 7763.5 | 7763.5 | 7763.5 | 7763.5 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 8270.8 | 8270.8 | 16271.9 | 0 | PROCESSED | 57532.6205324074 | 54247 | 54039.6718518518 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001018 | The center of the Fornax cluster was observed with Suzaku with a 80 ks exposure. We have detected excess hard-emission and derived O abundances of the ISM of NGC 1399 and NGC 1404, and the intracluster medium (ICM). Here, we propose to observe two offset pointings of the Fornax cluster for 160 ks (80 ks times 2) to study the distribution of the hard emission and the abundance distribution of O, Mg, Si, S and Fe. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MATSUSHITA | KYOKO | NULL | NULL | JAP | 0 | SWG | MAPPING HARD EXCESS EMISSION AND OXYGEN IN THE INTRACLUSTER MEDIUM OF THE FORNAX CLUSTER | NULL | N |
| FORNAX CLUSTER NORTH | 54.7043 | -35.2293 | 236.34100564 | -53.57224957 | 244.9996 | 53741.5137847222 | 53742.3336111111 | 800002020 | 37192.1 | 80000 | 37192.1 | 37216.1 | 37208.1 | 37200.1 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 39287.4 | 39287.4 | 70815.9 | 1 | PROCESSED | 57532.6432291667 | 54247 | 54039.8151041667 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001018 | The center of the Fornax cluster was observed with Suzaku with a 80 ks exposure. We have detected excess hard-emission and derived O abundances of the ISM of NGC 1399 and NGC 1404, and the intracluster medium (ICM). Here, we propose to observe two offset pointings of the Fornax cluster for 160 ks (80 ks times 2) to study the distribution of the hard emission and the abundance distribution of O, Mg, Si, S and Fe. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MATSUSHITA | KYOKO | NULL | NULL | JAP | 0 | SWG | MAPPING HARD EXCESS EMISSION AND OXYGEN IN THE INTRACLUSTER MEDIUM OF THE FORNAX CLUSTER | XIS | N |
| FORNAX CLUSTER NORTH | 54.7043 | -35.2294 | 236.34117402 | -53.57224789 | 244.9993 | 53749.1506134259 | 53750.3265509259 | 800002030 | 45575 | 80000 | 45583 | 45579 | 45575 | 45587 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 42571.3 | 42571.3 | 101600 | 1 | PROCESSED | 57532.6714236111 | 54247 | 54039.9702777778 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001018 | The center of the Fornax cluster was observed with Suzaku with a 80 ks exposure. We have detected excess hard-emission and derived O abundances of the ISM of NGC 1399 and NGC 1404, and the intracluster medium (ICM). Here, we propose to observe two offset pointings of the Fornax cluster for 160 ks (80 ks times 2) to study the distribution of the hard emission and the abundance distribution of O, Mg, Si, S and Fe. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MATSUSHITA | KYOKO | NULL | NULL | JAP | 0 | SWG | MAPPING HARD EXCESS EMISSION AND OXYGEN IN THE INTRACLUSTER MEDIUM OF THE FORNAX CLUSTER | XIS | N |
| A1060 | 159.1744 | -27.531 | 269.60056717 | 26.48279097 | 103.6438 | 53696.6258796296 | 53697.7211111111 | 800003010 | 39139 | 40000 | 39139 | 39147 | 39155 | 39155 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 34602.4 | 34602.4 | 94625.9 | 1 | PROCESSED | 57528.0675462963 | 54247 | 54037.8583449074 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001021 | A1060 is a bright non cD cluster and gives us a unique opportunity to study injection process of metals in the intracluster space. Reliable measurement of oxygen distribution with XIS will tell us whether the metals produced by Type-II supernova (mainly oxygen) ditributes over a different scale compared with the SN-Ia product (Fe). A1060 is the best cluster where we can directly observe distribution of metals produced by general cluster galaxies. Also, central increase of temperature by 20%, probably connected with motions of bright central galaxies, suggests that non-thermal X-rays may be produced. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | OHASHI | TAKAYA | NULL | NULL | JAP | 0 | SWG | OXYGEN DISTRIBUTION AND CENTRAL GAS FEATURES OF A1060 | XIS | N |
| A1060 OFFSET | 159.5124 | -27.532 | 269.88117164 | 26.64663217 | 96.4857 | 53694.9817708333 | 53696.6231365741 | 800004010 | 52402.5 | 60000 | 52402.5 | 53202.5 | 52418.5 | 52538.5 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 46203.9 | 46203.9 | 141801.8 | 1 | PROCESSED | 57528.0764583333 | 54247 | 54038.1216666667 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001021 | A1060 is a bright non cD cluster and gives us a unique opportunity to study injection process of metals in the intracluster space. Reliable measurement of oxygen distribution with XIS will tell us whether the metals produced by Type-II supernova (mainly oxygen) ditributes over a different scale compared with the SN-Ia product (Fe). A1060 is the best cluster where we can directly observe distribution of metals produced by general cluster galaxies. Also, central increase of temperature by 20%, probably connected with motions of bright central galaxies, suggests that non-thermal X-rays may be produced. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | OHASHI | TAKAYA | NULL | NULL | JAP | 0 | SWG | OXYGEN DISTRIBUTION AND CENTRAL GAS FEATURES OF A1060 | XIS | N |
| ABELL2811 | 10.4703 | -28.5552 | 358.34166022 | -87.45073592 | 232.1065 | 53702.1678240741 | 53702.8814699074 | 800005010 | 30654.6 | 25000 | 30662.6 | 30682.6 | 30654.6 | 30665.9 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 28325.4 | 28325.4 | 61656 | 0 | PROCESSED | 57528.0937268518 | 54247 | 54038.5109722222 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001025 | We propose to observe the central region of the Sculptor supercluster at z=0.11, in a search for the theoretically predicted Warm/Hot Intergalactic Medium (WHIM). The WHIM has been 'missing' observationally, until recent detection of the X-ray absorption due to the ionized light elements in the background quasar spectra. Still there is no confident detection of the expected soft X-ray emission. This is mainly because that the X-ray brightness is very low, compared to the Galactic diffuse emission in the soft X-ray band and/or the spectral sensitivity of previous experiments are limited. To separate the expected X-ray lines of the WHIM (mainly O VII) from the Galactic emission, we select an unique supercluster at z>0.1. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | TAMURA | TAKAYUKI | NULL | NULL | JAP | 0 | SWG | THE SCULPTOR SUPERCLUSTER: SEARCH FOR THE WARM/HOT INTERGALACTIC MEDIUM | XIS | N |
| ABELL2811-OFF | 10.1781 | -28.7333 | 358.19144602 | -87.13859798 | 232.6526 | 53702.8821296296 | 53703.731412037 | 800006010 | 33949.4 | 25000 | 33957.4 | 33965.4 | 33949.4 | 33949.8 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 30905.6 | 30905.6 | 73365.9 | 1 | PROCESSED | 57528.1125115741 | 54247 | 54038.6719560185 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001025 | We propose to observe the central region of the Sculptor supercluster at z=0.11, in a search for the theoretically predicted Warm/Hot Intergalactic Medium (WHIM). The WHIM has been 'missing' observationally, until recent detection of the X-ray absorption due to the ionized light elements in the background quasar spectra. Still there is no confident detection of the expected soft X-ray emission. This is mainly because that the X-ray brightness is very low, compared to the Galactic diffuse emission in the soft X-ray band and/or the spectral sensitivity of previous experiments are limited. To separate the expected X-ray lines of the WHIM (mainly O VII) from the Galactic emission, we select an unique supercluster at z>0.1. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | TAMURA | TAKAYUKI | NULL | NULL | JAP | 0 | SWG | THE SCULPTOR SUPERCLUSTER: SEARCH FOR THE WARM/HOT INTERGALACTIC MEDIUM | XIS | N |
| ABELL2804 | 9.8968 | -28.9096 | 357.98440451 | -86.83577265 | 234.7036 | 53706.3688078704 | 53707.166875 | 800007010 | 31612.9 | 25000 | 31612.9 | 31612.9 | 31612.9 | 31612.9 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 26914.5 | 26914.5 | 68950 | 2 | PROCESSED | 57532.3559259259 | 54247 | 54038.8727893518 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001025 | We propose to observe the central region of the Sculptor supercluster at z=0.11, in a search for the theoretically predicted Warm/Hot Intergalactic Medium (WHIM). The WHIM has been 'missing' observationally, until recent detection of the X-ray absorption due to the ionized light elements in the background quasar spectra. Still there is no confident detection of the expected soft X-ray emission. This is mainly because that the X-ray brightness is very low, compared to the Galactic diffuse emission in the soft X-ray band and/or the spectral sensitivity of previous experiments are limited. To separate the expected X-ray lines of the WHIM (mainly O VII) from the Galactic emission, we select an unique supercluster at z>0.1. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | TAMURA | TAKAYUKI | NULL | NULL | JAP | 0 | SWG | THE SCULPTOR SUPERCLUSTER: SEARCH FOR THE WARM/HOT INTERGALACTIC MEDIUM | XIS | N |
| ABELL2801 | 9.6433 | -29.1188 | 357.12193154 | -86.53506096 | 232.0377 | 53701.3547106482 | 53702.1668865741 | 800008010 | 34890 | 25000 | 34890 | 34890 | 34890 | 34890 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 30163.6 | 30163.6 | 70163.9 | 1 | PROCESSED | 57528.0891898148 | 54247 | 54038.3717361111 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001025 | We propose to observe the central region of the Sculptor supercluster at z=0.11, in a search for the theoretically predicted Warm/Hot Intergalactic Medium (WHIM). The WHIM has been 'missing' observationally, until recent detection of the X-ray absorption due to the ionized light elements in the background quasar spectra. Still there is no confident detection of the expected soft X-ray emission. This is mainly because that the X-ray brightness is very low, compared to the Galactic diffuse emission in the soft X-ray band and/or the spectral sensitivity of previous experiments are limited. To separate the expected X-ray lines of the WHIM (mainly O VII) from the Galactic emission, we select an unique supercluster at z>0.1. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | TAMURA | TAKAYUKI | NULL | NULL | JAP | 0 | SWG | THE SCULPTOR SUPERCLUSTER: SEARCH FOR THE WARM/HOT INTERGALACTIC MEDIUM | XIS | N |
| NGC720 | 28.2529 | -13.7362 | 173.01572713 | -70.35499124 | 242.5294 | 53734.3673611111 | 53739.5627546296 | 800009010 | 177192.9 | 100000 | 177192.9 | 177192.9 | 177192.9 | 177192.9 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 9662.1 | 9662.1 | 47540.8 | 0 | PROCESSED | 57532.602962963 | 54247 | 54039.6651736111 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001031 | We propose to observe an isolated elliptical galaxy NGC720 with Suzaku. Isolated elliptical galaxies are important to probe the ISM metal abundance, since their hot gas is not affected by the amibient bright intracluster medium which often exists around X-ray bright elliptical galaxies. Suzaku is expected to measure the Oxygen abundance in the ISM bettern than XMM-Newton and constrain the origin of metals in the ISM and also ICM. Dark matter content around elliptical galaxies can also be constrained better than XMM-Newton. Such a measurement is difficult for X-ray bright galaxies due to the superposition of the cluster potential. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | FUKAZAWA | YASUSHI | NULL | NULL | JAP | 0 | SWG | OXYGEN ABUNDANCE AND DARK MATTER CONTENT AROUDN AN ISOLATED ELLIPTICAL GALAXY NGC720 | XIS | N |
| A426 | 49.9554 | 41.5039 | 150.58326426 | -13.26576669 | 260.2176 | 53767.568900463 | 53768.5294560185 | 800010010 | 50398.6 | 50000 | 50406.6 | 50406.6 | 50398.6 | 50406.6 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 54436.4 | 54436.4 | 82975.8 | 0 | PROCESSED | 57532.8781365741 | 54247 | 54041.0862152778 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001036 | A426 is the X-ray brightest cluster in the Sky. The core is X-ray peaked, has a short radiative cooling time, a temperature drop and a central radio source which is blowing bubbles in the intracluster medium. A radio minihalo extends over the central 6 arcmin. A coincident power-law component is seen in deep Chandra data. This is likely to be inverse Compton emission from the electron population responsible for the radio emission. The region is expected to be a luminous, extended, hard X-ray source easily detectable by the Suzaku HXD. Confirmation of this hard X-ray component will enable the magnetic field to be securely determined in the intracluster gas. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | FABIAN | ANDREW | NULL | NULL | JAP | 0 | SWG | THE HARD X-RAY FLUX FROM THE CORE OF THE PERSEUS CLUSTER | XIS | N |
| A3376 WEST RELIC | 90.0415 | -39.9946 | 246.43569548 | -26.38071178 | 132.0018 | 53681.5938078704 | 53684.7883912037 | 800011010 | 126996.9 | 150000 | 126996.9 | 127180.9 | 127076.9 | 127028.9 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 112911.3 | 112911.3 | 230939.7 | 3 | PROCESSED | 57528.0013541667 | 54247 | 54037.6050231482 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001039 | We propose a 150 ks observation of the giant radio relic in the west of the A3376 cluster. A3376 is a low temperature (4.5 keV) cluster with possible excess hard X-ray emission in 2.7 sigma significance by Beppo-SAX, and also with a pair of giant radio relics. This target is best suited for cluster hard excess survey with HXD. Following the first observation planned around October 2005 located near the east relic, the observation of the west relic 23 arcmin away can bring us the first spacial information on cluster excess hard X-rays. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | NAKAZAWA | KAZUHIRO | NULL | NULL | JAP | 0 | SWG | SEARCH FOR EXCESS HARD X-RAY EMISSION FROM ABELL 3376 | XIS | N |
| A3376 WEST RELIC | 90.0363 | -39.9917 | 246.43145562 | -26.38385089 | 126.3601 | 54034.3950231482 | 54035.9176388889 | 800011020 | 62264.8 | 60000 | 62264.8 | 62264.8 | 62264.8 | 62264.8 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 55562.9 | 55562.9 | 131537.8 | 2 | PROCESSED | 57535.9705902778 | 54694 | 54090.2671643518 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001039 | We propose a 150 ks observation of the giant radio relic in the west of the A3376 cluster. A3376 is a low temperature (4.5 keV) cluster with possible excess hard X-ray emission in 2.7 sigma significance by Beppo-SAX, and also with a pair of giant radio relics. This target is best suited for cluster hard excess survey with HXD. Following the first observation planned around October 2005 located near the east relic, the observation of the west relic 23 arcmin away can bring us the first spacial information on cluster excess hard X-rays. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | NAKAZAWA | KAZUHIRO | NULL | NULL | JAP | 0 | SWG | SEARCH FOR EXCESS HARD X-RAY EMISSION FROM ABELL 3376 | HXD | Y |
| ABELL 1795 | 207.2241 | 26.601 | 33.84733119 | 77.1817764 | 130.8638 | 53714.5034259259 | 53714.7752199074 | 800012010 | 13098.2 | 120000 | 13106.2 | 13098.2 | 13106.2 | 13106.2 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 10375.9 | 10375.9 | 23463.9 | 1 | PROCESSED | 57532.3922453704 | 54247 | 54038.7903703704 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001056 | We propose a 120 ks Suzaku observation of Abell 1795. Five overlapping XIS pointings will: i) map the temperature to the virial radius for the first time; ii) check for the presence of soft excess emission and, if found, possibly determine whether the excess is associated with the cluster or our Galaxy; and iii) determine the run of abundance with radius in detail at r< 500. This observation will demonstrate the scientific value of the low-background and good spectral resolution of the Suzaku XIS in cluster studies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | BAUTZ | MARK | NULL | NULL | JAP | 0 | SWG | TEMPERATURE, MASS AND SOFT-EXCESS MAPS TO THE VIRIAL RADIUS IN ABELL 1795 | XIS | N |
| ABELL 1795 Near North | 207.2221 | 26.7993 | 34.737463 | 77.20142043 | 130.7334 | 53714.7756481482 | 53715.3203587963 | 800012020 | 24410.6 | 25000 | 24426.6 | 24410.6 | 24442.6 | 24434.6 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 25179.8 | 25179.8 | 47055.9 | 2 | PROCESSED | 57532.404375 | 54247 | 54038.8804166667 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001056 | We propose a 120 ks Suzaku observation of Abell 1795. Five overlapping XIS pointings will: i) map the temperature to the virial radius for the first time; ii) check for the presence of soft excess emission and, if found, possibly determine whether the excess is associated with the cluster or our Galaxy; and iii) determine the run of abundance with radius in detail at r< 500. This observation will demonstrate the scientific value of the low-background and good spectral resolution of the Suzaku XIS in cluster studies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | BAUTZ | MARK | NULL | NULL | JAP | 0 | SWG | TEMPERATURE, MASS AND SOFT-EXCESS MAPS TO THE VIRIAL RADIUS IN ABELL 1795 | XIS | N |
| ABELL 1795 Far North | 207.223 | 26.9995 | 35.63943573 | 77.21561208 | 130.4264 | 53715.3208796296 | 53715.9730092593 | 800012030 | 30640.6 | 30000 | 30648.6 | 30640.6 | 30663.9 | 30656.6 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 27883.3 | 27883.3 | 56337.9 | 1 | PROCESSED | 57532.4195833333 | 54247 | 54039.1003703704 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001056 | We propose a 120 ks Suzaku observation of Abell 1795. Five overlapping XIS pointings will: i) map the temperature to the virial radius for the first time; ii) check for the presence of soft excess emission and, if found, possibly determine whether the excess is associated with the cluster or our Galaxy; and iii) determine the run of abundance with radius in detail at r< 500. This observation will demonstrate the scientific value of the low-background and good spectral resolution of the Suzaku XIS in cluster studies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | BAUTZ | MARK | NULL | NULL | JAP | 0 | SWG | TEMPERATURE, MASS AND SOFT-EXCESS MAPS TO THE VIRIAL RADIUS IN ABELL 1795 | XIS | N |
| ABELL 1795 Near South | 207.2228 | 26.4007 | 32.94964182 | 77.16185549 | 129.833 | 53715.9739467593 | 53716.5355787037 | 800012040 | 26074 | 25000 | 26098 | 26091.9 | 26074 | 26086 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 25798.6 | 25798.6 | 48522 | 1 | PROCESSED | 57532.4329282407 | 54247 | 54039.0706018518 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001056 | We propose a 120 ks Suzaku observation of Abell 1795. Five overlapping XIS pointings will: i) map the temperature to the virial radius for the first time; ii) check for the presence of soft excess emission and, if found, possibly determine whether the excess is associated with the cluster or our Galaxy; and iii) determine the run of abundance with radius in detail at r< 500. This observation will demonstrate the scientific value of the low-background and good spectral resolution of the Suzaku XIS in cluster studies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | BAUTZ | MARK | NULL | NULL | JAP | 0 | SWG | TEMPERATURE, MASS AND SOFT-EXCESS MAPS TO THE VIRIAL RADIUS IN ABELL 1795 | XIS | N |
| ABELL 1795 Far South | 207.2227 | 26.2001 | 32.0541753 | 77.13779505 | 129.4115 | 53716.5361921296 | 53717.4168865741 | 800012050 | 40120.6 | 30000 | 40136.6 | 40152.6 | 40120.6 | 40136.6 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 39437.3 | 39437.3 | 76081.9 | 1 | PROCESSED | 57532.4477314815 | 54247 | 54039.1460069445 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001056 | We propose a 120 ks Suzaku observation of Abell 1795. Five overlapping XIS pointings will: i) map the temperature to the virial radius for the first time; ii) check for the presence of soft excess emission and, if found, possibly determine whether the excess is associated with the cluster or our Galaxy; and iii) determine the run of abundance with radius in detail at r< 500. This observation will demonstrate the scientific value of the low-background and good spectral resolution of the Suzaku XIS in cluster studies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | BAUTZ | MARK | NULL | NULL | JAP | 0 | SWG | TEMPERATURE, MASS AND SOFT-EXCESS MAPS TO THE VIRIAL RADIUS IN ABELL 1795 | XIS | N |
| HCG62 | 193.274 | -9.2022 | 303.62256693 | 53.66732525 | 113.6407 | 53755.3883333333 | 53758.5002199074 | 800013020 | 114848.8 | 100000 | 114856.8 | 114848.8 | 114848.8 | 114856.8 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 98783.6 | 98783.6 | 268849.8 | 4 | PROCESSED | 57532.7777199074 | 54247 | 54040.4546064815 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001057 | We propose to obtain high-quality spectra of the X-ray brightest, compact group of galaxies HCG62 with Suzaku. The previous ASCA observation has reported that this group has a hard tail in the spectrum. With 100 ksec exposure, we can constrain the flux of the hard component above ~3 keV with much higher accuracy. This will give a great impact in understanding the origin of the hard emission and non-thermal populations in the IGM. Furhtermore determining the metal abundance, particularly Oxygen, in the central and outer regions will give us new, valuable information on metal enrichment processes in the group that is not dominated by a cD galaxy. Suzaku/XIS is the best-suited for our scientific objectives since it has a low background level and the unprecedented high sensitivity. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | OTA | NAOMI | NULL | NULL | JAP | 0 | SWG | MEASURING HARD TAILS AND METAL DISTRIBUTIONS IN THE GALAXY GROUP HCG62 | XIS | N |
| CENTAURUS CLUSTER | 192.2012 | -41.3132 | 302.40029759 | 21.55583076 | 106.2442 | 53731.2579050926 | 53732.1808333333 | 800014010 | 36519.2 | 30000 | 36519.2 | 36546.4 | 36546.4 | 36522.4 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 32149.8 | 32149.8 | 79739.9 | 0 | PROCESSED | 57532.5349652778 | 54247 | 54039.373900463 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001070 | A dramatic central concentration of iron and silicon is present in the Centaurus cluster. Apart from this well-recognized contribution from Type Ia supernova, enrichment process due to Type II supernova is poorly understood. Centaurus cluster is most suited for the study of large-scale oxygen distribution, for which XIS is most sensitive. The XIS data will give us a key knowledge about how past Type II supernova have affected the enrichment process. The data would also confirm that the central gas is a mixture of hot and cool components with much better sensitivity than before. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | FUKAZAWA | YASUSHI | NULL | NULL | JAP | 0 | SWG | OXYGEN DISTRIBUTION AND MIXTURE OF HOT AND COOL GAS IN THE CENTAURUS CLUSTER | XIS | N |
| CENCL OFFSET1 | 192.2015 | -41.4461 | 302.40210867 | 21.42294125 | 106.2765 | 53732.1811689815 | 53733.2502199074 | 800015010 | 44880.2 | 40000 | 44896.2 | 44904.2 | 44880.2 | 44919.6 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 37226.7 | 37226.7 | 92347.8 | 2 | PROCESSED | 57532.5827893518 | 54247 | 54039.5403472222 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001070 | A dramatic central concentration of iron and silicon is present in the Centaurus cluster. Apart from this well-recognized contribution from Type Ia supernova, enrichment process due to Type II supernova is poorly understood. Centaurus cluster is most suited for the study of large-scale oxygen distribution, for which XIS is most sensitive. The XIS data will give us a key knowledge about how past Type II supernova have affected the enrichment process. The data would also confirm that the central gas is a mixture of hot and cool components with much better sensitivity than before. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | FUKAZAWA | YASUSHI | NULL | NULL | JAP | 0 | SWG | OXYGEN DISTRIBUTION AND MIXTURE OF HOT AND COOL GAS IN THE CENTAURUS CLUSTER | XIS | N |
| CENCL OFFSET2 | 192.2009 | -41.1804 | 302.39848339 | 21.68862024 | 106.52 | 53733.2507407407 | 53734.3543865741 | 800016010 | 43277.3 | 40000 | 43285.3 | 43285.3 | 43277.3 | 43293.3 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 35253.1 | 35253.1 | 95332 | 1 | PROCESSED | 57532.5900578704 | 54247 | 54039.6041203704 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001070 | A dramatic central concentration of iron and silicon is present in the Centaurus cluster. Apart from this well-recognized contribution from Type Ia supernova, enrichment process due to Type II supernova is poorly understood. Centaurus cluster is most suited for the study of large-scale oxygen distribution, for which XIS is most sensitive. The XIS data will give us a key knowledge about how past Type II supernova have affected the enrichment process. The data would also confirm that the central gas is a mixture of hot and cool components with much better sensitivity than before. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | FUKAZAWA | YASUSHI | NULL | NULL | JAP | 0 | SWG | OXYGEN DISTRIBUTION AND MIXTURE OF HOT AND COOL GAS IN THE CENTAURUS CLUSTER | XIS | N |
| NGC4388 | 186.4461 | 12.6674 | 279.11809751 | 74.34084148 | 119.622 | 53728.3779976852 | 53731.250162037 | 800017010 | 123634.1 | 100000 | 123924.9 | 125814.3 | 123634.1 | 124152.3 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 111820.9 | 111820.9 | 248128 | 3 | PROCESSED | 57532.5484143518 | 54247 | 54039.5984375 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001077 | Large-scale X-ray nebulae up to a few tens of kpc have been often found in starburst galaxies, which is thermally heated up by the superwind from the starburst nucleus. Iwasawa et al. (2003) found a large X-ray nebula up to 16kpc around NGC4388, which is photoiionized by Seyfert nucleus. Thus, this result suggests that the hard X-ray emission from active galactic nucleus could be a prime heat source of nebula. The goals of this observation are (1) to see how far the X-ray nebula is extended, (2) to obtain its precise X-ray spectrum, (3) to determine what is the X-ray emission mechanism, and (4) to exam if the photoionization by AGN could be a prime heat source of the galactic halo. We determine the photon index and the high energy cut-off of the power-law component from the HXD spectrum. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | TSURU | TAKESHI | NULL | NULL | JAP | 0 | SWG | VERY EXTENDED PHOTOIONIZED X-RAY NEBULA AROUND THE SEYFERT GALAXY NGC4388 | XIS | N |
| NGC 4636 | 190.7243 | 2.7556 | 297.77503713 | 65.54179663 | 112.2967 | 53710.1073726852 | 53711.9446643518 | 800018010 | 79201 | 80000 | 79201 | 79201 | 79201 | 79201 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 75777.1 | 75777.1 | 158727.8 | 2 | PROCESSED | 57532.4099421296 | 54247 | 54038.9551388889 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001083 | We propose to observe NGC 4636 for 50~ksec in a single pointing, to determine the chemical evolution of elliptical galaxies via the determination of the spatially resolved abundance of Oxygen and other elements. Being one of the most X-ray luminous ellipticals, and having been observed by both Chandra and XMM, this is also an important target to compare the capabilities of the three observatories and interpret the results of the Suzaku XIS in light of the source spectrum provided by the XMM RGS. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | FIGUEROA-FELICIANO | ENECTALI | NULL | NULL | JAP | 0 | SWG | OBSERVATION OF THE X-RAY LUMINOUS EXTENDED EARLY-TYPE GALAXY NGC 4636 | XIS | N |
| A 2218 CENTER | 249.0052 | 66.205 | 97.72589248 | 38.11630228 | 233.3294 | 53669.4904050926 | 53670.1905555556 | 800019010 | 31935.4 | 35000 | 31943.4 | 31943.4 | 31935.4 | 31943.4 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 28937.1 | 28937.1 | 60487.9 | 1 | PROCESSED | 57527.6471990741 | 54247 | 54036.9596990741 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001096 | To confirm the presence of redshifted oxygen lines from the WHIM surrounding A2218, we propose observations of 2 positions. One is a 35 ksec pointing on A2218 to raise the photon statistics of the oxygen feature, and the other is a 15 ksec pointing at about 1 degree west of the cluster to know the amplitude of the intensity variation of the Galactic oxygen lines. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | OHASHI | TAKAYA | NULL | NULL | JAP | 0 | SWG | SEARCH FOR OXYGEN LINES FROM WARM IGM | NULL | N |
| A 2218 OFFSETB | 249.9091 | 65.2119 | 96.37864193 | 38.09205953 | 233.3309 | 53670.1916319444 | 53670.4620833333 | 800020010 | 14921.5 | 15000 | 14937.5 | 14933.5 | 14921.5 | 14941.5 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 14193.1 | 14193.1 | 23356.1 | 0 | PROCESSED | 57527.6596180556 | 54247 | 54036.8343981482 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001096 | To confirm the presence of redshifted oxygen lines from the WHIM surrounding A2218, we propose observations of 2 positions. One is a 35 ksec pointing on A2218 to raise the photon statistics of the oxygen feature, and the other is a 15 ksec pointing at about 1 degree west of the cluster to know the amplitude of the intensity variation of the Galactic oxygen lines. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | OHASHI | TAKAYA | NULL | NULL | JAP | 0 | SWG | SEARCH FOR OXYGEN LINES FROM WARM IGM | NULL | N |
| NGC 2403 | 114.2007 | 65.5918 | 150.58117971 | 29.1798975 | 310.3004 | 53810.5896875 | 53811.5884143518 | 800021010 | 72368.7 | 70000 | 72376.7 | 72368.7 | 72376.7 | 72376.7 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 59359.1 | 59359.1 | 86277.9 | 0 | PROCESSED | 57533.2480439815 | 54247 | 54042.0667708333 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001101 | We propose to observe NGC 2403, which is a nearby luminous normal spiral. Our main objective is to search and investigation of diffuse emission components. These include both rather soft (kT = 0.1 - 1 keV) ones already detected from a fair number of spirals, and hot (kT = a few keV) emission which, if established, may become an analogue to the Galactic ridge emission. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MAKISHIMA | KAZUO | NULL | NULL | JAP | 0 | SWG | A PROPOSAL FOR A 70 KSEC SUZAKU OBSERVATION OF THE NORMAL SPIRAL GALAXY NGC 2403 | XIS | N |
| A2104W | 234.9146 | -3.2969 | 2.73337641 | 39.30878407 | 117.9077 | 54121.3401388889 | 54121.8960532407 | 801001010 | 19926.9 | 20000 | 19926.9 | 19926.9 | 0 | 19926.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17200.1 | 17200.1 | 48007.9 | 2 | PROCESSED | 57536.8971875 | 54735 | 54137.0936805556 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010012 | We propose to perform spatially resolved spectroscopy on relaxed clusters of galaxies A2104, A963 and A2261 to map their temperature out to the virial radius r_178 with 15% precision at 90% CL in a few arcmin scale. Combined with Chandra imaging of these clusters, the proposed measurements will be used for accurate virial and baryonic mass estimation assuming hydrostatic equilibrium. We use this information to calibrate the cluster M-T and L-T scaling relations, and their evolution. We will constrain the cosmological parameters Omega_M and Omega_Lambda via the baryonic fraction and the mass function. Due to the stable and low background of XIS detectors, with Suzaku it is possible to perform this challenging and cosmologically important task. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | HATTORI | MAKOTO | NULL | NULL | JAP | 1 | AO1 | TEMPERATURE PROFILES OF RELAXED CLUSTERS OF GALAXIES OUT TO VIRIAL RADIUS | XIS | Y |
| A2104N | 235.0318 | -3.1802 | 2.94593816 | 39.29281704 | 117.689 | 54119.2779166667 | 54119.7522337963 | 801002010 | 18842.4 | 20000 | 18842.4 | 18842.4 | 0 | 18842.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13644.8 | 13644.8 | 40977.9 | 1 | PROCESSED | 57536.8705439815 | 54735 | 54133.3893518518 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010012 | We propose to perform spatially resolved spectroscopy on relaxed clusters of galaxies A2104, A963 and A2261 to map their temperature out to the virial radius r_178 with 15% precision at 90% CL in a few arcmin scale. Combined with Chandra imaging of these clusters, the proposed measurements will be used for accurate virial and baryonic mass estimation assuming hydrostatic equilibrium. We use this information to calibrate the cluster M-T and L-T scaling relations, and their evolution. We will constrain the cosmological parameters Omega_M and Omega_Lambda via the baryonic fraction and the mass function. Due to the stable and low background of XIS detectors, with Suzaku it is possible to perform this challenging and cosmologically important task. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | HATTORI | MAKOTO | NULL | NULL | JAP | 1 | AO1 | TEMPERATURE PROFILES OF RELAXED CLUSTERS OF GALAXIES OUT TO VIRIAL RADIUS | XIS | Y |
| A2104E | 235.1486 | -3.297 | 2.9252225 | 39.1285511 | 117.6908 | 54118.1261226852 | 54118.6850231482 | 801003010 | 22784.7 | 20000 | 22784.7 | 22784.7 | 0 | 22784.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17735.2 | 17735.2 | 48287.9 | 1 | PROCESSED | 57536.8549189815 | 54735 | 54132.8631365741 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010012 | We propose to perform spatially resolved spectroscopy on relaxed clusters of galaxies A2104, A963 and A2261 to map their temperature out to the virial radius r_178 with 15% precision at 90% CL in a few arcmin scale. Combined with Chandra imaging of these clusters, the proposed measurements will be used for accurate virial and baryonic mass estimation assuming hydrostatic equilibrium. We use this information to calibrate the cluster M-T and L-T scaling relations, and their evolution. We will constrain the cosmological parameters Omega_M and Omega_Lambda via the baryonic fraction and the mass function. Due to the stable and low background of XIS detectors, with Suzaku it is possible to perform this challenging and cosmologically important task. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | HATTORI | MAKOTO | NULL | NULL | JAP | 1 | AO1 | TEMPERATURE PROFILES OF RELAXED CLUSTERS OF GALAXIES OUT TO VIRIAL RADIUS | XIS | Y |
| A2104S | 235.0317 | -3.4139 | 2.71321412 | 39.14413145 | 117.9978 | 54120.3324884259 | 54120.8266087963 | 801004010 | 17323.4 | 20000 | 17323.4 | 17323.4 | 0 | 17323.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13829.1 | 13829.1 | 42681.9 | 1 | PROCESSED | 57536.8854166667 | 54750 | 54137.3891898148 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010012 | We propose to perform spatially resolved spectroscopy on relaxed clusters of galaxies A2104, A963 and A2261 to map their temperature out to the virial radius r_178 with 15% precision at 90% CL in a few arcmin scale. Combined with Chandra imaging of these clusters, the proposed measurements will be used for accurate virial and baryonic mass estimation assuming hydrostatic equilibrium. We use this information to calibrate the cluster M-T and L-T scaling relations, and their evolution. We will constrain the cosmological parameters Omega_M and Omega_Lambda via the baryonic fraction and the mass function. Due to the stable and low background of XIS detectors, with Suzaku it is possible to perform this challenging and cosmologically important task. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | HATTORI | MAKOTO | NULL | NULL | JAP | 1 | AO1 | TEMPERATURE PROFILES OF RELAXED CLUSTERS OF GALAXIES OUT TO VIRIAL RADIUS | XIS | Y |
| RX J1347.5-1145 | 206.856 | -11.8093 | 323.97916756 | 48.76108187 | 292.056 | 53916.7756597222 | 53918.7600115741 | 801013010 | 69661.1 | 75000 | 69661.1 | 69661.1 | 69661.1 | 69661.1 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 60982 | 60982 | 171375.9 | 0 | PROCESSED | 57534.8555671296 | 54394 | 53926.4810300926 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010014 | We propose to obtain broad-band spectra of the most X-ray luminous cluster of galaxies RXJ1347.5-1145 at z=0.45. Our previous high-resolution Sunyaev-Zel'dovich obvervations of this cluster revealed that it exhibits an unusually violent merger activity. Its high X-ray luminosity ensures the unprecedented high-quality spectra with Suzaku. It is indeed a unique target to probe gas physics and particle acceleration mechanism associated with the violent mergers at high redshift. The continuum observations with HXD and XIS as well as the iron line spectroscopy will specify the physical states of both thermal and non-thermal components of the ICM. Combined with the Chandra and our SZ data, the Suzaku data will accomplish the first comprehensive modeling of a violent merger in distant clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | OTA | NAOMI | NULL | NULL | JAP | 1 | AO1 | BROAD-BAND SPECTROSCOPY OF THE MOST X-RAY LUMINOUS CLUSTER OF GALAXIES RXJ1347.5-1145 AT Z=0.45 | HXD | N |
| RX J1347.5-1145 | 206.8558 | -11.8095 | 323.97878779 | 48.76095676 | 291.7151 | 53931.2858333333 | 53933.2551388889 | 801013020 | 79110.5 | 75000 | 79126.5 | 79110.5 | 79126.5 | 79134.5 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 69567 | 69567 | 170109.8 | 2 | PROCESSED | 57534.9865393518 | 54394 | 53942.463587963 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010014 | We propose to obtain broad-band spectra of the most X-ray luminous cluster of galaxies RXJ1347.5-1145 at z=0.45. Our previous high-resolution Sunyaev-Zel'dovich obvervations of this cluster revealed that it exhibits an unusually violent merger activity. Its high X-ray luminosity ensures the unprecedented high-quality spectra with Suzaku. It is indeed a unique target to probe gas physics and particle acceleration mechanism associated with the violent mergers at high redshift. The continuum observations with HXD and XIS as well as the iron line spectroscopy will specify the physical states of both thermal and non-thermal components of the ICM. Combined with the Chandra and our SZ data, the Suzaku data will accomplish the first comprehensive modeling of a violent merger in distant clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | OTA | NAOMI | NULL | NULL | JAP | 1 | AO1 | BROAD-BAND SPECTROSCOPY OF THE MOST X-RAY LUMINOUS CLUSTER OF GALAXIES RXJ1347.5-1145 AT Z=0.45 | HXD | N |
| FORNAX A WEST LOBE | 50.4184 | -37.1645 | 240.1258488 | -56.89722719 | 219.7525 | 54092.8700462963 | 54095.6113888889 | 801014010 | 93309.3 | 100000 | 93309.3 | 93309.3 | 0 | 93309.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 96371.6 | 96371.6 | 236835.8 | 5 | PROCESSED | 57536.4597569444 | 54735 | 54111.6821875 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010029 | We propose Suzaku observations of the Fornax A west radio lobe and the host galaxy. By measuring the inverse-Compton X-ray spectrum from the radio lobe precisely up to 20 keV and comparing with radio observation results, we are able to determine the electron energy spectrum and to derive magnetic field without any assumptions. This will be an important sample to measure the kinetic energy outflow from an active galactic nucleus. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TASHIRO | MAKOTO | NULL | NULL | JAP | 1 | AO1 | RELATIVISTIC ELECTRON ENERGY SPECTRUM IN THE RADIO LOBE OF FORNAX A | HXD | Y |
| FORNAX A HOST GALAXY | 50.6684 | -37.2029 | 240.15407206 | -56.69497357 | 218.3809 | 54091.6179976852 | 54092.8689699074 | 801015010 | 48721.7 | 50000 | 48721.7 | 48721.7 | 0 | 48721.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48398.7 | 48398.7 | 108083.9 | 1 | PROCESSED | 57536.4184837963 | 54735 | 54132.9200347222 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010029 | We propose Suzaku observations of the Fornax A west radio lobe and the host galaxy. By measuring the inverse-Compton X-ray spectrum from the radio lobe precisely up to 20 keV and comparing with radio observation results, we are able to determine the electron energy spectrum and to derive magnetic field without any assumptions. This will be an important sample to measure the kinetic energy outflow from an active galactic nucleus. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TASHIRO | MAKOTO | NULL | NULL | JAP | 1 | AO1 | RELATIVISTIC ELECTRON ENERGY SPECTRUM IN THE RADIO LOBE OF FORNAX A | XIS | Y |
| PKS 2356-61 | 359.7661 | -60.908 | 314.02525269 | -55.07790138 | 249.6445 | 54075.7140740741 | 54078.21625 | 801016010 | 100837.2 | 100000 | 100845.2 | 100837.2 | 0 | 100853.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 92125.5 | 92125.5 | 216157.9 | 3 | PROCESSED | 57536.3143171296 | 54456 | 54088.6546759259 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010059 | We propose a 100 ksec Suzaku observation of the radio galaxy PKS 2356-61. PKS 2356-61 is reported to reside in a group of galaxies, and a sign of a diffuse X-ray emission with a possibly high temperature surrounding PKS 2356-61 was suggested with ASCA. Our objective is the determination of the origin of the diffuse emission to evaluate AGN heating of the intragroup gas by PKS 2356-61. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | HONG | SOOJING | NULL | NULL | JAP | 1 | AO1 | HIGH TEMPERATURE GROUP OF GALAXIES SURROUNDING THE RADIO GALAXY PKS 2356-61 | XIS | N |
| NGC 507 | 20.9105 | 33.2598 | 130.6367604 | -29.12969375 | 54.0771 | 53944.6189351852 | 53946.5544444444 | 801017010 | 79501.3 | 80000 | 79525.3 | 79501.3 | 79525.3 | 79525.3 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 80286.7 | 80286.7 | 167170 | 2 | PROCESSED | 57535.1047222222 | 54394 | 53955.7736689815 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010061 | We propose to observe luminous elliptical galaxies NGC 507 and NGC 499 for 80 and 100 ksec, respectively, to study abundance distribution of Fe and O. The good energy resolution and low background of the XIS instrument is crucial for this study, and we can perform the first reliable measurement of O distribution around elliptical galaxies. Comparison of O and Fe abundance profiles will tell us how metals produced by type Ia and II supernovae have been enriched in the intergalactic space. Comparison of NGC 507 and NGC 499 will show us how much metal production process differ with galaxy size. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | SATO | KOSUKE | NULL | NULL | JAP | 1 | AO1 | CHEMICAL EVOLUTION OF ELLIPTICAL GALAXIES IN GROUP OF GALAXIES: NGC 507 AND NGC 499 | XIS | N |
| NGC 4631 | 190.5387 | 32.5478 | 142.74124336 | 84.2191655 | 139.0678 | 54067.1412615741 | 54068.9133217593 | 801019010 | 81076.1 | 80000 | 81084.1 | 81076.1 | 0 | 81084.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 74435.8 | 74435.8 | 153070 | 0 | PROCESSED | 57536.2568865741 | 54735 | 54088.6914699074 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010062 | We propose to observe a edge-on nearby starburst galaxy, NGC 4631 for an exposure time of 80 ksec. This observation will give us a ``template'' of ejecta from type II SNe with less than 30% accuracy of abandance of alpha elemements. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | YAMASAKI | NORIKO | NULL | NULL | JAP | 1 | AO1 | OBSERVATION OF A STARBURST GALAXY NGC 4631 WITH XIS | XIS | Y |
| A399/401 FILAMENT | 44.7475 | 13.2485 | 164.45015039 | -39.12843885 | 74.1756 | 53966.1736921296 | 53969.4641666667 | 801020010 | 151060.1 | 150000 | 151060.1 | 151068.1 | 151068.1 | 151068.1 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 142203.6 | 142203.6 | 284273.8 | 5 | PROCESSED | 57535.3984837963 | 54526 | 54021.1056944444 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010063 | Although warm-hot intergalactic medium (WHIM) is supposed to account for most of the baryon in the Universe, its detection is extremely difficult. Here, we propose to observe the cosmological filament between clusters A399 and A401 with Suzaku. We try to detect the OVII emission line and confirm the existence of WHIM in the filament. We expect that the density of the WHIM in the filament is high, and that the detection will be easier than that in other regions in the Universe. Moreover, since the redshift of the filament is relatively high, we can discriminate between the OVII mission from the WHIM and that from our Galaxy by studying the redshift of the line. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | FUJITA | YUTAKA | NULL | NULL | JAP | 1 | AO1 | THE DETECTION OF WHIM IN THE A399/401 FILAMENT | XIS | N |
| OPHIUCHUS CLUSTER 0 | 258.0174 | -23.3865 | 0.50702706 | 9.33401192 | 88.8366 | 54183.0313078704 | 54183.5648726852 | 801021010 | 16641.1 | 15000 | 16641.1 | 16641.1 | 0 | 16641.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13520.9 | 13520.9 | 46095.9 | 0 | PROCESSED | 57537.9746643518 | 54736 | 54209.5175462963 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010065 | The Ophiuchus cluster is one of the few galaxy clusters from which hard X-ray emission was detected with INTEGRAL. The confidence level is higher than that of the Coma cluster. The hard X-ray emission was also detected with BeppoSAX. Complicated temperature structure observed with ASCA indicated that the cluster is in a merger phase at present. The hard X-ray emission is possibly originated from the cluster merger and the resultant particle acceleration. We propose a Suzaku observation of the cluster to reveal the mechanism of the particle acceleration in clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | FUJITA | YUTAKA | NULL | NULL | JAP | 1 | AO1 | PARTICLE ACCELERATION IN THE OPHIUCHUS CLUSTER | XIS | Y |
| OPHIUCHUS CLUSTER 1 | 258.2981 | -23.3868 | 0.65649186 | 9.12279372 | 88.7031 | 54180.6159953704 | 54181.1398611111 | 801022010 | 24067 | 15000 | 24075 | 24067 | 0 | 24075 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21821.3 | 21821.3 | 45254 | 1 | PROCESSED | 57537.7417476852 | 54736 | 54186.192650463 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010065 | The Ophiuchus cluster is one of the few galaxy clusters from which hard X-ray emission was detected with INTEGRAL. The confidence level is higher than that of the Coma cluster. The hard X-ray emission was also detected with BeppoSAX. Complicated temperature structure observed with ASCA indicated that the cluster is in a merger phase at present. The hard X-ray emission is possibly originated from the cluster merger and the resultant particle acceleration. We propose a Suzaku observation of the cluster to reveal the mechanism of the particle acceleration in clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | FUJITA | YUTAKA | NULL | NULL | JAP | 1 | AO1 | PARTICLE ACCELERATION IN THE OPHIUCHUS CLUSTER | XIS | Y |
| OPHIUCHUS CLUSTER 2 | 257.7375 | -23.3864 | 0.3572282 | 9.54416529 | 94.9391 | 54181.1423726852 | 54181.825162037 | 801023010 | 24678.2 | 15000 | 24702.2 | 24694.2 | 0 | 24678.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21278.1 | 21278.1 | 58987.9 | 1 | PROCESSED | 57537.9744097222 | 54736 | 54209.5433217593 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010065 | The Ophiuchus cluster is one of the few galaxy clusters from which hard X-ray emission was detected with INTEGRAL. The confidence level is higher than that of the Coma cluster. The hard X-ray emission was also detected with BeppoSAX. Complicated temperature structure observed with ASCA indicated that the cluster is in a merger phase at present. The hard X-ray emission is possibly originated from the cluster merger and the resultant particle acceleration. We propose a Suzaku observation of the cluster to reveal the mechanism of the particle acceleration in clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | FUJITA | YUTAKA | NULL | NULL | JAP | 1 | AO1 | PARTICLE ACCELERATION IN THE OPHIUCHUS CLUSTER | XIS | Y |
| OPHIUCHUS CLUSTER 5 | 258.0184 | -23.1077 | 0.73892155 | 9.49336651 | 88.7652 | 54181.8276736111 | 54182.4890277778 | 801026010 | 24255.7 | 15000 | 24255.7 | 24255.7 | 0 | 24255.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19227.1 | 19227.1 | 57135.9 | 0 | PROCESSED | 57537.9767013889 | 54736 | 54186.2070949074 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010065 | The Ophiuchus cluster is one of the few galaxy clusters from which hard X-ray emission was detected with INTEGRAL. The confidence level is higher than that of the Coma cluster. The hard X-ray emission was also detected with BeppoSAX. Complicated temperature structure observed with ASCA indicated that the cluster is in a merger phase at present. The hard X-ray emission is possibly originated from the cluster merger and the resultant particle acceleration. We propose a Suzaku observation of the cluster to reveal the mechanism of the particle acceleration in clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | FUJITA | YUTAKA | NULL | NULL | JAP | 1 | AO1 | PARTICLE ACCELERATION IN THE OPHIUCHUS CLUSTER | XIS | Y |
| OPHIUCHUS CLUSTER 8 | 258.0175 | -23.6665 | 0.2749393 | 9.17298979 | 88.8988 | 54182.4897337963 | 54183.0308333333 | 801029010 | 23738.9 | 15000 | 23746.9 | 23738.9 | 0 | 23746.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21678 | 21678 | 46746 | 0 | PROCESSED | 57537.9753240741 | 54736 | 54209.5725231482 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010065 | The Ophiuchus cluster is one of the few galaxy clusters from which hard X-ray emission was detected with INTEGRAL. The confidence level is higher than that of the Coma cluster. The hard X-ray emission was also detected with BeppoSAX. Complicated temperature structure observed with ASCA indicated that the cluster is in a merger phase at present. The hard X-ray emission is possibly originated from the cluster merger and the resultant particle acceleration. We propose a Suzaku observation of the cluster to reveal the mechanism of the particle acceleration in clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | FUJITA | YUTAKA | NULL | NULL | JAP | 1 | AO1 | PARTICLE ACCELERATION IN THE OPHIUCHUS CLUSTER | XIS | Y |
| OPHIUCHUS CLUSTER BG | 257.0147 | -25.0612 | 358.58755189 | 9.10838139 | 89.7146 | 54183.5662268518 | 54183.9169444444 | 801030010 | 15298.3 | 15000 | 15306.3 | 15306.3 | 0 | 15298.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14635.1 | 14635.1 | 30296 | 0 | PROCESSED | 57537.9841898148 | 54736 | 54209.5187384259 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010065 | The Ophiuchus cluster is one of the few galaxy clusters from which hard X-ray emission was detected with INTEGRAL. The confidence level is higher than that of the Coma cluster. The hard X-ray emission was also detected with BeppoSAX. Complicated temperature structure observed with ASCA indicated that the cluster is in a merger phase at present. The hard X-ray emission is possibly originated from the cluster merger and the resultant particle acceleration. We propose a Suzaku observation of the cluster to reveal the mechanism of the particle acceleration in clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | FUJITA | YUTAKA | NULL | NULL | JAP | 1 | AO1 | PARTICLE ACCELERATION IN THE OPHIUCHUS CLUSTER | XIS | Y |
| 3EGJ1234 1318_1 | 188.0173 | -13.3363 | 295.70141073 | 49.26333697 | 109.7313 | 54081.3723032407 | 54081.9273032407 | 801031010 | 19409.8 | 20000 | 19417.8 | 19417.8 | 0 | 19409.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18722.8 | 18722.8 | 47949.9 | 1 | PROCESSED | 57536.3099768518 | 54735 | 54094.2359722222 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010068 | We propose observations around 3EG J1234 1318, which is one of the EGRET un-ID sources. From recent optical survey, it is found that the source is located around a large scale structure at z ?sim 0.1. We propose a scenario that the GeV source is originating from a large shock wave within the structure formation. The XIS and the HXD provides a probe for thermal shock plasma and non-thermal IC emission, respectively. This observation will solve some questions on EGRET un-ID sources. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TOTANI | TOMONORI | NULL | NULL | JAP | 1 | AO1 | CONFIRMING GAMMA-RAY EMISSION FROM INTERGALACTIC SHOCKS: A NEW WINDOW TO STUDY THE COSMIC STRUCTURE FORMATION | HXD | Y |
| 3EGJ1234 1318_2 | 188.017 | -13.0869 | 295.65674578 | 49.51103665 | 109.9322 | 54081.9277777778 | 54082.7766087963 | 801032010 | 30942.7 | 30000 | 30966.7 | 30958.7 | 0 | 30942.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26083 | 26083 | 73333.9 | 1 | PROCESSED | 57536.3393055556 | 54735 | 54094.2665740741 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010068 | We propose observations around 3EG J1234 1318, which is one of the EGRET un-ID sources. From recent optical survey, it is found that the source is located around a large scale structure at z ?sim 0.1. We propose a scenario that the GeV source is originating from a large shock wave within the structure formation. The XIS and the HXD provides a probe for thermal shock plasma and non-thermal IC emission, respectively. This observation will solve some questions on EGRET un-ID sources. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TOTANI | TOMONORI | NULL | NULL | JAP | 1 | AO1 | CONFIRMING GAMMA-RAY EMISSION FROM INTERGALACTIC SHOCKS: A NEW WINDOW TO STUDY THE COSMIC STRUCTURE FORMATION | HXD | Y |
| AWM7 | 43.631 | 41.5933 | 146.34082925 | -15.61629549 | 90.4997 | 53954.2348842593 | 53954.71625 | 801035010 | 18985.8 | 20000 | 18985.8 | 18985.8 | 18985.8 | 18985.8 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 17554.2 | 17554.2 | 41588 | 0 | PROCESSED | 57535.2434953704 | 54422 | 54020.7471759259 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010076 | The bright elongated cluster AWM7 is likely to be the place of gas infall along the large-scale filament of the Pisces-Perseus supercluster. We propose to probe the gas motion by measuring the energy shift and line broadening of Fe-K line based on the good energy resolution and low background of the XIS instrument. The motion of 1000 km/s is a reliably detectable level and we can directly measure the cluster formation process and its relation with the large-scale filament for the first time. If no gas motion is found, then secular asymmetric structure of the dark matter halo is implied. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | OHASHI | TAKAYA | NULL | NULL | JAP | 1 | AO1 | SIGNATURE OF LARGE-SCALE GAS MOTION IN AWM7 | XIS | N |
| AWM7 EAST OFFSET | 44.0318 | 41.5949 | 146.61375919 | -15.47239178 | 90.4995 | 53952.2676967593 | 53953.2398611111 | 801036010 | 38536.1 | 40000 | 38536.1 | 38536.1 | 38536.1 | 38536.1 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 37541 | 37541 | 83959.9 | 0 | PROCESSED | 57535.0870138889 | 54394 | 54020.7498726852 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010076 | The bright elongated cluster AWM7 is likely to be the place of gas infall along the large-scale filament of the Pisces-Perseus supercluster. We propose to probe the gas motion by measuring the energy shift and line broadening of Fe-K line based on the good energy resolution and low background of the XIS instrument. The motion of 1000 km/s is a reliably detectable level and we can directly measure the cluster formation process and its relation with the large-scale filament for the first time. If no gas motion is found, then secular asymmetric structure of the dark matter halo is implied. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | OHASHI | TAKAYA | NULL | NULL | JAP | 1 | AO1 | SIGNATURE OF LARGE-SCALE GAS MOTION IN AWM7 | XIS | N |
| AWM7 WEST OFFSET | 43.2295 | 41.594 | 146.06522235 | -15.7568529 | 90.4999 | 53953.2407060185 | 53954.2343171296 | 801037010 | 39817.7 | 40000 | 39849.7 | 39817.7 | 39849.7 | 39849.7 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 38108.9 | 38108.9 | 85835.9 | 1 | PROCESSED | 57535.2509375 | 54394 | 54020.7562384259 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010076 | The bright elongated cluster AWM7 is likely to be the place of gas infall along the large-scale filament of the Pisces-Perseus supercluster. We propose to probe the gas motion by measuring the energy shift and line broadening of Fe-K line based on the good energy resolution and low background of the XIS instrument. The motion of 1000 km/s is a reliably detectable level and we can directly measure the cluster formation process and its relation with the large-scale filament for the first time. If no gas motion is found, then secular asymmetric structure of the dark matter halo is implied. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | OHASHI | TAKAYA | NULL | NULL | JAP | 1 | AO1 | SIGNATURE OF LARGE-SCALE GAS MOTION IN AWM7 | XIS | N |
| M87 CENTER | 187.7366 | 12.4456 | 283.82387862 | 74.55209055 | 120.529 | 54068.9187037037 | 54071.1266666667 | 801038010 | 98183.1 | 100000 | 98183.1 | 98183.1 | 0 | 98183.1 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 88250.3 | 88250.3 | 190730.8 | 2 | PROCESSED | 57536.2829050926 | 54735 | 54090.4156134259 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010084 | The black hole at the center of M87 is one of the most heaviest in the universe. Recently TeV-gamma ray emission from M87 was found. M87 is thus a very strong candidate for an accelerator of ultra-high energy cosmic rays. We aim at the detection of non-thermal hard X-rays from M87 to clarify the mechanism of the particle acceleration. The giant elliptical galaxy M87 is at the center of the Virgo cluster of galaxies, which is the nearest cluster. We can investigate the distribution of various metal elements. We will clarify how the metals, especially oxygen, diffuse to the intracluster space from the galaxy M87. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | AO1 | NON-THERMAL AND THERMAL EMISSIONS OF M87 AS OBSERVED WITH SUZAKU | HXD | Y |
| M87 50' SE | 188.2678 | 11.8367 | 286.30035277 | 74.11241529 | 119.899 | 54071.127650463 | 54072.312037037 | 801039010 | 53637.4 | 50000 | 53637.4 | 53658.1 | 0 | 53645.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46139.4 | 46139.4 | 102309 | 1 | PROCESSED | 57536.2354861111 | 54735 | 54088.5776736111 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010084 | The black hole at the center of M87 is one of the most heaviest in the universe. Recently TeV-gamma ray emission from M87 was found. M87 is thus a very strong candidate for an accelerator of ultra-high energy cosmic rays. We aim at the detection of non-thermal hard X-rays from M87 to clarify the mechanism of the particle acceleration. The giant elliptical galaxy M87 is at the center of the Virgo cluster of galaxies, which is the nearest cluster. We can investigate the distribution of various metal elements. We will clarify how the metals, especially oxygen, diffuse to the intracluster space from the galaxy M87. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MATSUMOTO | HIRONORI | NULL | NULL | JAP | 1 | AO1 | NON-THERMAL AND THERMAL EMISSIONS OF M87 AS OBSERVED WITH SUZAKU | XIS | Y |
| A2319CENTER | 290.3341 | 43.878 | 75.63759851 | 13.45022652 | 251.6652 | 54035.9326041667 | 54038.1466898148 | 801040010 | 99533.2 | 100000 | 99549.2 | 99541.2 | 99533.2 | 99549.2 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 93954.8 | 93954.8 | 191268 | 2 | PROCESSED | 57535.9905555556 | 54735 | 54063.5741666667 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010085 | We propose the observations of the A2319 cluster with the Suzaku HXD and XIS to investigate particle acceleration processes in the intracluster medium(ICM). A2319 is a nearby massive merging cluster whose collision axis is nearly along the line of sight, and has diffuse non-thermal radio emission. We will detect non-thermal hard X-ray with HXD, and determine the velocity difference between the two subclusters with XIS. With these results, we will determine dynamical status of the ICM and get implications on the particle acceleration processes. We will compare the results with theoretical models, numerical simulations, and radio and optical observations to get an overall picture of particle acceleration in clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | TAKIZAWA | MOTOKAZU | NULL | NULL | JAP | 1 | AO1 | PARTICLE ACCELERATION IN THE A2319 CLUSTER | HXD | Y |
| A85 | 10.4739 | -9.4292 | 115.23010576 | -72.15810594 | 248.2856 | 54105.4020023148 | 54108.0557175926 | 801041010 | 99201.2 | 100000 | 99201.2 | 99201.2 | 0 | 99201.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 84813.9 | 84813.9 | 229242.1 | 2 | PROCESSED | 57536.5180671296 | 54735 | 54132.9388773148 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010088 | We propose observations of A2199 and A85 clusters of galaxies with an each exposure time of 100 ks, in order to search for excess hard X-ray emission, to constrain the spectral shape, and to discuss the origin of the hard X-ray emission. Both are listed as the clusters which are detected non-thermal emission signal with 2 sigma confidence level by Beppo SAX PDS detector. In addition, these two clusters only have features of brighter X-ray flux, good size, relatively cool ICM temperature, and including no bright member AGNs. Therefore they are suitable target samples for our observational purpose about estimation photon index and flux for the excess hard X-ray emission with high significance wherever possible. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | SHIBATA | RYO | NULL | NULL | JAP | 1 | AO1 | SEARCH FOR EXCESS HARD X-RAY EMISSION FROM A2199 AND A85 GALAXY CLUSTERS | HXD | Y |
| M31 | 10.6944 | 41.2627 | 121.18191229 | -21.57961988 | 231.6592 | 54115.6775578704 | 54117.4572222222 | 801043010 | 99872.3 | 100000 | 99872.3 | 99872.3 | 0 | 99872.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 103912.4 | 103912.4 | 153723.8 | 1 | PROCESSED | 57536.8902777778 | 54744 | 54132.9457291667 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010089 | We propose the 100 ks Suzaku observation of the central region of Andromeda Nebula (M31). Our gaol is to detect 3 components (cool, hot and hard) of galactic diffuse X-ray emission (GDXE) with the XIS and HXD. This detection shows the existance of the GDXE hot and hard component in the extragalactic normal spiral galaxy, for the first time. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAKAHASHI | HIROMITSU | NULL | NULL | JAP | 1 | AO1 | DETECTION OF GALACTIC DIFFUSE X-RAY EMISSION FROM THE CENTRAL REGION OF THE ANDROMEDA NEBULA | XIS | Y |
| COMA CLUSTER OFFSET | 194.6939 | 27.9466 | 60.06105128 | 88.1791818 | 318.0815 | 53885.0996412037 | 53886.8384722222 | 801044010 | 79172 | 80000 | 79172 | 79172 | 79172 | 79172 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 75228.2 | 75228.2 | 150204.9 | 2 | PROCESSED | 57534.5195949074 | 54394 | 53926.7587384259 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010091 | In order to determine the distribution of O of the intracluster medium of the Coma cluster, we propose to observe the central region with a 40ks exposure and the offset region with a 80ks exposure. The most important in studying the history of nucleosynthesis by SN II is the O mass in the intracluster medium. Especially, the hot cluster contains most of the metals synthesized in the past. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MATSUSHITA | KYOKO | NULL | NULL | JAP | 1 | AO1 | THE DETERMINATION OF O ABUNDANCE OF THE INTRACLUSTER MEDIUM OF THE COMA CLUSTER | XIS | N |
| NGC 5044 | 198.8504 | -16.3899 | 311.2339251 | 46.09520433 | 290.0016 | 53918.7631712963 | 53919.3600115741 | 801046010 | 19746.6 | 20000 | 19746.6 | 19746.6 | 19746.6 | 19746.6 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 17971.6 | 17971.6 | 51562 | 1 | PROCESSED | 57534.8255208333 | 54394 | 53930.6133217593 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010092 | We propose to observe NGC 5044 group of galaxies in order to determine the distributions of O, Mg, Si, and Fe up to 0.3 r180. Suzaku is the best satellite to study the O and Mg abundance of extended objects. The low and stable background of Suzaku is useful to study low surface brightness regions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MATSUSHITA | KYOKO | NULL | NULL | JAP | 1 | AO1 | THE METAL DISTRIBUTION OF THE NGC 5044 GROUP | XIS | N |
| NGC 5044 OFFSET1 | 198.8505 | -16.143 | 311.28196707 | 46.33985641 | 290.0004 | 53919.3604398148 | 53920.9599305556 | 801047010 | 54620.4 | 60000 | 54620.4 | 54620.4 | 54620.4 | 54620.4 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 45803.3 | 45803.3 | 138189.9 | 1 | PROCESSED | 57534.8941203704 | 54394 | 53942.4615740741 | 3.0.22.43 | 6 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010092 | We propose to observe NGC 5044 group of galaxies in order to determine the distributions of O, Mg, Si, and Fe up to 0.3 r180. Suzaku is the best satellite to study the O and Mg abundance of extended objects. The low and stable background of Suzaku is useful to study low surface brightness regions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MATSUSHITA | KYOKO | NULL | NULL | JAP | 1 | AO1 | THE METAL DISTRIBUTION OF THE NGC 5044 GROUP | XIS | N |
| NGC 5044 OFFSET2 | 199.1117 | -16.388 | 311.59229028 | 46.06278821 | 290.7836 | 53920.9609143518 | 53922.7598842593 | 801048010 | 62451 | 60000 | 62451 | 62451 | 62451 | 62451 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 57110.2 | 57110.2 | 155314.9 | 2 | PROCESSED | 57534.8962615741 | 54422 | 54034.2926736111 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010092 | We propose to observe NGC 5044 group of galaxies in order to determine the distributions of O, Mg, Si, and Fe up to 0.3 r180. Suzaku is the best satellite to study the O and Mg abundance of extended objects. The low and stable background of Suzaku is useful to study low surface brightness regions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MATSUSHITA | KYOKO | NULL | NULL | JAP | 1 | AO1 | THE METAL DISTRIBUTION OF THE NGC 5044 GROUP | XIS | N |
| PERSEUS CL OFFSET | 49.6445 | 42.068 | 150.06631202 | -12.92163855 | 65.996 | 53980.0800925926 | 53980.7668287037 | 801049010 | 29243.8 | 30000 | 29255.9 | 29247.9 | 29251.8 | 29243.8 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 25672.9 | 25672.9 | 59329.9 | 1 | PROCESSED | 57535.4121296296 | 54526 | 54021.3135416667 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010097 | We propose to observe the X-ray brightest galaxy cluster, the Perseus cluster, with 4 pointings offset from the cluster center. In this observation, we will measure a nonthermal energy budget from three measurements; search for very high temperature electron deviated from the average temperature or suprathermal electrons, search for nonthermal powerlaw component, and doppler shift of Fe-K lines caused by the bulk motion of hot gas. Hot clusters, including the Perseus cluster, are believed to be now evolving, by absorbing poor groups at the cluster periphery, and thus nonthermal energy at the cluster periphery is important to probe the information of cluster evolution. Such a measurement can be performed by only Suzaku; HXD-PIN with narrow field of view, and XIS with stable low background. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | FUKAZAWA | YASUSHI | NULL | NULL | JAP | 1 | AO1 | MEASUREMENT OF NONTHERMAL ENERGY BUDGET IN THE PERSEUS CLUSTER | HXD | N |
| PERSEUS CL OFFSET | 49.2788 | 41.3719 | 150.2212005 | -13.65398882 | 65.9966 | 53980.7676273148 | 53981.4543287037 | 801049020 | 32464.6 | 30000 | 32480.6 | 32464.6 | 32496.6 | 32488.6 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 28291.2 | 28291.2 | 59319.9 | 1 | PROCESSED | 57535.422025463 | 54526 | 54021.2712731482 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010097 | We propose to observe the X-ray brightest galaxy cluster, the Perseus cluster, with 4 pointings offset from the cluster center. In this observation, we will measure a nonthermal energy budget from three measurements; search for very high temperature electron deviated from the average temperature or suprathermal electrons, search for nonthermal powerlaw component, and doppler shift of Fe-K lines caused by the bulk motion of hot gas. Hot clusters, including the Perseus cluster, are believed to be now evolving, by absorbing poor groups at the cluster periphery, and thus nonthermal energy at the cluster periphery is important to probe the information of cluster evolution. Such a measurement can be performed by only Suzaku; HXD-PIN with narrow field of view, and XIS with stable low background. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | FUKAZAWA | YASUSHI | NULL | NULL | JAP | 1 | AO1 | MEASUREMENT OF NONTHERMAL ENERGY BUDGET IN THE PERSEUS CLUSTER | HXD | N |
| PERSEUS CL OFFSET | 50.2242 | 41.1004 | 150.98569591 | -13.49005998 | 65.9967 | 53981.4552662037 | 53982.1418287037 | 801049030 | 32839.6 | 30000 | 32855.6 | 32847.6 | 32839.6 | 32863.6 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 31031.3 | 31031.3 | 59288 | 0 | PROCESSED | 57535.4291087963 | 54526 | 54020.8372106482 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010097 | We propose to observe the X-ray brightest galaxy cluster, the Perseus cluster, with 4 pointings offset from the cluster center. In this observation, we will measure a nonthermal energy budget from three measurements; search for very high temperature electron deviated from the average temperature or suprathermal electrons, search for nonthermal powerlaw component, and doppler shift of Fe-K lines caused by the bulk motion of hot gas. Hot clusters, including the Perseus cluster, are believed to be now evolving, by absorbing poor groups at the cluster periphery, and thus nonthermal energy at the cluster periphery is important to probe the information of cluster evolution. Such a measurement can be performed by only Suzaku; HXD-PIN with narrow field of view, and XIS with stable low background. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | FUKAZAWA | YASUSHI | NULL | NULL | JAP | 1 | AO1 | MEASUREMENT OF NONTHERMAL ENERGY BUDGET IN THE PERSEUS CLUSTER | HXD | N |
| PERSEUS CL OFFSET | 50.5735 | 41.8053 | 150.80595618 | -12.75877318 | 65.9956 | 53982.1426736111 | 53982.4377893518 | 801049040 | 10420.6 | 30000 | 10420.6 | 10420.6 | 10420.6 | 10420.6 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 7540.2 | 7540.2 | 25467.9 | 1 | PROCESSED | 57535.4390856482 | 54526 | 54021.0033680556 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010097 | We propose to observe the X-ray brightest galaxy cluster, the Perseus cluster, with 4 pointings offset from the cluster center. In this observation, we will measure a nonthermal energy budget from three measurements; search for very high temperature electron deviated from the average temperature or suprathermal electrons, search for nonthermal powerlaw component, and doppler shift of Fe-K lines caused by the bulk motion of hot gas. Hot clusters, including the Perseus cluster, are believed to be now evolving, by absorbing poor groups at the cluster periphery, and thus nonthermal energy at the cluster periphery is important to probe the information of cluster evolution. Such a measurement can be performed by only Suzaku; HXD-PIN with narrow field of view, and XIS with stable low background. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | FUKAZAWA | YASUSHI | NULL | NULL | JAP | 1 | AO1 | MEASUREMENT OF NONTHERMAL ENERGY BUDGET IN THE PERSEUS CLUSTER | HXD | N |
| Z348 | 16.7077 | 1.0407 | 131.03941429 | -61.58850223 | 247.9196 | 54110.9286689815 | 54111.5259722222 | 801050010 | 22647.7 | 23000 | 22647.7 | 22647.7 | 0 | 22647.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21340.3 | 21340.3 | 51589 | 1 | PROCESSED | 57536.8362384259 | 54735 | 54133.0321643518 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010098 | We propose to carry out the Suzaku/XIS observations of 4 massive clusters at low redshifts (z <0.3). Combining the X-ray data with the existing Subaru datasets that allow us to directly reconstruct the mass distribution from the gravitational lensing measurements, we will investigate the physical relations between the mass and gas distributions to understand the nature of cluster in a quantitative way. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | FUTAMASE | TOSHIFUMI | NULL | NULL | JAP | 1 | AO1 | THE ULTIMATE GRAVITATIONAL LENSING STUDY OF GALAXY CLUSTERS | XIS | Y |
| NGC3923 | 177.7599 | -28.8047 | 287.27787622 | 32.22445477 | 293.1988 | 53899.8430671296 | 53902.7293287037 | 801054010 | 115820 | 120000 | 115828 | 115820 | 115828 | 115828 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 107731.3 | 107731.3 | 249352.8 | 3 | PROCESSED | 57534.7187731482 | 54394 | 53927.2880902778 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010100 | We propose to observe an isolated elliptical galaxy NGC3923, to meaasure a dark matter distribution. The large effective area and stable low background of XIS enable us to measure a faint extended X-ray emission such as the periphery of elliptical galaxies more accurately than ever. Since X-ray bright elliptical galaxies have been found to be surrounded by group-scale emission, X-ray faint elliptical galaxies are the best to investigate the dark matter associated with the galaxy itself. The dark matter around galaxies is a key to resolve the problem of why X-ray bright and faint elliptical galaxies exist. The oxygen abundance distribution is also useful to probe the above issue. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | FUKAZAWA | YASUSHI | NULL | NULL | JAP | 1 | AO1 | ACCURATE MEASUREMENT OF DARK MATTER DISTRIBUTION AROUND AN ISOLATED ELLIPTICAL GALAXY NGC3923 | XIS | N |
| A2142 | 239.5312 | 27.2879 | 44.29837206 | 48.74478569 | 138.1624 | 54104.1546990741 | 54105.3891666667 | 801055010 | 51452.5 | 60000 | 51460.5 | 51452.5 | 0 | 51460.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 49209.8 | 49209.8 | 106632 | 1 | PROCESSED | 57536.4705555556 | 54735 | 54111.417037037 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010106 | We propose to reveal the formation and evolution of dense core with cold fronts with SUZAKU/XIS. Our strategy of observation is based on the results of Chandra, ROSAT and weak lensing analysis. A2142 is a galaxy cluster which has contact discontinuities, "cold fronts", between cold-dense cores and hot-thin surrounding gas. We have carried out "weak lensing analysis" and derived mass map in A2142. We measure the bulk velocity via Fe-K line in the central region. We derive the merger velocity by observing the temperatures of the heating and non-heating which are expected by our observational results. It leads to understand the formation and evolution of dense core with cold fronts, since the merger and core velocities are closely related to the evolution of dense cores with cold fronts. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | OKABE | NOBUHIRO | NULL | NULL | JAP | 1 | AO1 | REVEALING COLD FRONTS AND DENSE CORES IN GALAXY CLUSTER A2142 | XIS | Y |
| ABELL 2199 CENTER | 247.1922 | 39.484 | 62.84241749 | 43.66620611 | 252.3681 | 54009.2972222222 | 54009.8967361111 | 801056010 | 24928.2 | 25000 | 25479.9 | 24928.2 | 25479.9 | 25479.9 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 20519 | 20519 | 51793.9 | 1 | PROCESSED | 57535.7247453704 | 54735 | 54021.2246990741 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010138 | Detection of hard X-ray emission from clusters of Galaxies is one of the top goals of Suzaku. For this purpose, we propose 5 pointing observations of Abell 2199 each of which is 25 ks. Abell 2199 is one of objects from which significant hard X-ray emission have been detected by BeppoSAX PDS with 2 sigma significance level. Among them, Abell 2199 is unique in that it neither have a signature of cluster merger nor significant AGN activities. The HXD PIN detector can just covers the whole X-ray emission from Abell 2199, and determine photon index and flux of the hard component. The detection of hard X-ray emission from a relaxed cluster opens a new field of study in which particle accelerations occur generally in clusters even without energetic events like sub-cluster mergers. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KAWAHARADA | MADOKA | NULL | NULL | JAP | 1 | AO1 | PROBING HARD X-RAY EMISSION FROM A RELAXED CLUSTER OF GALAXIES | HXD | Y |
| ABELL 2199 OFFSET 1 | 247.0269 | 39.6504 | 63.06766091 | 43.79825488 | 251.7923 | 54009.8973958333 | 54010.4467476852 | 801057010 | 24631.5 | 25000 | 24631.5 | 24631.5 | 24631.5 | 24631.5 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 25534.3 | 25534.3 | 47454 | 0 | PROCESSED | 57535.7339814815 | 54735 | 54021.2449189815 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010138 | Detection of hard X-ray emission from clusters of Galaxies is one of the top goals of Suzaku. For this purpose, we propose 5 pointing observations of Abell 2199 each of which is 25 ks. Abell 2199 is one of objects from which significant hard X-ray emission have been detected by BeppoSAX PDS with 2 sigma significance level. Among them, Abell 2199 is unique in that it neither have a signature of cluster merger nor significant AGN activities. The HXD PIN detector can just covers the whole X-ray emission from Abell 2199, and determine photon index and flux of the hard component. The detection of hard X-ray emission from a relaxed cluster opens a new field of study in which particle accelerations occur generally in clusters even without energetic events like sub-cluster mergers. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KAWAHARADA | MADOKA | NULL | NULL | JAP | 1 | AO1 | PROBING HARD X-RAY EMISSION FROM A RELAXED CLUSTER OF GALAXIES | HXD | Y |
| ABELL 2199 OFFSET 2 | 247.3619 | 39.6495 | 63.07626508 | 43.54039287 | 251.2564 | 54011.5284722222 | 54012.1578587963 | 801058010 | 22707.2 | 25000 | 22723.2 | 22707.2 | 22723.2 | 22723.2 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 20704 | 20704 | 54360 | 0 | PROCESSED | 57535.7442476852 | 54735 | 54024.6719907407 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010138 | Detection of hard X-ray emission from clusters of Galaxies is one of the top goals of Suzaku. For this purpose, we propose 5 pointing observations of Abell 2199 each of which is 25 ks. Abell 2199 is one of objects from which significant hard X-ray emission have been detected by BeppoSAX PDS with 2 sigma significance level. Among them, Abell 2199 is unique in that it neither have a signature of cluster merger nor significant AGN activities. The HXD PIN detector can just covers the whole X-ray emission from Abell 2199, and determine photon index and flux of the hard component. The detection of hard X-ray emission from a relaxed cluster opens a new field of study in which particle accelerations occur generally in clusters even without energetic events like sub-cluster mergers. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KAWAHARADA | MADOKA | NULL | NULL | JAP | 1 | AO1 | PROBING HARD X-RAY EMISSION FROM A RELAXED CLUSTER OF GALAXIES | HXD | Y |
| ABELL 2199 OFFSET 3 | 247.3596 | 39.3165 | 62.61707687 | 43.53145251 | 252.4737 | 54012.1589351852 | 54012.6786921296 | 801059010 | 25246.7 | 25000 | 25246.7 | 25246.7 | 25246.7 | 25246.7 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 20505 | 20505 | 44887.9 | 1 | PROCESSED | 57535.7507291667 | 54735 | 54025.4730092593 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010138 | Detection of hard X-ray emission from clusters of Galaxies is one of the top goals of Suzaku. For this purpose, we propose 5 pointing observations of Abell 2199 each of which is 25 ks. Abell 2199 is one of objects from which significant hard X-ray emission have been detected by BeppoSAX PDS with 2 sigma significance level. Among them, Abell 2199 is unique in that it neither have a signature of cluster merger nor significant AGN activities. The HXD PIN detector can just covers the whole X-ray emission from Abell 2199, and determine photon index and flux of the hard component. The detection of hard X-ray emission from a relaxed cluster opens a new field of study in which particle accelerations occur generally in clusters even without energetic events like sub-cluster mergers. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KAWAHARADA | MADOKA | NULL | NULL | JAP | 1 | AO1 | PROBING HARD X-RAY EMISSION FROM A RELAXED CLUSTER OF GALAXIES | HXD | Y |
| ABELL 2199 OFFSET 4 | 247.0296 | 39.3161 | 62.60481799 | 43.78660639 | 250.4756 | 54012.6800462963 | 54013.3044444444 | 801060010 | 24454.6 | 25000 | 24470.6 | 24462.6 | 24454.6 | 24477.5 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 25811 | 25811 | 53939.9 | 0 | PROCESSED | 57535.7612615741 | 54735 | 54024.6738888889 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010138 | Detection of hard X-ray emission from clusters of Galaxies is one of the top goals of Suzaku. For this purpose, we propose 5 pointing observations of Abell 2199 each of which is 25 ks. Abell 2199 is one of objects from which significant hard X-ray emission have been detected by BeppoSAX PDS with 2 sigma significance level. Among them, Abell 2199 is unique in that it neither have a signature of cluster merger nor significant AGN activities. The HXD PIN detector can just covers the whole X-ray emission from Abell 2199, and determine photon index and flux of the hard component. The detection of hard X-ray emission from a relaxed cluster opens a new field of study in which particle accelerations occur generally in clusters even without energetic events like sub-cluster mergers. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KAWAHARADA | MADOKA | NULL | NULL | JAP | 1 | AO1 | PROBING HARD X-RAY EMISSION FROM A RELAXED CLUSTER OF GALAXIES | HXD | Y |
| A2256 | 256.0138 | 78.7112 | 111.08264828 | 31.72462704 | 207.9671 | 54049.8560069445 | 54052.0834722222 | 801061010 | 95511.1 | 100000 | 95511.1 | 95511.1 | 0 | 95511.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 103578.9 | 103578.9 | 192441.8 | 4 | PROCESSED | 57536.1203009259 | 54456 | 54089.4338425926 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010139 | A2256 is a nearby (z=0.058) rich cluster with strong X-ray emission. The cluster has variety of indications of a on-going merger; two peaks separated by 3.5 arcmin are clearly visible near the center of X-ray emission, gas temperature map show sub structure and a cold front etc. The velocity distribution of member galaxies also exhibits two or three sub groups in this cluster. We measure the bulk motion of the hot gas using Suzaku XIS, in particular, about 2000km/s velocity difference between the main-cluster and the sub-cluster is the target. We also aim to search for hard X-ray emission claimed by previous missions with Suzaku HXD. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | HAYASHIDA | KIYOSHI | NULL | NULL | JAP | 1 | AO1 | BULK MOTION AND NON THERMAL PROCESS IN THE MERGING CLUSTER A2256 | XIS | N |
| A1674 | 195.9676 | 67.5471 | 121.10331631 | 49.53698634 | 114.9985 | 54085.1434837963 | 54087.0426388889 | 801062010 | 68413.8 | 100000 | 68421.8 | 68421.8 | 0 | 68413.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 109013.1 | 109013.1 | 164064 | 2 | PROCESSED | 57536.3777546296 | 54750 | 54094.6003935185 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 010156 | A1674 is a nearby (z=0.106) richness class 3 clsuter with Abell galaxy count of 165, while its X-ray luminsity is as low as 6e43erg/s. We have observed this cluster with ASCA and XMM-Newton, and found iregular extended X-ray emission. The X-ray spectrum can be fitted with a thin thermal model of kT ~ 3keV, but the metal abundance is 0.07 with upper limit of 0.2. We assume this cluster may be a cluster under construction. Utilizing the low background level and high sensitivity of Suzaku XIS, we aim to obtain accurate X-ray spectrum of this cluster to constrain the metal abndance of each species. We also examine possible contribution of diffuse non-thermal emission in cluster scale. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | HAYASHIDA | KIYOSHI | NULL | NULL | JAP | 1 | AO1 | METAL DEFICIENT GAS OR NON THERMAL EMISSION? DIFFUSE X-RAYS IN A1674 | XIS | Y |
| M101 | 210.8841 | 54.3679 | 101.97854462 | 59.72940376 | 150.2959 | 54062.5790625 | 54064.7182175926 | 801063010 | 98852.2 | 100000 | 98876.2 | 98852.2 | 0 | 98876.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 89612.5 | 89612.5 | 184802 | 2 | PROCESSED | 57536.2145486111 | 54455 | 54088.707650463 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011402 | We wish to obtain a Suzaku spectrum of the diffuse X-ray emission in a typical galactic disk. The spectral resolution obtainable with Chandra/XMM does not allow the decomposition of the spectrum into more than two thermal components. The higher spectral resolution, better soft response, and lower instrumental background of Suzaku will allow the decomposition into at least three thermal components, and will place constraints on the number of thermal components and the distribution of temperatures and emission measures. The more refined fitting allowed by Suzaku spectra will allow a greater understanding of the sources of the X-ray emission. Given the Suzaku spatial resolution and detector size, M101 is the best observable example of a "typical" galactic disk. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KUNTZ | K. | NULL | NULL | USA | 1 | AO1 | SOFT DIFFUSE X-RAY EMISSION FROM M101 | XIS | N |
| NGC 4472 | 187.4441 | 8.005 | 286.9163593 | 70.20028227 | 117.8054 | 54072.8427893518 | 54075.7014699074 | 801064010 | 121035.8 | 120000 | 121035.8 | 121035.8 | 0 | 121035.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 103446.4 | 103446.4 | 246954.8 | 6 | PROCESSED | 57536.3089467593 | 54702 | 54089.1857523148 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011403 | We propose Suzaku observations of a sample of bright elliptical galaxies, with a preference toward galaxies that have (or potentially have) high quality XMM-Newton RGS data, as part of a program to investigate their star formation history and chemical evolution via abundance studies of the hot interstellar medium. Joint XIS/RGS analysis enables one to directly account for the effects of resonance scattering and thermal structure in order to minimize degeneracies in the abundance estimates. At the same time, the incidence of resonance scattering serves as an indicator of the prevalence and causes of ISM turbulence. The unprecedented opportunity to measure and map oxygen abundances afforded by the XIS is key to constraining nucleosynthetic origins and enrichment mechanisms. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | LOEWENSTEIN | MICHAEL | NULL | NULL | USA | 1 | AO1 | INVESTIGATING THE CHEMICAL EVOLUTION OF ELLIPTICAL GALAXIES WITH SUZAKU | XIS | Y |
| NGC 4649 | 190.9148 | 11.557 | 295.86493189 | 74.32191724 | 113.3108 | 54098.4203703704 | 54104.1473263889 | 801065010 | 224030.4 | 120000 | 224030.4 | 224030.4 | 0 | 224030.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26304.2 | 26304.2 | 69289.8 | 1 | PROCESSED | 57536.4300578704 | 54743 | 54132.9809027778 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011403 | We propose Suzaku observations of a sample of bright elliptical galaxies, with a preference toward galaxies that have (or potentially have) high quality XMM-Newton RGS data, as part of a program to investigate their star formation history and chemical evolution via abundance studies of the hot interstellar medium. Joint XIS/RGS analysis enables one to directly account for the effects of resonance scattering and thermal structure in order to minimize degeneracies in the abundance estimates. At the same time, the incidence of resonance scattering serves as an indicator of the prevalence and causes of ISM turbulence. The unprecedented opportunity to measure and map oxygen abundances afforded by the XIS is key to constraining nucleosynthetic origins and enrichment mechanisms. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | LOEWENSTEIN | MICHAEL | NULL | NULL | USA | 1 | AO1 | INVESTIGATING THE CHEMICAL EVOLUTION OF ELLIPTICAL GALAXIES WITH SUZAKU | XIS | Y |
| UGC03957 | 115.2433 | 55.429 | 162.22286538 | 28.93195726 | 271.243 | 53841.9927314815 | 53842.2828587963 | 801072010 | 10771.4 | 12000 | 10779.4 | 10779.4 | 10787.4 | 10771.4 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 9642 | 9642 | 25007.9 | 0 | PROCESSED | 57533.4729166667 | 54401 | 53906.7753240741 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | SCHARF | CALEB | NULL | NULL | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | N |
| A2572B | 349.6066 | 18.7294 | 94.21850787 | -38.90117923 | 59.1565 | 53922.7742939815 | 53923.3002199074 | 801073010 | 24059.5 | 21000 | 24075.5 | 24059.5 | 24067.5 | 24075.5 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 21495.1 | 21495.1 | 45397.9 | 1 | PROCESSED | 57534.8583912037 | 54401 | 53930.6043055556 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | SCHARF | CALEB | NULL | NULL | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | N |
| Z8852 | 347.6318 | 7.5789 | 84.17423864 | -47.55525942 | 260.3346 | 54065.5867013889 | 54066.1543287037 | 801074010 | 14852.6 | 15000 | 14852.6 | 14852.6 | 0 | 14852.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13983.4 | 13983.4 | 49037.9 | 0 | PROCESSED | 57536.1918402778 | 54695 | 54088.6000694444 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | SCHARF | CALEB | NULL | NULL | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | Y |
| IIZW108 | 318.5228 | 2.5728 | 53.56011975 | -29.86052353 | 77.7227 | 53864.5319791667 | 53864.7883680556 | 801075010 | 11605.2 | 11000 | 11605.2 | 11605.2 | 11605.2 | 11605.2 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 9632 | 9632 | 22149.9 | 1 | PROCESSED | 57534.2579398148 | 54401 | 53913.9958564815 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | SCHARF | CALEB | NULL | NULL | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | N |
| A2665 | 357.7161 | 6.1352 | 96.94047732 | -53.65177278 | 245.9817 | 54078.2252893518 | 54078.562037037 | 801076010 | 13944 | 15000 | 13944 | 13944 | 0 | 13944 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11607.3 | 11607.3 | 29087.9 | 0 | PROCESSED | 57536.2715393518 | 54695 | 54089.271412037 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | SCHARF | CALEB | NULL | NULL | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | Y |
| A1831 | 209.8007 | 27.9693 | 40.05378223 | 74.96810077 | 288.1207 | 53937.1181828704 | 53937.5106481482 | 801077010 | 18079.6 | 18000 | 18079.6 | 18079.6 | 18079.6 | 18079.6 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 17089.1 | 17089.1 | 33897.9 | 1 | PROCESSED | 57535.0011805556 | 54401 | 53943.553599537 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | SCHARF | CALEB | NULL | NULL | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | N |
| A1800 | 207.3618 | 28.0973 | 40.59651819 | 77.12066844 | 302.3644 | 53936.635625 | 53937.1140509259 | 801078010 | 20043.7 | 17000 | 20047.3 | 20055.3 | 20055.3 | 20043.7 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 19000.3 | 19000.3 | 41331.9 | 0 | PROCESSED | 57535.0036458333 | 54401 | 53943.5299652778 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | SCHARF | CALEB | NULL | NULL | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | N |
| Z8276 | 266.0474 | 32.9693 | 57.88393681 | 27.65216461 | 308.1365 | 53961.1406134259 | 53961.4723958333 | 801079010 | 14937.4 | 14000 | 14937.4 | 14937.4 | 14937.4 | 14937.4 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 15462 | 15462 | 28658 | 0 | PROCESSED | 57535.267962963 | 54391 | 54018.6023842593 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | SCHARF | CALEB | NULL | NULL | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | N |
| A2495 | 342.5777 | 10.9124 | 81.20126485 | -41.9387619 | 237.1467 | 54061.4694097222 | 54062.0787037037 | 801080010 | 18031.3 | 18000 | 18031.3 | 18367.3 | 0 | 18119.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16389.1 | 16389.1 | 52633.9 | 3 | PROCESSED | 57536.1381365741 | 54695 | 54088.9563194444 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | SCHARF | CALEB | NULL | NULL | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | Y |
| A2495 | 342.5662 | 10.9218 | 81.19678392 | -41.92445268 | 65.1354 | 54260.5857523148 | 54261.1668287037 | 801080020 | 25780.6 | 18000 | 25780.6 | 25780.6 | 0 | 25780.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20976.2 | 20976.2 | 50195.9 | 2 | PROCESSED | 57538.8757291667 | 54695 | 54270.430625 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | SCHARF | CALEB | NULL | NULL | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | Y |
| A2061 | 230.3095 | 30.6453 | 48.13899774 | 57.1713197 | 293.2901 | 53943.6955092593 | 53943.9946643518 | 801081010 | 13888.7 | 14000 | 13904.7 | 13904.7 | 13888.7 | 13896.7 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 11844.3 | 11844.3 | 25839.9 | 0 | PROCESSED | 57535.0552083333 | 54401 | 53955.6442939815 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | SCHARF | CALEB | NULL | NULL | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | N |
| A2249 | 257.46 | 34.4851 | 57.64541352 | 34.94797305 | 129.9858 | 54114.5939467593 | 54115.1252777778 | 801082010 | 22815.6 | 15000 | 22815.6 | 22823.6 | 0 | 22823.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 19763.7 | 19763.7 | 45903.9 | 1 | PROCESSED | 57536.8308333333 | 54695 | 54133.0295833333 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | SCHARF | CALEB | NULL | NULL | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | Y |
| Z235 | 10.9622 | 24.4059 | 120.72614401 | -38.43334342 | 59.0539 | 53944.0060185185 | 53944.6148032407 | 801083010 | 20033.5 | 20000 | 20041.5 | 20041.5 | 20041.5 | 20033.5 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 19526.3 | 19526.3 | 52589.9 | 1 | PROCESSED | 57535.0666782407 | 54401 | 53955.6800925926 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | SCHARF | CALEB | NULL | NULL | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | N |
| A272 | 28.7603 | 33.9026 | 137.73606223 | -27.1341127 | 64.9465 | 53943.0449537037 | 53943.6842476852 | 801084010 | 22245.5 | 21000 | 22253.5 | 22253.5 | 22245.5 | 22253.5 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 24603.5 | 24603.5 | 55231.9 | 0 | PROCESSED | 57535.0602430556 | 54401 | 53955.6516782407 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | SCHARF | CALEB | NULL | NULL | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | N |
| A566 | 106.0915 | 63.2647 | 152.76309519 | 25.45548296 | 285.637 | 54178.3128587963 | 54178.8029976852 | 801085010 | 22271.1 | 20000 | 22271.1 | 22271.1 | 0 | 22271.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22152.3 | 22152.3 | 42339.9 | 0 | PROCESSED | 57537.7151157407 | 54695 | 54185.9799305556 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011422 | We propose obtaining the first pointed X-ray spectroscopic imaging data on 14 nearby, luminous - otherwise overlooked - galaxy clusters which complete a statistical sample of 61 low-redshift objects spanning two orders of magnitude in luminosity. This unique sample, comprising Suzaku, Chandra, XMM-Newton, and ASCA data will not only allow a thorough investigation of outstanding questions on ICM physics but will also ensure that subsequent multi-wavelength studies of cluster evolution at higher redshift can be adequately calibrated as probes of cosmology. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | SCHARF | CALEB | NULL | NULL | USA | 1 | AO1 | A ZERO-REDSHIFT GALAXY CLUSTER BASELINE | XIS | Y |
| RXJ 0658 | 104.704 | -55.933 | 266.02429497 | -21.20357002 | 164.9362 | 54095.6181597222 | 54098.4099421296 | 801089010 | 101384.5 | 100000 | 101384.5 | 101384.5 | 0 | 101384.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 84367.9 | 84367.9 | 241154.7 | 2 | PROCESSED | 57637.5971180556 | 54702 | 54111.5842013889 | 3.0.22.44 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 011448 | We propose SUZAKU X-ray observations of an intriguing cluster of galaxies, RXJ0658, to determine and characterize the nature of the hard X-ray spectral emission and other nonthermal activity. It also has many other interesting features, such as a cold front, evidence for merger, a shock, and regions of unusually high temperature, all of which are related to the hard X-ray emission and the nonthermal activity. The more accurate measure of the spectral characteristics of the hard component, when combined with the radio and other past X-ray data, can reveal the nature of the emission process and the acceleration mechanism of the relativistic electrons, provide a means of measuring the magnetic field strength, and aid in understanding the process of formation of clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | PETROSIAN | VAHE | NULL | NULL | USA | 1 | AO1 | HARD X-RAY EMISSION FROM CLUSTER RXJ0658 | HXD | Y |
| SN 1987A | 83.9013 | -69.2655 | 279.69660922 | -31.92548266 | 330.0004 | 53894.6930555556 | 53895.6683449074 | 801090010 | 39646.4 | 40000 | 39646.4 | 39646.4 | 39646.4 | 39646.4 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 39251.9 | 39251.9 | 84239.9 | 0 | PROCESSED | 57534.6267592593 | 54400 | 53928.1346527778 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012006 | In an early Suzaku observation during the SWG time in November 2005 we have already obtained an excellent XIS spectrum. The flux of SN 1987A continues to rise exponentially with an e-folding time of ~800 days. The abundances in the ejecta could be measured with unprecedented accuracy. We confirm that Oxygen and Iron are significantly underabundant with respect to other elements, indicating the formation of dust, maybe even black rust grains (Fe3O4). We propose to monitor the chemical evolution of SN 1987A with Suzaku for 40 ksec in AO-1, where we expect about twice the previous flux. The exponential brightening and the chemical abundance is expected to change, when the full inner ring is engulfed. Simultaneously we can search for a periodic hard signal from the putative pulsar. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | HASINGER | G NTHER | NULL | NULL | EUR | 1 | AO1 | SN 1987A - A RUSTY REMNANT? | XIS | N |
| ABELL 2204 | 248.0963 | 5.6404 | 21.10023438 | 33.35451369 | 261.3606 | 53995.3098958333 | 53996.5098958333 | 801091010 | 49111.3 | 55000 | 49111.3 | 49111.3 | 49111.3 | 49111.3 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 51937.2 | 51937.2 | 103643.9 | 1 | PROCESSED | 57535.6038194444 | 54526 | 54020.8840277778 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012018 | Measurements of the intracluster gas temperatures out to large radii, where most of the cluster mass resides, are of the utmost importance for the use of clusters in precision cosmology and for studies of cluster physics. Previous attempts to measure temperatures at the cluster virial radius have failed. Here we show that such measurements appear feasible now for the first time with the Suzaku X-ray CCDs. Furthermore, we show that A2204 and A2163 are optimal targets for such an investigation. We, therefore, propose to observe A2204 for 55 ks and A2163 for 100 ks to measure the gas temperature to 10% and 15% accuracy (1-sigma), respectively, out to the cluster virial radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | REIPRICH | THOMAS | NULL | NULL | EUR | 1 | AO1 | A2204 AND A2163: GALAXY CLUSTER GAS TEMPERATURE MEASUREMENT UP TO THE VIRIAL RADIUS | SPE | N |
| SERSIC 159-03 | 348.4959 | -42.7314 | 348.33340728 | -64.81387916 | 47.3295 | 53851.5323611111 | 53853.2668055556 | 801093010 | 67784.3 | 70000 | 67800.3 | 67800.3 | 67784.3 | 67792.3 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 41583.3 | 41583.3 | 149827.8 | 2 | PROCESSED | 57533.6210532407 | 54400 | 53907.8625231482 | 3.0.22.43 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 012045 | We propose to observe the cluster of galaxies Sersic 159-03 using a total exposure time of 70 ks to investigate the soft excess emission previously detected in the observations with ROSAT and XMM-Newton. The superior redistribution function of Suzaku will allow us to determine whether the O VII line emission detected with XMM-Newton is of local (Galactic) origin or is emitted by the warm-hot intergalactic medium (WHIM) in the vicinity of the cluster. The strong soft emission around this cluster together with the much improved response function of the XIS detectors at low energies make Sersic 159-03 the most promising target to unambiguously detect the WHIM for the first time in emission with Suzaku. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KAASTRA | JELLE | NULL | NULL | EUR | 1 | AO1 | O VII LINE EMISSION IN SERSIC 159-03 - WHIM OR GALACTIC ORIGIN? | XIS | N |
| A3667_NW_RELIC | 302.5617 | -56.3599 | 341.42703548 | -33.08195751 | 74.7123 | 53858.7409837963 | 53861.2933449074 | 801094010 | 94394.6 | 95000 | 94402.6 | 94394.6 | 94394.6 | 94402.6 | 3 | 3 | 3 | 3 | 1 | 0 | 0 | 56250.6 | 56250.6 | 220489 | 4 | PROCESSED | 57533.7274074074 | 54394 | 53913.7574189815 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 013080 | We propose to observe along the north west relic of Abell 3667 cluster. The aim of this observation is to obtain a high quality hard X-ray spectra of the NW relic, utlizing the high sensitivity and norrow field of view of the HXD detector, as well as the high sensitivity of the XIS to widely diffuse souces. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | NAKAZAWA | KAZUHIRO | SARAZIN | CRAIG | JUS | 1 | AO1 | SUZAKU OBSERVATION OF A MERGING CLUSTER ABELL 3667 | HXD | N |
| A3667_NW_17OFF | 302.8177 | -56.56 | 341.18808838 | -33.22347241 | 74.1682 | 53861.293912037 | 53861.7356944444 | 801095010 | 17258.6 | 20000 | 17282.6 | 17274.6 | 17266.6 | 17258.6 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 14255.5 | 14255.5 | 38151.9 | 1 | PROCESSED | 57533.636099537 | 54735 | 53913.7593518518 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 013080 | We propose to observe along the north west relic of Abell 3667 cluster. The aim of this observation is to obtain a high quality hard X-ray spectra of the NW relic, utlizing the high sensitivity and norrow field of view of the HXD detector, as well as the high sensitivity of the XIS to widely diffuse souces. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | NAKAZAWA | KAZUHIRO | SARAZIN | CRAIG | JUS | 1 | AO1 | SUZAKU OBSERVATION OF A MERGING CLUSTER ABELL 3667 | HXD | N |
| A3667_NW_17OFF | 302.869 | -56.6666 | 341.06051648 | -33.2513141 | 258.9342 | 54038.8325578704 | 54039.0106944444 | 801095020 | 11963.4 | 10000 | 11979.4 | 11979.4 | 11963.4 | 11971.4 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 8724 | 8724 | 15383.9 | 0 | PROCESSED | 57535.9848032407 | 54735 | 54056.1858796296 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 013080 | We propose to observe along the north west relic of Abell 3667 cluster. The aim of this observation is to obtain a high quality hard X-ray spectra of the NW relic, utlizing the high sensitivity and norrow field of view of the HXD detector, as well as the high sensitivity of the XIS to widely diffuse souces. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | NAKAZAWA | KAZUHIRO | SARAZIN | CRAIG | JUS | 1 | AO1 | SUZAKU OBSERVATION OF A MERGING CLUSTER ABELL 3667 | HXD | Y |
| A3667_CENTER | 303.141 | -56.7974 | 340.90266514 | -33.39955413 | 74.263 | 53861.7363078704 | 53862.3843055556 | 801096010 | 20880.5 | 20000 | 20888.5 | 20888.5 | 20896.5 | 20880.5 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 8425 | 8425 | 55943.9 | 1 | PROCESSED | 57533.6497337963 | 54394 | 53913.7840509259 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 013080 | We propose to observe along the north west relic of Abell 3667 cluster. The aim of this observation is to obtain a high quality hard X-ray spectra of the NW relic, utlizing the high sensitivity and norrow field of view of the HXD detector, as well as the high sensitivity of the XIS to widely diffuse souces. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | NAKAZAWA | KAZUHIRO | SARAZIN | CRAIG | JUS | 1 | AO1 | SUZAKU OBSERVATION OF A MERGING CLUSTER ABELL 3667 | HXD | N |
| COMA RADIO HALO | 194.9267 | 27.9061 | 56.39742233 | 88.00849705 | 295.2687 | 53886.8435300926 | 53890.7439699074 | 801097010 | 178657.2 | 180000 | 178689.2 | 178657.2 | 178713.2 | 178689.2 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 167450.6 | 167450.6 | 336975.8 | 7 | PROCESSED | 57534.5953472222 | 54401 | 53926.6760416667 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 014446 | We will observe the central regions of the Coma cluster with the HXD/PIN to detect and characterize the nonthermal Inverse Compton (IC) emission from the radio halo. Coma has the best-studied and brightest radio halo, which makes it the best case to detect IC and the most useful one for testing theories for the origin of radio halos. Previous detections with BeppoSAX and RXTE are controversial. Suzaku is more sensitive, will avoid contamination by nearby AGNs including X Comae, and will detect IC even if it is fainter than the claimed BeppoSAX detection. The HXD/PIN data will allow the cluster magnetic field, and nonthermal energy and pressure to be derived. The XIS observations will be used to determine accurate abundances and gradients in Coma, and to test theories for ICM enrichment. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SARAZIN | CRAIG | MATSUSHITA | KYOKO | USJ | 1 | AO1 | NAILING DOWN THE HARD X-RAY INVERSE COMPTON EMISSION FROM THE RADIO HALO IN THE COMA CLUSTER | HXD | N |
| ABELL 262 CENTER | 28.1922 | 36.1591 | 136.56609466 | -25.08359968 | 69.9979 | 54329.1761921296 | 54330.0446643518 | 802001010 | 37164.5 | 36000 | 37164.5 | 37164.5 | 0 | 37164.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34130.4 | 34130.4 | 75029.9 | 1 | PROCESSED | 57539.6070949074 | 54730 | 54350.5576851852 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020004 | We propose to observe Abell 262. The temperature of the intracluster mediums of the cluster is 2 keV and therefore this cluster is between groups of galaxies and clusters of galaxies. The purpuse of the observation is to determine the distribution of O, Mg, Si and Fe f the intracluster medium upto 0.3 r180. The exposures are 30 ks for the central pointing and 40 ks for two offset pointings and the total exposure is 110ks. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MATSUSHITA | KYOKO | NULL | NULL | JAP | 2 | AO2 | O AND MG ABUNDANCES OF THE INTRACLUSTER MEDIUMS OF ABELL 262 | XIS | Y |
| 3EGJ1234 1318_3 | 188.2697 | -13.5708 | 296.11455637 | 49.05777767 | 113.9119 | 54445.0609375 | 54445.8543171296 | 802004010 | 1602 | 30000 | 1602 | 29779.4 | 0 | 29779.4 | 1 | 2 | 0 | 2 | 1 | 0 | 0 | 26304.8 | 26304.8 | 68519.8 | 0 | PROCESSED | 57637.5213888889 | 54999 | 54633.6933217593 | 3.0.22.44 | 5 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020007 | We propose observations around 3EG J1234 1318, which is one of the EGRET un-ID sources. From recent optical survey, it is found that the source is located around a large scale structure at z ~ 0.1. We propose a scenario that the GeV source is originating from a large shock wave within the structure formation. The XIS and the HXD provides a probe for thermal shock plasma and non-thermal IC emission, respectively. This observation will solve some questions on EGRET un-ID sources. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TOTANI | TOMONORI | NULL | NULL | JAP | 2 | AO2 | CONFIRMING GAMMA-RAY EMISSION FROM INTERGALACTIC SHOCKS: A NEW WINDOW TO STUDY THE COSMIC STRUCTURE FORMATION | HXD | Y |
| 3EGJ1234 1318_4 | 188.5214 | -13.4715 | 296.47032219 | 49.18242085 | 113.9125 | 54445.8547453704 | 54446.4655555556 | 802005010 | 20139.2 | 20000 | 0 | 20139.2 | 0 | 20155.2 | 0 | 2 | 0 | 2 | 1 | 0 | 0 | 20006.4 | 20006.4 | 52771.9 | 0 | PROCESSED | 57540.846875 | 55000 | 54633.6925347222 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020007 | We propose observations around 3EG J1234 1318, which is one of the EGRET un-ID sources. From recent optical survey, it is found that the source is located around a large scale structure at z ~ 0.1. We propose a scenario that the GeV source is originating from a large shock wave within the structure formation. The XIS and the HXD provides a probe for thermal shock plasma and non-thermal IC emission, respectively. This observation will solve some questions on EGRET un-ID sources. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TOTANI | TOMONORI | NULL | NULL | JAP | 2 | AO2 | CONFIRMING GAMMA-RAY EMISSION FROM INTERGALACTIC SHOCKS: A NEW WINDOW TO STUDY THE COSMIC STRUCTURE FORMATION | HXD | Y |
| CEN45 | 192.5119 | -41.3865 | 302.65166747 | 21.4844922 | 104.7288 | 54458.1467939815 | 54459.2294444444 | 802008010 | 58222.6 | 53000 | 58222.6 | 58236.5 | 0 | 58230.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 64517.1 | 64517.1 | 93521.8 | 2 | PROCESSED | 57540.9525810185 | 54854 | 54486.1941087963 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020011 | We propose to obtain high-quality X-ray spectra of the subcluster region in the Centaurus cluster, Cen45, aiming at the first reliable detection of a supersonic motion of the intracluster gas. Previous optical and X-ray observations suggest that Cen45 is indeed in the process of merging and has a high velocity relative to the main cluster. Utilizing the high-sensitivity Suzaku/XIS spectroscopy, the line-of-sight velocity of the X-ray emitting gas can be accurately measured from the Doppler shift of iron-K lines. With our proposed 40ks observation, we can put a strong constraint on the gas motion in the subcluster region. This will also have great impacts on our understanding of dynamical state of clusters and their evolution. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | OTA | NAOMI | NULL | NULL | JAP | 2 | AO2 | MEASURING GAS MOTIONS OF THE INFALLING SUBCLUSTER CEN45 | XIS | Y |
| A963N | 154.2645 | 39.1732 | 182.34163859 | 55.82043448 | 108.9136 | 54428.4751041667 | 54429.0522453704 | 802010010 | 29131.8 | 25000 | 29131.8 | 29141.3 | 0 | 29135.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27884.3 | 27884.3 | 49838.1 | 0 | PROCESSED | 57540.5914351852 | 54804 | 54434.2199305556 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020018 | We propose to perform spatially resolved spectroscopy on relaxed clusters of galaxies A2104, A963 and A2261 to map their temperature out to the virial radius r_178 with 10% precision in a few arcmin scale, which has not been done before to any cluster. Combined with Chandra imaging of these clusters, the proposed measurements will be used for accurate virial and baryonic mass estimation assuming hydrostatic equilibrium. We use this information to calibrate the cluster M-T and L-T scaling relations, and their evolution. We will constrain the cosmological parameters Omega_M and Omega_Lambda via the baryonic fraction and the mass function. Due to the stable and low background of XIS detectors, with Suzaku it is possible to perform this challenging and cosmologically important task. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | HATTORI | MAKOTO | NULL | NULL | JAP | 2 | AO2 | TEMPERATURE PROFILES OF RELAXED CLUSTERS OF GALAXIES OUT TO VIRIAL RADIUS | XIS | Y |
| A963E | 154.4148 | 39.0556 | 182.51717965 | 55.95361494 | 109.3314 | 54427.8082060185 | 54428.4745833333 | 802011010 | 29082.5 | 25000 | 29082.5 | 29082.5 | 0 | 29082.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 24469.9 | 24469.9 | 57567.9 | 0 | PROCESSED | 57540.5746412037 | 54804 | 54434.1859837963 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020018 | We propose to perform spatially resolved spectroscopy on relaxed clusters of galaxies A2104, A963 and A2261 to map their temperature out to the virial radius r_178 with 10% precision in a few arcmin scale, which has not been done before to any cluster. Combined with Chandra imaging of these clusters, the proposed measurements will be used for accurate virial and baryonic mass estimation assuming hydrostatic equilibrium. We use this information to calibrate the cluster M-T and L-T scaling relations, and their evolution. We will constrain the cosmological parameters Omega_M and Omega_Lambda via the baryonic fraction and the mass function. Due to the stable and low background of XIS detectors, with Suzaku it is possible to perform this challenging and cosmologically important task. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | HATTORI | MAKOTO | NULL | NULL | JAP | 2 | AO2 | TEMPERATURE PROFILES OF RELAXED CLUSTERS OF GALAXIES OUT TO VIRIAL RADIUS | XIS | Y |
| A963S | 154.2641 | 38.9388 | 182.75442962 | 55.85527134 | 107.1093 | 54432.4435300926 | 54432.9584953704 | 802012010 | 27717.2 | 25000 | 27725.2 | 27725.2 | 0 | 27717.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25654.6 | 25654.6 | 44492 | 1 | PROCESSED | 57540.6110185185 | 54811 | 54440.9716319444 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020018 | We propose to perform spatially resolved spectroscopy on relaxed clusters of galaxies A2104, A963 and A2261 to map their temperature out to the virial radius r_178 with 10% precision in a few arcmin scale, which has not been done before to any cluster. Combined with Chandra imaging of these clusters, the proposed measurements will be used for accurate virial and baryonic mass estimation assuming hydrostatic equilibrium. We use this information to calibrate the cluster M-T and L-T scaling relations, and their evolution. We will constrain the cosmological parameters Omega_M and Omega_Lambda via the baryonic fraction and the mass function. Due to the stable and low background of XIS detectors, with Suzaku it is possible to perform this challenging and cosmologically important task. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | HATTORI | MAKOTO | NULL | NULL | JAP | 2 | AO2 | TEMPERATURE PROFILES OF RELAXED CLUSTERS OF GALAXIES OUT TO VIRIAL RADIUS | XIS | Y |
| FORNAX CLUSTER N30' | 54.7324 | -34.9521 | 235.87381769 | -53.55297023 | 245 | 54479.2031134259 | 54480.3542708333 | 802021010 | 55810.7 | 53000 | 55810.7 | 55810.7 | 0 | 55810.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 58344.1 | 58344.1 | 99443.8 | 2 | PROCESSED | 57541.3134259259 | 54864 | 54490.3658680556 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020038 | To study chemical evolution of groups and clusters of galaxies, observations of outer regions are the most important. The surface brightness of these regions is very low. Thereofre, to derive metal abundances of the intracluster medium, Suzaku has an advantage due to its low stable background. We propose to observe two groups of galaxies and 1 clusters of galaxies whose central regions were observed during SWG time. The total exposure is 180 ks, with 5 pointings. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MATSUSHITA | KYOKO | NULL | NULL | JAP | 2 | AO2 | DETERMINATION OF METAL ABUNDANCES OF OUTSKIRTS OF CLUSTERS AND GROUPS OF GALAXIES | XIS | Y |
| NGC 4636 NORTH | 190.6832 | 3.0555 | 297.61641621 | 65.83736523 | 111.9967 | 54441.2091087963 | 54443.0530555556 | 802022010 | 71429.4 | 67000 | 0 | 71429.4 | 0 | 71429.4 | 0 | 2 | 0 | 2 | 1 | 0 | 0 | 61781 | 61781 | 159310.1 | 3 | PROCESSED | 57540.8428703704 | 55000 | 54633.6943402778 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020038 | To study chemical evolution of groups and clusters of galaxies, observations of outer regions are the most important. The surface brightness of these regions is very low. Thereofre, to derive metal abundances of the intracluster medium, Suzaku has an advantage due to its low stable background. We propose to observe two groups of galaxies and 1 clusters of galaxies whose central regions were observed during SWG time. The total exposure is 180 ks, with 5 pointings. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MATSUSHITA | KYOKO | NULL | NULL | JAP | 2 | AO2 | DETERMINATION OF METAL ABUNDANCES OF OUTSKIRTS OF CLUSTERS AND GROUPS OF GALAXIES | XIS | Y |
| A1060_OFFSET | 159.8425 | -27.5312 | 270.15539037 | 26.80693828 | 96.4852 | 54425.0245486111 | 54427.7988888889 | 802028010 | 103799.3 | 100000 | 103799.3 | 103799.3 | 0 | 103799.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 89111.9 | 89111.9 | 239679.7 | 2 | PROCESSED | 57540.6102662037 | 54804 | 54434.2515509259 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020060 | We propose to observe a 30' offset region of the cluster of galaxies Abell 1060 for 100 ksec to study the temperature and abundance profiles. The central region within ~0.3 times the virial radius, or 380 kpc, has been already observed as one of the SWG targets, and the temperature decrease and differnt profiles of metal abundances are clealy observed (Sato et al. 2006). This observation will reveal the temperature and abundance profiles to half the virial radius. Comparison of the abundance profiles will tell us how metals produced by type Ia and II supernovae have been enriched in the outer cluster region. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | SATO | KOSUKE | NULL | NULL | JAP | 2 | AO2 | TEMPERATURE AND ABUNDANCE PROFILES IN THE OUTER REGION OF THE NON-CD CLUSTER A1060 | XIS | Y |
| A2142 OFFSET1 | 239.3897 | 27.3899 | 44.41448178 | 48.88746657 | 283.7323 | 54316.0523726852 | 54317.0211226852 | 802030010 | 37622.7 | 30000 | 37630.7 | 37622.7 | 0 | 37630.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 29667.7 | 29667.7 | 83687.9 | 1 | PROCESSED | 57539.4231134259 | 54723 | 54347.3816087963 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020076 | We propose to search for redshifted OVII and OVIII lines from the warm-hot intergalactic medium (WHIM) in a large-scale filament outside of a massive merging cluster of galaxies A2142. This cluster is characterized by prominent cold fronts, elongated X-ray morphology, and Beppo-SAX detection of hard X-ray emission, which all point to a recent merger and the matter density outside should be high. The strong reason why we choose this target is its right redshift (z=0.909), in which XIS sensitivity for redshifted oxygen lines separated from the Galactic lines becomes the highest. We expect 3 times higher sensitivity than our previous attempt for A2218 (Takei et al. in press) where we set 5 times lower upper limit for OVII line intensity than the XMM reported levels in other clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | OHASHI | TAKAYA | NULL | NULL | JAP | 2 | AO2 | WHIM SEARCH AROUND A MASSIVE MERGING CLUSTER OF GALAXIES A2142 | XIS | Y |
| A2142 OFFSET2 | 239.2185 | 27.5666 | 44.63617571 | 49.06945571 | 260.7114 | 54358.4806597222 | 54360.0627893518 | 802031010 | 57718.7 | 50000 | 57718.7 | 57718.7 | 0 | 57718.7 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 52597.6 | 52597.6 | 136631.8 | 1 | PROCESSED | 57539.9791666667 | 54751 | 54371.4005208333 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020076 | We propose to search for redshifted OVII and OVIII lines from the warm-hot intergalactic medium (WHIM) in a large-scale filament outside of a massive merging cluster of galaxies A2142. This cluster is characterized by prominent cold fronts, elongated X-ray morphology, and Beppo-SAX detection of hard X-ray emission, which all point to a recent merger and the matter density outside should be high. The strong reason why we choose this target is its right redshift (z=0.909), in which XIS sensitivity for redshifted oxygen lines separated from the Galactic lines becomes the highest. We expect 3 times higher sensitivity than our previous attempt for A2218 (Takei et al. in press) where we set 5 times lower upper limit for OVII line intensity than the XMM reported levels in other clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | OHASHI | TAKAYA | NULL | NULL | JAP | 2 | AO2 | WHIM SEARCH AROUND A MASSIVE MERGING CLUSTER OF GALAXIES A2142 | XIS | Y |
| A2142 OFFSET3 | 239.0356 | 27.7434 | 44.85726257 | 49.26078026 | 283.7312 | 54341.8454166667 | 54342.3960532407 | 802032010 | 23789.9 | 20000 | 23789.9 | 23789.9 | 0 | 23789.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14242.5 | 14242.5 | 47569.9 | 0 | PROCESSED | 57539.8930671296 | 54724 | 54356.294849537 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020076 | We propose to search for redshifted OVII and OVIII lines from the warm-hot intergalactic medium (WHIM) in a large-scale filament outside of a massive merging cluster of galaxies A2142. This cluster is characterized by prominent cold fronts, elongated X-ray morphology, and Beppo-SAX detection of hard X-ray emission, which all point to a recent merger and the matter density outside should be high. The strong reason why we choose this target is its right redshift (z=0.909), in which XIS sensitivity for redshifted oxygen lines separated from the Galactic lines becomes the highest. We expect 3 times higher sensitivity than our previous attempt for A2218 (Takei et al. in press) where we set 5 times lower upper limit for OVII line intensity than the XMM reported levels in other clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | OHASHI | TAKAYA | NULL | NULL | JAP | 2 | AO2 | WHIM SEARCH AROUND A MASSIVE MERGING CLUSTER OF GALAXIES A2142 | XIS | Y |
| ABELL 2744 | 3.5397 | -30.3446 | 9.24871336 | -81.22170813 | 53.4742 | 54239.5874652778 | 54243.7709953704 | 802033010 | 153233.2 | 150000 | 153241.2 | 153241.2 | 0 | 153233.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 133863.1 | 133863.1 | 361439.8 | 2 | PROCESSED | 57538.8170138889 | 54745 | 54248.6974074074 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020077 | We propose a 150 ks Suzaku observation of Abell 2744 aiming at non-thermal hard X-ray detection. It has a red-shift of 0.3, a radio-halo flux of 57 mJy at 1.4 GHz and ICM temperature of 9 keV. Our strategy here is to observe a luminous merging cluster hosting a bright radio halo, whilst avoiding the thermal ICM emission to overwhelm the 10-40 keV band, in which the HXD has the best sensitivity. The key is to look for relatively high red-shift cluster. Since the CMB density increases as (1+z)^4, the inverse Compton emission relative to the radio flux increases typically as (1+z)^2, while the thermal ICM emission is red-shifted. We believe this is one of the best method to utilize the Suzaku power for cluster hard X-ray survey. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | NAKAZAWA | KAZUHIRO | NULL | NULL | JAP | 2 | AO2 | HARD X-RAY VIEW OF A DISTANT RADIO-HALO CLUSTER ABELL2744 | HXD | Y |
| MS 1512.4+3647 | 228.6059 | 36.6198 | 59.43888584 | 58.40149096 | 128.9265 | 54463.6508449074 | 54469.6946527778 | 802034010 | 268889.8 | 200000 | 268945.8 | 268889.8 | 0 | 268945.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47480.3 | 47480.3 | 102801.9 | 2 | PROCESSED | 57541.0217476852 | 54909 | 54542.2596296296 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020086 | Evolution of the amount of metals depends on history of super novae activities and metal tranport from inter-stellar space into the ICM. We observe a distant cluster, MS 1512+3647 (z=0.372), and determine the abundance ratio of alpha particles which are created by type II supernovae to iron by type Ia. This reveals the evolution of branch ratio of metals in a galaxy between stars and the ICM which has been unresolved observationally. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KAWAHARADA | MADOKA | NULL | NULL | JAP | 2 | AO2 | EVOLUTION STUDY ON AMOUNT OF METALS IN THE ICM USING A DISTANT CLUSTER | XIS | Y |
| ANTLIA CLUSTER | 157.5092 | -35.3277 | 272.94647188 | 19.18131972 | 90.0004 | 54423.2458796296 | 54425.0211111111 | 802035010 | 65952.8 | 60000 | 65960.8 | 65960.8 | 0 | 65952.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 58106.4 | 58106.4 | 153363.8 | 2 | PROCESSED | 57540.5835185185 | 54801 | 54433.3905092593 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020101 | Suzaku observation of the non-cD cluster Abell 1060 shows that temperature of intra-cluster medium (ICM) increases toward the center. This phenomenon is exact opposite of that of giant cD clusters, in which temperature of the ICM decreases toward the center. To explain this observation, we have proposed that galaxies moving through the ICM interact magnetohydrodynamically with the ICM. This scenario implies that the galaxies have lost some part of their kinetic energies, while the ICM received the released energies. As a result, the ICM have been efficiently heated near the center in which galaxy number density is high. To strengthen our scenario, we propose to observation and study temperature map of the Antlia cluster which is another non-cD, relaxed, and nearby (z=0.0087) cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KITAGUCHI | TAKAO | NULL | NULL | JAP | 2 | AO2 | SUZAKU OBSERVATION OF NON-CD ANTLIA CLUSTER | XIS | Y |
| FORNAX_GALACTIC_1 | 48.2958 | -37.68 | 241.51144521 | -58.49700193 | 45.4419 | 54279.8103240741 | 54280.3335532407 | 802037010 | 20417.5 | 20000 | 20417.5 | 20417.5 | 0 | 20417.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16191.2 | 16191.2 | 45184 | 0 | PROCESSED | 57539.0539814815 | 54695 | 54322.4346064815 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020119 | We propose observations of Galactic foreground emission around clusters of galaxies observed in the SWG or AO1 phase. Since the Galactic emission level is comparable to the cluster one in the cluster outskirts, spatial fluctuation of the Galactic emission would lead to a large systematic uncertainty in determining the cluster emission. To exclude the uncertainty, offset-pointing observations of the clusters are useful. We selected six clusters, with priority order, for which the offset-pointing is essential. Note that each 20--40 ks observation can sufficiently determine the Galactic emission level. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | TAKEI | YOH | NULL | NULL | JAP | 2 | AO2 | DETERMINING ACCURATE FOREGROUND GALACTIC EMISSION AROUND CLUSTERS OF GALAXIES | XIS | Y |
| A2052_GALACTIC_1 | 225.6293 | 8.2927 | 7.81905694 | 53.73503279 | 292.5625 | 54295.7150810185 | 54296.5765509259 | 802038010 | 33733.4 | 30000 | 33733.4 | 33733.4 | 0 | 33733.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 30527.2 | 30527.2 | 74423.9 | 1 | PROCESSED | 57539.2674305556 | 54709 | 54339.4114583333 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020119 | We propose observations of Galactic foreground emission around clusters of galaxies observed in the SWG or AO1 phase. Since the Galactic emission level is comparable to the cluster one in the cluster outskirts, spatial fluctuation of the Galactic emission would lead to a large systematic uncertainty in determining the cluster emission. To exclude the uncertainty, offset-pointing observations of the clusters are useful. We selected six clusters, with priority order, for which the offset-pointing is essential. Note that each 20--40 ks observation can sufficiently determine the Galactic emission level. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | TAKEI | YOH | NULL | NULL | JAP | 2 | AO2 | DETERMINING ACCURATE FOREGROUND GALACTIC EMISSION AROUND CLUSTERS OF GALAXIES | XIS | Y |
| NGC4636_GALACTIC_1 | 192.513 | 5.4558 | 301.99802564 | 68.32503562 | 300.0459 | 54268.8414930556 | 54269.9307175926 | 802039010 | 41499.7 | 30000 | 41515.7 | 41507.7 | 0 | 41499.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34337.1 | 34337.1 | 94047.9 | 0 | PROCESSED | 57553.0490393518 | 54695 | 54319.4765740741 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020119 | We propose observations of Galactic foreground emission around clusters of galaxies observed in the SWG or AO1 phase. Since the Galactic emission level is comparable to the cluster one in the cluster outskirts, spatial fluctuation of the Galactic emission would lead to a large systematic uncertainty in determining the cluster emission. To exclude the uncertainty, offset-pointing observations of the clusters are useful. We selected six clusters, with priority order, for which the offset-pointing is essential. Note that each 20--40 ks observation can sufficiently determine the Galactic emission level. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | TAKEI | YOH | NULL | NULL | JAP | 2 | AO2 | DETERMINING ACCURATE FOREGROUND GALACTIC EMISSION AROUND CLUSTERS OF GALAXIES | XIS | Y |
| FORNAX_GALACTIC_2 | 49.9904 | -32.0719 | 230.76086762 | -57.49880076 | 52.7651 | 54280.3368518518 | 54280.9897453704 | 802040010 | 21074.6 | 20000 | 21082.6 | 21082.6 | 0 | 21074.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20131 | 20131 | 56393.9 | 1 | PROCESSED | 57539.0651967593 | 54696 | 54322.4474537037 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020119 | We propose observations of Galactic foreground emission around clusters of galaxies observed in the SWG or AO1 phase. Since the Galactic emission level is comparable to the cluster one in the cluster outskirts, spatial fluctuation of the Galactic emission would lead to a large systematic uncertainty in determining the cluster emission. To exclude the uncertainty, offset-pointing observations of the clusters are useful. We selected six clusters, with priority order, for which the offset-pointing is essential. Note that each 20--40 ks observation can sufficiently determine the Galactic emission level. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | TAKEI | YOH | NULL | NULL | JAP | 2 | AO2 | DETERMINING ACCURATE FOREGROUND GALACTIC EMISSION AROUND CLUSTERS OF GALAXIES | XIS | Y |
| AWM7 EAST OFFSET | 44.9753 | 41.5792 | 147.26183994 | -15.14450792 | 259.3934 | 54492.7386458333 | 54494.7016087963 | 802044010 | 85617.7 | 80000 | 85617.7 | 85617.7 | 0 | 85617.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 80600.3 | 80600.3 | 169583.8 | 1 | PROCESSED | 57541.4783333333 | 54888 | 54515.5758796296 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020139 | The bright east-to-west elongated cluster of galaxies AWM7 lies along the large-scale filament of the Pisces-Perseus supercluster, which extends more than 50 Mpc scale. In AO1, we proposed to probe the gas motion up to 27 arcmin from the cluster center, however no significant energy shift of Fe-K line was detected so far in our preliminary results. This implies a secular asymmetric structure of the dark matter halo. We plan to extend the observation to 60 arcmin radius, which corresponds to the 0.6 times the virial radius. By making the east- and south-offset observations each in 60 ks, we intend to conduct precise measurements of temperature and metal abundances over the half virial radius for the first time. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | ISHISAKI | YOSHITAKA | NULL | NULL | JAP | 2 | AO2 | TEMPERATURE AND ABUNDAANCE OF ELONGATED CLUSTER AWM7 AT 0.6 R_180 AND POSSIBLE CONNECTION WITH SUPERCLUSTER FILAMENT | XIS | Y |
| AWM7 SOUTH OFFSET | 43.219 | 40.631 | 146.52769464 | -16.61135361 | 257.3934 | 54494.7028703704 | 54496.618275463 | 802045010 | 31295.9 | 0 | 31303.9 | 31303.9 | 0 | 31295.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 78229.8 | 78229.8 | 165471.8 | 1 | PROCESSED | 57541.4808796296 | 54888 | 54515.1834837963 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020139 | The bright east-to-west elongated cluster of galaxies AWM7 lies along the large-scale filament of the Pisces-Perseus supercluster, which extends more than 50 Mpc scale. In AO1, we proposed to probe the gas motion up to 27 arcmin from the cluster center, however no significant energy shift of Fe-K line was detected so far in our preliminary results. This implies a secular asymmetric structure of the dark matter halo. We plan to extend the observation to 60 arcmin radius, which corresponds to the 0.6 times the virial radius. By making the east- and south-offset observations each in 60 ks, we intend to conduct precise measurements of temperature and metal abundances over the half virial radius for the first time. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | ISHISAKI | YOSHITAKA | NULL | NULL | JAP | 2 | AO2 | TEMPERATURE AND ABUNDAANCE OF ELONGATED CLUSTER AWM7 AT 0.6 R_180 AND POSSIBLE CONNECTION WITH SUPERCLUSTER FILAMENT | XIS | Y |
| AWM7 SOUTH OFFSET | 43.2198 | 40.6314 | 146.52805812 | -16.61071542 | 257.3937 | 54519.4104861111 | 54521.6112847222 | 802045020 | 91227.2 | 80000 | 91227.2 | 91227.2 | 0 | 91227.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 80028.5 | 80028.5 | 190113.9 | 2 | PROCESSED | 57541.7536111111 | 54904 | 54535.283599537 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020139 | The bright east-to-west elongated cluster of galaxies AWM7 lies along the large-scale filament of the Pisces-Perseus supercluster, which extends more than 50 Mpc scale. In AO1, we proposed to probe the gas motion up to 27 arcmin from the cluster center, however no significant energy shift of Fe-K line was detected so far in our preliminary results. This implies a secular asymmetric structure of the dark matter halo. We plan to extend the observation to 60 arcmin radius, which corresponds to the 0.6 times the virial radius. By making the east- and south-offset observations each in 60 ks, we intend to conduct precise measurements of temperature and metal abundances over the half virial radius for the first time. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | ISHISAKI | YOSHITAKA | NULL | NULL | JAP | 2 | AO2 | TEMPERATURE AND ABUNDAANCE OF ELONGATED CLUSTER AWM7 AT 0.6 R_180 AND POSSIBLE CONNECTION WITH SUPERCLUSTER FILAMENT | XIS | Y |
| OPHIUCHUS CLUSTER | 258.1093 | -23.379 | 0.56233145 | 9.26925896 | 277.7852 | 54367.8835069444 | 54370.5939351852 | 802046010 | 100525 | 100000 | 100525 | 100525 | 0 | 100525 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 82949.5 | 82949.5 | 234161.9 | 3 | PROCESSED | 57540.1576041667 | 54770 | 54402.5613194444 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020143 | The verification of the resonance scattering effect to resonance lines in an intracluster medium (ICM) is a big problem that has been carried over from ASCA. Though two interpretations for abnormality of intensity ratio of Fe-Kalpha/Fe Kbeta line, "resonance scattering effect" and "Ni overabundance", have been proposed, a determinate result has not been obtained. Both interpretations give a very big impact to the understanding of chemical evolution of ICM that has been obtained so far. To solve the problem, we propose the measurement of Ni and Fe lines with high precision for Ophiuchus cluster which is bright and hot enough for measuring the K lines. Moreover, this cluster is suggested the existence of non-thermal radiation from observations with Beppo-SAX, INTEGRAL, Swift. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | FURUZAWA | AKIHIRO | NULL | NULL | JAP | 2 | AO2 | APPROCHING RESONANCE SCATTERING/NI-OVERABUNDANCE PROBLEM IN THE OPHIUCHUS CLUSTER | XIS | Y |
| COMA_45OFF | 194.2558 | 27.5714 | 52.91406039 | 88.6829823 | 127.9482 | 54436.4228703704 | 54437.2085185185 | 802047010 | 31615.1 | 30000 | 31615.1 | 31615.1 | 0 | 31615.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26169.1 | 26169.1 | 67824 | 0 | PROCESSED | 57540.7702083333 | 54814 | 54445.1600925926 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020149 | With XIS and HXD onboard Suzaku, we propose a scanning observation along the large-scale filament structure connecting the Coma cluster outskirts and the radio relic 1253+275. The scientific aims are: 1) to verify and delineate the spatial extent of the hard X-ray excess reported by BeppoSAX and RXTE, 2) to constrain the spatial distribution of large-scale magnetic fields, 3) to probe nonthermal processes associated with structure formation, such as ultra-high-energy particle acceleration at the cluster accretion shock, and 4) to provide complementary data in connection with observations in other wavebands, especially GeV-TeV gamma-rays. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | INOUE | SUSUMU | NULL | NULL | JAP | 2 | AO2 | EXPLORING PARTICLE ACCELERATION AND MAGNETIC FIELDS IN A LARGE-SCALE FILAMENT STRUCTURE ASSOCIATED WITH THE COMA CLUSTER | HXD | Y |
| COMA_60OFF | 194.0251 | 27.4252 | 49.19228369 | 88.92228234 | 126.7582 | 54438.1998726852 | 54439.1946990741 | 802048010 | 36666.9 | 30000 | 36666.9 | 36666.9 | 0 | 36666.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 31696.2 | 31696.2 | 85921.9 | 1 | PROCESSED | 57540.8231365741 | 54814 | 54445.3011689815 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 020149 | With XIS and HXD onboard Suzaku, we propose a scanning observation along the large-scale filament structure connecting the Coma cluster outskirts and the radio relic 1253+275. The scientific aims are: 1) to verify and delineate the spatial extent of the hard X-ray excess reported by BeppoSAX and RXTE, 2) to constrain the spatial distribution of large-scale magnetic fields, 3) to probe nonthermal processes associated with structure formation, such as ultra-high-energy particle acceleration at the cluster accretion shock, and 4) to provide complementary data in connection with observations in other wavebands, especially GeV-TeV gamma-rays. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | INOUE | SUSUMU | NULL | NULL | JAP | 2 | AO2 | EXPLORING PARTICLE ACCELERATION AND MAGNETIC FIELDS IN A LARGE-SCALE FILAMENT STRUCTURE ASSOCIATED WITH THE COMA CLUSTER | HXD | Y |
| NGC 1553 | 64.0253 | -55.7788 | 265.63371114 | -43.7014546 | 176.9406 | 54429.7042939815 | 54431.9029976852 | 802050010 | 98722.2 | 95000 | 98722.2 | 98722.2 | 0 | 98722.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 87790.3 | 87790.3 | 189915.9 | 2 | PROCESSED | 57540.6454976852 | 54806 | 54438.4258101852 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021401 | As driving engines of metal enrichment, early-type galaxies provide vital laboratories to investigate how it operates. In our Chandra survey of galaxies, we found solar ISM abundances (Zfe), similar to the stars and implying enrichment homology from clusters to moderate-Lx galaxies. The only outlier was NGC1553, for which we found a tantalizing hint of very subsolar Zfe, inconsistent with simple models. Unlike other galaxies with recent reports of low Zfe, NGC1553 has a bright gas halo, so the results are insensitive to the modelling of unresolved LMXB. We propose an 80ks observation of NGC1553 to measure definitively the ISM abundances of Fe and other crucial diagnostic elements. These data will either confirm enrichment bimodality or provide a vital low-Lx data-point to anchor models. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | HUMPHREY | PHILIP | NULL | NULL | USA | 2 | AO2 | NGC 1553: PROOF OF BIMODAL METAL ENRICHMENT? | XIS | Y |
| DRACO | 260.0265 | 57.929 | 86.38548758 | 34.73420948 | 52.1224 | 54196.7611458333 | 54198.2216898148 | 802051010 | 63323.2 | 67000 | 63323.2 | 63323.2 | 0 | 63323.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 64957.2 | 64957.2 | 126181.8 | 2 | PROCESSED | 57538.1232291667 | 54829 | 54203.3603703704 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021405 | We propose 50 ksec Suzaku observations of the Ursa Minor and Draco dwarf spheroidal galaxies. These dense, dark-matter-dominated systems are carefully selected as the strongest potential sources of line emission from radiatively decaying keV dark matter of any astrophysical object. The low-level, stable Suzaku background makes it the most sensitive instrument to-date for this purpose. At the very least, constraints that enter a significant new regime are derived: non-detections are still of great importance. In the best case, the long sought-after identity of dark matter will be discovered, pointing the way to physics beyond the Standard Model. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | LOEWENSTEIN | MICHAEL | NULL | NULL | USA | 2 | AO2 | SEARCH FOR WARM DARK MATTER WITH SUZAKU OBSERVATIONS OF DWARF SPHEROIDAL GALAXIES | XIS | Y |
| URSA MINOR | 227.2517 | 67.2307 | 104.9865755 | 44.80382561 | 40.7921 | 54195.7731944444 | 54196.7557175926 | 802052010 | 70882.3 | 67000 | 70890.3 | 70882.3 | 0 | 70890.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 59587.2 | 59587.2 | 84876 | 1 | PROCESSED | 57538.0737731482 | 54695 | 54203.3200462963 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021405 | We propose 50 ksec Suzaku observations of the Ursa Minor and Draco dwarf spheroidal galaxies. These dense, dark-matter-dominated systems are carefully selected as the strongest potential sources of line emission from radiatively decaying keV dark matter of any astrophysical object. The low-level, stable Suzaku background makes it the most sensitive instrument to-date for this purpose. At the very least, constraints that enter a significant new regime are derived: non-detections are still of great importance. In the best case, the long sought-after identity of dark matter will be discovered, pointing the way to physics beyond the Standard Model. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | LOEWENSTEIN | MICHAEL | NULL | NULL | USA | 2 | AO2 | SEARCH FOR WARM DARK MATTER WITH SUZAKU OBSERVATIONS OF DWARF SPHEROIDAL GALAXIES | XIS | Y |
| BOOTES GROUP 7 | 217.7796 | 35.0938 | 59.62119131 | 67.30227758 | 316.719 | 54266.3117592593 | 54267.3863310185 | 802053010 | 42124.4 | 38000 | 42132.4 | 42124.4 | 0 | 42132.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37338.4 | 37338.4 | 92823.8 | 0 | PROCESSED | 57538.9915509259 | 54695 | 54322.4630324074 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021424 | We propose four 30 ksec Suzaku pointings (120 ksec total) to obtain Lx and Tx for 4 distant (0.15 < z < 0.35) galaxy groups discovered in a contiguous, 9.3 sq. deg Chandra survey in Bootes. Our targets are spatially resolved by Chandra and are chosen to minimize point-source contamination of the Suzaku group spectra. The XIS data will significantly expand the sample of groups with known temperature in this redshift range, and so will improve constraints on group evolution mechanisms. We will use the existing, deep multicolor imaging and 20,000-object spectroscopic catalog for Bootes to study the effect of local environment on group properties, as well as the relationship between optically-selected and X-ray selected groups, for the first time in this redshift range. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | BAUTZ | MARSHALL | NULL | NULL | USA | 2 | AO2 | SUZAKU SPECTROSCOPY OF DISTANT GALAXY GROUPS IN BOOTES | XIS | Y |
| BOOTES GROUP 1 | 218.7136 | 35.7235 | 60.71261374 | 66.41229506 | 153.2269 | 54440.1222106482 | 54441.2015972222 | 802054010 | 42224.2 | 38000 | 42224.2 | 42224.2 | 0 | 42224.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41302.3 | 41302.3 | 93254 | 0 | PROCESSED | 57540.8293518518 | 54815 | 54448.2273842593 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021424 | We propose four 30 ksec Suzaku pointings (120 ksec total) to obtain Lx and Tx for 4 distant (0.15 < z < 0.35) galaxy groups discovered in a contiguous, 9.3 sq. deg Chandra survey in Bootes. Our targets are spatially resolved by Chandra and are chosen to minimize point-source contamination of the Suzaku group spectra. The XIS data will significantly expand the sample of groups with known temperature in this redshift range, and so will improve constraints on group evolution mechanisms. We will use the existing, deep multicolor imaging and 20,000-object spectroscopic catalog for Bootes to study the effect of local environment on group properties, as well as the relationship between optically-selected and X-ray selected groups, for the first time in this redshift range. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | BAUTZ | MARSHALL | NULL | NULL | USA | 2 | AO2 | SUZAKU SPECTROSCOPY OF DISTANT GALAXY GROUPS IN BOOTES | XIS | Y |
| BOOTES GROUP 26 | 219.0541 | 33.7727 | 55.78379271 | 66.53529007 | 323.2958 | 54265.160787037 | 54266.3092476852 | 802055010 | 43665.7 | 38000 | 43673.7 | 43681.7 | 0 | 43665.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38872.7 | 38872.7 | 99210.8 | 0 | PROCESSED | 57538.9553703704 | 54695 | 54271.4809837963 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021424 | We propose four 30 ksec Suzaku pointings (120 ksec total) to obtain Lx and Tx for 4 distant (0.15 < z < 0.35) galaxy groups discovered in a contiguous, 9.3 sq. deg Chandra survey in Bootes. Our targets are spatially resolved by Chandra and are chosen to minimize point-source contamination of the Suzaku group spectra. The XIS data will significantly expand the sample of groups with known temperature in this redshift range, and so will improve constraints on group evolution mechanisms. We will use the existing, deep multicolor imaging and 20,000-object spectroscopic catalog for Bootes to study the effect of local environment on group properties, as well as the relationship between optically-selected and X-ray selected groups, for the first time in this redshift range. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | BAUTZ | MARSHALL | NULL | NULL | USA | 2 | AO2 | SUZAKU SPECTROSCOPY OF DISTANT GALAXY GROUPS IN BOOTES | XIS | Y |
| BOOTES GROUP 30 | 219.4427 | 33.5107 | 55.01212205 | 66.25629851 | 308.903 | 54276.6949189815 | 54277.5271875 | 802056010 | 38504.5 | 38000 | 38504.5 | 38504.5 | 0 | 38504.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35747.3 | 35747.3 | 71897.9 | 1 | PROCESSED | 57539.0466782407 | 54702 | 54333.4389583333 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021424 | We propose four 30 ksec Suzaku pointings (120 ksec total) to obtain Lx and Tx for 4 distant (0.15 < z < 0.35) galaxy groups discovered in a contiguous, 9.3 sq. deg Chandra survey in Bootes. Our targets are spatially resolved by Chandra and are chosen to minimize point-source contamination of the Suzaku group spectra. The XIS data will significantly expand the sample of groups with known temperature in this redshift range, and so will improve constraints on group evolution mechanisms. We will use the existing, deep multicolor imaging and 20,000-object spectroscopic catalog for Bootes to study the effect of local environment on group properties, as well as the relationship between optically-selected and X-ray selected groups, for the first time in this redshift range. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | BAUTZ | MARSHALL | NULL | NULL | USA | 2 | AO2 | SUZAKU SPECTROSCOPY OF DISTANT GALAXY GROUPS IN BOOTES | XIS | Y |
| ABELL 2029 | 227.4644 | 6.0238 | 6.57368779 | 50.92713703 | 112.4532 | 54473.6848958333 | 54478.0211226852 | 802060010 | 169286.1 | 160000 | 169286.1 | 169286.1 | 0 | 169286.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 150766.1 | 150766.1 | 374620.1 | 4 | PROCESSED | 57541.3859953704 | 54860 | 54490.7163657407 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021433 | The properties of clusters of galaxies in very distant regions encompassing the virial radius (r_vir) are poorly understood yet these regions are sites of very important processes for the cluster formation and evolution. The recent generation of X-ray satellites (Chandra and XMM) thanks to their fine spatial resolution and high sensitivity have provided so far detailed spectral information mainly in the inner bright regions but they have not been very helpful in background dominated regimes typical of cluster outskirts' observations because of their high background. Suzaku has the capabilities to target those regions. We propose to observe the outskirts of the very relaxed cluster of galaxies A2029 with XIS to measure for the first time temperature and metallicity of the ICM up to r_vir. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ZAPPACOSTA | LUCA | NULL | NULL | USA | 2 | AO2 | EXPLORING THE OUTSKIRTS OF THE RELAXED CLUSTER ABELL 2029 | XIS | Y |
| PKS 0745-191 | 116.8852 | -19.2901 | 236.4397894 | 3.03527791 | 293.9994 | 54231.0124884259 | 54231.8216898148 | 802062010 | 32006.5 | 30000 | 32006.5 | 32030.5 | 0 | 32014.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27701.6 | 27701.6 | 69909.9 | 0 | PROCESSED | 57538.6154976852 | 54695 | 54238.8868518518 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021440 | PKS 0745-191 is the X-ray brightest galaxy cluster beyond a redshift of 0.1. It has a smooth surface brightness profile and appears relaxed. Using the low background of Suzaku we will measure the temperature of the intracluster medium to the virial radius of the cluster. Its high temperature means that we will be unaffected by any loss of effective area at low energies. In addition the cluster is bright enough so that the bremsstrahlung emission will be easily detected using the PIN detector. This will allow us to search for any nonthermal component as well as accurately determining the high temperature components in the cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOUNG | ANDREW | NULL | NULL | USA | 2 | AO2 | PKS 0745-191: THE BRIGHTEST CLUSTER BEYOND Z=0.1 | XIS | Y |
| PKS 0745-191 | 116.6543 | -19.2063 | 236.25768919 | 2.88874721 | 294.0002 | 54231.8221180556 | 54232.5001041667 | 802062020 | 31226.6 | 30000 | 31226.6 | 31226.6 | 0 | 31226.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25967 | 25967 | 58573.9 | 1 | PROCESSED | 57538.6330208333 | 54695 | 54238.8889814815 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021440 | PKS 0745-191 is the X-ray brightest galaxy cluster beyond a redshift of 0.1. It has a smooth surface brightness profile and appears relaxed. Using the low background of Suzaku we will measure the temperature of the intracluster medium to the virial radius of the cluster. Its high temperature means that we will be unaffected by any loss of effective area at low energies. In addition the cluster is bright enough so that the bremsstrahlung emission will be easily detected using the PIN detector. This will allow us to search for any nonthermal component as well as accurately determining the high temperature components in the cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOUNG | ANDREW | NULL | NULL | USA | 2 | AO2 | PKS 0745-191: THE BRIGHTEST CLUSTER BEYOND Z=0.1 | XIS | Y |
| PKS 0745-191 | 116.9737 | -19.0727 | 236.29361594 | 3.21678926 | 294.0001 | 54232.5006712963 | 54233.2258564815 | 802062030 | 30794.2 | 30000 | 30802.2 | 30794.2 | 0 | 30802.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26638.8 | 26638.8 | 62630.1 | 0 | PROCESSED | 57538.6331134259 | 54695 | 54245.5042592593 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021440 | PKS 0745-191 is the X-ray brightest galaxy cluster beyond a redshift of 0.1. It has a smooth surface brightness profile and appears relaxed. Using the low background of Suzaku we will measure the temperature of the intracluster medium to the virial radius of the cluster. Its high temperature means that we will be unaffected by any loss of effective area at low energies. In addition the cluster is bright enough so that the bremsstrahlung emission will be easily detected using the PIN detector. This will allow us to search for any nonthermal component as well as accurately determining the high temperature components in the cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOUNG | ANDREW | NULL | NULL | USA | 2 | AO2 | PKS 0745-191: THE BRIGHTEST CLUSTER BEYOND Z=0.1 | XIS | Y |
| PKS 0745-191 | 117.1155 | -19.3739 | 236.62179243 | 3.1809503 | 294.0002 | 54233.2263773148 | 54234.0369675926 | 802062040 | 32909.2 | 30000 | 32909.2 | 32909.2 | 0 | 32909.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 31008.5 | 31008.5 | 69999.9 | 0 | PROCESSED | 57538.6488541667 | 54695 | 54245.5354861111 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021440 | PKS 0745-191 is the X-ray brightest galaxy cluster beyond a redshift of 0.1. It has a smooth surface brightness profile and appears relaxed. Using the low background of Suzaku we will measure the temperature of the intracluster medium to the virial radius of the cluster. Its high temperature means that we will be unaffected by any loss of effective area at low energies. In addition the cluster is bright enough so that the bremsstrahlung emission will be easily detected using the PIN detector. This will allow us to search for any nonthermal component as well as accurately determining the high temperature components in the cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOUNG | ANDREW | NULL | NULL | USA | 2 | AO2 | PKS 0745-191: THE BRIGHTEST CLUSTER BEYOND Z=0.1 | XIS | Y |
| PKS 0745-191 | 116.7966 | -19.5079 | 236.58636127 | 2.85363493 | 294.0004 | 54234.0374884259 | 54234.8446643518 | 802062050 | 33414.6 | 30000 | 33414.6 | 33422.6 | 0 | 33422.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 31306.5 | 31306.5 | 69723.9 | 1 | PROCESSED | 57538.6567708333 | 54695 | 54245.5456712963 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021440 | PKS 0745-191 is the X-ray brightest galaxy cluster beyond a redshift of 0.1. It has a smooth surface brightness profile and appears relaxed. Using the low background of Suzaku we will measure the temperature of the intracluster medium to the virial radius of the cluster. Its high temperature means that we will be unaffected by any loss of effective area at low energies. In addition the cluster is bright enough so that the bremsstrahlung emission will be easily detected using the PIN detector. This will allow us to search for any nonthermal component as well as accurately determining the high temperature components in the cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YOUNG | ANDREW | NULL | NULL | USA | 2 | AO2 | PKS 0745-191: THE BRIGHTEST CLUSTER BEYOND Z=0.1 | XIS | Y |
| ABEL 754 | 137.2113 | -9.6361 | 239.25284371 | 24.7578079 | 295.1878 | 54249.7445833333 | 54252.4495949074 | 802063010 | 108977.9 | 100000 | 108985.9 | 108985.9 | 0 | 108977.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 97904 | 97904 | 233695.8 | 2 | PROCESSED | 57538.8549537037 | 54773 | 54257.5596759259 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021445 | We propose a 100 ksec observation of Abell 754 and a 50 ksec observation of Triangulum Australis, in order to measure the spectral shape and flux of possible nonthermal emission from clusters of galaxies. They are bright clusters of galaxies in the BAT all sky survey sample, which is crucial for making good spectral measurements by the HXD. And their spectra have a significant hard excess (power-law component). We intend to constrain the power-law photon index of the nonthermal emission for the first time and to determine the size of hard X-ray emitting region by using both of the HXD and Swift BAT data. We are aiming to test the origin of the hard flux and see whether it originates from either diffuse inverse Compton scattering by relativistic cosmic-ray electrons or an AGN. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | OKAJIMA | TAKASHI | NULL | NULL | USA | 2 | AO2 | OBSERVATIONS OF NONTHERMAL EMISSION FROM CLUSTERS OF GALAXIES | XIS | Y |
| RCS 1104-0445 | 166.1645 | -4.748 | 259.90521833 | 48.99506028 | 108.5039 | 54420.9087037037 | 54421.3210532407 | 802068010 | 19335 | 15000 | 19335 | 19335 | 0 | 19335 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15162.7 | 15162.7 | 35615.9 | 0 | PROCESSED | 57540.5367013889 | 54797 | 54430.2980787037 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021451 | We propose Suzaku observations of a sample of 10 galaxy clusters at redshifts between 0.6 and 0.95 from the RCS-1 cluster survey. These objects represent the optically richest clusters at these redshifts from the 100 square degree survey using the red-sequence method of cluster detection. As such, they form a critical sample for calibrating the mass-richness relationship for high redshift cluster surveys. Our proposed observations will allow us to determine their X-ray luminosities, as a first guide to estimating their masses, and enable future studies to determine accurate masses from their X-ray properties. These studies are complimentary to mass calibration programs we are carrying out using estimates based on lensing, IR stellar mass and galaxy dynamics. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | HICKS | AMALIA | NULL | NULL | USA | 2 | AO2 | A SUZAKU SNAPSHOT SURVEY OF HIGH-REDSHIFT GALAXY CLUSTERS FROM THE RCS SURVEY | XIS | Y |
| RCS 1122+2423 | 170.6071 | 24.3899 | 215.72830536 | 69.79971375 | 120.0624 | 54421.3268518518 | 54421.8891087963 | 802070010 | 20972.9 | 18000 | 20980.9 | 20980.9 | 0 | 20972.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19022 | 19022 | 48567.9 | 0 | PROCESSED | 57540.5406828704 | 54797 | 54430.3244097222 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 021451 | We propose Suzaku observations of a sample of 10 galaxy clusters at redshifts between 0.6 and 0.95 from the RCS-1 cluster survey. These objects represent the optically richest clusters at these redshifts from the 100 square degree survey using the red-sequence method of cluster detection. As such, they form a critical sample for calibrating the mass-richness relationship for high redshift cluster surveys. Our proposed observations will allow us to determine their X-ray luminosities, as a first guide to estimating their masses, and enable future studies to determine accurate masses from their X-ray properties. These studies are complimentary to mass calibration programs we are carrying out using estimates based on lensing, IR stellar mass and galaxy dynamics. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | HICKS | AMALIA | NULL | NULL | USA | 2 | AO2 | A SUZAKU SNAPSHOT SURVEY OF HIGH-REDSHIFT GALAXY CLUSTERS FROM THE RCS SURVEY | XIS | Y |
| ABELL2244 | 255.6885 | 34.0502 | 56.77689495 | 36.30222985 | 232.8204 | 54392.7992013889 | 54394.3959953704 | 802078010 | 71381.1 | 63000 | 71389.1 | 71397.1 | 0 | 71381.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 69107.7 | 69107.7 | 137949.8 | 3 | PROCESSED | 57540.332337963 | 54771 | 54403.2516666667 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 022036 | In order to use clusters as cosmological probes, accurate mass determinations are needed. The ICM is an ideal candidate since it provides a map of the DM potential. Measuring the gas properties to the virial radius is imperative for determining the proper cluster mass, since a large part of the cluster mass resides beyond 1/2 r_vir. Current discrepancies in outer cluster kT profiles are due to large uncertainties due to the high background in Chandra and XMM-Newton. With its lower background, Suzaku is able to make this measurement. We propose a 50 ks observation of A2244. A2244 is an ideal candidate to make this measurement; at a redshift of z~0.1, the virial radius can be fit inside Suzaku's field of view, moreover A2244 is an unusual example of a relaxed cluster without a cool core. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | HUDSON | DANIEL | NULL | NULL | EUR | 2 | AO2 | A2244 - MEASURING CLUSTER GAS TEMPERATURE TO THE VIRIAL RADIUS IN A RELAXED ISOTHERMAL CLUSTER | XIS | Y |
| ABELL 262 OFFSET1 | 28.5344 | 36.2686 | 136.82832457 | -24.90547123 | 69.9996 | 54318.8941898148 | 54320.0772337963 | 802079010 | 54589.4 | 48000 | 54597.4 | 54589.4 | 0 | 54602.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 50912.3 | 50912.3 | 102203.8 | 1 | PROCESSED | 57539.4485416667 | 54730 | 54347.4244791667 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 023004 | We propose to observe Abell 262. The temperature of the intracluster mediums of the cluster is 2 keV and therefore this cluster is between groups of galaxies and clusters of galaxies. The purpuse of the observation is to determine the distribution of O, Mg, Si and Fe f the intracluster medium upto 0.3 r180. The exposures are 30 ks for the central pointing and 40 ks for two offset pointings and the total exposure is 110ks. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MATSUSHITA | KYOKO | Gastaldello | Fabio | JUS | 2 | AO2 | O AND MG ABUNDANCES OF THE INTRACLUSTER MEDIUMS OF ABELL 262 | XIS | Y |
| ABELL 262 OFFSET2 | 28.0598 | 36.4356 | 136.37355079 | -24.84408055 | 69.9996 | 54320.0778935185 | 54321.2405555556 | 802080010 | 54708.1 | 48000 | 54724.1 | 54708.1 | 0 | 54724.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 50178.8 | 50178.8 | 100396.8 | 1 | PROCESSED | 57539.4536226852 | 54730 | 54347.6730671296 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 023004 | We propose to observe Abell 262. The temperature of the intracluster mediums of the cluster is 2 keV and therefore this cluster is between groups of galaxies and clusters of galaxies. The purpuse of the observation is to determine the distribution of O, Mg, Si and Fe f the intracluster medium upto 0.3 r180. The exposures are 30 ks for the central pointing and 40 ks for two offset pointings and the total exposure is 110ks. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MATSUSHITA | KYOKO | Gastaldello | Fabio | JUS | 2 | AO2 | O AND MG ABUNDANCES OF THE INTRACLUSTER MEDIUMS OF ABELL 262 | XIS | Y |
| COMA11 | 194.6305 | 28.3939 | 72.26601068 | 87.98563538 | 292.5148 | 54270.6441782407 | 54272.0078009259 | 802082010 | 53021.7 | 50000 | 53021.7 | 53021.7 | 0 | 53021.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46667.3 | 46667.3 | 117806 | 2 | PROCESSED | 57539.0191203704 | 54695 | 54322.5438888889 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 024438 | Several authors have claimed to detect soft X-ray excesses toward some clusters of galaxies, but most are contested by other studies. The only exception is the Coma cluster, where all investigators agree on the presence of the excess, which is especially bright toward one off-centered region, a potential cosmic filament draining into Coma. This excess has bright OVIII emission, so the gas must be thermal, and at the distance of Coma, the mass is of cosmological importance. However, it is possible that this soft excess is due to emission from the halo of the Milky Way, as Coma lies in a valley of particularly low Galactic column density. We propose to distinguish between the Milky Way and Coma origins by measuring the redshift of the OVIII emission line. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | BREGMAN | JOEL | Takei | Yoh | USJ | 2 | AO2 | THE SOFT X-RAY EXCESS TOWARD THE COMA CLUSTER | XIS | Y |
| COMABKG | 198.7472 | 31.648 | 75.72732699 | 83.16527783 | 295.0754 | 54272.0100347222 | 54272.7015046296 | 802083010 | 30783.1 | 30000 | 30783.1 | 30783.1 | 0 | 30783.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26505.8 | 26505.8 | 59739.9 | 0 | PROCESSED | 57539.0181597222 | 54702 | 54333.4315393518 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 024438 | Several authors have claimed to detect soft X-ray excesses toward some clusters of galaxies, but most are contested by other studies. The only exception is the Coma cluster, where all investigators agree on the presence of the excess, which is especially bright toward one off-centered region, a potential cosmic filament draining into Coma. This excess has bright OVIII emission, so the gas must be thermal, and at the distance of Coma, the mass is of cosmological importance. However, it is possible that this soft excess is due to emission from the halo of the Milky Way, as Coma lies in a valley of particularly low Galactic column density. We propose to distinguish between the Milky Way and Coma origins by measuring the redshift of the OVIII emission line. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | BREGMAN | JOEL | Takei | Yoh | USJ | 2 | AO2 | THE SOFT X-RAY EXCESS TOWARD THE COMA CLUSTER | XIS | Y |
| COMABKG2 | 194.3428 | 28.1403 | 70.87532192 | 88.34137752 | 297.3385 | 54272.7041550926 | 54273.4897453704 | 802084010 | 31973.1 | 30000 | 31973.1 | 33595.6 | 0 | 33595.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28853 | 28853 | 67850.1 | 1 | PROCESSED | 57539.0184143518 | 54695 | 54318.5135648148 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 024438 | Several authors have claimed to detect soft X-ray excesses toward some clusters of galaxies, but most are contested by other studies. The only exception is the Coma cluster, where all investigators agree on the presence of the excess, which is especially bright toward one off-centered region, a potential cosmic filament draining into Coma. This excess has bright OVIII emission, so the gas must be thermal, and at the distance of Coma, the mass is of cosmological importance. However, it is possible that this soft excess is due to emission from the halo of the Milky Way, as Coma lies in a valley of particularly low Galactic column density. We propose to distinguish between the Milky Way and Coma origins by measuring the redshift of the OVIII emission line. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | BREGMAN | JOEL | Takei | Yoh | USJ | 2 | AO2 | THE SOFT X-RAY EXCESS TOWARD THE COMA CLUSTER | XIS | Y |
| ZWCL 2341.1+0000 | 355.9117 | 0.3303 | 89.48591025 | -58.06988626 | 66.2761 | 54644.6873148148 | 54645.9258912037 | 803001010 | 50741.3 | 40000 | 50749.3 | 50741.3 | 0 | 50757.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39476.7 | 39476.7 | 107001.8 | 0 | PROCESSED | 57542.9355671296 | 55021 | 54655.1925578704 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030002 | Recent advances in observational cosmology have revealed that the large-scale distribution of galaxies in the universe has a honeycomb-like structure. However it is still a mystery how such diverse structures emerge out of primeval density fluctuations that grew over time due to the effects of gravity. An important role in the structure-formation process is played by the large-scale shocks that form as the primordial density fluctuations become non-linear and the accretion flows on collapsing structures become supersonic. In order to understand cosmic-rays acceleration greater than 1000 TeV and the structure formation in the early universe, we propose a 40 ksec observation of the proto-cluster filament ZwCl 2341.1+0000 (z = 0.27) with Suzaku. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KATAOKA | JUN | NULL | NULL | JAP | 3 | AO3 | COSMIC-RAY ACCELERATION AND STRUCTURE FORMATION IN A MPC-SCALE FILAMENTARY NETWORK OF GALAXIES | XIS | Y |
| IKT25 | 16.5704 | -72.153 | 301.32642461 | -44.92895011 | 33.6181 | 54601.2130208333 | 54603.3675810185 | 803002010 | 107322.3 | 100000 | 107330.3 | 107330.3 | 0 | 107322.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 124106.4 | 124106.4 | 186133.9 | 1 | PROCESSED | 57542.58375 | 54981 | 54613.1905439815 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030016 | In order for the white dwarf, the progenitor of SN Ia, to increase its mass to the Chandrasekhar limit, stellar wind driven by Fe contained in the accreting matter needs to be strong enough. For this reason, SN Ia is difficult to take place in the galaxy with low metallicity. We propose the observation on IKT 25, a type Ia SNR candidate in SMC, in order to decide its origin. Since the Fe abundance of SMC (0.2 solar) is lower than that of any other galaxys where SN Ia (or its remnant) had already been discovered, this observation will give the strongest restriction to the theory of the white dwarf evolution. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YAMAGUCHI | HIROYA | NULL | NULL | JAP | 3 | AO3 | IKT25: TYPE IA SNR CANDIDATE IN SMALL MAGELLANIC CLOUD | XIS | Y |
| NGC 253 OFFSET | 12.0926 | -25.0475 | 104.44696227 | -87.8082396 | 247.2843 | 54829.0152430556 | 54830.2502430556 | 803004010 | 56710.4 | 50000 | 56710.4 | 56710.4 | 0 | 56710.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51302.6 | 51302.6 | 106671.8 | 1 | PROCESSED | 57545.0814351852 | 55213 | 54847.4571296296 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030027 | Suzaku observations of a hot halo of nearby, edge-on starburst galaxy NGC 253 are proposed. The low background and high energy resolution of Suzaku XIS is the best tool to study the low surface brightness emission like halo emission around galaxies. In addition, we will eliminate the contamination from the the point source by XMM-Newton and the Galactic hot emission by an offset observation. The temperature and pressure structure and the chemical composition in the bright halo will reveal the physical condition and the dynamics of the galaxy outflow to the intergalactic space. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | YAMASAKI | NORIKO | NULL | NULL | JAP | 3 | AO3 | SUZAKU OBSERVATION OF A BRIGHTEST STARBURST GALAXY NGC 253 | XIS | Y |
| NGC 4382 | 186.3492 | 18.1851 | 267.72488674 | 79.23166289 | 294.1787 | 54638.1652199074 | 54640.4481944444 | 803005010 | 99068.2 | 90000 | 99068.2 | 99068.2 | 0 | 99068.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 93444.7 | 93444.7 | 197203.8 | 3 | PROCESSED | 57542.911412037 | 55020 | 54651.2282291667 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030033 | We proposeto observe a S0 galaxy, NGC 4382 for 90 ks with Suzaku. The purpose of the observation is to study abundance pattern of O/Ne/Mg/Si/Fe of S0 galaxies and to study history of S0 galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MATSUSHITA | KYOKO | NULL | NULL | JAP | 3 | AO3 | THE ISM ABUNDANCE OF A S0 GALAXY, NGC 4382 | XIS | Y |
| FORNAX OFFSET1 | 54.5865 | -35.7706 | 237.25707491 | -53.65522298 | 45.0001 | 54662.3087962963 | 54663.2106365741 | 803006010 | 35240.2 | 30000 | 35248.2 | 35240.2 | 0 | 35251.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30441 | 30441 | 77917.9 | 0 | PROCESSED | 57543.0490393518 | 55055 | 54686.1787384259 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030036 | We proposeto observe 5 offset pointings of the Fornax cluster for 160 ks with Suzaku. The purpose of the observation is to determine O, Mg and Fe distribution of the intracluster medium up to 0.15-0.2 r180 and to study the origin of the metals. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MATSUSHITA | KYOKO | NULL | NULL | JAP | 3 | AO3 | METAL DISTRIBUTION OF THE FORNAX CLUSTER UP TO 0.2R180. | XIS | Y |
| FORNAX OFFSET2 | 54.357 | -35.2813 | 236.43807346 | -53.85479755 | 63.6004 | 54663.2151388889 | 54664.1793287037 | 803007010 | 40647.7 | 30000 | 40678 | 40671.7 | 0 | 40647.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34835.8 | 34835.8 | 83297.9 | 0 | PROCESSED | 57595.6271875 | 55188 | 54822.5201736111 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030036 | We proposeto observe 5 offset pointings of the Fornax cluster for 160 ks with Suzaku. The purpose of the observation is to determine O, Mg and Fe distribution of the intracluster medium up to 0.15-0.2 r180 and to study the origin of the metals. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MATSUSHITA | KYOKO | NULL | NULL | JAP | 3 | AO3 | METAL DISTRIBUTION OF THE FORNAX CLUSTER UP TO 0.2R180. | XIS | Y |
| FORNAX OFFSET3 | 55.0322 | -35.1579 | 236.21473388 | -53.30533318 | 63.6008 | 54664.1800810185 | 54665.2009143518 | 803008010 | 41279.5 | 30000 | 41287.5 | 41279.5 | 0 | 41295.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35069.9 | 35069.9 | 88189.8 | 0 | PROCESSED | 57543.0818055556 | 55055 | 54689.4341087963 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030036 | We proposeto observe 5 offset pointings of the Fornax cluster for 160 ks with Suzaku. The purpose of the observation is to determine O, Mg and Fe distribution of the intracluster medium up to 0.15-0.2 r180 and to study the origin of the metals. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MATSUSHITA | KYOKO | NULL | NULL | JAP | 3 | AO3 | METAL DISTRIBUTION OF THE FORNAX CLUSTER UP TO 0.2R180. | XIS | Y |
| ZWCL_0823_FILAMENT-1 | 126.4596 | 4.2515 | 220.17063425 | 22.90045491 | 284.0603 | 54603.3781944444 | 54604.4551388889 | 803009010 | 41357.3 | 40000 | 41357.3 | 41361.9 | 0 | 41361.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35936.9 | 35936.9 | 93005.9 | 1 | PROCESSED | 57542.5603472222 | 54979 | 54613.0757060185 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030039 | We propose Suzaku X-ray follow-up observations of dark matter (DM) halo "sub-clumps" detected by the Subaru weak-lens survey. The sub-clumps we are interested in are the smaller DM halo associated with large scale structures. According to the CDM hierarchical structure formation scenario, they are the elemental component of the universe. Since the barion component associated to the clumps are supposed to be very faint, the X-ray follow-up requires the highest sensitivity for diffuse sources, i.e. the Suzaku XIS detectors. Our aim is to detect barion signals and reveal the history/nature of these sub-clumps. A total of four pointing, two aiming at A222/223 filament and another two at ZwCl0823--A664 filament are proposed. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NAKAZAWA | KAZUHIRO | NULL | NULL | JAP | 3 | AO3 | SUZAKU X-RAY FOLLOW-UP OF DARK MATTER SUB-CLUMPS DETECTED WITH SUBARU WEAK-LENS SURVEY | XIS | Y |
| NGC3556 | 167.883 | 55.6841 | 148.29932367 | 56.24590288 | 111.9355 | 54795.9750694444 | 54797.8890162037 | 803013010 | 84164.2 | 100000 | 84170.2 | 84165.9 | 0 | 84164.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 60353.7 | 60353.7 | 165287.9 | 2 | PROCESSED | 57544.6094212963 | 55175 | 54811.7645717593 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030058 | We propose to observe NGC 3556, a nearby edge-on spiral galaxy, with 100 ks exposure. Galactic coronal X-ray emission in and around several spiral galaxies have been spatially resolved using Chandra and XMM instruments. The target is one of these galaxies showing relatively luminous X-ray emission. Due to limited spectral capability of these instruments, X-ray spectral properties of these diffuse emission have not yet been investigated. We use good spectral capability of the SUZAKU/XIS to investigate the temperature structure and constrain the metal abundance pattern for the first time in galactic corona. We study origin, heating mechanism, and chemical properties of these galactic corona. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAMURA | TAKAYUKI | NULL | NULL | JAP | 3 | AO3 | GALACTIC CORONA IN AND AROUND THE EDGE-ON GALAXY NGC 3556 | XIS | Y |
| N1550_CENTER | 64.9488 | 2.4105 | 191.00239213 | -31.81480775 | 89.9981 | 54694.185474537 | 54696.3009143518 | 803017010 | 83270.2 | 80000 | 83710.2 | 83270.2 | 0 | 83710.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 64887.4 | 64887.4 | 182756 | 4 | PROCESSED | 57543.367974537 | 55080 | 54713.2652546296 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030070 | We propose 80 and 40 ksec observations of the central and 30' offset regions of fossil group, NGC 1550, respectively, to study metal abundance distributions of O to Fe to the ~0.2 times of virial radius. A good energy resolution, and a low and stable background level of the XIS instrument are crucial for this study. A comparison of O to Fe abundance profiles will tell us how metals produced by type Ia and II supernovae have been enriched in the intergalactic space. In addition, a comparison of the metal distributions of the nominal group of galaxies and fossil group will show us how much metal production and diffusion processes differ with system. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SATO | KOSUKE | NULL | NULL | JAP | 3 | AO3 | OBSERVATIONS OF METAL DISTRIBUTIONS IN FOSSIL GROUP: NGC1550 | XIS | Y |
| N1550_OFFSET | 65.2479 | 2.4086 | 191.20173857 | -31.56876902 | 90.0005 | 54693.1139351852 | 54694.185 | 803018010 | 41144.7 | 40000 | 41144.7 | 41144.7 | 0 | 41144.7 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 29946.9 | 29946.9 | 92508 | 0 | PROCESSED | 57543.3286226852 | 55079 | 54711.3163310185 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030070 | We propose 80 and 40 ksec observations of the central and 30' offset regions of fossil group, NGC 1550, respectively, to study metal abundance distributions of O to Fe to the ~0.2 times of virial radius. A good energy resolution, and a low and stable background level of the XIS instrument are crucial for this study. A comparison of O to Fe abundance profiles will tell us how metals produced by type Ia and II supernovae have been enriched in the intergalactic space. In addition, a comparison of the metal distributions of the nominal group of galaxies and fossil group will show us how much metal production and diffusion processes differ with system. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SATO | KOSUKE | NULL | NULL | JAP | 3 | AO3 | OBSERVATIONS OF METAL DISTRIBUTIONS IN FOSSIL GROUP: NGC1550 | XIS | Y |
| ABELL 3395 | 96.7698 | -54.5043 | 263.27498484 | -25.21804833 | 150.0003 | 54815.4865046296 | 54817.3168865741 | 803020010 | 104346.9 | 100000 | 104346.9 | 104346.9 | 0 | 104346.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 81661 | 81661 | 158129.9 | 3 | PROCESSED | 57545.0306828704 | 55210 | 54840.5412268518 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030078 | We propose to observe a merging cluster Abell 3395 with Suzaku for 100 ks. Abell 3395 has two X-ray emission peaks in the ICM, and they can have a large velocity difference of 3000 km/s at maximum. From the line shift of iron K line, we detect the bulk motion of the ICM, and compare it with the velocity distribution of galaxies. The difference of velocity distributions between the ICM and galaxies reflects the difference of their cross sections during the cluster merging. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KAWAHARADA | MADOKA | NULL | NULL | JAP | 3 | AO3 | COMPARISON BETWEEN VELOCITY DISTRIBUTIONS OF ICM AND GALAXIES IN A MERGING CLUSTER | XIS | Y |
| SHAPLEY OFFSET | 204.9135 | -29.8943 | 315.23466303 | 31.82297967 | 289.7009 | 54665.2119907407 | 54666.4244675926 | 803021010 | 47243.5 | 40000 | 47243.5 | 47243.5 | 0 | 47243.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38357.8 | 38357.8 | 104741.8 | 0 | PROCESSED | 57543.0903356482 | 55049 | 54682.1908680556 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030089 | We aim at the first significant detection of redshifted OVII and OVIII lines from the warm-hot intergalactic medium (WHIM) in the Shapley Supercluster. The system, located at z = 0.048, shows the richest concentration of X-ray clusters in the nearby universe. Previous ROSAT observation showed enhanced soft X-ray emission along the cluster connection. We propose to observe for 80 ksec a region between A3558 (the brightest central cluster) and A3556, separated by 0.9 virial radius from both clusters and along the line of cluster connection. A 40 ksec observation is also proposed at a 2-degree offest region to measure the foreground Galactic spectrum. Based on the ROSAT flux, we expect to detect redshifted OVII and OVII lines at more than 7 sigma confidence. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | OHASHI | TAKAYA | NULL | NULL | JAP | 3 | AO3 | SEARCH FOR WHIM IN THE SHAPLEY SUPERCLUSTER | XIS | Y |
| A2163_NE | 244.026 | -6.0591 | 6.90407558 | 30.45267126 | 113.8304 | 54870.8869560185 | 54872.1724421296 | 803022010 | 51797.4 | 40000 | 51805.4 | 51813.4 | 0 | 51797.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43861 | 43861 | 111051.8 | 1 | PROCESSED | 57545.4990162037 | 55330 | 54895.5963888889 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030094 | We propose 2 pointing observations of a hot cluster A2163 (z=0.2). A2163 is an X-ray brightest object among the violent merger candidates, which possess a huge radio halo and a complex temperature structure. Thus it is a unique target to discover extremely hot (>20keV) gas produced via merger shock. Thanks to the unprecedent high-quality broad-band spectra of Suzaku we can accurately determine the temperature of the hot gas. Which, at the same time, leads to the detection of the buried non-thermal hard X-ray emission. Combining this observation with the high-resolution images of our thermal SZ effect and the XMM observation, we can obtain a spatial distribution of the extremely hot thermal gas in the merging cluster for the first time. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | OTA | NAOMI | NULL | NULL | JAP | 3 | AO3 | BROAD-BAND SPECTROSCOPY OF THE HOTTEST ABELL GALAXY CLUSTER A2163 | XIS | Y |
| A1689-OFFSET1 | 198.0484 | -1.2633 | 313.73996571 | 61.17214089 | 289.9985 | 54670.1962962963 | 54671.3488773148 | 803024010 | 47070.3 | 40000 | 47070.3 | 47081.3 | 0 | 47078.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36328.3 | 36328.3 | 99543.9 | 1 | PROCESSED | 57543.121412037 | 55076 | 54707.0796180556 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030100 | We propose to conduct a joint X-ray, optical and weak-lensing analysis on the outsikrts (r_{500} < r < r_{vir}) of a massive cluster A1689, using Japanese X-ray and optical instruments of Suzaku/XIS and Subaru/Suprime-Cam. A joint analysis will provide us with a comprehensive picture of the interplay among the intracluster medimum (ICM), member galaxies and dark matter. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | OKABE | NOBUHIRO | NULL | NULL | JAP | 3 | AO3 | UNVEILING THE INTERPLAY AMONG ICM, GALAXIES AND DARK MATTER IN THE OUTSIKRST OF A1689 | XIS | Y |
| A1689-OFFSET2 | 197.956 | -1.5158 | 313.46570539 | 60.93832198 | 289.9994 | 54671.3493518518 | 54672.423125 | 803025010 | 43546.8 | 40000 | 43546.8 | 43546.8 | 0 | 43546.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36548.6 | 36548.6 | 92715.9 | 2 | PROCESSED | 57543.1297685185 | 55076 | 54707.2585763889 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030100 | We propose to conduct a joint X-ray, optical and weak-lensing analysis on the outsikrts (r_{500} < r < r_{vir}) of a massive cluster A1689, using Japanese X-ray and optical instruments of Suzaku/XIS and Subaru/Suprime-Cam. A joint analysis will provide us with a comprehensive picture of the interplay among the intracluster medimum (ICM), member galaxies and dark matter. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | OKABE | NOBUHIRO | NULL | NULL | JAP | 3 | AO3 | UNVEILING THE INTERPLAY AMONG ICM, GALAXIES AND DARK MATTER IN THE OUTSIKRST OF A1689 | XIS | Y |
| A1689-OFFSET3 | 197.7048 | -1.4241 | 312.98436439 | 61.06880263 | 289.9992 | 54672.423599537 | 54673.474525463 | 803026010 | 44094.2 | 40000 | 44094.2 | 44094.2 | 0 | 44094.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37706.3 | 37706.3 | 90787.8 | 1 | PROCESSED | 57543.149537037 | 55076 | 54707.1173263889 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030100 | We propose to conduct a joint X-ray, optical and weak-lensing analysis on the outsikrts (r_{500} < r < r_{vir}) of a massive cluster A1689, using Japanese X-ray and optical instruments of Suzaku/XIS and Subaru/Suprime-Cam. A joint analysis will provide us with a comprehensive picture of the interplay among the intracluster medimum (ICM), member galaxies and dark matter. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | OKABE | NOBUHIRO | NULL | NULL | JAP | 3 | AO3 | UNVEILING THE INTERPLAY AMONG ICM, GALAXIES AND DARK MATTER IN THE OUTSIKRST OF A1689 | XIS | Y |
| A1689-OFFSET4 | 197.7965 | -1.1735 | 313.25406527 | 61.301843 | 290 | 54673.475 | 54674.5091898148 | 803027010 | 42019.9 | 40000 | 42027.9 | 42027.9 | 0 | 42019.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36850.5 | 36850.5 | 89354 | 2 | PROCESSED | 57543.1496527778 | 55076 | 54707.0673032407 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030100 | We propose to conduct a joint X-ray, optical and weak-lensing analysis on the outsikrts (r_{500} < r < r_{vir}) of a massive cluster A1689, using Japanese X-ray and optical instruments of Suzaku/XIS and Subaru/Suprime-Cam. A joint analysis will provide us with a comprehensive picture of the interplay among the intracluster medimum (ICM), member galaxies and dark matter. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | OKABE | NOBUHIRO | NULL | NULL | JAP | 3 | AO3 | UNVEILING THE INTERPLAY AMONG ICM, GALAXIES AND DARK MATTER IN THE OUTSIKRST OF A1689 | XIS | Y |
| TRIANGULUM_AUSTRALIS | 249.6225 | -64.3477 | 324.61952374 | -11.529112 | 306.6841 | 54750.3809143518 | 54752.6453587963 | 803028010 | 86010.1 | 80000 | 86042.1 | 86010.1 | 0 | 86048.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 76967.5 | 76967.5 | 195637.8 | 1 | PROCESSED | 57544.1744560185 | 55148 | 54780.7199768518 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030101 | We propose an 80 ks pointed observation of one of the brightest near-by hot and merging galaxy cluster, Triangulum Australis. Recent Suzaku wide-band spectroscopy reveals a very hot (kT >20 keV) thermal component in several merging clusters (RXJ1347, Abell 3667 and so on). On the other hand, relaxed cluster (such as Abell 1060 and Centaurus) show no evidence of such component. These results suggests that the very-hot component is the key aspects of merging cluster. Triangulum Australis is a bright (f ~ 1e-10 cgs), mildly hot (kT ~ 9 keV) and relatively compact (size ~20x20 arcmin2) shaped cluster. ASCA detected a hot region in the center and to the east (Markevitch et al. 1996). Combination of these characteristics makes this cluster the best candidate for our research. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | OKUYAMA | SHO | NULL | NULL | JAP | 3 | AO3 | SEARCH FOR VERY-HIGH TEMPERATURE COMPONENT IN A NEAR-BY CLUSTER, TRIANGULUM AUSTRALIS | XIS | Y |
| A3627CENTER | 243.5672 | -60.8499 | 325.25917104 | -7.10560665 | 129.9148 | 54905.9231597222 | 54906.6072222222 | 803032010 | 46033.9 | 50000 | 46038.8 | 46041.9 | 0 | 46033.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 43396.9 | 43396.9 | 59095.9 | 0 | PROCESSED | 57545.823900463 | 55330 | 54917.2613657407 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030117 | We propsoe to observe the cluster of galaxies A3627, which has evidences of cluster merging, in order to detect hard X-rays from high energy particles acceralated in the cluster and also measure the doppler shift of the iron-K line. This cluster is a nearby bright cluster behind the Galactic plane, and thus so far X-ray studies have been poor. However, its proximity and relatively low temperature against other merging clusters enable us to constrain the hard X-ray emission more tightly. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NISHINO | SHO | NULL | NULL | JAP | 3 | AO3 | OBSERVATION OF MERGING CLUSTER A3627, LOCATED AROUND THE CENTER OF THE GREAT ATTRACTOR | XIS | Y |
| A3627SE | 243.9338 | -61.0124 | 325.27404641 | -7.34625911 | 86.273 | 54869.3739236111 | 54870.87875 | 803033010 | 52699.5 | 50000 | 52739.5 | 52699.5 | 0 | 52723.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48183.9 | 48183.9 | 129987.8 | 3 | PROCESSED | 57545.4958912037 | 55330 | 54881.3769212963 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 030117 | We propsoe to observe the cluster of galaxies A3627, which has evidences of cluster merging, in order to detect hard X-rays from high energy particles acceralated in the cluster and also measure the doppler shift of the iron-K line. This cluster is a nearby bright cluster behind the Galactic plane, and thus so far X-ray studies have been poor. However, its proximity and relatively low temperature against other merging clusters enable us to constrain the hard X-ray emission more tightly. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NISHINO | SHO | NULL | NULL | JAP | 3 | AO3 | OBSERVATION OF MERGING CLUSTER A3627, LOCATED AROUND THE CENTER OF THE GREAT ATTRACTOR | XIS | Y |
| N44 SB | 80.6234 | -67.9392 | 278.35092966 | -33.30497245 | 311.8533 | 54565.7359143518 | 54566.5084953704 | 803036010 | 30556.8 | 30000 | 30556.8 | 30556.8 | 0 | 30556.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26911.8 | 26911.8 | 66748 | 1 | PROCESSED | 57542.2791898148 | 54946 | 54580.4450810185 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031238 | Clusters of massive stars, through their stellar winds and supernovae, form large diffuse structures known as superbubbles (SBs), which play an essential role in shaping the local interstellar medium. Most SB models indicate that these objects should be dominated by thermal plasma processes. However, observations of 3 SBs have detected significant nonthermal contributions to their X-ray emission, which raises many questions. Is it generated by synchrotron, inverse-Compton, or nonthermal Bremsstrahlung processes? Are colliding stellar winds or internal supernova remnants responsible? We therefore propose to examine the X-ray emission from 3 X-ray bright SBs, to search for nonthermal X-ray emission, and if possible place strong constraints on the source of this emission. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MADDOX | LARRY | NULL | NULL | USA | 3 | AO3 | A SEARCH FOR NONTHERMAL X-RAY EMISSION FROM SUPERBUBBLES | XIS | Y |
| N154 SB | 84.0182 | -69.641 | 280.12884425 | -31.83619967 | 313.3253 | 54583.7906944444 | 54584.7849305556 | 803037010 | 50404 | 40000 | 50404 | 50404 | 0 | 50404 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 56617.1 | 56617.1 | 85887.8 | 1 | PROCESSED | 57542.411724537 | 54964 | 54598.4914699074 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031238 | Clusters of massive stars, through their stellar winds and supernovae, form large diffuse structures known as superbubbles (SBs), which play an essential role in shaping the local interstellar medium. Most SB models indicate that these objects should be dominated by thermal plasma processes. However, observations of 3 SBs have detected significant nonthermal contributions to their X-ray emission, which raises many questions. Is it generated by synchrotron, inverse-Compton, or nonthermal Bremsstrahlung processes? Are colliding stellar winds or internal supernova remnants responsible? We therefore propose to examine the X-ray emission from 3 X-ray bright SBs, to search for nonthermal X-ray emission, and if possible place strong constraints on the source of this emission. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MADDOX | LARRY | NULL | NULL | USA | 3 | AO3 | A SEARCH FOR NONTHERMAL X-RAY EMISSION FROM SUPERBUBBLES | XIS | Y |
| N206 SB | 82.6396 | -71.0391 | 281.83986558 | -32.08582418 | 315.5807 | 54584.7862384259 | 54585.7640509259 | 803038010 | 48834.5 | 40000 | 48834.5 | 48834.5 | 0 | 48834.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 54729.7 | 54729.7 | 84467.8 | 1 | PROCESSED | 57542.434837963 | 54964 | 54598.4969444445 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031238 | Clusters of massive stars, through their stellar winds and supernovae, form large diffuse structures known as superbubbles (SBs), which play an essential role in shaping the local interstellar medium. Most SB models indicate that these objects should be dominated by thermal plasma processes. However, observations of 3 SBs have detected significant nonthermal contributions to their X-ray emission, which raises many questions. Is it generated by synchrotron, inverse-Compton, or nonthermal Bremsstrahlung processes? Are colliding stellar winds or internal supernova remnants responsible? We therefore propose to examine the X-ray emission from 3 X-ray bright SBs, to search for nonthermal X-ray emission, and if possible place strong constraints on the source of this emission. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MADDOX | LARRY | NULL | NULL | USA | 3 | AO3 | A SEARCH FOR NONTHERMAL X-RAY EMISSION FROM SUPERBUBBLES | XIS | Y |
| NGC 3079 | 150.444 | 55.6163 | 157.91350273 | 48.36319014 | 294.1052 | 54590.7432407407 | 54591.1147800926 | 803039010 | 14408.3 | 100000 | 14408.3 | 14408.3 | 0 | 14408.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12953.8 | 12953.8 | 32079.9 | 0 | PROCESSED | 57542.4484027778 | 54999 | 54602.2023958333 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031303 | We will determine whether AGN can drive galactic-scale winds by observing NGC 3079, the best nearby candidate for such a wind. The edge-on spiral NGC 3079 hosts a Compton-thick AGN and is surrounded by a 40 kpc-scale soft X-ray nebula, the largest manifestation of outflow activity also seen in the optical and radio. Proving the outflow is AGN-driven requires Suzaku's unique abilities. We will measure the AGN luminosity using the HXD in the 15-40 keV range and the 2-10 keV band reflection spectrum to assess whether the AGN can radiatively-or-mechanically power the observed superwind. We will determine the origin of the soft X-ray nebula using the relative elemental abundances in the plasma. We can also detect any significant starburst through the 6.7 keV line emission it would create. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | STRICKLAND | DAVID | NULL | NULL | USA | 3 | AO3 | NGC 3079'S 40 KPC-SCALE OUTFLOW: AGN OR STARBURST-DRIVEN? | HXD | Y |
| NGC 3079 | 150.4972 | 55.6116 | 157.90048948 | 48.39234685 | 268.6689 | 54612.8709722222 | 54615.4362731482 | 803039020 | 102340 | 100000 | 102348 | 102340 | 0 | 102348 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 102003.1 | 102003.1 | 221601.9 | 2 | PROCESSED | 57542.6909027778 | 54999 | 54633.7055439815 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031303 | We will determine whether AGN can drive galactic-scale winds by observing NGC 3079, the best nearby candidate for such a wind. The edge-on spiral NGC 3079 hosts a Compton-thick AGN and is surrounded by a 40 kpc-scale soft X-ray nebula, the largest manifestation of outflow activity also seen in the optical and radio. Proving the outflow is AGN-driven requires Suzaku's unique abilities. We will measure the AGN luminosity using the HXD in the 15-40 keV range and the 2-10 keV band reflection spectrum to assess whether the AGN can radiatively-or-mechanically power the observed superwind. We will determine the origin of the soft X-ray nebula using the relative elemental abundances in the plasma. We can also detect any significant starburst through the 6.7 keV line emission it would create. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | STRICKLAND | DAVID | NULL | NULL | USA | 3 | AO3 | NGC 3079'S 40 KPC-SCALE OUTFLOW: AGN OR STARBURST-DRIVEN? | HXD | Y |
| NGC1961BACKGROUND | 85.5048 | 67.8763 | 145.2497599 | 18.81010884 | 72.0206 | 54748.602962963 | 54749.1197222222 | 803041010 | 24143.5 | 20000 | 24143.5 | 24143.5 | 0 | 24143.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20099 | 20099 | 44639.9 | 1 | PROCESSED | 57544.0915393518 | 55148 | 54780.6911342593 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031401 | Galaxies are missing most of their baryons when compared to the cosmological baryon to dark matter ratio. The Milky Way is missing at least 70% of its baryons while lower mass galaxies retain less than 10% of their baryons. Theory suggests that these baryons were expelled by intense galactic winds during the primary star formation period. These galactic winds carry gas far beyond the virial radius of small and modest galaxies, but the most massive galaxies should retain much of this gas. We propose to test this picture by searching for the missing baryons surrounding the very massive spiral galaxy, NGC 1961, which has 10 times the stellar content of M31 and with v_rot = 450 km/sec. If successful, we will detect a significant fraction of the 5E11 Msun of its missing baryons. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | BREGMAN | JOEL | NULL | NULL | USA | 3 | AO3 | THE BARYONS CONTENT OF THE MOST MASSIVE SPIRAL GALAXY | XIS | Y |
| NGC 5846 | 226.6234 | 1.6025 | 0.42380195 | 48.79350498 | 287.2336 | 54675.6192939815 | 54679.0008564815 | 803042010 | 155933.1 | 150000 | 155933.1 | 155933.1 | 0 | 155933.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 145470.4 | 145470.4 | 292151.9 | 2 | PROCESSED | 57543.2487152778 | 55059 | 54693.5527546296 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031404 | We propose Suzaku observations of three elliptical galaxies, selected on brightness and the availability of XMM-Newton RGS data, as part of a program to investigate their star formation history and chemical evolution via abundance studies of the hot interstellar medium. The low-energy sensitivity, spectral resolution, and low background of the Suzaku XIS enables the first accurate model-independent measurements of the abundance pattern while expanding the number of measurable temperature diagnostic features. Analysis of XIS spectra (critically, with SCI on), exclusively and in combination with RGS data, demonstrates the unique power of Suzaku to contribute to our understanding of the thermal and chemical properties of these systems. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | LOEWENSTEIN | MICHAEL | NULL | NULL | USA | 3 | AO3 | UNCOVERING THE TRUE ABUNDANCES OF ELLIPTICAL GALAXIES WITH SUZAKU | XIS | Y |
| NGC 4406 | 186.5483 | 12.9401 | 279.08850556 | 74.63107328 | 294.6659 | 55001.7603125 | 55004.4793287037 | 803043010 | 101773.6 | 90000 | 101773.6 | 101773.6 | 0 | 101773.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 86554.5 | 86554.5 | 234898.1 | 2 | PROCESSED | 57547.6610300926 | 55384 | 55015.2472569445 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031404 | We propose Suzaku observations of three elliptical galaxies, selected on brightness and the availability of XMM-Newton RGS data, as part of a program to investigate their star formation history and chemical evolution via abundance studies of the hot interstellar medium. The low-energy sensitivity, spectral resolution, and low background of the Suzaku XIS enables the first accurate model-independent measurements of the abundance pattern while expanding the number of measurable temperature diagnostic features. Analysis of XIS spectra (critically, with SCI on), exclusively and in combination with RGS data, demonstrates the unique power of Suzaku to contribute to our understanding of the thermal and chemical properties of these systems. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | LOEWENSTEIN | MICHAEL | NULL | NULL | USA | 3 | AO3 | UNCOVERING THE TRUE ABUNDANCES OF ELLIPTICAL GALAXIES WITH SUZAKU | XIS | Y |
| BOOTES_GROUP_37 | 216.3696 | 32.9366 | 54.59315934 | 68.88543442 | 308.8196 | 54640.4539467593 | 54641.6898611111 | 803044010 | 52903.4 | 40000 | 52911.4 | 52911.4 | 0 | 52903.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47652.7 | 47652.7 | 106765.8 | 2 | PROCESSED | 57542.9257638889 | 55020 | 54651.1591319444 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031411 | Galaxy groups are vital to our understanding of structure formation, cluster evolution, and galaxy evolution, yet they are difficult to study at even moderate redshift. We have undertaken a project to observe a flux-limited sample of intermediate-redshift groups identified by the XBootes Chandra survey, and here we propose Suzaku/XIS observations of two targets to continue this program. With the unique multiwavelength coverage of the XBootes field, we aim to understand the physical connection between the X-ray and optical properties of groups, and to probe the evolution of group X-ray emission in order to constrain the non-gravitational physics affecting the energetics of the intragroup medium. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MILLER | ERIC | NULL | NULL | USA | 3 | AO3 | UNDERSTANDING GROUP EVOLUTION WITH SUZAKU | XIS | Y |
| BOOTES_GROUP_32 | 217.4805 | 33.2976 | 55.13369931 | 67.90745799 | 91.5977 | 54868.4415740741 | 54869.3619675926 | 803045010 | 40728.7 | 40000 | 40744.7 | 40728.7 | 0 | 40744.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34656.3 | 34656.3 | 79487.8 | 2 | PROCESSED | 57545.4809490741 | 55328 | 54880.5918518518 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031411 | Galaxy groups are vital to our understanding of structure formation, cluster evolution, and galaxy evolution, yet they are difficult to study at even moderate redshift. We have undertaken a project to observe a flux-limited sample of intermediate-redshift groups identified by the XBootes Chandra survey, and here we propose Suzaku/XIS observations of two targets to continue this program. With the unique multiwavelength coverage of the XBootes field, we aim to understand the physical connection between the X-ray and optical properties of groups, and to probe the evolution of group X-ray emission in order to constrain the non-gravitational physics affecting the energetics of the intragroup medium. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MILLER | ERIC | NULL | NULL | USA | 3 | AO3 | UNDERSTANDING GROUP EVOLUTION WITH SUZAKU | XIS | Y |
| NGC 1550-OFFSET1 | 65.1493 | 2.6086 | 190.9426677 | -31.53770965 | 265.5852 | 54901.8171875 | 54903.699525463 | 803046010 | 66827.4 | 62000 | 66827.4 | 66827.4 | 0 | 66827.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 60930.7 | 60930.7 | 162600.1 | 2 | PROCESSED | 57545.8588541667 | 55329 | 54917.3952314815 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031422 | We propose a set of two 19 arcmin offset observations of the galaxy groups NGC 1550 and MKW 4 to measure spatially resolved densities, temperatures and iron abundances out to r_500. These measurements are crucial for an accurate determination of the gas mass profile and gas fraction, for probing the entropy profile near the region where the accretion shocks start to be important, and for exploring the chemical enrichment at a spatial scale which retains information of early SNII and SNIa enrichment. Due to their brightness, regularity and low temperature, the two objects are ideal candidates for an offset observation of their peripheral gas by Suzaku, making an excellent use of its low background and soft X-ray sensitivity. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | GASTALDELLO | FABIO | NULL | NULL | USA | 3 | AO3 | THE OUTSKIRTS OF NGC 1550 AND MKW 4 | XIS | Y |
| A496 P-OUT | 68.2513 | -13.0087 | 209.22191803 | -36.52315476 | 62.0525 | 54674.5225347222 | 54675.6050231482 | 803048010 | 37551.6 | 35000 | 37551.6 | 37559.6 | 0 | 37559.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 33159.9 | 33159.9 | 93493.9 | 1 | PROCESSED | 57543.1577314815 | 55055 | 54689.4360416667 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031424 | A496 is a "normal" nearby cluster that has been the testbed for metal enrichment models in clusters and, more recently, of different mechanisms to generate cold fronts. Suzaku's excellent spectral resolution, low background and high effective area, combined with the moderate temperatures of this cluster allows us to probe, with two short exposures, into the large scale metal enrichment processes through determination of elemental abundance ratios out to half the virial radius for the first time. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | DUPKE | RENATO | NULL | NULL | USA | 3 | AO3 | LARGE SCALE METAL ENRICHMENT MECHANISMS IN ABELL 496 | XIS | Y |
| CYGNUS A CLUSTER | 299.7609 | 40.7885 | 76.19456446 | 5.8531495 | 241.849 | 54785.9049537037 | 54786.9154976852 | 803050010 | 44658.7 | 45000 | 44658.7 | 44658.7 | 0 | 44658.7 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 42966 | 42966 | 87280 | 0 | PROCESSED | 57544.3868055556 | 55167 | 54796.9718981482 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031426 | The radio galaxy Cygnus A lies in a cooling core cluster which is currently undergoing a cluster merger with a particularly simple geometry. We propose XIS spectra of the radio source/cooling core interaction region, merger shock region, and second subcluster. The Fe K emission line will be used to measure gas velocities in these 3 regions to determine the dynamics of the merger, and to constrain hydro/N-body simulations of the merger. Collisionless merger shocks may produce detectable non-equilibrium effects. We will also determine an upper limit for the rate of expansion of the X-ray bubble around the radio source, studying the interaction of the radio galaxy and X-ray gas in the only FR-II radio galaxy in a nearby cluster. HXD data will constrain inverse Compton from the radio source. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | WIK | DANIEL | NULL | NULL | USA | 3 | AO3 | PROPERTIES OF THE MERGER AND RADIO SOURCE INTERACTION IN THE CYGNUS A CLUSTER | XIS | Y |
| COMA RADIO RELIC | 193.8629 | 27.2883 | 43.32885714 | 89.09337318 | 130.9989 | 54823.8794328704 | 54829.0002777778 | 803051010 | 205062 | 140000 | 205070 | 205070 | 0 | 205062 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 170622.2 | 170622.2 | 442391.7 | 3 | PROCESSED | 57545.2371412037 | 55218 | 54851.5095949074 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031431 | We will observe the Coma cluster radio relic with the HXD/PIN to detect nonthermal Inverse Compton emission. This is the second brightest cluster radio relic known. The small PIN FOV will separate the Coma radio relic and halo. The PIN data will be a strong test of merger shock acceleration processes; a nondetection would be inconsistent with current theories. The data will allow the relic magnetic field, and nonthermal energy and pressure to be derived. The XIS observation of the relic will be used to detect the merger shock. The relic is associated with the merging NGC 4839 subgroup, which will also be observed. The 2 XIS observations will determine the dynamics of the merging subgroup. We will search for redshift differences between the Coma cluster, subgroup, and merger shock. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | SARAZIN | CRAIG | NULL | NULL | USA | 3 | AO3 | HARD X-RAY INVERSE COMPTON EMISSION FROM THE RADIO RELIC AND THE DYNAMICS OF THE MERGING SUBGROUP IN THE COMA CLUSTER | HXD | Y |
| ABELL S753 RELIC | 211.0241 | -34.0331 | 319.70505054 | 26.46102153 | 102.5257 | 54838.0480555556 | 54841.6668287037 | 803053010 | 137527.5 | 120000 | 137535.5 | 137527.5 | 0 | 137535.5 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 99599.2 | 99599.2 | 312605.6 | 3 | PROCESSED | 57545.2410069444 | 55328 | 54851.4730787037 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031432 | The cluster radio relic PKS B1400-33 in the poor cluster Abell S753 will be observed with the HXD/PIN to detect and characterize the nonthermal Inverse Compton emission. This is one of the brightest cluster radio relics known. Remarkably, it is associated with a relatively poor, cool cluster. Although it has many properties similar to other cluster radio relics, it is possible that it is an old radio lobe, displaced by motions or buoyancy. The HXD/PIN data will be a strong test of merger shock acceleration processes. The XIS observations will constrain the low energy nonthermal spectrum and determine the thermal gas properties near the relic, and allow a merger shock to be detected. The long exposure with the XIS will also provide accurate abundances for the gas in this cool cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | SARAZIN | CRAIG | NULL | NULL | USA | 3 | AO3 | PKS B1400-33 AND ABELL S753: A VERY BRIGHT RADIO RELIC IN A POOR CLUSTER | XIS | Y |
| A3112 | 49.4785 | -44.2477 | 252.95565297 | -56.08416767 | 11.0983 | 54609.240162037 | 54611.0557638889 | 803054010 | 67498.2 | 60000 | 67498.2 | 67498.2 | 0 | 67498.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 59065.8 | 59065.8 | 156857.8 | 0 | PROCESSED | 57542.6456365741 | 54988 | 54620.3684490741 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031434 | We propose to perform spatially resolved spectroscopy on the X-ray bright relaxed galaxy cluster Abell 3112, in order to characterize its soft/hard X-ray excess component. Abell 3112 is one of two clusters with very strong soft excess emission (the other being Abell S1101, observed in AO1). The indications provided by this observation will be crucial in order to assess, beyond doubt, the reality of the soft excess emission, previously observed by all soft X-ray missions since EUVE. The proposed observation will constrain the nature of the excess emitter, and address outstanding questions in observational cosmology: the {it missing baryon} problem, the density of matter in the universe and the non-thermal energy in galaxy clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | BONAMENTE | MASSIMILIANO | NULL | NULL | USA | 3 | AO3 | SOFT EXCESS, HARD EXCESS AND THERMAL EMISSION IN ABELL 3112 | XIS | Y |
| RCS2347-3535 | 356.9535 | -35.5892 | 357.03141214 | -74.03003146 | 61.6856 | 54617.4612384259 | 54617.8890509259 | 803057010 | 15481.2 | 11000 | 15489.2 | 15489.2 | 0 | 15481.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14637.6 | 14637.6 | 36959.9 | 0 | PROCESSED | 57542.6853703704 | 54999 | 54633.6966087963 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031441 | Comparisons between moderate-z X-ray and high-z optically selected clusters indicate that the latter have lower Lx than expected for a given Tx, however it is hard to tell if such discrepancies are due to cluster evolution or selection effects. In an attempt to isolate these two variables, we propose the first detailed comparison of X-ray and optically selected clusters that are well-matched in both velocity dispersion (a quantity independent of both methods) and redshift. Our X-ray analysis of X-ray selected CNOC clusters is complete. Here we propose to determine Lx, Tx, and gas distribution/morphology for an optically selected sample, most of which already have velocity dispersion data in hand, enabling rigorous quantitative comparisons between physical characteristics of the two groups. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | HICKS | AMALIA | NULL | NULL | USA | 3 | AO3 | COSMOLOGY WITH CLUSTERS: CONSTRAINING PHYSICAL DIFFERENCES BETWEEN X-RAY AND OPTICALLY SELECTED SAMPLES AT MODERATE-Z | XIS | Y |
| RCS0442-2815 | 70.5602 | -28.2499 | 228.44078987 | -39.40072076 | 273.8381 | 54903.705462963 | 54905.2669444444 | 803060010 | 52357.3 | 40000 | 52357.3 | 52357.3 | 0 | 52357.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47413.7 | 47413.7 | 134877.9 | 1 | PROCESSED | 57545.8322222222 | 55329 | 54917.4174652778 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031441 | Comparisons between moderate-z X-ray and high-z optically selected clusters indicate that the latter have lower Lx than expected for a given Tx, however it is hard to tell if such discrepancies are due to cluster evolution or selection effects. In an attempt to isolate these two variables, we propose the first detailed comparison of X-ray and optically selected clusters that are well-matched in both velocity dispersion (a quantity independent of both methods) and redshift. Our X-ray analysis of X-ray selected CNOC clusters is complete. Here we propose to determine Lx, Tx, and gas distribution/morphology for an optically selected sample, most of which already have velocity dispersion data in hand, enabling rigorous quantitative comparisons between physical characteristics of the two groups. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | HICKS | AMALIA | NULL | NULL | USA | 3 | AO3 | COSMOLOGY WITH CLUSTERS: CONSTRAINING PHYSICAL DIFFERENCES BETWEEN X-RAY AND OPTICALLY SELECTED SAMPLES AT MODERATE-Z | XIS | Y |
| RCS1102-0340 | 165.6613 | -3.6697 | 258.27932815 | 49.53254853 | 114.238 | 54817.9779282407 | 54818.8987731482 | 803064010 | 37789 | 28000 | 37797 | 37797 | 0 | 37789 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27621 | 27621 | 79550 | 1 | PROCESSED | 57545.0002893518 | 55206 | 54840.5080439815 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031441 | Comparisons between moderate-z X-ray and high-z optically selected clusters indicate that the latter have lower Lx than expected for a given Tx, however it is hard to tell if such discrepancies are due to cluster evolution or selection effects. In an attempt to isolate these two variables, we propose the first detailed comparison of X-ray and optically selected clusters that are well-matched in both velocity dispersion (a quantity independent of both methods) and redshift. Our X-ray analysis of X-ray selected CNOC clusters is complete. Here we propose to determine Lx, Tx, and gas distribution/morphology for an optically selected sample, most of which already have velocity dispersion data in hand, enabling rigorous quantitative comparisons between physical characteristics of the two groups. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | HICKS | AMALIA | NULL | NULL | USA | 3 | AO3 | COSMOLOGY WITH CLUSTERS: CONSTRAINING PHYSICAL DIFFERENCES BETWEEN X-RAY AND OPTICALLY SELECTED SAMPLES AT MODERATE-Z | XIS | Y |
| RCS1102-0319 | 165.6362 | -3.316 | 257.90567893 | 49.79184665 | 114.0911 | 54817.3259259259 | 54817.9773611111 | 803065010 | 26381.1 | 21000 | 26381.1 | 26381.1 | 0 | 26381.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13908.9 | 13908.9 | 56270 | 0 | PROCESSED | 57544.9757407407 | 55206 | 54840.2609143518 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031441 | Comparisons between moderate-z X-ray and high-z optically selected clusters indicate that the latter have lower Lx than expected for a given Tx, however it is hard to tell if such discrepancies are due to cluster evolution or selection effects. In an attempt to isolate these two variables, we propose the first detailed comparison of X-ray and optically selected clusters that are well-matched in both velocity dispersion (a quantity independent of both methods) and redshift. Our X-ray analysis of X-ray selected CNOC clusters is complete. Here we propose to determine Lx, Tx, and gas distribution/morphology for an optically selected sample, most of which already have velocity dispersion data in hand, enabling rigorous quantitative comparisons between physical characteristics of the two groups. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | HICKS | AMALIA | NULL | NULL | USA | 3 | AO3 | COSMOLOGY WITH CLUSTERS: CONSTRAINING PHYSICAL DIFFERENCES BETWEEN X-RAY AND OPTICALLY SELECTED SAMPLES AT MODERATE-Z | XIS | Y |
| SHAPLEY OFF-FILAMENT | 201.0894 | -30.5701 | 311.26734846 | 31.76827748 | 298.8248 | 54666.4273958333 | 54670.1905439815 | 803068010 | 143466.9 | 140000 | 143474.9 | 143474.9 | 0 | 143466.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 110811.1 | 110811.1 | 325085.8 | 2 | PROCESSED | 57543.1803240741 | 55073 | 54707.3575694444 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 031451 | It is, in principle, possible to search for the signature of the Warm-Hot Intergalactic Medium (WHIM) in regions between clusters, where WHIM filaments are expected. However, the complexity of the filament network and the distance between clusters makes this approach very difficult (if not impossible), except in few cases where several clusters are sufficiently close together, such as within a supercluster. We propose an investigation using Suzaku of a region within the Shapley Supercluster where, following the cluster network, a filament is expected and a ROSAT PSPC investigation has found excess emission. Suzaku s characteristics will allow a clear detection and characterization of the filament. A second observation in an empty region nearby will be used as control field. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | GALEAZZI | MASSIMILIANO | NULL | NULL | USA | 3 | AO3 | FILAMENTARY X-RAY STRUCTURE IN THE SHAPLEY SUPERCLUSTER | XIS | Y |
| M87N FAINT | 187.6988 | 12.9392 | 283.11850774 | 75.01113844 | 297.6812 | 54625.626400463 | 54627.068275463 | 803069010 | 65247.4 | 60000 | 65247.4 | 65271.4 | 0 | 65255.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 57906.8 | 57906.8 | 124563.8 | 0 | PROCESSED | 57542.7828587963 | 55009 | 54642.2950694444 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 032011 | We propose to take advantage of Suzaku's low background and good collecting area to observe a strong surface brightness discontinuity, most likely a cold front, in the outskirts of M87. We will make accurate temperature and pressure profiles across this cold front, determine the energy associated with it, and compare this to the energy of known AGN-ICM interaction features in M87. With Suzaku's superior spectral redistribution function we will for the first time measure Mg and O in the M87 outskirts and improve constraints on relative contributions by SNIa and SNII. We will study abundance and abundance-ratio variations across the cold front and determine the role of gas sloshing in transporting metals produced by the central galaxy into the ICM. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | EUR | 3 | AO3 | THE ENERGETICS AND METAL ABUNDANCE PATTERNS IN THE OUTSKIRTS OF M87 | XIS | Y |
| M87N BRIGHT | 187.7 | 12.7001 | 283.404729 | 74.78396174 | 297.7704 | 54625.0923263889 | 54625.6259722222 | 803070010 | 24248.5 | 20000 | 24256.5 | 24248.5 | 0 | 24256.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 20270.9 | 20270.9 | 46103.9 | 1 | PROCESSED | 57542.7423263889 | 55009 | 54642.2018865741 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 032011 | We propose to take advantage of Suzaku's low background and good collecting area to observe a strong surface brightness discontinuity, most likely a cold front, in the outskirts of M87. We will make accurate temperature and pressure profiles across this cold front, determine the energy associated with it, and compare this to the energy of known AGN-ICM interaction features in M87. With Suzaku's superior spectral redistribution function we will for the first time measure Mg and O in the M87 outskirts and improve constraints on relative contributions by SNIa and SNII. We will study abundance and abundance-ratio variations across the cold front and determine the role of gas sloshing in transporting metals produced by the central galaxy into the ICM. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | EUR | 3 | AO3 | THE ENERGETICS AND METAL ABUNDANCE PATTERNS IN THE OUTSKIRTS OF M87 | XIS | Y |
| A2163 | 243.8156 | -6.2315 | 6.59879538 | 30.51803676 | 282.2871 | 54696.6726851852 | 54700.4008449074 | 803071010 | 135786.4 | 130000 | 135794.4 | 135786.4 | 0 | 135794.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 122126.2 | 122126.2 | 322061.5 | 5 | PROCESSED | 57543.4331597222 | 55080 | 54713.5071875 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 032023 | Measurements of intracluster gas temperatures out to large radii, where much of the cluster mass resides, are of the utmost importance for the use of clusters in precision cosmology and for studies of cluster physics. Previous attempts to measure robust temperatures at cluster virial radii failed. Here, we demonstrate that such measurements are feasible now for the first time with the Suzaku X-ray CCDs, using our observation of the cluster A2204, carefully treating background and PSF. To determine the temperature profile of the cluster population as a whole, more such observations are required. We show that A2163 is the optimal complementary target for such an investigation. We, therefore, propose to observe A2163 to measure the gas temperature to 15% accuracy out to the virial radius. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | REIPRICH | THOMAS | NULL | NULL | EUR | 3 | AO3 | GALAXY CLUSTER GAS TEMPERATURE MEASUREMENT UP TO THE VIRIAL RADIUS OF A2163 | XIS | Y |
| A3558 WEST OFF | 201.4503 | -31.5856 | 311.44383739 | 30.71755895 | 288.4754 | 54657.5304513889 | 54660.0225 | 803072010 | 81816.2 | 80000 | 81816.2 | 81816.2 | 0 | 81816.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 67394.1 | 67394.1 | 215285.7 | 1 | PROCESSED | 57543.1016898148 | 55037 | 54670.5540162037 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 033089 | We aim at the first significant detection of redshifted OVII and OVIII lines from the warm-hot intergalactic medium (WHIM) in the Shapley Supercluster. The system, located at z = 0.048, shows the richest concentration of X-ray clusters in the nearby universe. Previous ROSAT observation showed enhanced soft X-ray emission along the cluster connection. We propose to observe for 80 ksec a region between A3558 (the brightest central cluster) and A3556, separated by 0.9 virial radius from both clusters and along the line of cluster connection. A 40 ksec observation is also proposed at a 2-degree offest region to measure the foreground Galactic spectrum. Based on the ROSAT flux, we expect to detect redshifted OVII and OVII lines at more than 7 sigma confidence. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | OHASHI | TAKAYA | GALEAZZAI | MASSIMILIANO | JUS | 3 | AO3 | SEARCH FOR WHIM IN THE SHAPLEY SUPERCLUSTER | XIS | Y |
| A496 P-CENTER | 68.4146 | -13.2791 | 209.60984883 | -36.48888222 | 55.8718 | 54680.8514814815 | 54682.0543865741 | 803073010 | 44260.7 | 30000 | 44260.7 | 44260.7 | 0 | 44260.7 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 36935.5 | 36935.5 | 103904 | 2 | PROCESSED | 57543.1885416667 | 55059 | 54693.2133796296 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 034424 | A496 is a "normal" nearby cluster that has been the testbed for metal enrichment models in clusters and, more recently, of different mechanisms to generate cold fronts. Suzaku's excellent spectral resolution, low background and high effective area, combined with the moderate temperatures of this cluster allows us to probe, with two short exposures, into the large scale metal enrichment processes through determination of elemental abundance ratios out to half the virial radius for the first time. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | DUPKE | RENATO | MATSUSHITA | KYOKO | USJ | 3 | AO3 | LARGE SCALE METAL ENRICHMENT MECHANISMS IN ABELL 496 | XIS | Y |
| RXCJ0243.6-4834 | 40.9015 | -48.5654 | 265.11995755 | -59.50535864 | 228.2843 | 55191.5472685185 | 55192.0001967593 | 804001010 | 13205.9 | 10000 | 13213.9 | 13205.9 | 0 | 13221.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10544.8 | 10544.8 | 39129.9 | 0 | PROCESSED | 57549.9594097222 | 55575 | 55209.1119328704 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040005 | We propose Suzaku observations of 8 X-ray luminous clusters of galaxies at z~0.4 that were discovered in the flux-limited REFLEX2 survey. With a total exposure time of 80 ksec, we can determine the temperature of each cluster with 10% accuracy. This significantly improves the determination of the evolution of the luminosity-temperature relation, and will also have an impact on conducting precision cosmology with cluster observations. Thanks to the high sensitivity and low background, this study is carried out most efficiently by Suzaku. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | OTA | NAOMI | NULL | NULL | JAP | 4 | AO4 | LUMINOSITY-TEMPERATURE RELATION OF GALAXY CLUSTERS AT Z~0.4 | XIS | Y |
| RXCJ0234.5-5830 | 38.6494 | -58.5096 | 280.27566127 | -53.84414378 | 249.7915 | 55212.1975115741 | 55212.4794328704 | 804003010 | 13566.5 | 10000 | 13574.5 | 13566.5 | 0 | 13582.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10777.1 | 10777.1 | 24355.9 | 0 | PROCESSED | 57550.1603125 | 55594 | 55228.0359722222 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040005 | We propose Suzaku observations of 8 X-ray luminous clusters of galaxies at z~0.4 that were discovered in the flux-limited REFLEX2 survey. With a total exposure time of 80 ksec, we can determine the temperature of each cluster with 10% accuracy. This significantly improves the determination of the evolution of the luminosity-temperature relation, and will also have an impact on conducting precision cosmology with cluster observations. Thanks to the high sensitivity and low background, this study is carried out most efficiently by Suzaku. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | OTA | NAOMI | NULL | NULL | JAP | 4 | AO4 | LUMINOSITY-TEMPERATURE RELATION OF GALAXY CLUSTERS AT Z~0.4 | XIS | Y |
| RXCJ0018.9-4051 | 4.7354 | -40.8551 | 326.87167276 | -74.72717506 | 232.4175 | 55161.0142708333 | 55161.4169444444 | 804004010 | 19327.8 | 10000 | 19327.8 | 19327.8 | 0 | 19327.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13319.8 | 13319.8 | 34783.9 | 1 | PROCESSED | 57549.5606481482 | 55553 | 55182.6506712963 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040005 | We propose Suzaku observations of 8 X-ray luminous clusters of galaxies at z~0.4 that were discovered in the flux-limited REFLEX2 survey. With a total exposure time of 80 ksec, we can determine the temperature of each cluster with 10% accuracy. This significantly improves the determination of the evolution of the luminosity-temperature relation, and will also have an impact on conducting precision cosmology with cluster observations. Thanks to the high sensitivity and low background, this study is carried out most efficiently by Suzaku. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | OTA | NAOMI | NULL | NULL | JAP | 4 | AO4 | LUMINOSITY-TEMPERATURE RELATION OF GALAXY CLUSTERS AT Z~0.4 | XIS | Y |
| DEM L 192 | 81.4194 | -67.497 | 277.77177426 | -33.0775429 | 334.6993 | 54968.6808680556 | 54971.0113310185 | 804009010 | 87316.5 | 80000 | 87324.5 | 87316.5 | 0 | 87324.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 80058.9 | 80058.9 | 201327.7 | 2 | PROCESSED | 57546.6405439815 | 55356 | 54987.4577314815 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040009 | The combined actions of fast stellar winds and core-collapse supernova explosions of the massive stars create large shell-like structures, called superbubbles (SBs), by sweeping up the ambient medium. Large tenuous cavities created inside the SB walls allow that the blast shocks of the interior supernova remnants (SNRs) expand rapidly without decelerating for a long time. Therefore, the timescale of efficient cosmic-ray acceleration can be much longer than that of most isolated SNRs. We propose the observations on DEM L 192 and DEM L 205, which are the SBs in the Large Magellanic Cloud, in order to search the large non-thermal SNR shells hidden inside the SBs. They are the strong candidates of the accelerators of the "knee energy" particles. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YAMAGUCHI | HIROYA | NULL | NULL | JAP | 4 | AO4 | DEM L 192 AND DEM L 205: SUPERBUBBLES IN THE LARGE MAGELLANIC CLOUD | XIS | Y |
| DEM L 205 | 82.0576 | -67.4229 | 277.64219696 | -32.8462006 | 9.9744 | 55005.3430092593 | 55006.4578472222 | 804010010 | 41343.3 | 40000 | 41349.2 | 41349.2 | 0 | 41343.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37382.9 | 37382.9 | 96307.8 | 3 | PROCESSED | 57547.6717361111 | 55381 | 55015.1437268518 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040009 | The combined actions of fast stellar winds and core-collapse supernova explosions of the massive stars create large shell-like structures, called superbubbles (SBs), by sweeping up the ambient medium. Large tenuous cavities created inside the SB walls allow that the blast shocks of the interior supernova remnants (SNRs) expand rapidly without decelerating for a long time. Therefore, the timescale of efficient cosmic-ray acceleration can be much longer than that of most isolated SNRs. We propose the observations on DEM L 192 and DEM L 205, which are the SBs in the Large Magellanic Cloud, in order to search the large non-thermal SNR shells hidden inside the SBs. They are the strong candidates of the accelerators of the "knee energy" particles. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | YAMAGUCHI | HIROYA | NULL | NULL | JAP | 4 | AO4 | DEM L 192 AND DEM L 205: SUPERBUBBLES IN THE LARGE MAGELLANIC CLOUD | XIS | Y |
| A2219 | 250.0709 | 46.72 | 72.64070926 | 41.481603 | 57.4824 | 54924.5730787037 | 54927.1154282407 | 804011010 | 106648.1 | 100000 | 106648.1 | 106648.1 | 0 | 106659 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 114798.6 | 114798.6 | 219639.8 | 2 | PROCESSED | 57546.0936921296 | 55324 | 54949.5242939815 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040011 | We propose Suzaku observations of two massive clusters with different radio morphologies, A2219 and A2390, to search for extremely hot (~25 keV) thermal gas. Because of the presence of hot regions indicated in X-ray temperature maps as well as extended radio halo emission, they are the best candidates hosting strongly heated gas due to the past mergers. With the Suzaku broad-band spectroscopy, we can examine properties of very hot gas with high accuracy, and also put constraints on non-thermal emission. This study can only be achieved by the Suzaku's excellent sensitivity to spectral observations over the wide band, and will bring us new insights into physics of gas heating in clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | OTA | NAOMI | NULL | NULL | JAP | 4 | AO4 | SEARCH FOR EXTREMELY HOT GAS IN TWO MASSIVE GALAXY CLUSTERS | XIS | Y |
| A2390 | 328.3984 | 17.7035 | 73.96308198 | -27.80512015 | 79.9886 | 54955.5395486111 | 54957.6939583333 | 804012010 | 96464.5 | 90000 | 96464.5 | 96473 | 0 | 96472.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 85538.6 | 85538.6 | 186111.9 | 1 | PROCESSED | 57546.5371990741 | 55343 | 54976.1695023148 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040011 | We propose Suzaku observations of two massive clusters with different radio morphologies, A2219 and A2390, to search for extremely hot (~25 keV) thermal gas. Because of the presence of hot regions indicated in X-ray temperature maps as well as extended radio halo emission, they are the best candidates hosting strongly heated gas due to the past mergers. With the Suzaku broad-band spectroscopy, we can examine properties of very hot gas with high accuracy, and also put constraints on non-thermal emission. This study can only be achieved by the Suzaku's excellent sensitivity to spectral observations over the wide band, and will bring us new insights into physics of gas heating in clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | OTA | NAOMI | NULL | NULL | JAP | 4 | AO4 | SEARCH FOR EXTREMELY HOT GAS IN TWO MASSIVE GALAXY CLUSTERS | XIS | Y |
| NGC 5044 NORTH 30' | 199.0992 | -15.8941 | 311.67530339 | 46.55349501 | 110.0017 | 55220.5889814815 | 55222.2571064815 | 804013010 | 62848.2 | 60000 | 62856.2 | 62848.2 | 0 | 62856.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44592.6 | 44592.6 | 144099.8 | 1 | PROCESSED | 57550.396099537 | 55602 | 55235.338587963 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040013 | Why groups of galaxies contain smaller amount of metals than clusters of galaxies? To study metal sysnthesis history of galaxies in groups, we propose to observe two offset pointings of the NGC 5044 group and HCG 62 to derive metal distribution of intragroup medium up to 0.5 r180. Due to its low background, Suzaku enables us to study regions at low surface brightness. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MATSUSHITA | KYOKO | NULL | NULL | JAP | 4 | AO4 | METAL MASS TO LIGHT RATIOS OF GROUPS OF GALAXIES UP TO 0.5R180 | XIS | Y |
| NGC 5044 SOUTH 30' | 198.7482 | -16.8629 | 311.00467544 | 45.63931299 | 110.0008 | 55222.2581365741 | 55224.0190277778 | 804014010 | 65176.6 | 60000 | 65184.6 | 65176.6 | 0 | 65184.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44162.8 | 44162.8 | 152121.8 | 1 | PROCESSED | 57550.4424768518 | 55602 | 55236.2169675926 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040013 | Why groups of galaxies contain smaller amount of metals than clusters of galaxies? To study metal sysnthesis history of galaxies in groups, we propose to observe two offset pointings of the NGC 5044 group and HCG 62 to derive metal distribution of intragroup medium up to 0.5 r180. Due to its low background, Suzaku enables us to study regions at low surface brightness. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MATSUSHITA | KYOKO | NULL | NULL | JAP | 4 | AO4 | METAL MASS TO LIGHT RATIOS OF GROUPS OF GALAXIES UP TO 0.5R180 | XIS | Y |
| FERMI_0265 | 187.8001 | -14.1665 | 295.53023761 | 48.41419063 | 294.2648 | 55020.9540277778 | 55021.5418981482 | 804017010 | 26311.5 | 80000 | 26311.5 | 26311.5 | 0 | 26311.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22846.3 | 22846.3 | 50787.9 | 1 | PROCESSED | 57547.7938773148 | 55422 | 55034.2333217593 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040014 | We propose the first X-ray follow-up observations of 7 truly unidentified GeV sources at high Galactic latitude (b >10 deg), recently confirmed by Fermi gamma-ray space telescope. An exotic spectral energy distribution (where GeV flux is 6 orders of magnitude brighter than radio-to-X-ray) as well as quiescent emission over decades suggest they are NOT associated with QSOs and blazars, but a new-type of GeV gamma-ray emitters. Three of these are embedded in crowded regions of cluster pairs/groups and could be associated with large-scale shocks of cluster formation. Thanks to excellent sensitivity of Fermi, we have accurately determined their position within ~8 arcmin (95%) for a coverage of single XIS pointing. We propose a total exposure of 280 ks for 7 unID sources. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KATAOKA | JUN | NULL | NULL | JAP | 4 | AO4 | SUZAKU OBSERVATIONS OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE | XIS | Y |
| FERMI_0265 | 187.7993 | -14.1672 | 295.5292019 | 48.41340382 | 292.6305 | 55040.2233449074 | 55041.5002777778 | 804017020 | 52637.8 | 54000 | 52637.8 | 52909.8 | 0 | 52901.8 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 48060 | 48060 | 110304.1 | 0 | PROCESSED | 57547.9908333333 | 55422 | 55050.4462384259 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040014 | We propose the first X-ray follow-up observations of 7 truly unidentified GeV sources at high Galactic latitude (b >10 deg), recently confirmed by Fermi gamma-ray space telescope. An exotic spectral energy distribution (where GeV flux is 6 orders of magnitude brighter than radio-to-X-ray) as well as quiescent emission over decades suggest they are NOT associated with QSOs and blazars, but a new-type of GeV gamma-ray emitters. Three of these are embedded in crowded regions of cluster pairs/groups and could be associated with large-scale shocks of cluster formation. Thanks to excellent sensitivity of Fermi, we have accurately determined their position within ~8 arcmin (95%) for a coverage of single XIS pointing. We propose a total exposure of 280 ks for 7 unID sources. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KATAOKA | JUN | NULL | NULL | JAP | 4 | AO4 | SUZAKU OBSERVATIONS OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE | XIS | Y |
| FERMI_0281 | 197.9603 | -34.4918 | 307.70107754 | 28.19093927 | 309.4896 | 55047.2059606482 | 55048.3043287037 | 804018010 | 39903.8 | 40000 | 39903.8 | 39903.8 | 0 | 39903.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35570.8 | 35570.8 | 94881.9 | 1 | PROCESSED | 57548.0705902778 | 55423 | 55060.7435763889 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040014 | We propose the first X-ray follow-up observations of 7 truly unidentified GeV sources at high Galactic latitude (b >10 deg), recently confirmed by Fermi gamma-ray space telescope. An exotic spectral energy distribution (where GeV flux is 6 orders of magnitude brighter than radio-to-X-ray) as well as quiescent emission over decades suggest they are NOT associated with QSOs and blazars, but a new-type of GeV gamma-ray emitters. Three of these are embedded in crowded regions of cluster pairs/groups and could be associated with large-scale shocks of cluster formation. Thanks to excellent sensitivity of Fermi, we have accurately determined their position within ~8 arcmin (95%) for a coverage of single XIS pointing. We propose a total exposure of 280 ks for 7 unID sources. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KATAOKA | JUN | NULL | NULL | JAP | 4 | AO4 | SUZAKU OBSERVATIONS OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE | XIS | Y |
| FERMI_0291 | 203.2955 | 51.017 | 107.38909593 | 64.83295576 | 302.8355 | 54983.4258680556 | 54984.4725 | 804019010 | 46353.6 | 40000 | 46361.6 | 46353.6 | 0 | 46369.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42707.3 | 42707.3 | 90385.8 | 1 | PROCESSED | 57547.4428703704 | 55363 | 54994.2756018518 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040014 | We propose the first X-ray follow-up observations of 7 truly unidentified GeV sources at high Galactic latitude (b >10 deg), recently confirmed by Fermi gamma-ray space telescope. An exotic spectral energy distribution (where GeV flux is 6 orders of magnitude brighter than radio-to-X-ray) as well as quiescent emission over decades suggest they are NOT associated with QSOs and blazars, but a new-type of GeV gamma-ray emitters. Three of these are embedded in crowded regions of cluster pairs/groups and could be associated with large-scale shocks of cluster formation. Thanks to excellent sensitivity of Fermi, we have accurately determined their position within ~8 arcmin (95%) for a coverage of single XIS pointing. We propose a total exposure of 280 ks for 7 unID sources. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KATAOKA | JUN | NULL | NULL | JAP | 4 | AO4 | SUZAKU OBSERVATIONS OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE | XIS | Y |
| FERMI_0459 | 304.3461 | 6.0496 | 48.6197877 | -16.02859504 | 257.4741 | 55131.4269097222 | 55132.2224189815 | 804020010 | 32812.8 | 30000 | 32812.8 | 32812.8 | 0 | 32812.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28625.1 | 28625.1 | 68725.9 | 0 | PROCESSED | 57549.0265046296 | 55513 | 55149.4269791667 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040014 | We propose the first X-ray follow-up observations of 7 truly unidentified GeV sources at high Galactic latitude (b >10 deg), recently confirmed by Fermi gamma-ray space telescope. An exotic spectral energy distribution (where GeV flux is 6 orders of magnitude brighter than radio-to-X-ray) as well as quiescent emission over decades suggest they are NOT associated with QSOs and blazars, but a new-type of GeV gamma-ray emitters. Three of these are embedded in crowded regions of cluster pairs/groups and could be associated with large-scale shocks of cluster formation. Thanks to excellent sensitivity of Fermi, we have accurately determined their position within ~8 arcmin (95%) for a coverage of single XIS pointing. We propose a total exposure of 280 ks for 7 unID sources. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KATAOKA | JUN | NULL | NULL | JAP | 4 | AO4 | SUZAKU OBSERVATIONS OF FERMI UNID SOURCES AT HIGH GALACTIC LATITUDE | XIS | Y |
| A2029_1 | 227.7409 | 5.7498 | 6.48668362 | 50.54283023 | 112.9511 | 55224.0253819444 | 55224.3328703704 | 804024010 | 7692.5 | 10000 | 7692.5 | 7707.9 | 0 | 7700.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 4608.3 | 4608.3 | 26563.9 | 1 | PROCESSED | 57550.3752314815 | 55612 | 55245.2966203704 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040030 | Suzaku has enabled a breakthough to be made in the study of the outer parts of clusters. For the first time the gas properties have been measured in the cluster PKS 0745-19 to beyond the virial radius. This is important for understanding the properties of clusters, such as total mass and total gas mass which are required for cosmological studies. They are also needed for understanding how clusters match to the outer Universe in their temperature and entropy profiles. Are there any large scale accretion shocks? How do filaments match to clusters? The breakthrough has been possible due to low background of the Suzaku FI CCD and the use of a particularly bright cluster. We propose here to exploit Suzaku's unique capability to extend this result using the 2 X-ray bright, relaxed clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAWARA | YUZURU | NULL | NULL | JAP | 4 | AO4 | TO THE VIRIAL RADIUS IN THE BRIGHT LUMINOUS CLUSTERS, A2029 AND A478 | XIS | Y |
| A2029_2 | 227.8527 | 6.0108 | 6.92100367 | 50.6092725 | 112.9534 | 55224.3333912037 | 55224.9794444444 | 804024020 | 26018.5 | 22000 | 26022.5 | 26018.5 | 0 | 26026.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15903.3 | 15903.3 | 55814 | 0 | PROCESSED | 57550.4048726852 | 55637 | 55271.0156365741 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040030 | Suzaku has enabled a breakthough to be made in the study of the outer parts of clusters. For the first time the gas properties have been measured in the cluster PKS 0745-19 to beyond the virial radius. This is important for understanding the properties of clusters, such as total mass and total gas mass which are required for cosmological studies. They are also needed for understanding how clusters match to the outer Universe in their temperature and entropy profiles. Are there any large scale accretion shocks? How do filaments match to clusters? The breakthrough has been possible due to low background of the Suzaku FI CCD and the use of a particularly bright cluster. We propose here to exploit Suzaku's unique capability to extend this result using the 2 X-ray bright, relaxed clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAWARA | YUZURU | NULL | NULL | JAP | 4 | AO4 | TO THE VIRIAL RADIUS IN THE BRIGHT LUMINOUS CLUSTERS, A2029 AND A478 | XIS | Y |
| A2029_3 | 227.6311 | 5.4874 | 6.05366388 | 50.47243927 | 112.9537 | 55224.9801041667 | 55225.6140509259 | 804024030 | 17909.5 | 22000 | 17917.5 | 17925.5 | 0 | 17909.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 8926.8 | 8926.8 | 54765.9 | 0 | PROCESSED | 57550.4118865741 | 55637 | 55270.9888425926 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040030 | Suzaku has enabled a breakthough to be made in the study of the outer parts of clusters. For the first time the gas properties have been measured in the cluster PKS 0745-19 to beyond the virial radius. This is important for understanding the properties of clusters, such as total mass and total gas mass which are required for cosmological studies. They are also needed for understanding how clusters match to the outer Universe in their temperature and entropy profiles. Are there any large scale accretion shocks? How do filaments match to clusters? The breakthrough has been possible due to low background of the Suzaku FI CCD and the use of a particularly bright cluster. We propose here to exploit Suzaku's unique capability to extend this result using the 2 X-ray bright, relaxed clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAWARA | YUZURU | NULL | NULL | JAP | 4 | AO4 | TO THE VIRIAL RADIUS IN THE BRIGHT LUMINOUS CLUSTERS, A2029 AND A478 | XIS | Y |
| A2029_4 | 228.0053 | 5.6496 | 6.60771448 | 50.27207577 | 112.9543 | 55225.6146180556 | 55226.2501388889 | 804024040 | 25658.4 | 22000 | 25658.4 | 25682.4 | 0 | 25666.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19446 | 19446 | 54901.9 | 0 | PROCESSED | 57550.4263657407 | 55637 | 55271.0446064815 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040030 | Suzaku has enabled a breakthough to be made in the study of the outer parts of clusters. For the first time the gas properties have been measured in the cluster PKS 0745-19 to beyond the virial radius. This is important for understanding the properties of clusters, such as total mass and total gas mass which are required for cosmological studies. They are also needed for understanding how clusters match to the outer Universe in their temperature and entropy profiles. Are there any large scale accretion shocks? How do filaments match to clusters? The breakthrough has been possible due to low background of the Suzaku FI CCD and the use of a particularly bright cluster. We propose here to exploit Suzaku's unique capability to extend this result using the 2 X-ray bright, relaxed clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAWARA | YUZURU | NULL | NULL | JAP | 4 | AO4 | TO THE VIRIAL RADIUS IN THE BRIGHT LUMINOUS CLUSTERS, A2029 AND A478 | XIS | Y |
| A2029_5 | 227.4808 | 5.8608 | 6.38223601 | 50.81650996 | 112.9567 | 55226.2508912037 | 55226.875162037 | 804024050 | 21891 | 22000 | 21891 | 21891 | 0 | 21891 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14341.9 | 14341.9 | 53936 | 0 | PROCESSED | 57550.432337963 | 55638 | 55272.0370717593 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040030 | Suzaku has enabled a breakthough to be made in the study of the outer parts of clusters. For the first time the gas properties have been measured in the cluster PKS 0745-19 to beyond the virial radius. This is important for understanding the properties of clusters, such as total mass and total gas mass which are required for cosmological studies. They are also needed for understanding how clusters match to the outer Universe in their temperature and entropy profiles. Are there any large scale accretion shocks? How do filaments match to clusters? The breakthrough has been possible due to low background of the Suzaku FI CCD and the use of a particularly bright cluster. We propose here to exploit Suzaku's unique capability to extend this result using the 2 X-ray bright, relaxed clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAWARA | YUZURU | NULL | NULL | JAP | 4 | AO4 | TO THE VIRIAL RADIUS IN THE BRIGHT LUMINOUS CLUSTERS, A2029 AND A478 | XIS | Y |
| A1246_CENTER | 170.9992 | 21.4865 | 224.00399917 | 69.32667171 | 120.0006 | 55151.2043981482 | 55152.274525463 | 804028010 | 48456.4 | 40000 | 48472.4 | 48456.4 | 0 | 48472.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37215.6 | 37215.6 | 92433.9 | 0 | PROCESSED | 57549.4081018518 | 55531 | 55162.1616319445 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040053 | We propose 40 and 80 ksec observations of the central and offset regions of Abell 1246, respectively, to study the temperature and mass profiles out to the virial radius. This cluster is moderately distant (z=0.1902), and relaxed system (kT=5.7 keV), with a diameter of about 20'. The low background of the XIS instrument will enable us to observe the region around the virial radius. The dentity and temperature of ICM around the virial radius should directly reflect the process of gas infall and heating. The correct temperature curve is also vital to determine the gravitational mass distribution. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | SATO | KOSUKE | NULL | NULL | JAP | 4 | AO4 | MASS AND TEMPERATURE PROFILES OF THE RELAXED CLUSTER A1246 | XIS | Y |
| A1246_OFF | 171.128 | 21.4191 | 224.30142226 | 69.41574013 | 120.0005 | 55163.0212152778 | 55164.9606365741 | 804029010 | 80380.4 | 80000 | 80396.4 | 80380.4 | 0 | 80391 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 55158 | 55158 | 167555.8 | 1 | PROCESSED | 57549.6578472222 | 55549 | 55181.239849537 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040053 | We propose 40 and 80 ksec observations of the central and offset regions of Abell 1246, respectively, to study the temperature and mass profiles out to the virial radius. This cluster is moderately distant (z=0.1902), and relaxed system (kT=5.7 keV), with a diameter of about 20'. The low background of the XIS instrument will enable us to observe the region around the virial radius. The dentity and temperature of ICM around the virial radius should directly reflect the process of gas infall and heating. The correct temperature curve is also vital to determine the gravitational mass distribution. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | SATO | KOSUKE | NULL | NULL | JAP | 4 | AO4 | MASS AND TEMPERATURE PROFILES OF THE RELAXED CLUSTER A1246 | XIS | Y |
| NGC 2300 GROUP | 112.8158 | 85.6965 | 127.72434362 | 27.79082708 | 339.9138 | 55235.7626388889 | 55236.5002893518 | 804030010 | 37059.1 | 100000 | 37059.1 | 37059.1 | 0 | 37059.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34453.4 | 34453.4 | 63729.9 | 1 | PROCESSED | 57550.5366666667 | 55619 | 55251.1588310185 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040055 | We propose to observe the NGC 2300 group for 100 ks and a offset pointing for 200 ks to evaluate the background emission from the Galaxy. The purpose of the observations are to measure O, Mg, Si and Fe abundances of intragaractic medium to study metal synthesis in this small group of galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MATSUSHITA | KYOKO | NULL | NULL | JAP | 4 | AO4 | O, MG, S AND FE ABUNDANCES OF INTRAGROUP MEDIUM IN THE NGC 2300 GROUP | XIS | Y |
| NGC 2300 GROUP | 112.834 | 85.6974 | 127.72312729 | 27.79205873 | 339.9186 | 55237.1794907407 | 55238.2502777778 | 804030020 | 52561.1 | 100000 | 52561.1 | 52561.1 | 0 | 52561.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47712 | 47712 | 92498 | 0 | PROCESSED | 57550.5807986111 | 55633 | 55266.3365625 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040055 | We propose to observe the NGC 2300 group for 100 ks and a offset pointing for 200 ks to evaluate the background emission from the Galaxy. The purpose of the observations are to measure O, Mg, Si and Fe abundances of intragaractic medium to study metal synthesis in this small group of galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MATSUSHITA | KYOKO | NULL | NULL | JAP | 4 | AO4 | O, MG, S AND FE ABUNDANCES OF INTRAGROUP MEDIUM IN THE NGC 2300 GROUP | XIS | Y |
| NGC 2300 OFFSET | 116.7261 | 85.6829 | 127.68344404 | 28.08274711 | 339.9009 | 55235.4123148148 | 55235.7606365741 | 804031010 | 19196 | 20000 | 19196 | 19196 | 0 | 19196 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17147.7 | 17147.7 | 30087.9 | 0 | PROCESSED | 57550.5104282407 | 55633 | 55266.1898148148 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040055 | We propose to observe the NGC 2300 group for 100 ks and a offset pointing for 200 ks to evaluate the background emission from the Galaxy. The purpose of the observations are to measure O, Mg, Si and Fe abundances of intragaractic medium to study metal synthesis in this small group of galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MATSUSHITA | KYOKO | NULL | NULL | JAP | 4 | AO4 | O, MG, S AND FE ABUNDANCES OF INTRAGROUP MEDIUM IN THE NGC 2300 GROUP | XIS | Y |
| FORNAX A W-LOBE W | 50.2219 | -37.0341 | 239.92107074 | -57.06786371 | 27.0759 | 54990.6810763889 | 54991.75375 | 804036010 | 60362.5 | 50000 | 60362.5 | 60362.5 | 0 | 60362.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 56396.5 | 56396.5 | 92651.9 | 1 | PROCESSED | 57547.532974537 | 55367 | 55001.0562615741 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040073 | We propose Suzaku offset mapping observations of the Fornax A west radio lobe. By measuring the inverse-Compton X-ray spectra from the radio lobe with the mapping observations, we measure the brightness profile in the non-thermal X-ray emission. The results show us the spatial distribution of the relativistic electrons independently from the magnetic field structures determining the synchrotron radio emissions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | TASHIRO | MAKOTO | NULL | NULL | JAP | 4 | AO4 | X-RAY MAPPING OF THE FORNAX A WEST LOBE | XIS | Y |
| FORNAX A W-LOBE N | 50.5227 | -36.9675 | 239.75066849 | -56.83654313 | 27.8129 | 54991.7546875 | 54992.8119675926 | 804037010 | 60762.7 | 50000 | 60770.7 | 60762.7 | 0 | 60770.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 54817 | 54817 | 91325.8 | 1 | PROCESSED | 57547.5602777778 | 55367 | 55001.1883912037 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040073 | We propose Suzaku offset mapping observations of the Fornax A west radio lobe. By measuring the inverse-Compton X-ray spectra from the radio lobe with the mapping observations, we measure the brightness profile in the non-thermal X-ray emission. The results show us the spatial distribution of the relativistic electrons independently from the magnetic field structures determining the synchrotron radio emissions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | TASHIRO | MAKOTO | NULL | NULL | JAP | 4 | AO4 | X-RAY MAPPING OF THE FORNAX A WEST LOBE | XIS | Y |
| FORNAX A W-LOBE S | 50.358 | -37.3109 | 240.40250552 | -56.92779805 | 62.5011 | 55012.4989930556 | 55013.9619675926 | 804038010 | 52425.3 | 50000 | 52433.3 | 52433.3 | 0 | 52425.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11712.1 | 11712.1 | 36360 | 1 | PROCESSED | 57547.7267013889 | 55393 | 55026.4458564815 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040073 | We propose Suzaku offset mapping observations of the Fornax A west radio lobe. By measuring the inverse-Compton X-ray spectra from the radio lobe with the mapping observations, we measure the brightness profile in the non-thermal X-ray emission. The results show us the spatial distribution of the relativistic electrons independently from the magnetic field structures determining the synchrotron radio emissions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | TASHIRO | MAKOTO | NULL | NULL | JAP | 4 | AO4 | X-RAY MAPPING OF THE FORNAX A WEST LOBE | XIS | Y |
| FORNAX A W-LOBE S | 50.3569 | -37.3111 | 240.40306132 | -56.92864271 | 79.0007 | 55065.4424189815 | 55066.6731365741 | 804038020 | 45569.3 | 42000 | 45569.3 | 45569.3 | 0 | 45569.3 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 38953.4 | 38953.4 | 106259.9 | 0 | PROCESSED | 57548.3175347222 | 55444 | 55078.0721064815 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040073 | We propose Suzaku offset mapping observations of the Fornax A west radio lobe. By measuring the inverse-Compton X-ray spectra from the radio lobe with the mapping observations, we measure the brightness profile in the non-thermal X-ray emission. The results show us the spatial distribution of the relativistic electrons independently from the magnetic field structures determining the synchrotron radio emissions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | TASHIRO | MAKOTO | NULL | NULL | JAP | 4 | AO4 | X-RAY MAPPING OF THE FORNAX A WEST LOBE | XIS | Y |
| N103B | 77.15 | -68.7359 | 279.60217418 | -34.399508 | 199.4598 | 55194.4728356482 | 55200.6044560185 | 804039010 | 223899.9 | 150000 | 224010.8 | 223899.9 | 0 | 224002.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46096 | 46096 | 129955.8 | 0 | PROCESSED | 57550.0511805556 | 55584 | 55218.4707060185 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040080 | We aim to detect very low abundance lines, Cr and Mn, from SNR N103B in the Large Magellanic Cloud which is a low metaricity galaxy. It is known that a mass ratio of Mn to Cr synthesized in Type Ia supernovae is strongly correrated with the metaricity of the progenitor white dwarf. In the early Suzaku observation, we already detected the Cr line with about 3-sigma confidence level. In this follow-up observation, we detect the Cr and Mn lines with significant confidence, and determine the metaricity of the progenitor of SNR N103B. This will be the first measurement of the white dwarf's metaricity in the extra-galactic object. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | TAMAGAWA | TORU | NULL | NULL | JAP | 4 | AO4 | A MANGANESE LINE DETECTION FROM SNR N103B IN A LOW METARICITY GALAXY | XIS | Y |
| ABELL 2255 CENTER | 258.2484 | 64.1467 | 94.02951141 | 34.88778486 | 111.176 | 55234.3014814815 | 55235.405775463 | 804041010 | 44533.7 | 50000 | 44533.7 | 44541.7 | 0 | 44541.7 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 43339 | 43339 | 95375.9 | 1 | PROCESSED | 57550.5171180556 | 55617 | 55250.1645601852 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 040091 | Suzaku discovered an supra thermal component in the plasma of Abell 3667 which exceeds 13 keV. In order to establish this component in merging clusters, we propose two pointing observations of Abell 2255, which hosts a huge radio halo and a radio relic. With these two pointings, we aim at roughly spotting the location of the supra thermal plasma. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KAWAHARADA | MADOKA | NULL | NULL | JAP | 4 | AO4 | PROBING SUPRA THERMAL PLASMA IN ABELL 2255 WITH SUZAKU | HXD | Y |
| NGC 4125 | 182.0568 | 65.1777 | 130.16762444 | 51.33919783 | 175.9017 | 55103.512037037 | 55105.4578009259 | 804047010 | 104080.1 | 100000 | 104080.1 | 104088.1 | 0 | 104096.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 93725.7 | 93725.7 | 168085.7 | 0 | PROCESSED | 57548.726712963 | 55491 | 55125.5744212963 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041502 | Recent observations of relaxed galaxy groups have revealed ubiquitous abundance gradients, indicating large-scale mixing of the gas, possibly driven by AGN feedback. Exploiting the low background and good sensitivity of Suzaku, we have found similar gradients in two lower mass, galaxy-scale systems, which has important implications for models of feedback and chemical enrichment. We propose to observe two more isolated elliptical galaxies, thus starting to building a sample for determining the frequency and properties of such abundance gradients in early-type galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | HUMPHREY | PHILIP | NULL | NULL | USA | 4 | AO4 | ABUNDANCE GRADIENTS IN EARLY-TYPE GALAXIES | XIS | Y |
| NGC 5174 | 202.3569 | 11.0203 | 333.76702191 | 71.58014685 | 102.4436 | 55219.0472685185 | 55220.5835532407 | 804048010 | 54515.1 | 50000 | 54523.1 | 54515.1 | 0 | 54523.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44036.2 | 44036.2 | 132697.9 | 0 | PROCESSED | 57550.3479050926 | 55595 | 55229.1361226852 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041504 | Galaxies are missing most of their baryons when compared to the cosmological baryon to dark matter ratio: the Milky Way retained only 30% of its baryons while lower mass galaxies retain less than 10%. Probably, these baryons were expelled by intense galactic winds during the early star formation period at z = 1-3. These galactic winds can carry gas far beyond the virial radius of small and modest galaxies, but the most massive galaxies should retain much of this gas. We propose to test this picture by searching for the missing baryons surrounding two extremely massive spiral galaxies, with 6-8 times the stellar content of M31 and with v_rot = 370, 420 km/s. If successful, we will detect a significant fraction of the 3-4E11 Msun of the missing baryons as hot gas. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | BREGMAN | JOEL | NULL | NULL | USA | 4 | AO4 | THE BARYON CONTENT OF MASSIVE SPIRAL GALAXIES | XIS | Y |
| NGC 669 | 26.8113 | 35.5683 | 135.52840833 | -25.9346715 | 67.5273 | 55017.2207523148 | 55018.4377777778 | 804049010 | 50252.8 | 50000 | 50260.8 | 50252.8 | 0 | 50260.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 45402.3 | 45402.3 | 105119.9 | 11 | PROCESSED | 57547.7727430556 | 55395 | 55029.2656944444 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041504 | Galaxies are missing most of their baryons when compared to the cosmological baryon to dark matter ratio: the Milky Way retained only 30% of its baryons while lower mass galaxies retain less than 10%. Probably, these baryons were expelled by intense galactic winds during the early star formation period at z = 1-3. These galactic winds can carry gas far beyond the virial radius of small and modest galaxies, but the most massive galaxies should retain much of this gas. We propose to test this picture by searching for the missing baryons surrounding two extremely massive spiral galaxies, with 6-8 times the stellar content of M31 and with v_rot = 370, 420 km/s. If successful, we will detect a significant fraction of the 3-4E11 Msun of the missing baryons as hot gas. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | BREGMAN | JOEL | NULL | NULL | USA | 4 | AO4 | THE BARYON CONTENT OF MASSIVE SPIRAL GALAXIES | XIS | Y |
| NGC6482 | 267.957 | 23.086 | 48.10607859 | 22.91404378 | 109.6205 | 55238.2645949074 | 55239.2919444444 | 804050010 | 46546.7 | 45000 | 46546.7 | 46546.7 | 0 | 46546.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28516.6 | 28516.6 | 88743.8 | 0 | PROCESSED | 57550.5834143518 | 55622 | 55251.3186458333 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041513 | Fossil groups present a puzzle to current theories of structure formation. Despite the low number of bright galaxies, their high velocity dispersions and gas temperatures indicate potential wells deeper than that of normal groups. Their measured c200 are high indicating very early formation epochs, which is in contradiction with the lack of cooling cores observed. We can constrain their ages by looking at the distribution of the SN Ia and II ejecta near their core. If they are formed more recently than normal groups by galaxy merging near the core, the central gas should have a reduction of SN Ia dominance, differently from what is observed in normal groups. We propose to test this with the most optimal and nearest fossil group, NGC6482, matching very well the capabilities of Suzaku. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | DUPKE | RENATO | NULL | NULL | USA | 4 | AO4 | DISCRIMINATING COMPETING MODELS FOR THE ORIGIN OF FOSSIL GROUPS OF GALAXIES WITH SUZAKU | XIS | Y |
| RXJ1159+5531 | 179.953 | 55.611 | 137.55848692 | 60.02702904 | 317.8793 | 54953.4172222222 | 54955.52875 | 804051010 | 85489.2 | 75000 | 85497.2 | 85489.2 | 0 | 85497.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 82412.8 | 82412.8 | 182421.8 | 2 | PROCESSED | 57546.517974537 | 55343 | 54976.1055439815 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041514 | We propose a 75ks observation of the galaxy group RXJ1159+5531 to place definitive constraints on its gas out to the virial radius (Rvir). These unprecedented measurements will enable us to study the entropy profile at scales near the region in which accretion shocks become important, and will reveal whether its flattening outside the core of the group extends as far as Rvir. Furthermore, we will obtain the mass profile and test the validity of the NFW model in the outer parts of the halo. Due to its high surface brightness and favourable distance, RXJ1159+5531 is the ideal target with which to carry out this study. It will constitute a textbook case for constraining the feedback and other nongravitational processes which shape the distribution of hot gas in galaxy groups. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | HUMPHREY | PHILIP | NULL | NULL | USA | 4 | AO4 | GAS IN A GALAXY GROUP AT THE VIRIAL RADIUS: RXJ1159+5531, A TEXTBOOK EXAMPLE | XIS | Y |
| NGC741MOSAICE_P1 | 29.7199 | 5.461 | 152.014798 | -53.55912322 | 71.7248 | 55053.8433796296 | 55054.0834837963 | 804052010 | 10830.2 | 10000 | 10834.2 | 10830.2 | 0 | 10838.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 7862.7 | 7862.7 | 20740 | 0 | PROCESSED | 57548.1137847222 | 55448 | 55081.2096875 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041515 | Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | BREGMAN | JOEL | NULL | NULL | USA | 4 | AO4 | THE MISSING BARYONS IN GALAXY GROUPS | XIS | Y |
| NGC741MOSAICE_P2 | 29.9595 | 5.5362 | 152.32010482 | -53.38732445 | 71.7775 | 55054.083912037 | 55054.3334837963 | 804052020 | 12734.1 | 10000 | 12734.1 | 12742.1 | 0 | 12742.1 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12015.9 | 12015.9 | 21559.9 | 0 | PROCESSED | 57548.1149884259 | 55448 | 55081.2532060185 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041515 | Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | BREGMAN | JOEL | NULL | NULL | USA | 4 | AO4 | THE MISSING BARYONS IN GALAXY GROUPS | XIS | Y |
| NGC741MOSAICE_P3 | 29.6423 | 5.6966 | 151.72656453 | -53.38013742 | 71.7748 | 55054.3340509259 | 55054.5765393518 | 804052030 | 9891.8 | 10000 | 9891.8 | 9891.8 | 0 | 9907.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7959.9 | 7959.9 | 20943.9 | 1 | PROCESSED | 57548.1180555556 | 55448 | 55081.2008101852 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041515 | Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | BREGMAN | JOEL | NULL | NULL | USA | 4 | AO4 | THE MISSING BARYONS IN GALAXY GROUPS | XIS | Y |
| NGC741MOSAICE_P4 | 29.8808 | 5.7741 | 152.02832852 | -53.20754513 | 71.8261 | 55054.5770138889 | 55054.8084953704 | 804052040 | 11025.7 | 10000 | 11025.7 | 11321.7 | 0 | 11305.7 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 11390.2 | 11390.2 | 19995.9 | 0 | PROCESSED | 57548.1244328704 | 55448 | 55081.2593055556 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041515 | Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | BREGMAN | JOEL | NULL | NULL | USA | 4 | AO4 | THE MISSING BARYONS IN GALAXY GROUPS | XIS | Y |
| NGC741 E | 29.459 | 5.6113 | 151.51137993 | -53.53548595 | 71.776 | 55054.8091087963 | 55055.0619675926 | 804053010 | 11377.8 | 10000 | 11377.8 | 11385.8 | 0 | 11393.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 8005.2 | 8005.2 | 21838 | 0 | PROCESSED | 57548.1250231482 | 55430 | 55064.1656134259 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041515 | Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | BREGMAN | JOEL | NULL | NULL | USA | 4 | AO4 | THE MISSING BARYONS IN GALAXY GROUPS | XIS | Y |
| NGC741MOSAICS_P1 | 29.0595 | 4.7357 | 151.53660126 | -54.49712787 | 71.6617 | 55052.4780671296 | 55052.6946643518 | 804054010 | 9322.2 | 10000 | 9330.2 | 9322.2 | 0 | 9330.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8003 | 8003 | 18671.9 | 1 | PROCESSED | 57548.0801967593 | 55451 | 55084.9869212963 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041515 | Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | BREGMAN | JOEL | NULL | NULL | USA | 4 | AO4 | THE MISSING BARYONS IN GALAXY GROUPS | XIS | Y |
| NGC741MOSAICS_P2 | 29.298 | 4.8125 | 151.84866444 | -54.32564909 | 71.7104 | 55052.6950925926 | 55052.9238310185 | 804054020 | 11428.9 | 10000 | 11452.9 | 11428.9 | 0 | 11452.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 6312.3 | 6312.3 | 19743.9 | 0 | PROCESSED | 57548.0884953704 | 55451 | 55085.0388425926 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041515 | Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | BREGMAN | JOEL | NULL | NULL | USA | 4 | AO4 | THE MISSING BARYONS IN GALAXY GROUPS | XIS | Y |
| NGC741MOSAICS_P3 | 28.9813 | 4.9712 | 151.24323938 | -54.31718683 | 71.7124 | 55052.9243981482 | 55053.1529976852 | 804054030 | 9401.3 | 10000 | 9409.3 | 9401.3 | 0 | 9415 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7068.3 | 7068.3 | 19720 | 0 | PROCESSED | 57548.0955671296 | 55451 | 55085.0001736111 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041515 | Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | BREGMAN | JOEL | NULL | NULL | USA | 4 | AO4 | THE MISSING BARYONS IN GALAXY GROUPS | XIS | Y |
| NGC741MOSAICS_P4 | 29.2193 | 5.0492 | 151.55342081 | -54.14565062 | 71.7599 | 55053.1534259259 | 55053.3759143518 | 804054040 | 10589 | 10000 | 10597 | 10589 | 0 | 10589 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9968.9 | 9968.9 | 19191.9 | 0 | PROCESSED | 57548.09625 | 55451 | 55084.9935763889 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041515 | Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | BREGMAN | JOEL | NULL | NULL | USA | 4 | AO4 | THE MISSING BARYONS IN GALAXY GROUPS | XIS | Y |
| NGC741S2_P1 | 29.0961 | 5.1589 | 151.28423043 | -54.09870829 | 71.6444 | 55053.3762962963 | 55053.6078587963 | 804055010 | 8601.6 | 10000 | 8617.6 | 8601.6 | 0 | 8625.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8748 | 8748 | 19984 | 1 | PROCESSED | 57548.1032291667 | 55465 | 55098.1609375 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041515 | Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | BREGMAN | JOEL | NULL | NULL | USA | 4 | AO4 | THE MISSING BARYONS IN GALAXY GROUPS | XIS | Y |
| NGC741S2_P2 | 29.0179 | 5.3952 | 150.99426375 | -53.91742537 | 71.6631 | 55053.608287037 | 55053.8425347222 | 804055020 | 10548.1 | 10000 | 10548.1 | 10548.1 | 0 | 10548.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 9548 | 9548 | 20229.9 | 0 | PROCESSED | 57548.1047800926 | 55465 | 55098.1704166667 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041515 | Galaxies have a baryon fraction only 1/3 of the cosmological value, so powerful galactic winds must have driven the gas out. In galaxy groups, the sites of most galaxies, the baryon fraction is also 1/3-1/2 of the cosmological value within half the virial radius, so the gas has been pushed further outward, probably from the heating of the same galactic superwinds. Studies with other telescopes do not go beyond half of the virial radius due to background limitations. With Suzaku, we can observe to the virial radius by using the low background XIS and choosing a galaxy group in a region of low Galactic XRB. We will discover whether the missing baryons reside in the outer parts of the group or if they have been expelled beyond the virial radius. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | BREGMAN | JOEL | NULL | NULL | USA | 4 | AO4 | THE MISSING BARYONS IN GALAXY GROUPS | XIS | Y |
| ABELL 426 E1 | 50.3027 | 41.5257 | 150.79331238 | -13.10366228 | 89.0025 | 55041.5144560185 | 55041.7141666667 | 804056010 | 9696 | 10000 | 9696 | 9696 | 0 | 9696 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7856 | 7856 | 17247.9 | 0 | PROCESSED | 57547.9587268518 | 55419 | 55050.256400463 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041522 | Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 4 | AO4 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY | XIS | Y |
| ABELL 426 E2 | 50.6767 | 41.5228 | 151.03351832 | -12.94989772 | 90.0008 | 55041.7150115741 | 55041.9654976852 | 804057010 | 12904.8 | 10000 | 12904.8 | 12904.8 | 0 | 12904.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12962 | 12962 | 21639.9 | 1 | PROCESSED | 57547.969849537 | 55419 | 55050.2440277778 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041522 | Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 4 | AO4 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY | XIS | Y |
| ABELL 426 E3 | 51.0503 | 41.5202 | 151.27232524 | -12.79481746 | 89.0003 | 55041.9666666667 | 55042.2904398148 | 804058010 | 11279.8 | 10000 | 11279.8 | 11551.8 | 0 | 11551.8 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 10720.1 | 10720.1 | 27966.1 | 0 | PROCESSED | 57547.981412037 | 55427 | 55060.7814236111 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041522 | Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 4 | AO4 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY | XIS | Y |
| ABELL 426 E4 | 51.4246 | 41.5162 | 151.51141512 | -12.63936589 | 90 | 55042.2912847222 | 55042.7466898148 | 804059010 | 21861.3 | 20000 | 21861.3 | 21861.3 | 0 | 21861.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 19707 | 19707 | 39336 | 0 | PROCESSED | 57547.9976736111 | 55427 | 55060.7938425926 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041522 | Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 4 | AO4 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY | XIS | Y |
| ABELL 426 E5 | 51.7975 | 41.5108 | 151.74947693 | -12.48443224 | 87.0002 | 55042.7485069444 | 55043.2932175926 | 804060010 | 21649 | 20000 | 21649 | 21942.3 | 0 | 21929 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 22139.1 | 22139.1 | 47048.1 | 0 | PROCESSED | 57548.0130208333 | 55427 | 55060.702349537 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041522 | Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 4 | AO4 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY | XIS | Y |
| ABELL 426 E6 | 52.1705 | 41.5044 | 151.98723888 | -12.32905015 | 86.9996 | 55043.2937847222 | 55043.9501736111 | 804061010 | 31943.1 | 30000 | 31943.1 | 31943.1 | 0 | 31943.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 29943.6 | 29943.6 | 56702 | 1 | PROCESSED | 57548.0213657407 | 55427 | 55060.7142013889 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041522 | Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 4 | AO4 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY | XIS | Y |
| ABELL 426 E7 | 52.5439 | 41.4965 | 152.22519414 | -12.17349332 | 85.5 | 55043.9514814815 | 55044.6843055556 | 804062010 | 30951.6 | 30000 | 30951.6 | 31221.6 | 0 | 31205.6 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 28544.9 | 28544.9 | 63314 | 0 | PROCESSED | 57548.0327083333 | 55427 | 55060.8353703704 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041522 | Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 4 | AO4 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY | XIS | Y |
| ABELL 426 N1 | 49.7797 | 41.7196 | 150.34867405 | -13.15794685 | 59.9997 | 55061.841099537 | 55062.1397453704 | 804063010 | 14727.6 | 10000 | 14735.6 | 14727.6 | 0 | 14737 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13172.4 | 13172.4 | 25791.9 | 0 | PROCESSED | 57548.2770833333 | 55441 | 55075.0515740741 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041522 | Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 4 | AO4 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY | XIS | Y |
| ABELL 426 N2 | 49.5875 | 41.9633 | 150.08864093 | -13.03246307 | 59.9939 | 55062.1402662037 | 55062.4716898148 | 804064010 | 13166 | 10000 | 13166 | 13166 | 0 | 13166 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9647 | 9647 | 28623.9 | 0 | PROCESSED | 57548.2750578704 | 55441 | 55075.0035416667 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041522 | Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 4 | AO4 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY | XIS | Y |
| ABELL 426 N3 | 49.4023 | 42.2033 | 149.83616068 | -12.90614214 | 59.9986 | 55062.4722106482 | 55062.7542708333 | 804065010 | 12249.8 | 10000 | 12249.8 | 12249.8 | 0 | 12249.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11858.2 | 11858.2 | 24361.9 | 0 | PROCESSED | 57548.2751157407 | 55441 | 55074.9931597222 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041522 | Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 4 | AO4 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY | XIS | Y |
| ABELL 426 N4 | 49.2103 | 42.4455 | 149.57911953 | -12.77962749 | 59.999 | 55062.754837963 | 55063.2460532407 | 804066010 | 25304.6 | 20000 | 25304.6 | 25306.5 | 0 | 25308.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21629.5 | 21629.5 | 42440 | 0 | PROCESSED | 57548.2829282407 | 55441 | 55075.0762384259 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041522 | Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 4 | AO4 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY | XIS | Y |
| ABELL 426 N5 | 49.0181 | 42.6863 | 149.32374876 | -12.65326208 | 59.9992 | 55063.2465740741 | 55063.8238310185 | 804067010 | 23607.4 | 20000 | 23631.4 | 23607.4 | 0 | 23639.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21143.5 | 21143.5 | 49865.9 | 1 | PROCESSED | 57548.2975115741 | 55441 | 55075.0347685185 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041522 | Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 4 | AO4 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY | XIS | Y |
| ABELL 426 N6 | 48.8242 | 42.9264 | 149.06870737 | -12.52705179 | 59.999 | 55063.8243055556 | 55064.6334837963 | 804068010 | 36526.5 | 30000 | 36534.5 | 36526.5 | 0 | 36542.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30884.3 | 30884.3 | 69911.9 | 0 | PROCESSED | 57548.3037731482 | 55441 | 55075.1362037037 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041522 | Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 4 | AO4 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY | XIS | Y |
| ABELL 426 N7 | 48.6285 | 43.1676 | 148.81295674 | -12.39950143 | 59.9993 | 55064.6340509259 | 55065.4329166667 | 804069010 | 36490.1 | 30000 | 36490.1 | 36510.1 | 0 | 36502.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30369.6 | 30369.6 | 69018 | 0 | PROCESSED | 57548.3120486111 | 55441 | 55075.0667708333 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041522 | Suzaku has enabled a breakthrough to be made in the study of the outer regions of galaxy clusters. For the first time, gas properties have been measured to beyond the virial radius. This is important for understanding properties such as the cluster gas and total mass, required for cosmological studies. It is also crucial for understanding how clusters link into their surrounding environments. How do large-scale filaments channel matter into clusters? Are there associated large-scale accretion shocks? This has been possible due to Suzaku's low orbit and the low background of its FI detectors, and the study of a particularly bright cluster. We propose to exploit Suzaku's unique capability to extend this result to the X-ray brightest cluster, and best target in the sky: the Perseus Cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 4 | AO4 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST CLUSTER IN THE SKY | XIS | Y |
| RCS0928+3646 | 142.0898 | 36.7798 | 186.98438508 | 46.37223207 | 116.6063 | 55148.3222800926 | 55149.1064699074 | 804080010 | 36516.7 | 30000 | 36532.7 | 36516.7 | 0 | 36532.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27058.4 | 27058.4 | 67743.9 | 1 | PROCESSED | 57549.3099652778 | 55546 | 55180.0365972222 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041525 | Understanding relationships between baryons in galaxy clusters and the underlying dark matter distributions is crucial for using clusters as cosmological probes. Recent work indicates massive low-Lx clusters at all redshifts, in conflict with self-similarity predictions. The only way to quantify these findings is to observe a cluster sample chosen independently of X-ray properties. We propose to study 14 clusters at 0.15<z<0.45, for which robust velocity dispersions are measured. We were awarded Chandra observations of 8 high-dispersion, low-z targets. Suzaku s superior throughput is required to probe the low-dispersion, high-z side of the distribution. We propose XIS observations of the remaining 6 targets, allowing us to rigorously assess baryon content in an unbiased sample of clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | HICKS | AMALIA | NULL | NULL | USA | 4 | AO4 | DECIPHERING CLUSTER OBSERVABLES: TRACING THE BARYONS IN CLUSTERS OF GALAXIES | XIS | Y |
| RCS1620+3046 | 245.0418 | 30.7908 | 50.54291734 | 44.60353773 | 131.519 | 55203.6116666667 | 55204.6008564815 | 804081010 | 43488.2 | 38000 | 43488.2 | 43488.2 | 0 | 43488.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16632.4 | 16632.4 | 85453.8 | 0 | PROCESSED | 57550.1212615741 | 55584 | 55218.2018402778 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041525 | Understanding relationships between baryons in galaxy clusters and the underlying dark matter distributions is crucial for using clusters as cosmological probes. Recent work indicates massive low-Lx clusters at all redshifts, in conflict with self-similarity predictions. The only way to quantify these findings is to observe a cluster sample chosen independently of X-ray properties. We propose to study 14 clusters at 0.15<z<0.45, for which robust velocity dispersions are measured. We were awarded Chandra observations of 8 high-dispersion, low-z targets. Suzaku s superior throughput is required to probe the low-dispersion, high-z side of the distribution. We propose XIS observations of the remaining 6 targets, allowing us to rigorously assess baryon content in an unbiased sample of clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | HICKS | AMALIA | NULL | NULL | USA | 4 | AO4 | DECIPHERING CLUSTER OBSERVABLES: TRACING THE BARYONS IN CLUSTERS OF GALAXIES | XIS | Y |
| A1795_FAR_NORTHEAST | 207.4803 | 26.8793 | 35.17669327 | 76.97815393 | 300.5693 | 55010.6105439815 | 55011.5556712963 | 804082010 | 40026.3 | 35000 | 40026.3 | 40026.3 | 0 | 40026.3 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57547.6967476852 | 55395 | 55026.4466087963 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041528 | The outer regions of clusters beyond 0.5 r200 contain a large amount of the dark matter, baryons and metals in the system, yet they are poorly understood. We propose to conduct a new test of cluster and structure formation by probing the distribution of dark matter and the thermodynamic history of the ICM in the outskirts of the cluster Abell 1795. Our previous Suzaku observations of Abell 1795 indicate deviations from hydrostatic equilibrium; we sample two disjoint regions beyond r500, detecting cluster emission in one but not the other (a difference of 5-sigma). With the proposed observations spanning r500-r200, we will obtain a more sensitive measurement of the azimuthally averaged temperature and density at this radius and search for variations over a wider range of azimuth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MILLER | ERIC | NULL | NULL | USA | 4 | AO4 | ABELL 1795 WITH SUZAKU: A NEW WINDOW ON CLUSTER FORMATION AND STRUCTURE | XIS | Y |
| A1795_FAR_SOUTHWEST | 206.9673 | 26.3143 | 32.43951308 | 77.37921169 | 300.5685 | 55011.5565162037 | 55012.4849537037 | 804083010 | 38357.3 | 35000 | 38357.3 | 38625.3 | 0 | 38633.3 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57598.4742013889 | 55395 | 55027.5898726852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041528 | The outer regions of clusters beyond 0.5 r200 contain a large amount of the dark matter, baryons and metals in the system, yet they are poorly understood. We propose to conduct a new test of cluster and structure formation by probing the distribution of dark matter and the thermodynamic history of the ICM in the outskirts of the cluster Abell 1795. Our previous Suzaku observations of Abell 1795 indicate deviations from hydrostatic equilibrium; we sample two disjoint regions beyond r500, detecting cluster emission in one but not the other (a difference of 5-sigma). With the proposed observations spanning r500-r200, we will obtain a more sensitive measurement of the azimuthally averaged temperature and density at this radius and search for variations over a wider range of azimuth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MILLER | ERIC | NULL | NULL | USA | 4 | AO4 | ABELL 1795 WITH SUZAKU: A NEW WINDOW ON CLUSTER FORMATION AND STRUCTURE | XIS | Y |
| A1795_FAR_WEST | 206.824 | 26.695 | 34.12189199 | 77.54661564 | 300.5663 | 55008.5840625 | 55009.4634143518 | 804084010 | 35476.3 | 35000 | 35484.3 | 35476.3 | 0 | 35484.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30346.6 | 30346.6 | 75937.8 | 1 | PROCESSED | 57547.7077662037 | 55395 | 55022.2936458333 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041528 | The outer regions of clusters beyond 0.5 r200 contain a large amount of the dark matter, baryons and metals in the system, yet they are poorly understood. We propose to conduct a new test of cluster and structure formation by probing the distribution of dark matter and the thermodynamic history of the ICM in the outskirts of the cluster Abell 1795. Our previous Suzaku observations of Abell 1795 indicate deviations from hydrostatic equilibrium; we sample two disjoint regions beyond r500, detecting cluster emission in one but not the other (a difference of 5-sigma). With the proposed observations spanning r500-r200, we will obtain a more sensitive measurement of the azimuthally averaged temperature and density at this radius and search for variations over a wider range of azimuth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MILLER | ERIC | NULL | NULL | USA | 4 | AO4 | ABELL 1795 WITH SUZAKU: A NEW WINDOW ON CLUSTER FORMATION AND STRUCTURE | XIS | Y |
| A1795_NEAR_WEST | 206.9975 | 26.5902 | 33.70837645 | 77.38236805 | 300.5681 | 55009.4637962963 | 55010.100162037 | 804085010 | 24266.4 | 20000 | 24266.4 | 24536.3 | 0 | 24520.3 | 5 | 2 | 0 | 2 | 1 | 0 | 0 | 9971.1 | 9971.1 | 22761.9 | 0 | PROCESSED | 57598.4788425926 | 55386 | 55020.3655555556 | 3.0.22.44 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 041528 | The outer regions of clusters beyond 0.5 r200 contain a large amount of the dark matter, baryons and metals in the system, yet they are poorly understood. We propose to conduct a new test of cluster and structure formation by probing the distribution of dark matter and the thermodynamic history of the ICM in the outskirts of the cluster Abell 1795. Our previous Suzaku observations of Abell 1795 indicate deviations from hydrostatic equilibrium; we sample two disjoint regions beyond r500, detecting cluster emission in one but not the other (a difference of 5-sigma). With the proposed observations spanning r500-r200, we will obtain a more sensitive measurement of the azimuthally averaged temperature and density at this radius and search for variations over a wider range of azimuth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MILLER | ERIC | NULL | NULL | USA | 4 | AO4 | ABELL 1795 WITH SUZAKU: A NEW WINDOW ON CLUSTER FORMATION AND STRUCTURE | XIS | Y |
| A76 EAST | 10.1332 | 6.8374 | 118.09579875 | -55.93191571 | 260.0024 | 55183.3444212963 | 55183.8752199074 | 804087010 | 23621 | 15000 | 23637 | 23621 | 0 | 23629 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 18640.1 | 18640.1 | 45855.9 | 0 | PROCESSED | 57549.8965393518 | 55575 | 55209.4624652778 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 042018 | In our flux limited survey of galaxy clusters in the ROSAT All-Sky Atlas we find that about 5 - 10 percent of the galaxy clusters have a diffuse, low X-ray surface brightness. These objects could possibly be explained as dynamically very young clusters, which have not yet formed a central core. Three such clusters in our XMM-Newton study of an unbiased sub-sample of 33 galaxy clusters, REXCESS, show suprisingly high entropies in their centers which does not readily support the early formation stage. To shed more light on the nature of these clusters we propose to observe two extremely low surface brightness clusters at low redshift, for which we also have detailed optical data. SUZAKU with its low background is ideally suited for this study. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | BOEHRINGER | HANS | NULL | NULL | EUR | 4 | AO4 | SHEDDING LIGHT ON THE NATURE OF EXTREMELY LOW SURFACE BRIGHTNESS CLUSTERS | XIS | Y |
| A76 WEST | 9.903 | 6.838 | 117.68922859 | -55.91332108 | 260 | 55183.8756481482 | 55184.3334953704 | 804088010 | 15116.4 | 15000 | 15124.4 | 15116.4 | 0 | 15132.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14206.6 | 14206.6 | 39547.9 | 0 | PROCESSED | 57549.8934722222 | 55575 | 55209.4668055556 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 042018 | In our flux limited survey of galaxy clusters in the ROSAT All-Sky Atlas we find that about 5 - 10 percent of the galaxy clusters have a diffuse, low X-ray surface brightness. These objects could possibly be explained as dynamically very young clusters, which have not yet formed a central core. Three such clusters in our XMM-Newton study of an unbiased sub-sample of 33 galaxy clusters, REXCESS, show suprisingly high entropies in their centers which does not readily support the early formation stage. To shed more light on the nature of these clusters we propose to observe two extremely low surface brightness clusters at low redshift, for which we also have detailed optical data. SUZAKU with its low background is ideally suited for this study. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | BOEHRINGER | HANS | NULL | NULL | EUR | 4 | AO4 | SHEDDING LIGHT ON THE NATURE OF EXTREMELY LOW SURFACE BRIGHTNESS CLUSTERS | XIS | Y |
| A3404 | 101.1266 | -54.2028 | 263.61200949 | -22.68018452 | 319.1401 | 54971.6181944444 | 54974.625162037 | 804089010 | 122092.9 | 121000 | 122100.9 | 122100.9 | 0 | 122092.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 106126.1 | 106126.1 | 259787.9 | 4 | PROCESSED | 57546.7060532407 | 55358 | 54992.6862615741 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 042025 | Robust and precise mass measurements for a large number of galaxy clusters represent the single most important step to prepare for dark energy cluster surveys to be performed, e.g., with eROSITA. Robustness and precision can best be achieved by a comparative and combined analysis of independent techniques. Here, we propose to use measurements from Suzaku, APEX-SZ, and wide-field optical telescopes to determine cluster masses up to the virial radius. X-ray, SZ, and gravitational lensing reduction and analyses will all be performed by experts at a single location. We demonstrate that we have selected the optimal targets for this study. Further, we show promising results from our Suzaku analysis of cluster outskirts, from our lensing pipeline, as well as from our combined SZ/X-ray method. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | REIPRICH | THOMAS | NULL | NULL | EUR | 4 | AO4 | COMBINED SUZAKU/APEX-SZ/LENSING MASS MEASUREMENTS OF THE GALAXY CLUSTERS A3404 AND A2537 | XIS | Y |
| A478 OFFSET A | 63.4449 | 10.2053 | 182.72704568 | -28.38203256 | 259.1008 | 55600.4642361111 | 55601.5488194444 | 805001010 | 44396.4 | 45000 | 44396.4 | 44396.4 | 0 | 44396.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35237.4 | 35237.4 | 93699.8 | 1 | PROCESSED | 57600.8998148148 | 55983 | 55617.4093981482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050008 | Clusters of galaxies are thought to form from accretion and merging of smaller systems among large-scale filaments. X-ray observations of cluster outskirts give us valuable information about the structure formation, gas heating and cooling, and metal enrichment of clusters of galaxies. Here, we propose deep surveys of a representative regular cluster, Abell 478 | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MATSUSHITA | KYOKO | FABIAN | ANDREW | JAP | 5 | AO5 | DISTRIBUTION OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF ABELL 478 UP TO VIRIAL RADIUS | XIS | Y |
| A478 OFFSET B | 63.3675 | 10.7352 | 182.20374123 | -28.1098658 | 260.0004 | 55601.549849537 | 55602.6897685185 | 805002010 | 45321.1 | 45000 | 45321.1 | 45321.1 | 0 | 45321.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34211.7 | 34211.7 | 98477.9 | 1 | PROCESSED | 57600.9178935185 | 55983 | 55617.4110763889 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050008 | Clusters of galaxies are thought to form from accretion and merging of smaller systems among large-scale filaments. X-ray observations of cluster outskirts give us valuable information about the structure formation, gas heating and cooling, and metal enrichment of clusters of galaxies. Here, we propose deep surveys of a representative regular cluster, Abell 478 | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MATSUSHITA | KYOKO | FABIAN | ANDREW | JAP | 5 | AO5 | DISTRIBUTION OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF ABELL 478 UP TO VIRIAL RADIUS | XIS | Y |
| A478 OFFSET C | 63.6328 | 10.5074 | 182.59008129 | -28.04907037 | 259.6787 | 55604.2488888889 | 55605.3522685185 | 805003010 | 47148.6 | 45000 | 47164.6 | 47148.6 | 0 | 47164.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39989.8 | 39989.8 | 95319.8 | 2 | PROCESSED | 57600.9430671296 | 55983 | 55617.4134490741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050008 | Clusters of galaxies are thought to form from accretion and merging of smaller systems among large-scale filaments. X-ray observations of cluster outskirts give us valuable information about the structure formation, gas heating and cooling, and metal enrichment of clusters of galaxies. Here, we propose deep surveys of a representative regular cluster, Abell 478 | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MATSUSHITA | KYOKO | FABIAN | ANDREW | JAP | 5 | AO5 | DISTRIBUTION OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF ABELL 478 UP TO VIRIAL RADIUS | XIS | Y |
| A478 OFFSET D | 63.1009 | 10.3754 | 182.33525373 | -28.5396849 | 259.0002 | 55612.7107986111 | 55613.7362731482 | 805004010 | 47106.6 | 45000 | 47106.6 | 47106.6 | 0 | 47106.6 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 42161 | 42161 | 88595.9 | 1 | PROCESSED | 57601.0027314815 | 56018 | 55649.2441203704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050008 | Clusters of galaxies are thought to form from accretion and merging of smaller systems among large-scale filaments. X-ray observations of cluster outskirts give us valuable information about the structure formation, gas heating and cooling, and metal enrichment of clusters of galaxies. Here, we propose deep surveys of a representative regular cluster, Abell 478 | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MATSUSHITA | KYOKO | FABIAN | ANDREW | JAP | 5 | AO5 | DISTRIBUTION OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF ABELL 478 UP TO VIRIAL RADIUS | XIS | Y |
| HYDRA A-1 | 139.3695 | -11.9475 | 242.69436566 | 25.06487811 | 95 | 55508.1097569444 | 55509.1800115741 | 805007010 | 42564.7 | 40000 | 42572.7 | 42564.7 | 0 | 42572.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35207.2 | 35207.2 | 92455.8 | 1 | PROCESSED | 57554.0434143518 | 55890 | 55524.1752430556 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050012 | X-ray observations of cluster outskirts give us valuable information about star-formation and metal-enrichment histories in clusters. Here, we propose surveys of two regular clusters of galaxies, Hydra A cluster | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MATSUSHITA | KYOKO | NULL | NULL | JAP | 5 | AO5 | DISTRIBUTION OF FE IN THE INTRACLUSTER MEDIUM UP TO 0.7R180 | XIS | Y |
| HYDRA A-2 | 139.672 | -11.9467 | 242.89463155 | 25.29884455 | 94.9986 | 55509.1804861111 | 55510.3008680556 | 805008010 | 41823.1 | 40000 | 41831.1 | 41823.1 | 0 | 41831.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34589.6 | 34589.6 | 96789.8 | 2 | PROCESSED | 57554.050162037 | 55890 | 55524.1344791667 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050012 | X-ray observations of cluster outskirts give us valuable information about star-formation and metal-enrichment histories in clusters. Here, we propose surveys of two regular clusters of galaxies, Hydra A cluster | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MATSUSHITA | KYOKO | NULL | NULL | JAP | 5 | AO5 | DISTRIBUTION OF FE IN THE INTRACLUSTER MEDIUM UP TO 0.7R180 | XIS | Y |
| A2744_SW | 3.5132 | -30.5508 | 8.03425743 | -81.13040471 | 233.4967 | 55540.2569791667 | 55542.2883217593 | 805015010 | 69776.3 | 65000 | 69776.3 | 69776.3 | 0 | 69776.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 59239.6 | 59239.6 | 175481.7 | 0 | PROCESSED | 57554.4226851852 | 55917 | 55551.0433101852 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050013 | We propose Suzaku observations of two merging clusters of galaxies, A2744 and the Bullet Cluster, to map the entropy variation out to the virial radius. Recent numerical simulations indicate that the entropy generation occurs through two-shock propagations, which is to be markedly seen in the cluster outskirts. On the other hand, little observational testing has been done for this regime of merging systems. We thus request three additional pointings to cover regions of large-scale filaments discovered in the optical. This study can only be achieved by Suzaku because of the lowest background level and excellent sensitivity, and will bring us new constraints on the thermodynamical history of the clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | OTA | NAOMI | NULL | NULL | JAP | 5 | AO5 | MAPPING THE GAS ENTROPY GENERATION IN A SEQUENCE OF MERGING CLUSTERS | XIS | Y |
| NGC 253 | 11.8603 | -25.2295 | 97.43086004 | -87.9001973 | 242.9983 | 55544.0947685185 | 55546.9460763889 | 805018010 | 101002.6 | 100000 | 101002.6 | 101002.6 | 0 | 101002.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 82668.9 | 82668.9 | 246335.9 | 1 | PROCESSED | 57554.5316203704 | 55975 | 55607.3286111111 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050015 | Suzaku observations of a hot halo of nearby, edge-on starburst galaxy, NGC 253 are proposed. The low background and high energy resolution of Suzaku XIS is the best tool to study the low surface brightness emission like halo emission around galaxies. In addition, we will eliminate the contamination from the the point source by XMM-Newton and the Galactic hot emission by a previous offset observation. The temperature and pressure structure and the chemical composition in the bright halo will reveal the physical condition and dynamics of the galaxy outflow to the intergalactic space. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | YAMASAKI | NORIKO | NULL | NULL | JAP | 5 | AO5 | SUZAKU OBSERVATION OF A BRIGHTEST STARBURST GALAXY NGC 253 | XIS | Y |
| A133_W | 15.4513 | -21.8877 | 147.70952455 | -84.25382555 | 44.9935 | 55354.0979513889 | 55355.296099537 | 805019010 | 50044.9 | 50000 | 50044.9 | 50044.9 | 0 | 50044.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41281.3 | 41281.3 | 103475.8 | 0 | PROCESSED | 57551.9211689815 | 55765 | 55393.3189467593 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050019 | We propose a mapping observation of Abell 133 to study temperature and metal abundance distributions up to ~0.8 times of virial radius. A good energy resolution, and a low and stable background level of the XIS instrument are crucial for this study. This data allow us to put constraints on the metal enrichment processes in the intergalactic space. We also investigate the magnetic field in the central region associated with the radio relic of Abell 133. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SATO | KOSUKE | NULL | NULL | JAP | 5 | AO5 | METALLICITY OF ABELL 133 FOR INVESTIGATING OF THE METAL ENRICHMENT PROCESS | XIS | Y |
| A133_N | 15.6732 | -21.6726 | 148.68503798 | -83.97324559 | 44.9987 | 55352.9000347222 | 55354.0974768518 | 805020010 | 50233.4 | 50000 | 50233.4 | 50233.4 | 0 | 50233.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 44176 | 44176 | 103416 | 1 | PROCESSED | 57551.8040740741 | 55765 | 55393.4422916667 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050019 | We propose a mapping observation of Abell 133 to study temperature and metal abundance distributions up to ~0.8 times of virial radius. A good energy resolution, and a low and stable background level of the XIS instrument are crucial for this study. This data allow us to put constraints on the metal enrichment processes in the intergalactic space. We also investigate the magnetic field in the central region associated with the radio relic of Abell 133. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SATO | KOSUKE | NULL | NULL | JAP | 5 | AO5 | METALLICITY OF ABELL 133 FOR INVESTIGATING OF THE METAL ENRICHMENT PROCESS | XIS | Y |
| A133_E | 15.9075 | -21.8935 | 151.49316881 | -84.07673835 | 44.9955 | 55356.7284953704 | 55358.0015393518 | 805021010 | 51552.3 | 50000 | 51564.1 | 51560.3 | 0 | 51552.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46254.7 | 46254.7 | 109984 | 1 | PROCESSED | 57551.9411458333 | 55737 | 55375.7548842593 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050019 | We propose a mapping observation of Abell 133 to study temperature and metal abundance distributions up to ~0.8 times of virial radius. A good energy resolution, and a low and stable background level of the XIS instrument are crucial for this study. This data allow us to put constraints on the metal enrichment processes in the intergalactic space. We also investigate the magnetic field in the central region associated with the radio relic of Abell 133. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SATO | KOSUKE | NULL | NULL | JAP | 5 | AO5 | METALLICITY OF ABELL 133 FOR INVESTIGATING OF THE METAL ENRICHMENT PROCESS | XIS | Y |
| A133_S | 15.6819 | -22.1029 | 150.58121257 | -84.35810156 | 44.9946 | 55355.2966203704 | 55356.727974537 | 805022010 | 51128 | 50000 | 51128 | 51128 | 0 | 51128 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42859.9 | 42859.9 | 123655.8 | 1 | PROCESSED | 57551.9312962963 | 55737 | 55370.2538310185 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050019 | We propose a mapping observation of Abell 133 to study temperature and metal abundance distributions up to ~0.8 times of virial radius. A good energy resolution, and a low and stable background level of the XIS instrument are crucial for this study. This data allow us to put constraints on the metal enrichment processes in the intergalactic space. We also investigate the magnetic field in the central region associated with the radio relic of Abell 133. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SATO | KOSUKE | NULL | NULL | JAP | 5 | AO5 | METALLICITY OF ABELL 133 FOR INVESTIGATING OF THE METAL ENRICHMENT PROCESS | XIS | Y |
| RXCJ0013.2-4905 | 3.3206 | -49.1017 | 318.93482177 | -66.82406097 | 263.5597 | 55565.2569328704 | 55565.4036689815 | 805023010 | 8432 | 10000 | 8432 | 8432 | 0 | 8432 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57600.5421875 | 56016 | 55627.5157638889 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050021 | We propose Suzaku observations of 5 X-ray luminous clusters of galaxies at z~0.4 that were discovered in the flux-limited REFLEX2 survey. Since some of the targets are to be observed in the AO4, we request an additional exposure for the remaining clusters to complete the program. With a short exposure time of 10 ks per cluster, we can determine the temperature of each cluster with 10% accuracy. This significantly improves the determination of the evolution of the luminosity-temperature relation, and will also have an impact on conducting precision cosmology with cluster observations. Thanks to the high sensitivity and low background, this study is carried out most efficiently by Suzaku. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | OTA | NAOMI | NULL | NULL | JAP | 5 | AO5 | LUMINOSITY-TEMPERATURE RELATION OF GALAXY CLUSTERS AT Z~0.4 | XIS | Y |
| RXCJ0411.2-4819 | 62.816 | -48.3247 | 255.63059498 | -46.16240445 | 110.1457 | 55461.4637384259 | 55461.7793865741 | 805024010 | 11364.9 | 10000 | 11364.9 | 11364.9 | 0 | 11364.9 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 10396 | 10396 | 27264 | 0 | PROCESSED | 57553.4942361111 | 55836 | 55470.1084606482 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050021 | We propose Suzaku observations of 5 X-ray luminous clusters of galaxies at z~0.4 that were discovered in the flux-limited REFLEX2 survey. Since some of the targets are to be observed in the AO4, we request an additional exposure for the remaining clusters to complete the program. With a short exposure time of 10 ks per cluster, we can determine the temperature of each cluster with 10% accuracy. This significantly improves the determination of the evolution of the luminosity-temperature relation, and will also have an impact on conducting precision cosmology with cluster observations. Thanks to the high sensitivity and low background, this study is carried out most efficiently by Suzaku. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | OTA | NAOMI | NULL | NULL | JAP | 5 | AO5 | LUMINOSITY-TEMPERATURE RELATION OF GALAXY CLUSTERS AT Z~0.4 | XIS | Y |
| NGC2841 | 140.401 | 51.0226 | 166.8971148 | 44.0746119 | 94.9994 | 55518.5609259259 | 55519.8036342593 | 805028010 | 85526.9 | 80000 | 85542.9 | 85526.9 | 0 | 85542.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 59375 | 59375 | 107351.8 | 1 | PROCESSED | 57554.1596180556 | 55898 | 55530.1645949074 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050028 | We propose a 80 ksec observation of an edge-on nearby spiral galaxy, NGC 2841 and the halo region. The expected temperature of the halo is ∼0.5 keV, and the characteristics enable Suzku to study the gas properties out to intergalactic space in a reliable way. We aim to obtain the temperature in the halo region within ∼5%, and hopefully an evidence for the gas dynamics not only between the disk and the halo region, but also between the halo and the intergalactic medium. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MITSUISHI | IKUYUKI | NULL | NULL | JAP | 5 | AO5 | STUDY OF X-RAY HALO OF AN EDGE-ON GALAXY NGC 2841 | XIS | Y |
| FILAMENT OF GALAXIES | 238.8797 | 27.1312 | 43.89595297 | 49.28386381 | 298.9982 | 55406.9857060185 | 55408.8592939815 | 805029010 | 73938.7 | 80000 | 73950.1 | 73944.7 | 0 | 73938.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 66404.5 | 66404.5 | 161855.7 | 1 | PROCESSED | 57552.8140972222 | 55791 | 55418.4520717593 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050032 | Warm Hot Intergalactic Medium (WHIM) is the most promising candidate for the cosmic missing baryons. Nevertheless, no concrete evidence of the presence of the WHIM has been unveiled yet. We propose a SUZAKU observation of a filament discovered through a systematic analysis of the SDSS galaxy catalogue. The observation toward a 10 Mpc long section of this filament aligned with the line of sight will provide the redshifted OVII and OVIII emission lines from the WHIM or much stronger constraint on the overdensity of the WHIM. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KAWAHARA | HAJIME | NULL | NULL | JAP | 5 | AO5 | SEARCHING FOR MISSING BARYONS ALONG A FILAMENT OF GALAXIES | XIS | Y |
| FILAMENT OF GALAXIES | 238.2847 | 27.6247 | 44.49442625 | 49.89393343 | 305.997 | 55408.8620833333 | 55410.6883101852 | 805030010 | 61770.3 | 80000 | 61770.3 | 61770.3 | 0 | 61770.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 55583.3 | 55583.3 | 157751.8 | 0 | PROCESSED | 57552.8205671296 | 55793 | 55427.2133449074 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050032 | Warm Hot Intergalactic Medium (WHIM) is the most promising candidate for the cosmic missing baryons. Nevertheless, no concrete evidence of the presence of the WHIM has been unveiled yet. We propose a SUZAKU observation of a filament discovered through a systematic analysis of the SDSS galaxy catalogue. The observation toward a 10 Mpc long section of this filament aligned with the line of sight will provide the redshifted OVII and OVIII emission lines from the WHIM or much stronger constraint on the overdensity of the WHIM. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KAWAHARA | HAJIME | NULL | NULL | JAP | 5 | AO5 | SEARCHING FOR MISSING BARYONS ALONG A FILAMENT OF GALAXIES | XIS | Y |
| HCG62_W | 192.9973 | -9.0837 | 303.16227701 | 53.78780217 | 292.9782 | 55405.1509953704 | 55406.9773611111 | 805031010 | 66947 | 60000 | 66955 | 66955 | 0 | 66947 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 52997.2 | 52997.2 | 157775.8 | 1 | PROCESSED | 57552.8094675926 | 55808 | 55441.3150925926 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050034 | We propose offset observations of groups of galaxies to study the metal distributions up to ~0.5 times of the virial radius. Metal mass to galaxy light ratios (MLRs) for groups are much smaller than those for clusters of galaxies. In order to solve the problem which is important to understand the chemical history of the universe, we need much information of the metal abundance and distributions to the outer region of the groups. Suzaku firstly enable us to measure the metals to such an outer region of groups. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | SATO | KOSUKE | NULL | NULL | JAP | 5 | AO5 | SEARCH FOR THE METAL DISTRIBUTIONS OF GROUPS OF GALAXIES TO 0.5 R180 | XIS | Y |
| A222/223 BRIDGE | 24.4438 | -12.9141 | 162.54430913 | -72.12239011 | 224.9995 | 55555.161099537 | 55557.4654861111 | 805035010 | 101214.9 | 100000 | 101284.3 | 101214.9 | 0 | 101284.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 88917.1 | 88917.1 | 199069.9 | 4 | PROCESSED | 57554.5537268518 | 55961 | 55595.1387847222 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050035 | We propose to observe the unusual X-ray bridge connecting the two clusters of galaxies Abell 222 and Abell 223 (z=0.21). XMM observation showed the temperature to be 0.9 keV, interpreted as due to WHIM. Suzaku will observe the temperature distribution over the bridge region, which will tell us the origin of the bridge to be either WHIM or merger onset. Merger process should indicate a characteristic temperature increase. Redshifted oxygen lines, if detected, will be the clear evidence of WHIM. Joint study with weak lensing analysis will show us spatial offset of the dark matter against baryons, helping us to constrain dark matter properties. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | HENMI | KAORI | NULL | NULL | JAP | 5 | AO5 | ORIGIN OF THE X-RAY BRIDGE CONNECTING THE CLUSTERS OF GALAXIES ABELL 222 AND ABELL 223 | XIS | Y |
| A3667_SE | 303.4605 | -57.0338 | 340.61636005 | -33.57067764 | 74.2668 | 55298.167349537 | 55299.2716435185 | 805036010 | 66287.2 | 50000 | 66295.2 | 66287.2 | 0 | 66287.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51249 | 51249 | 95397.8 | 1 | PROCESSED | 57551.2001967593 | 55675 | 55309.2055324074 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050039 | We propose an additional offset pointing of Abell 3667, one of the nearest, typical merging cluster. Using the 3 observations pointed along the merger axis on AO-1, we detected a possible super hot component around the cluster center (Nakazawa et al. 2009). To identify the existence and location of this component, we propose to observe the South-East Relic region, about 17 f south to the original southern-most pointing. This observation aims at verifying and locating the super hot component in this cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | NAKAZAWA | KAZUHIRO | NULL | NULL | JAP | 5 | AO5 | TRACING THE POSSIBLE SUPER-HOT COMPONENT IN THE MERGING CLUSTER ABELL 3667 | XIS | Y |
| ABELL1835 OFFSET1 | 210.441 | 2.9038 | 340.72312739 | 60.50812136 | 306.2398 | 55382.6847453704 | 55384.1217361111 | 805037010 | 49439.1 | 50000 | 49447.1 | 49439.1 | 0 | 49447.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43059.9 | 43059.9 | 124139.8 | 1 | PROCESSED | 57552.5235532407 | 55807 | 55441.2415856482 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050040 | We propose to conduct a joint X-ray, optical and weak-lensing analysis out to virial radius of a massive cluster A1835, using Japanese X-ray and optical instruments of Suzaku/XIS and Subaru/Suprime-Cam and SDSS archival data. A joint analysis will provide us with a comprehensive picture of the interplay among the intracluster medimum (ICM), member galaxies, large-scale structure and dark matter. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | OKABE | NOBUHIRO | NULL | NULL | JAP | 5 | AO5 | UNVEILING THE INTERPLAY AMONG ICM, LARGE-SCALE STRUCTURE AND DARK MATTER OUT TO VIRIAL RADIUS OF A1835 | XIS | Y |
| ABELL1835 OFFSET2 | 210.2863 | 2.6798 | 340.21334307 | 60.40388756 | 306.816 | 55384.1224884259 | 55385.4667939815 | 805038010 | 45603.6 | 50000 | 45603.6 | 45627.6 | 0 | 45611.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41282.6 | 41282.6 | 116129.8 | 0 | PROCESSED | 57552.5623611111 | 55801 | 55434.3364930556 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050040 | We propose to conduct a joint X-ray, optical and weak-lensing analysis out to virial radius of a massive cluster A1835, using Japanese X-ray and optical instruments of Suzaku/XIS and Subaru/Suprime-Cam and SDSS archival data. A joint analysis will provide us with a comprehensive picture of the interplay among the intracluster medimum (ICM), member galaxies, large-scale structure and dark matter. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | OKABE | NOBUHIRO | NULL | NULL | JAP | 5 | AO5 | UNVEILING THE INTERPLAY AMONG ICM, LARGE-SCALE STRUCTURE AND DARK MATTER OUT TO VIRIAL RADIUS OF A1835 | XIS | Y |
| ABELL1835 OFFSET3 | 210.0673 | 2.8311 | 340.00426802 | 60.64916276 | 306.4895 | 55385.4673611111 | 55386.9855555556 | 805039010 | 53697.1 | 50000 | 53720.1 | 53713.1 | 0 | 53697.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44837.7 | 44837.7 | 131159.8 | 3 | PROCESSED | 57552.5941087963 | 55779 | 55411.2395717593 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050040 | We propose to conduct a joint X-ray, optical and weak-lensing analysis out to virial radius of a massive cluster A1835, using Japanese X-ray and optical instruments of Suzaku/XIS and Subaru/Suprime-Cam and SDSS archival data. A joint analysis will provide us with a comprehensive picture of the interplay among the intracluster medimum (ICM), member galaxies, large-scale structure and dark matter. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | OKABE | NOBUHIRO | NULL | NULL | JAP | 5 | AO5 | UNVEILING THE INTERPLAY AMONG ICM, LARGE-SCALE STRUCTURE AND DARK MATTER OUT TO VIRIAL RADIUS OF A1835 | XIS | Y |
| ABELL1835 OFFSET4 | 210.2225 | 3.0556 | 340.51868842 | 60.75430015 | 304.9986 | 55390.9913194444 | 55392.4001736111 | 805040010 | 48818.5 | 50000 | 48826.5 | 48826.5 | 0 | 48818.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43963.1 | 43963.1 | 121683.9 | 4 | PROCESSED | 57552.6731828704 | 55793 | 55427.1333796296 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050040 | We propose to conduct a joint X-ray, optical and weak-lensing analysis out to virial radius of a massive cluster A1835, using Japanese X-ray and optical instruments of Suzaku/XIS and Subaru/Suprime-Cam and SDSS archival data. A joint analysis will provide us with a comprehensive picture of the interplay among the intracluster medimum (ICM), member galaxies, large-scale structure and dark matter. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | OKABE | NOBUHIRO | NULL | NULL | JAP | 5 | AO5 | UNVEILING THE INTERPLAY AMONG ICM, LARGE-SCALE STRUCTURE AND DARK MATTER OUT TO VIRIAL RADIUS OF A1835 | XIS | Y |
| NGC 4697 | 192.1513 | -5.7906 | 301.63561999 | 57.07401872 | 112.9816 | 55575.4840277778 | 55578.1905324074 | 805041010 | 102309.1 | 100000 | 102309.1 | 102309.1 | 0 | 102309.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 76047.1 | 76047.1 | 233816.1 | 1 | PROCESSED | 57600.7175462963 | 55962 | 55595.5109027778 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050080 | We propose the observation of the elliptical galaxy NGC 4697, whose temperature of interstellar medium is low, 0.3 keV. Hot X-ray emitting interstellar medium (ISM) carries important information about the history of star formation and evolution of galaxies. The different abundance pattern between S0 and elliptical galaxies was reported in recent study. To understand the formation process of early-type galaxies in more detail, it is very important to appreciate whether the different abundance pattern is due to morphology or temperature of system. The purpose of this proposal is to reveal the relation between abundance pattern, morphology, and temperature of system by investigating the abundance pattern of the elliptical galaxy, which has lower temperature. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KONAMI | SAORI | NULL | NULL | JAP | 5 | AO5 | MEASUREMENT OF ABUNDANCE PATTERN IN LOW TEMPARTURE ISM OF ELLIPTICAL GALAXY | XIS | Y |
| A2199 EAST OFFSET | 246.7666 | 40.2374 | 63.87682573 | 44.00920476 | 240.0015 | 55458.2941666667 | 55459.7155324074 | 805042010 | 58439.8 | 60000 | 58439.9 | 58439.8 | 0 | 58439.8 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 52507.6 | 52507.6 | 122791.9 | 1 | PROCESSED | 57553.4778935185 | 55836 | 55470.1049884259 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050081 | We propose to observe the virial radius region of the cluster of galaxies A2199 (z=0.0309) over the virial radius. This cluster lies in the Great Wall, and a cosmic filament runs from north to south. We aim to explore possible influence from the filament gives onto the formation process of the cluster, by comparing the hot-gas density and temperature around the virial radius in parallel and vertical directions to the filament. With the high sensitivity of XIS to faint extended emission, we expect to detect denser and hotter gas in the filement even outside the virial radius. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | AKAMATSU | HIROKI | NULL | NULL | JAP | 5 | AO5 | TEMPERATURE OVER THE VIRIAL RADIUS OF ABELL 2199, AND INFLUENCE OF THE LARGE-SCALE STRUCTURE. | XIS | Y |
| PERSEUS OFFSET-E | 49.943 | 41.2145 | 150.73941272 | -13.51227041 | 269.9995 | 55615.1921180556 | 55615.8335416667 | 805045010 | 27459.5 | 25000 | 27475.5 | 27459.5 | 0 | 27475.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25529.6 | 25529.6 | 55391.9 | 0 | PROCESSED | 57601.0240856482 | 55996 | 55628.1301157407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050093 | We propose to map the central region (R<20') of the Perseus cluster of galaxies. The cluster is the X-ray brightest one at z=0.02. This unique object along with good performance of the SUZAKU XIS and HXD provides the best quality, wide-band and spatially-resolved X-ray spectroscopy of the ICM. Using the data, we attempt to understand temperature structure, gas dynamics and metal distribution in the ICM. In particular, this observation should provide the most robust measurement of the ICM bulk motions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAMURA | TAKAYUKI | NULL | NULL | JAP | 5 | AO5 | MAPPING OF THE CENTRAL REGION OF THE PERSEUS CLUSTER | XIS | Y |
| PERSEUS OFFSET-F | 49.9431 | 41.79 | 150.41345254 | -13.03211324 | 269.9991 | 55609.6649305556 | 55610.152974537 | 805046010 | 20719.7 | 25000 | 20719.7 | 20719.7 | 0 | 20719.7 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 18813 | 18813 | 42159.9 | 0 | PROCESSED | 57600.9628125 | 55990 | 55621.2476967593 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050093 | We propose to map the central region (R<20') of the Perseus cluster of galaxies. The cluster is the X-ray brightest one at z=0.02. This unique object along with good performance of the SUZAKU XIS and HXD provides the best quality, wide-band and spatially-resolved X-ray spectroscopy of the ICM. Using the data, we attempt to understand temperature structure, gas dynamics and metal distribution in the ICM. In particular, this observation should provide the most robust measurement of the ICM bulk motions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAMURA | TAKAYUKI | NULL | NULL | JAP | 5 | AO5 | MAPPING OF THE CENTRAL REGION OF THE PERSEUS CLUSTER | XIS | Y |
| PERSEUS OFFSET-G | 50.3247 | 41.3807 | 150.89015689 | -13.2150361 | 270.0001 | 55596.3541550926 | 55596.8335648148 | 805047010 | 19676.8 | 25000 | 19700.8 | 19692.8 | 0 | 19676.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13192 | 13192 | 41411.9 | 1 | PROCESSED | 57600.8412731482 | 55979 | 55613.0840856482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050093 | We propose to map the central region (R<20') of the Perseus cluster of galaxies. The cluster is the X-ray brightest one at z=0.02. This unique object along with good performance of the SUZAKU XIS and HXD provides the best quality, wide-band and spatially-resolved X-ray spectroscopy of the ICM. Using the data, we attempt to understand temperature structure, gas dynamics and metal distribution in the ICM. In particular, this observation should provide the most robust measurement of the ICM bulk motions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAMURA | TAKAYUKI | NULL | NULL | JAP | 5 | AO5 | MAPPING OF THE CENTRAL REGION OF THE PERSEUS CLUSTER | XIS | Y |
| PERSEUS OFFSET-H | 50.3251 | 41.6598 | 150.73113668 | -12.9828544 | 270.0006 | 55595.9611458333 | 55596.3536805556 | 805048010 | 18241 | 25000 | 18249 | 18249 | 0 | 18241 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 14880 | 14880 | 33903.9 | 0 | PROCESSED | 57600.8294560185 | 55979 | 55610.233287037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050093 | We propose to map the central region (R<20') of the Perseus cluster of galaxies. The cluster is the X-ray brightest one at z=0.02. This unique object along with good performance of the SUZAKU XIS and HXD provides the best quality, wide-band and spatially-resolved X-ray spectroscopy of the ICM. Using the data, we attempt to understand temperature structure, gas dynamics and metal distribution in the ICM. In particular, this observation should provide the most robust measurement of the ICM bulk motions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAMURA | TAKAYUKI | NULL | NULL | JAP | 5 | AO5 | MAPPING OF THE CENTRAL REGION OF THE PERSEUS CLUSTER | XIS | Y |
| VIRGOHI 21 | 184.472 | 14.7597 | 268.97789082 | 75.3718003 | 123.3105 | 55535.5218518518 | 55537.7911574074 | 805054010 | 103191.5 | 100000 | 103399.5 | 103191.5 | 0 | 103399.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 81920.9 | 81920.9 | 196016.8 | 4 | PROCESSED | 57554.4175694444 | 55916 | 55550.3035185185 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 050114 | We propose a 100 ksec observation of "VIRGOHI 21" in the Virgo galaxy cluster. VIRGOHI 21 with no optical counterpart, is called a "dark galaxy" from the presence of velocity informed gas clouds with 21-cm observations somewhat like a disk galaxy. Origins are said to be traces of density fluctuation at cluster birth, or gas stripped from galaxies, but nothing clear is yet not introduced. Using the energy resolution of the XIS, we would like to explain the origin, deciding heavy element abundances of VIRGOHI 21. Extremely low abundance will give us the first "dark galaxy". Discovery of a "dark galaxy" with its information of prehistoric universe, will lead us to not just galaxy evolution, but also mighty mechanisms to understand cosmology, giving great impact to astrophysics itself. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | IIZUKA | RYO | NULL | NULL | JAP | 5 | AO5 | X-RAY SEARCH FOR A DARK GALAXY IN THE VIRGO CLUSTER | XIS | Y |
| A2204_FIELD_1 | 248.3552 | 5.4547 | 21.05505633 | 33.03914402 | 261.0004 | 55440.0008217593 | 55441.1467013889 | 805056010 | 40667.4 | 40000 | 40667.4 | 40667.4 | 0 | 40667.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37488 | 37488 | 98994.1 | 1 | PROCESSED | 57553.2764699074 | 55287 | 55456.099849537 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051115 | We propose observations of 5 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters, including those apparently discrepant with numerical simulations; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray mass determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MILLER | ERIC | NULL | NULL | USA | 5 | AO5 | THE OUTER LIMITS OF RICH CLUSTERS: SUZAKU OBSERVATIONS TO R200 | XIS | Y |
| A2204_FIELD_2 | 248.1003 | 5.3993 | 20.85022945 | 33.23419381 | 260.9996 | 55435.6212615741 | 55436.6744675926 | 805057010 | 39731.2 | 40000 | 39739.2 | 39731.2 | 0 | 39742.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35315.7 | 35315.7 | 90981.8 | 1 | PROCESSED | 57553.2244444445 | 55287 | 55449.2310416667 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051115 | We propose observations of 5 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters, including those apparently discrepant with numerical simulations; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray mass determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MILLER | ERIC | NULL | NULL | USA | 5 | AO5 | THE OUTER LIMITS OF RICH CLUSTERS: SUZAKU OBSERVATIONS TO R200 | XIS | Y |
| A2204_FIELD_3 | 248.3129 | 5.7152 | 21.30307351 | 33.20188623 | 261.0004 | 55436.6750347222 | 55437.758587963 | 805058010 | 36230.7 | 40000 | 36238.7 | 36230.7 | 0 | 36246.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 31656.4 | 31656.4 | 93601.8 | 2 | PROCESSED | 57553.2217361111 | 55287 | 55449.3168634259 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051115 | We propose observations of 5 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters, including those apparently discrepant with numerical simulations; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray mass determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MILLER | ERIC | NULL | NULL | USA | 5 | AO5 | THE OUTER LIMITS OF RICH CLUSTERS: SUZAKU OBSERVATIONS TO R200 | XIS | Y |
| A1413_FIELD_1 | 178.851 | 23.2234 | 226.97411288 | 76.74388731 | 303.0003 | 55345.0808333333 | 55346.139849537 | 805059010 | 40204.1 | 40000 | 40204.1 | 40204.1 | 0 | 40204.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34564 | 34564 | 91491.9 | 1 | PROCESSED | 57551.6776041667 | 55287 | 55365.2529513889 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051115 | We propose observations of 5 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters, including those apparently discrepant with numerical simulations; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray mass determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MILLER | ERIC | NULL | NULL | USA | 5 | AO5 | THE OUTER LIMITS OF RICH CLUSTERS: SUZAKU OBSERVATIONS TO R200 | XIS | Y |
| A1413_FIELD_2 | 178.6363 | 23.4218 | 225.87600909 | 76.62442609 | 303.0004 | 55346.1403240741 | 55347.1856828704 | 805060010 | 40951.2 | 40000 | 40959.2 | 40951.2 | 0 | 40951.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 34546.4 | 34546.4 | 90295.9 | 0 | PROCESSED | 57551.669837963 | 55287 | 55365.258912037 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051115 | We propose observations of 5 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters, including those apparently discrepant with numerical simulations; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray mass determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MILLER | ERIC | NULL | NULL | USA | 5 | AO5 | THE OUTER LIMITS OF RICH CLUSTERS: SUZAKU OBSERVATIONS TO R200 | XIS | Y |
| A1413_FIELD_3 | 179.0207 | 23.4251 | 226.37028623 | 76.95859752 | 302.9994 | 55347.1862037037 | 55348.2079050926 | 805061010 | 40922.5 | 40000 | 40922.5 | 40938.5 | 0 | 40930.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32994.4 | 32994.4 | 88257.8 | 0 | PROCESSED | 57553.3965856482 | 55287 | 55393.4280208333 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051115 | We propose observations of 5 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters, including those apparently discrepant with numerical simulations; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray mass determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MILLER | ERIC | NULL | NULL | USA | 5 | AO5 | THE OUTER LIMITS OF RICH CLUSTERS: SUZAKU OBSERVATIONS TO R200 | XIS | Y |
| A383_FIELD_1 | 42.1211 | -3.4616 | 177.79816007 | -53.37318565 | 60.9988 | 55388.2747337963 | 55389.1376388889 | 805062010 | 40391.5 | 40000 | 40415.5 | 40391.5 | 0 | 40415.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 35372.1 | 35372.1 | 74520 | 1 | PROCESSED | 57552.5965046296 | 55287 | 55411.2489467593 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051115 | We propose observations of 5 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters, including those apparently discrepant with numerical simulations; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray mass determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MILLER | ERIC | NULL | NULL | USA | 5 | AO5 | THE OUTER LIMITS OF RICH CLUSTERS: SUZAKU OBSERVATIONS TO R200 | XIS | Y |
| A383_FIELD_2 | 41.9447 | -3.4083 | 177.53047769 | -53.46482162 | 60.9996 | 55389.1380208333 | 55390.062662037 | 805063010 | 43341.5 | 40000 | 43357.5 | 43341.5 | 0 | 43357.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39258.9 | 39258.9 | 79874.9 | 0 | PROCESSED | 57552.6168055556 | 55287 | 55411.2445601852 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051115 | We propose observations of 5 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters, including those apparently discrepant with numerical simulations; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray mass determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MILLER | ERIC | NULL | NULL | USA | 5 | AO5 | THE OUTER LIMITS OF RICH CLUSTERS: SUZAKU OBSERVATIONS TO R200 | XIS | Y |
| A383_FIELD_3 | 41.9643 | -3.6473 | 177.84591826 | -53.61436812 | 60.9989 | 55390.0630902778 | 55390.9764930556 | 805064010 | 43196.8 | 40000 | 43196.8 | 43196.8 | 0 | 43196.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39592.9 | 39592.9 | 78895.9 | 1 | PROCESSED | 57552.6323842593 | 55287 | 55411.2967592593 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051115 | We propose observations of 5 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters, including those apparently discrepant with numerical simulations; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray mass determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MILLER | ERIC | NULL | NULL | USA | 5 | AO5 | THE OUTER LIMITS OF RICH CLUSTERS: SUZAKU OBSERVATIONS TO R200 | XIS | Y |
| RXCJ0605 | 91.4958 | -35.4837 | 241.98342334 | -24.04647163 | 309.0856 | 55321.4301041667 | 55322.221712963 | 805065010 | 40976.2 | 40000 | 40976.2 | 40976.2 | 0 | 40976.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35509.5 | 35509.5 | 68368.1 | 0 | PROCESSED | 57551.3998032407 | 55287 | 55341.4983217593 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051115 | We propose observations of 5 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters, including those apparently discrepant with numerical simulations; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray mass determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MILLER | ERIC | NULL | NULL | USA | 5 | AO5 | THE OUTER LIMITS OF RICH CLUSTERS: SUZAKU OBSERVATIONS TO R200 | XIS | Y |
| RXCJ0605 | 91.2587 | -35.3175 | 241.74700639 | -24.18215725 | 309.9853 | 55322.2226041667 | 55323.0307060185 | 805065020 | 40023.1 | 40000 | 40023.1 | 40023.1 | 0 | 40023.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 33176.2 | 33176.2 | 69789.9 | 0 | PROCESSED | 57551.4119097222 | 55287 | 55341.5093981482 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051115 | We propose observations of 5 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters, including those apparently discrepant with numerical simulations; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray mass determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MILLER | ERIC | NULL | NULL | USA | 5 | AO5 | THE OUTER LIMITS OF RICH CLUSTERS: SUZAKU OBSERVATIONS TO R200 | XIS | Y |
| RXCJ0605 | 91.7111 | -35.2772 | 241.82465393 | -23.81756849 | 309.9841 | 55323.0313194444 | 55323.8550810185 | 805065030 | 42423.9 | 40000 | 42431.9 | 42431.9 | 0 | 42423.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39146 | 39146 | 71161.9 | 0 | PROCESSED | 57551.4298263889 | 55287 | 55341.5040393518 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051115 | We propose observations of 5 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters, including those apparently discrepant with numerical simulations; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray mass determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MILLER | ERIC | NULL | NULL | USA | 5 | AO5 | THE OUTER LIMITS OF RICH CLUSTERS: SUZAKU OBSERVATIONS TO R200 | XIS | Y |
| RXCJ0605 | 91.4642 | -35.1179 | 241.59260677 | -23.96271915 | 309.9856 | 55323.8555555556 | 55324.6821412037 | 805065040 | 43694.6 | 40000 | 43694.6 | 43694.6 | 0 | 43710.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39332.1 | 39332.1 | 71413.9 | 0 | PROCESSED | 57551.4409837963 | 55287 | 55341.5146990741 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051115 | We propose observations of 5 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters, including those apparently discrepant with numerical simulations; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray mass determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MILLER | ERIC | NULL | NULL | USA | 5 | AO5 | THE OUTER LIMITS OF RICH CLUSTERS: SUZAKU OBSERVATIONS TO R200 | XIS | Y |
| NGC 720 OFFSET | 28.2673 | -13.4983 | 172.55217141 | -70.17529179 | 242.404 | 55560.2543634259 | 55565.2502083333 | 805069010 | 223966.3 | 150000 | 223972.2 | 223966.3 | 0 | 223972.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13357.1 | 13357.1 | 28363.9 | 0 | PROCESSED | 57600.5655671296 | 55994 | 55627.1378009259 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051503 | Models of galaxy formation suggest that as many as half the baryons may reside in an extended, hot halo. Detecting such a halo around a disk galaxy is, however, extremely challenging for current instrumentation. We propose instead to measure the baryon content of an isolated, X-ray bright elliptical galaxy (Mvir~6E12Msun), which provides the best opportunity to take a census of the baryons in a normal, galaxy-scale system. Currently little is known about the total baryon content of such objects, which are the likely end points of spiral galaxy merging. Combined with archival data, our offset pointing will enable the gas to be traced to ~0.75R500, comparable to what has been achieved for galaxy groups and clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | HUMPHREY | PHILIP | NULL | NULL | USA | 5 | AO5 | THE BARYON FRACTION OF AN ISOLATED ELLIPTICAL GALAXY | XIS | Y |
| NGC3402 OFF-CENTER | 162.4923 | -13.1954 | 262.91388856 | 40.05493452 | 124.5885 | 55557.4779513889 | 55558.1231134259 | 805070010 | 27866.4 | 30000 | 27874.4 | 27874.4 | 0 | 27866.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25029.4 | 25029.4 | 55740 | 1 | PROCESSED | 57554.5274421296 | 55961 | 55595.0278703704 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051512 | Using the composite data from dwarf galaxies to rich clusters, we find that the baryon fraction is mainly set by the system's potential well depth. The small scatter of baryon fractions as a function of the gravitational potential well depth indicates a universal baryon loss mechanism for these systems. However, the relation is most poorly constrained in the poor galaxy group regime below 1keV, where few individual measurements exists. Since most galaxies reside in these groups, it is also important to test whether the missing baryons from the galaxies are actually in these poor groups. We propose deep, off-center observations of two such groups, doubling the sample, to better delineate and understand the transition of the baryon loss from clusters to galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | DAI | XINYU | NULL | NULL | USA | 5 | AO5 | BARYON LOSS IN POOR GALAXY GROUPS: DISTINGUISHING PRE-HEATING AND FEEDBACK MODELS | XIS | Y |
| NGC3402 BACKGROUND | 161.6656 | -13.5535 | 262.34680831 | 39.29035073 | 110.091 | 55549.4379282407 | 55549.7563425926 | 805071010 | 12518.4 | 10000 | 12534.4 | 12518.4 | 0 | 12534.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11858.2 | 11858.2 | 27479.9 | 0 | PROCESSED | 57554.4605439815 | 55960 | 55593.0714699074 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051512 | Using the composite data from dwarf galaxies to rich clusters, we find that the baryon fraction is mainly set by the system's potential well depth. The small scatter of baryon fractions as a function of the gravitational potential well depth indicates a universal baryon loss mechanism for these systems. However, the relation is most poorly constrained in the poor galaxy group regime below 1keV, where few individual measurements exists. Since most galaxies reside in these groups, it is also important to test whether the missing baryons from the galaxies are actually in these poor groups. We propose deep, off-center observations of two such groups, doubling the sample, to better delineate and understand the transition of the baryon loss from clusters to galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | DAI | XINYU | NULL | NULL | USA | 5 | AO5 | BARYON LOSS IN POOR GALAXY GROUPS: DISTINGUISHING PRE-HEATING AND FEEDBACK MODELS | XIS | Y |
| NGC5129 OFF-CENTER1 | 201.3141 | 14.0346 | 335.68408417 | 74.71314923 | 124.7585 | 55548.0427314815 | 55548.7883101852 | 805072010 | 30251.2 | 30000 | 30251.2 | 30251.2 | 0 | 30251.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 24461.1 | 24461.1 | 64411.9 | 0 | PROCESSED | 57554.4566203704 | 55960 | 55592.9994444444 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051512 | Using the composite data from dwarf galaxies to rich clusters, we find that the baryon fraction is mainly set by the system's potential well depth. The small scatter of baryon fractions as a function of the gravitational potential well depth indicates a universal baryon loss mechanism for these systems. However, the relation is most poorly constrained in the poor galaxy group regime below 1keV, where few individual measurements exists. Since most galaxies reside in these groups, it is also important to test whether the missing baryons from the galaxies are actually in these poor groups. We propose deep, off-center observations of two such groups, doubling the sample, to better delineate and understand the transition of the baryon loss from clusters to galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | DAI | XINYU | NULL | NULL | USA | 5 | AO5 | BARYON LOSS IN POOR GALAXY GROUPS: DISTINGUISHING PRE-HEATING AND FEEDBACK MODELS | XIS | Y |
| NGC5129 OFF-CENTER2 | 201.1253 | 13.7341 | 334.52733324 | 74.54035563 | 127.8098 | 55548.7900810185 | 55549.42875 | 805073010 | 30765.1 | 30000 | 30781.1 | 30765.1 | 0 | 30781.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25247.5 | 25247.5 | 55168 | 0 | PROCESSED | 57554.4510416667 | 55960 | 55593.1036805556 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051512 | Using the composite data from dwarf galaxies to rich clusters, we find that the baryon fraction is mainly set by the system's potential well depth. The small scatter of baryon fractions as a function of the gravitational potential well depth indicates a universal baryon loss mechanism for these systems. However, the relation is most poorly constrained in the poor galaxy group regime below 1keV, where few individual measurements exists. Since most galaxies reside in these groups, it is also important to test whether the missing baryons from the galaxies are actually in these poor groups. We propose deep, off-center observations of two such groups, doubling the sample, to better delineate and understand the transition of the baryon loss from clusters to galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | DAI | XINYU | NULL | NULL | USA | 5 | AO5 | BARYON LOSS IN POOR GALAXY GROUPS: DISTINGUISHING PRE-HEATING AND FEEDBACK MODELS | XIS | Y |
| NGC5129 BACKGROUND | 201.7433 | 13.5725 | 336.16988197 | 74.1046924 | 116.4041 | 55547.7947106482 | 55548.0397106482 | 805074010 | 12276.7 | 10000 | 12276.7 | 12284.7 | 0 | 12292.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10781.1 | 10781.1 | 21160 | 0 | PROCESSED | 57554.4321180556 | 55960 | 55592.9616435185 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051512 | Using the composite data from dwarf galaxies to rich clusters, we find that the baryon fraction is mainly set by the system's potential well depth. The small scatter of baryon fractions as a function of the gravitational potential well depth indicates a universal baryon loss mechanism for these systems. However, the relation is most poorly constrained in the poor galaxy group regime below 1keV, where few individual measurements exists. Since most galaxies reside in these groups, it is also important to test whether the missing baryons from the galaxies are actually in these poor groups. We propose deep, off-center observations of two such groups, doubling the sample, to better delineate and understand the transition of the baryon loss from clusters to galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | DAI | XINYU | NULL | NULL | USA | 5 | AO5 | BARYON LOSS IN POOR GALAXY GROUPS: DISTINGUISHING PRE-HEATING AND FEEDBACK MODELS | XIS | Y |
| ESO3060170 | 85.0359 | -40.9515 | 246.54247084 | -30.30516606 | 320.0075 | 55327.721400463 | 55328.2676388889 | 805075010 | 31395.9 | 30000 | 31403.9 | 31395.9 | 0 | 31411.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28684 | 28684 | 47189.9 | 2 | PROCESSED | 57551.4609953704 | 55707 | 55341.5181365741 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051513 | We propose 30 and 80 ksec observations of the X-ray brightest fossil group, ESO 3060170. The target pointings will reach to 75% of the virial radius from the center of the galaxy, in order to determine the temperature and metal abundances of group gas at large radii. This will allow us to determine the radial profiles of the gaseous iron mass to stellar light ratio, the relative distributions of ejecta from SN Ia and SN II, the entropy, the total mass to light ratio, and the dark matter concentration for this fossil group. The energy resolution and low background of the XIS instrument are crucial for this study, which will help constrain the evolutional history of this fossil group and tell us how fossil groups relate to normal groups and clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | SU | YUANYUAN | NULL | NULL | USA | 5 | AO5 | HOW DO FOSSIL GROUPS OF GALAXIES DIFFER FROM NORMAL GROUPS? | XIS | Y |
| ESO3060170 OFFSET | 85.0343 | -41.2366 | 246.8664627 | -30.36071331 | 321.0164 | 55326.497025463 | 55327.7204166667 | 805076010 | 78678.2 | 80000 | 78678.2 | 78686.2 | 0 | 78686.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 69782.7 | 69782.7 | 105685.8 | 1 | PROCESSED | 57551.4828240741 | 55707 | 55341.5427893518 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051513 | We propose 30 and 80 ksec observations of the X-ray brightest fossil group, ESO 3060170. The target pointings will reach to 75% of the virial radius from the center of the galaxy, in order to determine the temperature and metal abundances of group gas at large radii. This will allow us to determine the radial profiles of the gaseous iron mass to stellar light ratio, the relative distributions of ejecta from SN Ia and SN II, the entropy, the total mass to light ratio, and the dark matter concentration for this fossil group. The energy resolution and low background of the XIS instrument are crucial for this study, which will help constrain the evolutional history of this fossil group and tell us how fossil groups relate to normal groups and clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | SU | YUANYUAN | NULL | NULL | USA | 5 | AO5 | HOW DO FOSSIL GROUPS OF GALAXIES DIFFER FROM NORMAL GROUPS? | XIS | Y |
| ABELL 115 | 13.9939 | 26.3802 | 124.19588168 | -36.48041221 | 44.0022 | 55401.606087963 | 55403.0529398148 | 805077010 | 66155.6 | 65000 | 66162.9 | 66155.6 | 0 | 66182.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 61829.8 | 61829.8 | 124968 | 2 | PROCESSED | 57552.6853472222 | 55780 | 55414.1298148148 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051521 | We propose central and offset pointed observations of the strongly merging ``double'' cluster A115 to study the properties of the intracluster gas at the virial radius. Ultimately, the results can be compared with results from both relaxed and other merging systems to determine the effects of mergers on the extended gas halos of clusters (e.g., departures from hydrostatic equilibrium, and the level of non-thermal pressure support). Additionally, we will verify the presence of hard X-ray emission between the subclusters, marginally detected in Chandra observations, accurately measure its temperature, and determine its origin by confirming it as hot thermal (shock heated gas) or non-thermal (shock or turbulent accelerated particles) emission. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | RANDALL | SCOTT | NULL | NULL | USA | 5 | AO5 | THE EXTENDED ATMOSPHERES OF STRONGLY MERGING GALAXY CLUSTERS | XIS | Y |
| ABELL 115 OFFSET | 13.7779 | 26.1853 | 123.95957255 | -36.67911837 | 45.0019 | 55399.3766666667 | 55401.6050115741 | 805078010 | 101806.5 | 100000 | 101806.5 | 101806.5 | 0 | 101806.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 91113.4 | 91113.4 | 192505.8 | 3 | PROCESSED | 57552.7084259259 | 55779 | 55413.4333449074 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051521 | We propose central and offset pointed observations of the strongly merging ``double'' cluster A115 to study the properties of the intracluster gas at the virial radius. Ultimately, the results can be compared with results from both relaxed and other merging systems to determine the effects of mergers on the extended gas halos of clusters (e.g., departures from hydrostatic equilibrium, and the level of non-thermal pressure support). Additionally, we will verify the presence of hard X-ray emission between the subclusters, marginally detected in Chandra observations, accurately measure its temperature, and determine its origin by confirming it as hot thermal (shock heated gas) or non-thermal (shock or turbulent accelerated particles) emission. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | RANDALL | SCOTT | NULL | NULL | USA | 5 | AO5 | THE EXTENDED ATMOSPHERES OF STRONGLY MERGING GALAXY CLUSTERS | XIS | Y |
| COMA CLUSTER | 194.3893 | 26.9261 | 24.84225016 | 88.62234831 | 316.4746 | 55348.2119907407 | 55350.6877199074 | 805079010 | 101780.5 | 100000 | 101780.5 | 101780.5 | 0 | 101780.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 77430.8 | 77430.8 | 213863.9 | 1 | PROCESSED | 57553.0722685185 | 55731 | 55365.54125 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051523 | The metal-enrichment mechanism of the hot gas in clusters of galaxies is still not completely understood, particularly at large (~virial) radii where current metallicity measurements are virtually non-existent. Yet a determinaton of elemental abundances of the gas at this radius will allow us to determine which enrichment mechanism (ram pressure stripping or galactic winds) is prevalant in the outskirts of clusters. We propose a 100 kec Suzaku observation of Coma at the virial radius to determine the Fe and S abundances at this location. The ratio of these two elements will allow us to discriminate among competing models for chemical enrichment. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | IRWIN | JIMMY | NULL | NULL | USA | 5 | AO5 | THE DETERMINATION OF THE METALLICITY OF COMA AT THE VIRIAL RADIUS | XIS | Y |
| MKW 4-OFFSET1 | 181.1304 | 2.2289 | 276.66004128 | 62.68282085 | 114.5816 | 55528.2862847222 | 55530.2501967593 | 805081010 | 79426.1 | 80000 | 79426.1 | 79426.1 | 0 | 79426.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 68211.2 | 68211.2 | 169667.9 | 2 | PROCESSED | 57554.312025463 | 55909 | 55543.4043402778 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051525 | We propose a set of two 19 arcmin offset observations for the galaxy groups MKW 4 to measure spatially resolved density, temperature and iron abundance out to r_{500}. These measurements are crucial for an accurate determination of the gas mass profile and gas fraction, for probing the entropy profile near the region where the accretion shocks start to be important, and for exploring the chemical enrichment at a spatial scale which retains information of early SNII and SNIa enrichment. Due to its brightness, regularity and low temperature, the object is an ideal candidate for an offset observation of its peripheral gas by Suzaku, making an excellent use of its low background and soft X-ray sensitivity. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | GASTALDELLO | FABIO | NULL | NULL | USA | 5 | AO5 | THE OUTSKIRTS OF MKW 4 | XIS | Y |
| MKW 4-OFFSET2 | 181.4291 | 1.9058 | 277.53009765 | 62.50090006 | 114.4199 | 55530.2508101852 | 55532.2286805556 | 805082010 | 82936.1 | 80000 | 82940.1 | 82936.1 | 0 | 82944.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70061.9 | 70061.9 | 170854.1 | 2 | PROCESSED | 57554.329525463 | 55910 | 55544.2869328704 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051525 | We propose a set of two 19 arcmin offset observations for the galaxy groups MKW 4 to measure spatially resolved density, temperature and iron abundance out to r_{500}. These measurements are crucial for an accurate determination of the gas mass profile and gas fraction, for probing the entropy profile near the region where the accretion shocks start to be important, and for exploring the chemical enrichment at a spatial scale which retains information of early SNII and SNIa enrichment. Due to its brightness, regularity and low temperature, the object is an ideal candidate for an offset observation of its peripheral gas by Suzaku, making an excellent use of its low background and soft X-ray sensitivity. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | GASTALDELLO | FABIO | NULL | NULL | USA | 5 | AO5 | THE OUTSKIRTS OF MKW 4 | XIS | Y |
| PKS 0745-191 | 117.0925 | -18.8008 | 236.11480248 | 3.4506494 | 113.9994 | 55514.1140625 | 55515.1105324074 | 805083010 | 37208.4 | 35000 | 37216.4 | 37208.4 | 0 | 37216.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 31522.8 | 31522.8 | 86087.9 | 1 | PROCESSED | 57554.0728703704 | 55903 | 55537.2095486111 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051526 | Suzaku has enabled us to make the first measurement of the temperature profile beyond the virial radius of any cluster. The gas in the outskirts of galaxy clusters presents information of astrophysical and cosmological importance. Measurements at the virial radius, where the dominant gas behavior switches from infall to equilibrium, can improve cluster mass estimates. Temperature and entropy profiles in the outskirts describe the accretion history and energy balance of clusters, near where they must match the background properties of the Universe. But these observations are just beginning. How do clusters grow? Are there large scale accretion shocks? To what extent are clusters relaxed? Here we propose to continue our study of PKS 0745-191 using Suzaku's unique capability to map this area. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | GEORGE | MATTHEW | NULL | NULL | USA | 5 | AO5 | BEYOND THE VIRIAL RADIUS OF PKS 0745-191, THE BRIGHTEST CLUSTER PAST Z=0.1 | XIS | Y |
| PKS 0745-191 | 116.7033 | -18.9048 | 236.01965558 | 3.07990407 | 294.0011 | 55315.865462963 | 55316.6418518518 | 805084010 | 34835.6 | 35000 | 34835.6 | 34835.6 | 0 | 34835.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 29506.7 | 29506.7 | 67075.9 | 1 | PROCESSED | 57551.3211458333 | 55696 | 55330.1469675926 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051526 | Suzaku has enabled us to make the first measurement of the temperature profile beyond the virial radius of any cluster. The gas in the outskirts of galaxy clusters presents information of astrophysical and cosmological importance. Measurements at the virial radius, where the dominant gas behavior switches from infall to equilibrium, can improve cluster mass estimates. Temperature and entropy profiles in the outskirts describe the accretion history and energy balance of clusters, near where they must match the background properties of the Universe. But these observations are just beginning. How do clusters grow? Are there large scale accretion shocks? To what extent are clusters relaxed? Here we propose to continue our study of PKS 0745-191 using Suzaku's unique capability to map this area. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | GEORGE | MATTHEW | NULL | NULL | USA | 5 | AO5 | BEYOND THE VIRIAL RADIUS OF PKS 0745-191, THE BRIGHTEST CLUSTER PAST Z=0.1 | XIS | Y |
| PKS 0745-191 | 116.3632 | -19.0871 | 236.01662317 | 2.71025988 | 294.0001 | 55316.6424189815 | 55317.3675231482 | 805085010 | 34999.9 | 35000 | 34999.9 | 34999.9 | 0 | 34999.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32780.4 | 32780.4 | 62641.9 | 2 | PROCESSED | 57551.3324074074 | 55696 | 55330.1114236111 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051526 | Suzaku has enabled us to make the first measurement of the temperature profile beyond the virial radius of any cluster. The gas in the outskirts of galaxy clusters presents information of astrophysical and cosmological importance. Measurements at the virial radius, where the dominant gas behavior switches from infall to equilibrium, can improve cluster mass estimates. Temperature and entropy profiles in the outskirts describe the accretion history and energy balance of clusters, near where they must match the background properties of the Universe. But these observations are just beginning. How do clusters grow? Are there large scale accretion shocks? To what extent are clusters relaxed? Here we propose to continue our study of PKS 0745-191 using Suzaku's unique capability to map this area. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | GEORGE | MATTHEW | NULL | NULL | USA | 5 | AO5 | BEYOND THE VIRIAL RADIUS OF PKS 0745-191, THE BRIGHTEST CLUSTER PAST Z=0.1 | XIS | Y |
| PKS 0745-191 | 116.4685 | -19.4632 | 236.39245911 | 2.60836561 | 294.0003 | 55317.3681365741 | 55318.1516087963 | 805086010 | 31729.9 | 35000 | 31729.9 | 31729.9 | 0 | 31729.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27646 | 27646 | 67682 | 0 | PROCESSED | 57551.3418981482 | 55696 | 55330.121087963 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051526 | Suzaku has enabled us to make the first measurement of the temperature profile beyond the virial radius of any cluster. The gas in the outskirts of galaxy clusters presents information of astrophysical and cosmological importance. Measurements at the virial radius, where the dominant gas behavior switches from infall to equilibrium, can improve cluster mass estimates. Temperature and entropy profiles in the outskirts describe the accretion history and energy balance of clusters, near where they must match the background properties of the Universe. But these observations are just beginning. How do clusters grow? Are there large scale accretion shocks? To what extent are clusters relaxed? Here we propose to continue our study of PKS 0745-191 using Suzaku's unique capability to map this area. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | GEORGE | MATTHEW | NULL | NULL | USA | 5 | AO5 | BEYOND THE VIRIAL RADIUS OF PKS 0745-191, THE BRIGHTEST CLUSTER PAST Z=0.1 | XIS | Y |
| PKS 0745-191 | 116.6522 | -19.7838 | 236.7569882 | 2.59757333 | 114.0013 | 55515.1115162037 | 55516.1335416667 | 805087010 | 37928.6 | 35000 | 37952.6 | 37944.6 | 0 | 37928.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32103.7 | 32103.7 | 88285.8 | 2 | PROCESSED | 57554.1054976852 | 55895 | 55526.1606018518 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051526 | Suzaku has enabled us to make the first measurement of the temperature profile beyond the virial radius of any cluster. The gas in the outskirts of galaxy clusters presents information of astrophysical and cosmological importance. Measurements at the virial radius, where the dominant gas behavior switches from infall to equilibrium, can improve cluster mass estimates. Temperature and entropy profiles in the outskirts describe the accretion history and energy balance of clusters, near where they must match the background properties of the Universe. But these observations are just beginning. How do clusters grow? Are there large scale accretion shocks? To what extent are clusters relaxed? Here we propose to continue our study of PKS 0745-191 using Suzaku's unique capability to map this area. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | GEORGE | MATTHEW | NULL | NULL | USA | 5 | AO5 | BEYOND THE VIRIAL RADIUS OF PKS 0745-191, THE BRIGHTEST CLUSTER PAST Z=0.1 | XIS | Y |
| RCS2343-3517 | 355.9933 | -35.2927 | 359.21699124 | -73.45928386 | 237.6557 | 55523.8239930556 | 55525.0418171296 | 805088010 | 48316.7 | 61000 | 48316.7 | 48316.7 | 0 | 48316.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40145.4 | 40145.4 | 105185.9 | 1 | PROCESSED | 57554.2088078704 | 55903 | 55537.0179861111 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051527 | Understanding relationships between baryons in galaxy clusters and underlying dark matter distributions is crucial for using clusters as cosmological probes. Recent work indicates massive low-Lx clusters at all redshifts, in conflict with self-similarity predictions. The only way to quantify these findings is to observe a sample chosen independently of X-ray properties. We propose to study 13 clusters at 0.15<z<0.45, for which robust velocity dispersions are measured. We were awarded Suzaku/Chandra observations of 11 high-dispersion, low-z targets. Suzaku's superior throughput is required to complete the low-dispersion, high-z side of the distribution. We propose XIS observations of the remaining 2 targets, allowing us to rigorously assess baryon content in an unbiased sample of clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | HICKS | AMALIA | NULL | NULL | USA | 5 | AO5 | DECIPHERING CLUSTER OBSERVABLES: TRACING THE BARYONS IN CLUSTERS OF GALAXIES | XIS | Y |
| RCS2318-0024 | 349.6301 | -0.4169 | 79.21894267 | -55.19865221 | 248.0438 | 55526.0185648148 | 55527.293912037 | 805089010 | 50305 | 73000 | 50329 | 50305 | 0 | 50337 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45634.6 | 45634.6 | 110173.8 | 0 | PROCESSED | 57554.2552893518 | 55903 | 55537.0791898148 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 051527 | Understanding relationships between baryons in galaxy clusters and underlying dark matter distributions is crucial for using clusters as cosmological probes. Recent work indicates massive low-Lx clusters at all redshifts, in conflict with self-similarity predictions. The only way to quantify these findings is to observe a sample chosen independently of X-ray properties. We propose to study 13 clusters at 0.15<z<0.45, for which robust velocity dispersions are measured. We were awarded Suzaku/Chandra observations of 11 high-dispersion, low-z targets. Suzaku's superior throughput is required to complete the low-dispersion, high-z side of the distribution. We propose XIS observations of the remaining 2 targets, allowing us to rigorously assess baryon content in an unbiased sample of clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | HICKS | AMALIA | NULL | NULL | USA | 5 | AO5 | DECIPHERING CLUSTER OBSERVABLES: TRACING THE BARYONS IN CLUSTERS OF GALAXIES | XIS | Y |
| ABELL 2537 | 347.0895 | -2.1864 | 73.83613509 | -54.91382092 | 56.4647 | 55368.5295486111 | 55371.9946875 | 805090010 | 124823.2 | 129000 | 124847.2 | 124823.2 | 0 | 124847.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 108390.8 | 108390.8 | 281217.6 | 1 | PROCESSED | 57552.4996412037 | 55772 | 55403.4592361111 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 052007 | Robust and precise mass measurements for a large number of galaxy clusters represent the single most important step to prepare for dark energy cluster surveys to be performed, e.g., with eROSITA. Robustness and precision can best be achieved by a comparative and combined analysis of independent techniques. Here, we propose to use measurements from Suzaku, APEX-SZ, and wide-field optical telescopes to determine cluster masses up to the virial radius. X-ray, SZ, and gravitational lensing reductions and analyses will all be performed by experts at a single location. We demonstrate that we have selected the optimal targets for this study. Further, we show promising results from our Suzaku analysis of cluster outskirts, from our lensing pipeline, as well as from our combined SZ/X-ray method. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | REIPRICH | THOMAS | NULL | NULL | EUR | 5 | AO5 | COMBINED SUZAKU/APEX-SZ/LENSING MASS MEASUREMENTS OF THE GALAXY CLUSTER A2537 | XIS | Y |
| A1914_OFFSET1 | 216.5507 | 38.0175 | 67.63121502 | 67.35438204 | 324.9943 | 55362.5248148148 | 55363.4724768518 | 805091010 | 32203.4 | 40000 | 32203.4 | 32203.4 | 0 | 32203.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27508.6 | 27508.6 | 81876 | 1 | PROCESSED | 57552.3572569445 | 55766 | 55399.2609722222 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 053087 | We propose four pointing observations of the merging cluster Abell 1914 with exposure of 160 ks (40 ks each). We measure temperature, electron density, and entropy distributions of the ICM out to the virial radius to study the merging history of this cluster. We determine the supra-thermal component expected by the merger with a wide-band spectroscopy using XIS and HXD-PIN, and quantify heat input to the ICM by a joint analysis with weak lensing data of Subaru telescope. Then, we aim to estimate the energy ratio of the heat input to total delivered energy through the merger. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KAWAHARADA | MADOKA | MILLER | ERIC | JUS | 5 | AO5 | THERMODYNAMICS OF INTRACLUSTER MEDIUM IN THE MERGING CLUSTER ABELL 1914 | XIS | Y |
| A1914_OFFSET1 | 216.5784 | 38.0421 | 67.66951456 | 67.3249966 | 134.001 | 55565.4188194445 | 55565.728599537 | 805091020 | 11393 | 10000 | 11401 | 11393 | 0 | 11401 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11376.3 | 11376.3 | 25497.9 | 0 | PROCESSED | 57600.5573263889 | 55995 | 55627.1165625 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 053087 | We propose four pointing observations of the merging cluster Abell 1914 with exposure of 160 ks (40 ks each). We measure temperature, electron density, and entropy distributions of the ICM out to the virial radius to study the merging history of this cluster. We determine the supra-thermal component expected by the merger with a wide-band spectroscopy using XIS and HXD-PIN, and quantify heat input to the ICM by a joint analysis with weak lensing data of Subaru telescope. Then, we aim to estimate the energy ratio of the heat input to total delivered energy through the merger. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KAWAHARADA | MADOKA | NAGINO | RYO | JUS | 5 | AO5 | THERMODYNAMICS OF INTRACLUSTER MEDIUM IN THE MERGING CLUSTER ABELL 1914 | XIS | Y |
| A1914_OFFSET2 | 216.7383 | 37.763 | 66.87630822 | 67.3091462 | 329.9943 | 55363.4747569444 | 55364.3800115741 | 805092010 | 28546.2 | 40000 | 28554.2 | 28554.2 | 0 | 28546.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25834.3 | 25834.3 | 78204 | 0 | PROCESSED | 57552.3515856482 | 55766 | 55399.3275231482 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 053087 | We propose four pointing observations of the merging cluster Abell 1914 with exposure of 160 ks (40 ks each). We measure temperature, electron density, and entropy distributions of the ICM out to the virial radius to study the merging history of this cluster. We determine the supra-thermal component expected by the merger with a wide-band spectroscopy using XIS and HXD-PIN, and quantify heat input to the ICM by a joint analysis with weak lensing data of Subaru telescope. Then, we aim to estimate the energy ratio of the heat input to total delivered energy through the merger. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KAWAHARADA | MADOKA | MILLER | ERIC | JUS | 5 | AO5 | THERMODYNAMICS OF INTRACLUSTER MEDIUM IN THE MERGING CLUSTER ABELL 1914 | XIS | Y |
| A1914_OFFSET2 | 216.77 | 37.7885 | 66.91478771 | 67.27662817 | 134.0016 | 55565.7291203704 | 55566.0216550926 | 805092020 | 17091.2 | 12000 | 17099.2 | 17091.2 | 0 | 17107.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13205.8 | 13205.8 | 25271.9 | 0 | PROCESSED | 57600.5511689815 | 56037 | 55670.1137384259 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 053087 | We propose four pointing observations of the merging cluster Abell 1914 with exposure of 160 ks (40 ks each). We measure temperature, electron density, and entropy distributions of the ICM out to the virial radius to study the merging history of this cluster. We determine the supra-thermal component expected by the merger with a wide-band spectroscopy using XIS and HXD-PIN, and quantify heat input to the ICM by a joint analysis with weak lensing data of Subaru telescope. Then, we aim to estimate the energy ratio of the heat input to total delivered energy through the merger. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KAWAHARADA | MADOKA | MILLER | ERIC | JUS | 5 | AO5 | THERMODYNAMICS OF INTRACLUSTER MEDIUM IN THE MERGING CLUSTER ABELL 1914 | XIS | Y |
| A1914_OFFSET3 | 216.2252 | 37.8719 | 67.5271644 | 67.6467927 | 330.9949 | 55364.3811805556 | 55365.2953587963 | 805093010 | 28506.6 | 40000 | 28506.6 | 28506.6 | 0 | 28506.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26381.3 | 26381.3 | 78967.9 | 1 | PROCESSED | 57552.3531018518 | 55769 | 55400.3084375 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 053087 | We propose four pointing observations of the merging cluster Abell 1914 with exposure of 160 ks (40 ks each). We measure temperature, electron density, and entropy distributions of the ICM out to the virial radius to study the merging history of this cluster. We determine the supra-thermal component expected by the merger with a wide-band spectroscopy using XIS and HXD-PIN, and quantify heat input to the ICM by a joint analysis with weak lensing data of Subaru telescope. Then, we aim to estimate the energy ratio of the heat input to total delivered energy through the merger. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KAWAHARADA | MADOKA | MILLER | ERIC | JUS | 5 | AO5 | THERMODYNAMICS OF INTRACLUSTER MEDIUM IN THE MERGING CLUSTER ABELL 1914 | XIS | Y |
| A1914_OFFSET3 | 216.2544 | 37.895 | 67.56094175 | 67.61680074 | 134.0009 | 55566.0223148148 | 55566.4306365741 | 805093020 | 12829.4 | 12000 | 12829.4 | 12829.4 | 0 | 12829.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13721 | 13721 | 35269.9 | 0 | PROCESSED | 57600.553599537 | 55995 | 55627.1328009259 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 053087 | We propose four pointing observations of the merging cluster Abell 1914 with exposure of 160 ks (40 ks each). We measure temperature, electron density, and entropy distributions of the ICM out to the virial radius to study the merging history of this cluster. We determine the supra-thermal component expected by the merger with a wide-band spectroscopy using XIS and HXD-PIN, and quantify heat input to the ICM by a joint analysis with weak lensing data of Subaru telescope. Then, we aim to estimate the energy ratio of the heat input to total delivered energy through the merger. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KAWAHARADA | MADOKA | MILLER | ERIC | JUS | 5 | AO5 | THERMODYNAMICS OF INTRACLUSTER MEDIUM IN THE MERGING CLUSTER ABELL 1914 | XIS | Y |
| A1914_OFFSET4 | 216.4138 | 37.6152 | 66.75628519 | 67.60183749 | 330.9949 | 55365.2958333333 | 55366.115462963 | 805094010 | 27290.4 | 40000 | 27290.4 | 27300.1 | 0 | 27294.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25420.3 | 25420.3 | 70816 | 0 | PROCESSED | 57552.407037037 | 55769 | 55403.4672106482 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 053087 | We propose four pointing observations of the merging cluster Abell 1914 with exposure of 160 ks (40 ks each). We measure temperature, electron density, and entropy distributions of the ICM out to the virial radius to study the merging history of this cluster. We determine the supra-thermal component expected by the merger with a wide-band spectroscopy using XIS and HXD-PIN, and quantify heat input to the ICM by a joint analysis with weak lensing data of Subaru telescope. Then, we aim to estimate the energy ratio of the heat input to total delivered energy through the merger. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KAWAHARADA | MADOKA | MILLER | ERIC | JUS | 5 | AO5 | THERMODYNAMICS OF INTRACLUSTER MEDIUM IN THE MERGING CLUSTER ABELL 1914 | XIS | Y |
| A1914_OFFSET4 | 216.4424 | 37.6372 | 66.78881215 | 67.57279807 | 134.0011 | 55566.4311574074 | 55566.8258912037 | 805094020 | 17353.1 | 12000 | 17353.1 | 17361.1 | 0 | 17369.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16060.6 | 16060.6 | 34100 | 0 | PROCESSED | 57600.564375 | 55995 | 55627.1583333333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 053087 | We propose four pointing observations of the merging cluster Abell 1914 with exposure of 160 ks (40 ks each). We measure temperature, electron density, and entropy distributions of the ICM out to the virial radius to study the merging history of this cluster. We determine the supra-thermal component expected by the merger with a wide-band spectroscopy using XIS and HXD-PIN, and quantify heat input to the ICM by a joint analysis with weak lensing data of Subaru telescope. Then, we aim to estimate the energy ratio of the heat input to total delivered energy through the merger. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KAWAHARADA | MADOKA | MILLER | ERIC | JUS | 5 | AO5 | THERMODYNAMICS OF INTRACLUSTER MEDIUM IN THE MERGING CLUSTER ABELL 1914 | XIS | Y |
| NGC 1332 | 51.5732 | -21.333 | 212.17958034 | -54.36451308 | 243.6482 | 55581.2509027778 | 55584.0883333333 | 805095010 | 101423 | 100000 | 101423 | 101423 | 0 | 101423 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 89968.3 | 89968.3 | 245125.9 | 2 | PROCESSED | 57600.7603935185 | 55965 | 55599.216724537 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 054502 | Recent observations of relaxed galaxy groups have revealed ubiquitous abundance gradients. The broad peaks of Fe abundance indicate (turbulent) diffusion of metals possibly driven by AGN feedback. Exploiting the low background and good sensitivity of Suzaku XIS, we have found similar gradients in three lower mass (virial mass 5-10E12 Msun) elliptical galaxies, which has important implications for models of feedback and chemical enrichment. We propose to observe another two carefully chosen galaxies, thus starting to build a sample for determining the frequency and properties of such abundance gradients in early-type galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | HUMPHREY | PHILIP | NAGINO | RYO | USJ | 5 | AO5 | ABUNDANCE GRADIENTS IN EARLY-TYPE GALAXIES | XIS | Y |
| ABELL 426 S1 | 49.8666 | 41.2611 | 150.66369426 | -13.50507569 | 88 | 55424.9920601852 | 55425.2995138889 | 805096010 | 8434.3 | 10000 | 8442.3 | 8450.3 | 0 | 8434.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 7861.1 | 7861.1 | 26549.9 | 0 | PROCESSED | 57553.0919675926 | 55287 | 55439.0952662037 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 5 | AO5 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 S2 | 49.8015 | 40.983 | 150.77920085 | -13.76419767 | 87.9994 | 55425.2999884259 | 55425.5946527778 | 805097010 | 10904.6 | 10000 | 10934.7 | 10928.6 | 0 | 10904.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8238.7 | 8238.7 | 25455.9 | 0 | PROCESSED | 57553.0977546296 | 55287 | 55439.1113888889 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 5 | AO5 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 S3 | 49.7347 | 40.7118 | 150.88956259 | -14.01841244 | 87.9998 | 55425.5951273148 | 55425.804375 | 805098010 | 11030.8 | 10000 | 11054.8 | 11046.8 | 0 | 11030.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7789.6 | 7789.6 | 18071.9 | 0 | PROCESSED | 57553.1040162037 | 55287 | 55439.0928935185 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 5 | AO5 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 S4 | 49.6689 | 40.4337 | 151.00436531 | -14.27811504 | 87.9984 | 55425.804849537 | 55426.0731018518 | 805099010 | 12307.2 | 10000 | 12307.2 | 12307.2 | 0 | 12307.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 9950 | 9950 | 23169.9 | 0 | PROCESSED | 57553.1090277778 | 55287 | 55439.1353009259 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 5 | AO5 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 S5 | 49.6049 | 40.1572 | 151.11933243 | -14.5358666 | 87.9995 | 55426.4039930556 | 55426.6474537037 | 805100010 | 10620.9 | 10000 | 10628.9 | 10620.9 | 0 | 10628.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10325.7 | 10325.7 | 21031.9 | 0 | PROCESSED | 57553.1198148148 | 55287 | 55439.1414699074 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 5 | AO5 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 S6 | 49.5399 | 39.884 | 151.23166434 | -14.79141746 | 87.9993 | 55426.858900463 | 55427.3321759259 | 805101010 | 16488.8 | 15000 | 16504.8 | 16504.8 | 0 | 16488.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13484.5 | 13484.5 | 40887.9 | 1 | PROCESSED | 57553.1336342593 | 55287 | 55439.1815625 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 5 | AO5 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 S7 | 49.4762 | 39.609 | 151.34578769 | -15.04805542 | 88.0004 | 55427.7102430556 | 55428.0731481482 | 805102010 | 17209.3 | 15000 | 17209.3 | 17233.3 | 0 | 17217.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13795.4 | 13795.4 | 31347.9 | 0 | PROCESSED | 57553.1341550926 | 55287 | 55439.2187847222 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 5 | AO5 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 W1 | 49.5928 | 41.5523 | 150.3228425 | -13.37443973 | 94.0008 | 55428.5346759259 | 55428.7397569445 | 805103010 | 10068 | 10000 | 10068 | 10068 | 0 | 10068 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7321.3 | 7321.3 | 17711.9 | 0 | PROCESSED | 57553.1427777778 | 55287 | 55439.2175 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 5 | AO5 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 W2 | 49.2188 | 41.5721 | 150.07049245 | -13.51031958 | 93.9951 | 55428.7403240741 | 55428.9654513889 | 805104010 | 9989.2 | 10000 | 9997.2 | 9997.2 | 0 | 9989.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7278.7 | 7278.7 | 19447.9 | 1 | PROCESSED | 57553.1453240741 | 55287 | 55460.9467708333 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 5 | AO5 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 W3 | 48.8462 | 41.5856 | 149.82172461 | -13.64958161 | 93.9989 | 55428.9659722222 | 55429.3022916667 | 805105010 | 11166.1 | 10000 | 11190.1 | 11182.1 | 0 | 11166.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 9164.7 | 9164.7 | 29036 | 0 | PROCESSED | 57553.1487962963 | 55287 | 55445.2284143518 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 5 | AO5 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 W4 | 48.4696 | 41.6016 | 149.56812051 | -13.78700029 | 86.9981 | 55429.3049884259 | 55429.5696527778 | 805106010 | 10365.2 | 10000 | 10365.2 | 10373.2 | 0 | 10373.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9680 | 9680 | 22855.9 | 0 | PROCESSED | 57553.1536111111 | 55287 | 55445.2490509259 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 5 | AO5 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 W5 | 48.1001 | 41.6131 | 149.32075885 | -13.92405492 | 94.0016 | 55429.7828125 | 55429.9946296296 | 805107010 | 9219.2 | 10000 | 9219.2 | 9219.2 | 0 | 9219.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 7816.6 | 7816.6 | 18297.9 | 0 | PROCESSED | 57553.1586689815 | 55287 | 55445.231087963 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 5 | AO5 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 W6 | 47.7251 | 41.6255 | 149.06845077 | -14.06119334 | 94.0002 | 55430.3630324074 | 55430.696724537 | 805108010 | 15399.6 | 15000 | 15407.6 | 15399.6 | 0 | 15407.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13610.6 | 13610.6 | 28823.9 | 0 | PROCESSED | 57553.1647569444 | 55287 | 55446.1712384259 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 5 | AO5 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 W7 | 47.3511 | 41.6379 | 148.81593544 | -14.19658633 | 93.9992 | 55431.0429398148 | 55431.5078356482 | 805109010 | 15416.1 | 15000 | 15448.1 | 15432.1 | 0 | 15416.1 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13282.4 | 13282.4 | 40159.9 | 0 | PROCESSED | 57553.1742824074 | 55287 | 55449.2612731482 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 5 | AO5 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 S4.5 | 49.6359 | 40.2959 | 151.06094801 | -14.4070178 | 87.9989 | 55426.0734375 | 55426.4037037037 | 805110010 | 9179.3 | 10000 | 9179.3 | 9179.3 | 0 | 9179.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 6745.9 | 6745.9 | 28530 | 0 | PROCESSED | 57553.1162384259 | 55287 | 55439.1536342593 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 5 | AO5 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 S5.5 | 49.5719 | 40.0219 | 151.17444164 | -14.66274998 | 88.0005 | 55426.6477430556 | 55426.8585648148 | 805111010 | 11132.9 | 10000 | 11156.9 | 11140.9 | 0 | 11132.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7151.8 | 7151.8 | 18207.9 | 0 | PROCESSED | 57553.1273032407 | 55287 | 55439.1544212963 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 5 | AO5 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 S6.5 | 49.508 | 39.7472 | 151.28830519 | -14.91915669 | 87.9995 | 55427.3325115741 | 55427.7099537037 | 805112010 | 15704.6 | 15000 | 15712.6 | 15704.6 | 0 | 15720.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 14403.3 | 14403.3 | 32607.9 | 0 | PROCESSED | 57553.1322222222 | 55287 | 55439.1853587963 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 5 | AO5 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 S7.5 | 49.4444 | 39.4701 | 151.40364882 | -15.177571 | 87.9989 | 55428.0734375 | 55428.5321180556 | 805113010 | 14870 | 15000 | 14870 | 14870 | 0 | 14870 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13072.3 | 13072.3 | 39628 | 0 | PROCESSED | 57553.1466898148 | 55287 | 55439.2152546296 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 5 | AO5 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 W4.5 | 48.2846 | 41.6054 | 149.44545041 | -13.85744176 | 86.9992 | 55429.5700347222 | 55429.7800694444 | 805114010 | 10857.6 | 10000 | 10879.6 | 10865.6 | 0 | 10857.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7734.3 | 7734.3 | 18143.9 | 0 | PROCESSED | 57553.1551388889 | 55287 | 55445.224224537 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 5 | AO5 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 W5.5 | 47.9127 | 41.6204 | 149.19418163 | -13.99181892 | 94.0012 | 55429.9950115741 | 55430.3626967593 | 805115010 | 9821.6 | 10000 | 9825.6 | 9835.6 | 0 | 9821.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 6999 | 6999 | 31768 | 0 | PROCESSED | 57553.1611342593 | 55287 | 55446.1245023148 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 5 | AO5 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 W6.5 | 47.5391 | 41.63 | 148.94387316 | -14.13011853 | 94.0011 | 55430.6970601852 | 55431.0425578704 | 805116010 | 15408.6 | 15000 | 16016.2 | 15408.6 | 0 | 16048.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12581.2 | 12581.2 | 29839.9 | 0 | PROCESSED | 57553.1669560185 | 55287 | 55449.2772916667 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 5 | AO5 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 W7.5 | 47.1647 | 41.6449 | 148.68932505 | -14.26285782 | 94.0006 | 55431.5082175926 | 55431.8251967593 | 805117010 | 15065.6 | 15000 | 15089.6 | 15065.6 | 0 | 15089.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10992 | 10992 | 27383.9 | 0 | PROCESSED | 57553.174525463 | 55287 | 55446.2098263889 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 056005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 5 | AO5 | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| CIZA J2242.8+5301 | 340.7602 | 53.1616 | 104.28022824 | -4.9963098 | 17.994 | 55770.5553703704 | 55772.8210185185 | 806001010 | 122941.9 | 120000 | 122949.9 | 122949.9 | 0 | 122941.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 134804.3 | 134804.3 | 195707.9 | 1 | PROCESSED | 57602.7365393518 | 56162 | 55792.3410069445 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060014 | Radio relics in merging clusters have been considered to be synchrotron emission at a shock front. Nevertheless, no concrete evidence of the connection between relics and shocks has been unveiled yet. We propose a SUZAKU observation of a giant radio relic in a new merging cluster CIZA J2242.8+5301 recently discovered. Temperature and density maps across the giant radio relic will provide a clear illustration of the shock structure or a strong constraint of an origin of the radio relic. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KAWAHARA | HAJIME | NISHINO | SHO | JAP | 6 | AO6 | SUZAKU OBSERVATION OF A NEW MERGING CLUSTER WITH A GIANT RADIO RELIC | XIS | Y |
| CIZA J2242 OFFSET | 339.3149 | 52.6806 | 103.28112871 | -4.99517915 | 17.9944 | 55772.8222337963 | 55774.1446180556 | 806002010 | 55913.4 | 60000 | 55935.6 | 55913.4 | 0 | 55913.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 73189.1 | 73189.1 | 114200 | 2 | PROCESSED | 57602.7241666667 | 56162 | 55792.2422222222 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060014 | Radio relics in merging clusters have been considered to be synchrotron emission at a shock front. Nevertheless, no concrete evidence of the connection between relics and shocks has been unveiled yet. We propose a SUZAKU observation of a giant radio relic in a new merging cluster CIZA J2242.8+5301 recently discovered. Temperature and density maps across the giant radio relic will provide a clear illustration of the shock structure or a strong constraint of an origin of the radio relic. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KAWAHARA | HAJIME | NISHINO | SHO | JAP | 6 | AO6 | SUZAKU OBSERVATION OF A NEW MERGING CLUSTER WITH A GIANT RADIO RELIC | XIS | Y |
| FILAMENT JUNCTION 1 | 204.175 | 43.8307 | 97.2080472 | 70.96687365 | 328.3601 | 55706.688900463 | 55707.984224537 | 806003010 | 52509.1 | 60000 | 52509.1 | 52517.1 | 0 | 52517.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 50133.9 | 50133.9 | 111889.9 | 0 | PROCESSED | 57602.1515509259 | 56093 | 55725.311412037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060015 | Haloes, such as galaxy clusters or groups have been considered to form at intersections of cosmological filaments. Nevertheless, there are a lot of junctions of galaxy filaments without X-ray strong signal from massive clusters. We propose a SUZAKU observation of three filamentary junctions of galaxies identified in the Sloan Digital Sky Survey using a new method. The SUZAKU observation of high sensitivity in low energy will reveal nature of faint haloes growing in the large filament junctions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KAWAHARA | HAJIME | NULL | NULL | JAP | 6 | AO6 | EXPLORING JUNCTIONS OF GALAXY FILAMENTS BY SUZAKU | XIS | Y |
| FILAMENT JUNCTION 2 | 149.2538 | 26.1497 | 204.13118538 | 51.20952403 | 290.4949 | 55699.3618402778 | 55701.114849537 | 806004010 | 70159.1 | 70000 | 70159.1 | 70167.1 | 0 | 70167.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 63329.5 | 63329.5 | 151435.7 | 1 | PROCESSED | 57602.1051851852 | 56092 | 55722.7303356482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060015 | Haloes, such as galaxy clusters or groups have been considered to form at intersections of cosmological filaments. Nevertheless, there are a lot of junctions of galaxy filaments without X-ray strong signal from massive clusters. We propose a SUZAKU observation of three filamentary junctions of galaxies identified in the Sloan Digital Sky Survey using a new method. The SUZAKU observation of high sensitivity in low energy will reveal nature of faint haloes growing in the large filament junctions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KAWAHARA | HAJIME | NULL | NULL | JAP | 6 | AO6 | EXPLORING JUNCTIONS OF GALAXY FILAMENTS BY SUZAKU | XIS | Y |
| FILAMENT JUNCTION 3 | 151.4159 | 39.7399 | 181.90509124 | 53.56333781 | 291.576 | 55672.3023611111 | 55673.6362268518 | 806005010 | 55023.2 | 60000 | 55023.2 | 55031.2 | 0 | 55039.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 49866.9 | 49866.9 | 115229.9 | 2 | PROCESSED | 57601.5861921296 | 56061 | 55692.3338425926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060015 | Haloes, such as galaxy clusters or groups have been considered to form at intersections of cosmological filaments. Nevertheless, there are a lot of junctions of galaxy filaments without X-ray strong signal from massive clusters. We propose a SUZAKU observation of three filamentary junctions of galaxies identified in the Sloan Digital Sky Survey using a new method. The SUZAKU observation of high sensitivity in low energy will reveal nature of faint haloes growing in the large filament junctions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KAWAHARA | HAJIME | NULL | NULL | JAP | 6 | AO6 | EXPLORING JUNCTIONS OF GALAXY FILAMENTS BY SUZAKU | XIS | Y |
| MACSJ0717.5+3547 | 109.4283 | 37.7329 | 180.28338253 | 21.07400371 | 90.0014 | 55841.8814699074 | 55844.0440046296 | 806006010 | 100547.3 | 100000 | 100547.3 | 100555.3 | 0 | 100555.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 93847 | 93847 | 186827.9 | 1 | PROCESSED | 57603.4085763889 | 56240 | 55872.2982523148 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060016 | MACSJ0717.5+3547 is a forming hot cluster located at z=0.55. Chandra observation resolved a >20 keV hot component near its center, in addition to the average ICM temperature of 11.6 keV. With the most luminous radio halo observed to date, the cluster is in a moment of major merging event. It is also associated with a stream of galaxies oriented to the south east. We propose a Suzaku observation with an exposure of 100 ks, aiming at; confirming the bright > 20 keV component, the very hot component (e.g. Nakazawa+ 2010) evidencing the strong merger, and obtain temperature map of the dim diffuse X-ray observed to the south east and the south west to resolve the nature of these emission. With these observation, merging orientation and phase in this very hot cluster can be resolved. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | NAKAZAWA | KAZUHIRO | NULL | NULL | JAP | 6 | AO6 | OBSERVING THE FORMATION EPOCH OF A HOT CLUSTER : SUZAKU OBSERVATION OF MACSJ0717.5+3547 | XIS | Y |
| SNR B0532-675 | 83.0766 | -67.535 | 277.71335978 | -32.44457154 | 140.0497 | 55871.6295601852 | 55874.1570601852 | 806007010 | 82490.9 | 80000 | 82490.9 | 82490.9 | 0 | 82490.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 77457.3 | 77457.3 | 218354.7 | 4 | PROCESSED | 57603.7734027778 | 56257 | 55890.6997337963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060025 | Interstellar medium (ISM) heated by a forward shock of supernova remnants (SNRs) gives us a unique opportunity to study local metal abundance and density. Systematic study of the shock-heated ISM in a galaxy unveils its overall metal distribution and provides a key to understand its chemical evolution. On the basis of this idea, we have performed observations of SNRs in the Large Magellanic Cloud (LMC). We here propose to observe the LMC SNR B0532-675 for 80 ks. Since it locates near the star formation region LH76, we expect that we can study the process of metal diffusion from a star forming region by utilizing the result from another SNR DEM L241 near LH76 already observed. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | SOMEYA | KENTARO | NULL | NULL | JAP | 6 | AO6 | STUDY OF CHEMICAL EVOLUTION OF THE LARGE MAGELLANIC CLOUD WITH SNRS | XIS | Y |
| AWM7 45' EAST | 44.4244 | 41.5971 | 146.87973673 | -15.32937684 | 74.1373 | 55780.4446527778 | 55781.3155208333 | 806008010 | 36879.4 | 35000 | 36879.4 | 36879.4 | 0 | 36879.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 35703.9 | 35703.9 | 75239.9 | 0 | PROCESSED | 57602.7523726852 | 56169 | 55802.4637384259 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060029 | X-ray observations of cluster outskirts give us valuable information about star formation and metal enrichment histories in clusters. Here, we propose to observe three fields with total exposures of 100 ks, 45' east, 27' and 45' south from the center. With these observations, we will compare distributions of Fe and galaxies up to 0.6r180, and study metal-enrichment history in filaments of large-scale structure. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MATSUSHITA | KYOKO | NULL | NULL | JAP | 6 | AO6 | DISTRIBUTION OF FE IN THE INTRACLUSTER MEDIUM OF AWM7 CLUSTER | XIS | Y |
| AWM7 27' SOUTH | 43.6454 | 41.2726 | 146.50839268 | -15.89370788 | 257.401 | 55975.6646296296 | 55976.5071180556 | 806009010 | 34973.5 | 30000 | 34981.5 | 34973.5 | 0 | 34973.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 33645.2 | 33645.2 | 72781.9 | 1 | PROCESSED | 57604.6468055556 | 56361 | 55994.9781828704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060029 | X-ray observations of cluster outskirts give us valuable information about star formation and metal enrichment histories in clusters. Here, we propose to observe three fields with total exposures of 100 ks, 45' east, 27' and 45' south from the center. With these observations, we will compare distributions of Fe and galaxies up to 0.6r180, and study metal-enrichment history in filaments of large-scale structure. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MATSUSHITA | KYOKO | NULL | NULL | JAP | 6 | AO6 | DISTRIBUTION OF FE IN THE INTRACLUSTER MEDIUM OF AWM7 CLUSTER | XIS | Y |
| AWM7 45' SOUTH | 43.6476 | 40.9695 | 146.6593781 | -16.15981584 | 257.4009 | 55974.8888078704 | 55975.6641087963 | 806010010 | 34360.2 | 35000 | 34360.2 | 34360.2 | 0 | 34360.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 32015.5 | 32015.5 | 66978 | 1 | PROCESSED | 57604.6274768518 | 56361 | 55994.9866319444 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060029 | X-ray observations of cluster outskirts give us valuable information about star formation and metal enrichment histories in clusters. Here, we propose to observe three fields with total exposures of 100 ks, 45' east, 27' and 45' south from the center. With these observations, we will compare distributions of Fe and galaxies up to 0.6r180, and study metal-enrichment history in filaments of large-scale structure. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MATSUSHITA | KYOKO | NULL | NULL | JAP | 6 | AO6 | DISTRIBUTION OF FE IN THE INTRACLUSTER MEDIUM OF AWM7 CLUSTER | XIS | Y |
| CENTAURUS CLUSTER N | 192.2138 | -40.9141 | 302.40583252 | 21.95501054 | 115.2417 | 55961.0060763889 | 55962.6667939815 | 806011010 | 54049.6 | 50000 | 54049.6 | 54049.6 | 0 | 54049.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48610.9 | 48610.9 | 143475.8 | 2 | PROCESSED | 57604.5565972222 | 56360 | 55992.1577546296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060035 | We propose to observe two fields at 0.1-0.2r180 of the Centaurus cluster for total 90 ks exposures with Suzaku. The purpose of the observations is to determine Mg and Fe distributions of the intracluster medium up to 0.2 r180 and to study origin of metals in the intracluster medium. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MATSUSHITA | KYOKO | NULL | NULL | JAP | 6 | AO6 | MG AND FE ABUNDANCES OF THE ICM IN THE CENTAURUS CLUSTER UP TO 0.2R180 | XIS | Y |
| XMMU 2235.3-2557 | 338.8435 | -25.9657 | 27.27021923 | -59.64080614 | 244.5944 | 55878.6378125 | 55881.5577777778 | 806013010 | 101122.7 | 100000 | 101122.7 | 101122.7 | 0 | 101122.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 90624.4 | 90624.4 | 252241.7 | 4 | PROCESSED | 57603.8656481482 | 56257 | 55890.7014583333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060038 | Galaxy clusters at high redshift are useful as a cosmological probe that have a potential to constrain the inflation theory via its mass function. A massive cluster, XMMU 2235.3-2557 found at z=1.4 is especially important because the presence itself should be quite rare if the standard theory with the Gaussian random field is correct. However, there can be a lot of systematic errors of the mass estimates, that is, the temperature measurement of the cluster. Hence, we propose an independent measurement of X-ray spectroscopic temperature by SUZAKU. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KAWAHARA | HAJIME | NULL | NULL | JAP | 6 | AO6 | TEMPERATURE MEASUREMENT OF A MASSIVE HIGH-Z CLUSTER XMMU 2235.3-2557 BY SUZAKU | XIS | Y |
| A2319NORTH | 290.2404 | 44.0121 | 75.73364984 | 13.56775034 | 191.4804 | 55925.1947222222 | 55927.5001273148 | 806014010 | 104789.3 | 100000 | 104829.3 | 104789.3 | 0 | 104829.3 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 1866.1 | 0 | PROCESSED | 57604.2771064815 | 56340 | 55973.7475115741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060044 | We propose the observations of the north subgroup region in the A2319 cluster with Suzaku to investigate dynamical status and particle acceleration process in the intracluster medium (ICM). A2319 is a nearby massive merging cluster whose collision axis is nearly along the line of sight, and has diffuse non-thermal radio emission. We will determine the radial velocity of the ICM in the north subgroup region, and compare it with that in the central region which has been already determined from the AO1 data (Sugawara et al. 2009). Using these results and optical observational data of member galaxies, we will determine dynamical status of the ICM and get implications on the particle acceleration process. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAKIZAWA | MOTOKAZU | NULL | NULL | JAP | 6 | AO6 | DYNAMICAL STATUS OF THE HOT GAS AROUND THE NORTH SUBGROUP IN THE A2319 CLUSTER | XIS | Y |
| NGC 6251 | 247.2266 | 82.6554 | 115.95247359 | 31.23340212 | 185.0319 | 55885.7751736111 | 55887.7821875 | 806015010 | 100157.1 | 100000 | 100165.1 | 100157.1 | 0 | 100165.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 98594.3 | 98594.3 | 173375.9 | 1 | PROCESSED | 57603.983599537 | 56264 | 55897.1810300926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060045 | Suzaku observations of lobes of Fanaroff-Riley Type-1 Radio Galaxies NGC 6251 and IC 4296 are proposed. Utilizing the high sensitivity for the diffuse sources of Suzaku, we propose precise measurement of the inverse-Compton X-rays form Fanaroff-Riley Type-1 Radio lobes to determine the electron energy density. Comparing the electron energy density with those of Fanaroff-Riley Type-2 Radio lobes, we examine an evolution model of the radio galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | SETA | HIROMI | NULL | NULL | JAP | 6 | AO6 | OBSERVATIONS OF LOBES OF FANAROFF-RILEY TYPE-1 RADIO GALAXIES | XIS | Y |
| CENTAURUS B | 206.7067 | -60.4086 | 309.7224369 | 1.73083578 | 275.5009 | 55758.843912037 | 55760.4932060185 | 806017010 | 93617.2 | 120000 | 93645 | 93617.2 | 0 | 93637 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 27695.9 | 0 | PROCESSED | 57602.5915625 | 56152 | 55830.7256134259 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060070 | X-ray observation of radio lobe is essential to reveal the particle acceleration mechanism in the lobe, because we can obtain magnetic field and electron energy density without assumption of equipartition. The radio lobe of FR I radio galaxy Centaurus B was previously detected by ASCA. For revealing the mechanism of particle acceleration in radio lobes, detailed multi-wavelength observations are very important. We propose a deep observation of the radio lobe by Suzaku, which has the advantage of low background and high sensitivity for diffuse X-ray. Good quality Suzaku data combined with a detailed modeling reveals particle acceleration mechanism working in the radio lobe. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | TANAKA | YASUYUKI | NULL | NULL | JAP | 6 | AO6 | X-RAY OBSERVATION OF RADIO LOBE OF FR I RADIO GALAXY CENTAURUS B | XIS | Y |
| NGC3628 | 170.0699 | 13.5986 | 240.83294046 | 64.7853987 | 100 | 55890.624212963 | 55892.4070601852 | 806018010 | 81511.5 | 80000 | 81527.5 | 81511.5 | 0 | 81521.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70592.5 | 70592.5 | 153993.8 | 1 | PROCESSED | 57603.996087963 | 56269 | 55901.2586689815 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060082 | We propose 80 ksec observations of edge-on nearby spiral starburst galaxies, NGC3628 and NGC891. We aim to obtain the temperature and the abundance pattern in both the disk and halo regions of two starburst galaxies and hopefully constrain the model of the interactions between not only disk and halo but also halo and intergalactic medium. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MITSUISHI | IKUYUKI | NULL | NULL | JAP | 6 | AO6 | OBSERVATIONS OF AN EDGE-ON STARBURST GALAXIES NGC3628 & NGC891 | XIS | Y |
| COMA OUTSKIRTS1 | 196.4834 | 28.9037 | 62.80265316 | 86.34142243 | 115.9997 | 55900.1880092593 | 55901.4341203704 | 806020010 | 48334 | 50000 | 48334 | 48334 | 0 | 48334 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42251.4 | 42251.4 | 107653.8 | 0 | PROCESSED | 57604.0541898148 | 56282 | 55914.2892013889 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060099 | In order to search cluster evolutions, we propose to observe high temperature cluster(about 8 keV), Coma cluster(z = 0.0231) with six pointings. Three of the field lie in the direction of the large-scale filament, and others are in the perpendicular direction, with their total exposure is 200 ks from 0.5r_180 to virial radius. Thanks to its low background, we can derive the anisotropy of temperature and density profile up to virial radius in detail, and we will search thermalization process in the cluster outskirts region. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | SATO | TAKUYA | NULL | NULL | JAP | 6 | AO6 | STUDY OF CLUSTER EVOLUTION IN THE COMA CLUSTER OUTSKIRTS | XIS | Y |
| COMA OUTSKIRTS2 | 195.8535 | 28.5112 | 61.20140467 | 87.01280614 | 116.0004 | 55901.4349189815 | 55901.9223842593 | 806021010 | 20357.7 | 20000 | 20361.7 | 20357.7 | 0 | 20364.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19194.6 | 19194.6 | 42114 | 0 | PROCESSED | 57604.0414351852 | 56282 | 55914.2609375 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060099 | In order to search cluster evolutions, we propose to observe high temperature cluster(about 8 keV), Coma cluster(z = 0.0231) with six pointings. Three of the field lie in the direction of the large-scale filament, and others are in the perpendicular direction, with their total exposure is 200 ks from 0.5r_180 to virial radius. Thanks to its low background, we can derive the anisotropy of temperature and density profile up to virial radius in detail, and we will search thermalization process in the cluster outskirts region. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | SATO | TAKUYA | NULL | NULL | JAP | 6 | AO6 | STUDY OF CLUSTER EVOLUTION IN THE COMA CLUSTER OUTSKIRTS | XIS | Y |
| COMA OUTSKIRTS3 | 196.1692 | 28.7094 | 62.09765822 | 86.67565791 | 116.0002 | 55901.9229513889 | 55902.7161342593 | 806022010 | 31220 | 30000 | 31244 | 31220 | 0 | 31220 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28724.1 | 28724.1 | 68519.9 | 0 | PROCESSED | 57604.0669212963 | 56284 | 55915.1959837963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060099 | In order to search cluster evolutions, we propose to observe high temperature cluster(about 8 keV), Coma cluster(z = 0.0231) with six pointings. Three of the field lie in the direction of the large-scale filament, and others are in the perpendicular direction, with their total exposure is 200 ks from 0.5r_180 to virial radius. Thanks to its low background, we can derive the anisotropy of temperature and density profile up to virial radius in detail, and we will search thermalization process in the cluster outskirts region. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | SATO | TAKUYA | NULL | NULL | JAP | 6 | AO6 | STUDY OF CLUSTER EVOLUTION IN THE COMA CLUSTER OUTSKIRTS | XIS | Y |
| COMA OUTSKIRTS4 | 193.3444 | 28.9037 | 109.48887466 | 88.17367696 | 116.0002 | 55902.7178125 | 55903.9105324074 | 806023010 | 51656.3 | 50000 | 51664.3 | 51656.3 | 0 | 51671.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 49019.8 | 49019.8 | 103041.9 | 1 | PROCESSED | 57604.0840972222 | 56284 | 55915.2433449074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060099 | In order to search cluster evolutions, we propose to observe high temperature cluster(about 8 keV), Coma cluster(z = 0.0231) with six pointings. Three of the field lie in the direction of the large-scale filament, and others are in the perpendicular direction, with their total exposure is 200 ks from 0.5r_180 to virial radius. Thanks to its low background, we can derive the anisotropy of temperature and density profile up to virial radius in detail, and we will search thermalization process in the cluster outskirts region. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | SATO | TAKUYA | NULL | NULL | JAP | 6 | AO6 | STUDY OF CLUSTER EVOLUTION IN THE COMA CLUSTER OUTSKIRTS | XIS | Y |
| COMA OUTSKIRTS5 | 193.6628 | 28.7109 | 98.9627641 | 88.26548083 | 115.9998 | 55903.9110532407 | 55904.722349537 | 806024010 | 31635 | 30000 | 31659 | 31651 | 0 | 31635 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 29449.1 | 29449.1 | 70089.9 | 0 | PROCESSED | 57604.0811226852 | 56284 | 55915.2478587963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060099 | In order to search cluster evolutions, we propose to observe high temperature cluster(about 8 keV), Coma cluster(z = 0.0231) with six pointings. Three of the field lie in the direction of the large-scale filament, and others are in the perpendicular direction, with their total exposure is 200 ks from 0.5r_180 to virial radius. Thanks to its low background, we can derive the anisotropy of temperature and density profile up to virial radius in detail, and we will search thermalization process in the cluster outskirts region. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | SATO | TAKUYA | NULL | NULL | JAP | 6 | AO6 | STUDY OF CLUSTER EVOLUTION IN THE COMA CLUSTER OUTSKIRTS | XIS | Y |
| COMA OUTSKIRTS6 | 193.974 | 28.5108 | 87.70306179 | 88.30207114 | 115.9975 | 55904.7228703704 | 55905.1452662037 | 806025010 | 21503 | 20000 | 21503 | 21503 | 0 | 21503 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 20265 | 20265 | 36471.9 | 0 | PROCESSED | 57604.0827083333 | 56284 | 55915.2118402778 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 060099 | In order to search cluster evolutions, we propose to observe high temperature cluster(about 8 keV), Coma cluster(z = 0.0231) with six pointings. Three of the field lie in the direction of the large-scale filament, and others are in the perpendicular direction, with their total exposure is 200 ks from 0.5r_180 to virial radius. Thanks to its low background, we can derive the anisotropy of temperature and density profile up to virial radius in detail, and we will search thermalization process in the cluster outskirts region. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | SATO | TAKUYA | NULL | NULL | JAP | 6 | AO6 | STUDY OF CLUSTER EVOLUTION IN THE COMA CLUSTER OUTSKIRTS | XIS | Y |
| SNR 0519-69.0 | 79.8865 | -69.038 | 279.70295655 | -33.37204199 | 53.6181 | 55782.8380324074 | 55789.4030555556 | 806026010 | 347568.1 | 350000 | 347568.1 | 347576.1 | 0 | 347576.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 355072.4 | 355072.4 | 395811.5 | 7 | PROCESSED | 57602.9665740741 | 55652 | 55802.468900463 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061102 | We propose two relatively deep observations of the young ejecta-dominated supernova remnants 0509-67.5 and 0519-69.0 in the Large Magellanic Cloud. Our goal is to seek line emission from the trace elements Mn and Cr in these remnants of Type Ia supernovae, and to measure the corresponding abundances using calculated atomic data. The relative masses of Mn and Cr produced in Type Ia supernovae are a diagnostic of the initial metallicity of the progenitor system. Of the supernovae that produced these two remnants, one had a normal luminosity, while the other was over-luminous. Together with existing data for another LMC Ia remnant, N103B, which shows evidence for circumstellar interactions, these observations will provide a broad sample of the variety seen in Ia events. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | HWANG | UNA | NULL | NULL | USA | 6 | AO6-LP | ABUNDANCES OF CR AND MN AND THE PROGENITOR METALLICITY IN TWO TYPE IA MAGELLANIC CLOUD SNRS | XIS | Y |
| ABELL 773 | 139.6885 | 51.8172 | 165.93230971 | 43.4884399 | 276.9986 | 55682.3638888889 | 55683.2105902778 | 806027010 | 42577.9 | 50000 | 42585.9 | 42585.9 | 0 | 42577.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 32705.2 | 32705.2 | 73143.9 | 0 | PROCESSED | 57601.9080555556 | 55652 | 55697.2644560185 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061116 | We propose observations of 3 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in AO5, and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MILLER | ERIC | NULL | NULL | USA | 6 | AO6-LP | THE SUZAKU CLUSTER OUTSKIRTS PROJECT: OBSERVATIONS TO R200 | XIS | Y |
| ABELL 773 | 139.6415 | 51.5835 | 166.25628799 | 43.50358503 | 276.9979 | 55683.2110185185 | 55684.0730208333 | 806027020 | 47222.3 | 50000 | 47230.3 | 47222.3 | 0 | 47238.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46511.5 | 46511.5 | 74471.9 | 0 | PROCESSED | 57601.9085185185 | 55652 | 55697.3168981482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061116 | We propose observations of 3 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in AO5, and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MILLER | ERIC | NULL | NULL | USA | 6 | AO6-LP | THE SUZAKU CLUSTER OUTSKIRTS PROJECT: OBSERVATIONS TO R200 | XIS | Y |
| ABELL 773 | 139.2619 | 51.6127 | 166.27594696 | 43.26641657 | 277.0001 | 55684.0736342593 | 55684.909212963 | 806027030 | 47578 | 50000 | 47578 | 47578 | 0 | 47578 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44109.5 | 44109.5 | 72181.9 | 0 | PROCESSED | 57601.9127083333 | 55652 | 55697.2793518518 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061116 | We propose observations of 3 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in AO5, and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MILLER | ERIC | NULL | NULL | USA | 6 | AO6-LP | THE SUZAKU CLUSTER OUTSKIRTS PROJECT: OBSERVATIONS TO R200 | XIS | Y |
| ABELL 773 | 139.3092 | 51.8461 | 165.95348434 | 43.2527698 | 276.9988 | 55684.9096412037 | 55685.7363541667 | 806027040 | 49869.1 | 50000 | 49880.5 | 49877.1 | 0 | 49869.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44128.5 | 44128.5 | 71422 | 1 | PROCESSED | 57601.942962963 | 55652 | 55697.3061458333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061116 | We propose observations of 3 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in AO5, and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MILLER | ERIC | NULL | NULL | USA | 6 | AO6-LP | THE SUZAKU CLUSTER OUTSKIRTS PROJECT: OBSERVATIONS TO R200 | XIS | Y |
| ABELL 1068 | 160.1718 | 40.1411 | 178.75085582 | 60.06234552 | 130.0011 | 55860.7020601852 | 55861.8821527778 | 806028010 | 51982.6 | 50000 | 51990.6 | 51982.6 | 0 | 51982.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44534.7 | 44534.7 | 101937.8 | 1 | PROCESSED | 57603.6168981482 | 55652 | 55874.1455324074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061116 | We propose observations of 3 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in AO5, and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MILLER | ERIC | NULL | NULL | USA | 6 | AO6-LP | THE SUZAKU CLUSTER OUTSKIRTS PROJECT: OBSERVATIONS TO R200 | XIS | Y |
| ABELL 1068 | 160.4236 | 39.9791 | 178.96037586 | 60.29153459 | 130.001 | 55861.8826273148 | 55863.1258564815 | 806028020 | 52005.6 | 50000 | 52013.6 | 52005.6 | 0 | 52019.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43275.9 | 43275.9 | 107403.8 | 1 | PROCESSED | 57603.6533333333 | 55652 | 55874.1687615741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061116 | We propose observations of 3 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in AO5, and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MILLER | ERIC | NULL | NULL | USA | 6 | AO6-LP | THE SUZAKU CLUSTER OUTSKIRTS PROJECT: OBSERVATIONS TO R200 | XIS | Y |
| ABELL 1068 | 160.2123 | 39.7867 | 179.4205229 | 60.1860041 | 130.0008 | 55863.1263310185 | 55864.5459837963 | 806028030 | 53318.6 | 50000 | 53318.6 | 53335 | 0 | 53326.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 49071.3 | 49071.3 | 122643.8 | 0 | PROCESSED | 57603.6522800926 | 55652 | 55874.122662037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061116 | We propose observations of 3 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in AO5, and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MILLER | ERIC | NULL | NULL | USA | 6 | AO6-LP | THE SUZAKU CLUSTER OUTSKIRTS PROJECT: OBSERVATIONS TO R200 | XIS | Y |
| ABELL 1068 | 159.9611 | 39.9499 | 179.20513519 | 59.95740225 | 130.001 | 55864.5464583333 | 55865.764849537 | 806028040 | 51149.3 | 50000 | 51157.3 | 51149.3 | 0 | 51165.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46570.1 | 46570.1 | 105249.8 | 0 | PROCESSED | 57603.6525810185 | 55652 | 55879.1651967593 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061116 | We propose observations of 3 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in AO5, and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MILLER | ERIC | NULL | NULL | USA | 6 | AO6-LP | THE SUZAKU CLUSTER OUTSKIRTS PROJECT: OBSERVATIONS TO R200 | XIS | Y |
| ABELL 2667 | 357.9715 | -25.9262 | 34.71945037 | -76.63317585 | 64.8859 | 55721.5923611111 | 55722.9050925926 | 806029010 | 51221.4 | 50000 | 51229.4 | 51229.4 | 0 | 51221.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40484.3 | 40484.3 | 113409.8 | 1 | PROCESSED | 57602.2712962963 | 55652 | 55757.6995486111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061116 | We propose observations of 3 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in AO5, and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MILLER | ERIC | NULL | NULL | USA | 6 | AO6-LP | THE SUZAKU CLUSTER OUTSKIRTS PROJECT: OBSERVATIONS TO R200 | XIS | Y |
| ABELL 2667 | 357.7341 | -26.0226 | 34.17814736 | -76.43580815 | 64.8804 | 55722.9055208333 | 55724.4196990741 | 806029020 | 51657.7 | 50000 | 51665.7 | 51657.7 | 0 | 51672.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45656 | 45656 | 130802 | 1 | PROCESSED | 57602.2808333333 | 55652 | 55757.7009027778 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061116 | We propose observations of 3 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in AO5, and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MILLER | ERIC | NULL | NULL | USA | 6 | AO6-LP | THE SUZAKU CLUSTER OUTSKIRTS PROJECT: OBSERVATIONS TO R200 | XIS | Y |
| ABELL 2667 | 357.8478 | -26.2362 | 33.32905605 | -76.56526922 | 64.8822 | 55724.4201273148 | 55725.7009490741 | 806029030 | 52286.2 | 50000 | 52302.2 | 52286.2 | 0 | 52310.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 42969.7 | 42969.7 | 110655.9 | 1 | PROCESSED | 57602.2711574074 | 55652 | 55757.6986458333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061116 | We propose observations of 3 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in AO5, and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MILLER | ERIC | NULL | NULL | USA | 6 | AO6-LP | THE SUZAKU CLUSTER OUTSKIRTS PROJECT: OBSERVATIONS TO R200 | XIS | Y |
| ABELL 2667 | 358.0843 | -26.1324 | 33.89369276 | -76.76238411 | 64.8814 | 55725.7013773148 | 55726.9814351852 | 806029040 | 51793.6 | 50000 | 51793.6 | 51816.1 | 0 | 51801.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43642.7 | 43642.7 | 110581.8 | 1 | PROCESSED | 57602.3116319444 | 55652 | 55757.7024652778 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061116 | We propose observations of 3 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in AO5, and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MILLER | ERIC | NULL | NULL | USA | 6 | AO6-LP | THE SUZAKU CLUSTER OUTSKIRTS PROJECT: OBSERVATIONS TO R200 | XIS | Y |
| COMA E1 | 195.2288 | 27.9019 | 53.6887936 | 87.76083997 | 279.9992 | 55728.9920601852 | 55729.2682523148 | 806030010 | 9184 | 10000 | 9200 | 9184 | 0 | 9200 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10203.8 | 10203.8 | 23858 | 0 | PROCESSED | 57602.3046296296 | 55652 | 55770.1007407407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y |
| COMA E2 | 195.5294 | 27.8966 | 51.52244118 | 87.51055859 | 279.9995 | 55729.2687268518 | 55729.4890856482 | 806031010 | 9125.6 | 10000 | 9133.6 | 9125.6 | 0 | 9141.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8910.8 | 8910.8 | 19031.9 | 0 | PROCESSED | 57602.3188194444 | 55652 | 55770.1098958333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y |
| COMA E3 | 195.8278 | 27.896 | 49.87218267 | 87.25778961 | 279.9974 | 55729.4896064815 | 55729.6863078704 | 806032010 | 7980.1 | 10000 | 7980.1 | 7980.1 | 0 | 7980.1 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 5764 | 5764 | 16983.9 | 0 | PROCESSED | 57602.3229976852 | 55652 | 55770.1022453704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y |
| COMA E3.5 | 195.93 | 27.9076 | 49.60850486 | 87.16763542 | 128.002 | 55917.6227314815 | 55917.9487384259 | 806032020 | 14769 | 15000 | 14777 | 14785 | 0 | 14769 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9616.9 | 9616.9 | 28159.9 | 1 | PROCESSED | 57604.2057175926 | 55652 | 55937.7819444444 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y |
| COMA E4 | 196.1292 | 27.8947 | 48.48781449 | 87.00057059 | 279.9984 | 55729.6868287037 | 55730.3355671296 | 806033010 | 20202.3 | 20000 | 20202.3 | 20210.3 | 0 | 20218.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20516 | 20516 | 56041.9 | 1 | PROCESSED | 57602.3427199074 | 55652 | 55770.1680092593 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y |
| COMA E5 | 196.4286 | 27.8904 | 47.28907584 | 86.74411283 | 279.9981 | 55730.3360416667 | 55730.7848726852 | 806034010 | 18270.6 | 20000 | 18270.6 | 18294.6 | 0 | 18278.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15075.1 | 15075.1 | 38759.9 | 0 | PROCESSED | 57602.3384259259 | 55652 | 55770.1405324074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y |
| COMA E5.5 | 196.6115 | 27.8944 | 46.75951976 | 86.58537166 | 280.0017 | 55730.7852546296 | 55731.2738657407 | 806035010 | 10879.1 | 15000 | 10887.1 | 10887.1 | 0 | 10879.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12559.7 | 12559.7 | 42197.9 | 0 | PROCESSED | 57602.3474537037 | 55652 | 55770.1742939815 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y |
| COMA E6 | 196.7721 | 27.8867 | 46.15941504 | 86.44797144 | 279.9997 | 55731.2742013889 | 55731.589837963 | 806036010 | 12458.6 | 15000 | 12466.6 | 12458.6 | 0 | 12466.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12206.5 | 12206.5 | 27251.9 | 0 | PROCESSED | 57602.3498263889 | 55652 | 55770.1165046296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y |
| COMA E6.5 | 196.9526 | 27.8857 | 45.6576416 | 86.29162208 | 279.9993 | 55731.5902199074 | 55732.0578935185 | 806037010 | 14959.6 | 15000 | 14967.6 | 14959.6 | 0 | 14967.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13614.2 | 13614.2 | 40399.9 | 0 | PROCESSED | 57602.3577314815 | 55652 | 55770.17125 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y |
| COMA E7 | 197.1143 | 27.885 | 45.24852034 | 86.15126123 | 280.0002 | 55732.0582291667 | 55732.4446990741 | 806038010 | 15117.5 | 15000 | 15133.5 | 15117.5 | 0 | 15141.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16329.5 | 16329.5 | 33303.9 | 0 | PROCESSED | 57602.3596643518 | 55652 | 55770.1779398148 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y |
| COMA NW1 | 194.8094 | 28.1686 | 64.44263169 | 87.98368038 | 319.9994 | 55732.4516550926 | 55732.6453935185 | 806039010 | 9633 | 10000 | 9633 | 9633 | 0 | 9633 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8038 | 8038 | 16727.9 | 0 | PROCESSED | 57602.3588310185 | 55652 | 55768.2335416667 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y |
| COMA NW3 | 194.5571 | 28.6697 | 79.10101688 | 87.84902047 | 319.997 | 55732.646099537 | 55732.9793865741 | 806040010 | 10469 | 10000 | 10469 | 10469 | 0 | 10469 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10176.8 | 10176.8 | 28789.9 | 0 | PROCESSED | 57602.3615856482 | 55652 | 55768.2657523148 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y |
| COMA NW3.5 | 194.5289 | 28.7386 | 80.83345269 | 87.81635354 | 116.0021 | 55917.9522685185 | 55918.5091898148 | 806040020 | 16740.7 | 15000 | 16740.7 | 16763.1 | 0 | 16748.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15805.1 | 15805.1 | 48115.9 | 0 | PROCESSED | 57604.2115509259 | 55652 | 55972.6802662037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y |
| COMA NW4 | 194.43 | 28.912 | 85.44172027 | 87.7408795 | 319.999 | 55732.9798611111 | 55733.468912037 | 806041010 | 21119.6 | 20000 | 21123.6 | 21143.4 | 0 | 21119.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21591.5 | 21591.5 | 42246 | 0 | PROCESSED | 57602.3778819444 | 55652 | 55768.2688888889 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y |
| COMA NW5 | 194.3037 | 29.1454 | 91.00313756 | 87.61452721 | 319.9965 | 55733.4693865741 | 55734.0682407407 | 806042010 | 21097.2 | 20000 | 21120.1 | 21113.2 | 0 | 21097.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20440.1 | 20440.1 | 51724 | 0 | PROCESSED | 57602.3799537037 | 55652 | 55768.342025463 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y |
| COMA NW5.5 | 194.2342 | 29.281 | 93.88493667 | 87.52983745 | 319.9944 | 55734.0685763889 | 55734.4155439815 | 806043010 | 15663.1 | 15000 | 15663.1 | 15663.1 | 0 | 15663.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16384 | 16384 | 29955.9 | 1 | PROCESSED | 57602.3741203704 | 55652 | 55768.2836458333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y |
| COMA NW6 | 194.1545 | 29.4183 | 96.76135884 | 87.44172405 | 319.9992 | 55734.4158796296 | 55734.7419328704 | 806044010 | 13520 | 15000 | 13520 | 13520 | 0 | 13520 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11594.5 | 11594.5 | 28167.9 | 1 | PROCESSED | 57602.3747453704 | 55652 | 55768.2886574074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y |
| COMA NW6.5 | 194.0774 | 29.5523 | 99.36309014 | 87.34957637 | 319.9974 | 55734.7422685185 | 55735.2522569444 | 806045010 | 15501.3 | 15000 | 15501.3 | 15515.1 | 0 | 15509.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17376.4 | 17376.4 | 44059.9 | 0 | PROCESSED | 57602.3928587963 | 55652 | 55768.3250231482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y |
| COMA NW7 | 194.0035 | 29.6909 | 101.76403044 | 87.24693436 | 319.9995 | 55735.2525925926 | 55735.5383680556 | 806046010 | 16121.8 | 15000 | 16151.4 | 16145.8 | 0 | 16121.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 14851.7 | 14851.7 | 24687.9 | 0 | PROCESSED | 57602.3868518518 | 55652 | 55768.6489930556 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y |
| COMA SW1 | 194.4352 | 27.7266 | 56.45564066 | 88.47880121 | 314.5924 | 55735.5408796296 | 55735.8654166667 | 806047010 | 8994.8 | 10000 | 9002.8 | 8994.8 | 0 | 9010.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 8542.3 | 8542.3 | 28033.9 | 1 | PROCESSED | 57602.3938773148 | 55652 | 55794.9989583333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y |
| COMA SW5.5 | 193.6448 | 27.0863 | 29.67661506 | 89.29968791 | 314.5983 | 55735.866400463 | 55736.3037037037 | 806048010 | 15234.5 | 15000 | 15245 | 15234.5 | 0 | 15234.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16437.5 | 16437.5 | 37776 | 0 | PROCESSED | 57602.4025347222 | 55652 | 55794.9965625 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y |
| COMA SW6 | 193.5264 | 26.9952 | 20.45636346 | 89.39137704 | 314.5991 | 55736.3040393518 | 55736.5884259259 | 806049010 | 15693.8 | 15000 | 15693.8 | 15725.8 | 0 | 15709.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13093.4 | 13093.4 | 24559.9 | 0 | PROCESSED | 57602.3988657407 | 55652 | 55795.0033333333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y |
| COMA SW6.5 | 193.4098 | 26.8733 | 5.58469416 | 89.44734556 | 314.5984 | 55736.5887615741 | 55737.1238773148 | 806050010 | 16537.6 | 15000 | 16561.6 | 16553.6 | 0 | 16537.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16662.3 | 16662.3 | 46208 | 2 | PROCESSED | 57602.4126157407 | 55652 | 55795.0480324074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y |
| COMA SW7 | 193.2936 | 26.7739 | 350.54999025 | 89.47529971 | 314.5993 | 55737.124212963 | 55737.4447106482 | 806051010 | 15415.2 | 15000 | 15415.2 | 15423.2 | 0 | 15423.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15036.8 | 15036.8 | 27671.9 | 0 | PROCESSED | 57602.4087847222 | 55652 | 55795.0185763889 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061117 | Our observations of the Perseus Cluster allowed us to determine the first accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of a galaxy cluster. To complement those results, we propose Suzaku observations of two other nearby bright systems: the hot unrelaxed Coma Cluster and the highly relaxed, intermediate temperature Abell 2199. We will test the self-similarity of clusters with different properties at large radii, using profiles of the density, temperature, entropy, pressure, gas mass fraction, and clumping factor. This will provide critical information for the use of clusters as cosmological probes, constraining theoretical feedback models, and understanding the physics of cluster growth. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 6 | AO6-LP | BARYONS AT THE VIRIAL RADII OF NEARBY GALAXY CLUSTERS | XIS | Y |
| 30 DORADUS | 84.6512 | -69.1008 | 279.46621821 | -31.68092384 | 162.7542 | 55895.6278472222 | 55897.0640162037 | 806052010 | 101644.8 | 100000 | 101652.8 | 101652.8 | 0 | 101644.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 89082.3 | 89082.3 | 124076 | 0 | PROCESSED | 57604.044837963 | 56281 | 55907.9795486111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061322 | We propose a deep Suzaku observation of 30 Doradus to provide a direct X-ray measurement of the chemical enrichment in the enclosed hot gas. The soft X-ray sensitivity and spectral resolution of this observation will allow us to measure key elemental abundances and thus to test models for metal yields of massive stars. We will determine the spatial variation in the thermal and chemical properties of the hot gas and the effect on the global estimation of the chemical enrichment from an integrated spectrum, as would be obtained for a distant starburst region. We will also estimate the mass-loading from the general interstellar medium --- a key parameter for determining the evolution of the hot gas. The results will serve as an observational benchmark for understanding massive star feedback. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | WANG | Q. DANIEL | NULL | NULL | USA | 6 | AO6 | X-RAY SPECTROSCOPIC MAPPING OF 30 DORADUS: CHEMICAL ENRICHMENT BY MASSIVE STARS IN A CLOSED BOX | XIS | Y |
| NGC5866 | 226.5977 | 55.7554 | 92.03719886 | 52.50531538 | 352.5583 | 55701.1230092593 | 55703.3466898148 | 806053010 | 101834.6 | 100000 | 101842.6 | 101834.6 | 0 | 101842.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 94781.2 | 94781.2 | 192071.8 | 2 | PROCESSED | 57602.140787037 | 56102 | 55735.3197800926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061502 | An existing Chandra observation indicates hot gas in the S0 galaxy NGC5866 has a supersolar iron abundance and an unusually low O/Fe ratio. The galaxy is also rich in molecular gas and shows distinct vertical dusty filaments, which most likely represent cold gas blown out by SNe from the disk. We herein propose a 100ks Suzaku observation of it to better measure the hot gas properties and its spatial distribution. The energy resolution and counting statistics of the observation will enable us to greatly improve the measurement of the abundances. By further comparing such measurements among galaxies of different cold gas contents, we will investigate the effect of cold/hot gas interaction on the dynamics of the hot gas, as well as its thermal and chemical properties. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | LI | JIANG-TAO | NULL | NULL | USA | 6 | AO6 | X-RAY SPECTROSCOPY OF STELLAR FEEDBACK PROCESSES IN A COOL GAS-RICH S0 GALAXY | XIS | Y |
| BEYOND VIRGO 1 | 187.7129 | 16.0953 | 278.48728746 | 77.9786094 | 118.4704 | 55905.1491666667 | 55905.8431828704 | 806060010 | 22259.8 | 20000 | 22267.8 | 22267.8 | 0 | 22259.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20630 | 20630 | 59953.9 | 1 | PROCESSED | 57604.1022569444 | 56284 | 55917.0698958333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061523 | To have a complete picture of how galaxy clusters evolve and grow, it is vital to understand the thermodynamic properties of their outskirts. Our recent analysis of XMM pointings covering the Virgo Cluster out to large radii provided the first accurate and well resolved measurements of the thermodynamic properties and metallicity of a low-temperature, modestly sized galaxy cluster out to the virial radius (~1.1Mpc). These observations present an exciting insight into the physical conditions of the ICM at large radii, indicating a high level of clumping. We propose to extend these observations significantly further with Suzaku, into an as yet unexplored regime, making precise measurements out to 1.4 virial radii. This will provide our first detailed look beyond the edge of a galaxy cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | WERNER | NORBERT | NULL | NULL | USA | 6 | AO6 | LOOKING PAST THE EDGE OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| BEYOND VIRGO 2 | 187.7135 | 16.3643 | 277.98453264 | 78.22684296 | 118.4711 | 55905.8436574074 | 55906.3980439815 | 806061010 | 21411.5 | 20000 | 21427.5 | 21411.5 | 0 | 21433.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 19181.6 | 19181.6 | 47872 | 1 | PROCESSED | 57604.0951041667 | 56284 | 55917.0723842593 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061523 | To have a complete picture of how galaxy clusters evolve and grow, it is vital to understand the thermodynamic properties of their outskirts. Our recent analysis of XMM pointings covering the Virgo Cluster out to large radii provided the first accurate and well resolved measurements of the thermodynamic properties and metallicity of a low-temperature, modestly sized galaxy cluster out to the virial radius (~1.1Mpc). These observations present an exciting insight into the physical conditions of the ICM at large radii, indicating a high level of clumping. We propose to extend these observations significantly further with Suzaku, into an as yet unexplored regime, making precise measurements out to 1.4 virial radii. This will provide our first detailed look beyond the edge of a galaxy cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | WERNER | NORBERT | NULL | NULL | USA | 6 | AO6 | LOOKING PAST THE EDGE OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| BEYOND VIRGO 3 | 187.7131 | 16.6287 | 277.46526397 | 78.4695575 | 119.4716 | 55906.3990277778 | 55907.0070717593 | 806062010 | 24133.6 | 30000 | 24133.6 | 24133.6 | 0 | 24133.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 22399 | 22399 | 52511.9 | 1 | PROCESSED | 57604.102974537 | 56289 | 55920.9612731482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061523 | To have a complete picture of how galaxy clusters evolve and grow, it is vital to understand the thermodynamic properties of their outskirts. Our recent analysis of XMM pointings covering the Virgo Cluster out to large radii provided the first accurate and well resolved measurements of the thermodynamic properties and metallicity of a low-temperature, modestly sized galaxy cluster out to the virial radius (~1.1Mpc). These observations present an exciting insight into the physical conditions of the ICM at large radii, indicating a high level of clumping. We propose to extend these observations significantly further with Suzaku, into an as yet unexplored regime, making precise measurements out to 1.4 virial radii. This will provide our first detailed look beyond the edge of a galaxy cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | WERNER | NORBERT | NULL | NULL | USA | 6 | AO6 | LOOKING PAST THE EDGE OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| BEYOND VIRGO 4 | 187.7154 | 16.9006 | 276.92044319 | 78.71921322 | 118.472 | 55915.331099537 | 55916.0466666667 | 806063010 | 30136.1 | 30000 | 30136.1 | 30136.1 | 0 | 30136.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22733.4 | 22733.4 | 61818 | 0 | PROCESSED | 57604.1732407407 | 56299 | 55932.1295949074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061523 | To have a complete picture of how galaxy clusters evolve and grow, it is vital to understand the thermodynamic properties of their outskirts. Our recent analysis of XMM pointings covering the Virgo Cluster out to large radii provided the first accurate and well resolved measurements of the thermodynamic properties and metallicity of a low-temperature, modestly sized galaxy cluster out to the virial radius (~1.1Mpc). These observations present an exciting insight into the physical conditions of the ICM at large radii, indicating a high level of clumping. We propose to extend these observations significantly further with Suzaku, into an as yet unexplored regime, making precise measurements out to 1.4 virial radii. This will provide our first detailed look beyond the edge of a galaxy cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | WERNER | NORBERT | NULL | NULL | USA | 6 | AO6 | LOOKING PAST THE EDGE OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| BEYOND VIRGO 5 | 187.715 | 17.1647 | 276.35604201 | 78.95966269 | 118.1329 | 55918.8504976852 | 55919.8960300926 | 806064010 | 41769.2 | 40000 | 41777.2 | 41769.2 | 0 | 41777.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34312.4 | 34312.4 | 90291.9 | 1 | PROCESSED | 57604.2418402778 | 56340 | 55972.6886458333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061523 | To have a complete picture of how galaxy clusters evolve and grow, it is vital to understand the thermodynamic properties of their outskirts. Our recent analysis of XMM pointings covering the Virgo Cluster out to large radii provided the first accurate and well resolved measurements of the thermodynamic properties and metallicity of a low-temperature, modestly sized galaxy cluster out to the virial radius (~1.1Mpc). These observations present an exciting insight into the physical conditions of the ICM at large radii, indicating a high level of clumping. We propose to extend these observations significantly further with Suzaku, into an as yet unexplored regime, making precise measurements out to 1.4 virial radii. This will provide our first detailed look beyond the edge of a galaxy cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | WERNER | NORBERT | NULL | NULL | USA | 6 | AO6 | LOOKING PAST THE EDGE OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| BEYOND VIRGO 6 | 187.7152 | 17.4312 | 275.76419982 | 79.20143703 | 118.777 | 55919.8968287037 | 55920.9286574074 | 806065010 | 39576.9 | 40000 | 39616.9 | 39576.9 | 0 | 39616.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 33770.3 | 33770.3 | 89136 | 2 | PROCESSED | 57604.2337962963 | 56339 | 55972.6645833333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061523 | To have a complete picture of how galaxy clusters evolve and grow, it is vital to understand the thermodynamic properties of their outskirts. Our recent analysis of XMM pointings covering the Virgo Cluster out to large radii provided the first accurate and well resolved measurements of the thermodynamic properties and metallicity of a low-temperature, modestly sized galaxy cluster out to the virial radius (~1.1Mpc). These observations present an exciting insight into the physical conditions of the ICM at large radii, indicating a high level of clumping. We propose to extend these observations significantly further with Suzaku, into an as yet unexplored regime, making precise measurements out to 1.4 virial radii. This will provide our first detailed look beyond the edge of a galaxy cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | WERNER | NORBERT | NULL | NULL | USA | 6 | AO6 | LOOKING PAST THE EDGE OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| BEYOND VIRGO 7 | 187.7158 | 17.6999 | 275.1422843 | 79.44418151 | 118.4175 | 55920.9292708333 | 55922.3029166667 | 806066010 | 51501.8 | 50000 | 51525.8 | 51517.8 | 0 | 51501.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45020.9 | 45020.9 | 118669.8 | 0 | PROCESSED | 57604.2629861111 | 56340 | 55972.6991203704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061523 | To have a complete picture of how galaxy clusters evolve and grow, it is vital to understand the thermodynamic properties of their outskirts. Our recent analysis of XMM pointings covering the Virgo Cluster out to large radii provided the first accurate and well resolved measurements of the thermodynamic properties and metallicity of a low-temperature, modestly sized galaxy cluster out to the virial radius (~1.1Mpc). These observations present an exciting insight into the physical conditions of the ICM at large radii, indicating a high level of clumping. We propose to extend these observations significantly further with Suzaku, into an as yet unexplored regime, making precise measurements out to 1.4 virial radii. This will provide our first detailed look beyond the edge of a galaxy cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | WERNER | NORBERT | NULL | NULL | USA | 6 | AO6 | LOOKING PAST THE EDGE OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| ABELL 3364 | 86.8402 | -31.7251 | 236.7542178 | -26.65907095 | 295.0034 | 55669.7134722222 | 55670.3585416667 | 806067010 | 30073.7 | 29500 | 30089.7 | 30073.7 | 0 | 30089.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28543.7 | 28543.7 | 55727.9 | 1 | PROCESSED | 57601.535787037 | 56067 | 55691.1662962963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061524 | Precision cosmology studies with regular galaxy clusters require a full understanding of cluster physics with a few percent systematic uncertainty. Most of the studies on regular cluster outskirts are limited to cool core clusters but none was studied for non-cool core clusters. We propose a 118 ks Suzaku observation of a regular non-cool core cluster (for the first time) Abell 3364. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will compare results to cool core clusters and test models for pre-heating, shock heating, thermal conduction, e-p equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | WONG | KA-WAH | NULL | NULL | USA | 6 | AO6 | THE FIRST REGULAR NON-COOL CORE GALAXY CLUSTER TO BE STUDIED NEAR THE VIRIAL RADIUS | XIS | Y |
| ABELL 3364 | 87.0888 | -31.8215 | 236.92588426 | -26.48475311 | 295.0036 | 55670.3589699074 | 55670.9259027778 | 806067020 | 29991.3 | 29500 | 29999.3 | 29991.3 | 0 | 30007.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 26718 | 26718 | 48975.9 | 0 | PROCESSED | 57601.5361689815 | 56067 | 55691.2162037037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061524 | Precision cosmology studies with regular galaxy clusters require a full understanding of cluster physics with a few percent systematic uncertainty. Most of the studies on regular cluster outskirts are limited to cool core clusters but none was studied for non-cool core clusters. We propose a 118 ks Suzaku observation of a regular non-cool core cluster (for the first time) Abell 3364. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will compare results to cool core clusters and test models for pre-heating, shock heating, thermal conduction, e-p equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | WONG | KA-WAH | NULL | NULL | USA | 6 | AO6 | THE FIRST REGULAR NON-COOL CORE GALAXY CLUSTER TO BE STUDIED NEAR THE VIRIAL RADIUS | XIS | Y |
| ABELL 3364 | 86.7248 | -31.9341 | 236.9466602 | -26.81319905 | 295.0042 | 55670.9264699074 | 55671.5940162037 | 806067030 | 30780.2 | 29500 | 30780.2 | 30780.2 | 0 | 30780.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30276.2 | 30276.2 | 57663.9 | 1 | PROCESSED | 57601.5516782407 | 56059 | 55692.1831018518 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061524 | Precision cosmology studies with regular galaxy clusters require a full understanding of cluster physics with a few percent systematic uncertainty. Most of the studies on regular cluster outskirts are limited to cool core clusters but none was studied for non-cool core clusters. We propose a 118 ks Suzaku observation of a regular non-cool core cluster (for the first time) Abell 3364. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will compare results to cool core clusters and test models for pre-heating, shock heating, thermal conduction, e-p equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | WONG | KA-WAH | NULL | NULL | USA | 6 | AO6 | THE FIRST REGULAR NON-COOL CORE GALAXY CLUSTER TO BE STUDIED NEAR THE VIRIAL RADIUS | XIS | Y |
| ABELL 3364 | 86.9739 | -32.0342 | 237.12200328 | -26.63960547 | 295.0051 | 55671.5944444444 | 55672.2917939815 | 806067040 | 31886.9 | 29500 | 31894.9 | 31894.9 | 0 | 31886.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 29615.4 | 29615.4 | 60245.9 | 0 | PROCESSED | 57601.5617939815 | 56067 | 55692.2490277778 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061524 | Precision cosmology studies with regular galaxy clusters require a full understanding of cluster physics with a few percent systematic uncertainty. Most of the studies on regular cluster outskirts are limited to cool core clusters but none was studied for non-cool core clusters. We propose a 118 ks Suzaku observation of a regular non-cool core cluster (for the first time) Abell 3364. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will compare results to cool core clusters and test models for pre-heating, shock heating, thermal conduction, e-p equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | WONG | KA-WAH | NULL | NULL | USA | 6 | AO6 | THE FIRST REGULAR NON-COOL CORE GALAXY CLUSTER TO BE STUDIED NEAR THE VIRIAL RADIUS | XIS | Y |
| SPT-CL J0546-5345 | 86.64 | -53.7518 | 261.46331102 | -30.97881567 | 53.9016 | 55781.3261805556 | 55782.8335763889 | 806071010 | 99736.6 | 110000 | 99736.6 | 99736.6 | 0 | 99736.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 78911.4 | 78911.4 | 130207.9 | 3 | PROCESSED | 57602.7921180556 | 56169 | 55802.4644907407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061531 | We propose observations of four high-redshift galaxy clusters to constrain the metal enrichment history of the intra-cluster medium (ICM). The clusters, two at z ~ 1.0 and two at z ~ 0.75, are chosen from an initial mass-limited sample identified by the South Pole Telescope (SPT) cluster project, and they are among the most massive high-redshift clusters known. Chandra observations have verified the absence of point sources in these targets. The proposed Suzaku observations will increase the X-ray cluster counts by a factor of four, they will yield the most precise ICM abundance measurements at these redshifts to date, and they will provide a path-finder for future Suzaku studies of large, representative samples of high-redshift clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MILLER | ERIC | NULL | NULL | USA | 6 | AO6 | THE METAL ABUNDANCE OF HIGH-REDSHIFT GALAXY CLUSTERS | XIS | Y |
| SPT-CL J2341-5119 | 355.3013 | -51.333 | 326.93544545 | -62.39708341 | 56.9213 | 55703.3602662037 | 55706.0800810185 | 806072010 | 100234.7 | 100000 | 100242.7 | 100234.7 | 0 | 100250.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 88208.1 | 88208.1 | 234979.9 | 3 | PROCESSED | 57602.1463310185 | 56092 | 55725.3016550926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061531 | We propose observations of four high-redshift galaxy clusters to constrain the metal enrichment history of the intra-cluster medium (ICM). The clusters, two at z ~ 1.0 and two at z ~ 0.75, are chosen from an initial mass-limited sample identified by the South Pole Telescope (SPT) cluster project, and they are among the most massive high-redshift clusters known. Chandra observations have verified the absence of point sources in these targets. The proposed Suzaku observations will increase the X-ray cluster counts by a factor of four, they will yield the most precise ICM abundance measurements at these redshifts to date, and they will provide a path-finder for future Suzaku studies of large, representative samples of high-redshift clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MILLER | ERIC | NULL | NULL | USA | 6 | AO6 | THE METAL ABUNDANCE OF HIGH-REDSHIFT GALAXY CLUSTERS | XIS | Y |
| SPT-CL J2337-5942 | 354.3472 | -59.706 | 319.15808948 | -55.0279039 | 35.9387 | 55674.1154282407 | 55674.9342592593 | 806073010 | 38841.5 | 35000 | 38841.5 | 38841.5 | 0 | 38841.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 33842.3 | 33842.3 | 70740 | 0 | PROCESSED | 57601.5793402778 | 56067 | 55692.2710069445 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061531 | We propose observations of four high-redshift galaxy clusters to constrain the metal enrichment history of the intra-cluster medium (ICM). The clusters, two at z ~ 1.0 and two at z ~ 0.75, are chosen from an initial mass-limited sample identified by the South Pole Telescope (SPT) cluster project, and they are among the most massive high-redshift clusters known. Chandra observations have verified the absence of point sources in these targets. The proposed Suzaku observations will increase the X-ray cluster counts by a factor of four, they will yield the most precise ICM abundance measurements at these redshifts to date, and they will provide a path-finder for future Suzaku studies of large, representative samples of high-redshift clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MILLER | ERIC | NULL | NULL | USA | 6 | AO6 | THE METAL ABUNDANCE OF HIGH-REDSHIFT GALAXY CLUSTERS | XIS | Y |
| SPT-CL J0000-5748 | 0.2511 | -57.8123 | 315.62746494 | -58.05556131 | 46.7517 | 55694.989849537 | 55696.1169097222 | 806074010 | 50398.6 | 50000 | 50398.6 | 50398.6 | 0 | 50398.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42456.3 | 42456.3 | 97349.8 | 0 | PROCESSED | 57602.0636921296 | 56072 | 55705.1979166667 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061531 | We propose observations of four high-redshift galaxy clusters to constrain the metal enrichment history of the intra-cluster medium (ICM). The clusters, two at z ~ 1.0 and two at z ~ 0.75, are chosen from an initial mass-limited sample identified by the South Pole Telescope (SPT) cluster project, and they are among the most massive high-redshift clusters known. Chandra observations have verified the absence of point sources in these targets. The proposed Suzaku observations will increase the X-ray cluster counts by a factor of four, they will yield the most precise ICM abundance measurements at these redshifts to date, and they will provide a path-finder for future Suzaku studies of large, representative samples of high-redshift clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MILLER | ERIC | NULL | NULL | USA | 6 | AO6 | THE METAL ABUNDANCE OF HIGH-REDSHIFT GALAXY CLUSTERS | XIS | Y |
| EN2-109 | 248.6774 | 40.3802 | 64.11782178 | 42.55568423 | 145.2754 | 55927.5063425926 | 55929.8577314815 | 806075010 | 108616 | 100000 | 108632 | 108616 | 0 | 108640 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 571 | 571 | 572.9 | 0 | PROCESSED | 57604.2767592593 | 56065 | 55946.1449537037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061532 | We propose Suzaku XIS observations of a sample of three high redshift galaxy clusters with 0.87 < z < 1.20 discovered by the 42 square degree Spitzer Adaptation of the Red Sequence Survey (SpARCS). This survey is currently the largest optical/IR survey for high redshift clusters, and includes significant multi-wavelength follow-up. Extensive Gemini spectroscopic observations have confirmed that all of our targets are rich, massive clusters with velocity dispersions ranging from 550-800 km/sec. Our Suzaku observations are designed to detect the extended intra-cluster medium in the cluster cores, provide first estimates of cluster X-ray luminosities, and broadly investigate the core gas densities of our targets. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | HICKS | AMALIA | NULL | NULL | USA | 6 | AO6 | OBSERVING DISTANT GALAXY CLUSTERS FROM THE SPITZER SPARCS SURVEY WITH SUZAKU | XIS | Y |
| ES1-230 | 9.1906 | -44.1805 | 311.80619624 | -72.69400023 | 239.5046 | 55907.020787037 | 55907.8925694444 | 806076010 | 44802.4 | 40000 | 44802.4 | 44802.4 | 0 | 44802.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 52019.3 | 52019.3 | 75319.9 | 0 | PROCESSED | 57604.1212037037 | 56065 | 55920.9678587963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061532 | We propose Suzaku XIS observations of a sample of three high redshift galaxy clusters with 0.87 < z < 1.20 discovered by the 42 square degree Spitzer Adaptation of the Red Sequence Survey (SpARCS). This survey is currently the largest optical/IR survey for high redshift clusters, and includes significant multi-wavelength follow-up. Extensive Gemini spectroscopic observations have confirmed that all of our targets are rich, massive clusters with velocity dispersions ranging from 550-800 km/sec. Our Suzaku observations are designed to detect the extended intra-cluster medium in the cluster cores, provide first estimates of cluster X-ray luminosities, and broadly investigate the core gas densities of our targets. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | HICKS | AMALIA | NULL | NULL | USA | 6 | AO6 | OBSERVING DISTANT GALAXY CLUSTERS FROM THE SPITZER SPARCS SURVEY WITH SUZAKU | XIS | Y |
| LOCK-365 | 161.9095 | 57.7105 | 149.74973686 | 52.48617693 | 106.5217 | 55897.0768981482 | 55900.1780439815 | 806077010 | 149910.2 | 150000 | 149942.2 | 149910.2 | 0 | 149942.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 131125.9 | 131125.9 | 267907.6 | 0 | PROCESSED | 57604.1079050926 | 56065 | 55914.3640393518 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061532 | We propose Suzaku XIS observations of a sample of three high redshift galaxy clusters with 0.87 < z < 1.20 discovered by the 42 square degree Spitzer Adaptation of the Red Sequence Survey (SpARCS). This survey is currently the largest optical/IR survey for high redshift clusters, and includes significant multi-wavelength follow-up. Extensive Gemini spectroscopic observations have confirmed that all of our targets are rich, massive clusters with velocity dispersions ranging from 550-800 km/sec. Our Suzaku observations are designed to detect the extended intra-cluster medium in the cluster cores, provide first estimates of cluster X-ray luminosities, and broadly investigate the core gas densities of our targets. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | HICKS | AMALIA | NULL | NULL | USA | 6 | AO6 | OBSERVING DISTANT GALAXY CLUSTERS FROM THE SPITZER SPARCS SURVEY WITH SUZAKU | XIS | Y |
| RCS131723-0201.3 | 199.3422 | -2.034 | 316.04491283 | 60.17589221 | 291.8811 | 55756.3454513889 | 55756.9585532407 | 806078010 | 24921 | 25000 | 24921 | 24921 | 0 | 24921 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 23120.5 | 23120.5 | 52961.9 | 1 | PROCESSED | 57602.5803009259 | 56163 | 55783.6867939815 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061533 | Accurate relationships between baryons in galaxy clusters and underlying dark matter distributions are crucial for using clusters as cosmological probes. Understanding the gamut of ICM properties, however, requires X-ray observations of samples chosen independently of their X-ray characteristics; likewise, such samples provide a powerful tool for quantifying redshift evolution in cluster properties. We have amassed X-ray observations of 19 optically-selected clusters of galaxies, half at z~0.3 and half at z~0.8. Here we propose 6 additional observations in order to uniformly span a total redshift range of 0.15<z<0.9, for the purposes of constraining cluster evolution with a wholly unbiased sample. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | HICKS | AMALIA | NULL | NULL | USA | 6 | AO6 | AN UNBIASED SAMPLE: CONSTRAINING REDSHIFT EVOLUTION WITH OPTICALLY-SELECTED CLUSTERS OF GALAXIES | XIS | Y |
| RCS211853-6334.5 | 319.7157 | -63.5732 | 330.73727963 | -40.23433007 | 78.3879 | 55689.9756018518 | 55691.0148148148 | 806079010 | 69544.6 | 70000 | 69552.6 | 69544.6 | 0 | 69552.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 57383.6 | 57383.6 | 89773.9 | 0 | PROCESSED | 57601.9954398148 | 56068 | 55701.1727314815 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061533 | Accurate relationships between baryons in galaxy clusters and underlying dark matter distributions are crucial for using clusters as cosmological probes. Understanding the gamut of ICM properties, however, requires X-ray observations of samples chosen independently of their X-ray characteristics; likewise, such samples provide a powerful tool for quantifying redshift evolution in cluster properties. We have amassed X-ray observations of 19 optically-selected clusters of galaxies, half at z~0.3 and half at z~0.8. Here we propose 6 additional observations in order to uniformly span a total redshift range of 0.15<z<0.9, for the purposes of constraining cluster evolution with a wholly unbiased sample. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | HICKS | AMALIA | NULL | NULL | USA | 6 | AO6 | AN UNBIASED SAMPLE: CONSTRAINING REDSHIFT EVOLUTION WITH OPTICALLY-SELECTED CLUSTERS OF GALAXIES | XIS | Y |
| RCS044406-2820.4 | 71.0221 | -28.343 | 228.67801491 | -39.02616141 | 99.3268 | 55827.6316319444 | 55828.8751736111 | 806080010 | 50672.3 | 50000 | 50672.3 | 50672.3 | 0 | 50672.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41902.7 | 41902.7 | 107431.8 | 3 | PROCESSED | 57603.2531134259 | 56222 | 55854.3160300926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061533 | Accurate relationships between baryons in galaxy clusters and underlying dark matter distributions are crucial for using clusters as cosmological probes. Understanding the gamut of ICM properties, however, requires X-ray observations of samples chosen independently of their X-ray characteristics; likewise, such samples provide a powerful tool for quantifying redshift evolution in cluster properties. We have amassed X-ray observations of 19 optically-selected clusters of galaxies, half at z~0.3 and half at z~0.8. Here we propose 6 additional observations in order to uniformly span a total redshift range of 0.15<z<0.9, for the purposes of constraining cluster evolution with a wholly unbiased sample. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | HICKS | AMALIA | NULL | NULL | USA | 6 | AO6 | AN UNBIASED SAMPLE: CONSTRAINING REDSHIFT EVOLUTION WITH OPTICALLY-SELECTED CLUSTERS OF GALAXIES | XIS | Y |
| RCS215222-0503.9 | 328.0881 | -5.0633 | 52.1030598 | -42.03624594 | 70.7002 | 55696.1248842593 | 55696.8398263889 | 806081010 | 30648.2 | 30000 | 30648.2 | 30648.2 | 0 | 30648.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 25372.8 | 25372.8 | 61744 | 0 | PROCESSED | 57602.0507986111 | 56072 | 55705.2063310185 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061533 | Accurate relationships between baryons in galaxy clusters and underlying dark matter distributions are crucial for using clusters as cosmological probes. Understanding the gamut of ICM properties, however, requires X-ray observations of samples chosen independently of their X-ray characteristics; likewise, such samples provide a powerful tool for quantifying redshift evolution in cluster properties. We have amassed X-ray observations of 19 optically-selected clusters of galaxies, half at z~0.3 and half at z~0.8. Here we propose 6 additional observations in order to uniformly span a total redshift range of 0.15<z<0.9, for the purposes of constraining cluster evolution with a wholly unbiased sample. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | HICKS | AMALIA | NULL | NULL | USA | 6 | AO6 | AN UNBIASED SAMPLE: CONSTRAINING REDSHIFT EVOLUTION WITH OPTICALLY-SELECTED CLUSTERS OF GALAXIES | XIS | Y |
| RCS212414-6325.8 | 321.0509 | -63.4275 | 330.62476764 | -40.84164156 | 79.2319 | 55691.4113541667 | 55691.979375 | 806082010 | 36322.4 | 35000 | 36330.4 | 36330.4 | 0 | 36322.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26914 | 26914 | 49067.9 | 1 | PROCESSED | 57602.0065046296 | 56068 | 55701.1927546296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061533 | Accurate relationships between baryons in galaxy clusters and underlying dark matter distributions are crucial for using clusters as cosmological probes. Understanding the gamut of ICM properties, however, requires X-ray observations of samples chosen independently of their X-ray characteristics; likewise, such samples provide a powerful tool for quantifying redshift evolution in cluster properties. We have amassed X-ray observations of 19 optically-selected clusters of galaxies, half at z~0.3 and half at z~0.8. Here we propose 6 additional observations in order to uniformly span a total redshift range of 0.15<z<0.9, for the purposes of constraining cluster evolution with a wholly unbiased sample. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | HICKS | AMALIA | NULL | NULL | USA | 6 | AO6 | AN UNBIASED SAMPLE: CONSTRAINING REDSHIFT EVOLUTION WITH OPTICALLY-SELECTED CLUSTERS OF GALAXIES | XIS | Y |
| RCS051838-4324.9 | 79.6593 | -43.4168 | 248.71475233 | -34.61566895 | 286.4929 | 56016.4337268518 | 56018.0001388889 | 806083010 | 67666.6 | 75000 | 67690.6 | 67666.6 | 0 | 67690.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 57511 | 57511 | 135293.8 | 1 | PROCESSED | 57605.0718402778 | 56399 | 56027.1518287037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 061533 | Accurate relationships between baryons in galaxy clusters and underlying dark matter distributions are crucial for using clusters as cosmological probes. Understanding the gamut of ICM properties, however, requires X-ray observations of samples chosen independently of their X-ray characteristics; likewise, such samples provide a powerful tool for quantifying redshift evolution in cluster properties. We have amassed X-ray observations of 19 optically-selected clusters of galaxies, half at z~0.3 and half at z~0.8. Here we propose 6 additional observations in order to uniformly span a total redshift range of 0.15<z<0.9, for the purposes of constraining cluster evolution with a wholly unbiased sample. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | HICKS | AMALIA | NULL | NULL | USA | 6 | AO6 | AN UNBIASED SAMPLE: CONSTRAINING REDSHIFT EVOLUTION WITH OPTICALLY-SELECTED CLUSTERS OF GALAXIES | XIS | Y |
| A3526 | 192.0509 | -41.0558 | 302.27518183 | 21.81182444 | 109.9986 | 55942.2296990741 | 55942.6807291667 | 806084010 | 16964.5 | 10000 | 16964.5 | 16964.5 | 0 | 16964.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12660.5 | 12660.5 | 38963.9 | 0 | PROCESSED | 57604.361875 | 56331 | 55960.1781712963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 062001 | Suzaku has enabled a breakthrough to be made in the study of the outer parts of clusters. For the first time the gas properties have been measured in a cluster to beyond the virial radius. This is important for understanding the properties of clusters and for cosmological studies. They are also needed for understanding how clusters match to the outer Universe in their temperature and entropy profiles. Are there any large scale accretion shocks? How do filaments match to clusters? The observational breakthrough has been possible due to the combination of the low orbit and thus low background of the Suzaku FI detectors and particularly X-ray bright clusters. We propose here to exploit Suzaku's unique capability to extend this result to an X-ray bright nearby relaxed cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | FABIAN | ANDREW | NULL | NULL | EUR | 6 | AO6 | TO BEYOND THE VIRIAL RADIUS IN THE NEARBY CENTAURUS CLUSTER | XIS | Y |
| A3526 | 191.8847 | -40.8272 | 302.13618529 | 22.03852437 | 109.9993 | 55942.6812037037 | 55942.9772569444 | 806085010 | 15005.7 | 11000 | 15009.7 | 15005.7 | 0 | 15011.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14929.7 | 14929.7 | 25576 | 0 | PROCESSED | 57604.3736805556 | 56331 | 55960.1598726852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 062001 | Suzaku has enabled a breakthrough to be made in the study of the outer parts of clusters. For the first time the gas properties have been measured in a cluster to beyond the virial radius. This is important for understanding the properties of clusters and for cosmological studies. They are also needed for understanding how clusters match to the outer Universe in their temperature and entropy profiles. Are there any large scale accretion shocks? How do filaments match to clusters? The observational breakthrough has been possible due to the combination of the low orbit and thus low background of the Suzaku FI detectors and particularly X-ray bright clusters. We propose here to exploit Suzaku's unique capability to extend this result to an X-ray bright nearby relaxed cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | FABIAN | ANDREW | NULL | NULL | EUR | 6 | AO6 | TO BEYOND THE VIRIAL RADIUS IN THE NEARBY CENTAURUS CLUSTER | XIS | Y |
| A3526 | 191.7105 | -40.5689 | 301.98862911 | 22.29443097 | 109.9992 | 55942.9777314815 | 55943.2362847222 | 806086010 | 13639.1 | 12000 | 13647.1 | 13647.1 | 0 | 13639.1 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11410 | 11410 | 22327.9 | 0 | PROCESSED | 57604.3734606482 | 56352 | 55985.0806944444 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 062001 | Suzaku has enabled a breakthrough to be made in the study of the outer parts of clusters. For the first time the gas properties have been measured in a cluster to beyond the virial radius. This is important for understanding the properties of clusters and for cosmological studies. They are also needed for understanding how clusters match to the outer Universe in their temperature and entropy profiles. Are there any large scale accretion shocks? How do filaments match to clusters? The observational breakthrough has been possible due to the combination of the low orbit and thus low background of the Suzaku FI detectors and particularly X-ray bright clusters. We propose here to exploit Suzaku's unique capability to extend this result to an X-ray bright nearby relaxed cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | FABIAN | ANDREW | NULL | NULL | EUR | 6 | AO6 | TO BEYOND THE VIRIAL RADIUS IN THE NEARBY CENTAURUS CLUSTER | XIS | Y |
| A3526 | 191.5735 | -40.3305 | 301.8706053 | 22.53064841 | 109.9984 | 55943.2367592593 | 55943.6161574074 | 806087010 | 14494.3 | 13000 | 14494.3 | 14494.3 | 0 | 14494.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10386.5 | 10386.5 | 32779.9 | 1 | PROCESSED | 57604.3860416667 | 56332 | 55964.1523148148 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 062001 | Suzaku has enabled a breakthrough to be made in the study of the outer parts of clusters. For the first time the gas properties have been measured in a cluster to beyond the virial radius. This is important for understanding the properties of clusters and for cosmological studies. They are also needed for understanding how clusters match to the outer Universe in their temperature and entropy profiles. Are there any large scale accretion shocks? How do filaments match to clusters? The observational breakthrough has been possible due to the combination of the low orbit and thus low background of the Suzaku FI detectors and particularly X-ray bright clusters. We propose here to exploit Suzaku's unique capability to extend this result to an X-ray bright nearby relaxed cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | FABIAN | ANDREW | NULL | NULL | EUR | 6 | AO6 | TO BEYOND THE VIRIAL RADIUS IN THE NEARBY CENTAURUS CLUSTER | XIS | Y |
| A3526 | 191.429 | -40.092 | 301.74515791 | 22.76656347 | 109.9976 | 55943.6166319444 | 55943.9461111111 | 806088010 | 15066.2 | 14000 | 15070.2 | 15066.2 | 0 | 15066.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14843.4 | 14843.4 | 28458 | 1 | PROCESSED | 57604.3884490741 | 56332 | 55964.2169675926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 062001 | Suzaku has enabled a breakthrough to be made in the study of the outer parts of clusters. For the first time the gas properties have been measured in a cluster to beyond the virial radius. This is important for understanding the properties of clusters and for cosmological studies. They are also needed for understanding how clusters match to the outer Universe in their temperature and entropy profiles. Are there any large scale accretion shocks? How do filaments match to clusters? The observational breakthrough has been possible due to the combination of the low orbit and thus low background of the Suzaku FI detectors and particularly X-ray bright clusters. We propose here to exploit Suzaku's unique capability to extend this result to an X-ray bright nearby relaxed cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | FABIAN | ANDREW | NULL | NULL | EUR | 6 | AO6 | TO BEYOND THE VIRIAL RADIUS IN THE NEARBY CENTAURUS CLUSTER | XIS | Y |
| A3526 | 191.2847 | -39.8559 | 301.61867579 | 22.99978629 | 109.9984 | 55943.9465393518 | 55944.2683333333 | 806089010 | 15910.6 | 15000 | 15918.6 | 15910.6 | 0 | 15918.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12985 | 12985 | 27791.9 | 0 | PROCESSED | 57604.3987268518 | 56332 | 55964.1580439815 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 062001 | Suzaku has enabled a breakthrough to be made in the study of the outer parts of clusters. For the first time the gas properties have been measured in a cluster to beyond the virial radius. This is important for understanding the properties of clusters and for cosmological studies. They are also needed for understanding how clusters match to the outer Universe in their temperature and entropy profiles. Are there any large scale accretion shocks? How do filaments match to clusters? The observational breakthrough has been possible due to the combination of the low orbit and thus low background of the Suzaku FI detectors and particularly X-ray bright clusters. We propose here to exploit Suzaku's unique capability to extend this result to an X-ray bright nearby relaxed cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | FABIAN | ANDREW | NULL | NULL | EUR | 6 | AO6 | TO BEYOND THE VIRIAL RADIUS IN THE NEARBY CENTAURUS CLUSTER | XIS | Y |
| A3526 | 191.1432 | -39.6142 | 301.49310157 | 23.23836897 | 110.0059 | 55944.2688078704 | 55944.754375 | 806090010 | 18370.2 | 16000 | 18378.2 | 18370.2 | 0 | 18385.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14795 | 14795 | 41949.9 | 2 | PROCESSED | 57604.405775463 | 56352 | 55985.1138310185 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 062001 | Suzaku has enabled a breakthrough to be made in the study of the outer parts of clusters. For the first time the gas properties have been measured in a cluster to beyond the virial radius. This is important for understanding the properties of clusters and for cosmological studies. They are also needed for understanding how clusters match to the outer Universe in their temperature and entropy profiles. Are there any large scale accretion shocks? How do filaments match to clusters? The observational breakthrough has been possible due to the combination of the low orbit and thus low background of the Suzaku FI detectors and particularly X-ray bright clusters. We propose here to exploit Suzaku's unique capability to extend this result to an X-ray bright nearby relaxed cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | FABIAN | ANDREW | NULL | NULL | EUR | 6 | AO6 | TO BEYOND THE VIRIAL RADIUS IN THE NEARBY CENTAURUS CLUSTER | XIS | Y |
| UGC03957 NORTH | 114.9138 | 55.8102 | 161.76581362 | 28.79157051 | 294.9973 | 56006.0767939815 | 56007.0710532407 | 806091010 | 41366.2 | 45000 | 41366.2 | 41366.2 | 0 | 41366.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40631.2 | 40631.2 | 85901.9 | 1 | PROCESSED | 57604.9833217593 | 56389 | 56022.2738888889 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 062024 | Upcoming surveys of galaxy clusters require precise calibration of X-ray observables and mass down to low mass regimes to constraint cosmological parameters. However, it's still debated if groups can be treated as simply scaled-down clusters. Precise calibration needs to account for systematics due to the complex baryonic physics. Detailed and extended measurements out to large radii have the potential of accomplish this by exploring most of the system's volume and getting rid of biases derived from extrapolations. Suzaku is a powerful tool to address these studies with massive cluster, but we propose to demonstrate that by selecting the optimal target this can be extended to groups. We also show promising results from our Suzaku analysis of cluster outskirts. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MIRANDA OCEJO | BRENDA | NULL | NULL | EUR | 6 | AO6 | MEASUREMENTS OF THE INTRACLUSTER EMISSION OF THE GROUP OF GALAXIES UGC03957 OUT TO $R_{200}$ WITH SUZAKU | XIS | Y |
| UGC03957 SOUTH | 115.5259 | 55.024 | 162.70412876 | 29.04503782 | 294.9967 | 56007.0719907407 | 56008.1328125 | 806092010 | 48815.9 | 45000 | 48815.9 | 48815.9 | 0 | 48815.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46416.9 | 46416.9 | 91643.9 | 3 | PROCESSED | 57604.9862731482 | 56389 | 56022.2514930556 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 062024 | Upcoming surveys of galaxy clusters require precise calibration of X-ray observables and mass down to low mass regimes to constraint cosmological parameters. However, it's still debated if groups can be treated as simply scaled-down clusters. Precise calibration needs to account for systematics due to the complex baryonic physics. Detailed and extended measurements out to large radii have the potential of accomplish this by exploring most of the system's volume and getting rid of biases derived from extrapolations. Suzaku is a powerful tool to address these studies with massive cluster, but we propose to demonstrate that by selecting the optimal target this can be extended to groups. We also show promising results from our Suzaku analysis of cluster outskirts. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MIRANDA OCEJO | BRENDA | NULL | NULL | EUR | 6 | AO6 | MEASUREMENTS OF THE INTRACLUSTER EMISSION OF THE GROUP OF GALAXIES UGC03957 OUT TO $R_{200}$ WITH SUZAKU | XIS | Y |
| UGC03957 WEST | 114.5487 | 55.2415 | 162.38027408 | 28.51701147 | 289.9984 | 56004.175150463 | 56005.2466550926 | 806093010 | 48216.9 | 45000 | 48224.9 | 48216.9 | 0 | 48224.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 46846 | 46846 | 92567.9 | 0 | PROCESSED | 57604.9538773148 | 56388 | 56020.0984837963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 062024 | Upcoming surveys of galaxy clusters require precise calibration of X-ray observables and mass down to low mass regimes to constraint cosmological parameters. However, it's still debated if groups can be treated as simply scaled-down clusters. Precise calibration needs to account for systematics due to the complex baryonic physics. Detailed and extended measurements out to large radii have the potential of accomplish this by exploring most of the system's volume and getting rid of biases derived from extrapolations. Suzaku is a powerful tool to address these studies with massive cluster, but we propose to demonstrate that by selecting the optimal target this can be extended to groups. We also show promising results from our Suzaku analysis of cluster outskirts. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MIRANDA OCEJO | BRENDA | NULL | NULL | EUR | 6 | AO6 | MEASUREMENTS OF THE INTRACLUSTER EMISSION OF THE GROUP OF GALAXIES UGC03957 OUT TO $R_{200}$ WITH SUZAKU | XIS | Y |
| UGC03957 EAST | 115.9739 | 55.4967 | 162.19834712 | 29.35111138 | 294.9944 | 56008.1335648148 | 56009.1717476852 | 806094010 | 46622.1 | 45000 | 46622.1 | 46622.1 | 0 | 46622.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 45260.8 | 45260.8 | 89687.9 | 1 | PROCESSED | 57604.9930324074 | 56434 | 56068.628900463 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 062024 | Upcoming surveys of galaxy clusters require precise calibration of X-ray observables and mass down to low mass regimes to constraint cosmological parameters. However, it's still debated if groups can be treated as simply scaled-down clusters. Precise calibration needs to account for systematics due to the complex baryonic physics. Detailed and extended measurements out to large radii have the potential of accomplish this by exploring most of the system's volume and getting rid of biases derived from extrapolations. Suzaku is a powerful tool to address these studies with massive cluster, but we propose to demonstrate that by selecting the optimal target this can be extended to groups. We also show promising results from our Suzaku analysis of cluster outskirts. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MIRANDA OCEJO | BRENDA | NULL | NULL | EUR | 6 | AO6 | MEASUREMENTS OF THE INTRACLUSTER EMISSION OF THE GROUP OF GALAXIES UGC03957 OUT TO $R_{200}$ WITH SUZAKU | XIS | Y |
| A1750C | 202.6943 | -1.8873 | 322.57262201 | 59.47596371 | 293.5241 | 55766.9371064815 | 55767.8814814815 | 806095010 | 41489.3 | 40000 | 41504.9 | 41489.3 | 0 | 41504.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41099.1 | 41099.1 | 81577.8 | 0 | PROCESSED | 57602.6723148148 | 56219 | 55851.4572106482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 063019 | We observe Abell 1750 which has three clusters of galaxies in a filamentary structure of the large-scale structure, with 4 pointing observations (80 x 3 + 40 ks). We reveal global spatial structures of temperature, density, and entropy in Abell 1750 for the first time. By a correlation with a galaxy map obtained from SDSS, and a comparison between thermal pressure and total pressure required by the total mass derived from weal lensing analysis, we explore the inflow of matter and evolutionary process in this system. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KAWAHARADA | MADOKA | RANDALL | SCOTT | JUS | 6 | AO6 | SUZAKU OBSERVATION OF ABELL 1750 IN THE LARGE-SCALE STRUCTURE | XIS | Y |
| A1750N | 202.8147 | -1.6537 | 322.93839507 | 59.66232121 | 293.5219 | 55744.8544444444 | 55746.9911111111 | 806096010 | 74713.4 | 80000 | 74729.4 | 74713.4 | 0 | 74729.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 61640.2 | 61640.2 | 184597.9 | 1 | PROCESSED | 57602.5091435185 | 56144 | 55775.4134027778 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 063019 | We observe Abell 1750 which has three clusters of galaxies in a filamentary structure of the large-scale structure, with 4 pointing observations (80 x 3 + 40 ks). We reveal global spatial structures of temperature, density, and entropy in Abell 1750 for the first time. By a correlation with a galaxy map obtained from SDSS, and a comparison between thermal pressure and total pressure required by the total mass derived from weal lensing analysis, we explore the inflow of matter and evolutionary process in this system. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KAWAHARADA | MADOKA | RANDALL | SCOTT | JUS | 6 | AO6 | SUZAKU OBSERVATION OF ABELL 1750 IN THE LARGE-SCALE STRUCTURE | XIS | Y |
| A1750S | 202.5548 | -2.1063 | 322.18359807 | 59.30814244 | 293.521 | 55751.0328009259 | 55753.0002314815 | 806097010 | 80166.8 | 80000 | 80166.8 | 80166.8 | 0 | 80166.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 67044.8 | 67044.8 | 169961.8 | 3 | PROCESSED | 57602.5725578704 | 56148 | 55778.4321412037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 063019 | We observe Abell 1750 which has three clusters of galaxies in a filamentary structure of the large-scale structure, with 4 pointing observations (80 x 3 + 40 ks). We reveal global spatial structures of temperature, density, and entropy in Abell 1750 for the first time. By a correlation with a galaxy map obtained from SDSS, and a comparison between thermal pressure and total pressure required by the total mass derived from weal lensing analysis, we explore the inflow of matter and evolutionary process in this system. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KAWAHARADA | MADOKA | RANDALL | SCOTT | JUS | 6 | AO6 | SUZAKU OBSERVATION OF ABELL 1750 IN THE LARGE-SCALE STRUCTURE | XIS | Y |
| A1750R | 202.8633 | -2.0722 | 322.77954726 | 59.24881782 | 293.5198 | 55748.0658796296 | 55750.0419097222 | 806098010 | 66503.5 | 80000 | 66511.5 | 66503.5 | 0 | 66511.5 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 54782.1 | 54782.1 | 170712.8 | 3 | PROCESSED | 57602.5535763889 | 56311 | 55795.163912037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 063019 | We observe Abell 1750 which has three clusters of galaxies in a filamentary structure of the large-scale structure, with 4 pointing observations (80 x 3 + 40 ks). We reveal global spatial structures of temperature, density, and entropy in Abell 1750 for the first time. By a correlation with a galaxy map obtained from SDSS, and a comparison between thermal pressure and total pressure required by the total mass derived from weal lensing analysis, we explore the inflow of matter and evolutionary process in this system. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KAWAHARADA | MADOKA | RANDALL | SCOTT | JUS | 6 | AO6 | SUZAKU OBSERVATION OF ABELL 1750 IN THE LARGE-SCALE STRUCTURE | XIS | Y |
| A1750R | 202.8691 | -2.0415 | 322.80853082 | 59.27632496 | 111.4517 | 55918.5150810185 | 55918.843912037 | 806098020 | 16062 | 13000 | 16062 | 16062 | 0 | 16062 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11964 | 11964 | 28407.9 | 0 | PROCESSED | 57604.214375 | 56311 | 55972.6764236111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 063019 | We observe Abell 1750 which has three clusters of galaxies in a filamentary structure of the large-scale structure, with 4 pointing observations (80 x 3 + 40 ks). We reveal global spatial structures of temperature, density, and entropy in Abell 1750 for the first time. By a correlation with a galaxy map obtained from SDSS, and a comparison between thermal pressure and total pressure required by the total mass derived from weal lensing analysis, we explore the inflow of matter and evolutionary process in this system. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KAWAHARADA | MADOKA | NULL | NULL | JUS | 6 | AO6 | SUZAKU OBSERVATION OF ABELL 1750 IN THE LARGE-SCALE STRUCTURE | XIS | Y |
| ABELL 426 SW1 | 49.6666 | 41.3604 | 150.47849352 | -13.50469455 | 88.4985 | 55803.5918402778 | 55803.8230671296 | 806099010 | 11559.2 | 10000 | 11575.2 | 11559.2 | 0 | 11575.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11542.1 | 11542.1 | 19970.1 | 0 | PROCESSED | 57603.0124189815 | 55652 | 55826.1721875 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 SW2 | 49.3858 | 41.1787 | 150.39892317 | -13.77223683 | 94.9997 | 55800.6450115741 | 55800.8411111111 | 806100010 | 9004.3 | 10000 | 9004.3 | 9012.3 | 0 | 9020.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 8933 | 8933 | 16934 | 0 | PROCESSED | 57602.9794791667 | 55652 | 55818.1552083333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 SW2.5 | 49.2375 | 41.0889 | 150.35281041 | -13.90838125 | 95.0009 | 55800.8414467593 | 55801.0598611111 | 806101010 | 10634.4 | 10000 | 10658.4 | 10650.4 | 0 | 10634.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10341.7 | 10341.7 | 18855.9 | 0 | PROCESSED | 57602.9850925926 | 55652 | 55818.1410069444 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 SW3 | 49.102 | 40.9982 | 150.31514223 | -14.0400409 | 94.9993 | 55801.0601967593 | 55801.3084722222 | 806102010 | 11955 | 10000 | 11955 | 11955 | 0 | 11955 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7864 | 7864 | 21423.9 | 1 | PROCESSED | 57602.9856134259 | 55652 | 55818.1485185185 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 SW3.5 | 48.9544 | 40.9043 | 150.27094965 | -14.17935173 | 88.4992 | 55801.3110763889 | 55801.6063888889 | 806103010 | 10263.6 | 10000 | 10263.6 | 10263.6 | 0 | 10263.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9568.9 | 9568.9 | 25471.9 | 1 | PROCESSED | 57602.9865046296 | 55652 | 55825.0922337963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 SW4 | 48.8197 | 40.8139 | 150.23286022 | -14.31045471 | 88.4993 | 55801.606724537 | 55801.8501388889 | 806104010 | 13203 | 10000 | 13203 | 13203 | 0 | 13203 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13335 | 13335 | 21007.9 | 0 | PROCESSED | 57602.9897685185 | 55652 | 55826.0785763889 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 SW4.5 | 48.6726 | 40.7228 | 150.18660509 | -14.44721412 | 88.498 | 55801.850474537 | 55802.08625 | 806105010 | 10749.4 | 10000 | 10757.4 | 10757.4 | 0 | 10749.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8915 | 8915 | 20367.9 | 0 | PROCESSED | 57602.9947337963 | 55652 | 55826.0978935185 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 SW5 | 48.5394 | 40.6338 | 150.14795961 | -14.57654163 | 88.4979 | 55802.0865856482 | 55802.4896875 | 806106010 | 16724.1 | 15000 | 16740.1 | 16724.1 | 0 | 16748.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13040.6 | 13040.6 | 34823.9 | 0 | PROCESSED | 57602.9971990741 | 55652 | 55826.1207638889 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 SW5.5 | 48.3936 | 40.5388 | 150.10390207 | -14.71606913 | 88.4991 | 55802.4900694445 | 55802.8161458333 | 806107010 | 15195.1 | 15000 | 15195.1 | 15199.1 | 0 | 15212.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14824.7 | 14824.7 | 28170 | 0 | PROCESSED | 57603.0002083333 | 55652 | 55826.144224537 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 SW6 | 48.2625 | 40.4485 | 150.06660907 | -14.84565948 | 88.4982 | 55802.8164814815 | 55803.0348958333 | 806108010 | 11533.6 | 10000 | 11565.6 | 11557.6 | 0 | 11533.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10755.1 | 10755.1 | 18856.1 | 0 | PROCESSED | 57603.0017476852 | 55652 | 55826.1269444444 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 SW6.5 | 48.1163 | 40.3561 | 150.02002462 | -14.98316021 | 88.4979 | 55803.0352314815 | 55803.3008680556 | 806109010 | 11580.6 | 10000 | 11588.6 | 11580.6 | 0 | 11596.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7067.9 | 7067.9 | 22935.9 | 0 | PROCESSED | 57603.0076041667 | 55652 | 55826.1781481482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 SW7 | 47.984 | 40.268 | 149.97996332 | -15.11138755 | 88.498 | 55803.3012037037 | 55803.5903935185 | 806110010 | 10409 | 10000 | 10409 | 10409 | 0 | 10409 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 9720 | 9720 | 24959.9 | 0 | PROCESSED | 57603.007662037 | 55652 | 55826.1493287037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 SE1 | 50.1688 | 41.3334 | 150.81714435 | -13.31934713 | 89.5646 | 55797.4683912037 | 55797.7113194444 | 806111010 | 10809.9 | 10000 | 10809.9 | 10809.9 | 0 | 10809.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10373.3 | 10373.3 | 20987.9 | 0 | PROCESSED | 57602.9312268518 | 55652 | 55855.1291550926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 SE2 | 50.4145 | 41.1258 | 151.09363465 | -13.389164 | 89.5623 | 55797.7118402778 | 55797.9342824074 | 806112010 | 10834.3 | 10000 | 10838.3 | 10834.3 | 0 | 10842.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10649.6 | 10649.6 | 19210 | 0 | PROCESSED | 57602.9407175926 | 55652 | 55855.1191782407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 SE2.5 | 50.5437 | 41.0145 | 151.24059841 | -13.42708975 | 89.5612 | 55797.9346180556 | 55798.1676041667 | 806113010 | 11042.3 | 10000 | 11050.3 | 11058.3 | 0 | 11042.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9671.1 | 9671.1 | 20119.9 | 0 | PROCESSED | 57602.9433217593 | 55652 | 55855.134849537 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 SE3 | 50.6611 | 40.9157 | 151.37300481 | -13.45928131 | 89.561 | 55798.1679398148 | 55798.4321990741 | 806114010 | 11791.9 | 10000 | 11799.9 | 11791.9 | 0 | 11799.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9246.8 | 9246.8 | 22823.9 | 1 | PROCESSED | 57602.9457407407 | 55652 | 55855.1445949074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 SE3.5 | 50.7904 | 40.8069 | 151.51904657 | -13.49435734 | 89.5614 | 55798.4325347222 | 55798.7085763889 | 806115010 | 11904.5 | 10000 | 11912.5 | 11904.5 | 0 | 11920.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11332.6 | 11332.6 | 23847.9 | 0 | PROCESSED | 57602.9521643518 | 55652 | 55855.1551157407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 SE4 | 50.9063 | 40.7039 | 151.65332772 | -13.52999243 | 89.5612 | 55798.708912037 | 55798.9210300926 | 806116010 | 10835.7 | 10000 | 10840.6 | 10844.6 | 0 | 10835.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10839.4 | 10839.4 | 18320 | 0 | PROCESSED | 57602.9537615741 | 55652 | 55855.1658449074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 SE4.5 | 51.0328 | 40.5957 | 151.7976658 | -13.56504097 | 89.5625 | 55798.9213657407 | 55799.1758912037 | 806117010 | 12019.6 | 10000 | 12019.6 | 12019.6 | 0 | 12035.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10495.9 | 10495.9 | 21983.9 | 0 | PROCESSED | 57602.9577893518 | 55652 | 55855.1616435185 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 SE5 | 51.1493 | 40.4958 | 151.9309414 | -13.59719782 | 89.5614 | 55799.1762268518 | 55799.6029861111 | 806118010 | 16438.2 | 15000 | 16446.2 | 16438.2 | 0 | 16453.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13253.9 | 13253.9 | 36869.9 | 0 | PROCESSED | 57602.9664814815 | 55652 | 55855.1847685185 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 SE5.5 | 51.277 | 40.3868 | 152.07695425 | -13.63166747 | 96.5598 | 55799.6056828704 | 55799.9189351852 | 806119010 | 16270.3 | 15000 | 16278.3 | 16270.3 | 0 | 16278.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16209 | 16209 | 27058 | 0 | PROCESSED | 57602.9656597222 | 55652 | 55865.074224537 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 SE6 | 51.3915 | 40.2857 | 152.21004388 | -13.66501615 | 96.5621 | 55799.9192708333 | 55800.1515856482 | 806120010 | 10145.5 | 10000 | 10145.5 | 10169.5 | 0 | 10153.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8858.7 | 8858.7 | 20063.9 | 0 | PROCESSED | 57602.969212963 | 55652 | 55865.0772569444 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 SE6.5 | 51.5164 | 40.175 | 152.35568667 | -13.7013792 | 87.5613 | 55800.1546990741 | 55800.3765856482 | 806121010 | 10189.9 | 10000 | 10197.9 | 10189.9 | 0 | 10205.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7353 | 7353 | 19167.9 | 0 | PROCESSED | 57602.9755324074 | 55652 | 55865.0897569444 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 SE7 | 51.6308 | 40.0717 | 152.49041219 | -13.73591885 | 87.5626 | 55800.376875 | 55800.6418055556 | 806122010 | 10328.8 | 10000 | 10328.8 | 10328.8 | 0 | 10328.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 9822 | 9822 | 22883.9 | 0 | PROCESSED | 57602.977337963 | 55652 | 55865.0862731482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 NE1 | 50.2177 | 41.6975 | 150.64118254 | -12.9960031 | 89.2472 | 55809.6259259259 | 55809.8452662037 | 806123010 | 10932.5 | 10000 | 10932.5 | 10953.3 | 0 | 10940.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12245.1 | 12245.1 | 18936.1 | 0 | PROCESSED | 57603.0729398148 | 55652 | 55866.0873842593 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 NE2 | 50.5182 | 41.8628 | 150.73800989 | -12.73403508 | 89.4986 | 55808.6745949074 | 55808.8752314815 | 806124010 | 10210.6 | 10000 | 10242.6 | 10234.6 | 0 | 10210.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11683.5 | 11683.5 | 17327.9 | 0 | PROCESSED | 57603.0596412037 | 55652 | 55865.9664467593 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 NE2.5 | 50.6676 | 41.9537 | 150.78054856 | -12.59654862 | 89.499 | 55808.8756134259 | 55809.0717592593 | 806125010 | 9739.4 | 10000 | 9755.4 | 9739.4 | 0 | 9763.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7367.1 | 7367.1 | 16943.9 | 0 | PROCESSED | 57603.064224537 | 55652 | 55865.9792361111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 NE3 | 50.8162 | 42.0347 | 150.82784183 | -12.4676031 | 89.4977 | 55809.0721412037 | 55809.4029513889 | 806126010 | 10566.6 | 10000 | 10566.6 | 10590.6 | 0 | 10574.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10704 | 10704 | 28575.9 | 0 | PROCESSED | 57603.0680902778 | 55652 | 55866.0158333333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 NE3.5 | 50.9699 | 42.1175 | 150.87690614 | -12.33503289 | 89.4979 | 55809.4033333333 | 55809.6251273148 | 806127010 | 10320 | 10000 | 10332 | 10320 | 0 | 10336 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 9379 | 9379 | 19156 | 0 | PROCESSED | 57603.0714583333 | 55652 | 55866.0295833333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 NE4 | 51.1184 | 42.2072 | 150.91831547 | -12.19892536 | 89.4976 | 55808.4229282407 | 55808.6738425926 | 806128010 | 10338.5 | 10000 | 10338.5 | 10346.5 | 0 | 10346.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9776.1 | 9776.1 | 21671.9 | 0 | PROCESSED | 57603.0579282407 | 55652 | 55865.1235069444 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 NE4.5 | 51.271 | 42.2915 | 150.96498821 | -12.06556882 | 89.4971 | 55809.84625 | 55810.0452662037 | 806129010 | 10381 | 10000 | 10381 | 10381 | 0 | 10381 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8933 | 8933 | 17184 | 0 | PROCESSED | 57603.0777777778 | 55652 | 55866.1125462963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 NE5 | 51.4212 | 42.371 | 151.01253218 | -11.93716766 | 89.4976 | 55810.0456481482 | 55810.5418287037 | 806130010 | 17527.6 | 15000 | 17527.6 | 17535.6 | 0 | 17535.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17780.2 | 17780.2 | 42862 | 0 | PROCESSED | 57603.0838888889 | 55652 | 55866.1625925926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 NE5.5 | 51.5754 | 42.4541 | 151.06006994 | -11.8041168 | 89.4991 | 55810.5422569444 | 55810.8217361111 | 806131010 | 14845.8 | 15000 | 14861.8 | 14861.8 | 0 | 14845.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16219.8 | 16219.8 | 24143.9 | 0 | PROCESSED | 57603.0838310185 | 55652 | 55866.1408101852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 NE6 | 51.7255 | 42.539 | 151.10360581 | -11.67130403 | 89.4994 | 55810.8220717593 | 55811.0314583333 | 806132010 | 11424.6 | 10000 | 11440.6 | 11424.6 | 0 | 11448.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10064.5 | 10064.5 | 18087.9 | 0 | PROCESSED | 57603.0828703704 | 55652 | 55866.2046759259 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 NE6.5 | 51.8822 | 42.6245 | 151.15044966 | -11.53522591 | 89.4983 | 55811.0317939815 | 55811.396712963 | 806133010 | 10280.4 | 10000 | 10295.9 | 10287.9 | 0 | 10280.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13727.7 | 13727.7 | 31525.9 | 0 | PROCESSED | 57603.0893634259 | 55652 | 55866.233587963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 NE7 | 52.033 | 42.7019 | 151.19797458 | -11.40826829 | 89.5003 | 55811.3970486111 | 55811.6487384259 | 806134010 | 11079 | 10000 | 11090.8 | 11087 | 0 | 11079 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 10788.6 | 10788.6 | 21736.1 | 0 | PROCESSED | 57603.0933449074 | 55652 | 55868.9251967593 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 NNE1 | 50.001 | 41.7793 | 150.45648036 | -13.01724466 | 60.4921 | 55803.8286805556 | 55804.0543171296 | 806135010 | 11392 | 10000 | 11392 | 11392 | 0 | 11392 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9824 | 9824 | 19487.9 | 0 | PROCESSED | 57603.0136574074 | 55652 | 55830.2051273148 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 NNE2 | 50.087 | 42.0498 | 150.35811431 | -12.75634017 | 60.4956 | 55804.0547916667 | 55804.3098726852 | 806136010 | 10686 | 10000 | 10686 | 10686 | 0 | 10686 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 6899 | 6899 | 22031.9 | 1 | PROCESSED | 57603.0180208333 | 55652 | 55830.1908333333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 NNE2.5 | 50.1251 | 42.1872 | 150.30450115 | -12.62617945 | 60.4949 | 55804.3102083333 | 55804.5820833333 | 806137010 | 10544.4 | 10000 | 10544.4 | 10544.4 | 0 | 10544.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 9962 | 9962 | 23472.1 | 0 | PROCESSED | 57603.0188773148 | 55652 | 55830.2163888889 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 NNE3 | 50.1707 | 42.3226 | 150.2566965 | -12.4946686 | 60.4975 | 55804.5824189815 | 55804.7849768518 | 806138010 | 9859 | 10000 | 9859 | 9859 | 0 | 9859 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 10125 | 10125 | 17471.9 | 0 | PROCESSED | 57603.0234606482 | 55652 | 55871.8708680556 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 NNE3.5 | 50.2092 | 42.4612 | 150.20252687 | -12.36344342 | 60.4978 | 55804.7853125 | 55805.0002546296 | 806139010 | 10020 | 10000 | 10020 | 10020 | 0 | 10020 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9507 | 9507 | 18559.9 | 0 | PROCESSED | 57603.0247916667 | 55652 | 55830.1973958333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 NNE4 | 50.2584 | 42.5938 | 150.15840734 | -12.23290919 | 60.4999 | 55805.0005902778 | 55805.2398263889 | 806140010 | 11808.2 | 10000 | 11808.2 | 11808.2 | 0 | 11808.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7236.1 | 7236.1 | 20656 | 1 | PROCESSED | 57603.0290509259 | 55652 | 55871.8764583333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 NNE4.5 | 50.2947 | 42.7325 | 150.10266361 | -12.10259839 | 60.4962 | 55806.265 | 55806.5613078704 | 806141010 | 11085 | 10000 | 11085 | 11085 | 0 | 11085 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11095.4 | 11095.4 | 25595.9 | 1 | PROCESSED | 57603.0357060185 | 55652 | 55845.2700578704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 NNE5 | 50.3399 | 42.8692 | 150.05355099 | -11.97038799 | 60.497 | 55806.5616898148 | 55806.8931944444 | 806142010 | 16335.9 | 15000 | 16347.1 | 16335.9 | 0 | 16335.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 17034.2 | 17034.2 | 28638 | 0 | PROCESSED | 57603.0391898148 | 55652 | 55845.258900463 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 NNE5.5 | 50.3796 | 43.0058 | 150.00098645 | -11.84054635 | 60.4963 | 55806.8935300926 | 55807.3024074074 | 806143010 | 16450.6 | 15000 | 16472.7 | 16466.6 | 0 | 16450.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11697.5 | 11697.5 | 35319.9 | 1 | PROCESSED | 57603.0430208333 | 55652 | 55845.2820486111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 NNE6 | 50.4234 | 43.1429 | 149.95061465 | -11.70868128 | 60.4955 | 55807.3026967593 | 55807.5834375 | 806144010 | 10430.6 | 10000 | 10430.6 | 10430.6 | 0 | 10430.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10723 | 10723 | 24253.9 | 0 | PROCESSED | 57603.0471990741 | 55652 | 55845.2864467593 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 NNE6.5 | 50.4676 | 43.2769 | 149.90216136 | -11.57929144 | 60.499 | 55807.5838194445 | 55807.8391203704 | 806145010 | 13333.2 | 10000 | 13333.2 | 13333.2 | 0 | 13333.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14162.1 | 14162.1 | 22052 | 0 | PROCESSED | 57603.0507060185 | 55652 | 55845.2486226852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 426 NNE7 | 50.5088 | 43.4191 | 149.84713218 | -11.44434377 | 60.4957 | 55807.8394560185 | 55808.0773148148 | 806146010 | 11093.2 | 10000 | 11093.2 | 11093.2 | 0 | 11093.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8953.4 | 8953.4 | 20519.9 | 0 | PROCESSED | 57603.0508217593 | 55652 | 55845.2850578704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066005 | We propose to exploit Suzaku's unique capabilities to carry out a legacy-class observation of the X-ray emitting gas to beyond the virial radius in the brightest and best cluster target: the Perseus Cluster. Our ultra-deep observation will provide unparalleled insight into the physics of the outer regions of clusters, and the tightest possible control of systematic uncertainties. We will obtain new understanding of the distributions of gas mass and total mass at large radii, as required for cosmological studies. Our study will shed new light on the thermodynamics of cluster outskirts and how large-scale filaments channel matter into clusters. This work is only possible due to Suzaku's low orbit and the low background of its detectors. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ALLEN | STEVEN | NULL | NULL | USA | 6 | AO6-KP | TO BEYOND THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| A2199 OFFSET1 | 247.4695 | 38.9998 | 62.18539249 | 43.43422484 | 299.9971 | 55789.6293171296 | 55790.1995717593 | 806147010 | 20296.5 | 20000 | 20296.5 | 20296.5 | 0 | 20296.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19298.2 | 19298.2 | 49259.9 | 0 | PROCESSED | 57602.803287037 | 55652 | 55806.270150463 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066024 | Clusters of galaxies are thought to form from accretion and merging of smaller systems among large-scale filaments. X-ray observations of cluster outskirts give us valuable information about the structure formation, gas heating and cooling, and metal enrichment of clusters of galaxies. Here, we propose deep surveys of two representative regular clusters with redshift of 0.03-0.04 (Abell 2199 | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MATSUSHITA | KYOKO | SIMIONESCU | AURORA | JAP | 6 | AO6-KP | DISTRIBUTIONS OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF NEARBY CLUSTERS UP TO VIRIAL RADIUS | XIS | Y |
| A2199 OFFSET2 | 247.0222 | 38.9947 | 62.15962406 | 43.78139177 | 300.0001 | 55790.2001851852 | 55790.5974884259 | 806148010 | 20285.6 | 20000 | 20285.6 | 20285.6 | 0 | 20285.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15074 | 15074 | 34319.9 | 1 | PROCESSED | 57602.8518287037 | 55652 | 55806.1895601852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066024 | Clusters of galaxies are thought to form from accretion and merging of smaller systems among large-scale filaments. X-ray observations of cluster outskirts give us valuable information about the structure formation, gas heating and cooling, and metal enrichment of clusters of galaxies. Here, we propose deep surveys of two representative regular clusters with redshift of 0.03-0.04 (Abell 2199 | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MATSUSHITA | KYOKO | SIMIONESCU | AURORA | JAP | 6 | AO6-KP | DISTRIBUTIONS OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF NEARBY CLUSTERS UP TO VIRIAL RADIUS | XIS | Y |
| A2199 OFFSET3 | 246.6242 | 39.5648 | 62.9383018 | 44.10633033 | 299.9982 | 55790.598287037 | 55791.1863425926 | 806149010 | 21366 | 20000 | 21374 | 21374 | 0 | 21366 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20274.3 | 20274.3 | 50801.9 | 1 | PROCESSED | 57602.8605787037 | 55652 | 55806.2156365741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066024 | Clusters of galaxies are thought to form from accretion and merging of smaller systems among large-scale filaments. X-ray observations of cluster outskirts give us valuable information about the structure formation, gas heating and cooling, and metal enrichment of clusters of galaxies. Here, we propose deep surveys of two representative regular clusters with redshift of 0.03-0.04 (Abell 2199 | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MATSUSHITA | KYOKO | SIMIONESCU | AURORA | JAP | 6 | AO6-KP | DISTRIBUTIONS OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF NEARBY CLUSTERS UP TO VIRIAL RADIUS | XIS | Y |
| A2199 OFFSET4 | 247.7662 | 39.3698 | 62.70620415 | 43.21916708 | 270.0003 | 55791.1922337963 | 55791.5912037037 | 806150010 | 18711.6 | 20000 | 18711.6 | 18711.6 | 0 | 18711.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13643 | 13643 | 34463.9 | 0 | PROCESSED | 57602.8546064815 | 55652 | 55806.2666087963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066024 | Clusters of galaxies are thought to form from accretion and merging of smaller systems among large-scale filaments. X-ray observations of cluster outskirts give us valuable information about the structure formation, gas heating and cooling, and metal enrichment of clusters of galaxies. Here, we propose deep surveys of two representative regular clusters with redshift of 0.03-0.04 (Abell 2199 | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MATSUSHITA | KYOKO | SIMIONESCU | AURORA | JAP | 6 | AO6-KP | DISTRIBUTIONS OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF NEARBY CLUSTERS UP TO VIRIAL RADIUS | XIS | Y |
| A2199 OFFSET5 | 248.9722 | 38.6569 | 61.80111812 | 42.24739511 | 272.0003 | 55791.5924652778 | 55792.1787152778 | 806151010 | 21084 | 20000 | 21092 | 21092 | 0 | 21084 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18953.6 | 18953.6 | 50645.9 | 0 | PROCESSED | 57602.8747916667 | 55652 | 55806.2354050926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066024 | Clusters of galaxies are thought to form from accretion and merging of smaller systems among large-scale filaments. X-ray observations of cluster outskirts give us valuable information about the structure formation, gas heating and cooling, and metal enrichment of clusters of galaxies. Here, we propose deep surveys of two representative regular clusters with redshift of 0.03-0.04 (Abell 2199 | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MATSUSHITA | KYOKO | SIMIONESCU | AURORA | JAP | 6 | AO6-KP | DISTRIBUTIONS OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF NEARBY CLUSTERS UP TO VIRIAL RADIUS | XIS | Y |
| A2199 OFFSET6 | 247.2752 | 38.7861 | 61.88224995 | 43.57632899 | 299.9992 | 55792.1844212963 | 55792.9321875 | 806152010 | 29785.1 | 30000 | 29785.1 | 29785.1 | 0 | 29785.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22210.5 | 22210.5 | 64597.9 | 1 | PROCESSED | 57602.8830324074 | 55652 | 55806.2639467593 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066024 | Clusters of galaxies are thought to form from accretion and merging of smaller systems among large-scale filaments. X-ray observations of cluster outskirts give us valuable information about the structure formation, gas heating and cooling, and metal enrichment of clusters of galaxies. Here, we propose deep surveys of two representative regular clusters with redshift of 0.03-0.04 (Abell 2199 | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MATSUSHITA | KYOKO | SIMIONESCU | AURORA | JAP | 6 | AO6-KP | DISTRIBUTIONS OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF NEARBY CLUSTERS UP TO VIRIAL RADIUS | XIS | Y |
| A2199 OFFSET7 | 247.8714 | 39.0623 | 62.28955825 | 43.12499555 | 270.0014 | 55792.9380324074 | 55793.5717708333 | 806153010 | 28978.6 | 30000 | 28994.6 | 28978.6 | 0 | 28994.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 23622.1 | 23622.1 | 54743.9 | 1 | PROCESSED | 57602.8895138889 | 55652 | 55806.2932175926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066024 | Clusters of galaxies are thought to form from accretion and merging of smaller systems among large-scale filaments. X-ray observations of cluster outskirts give us valuable information about the structure formation, gas heating and cooling, and metal enrichment of clusters of galaxies. Here, we propose deep surveys of two representative regular clusters with redshift of 0.03-0.04 (Abell 2199 | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MATSUSHITA | KYOKO | SIMIONESCU | AURORA | JAP | 6 | AO6-KP | DISTRIBUTIONS OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF NEARBY CLUSTERS UP TO VIRIAL RADIUS | XIS | Y |
| A2199 OFFSET8 | 247.7871 | 40.0108 | 63.58609445 | 43.22438175 | 270.3665 | 55796.7271180556 | 55797.4578703704 | 806154010 | 30708.4 | 30000 | 30708.4 | 30708.4 | 0 | 30708.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25648.7 | 25648.7 | 63134 | 2 | PROCESSED | 57602.9315046296 | 55652 | 55806.3170138889 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066024 | Clusters of galaxies are thought to form from accretion and merging of smaller systems among large-scale filaments. X-ray observations of cluster outskirts give us valuable information about the structure formation, gas heating and cooling, and metal enrichment of clusters of galaxies. Here, we propose deep surveys of two representative regular clusters with redshift of 0.03-0.04 (Abell 2199 | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MATSUSHITA | KYOKO | SIMIONESCU | AURORA | JAP | 6 | AO6-KP | DISTRIBUTIONS OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF NEARBY CLUSTERS UP TO VIRIAL RADIUS | XIS | Y |
| A2199 OFFSET9 | 246.619 | 38.9138 | 62.03199075 | 44.09189055 | 267.0002 | 55816.7374652778 | 55817.4077546296 | 806155010 | 28130.4 | 30000 | 28130.4 | 28130.4 | 0 | 28130.4 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 27030.3 | 27030.3 | 57897.9 | 0 | PROCESSED | 57603.128287037 | 55652 | 55851.4428356482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066024 | Clusters of galaxies are thought to form from accretion and merging of smaller systems among large-scale filaments. X-ray observations of cluster outskirts give us valuable information about the structure formation, gas heating and cooling, and metal enrichment of clusters of galaxies. Here, we propose deep surveys of two representative regular clusters with redshift of 0.03-0.04 (Abell 2199 | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MATSUSHITA | KYOKO | SIMIONESCU | AURORA | JAP | 6 | AO6-KP | DISTRIBUTIONS OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF NEARBY CLUSTERS UP TO VIRIAL RADIUS | XIS | Y |
| A2199 OFFSET10 | 245.7785 | 38.4489 | 61.35085602 | 44.73212253 | 143.0073 | 55922.3113541667 | 55923.0174074074 | 806156010 | 32686 | 30000 | 32686 | 32686 | 0 | 32686 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30452 | 30452 | 60995.9 | 1 | PROCESSED | 57604.2399074074 | 55652 | 55972.658599537 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066024 | Clusters of galaxies are thought to form from accretion and merging of smaller systems among large-scale filaments. X-ray observations of cluster outskirts give us valuable information about the structure formation, gas heating and cooling, and metal enrichment of clusters of galaxies. Here, we propose deep surveys of two representative regular clusters with redshift of 0.03-0.04 (Abell 2199 | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MATSUSHITA | KYOKO | SIMIONESCU | AURORA | JAP | 6 | AO6-KP | DISTRIBUTIONS OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF NEARBY CLUSTERS UP TO VIRIAL RADIUS | XIS | Y |
| A2199 OFFSET11 | 246.6136 | 39.2216 | 62.4602069 | 44.10568707 | 268 | 55815.9308449074 | 55816.4036342593 | 806157010 | 20653.3 | 20000 | 20661.3 | 20653.3 | 0 | 20661.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20551 | 20551 | 40843.9 | 3 | PROCESSED | 57603.1066898148 | 55652 | 55865.9405555556 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066024 | Clusters of galaxies are thought to form from accretion and merging of smaller systems among large-scale filaments. X-ray observations of cluster outskirts give us valuable information about the structure formation, gas heating and cooling, and metal enrichment of clusters of galaxies. Here, we propose deep surveys of two representative regular clusters with redshift of 0.03-0.04 (Abell 2199 | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MATSUSHITA | KYOKO | SIMIONESCU | AURORA | JAP | 6 | AO6-KP | DISTRIBUTIONS OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF NEARBY CLUSTERS UP TO VIRIAL RADIUS | XIS | Y |
| A2199 OFFSET12 | 246.9232 | 39.9293 | 63.45171294 | 43.88430519 | 267.9996 | 55820.7013657407 | 55821.2488078704 | 806158010 | 23590.2 | 20000 | 23590.2 | 23590.2 | 0 | 23590.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22154.4 | 22154.4 | 47291.9 | 0 | PROCESSED | 57603.1801851852 | 55652 | 55865.2446412037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066024 | Clusters of galaxies are thought to form from accretion and merging of smaller systems among large-scale filaments. X-ray observations of cluster outskirts give us valuable information about the structure formation, gas heating and cooling, and metal enrichment of clusters of galaxies. Here, we propose deep surveys of two representative regular clusters with redshift of 0.03-0.04 (Abell 2199 | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MATSUSHITA | KYOKO | SIMIONESCU | AURORA | JAP | 6 | AO6-KP | DISTRIBUTIONS OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF NEARBY CLUSTERS UP TO VIRIAL RADIUS | XIS | Y |
| A2199 OFFSET13 | 247.4008 | 39.9951 | 63.55387948 | 43.51978117 | 252.5011 | 55815.2934375 | 55815.9266203704 | 806159010 | 28648 | 20000 | 28648 | 29342.9 | 0 | 29358.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 26783.1 | 26783.1 | 54695.9 | 0 | PROCESSED | 57603.1066087963 | 55652 | 55851.4378703704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066024 | Clusters of galaxies are thought to form from accretion and merging of smaller systems among large-scale filaments. X-ray observations of cluster outskirts give us valuable information about the structure formation, gas heating and cooling, and metal enrichment of clusters of galaxies. Here, we propose deep surveys of two representative regular clusters with redshift of 0.03-0.04 (Abell 2199 | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MATSUSHITA | KYOKO | SIMIONESCU | AURORA | JAP | 6 | AO6-KP | DISTRIBUTIONS OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF NEARBY CLUSTERS UP TO VIRIAL RADIUS | XIS | Y |
| A2199 OFFSET14 | 246.2604 | 39.5212 | 62.86911341 | 44.38588157 | 254.9999 | 55825.6665625 | 55826.3946527778 | 806160010 | 27441.3 | 30000 | 27441.4 | 27441.3 | 0 | 27441.3 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 26949.1 | 26949.1 | 62901.9 | 0 | PROCESSED | 57603.222962963 | 55652 | 55851.4517361111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066024 | Clusters of galaxies are thought to form from accretion and merging of smaller systems among large-scale filaments. X-ray observations of cluster outskirts give us valuable information about the structure formation, gas heating and cooling, and metal enrichment of clusters of galaxies. Here, we propose deep surveys of two representative regular clusters with redshift of 0.03-0.04 (Abell 2199 | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MATSUSHITA | KYOKO | SIMIONESCU | AURORA | JAP | 6 | AO6-KP | DISTRIBUTIONS OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF NEARBY CLUSTERS UP TO VIRIAL RADIUS | XIS | Y |
| A2199 OFFSET15 | 246.482 | 39.889 | 63.3872074 | 44.22195617 | 255.0003 | 55823.9923726852 | 55824.6403935185 | 806161010 | 28166.9 | 30000 | 28182.9 | 28166.9 | 0 | 28182.9 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 28074.6 | 28074.6 | 55981.9 | 0 | PROCESSED | 57603.196412037 | 55652 | 55851.4457060185 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066024 | Clusters of galaxies are thought to form from accretion and merging of smaller systems among large-scale filaments. X-ray observations of cluster outskirts give us valuable information about the structure formation, gas heating and cooling, and metal enrichment of clusters of galaxies. Here, we propose deep surveys of two representative regular clusters with redshift of 0.03-0.04 (Abell 2199 | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MATSUSHITA | KYOKO | SIMIONESCU | AURORA | JAP | 6 | AO6-KP | DISTRIBUTIONS OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF NEARBY CLUSTERS UP TO VIRIAL RADIUS | XIS | Y |
| A2199 OFFSET16 | 247.7994 | 39.696 | 63.15474779 | 43.20527386 | 235.0008 | 55840.9241666667 | 55841.4308217593 | 806162010 | 28315.8 | 30000 | 28315.8 | 28315.8 | 0 | 28315.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 28698.3 | 28698.3 | 43767.9 | 0 | PROCESSED | 57603.3467824074 | 55652 | 55858.377037037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 066024 | Clusters of galaxies are thought to form from accretion and merging of smaller systems among large-scale filaments. X-ray observations of cluster outskirts give us valuable information about the structure formation, gas heating and cooling, and metal enrichment of clusters of galaxies. Here, we propose deep surveys of two representative regular clusters with redshift of 0.03-0.04 (Abell 2199 | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MATSUSHITA | KYOKO | SIMIONESCU | AURORA | JAP | 6 | AO6-KP | DISTRIBUTIONS OF TEMPERATURE AND ENTROPY OF INTRACLUSTER MEDIUM OF NEARBY CLUSTERS UP TO VIRIAL RADIUS | XIS | Y |
| 1RXJ0603 | 90.7832 | 42.2686 | 170.16927881 | 9.72454424 | 80.0992 | 56207.7131828704 | 56210.6307986111 | 807001010 | 124341.6 | 120000 | 124351.1 | 124343.9 | 0 | 124341.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 125194.8 | 125194.8 | 252055.9 | 1 | PROCESSED | 57607.7803009259 | 56595 | 56226.6645717593 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070025 | We propose to 120 ks + 30 ks (background) Suzaku observations of a new cluster scale shock front candiate in merger cluster of galaxies 1RXJ0603. 1RXJ0603 has irregular shape radio relic with remarkable steep radio spectrum index, which indicate the existence of shock fronts with mach number M ~ 4.5. The temperature and density of Intra ClusterMedium across radio relics will provide the nature of shock front. Our study will shed new light on the origin of the cluster scale shock fronts. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | AKAMATSU | HIROKI | NULL | NULL | JAP | 7 | AO7 | SUZAKU OBSERVATION OF A NEW CLUSTER SCALE SHOCK FRONT CANDIATE IN MERGING CLUSTER OF GALAXIES 1RXJ0603 | XIS | Y |
| 1RXJ0603 OFFSET | 92.2783 | 42.2687 | 170.6889541 | 10.70559867 | 80.0991 | 56214.8308564815 | 56215.5314236111 | 807002010 | 26833.4 | 30000 | 26833.4 | 26857.4 | 0 | 26841.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28353.1 | 28353.1 | 60515.9 | 1 | PROCESSED | 57607.7719907407 | 56690 | 56323.4936574074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070025 | We propose to 120 ks + 30 ks (background) Suzaku observations of a new cluster scale shock front candiate in merger cluster of galaxies 1RXJ0603. 1RXJ0603 has irregular shape radio relic with remarkable steep radio spectrum index, which indicate the existence of shock fronts with mach number M ~ 4.5. The temperature and density of Intra ClusterMedium across radio relics will provide the nature of shock front. Our study will shed new light on the origin of the cluster scale shock fronts. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | AKAMATSU | HIROKI | NULL | NULL | JAP | 7 | AO7 | SUZAKU OBSERVATION OF A NEW CLUSTER SCALE SHOCK FRONT CANDIATE IN MERGING CLUSTER OF GALAXIES 1RXJ0603 | XIS | Y |
| A1631_N | 193.3404 | -15.1138 | 303.62251983 | 47.75536925 | 113.0007 | 56303.6628356482 | 56304.4904861111 | 807003010 | 28043.3 | 20000 | 28183 | 28183 | 0 | 28043.3 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 25305.9 | 25305.9 | 71480 | 1 | PROCESSED | 57608.4621296296 | 56703 | 56337.5115393518 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070029 | In the ROSAT flux-limited survey, we find that about 5-10 % of the galaxy clusters have a very diffuse, low X-ray surface brightness (hereafter, LSB clusters). They could possibly be explained as dynamically young systems, which have not yet formed a central core. Three such clusters in our XMM study of the REXCESS sample show surprisingly high entropies in the centers, which does not readily support the early formation stage. To shed more light on their nature, we propose to observe the extreme LSB cluster, A1631. This object has a higher optical to X-ray luminosity ratio than the bulk of other clusters and is expected to provide a key to understand the evolutionary scenario of the LSB clusters. Suzaku with its low background is best-suited for this study. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | OTA | NAOMI | NULL | NULL | JAP | 7 | AO7 | PROBING THE NATURE OF A VERY LOW SURFACE BRIGHTNESS CLUSTER A1631 | XIS | Y |
| A1631_C | 193.2396 | -15.343 | 303.4747971 | 47.52714603 | 112.9996 | 56304.4910069444 | 56305.0106944444 | 807004010 | 23805.7 | 20000 | 23813.7 | 23805.7 | 0 | 23805.7 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 19936.9 | 19936.9 | 44871.9 | 0 | PROCESSED | 57608.4757986111 | 56704 | 56337.5260300926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070029 | In the ROSAT flux-limited survey, we find that about 5-10 % of the galaxy clusters have a very diffuse, low X-ray surface brightness (hereafter, LSB clusters). They could possibly be explained as dynamically young systems, which have not yet formed a central core. Three such clusters in our XMM study of the REXCESS sample show surprisingly high entropies in the centers, which does not readily support the early formation stage. To shed more light on their nature, we propose to observe the extreme LSB cluster, A1631. This object has a higher optical to X-ray luminosity ratio than the bulk of other clusters and is expected to provide a key to understand the evolutionary scenario of the LSB clusters. Suzaku with its low background is best-suited for this study. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | OTA | NAOMI | NULL | NULL | JAP | 7 | AO7 | PROBING THE NATURE OF A VERY LOW SURFACE BRIGHTNESS CLUSTER A1631 | XIS | Y |
| A1631_E | 193.4806 | -15.4427 | 303.81684947 | 47.4247798 | 113.0006 | 56305.0111226852 | 56305.7231944445 | 807005010 | 20523.6 | 20000 | 20523.6 | 20523.6 | 0 | 20547.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 20111.1 | 20111.1 | 61511.9 | 1 | PROCESSED | 57608.4784143518 | 56703 | 56337.4913425926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070029 | In the ROSAT flux-limited survey, we find that about 5-10 % of the galaxy clusters have a very diffuse, low X-ray surface brightness (hereafter, LSB clusters). They could possibly be explained as dynamically young systems, which have not yet formed a central core. Three such clusters in our XMM study of the REXCESS sample show surprisingly high entropies in the centers, which does not readily support the early formation stage. To shed more light on their nature, we propose to observe the extreme LSB cluster, A1631. This object has a higher optical to X-ray luminosity ratio than the bulk of other clusters and is expected to provide a key to understand the evolutionary scenario of the LSB clusters. Suzaku with its low background is best-suited for this study. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | OTA | NAOMI | NULL | NULL | JAP | 7 | AO7 | PROBING THE NATURE OF A VERY LOW SURFACE BRIGHTNESS CLUSTER A1631 | XIS | Y |
| A1631_W | 193.0037 | -15.2462 | 303.13836962 | 47.6253175 | 112.9992 | 56305.7238541667 | 56306.3738194444 | 807006010 | 21005.2 | 20000 | 21021.2 | 21005.2 | 0 | 21027 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18599.9 | 18599.9 | 56153.9 | 0 | PROCESSED | 57608.4939351852 | 56703 | 56337.5213541667 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070029 | In the ROSAT flux-limited survey, we find that about 5-10 % of the galaxy clusters have a very diffuse, low X-ray surface brightness (hereafter, LSB clusters). They could possibly be explained as dynamically young systems, which have not yet formed a central core. Three such clusters in our XMM study of the REXCESS sample show surprisingly high entropies in the centers, which does not readily support the early formation stage. To shed more light on their nature, we propose to observe the extreme LSB cluster, A1631. This object has a higher optical to X-ray luminosity ratio than the bulk of other clusters and is expected to provide a key to understand the evolutionary scenario of the LSB clusters. Suzaku with its low background is best-suited for this study. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | OTA | NAOMI | NULL | NULL | JAP | 7 | AO7 | PROBING THE NATURE OF A VERY LOW SURFACE BRIGHTNESS CLUSTER A1631 | XIS | Y |
| N49 | 81.5075 | -66.0821 | 276.09278992 | -33.24378088 | 327.2258 | 56056.8032986111 | 56060.6898148148 | 807007010 | 184543 | 190000 | 184559 | 184543 | 0 | 184559 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 206582.9 | 206582.9 | 335755.8 | 3 | PROCESSED | 57605.4699189815 | 56527 | 56161.1703935185 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070036 | Recently, we discovered recombining plasma (RP) from several mixed-morphology (MM) SNRs in our galaxy, which provides us a new insight into the evolution of SNRs. On the other hand, the RP has not been detected yet from extragalactic SNRs, while many MM-SNRs exist also in extra galaxies. We investigated all the X-ray spectra obtained from previous observations with Suzaku, XMM-Newton and Chandra and found a clear signal of the RP from three LMC SNRs (N49, N23 and DEM L71). Long-time observations with Suzaku XIS will provide us a first evidence of RP from extra galaxies. We propose 2-pointing observations of three SNRs for 290ks. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | UCHIDA | HIROYUKI | NULL | NULL | JAP | 7 | AO7 | FIRST INVESTIGATION OF RECOMBINING PLASMA FROM EXTRAGALACTIC SNRS | XIS | Y |
| N23_DEML71 | 76.4544 | -67.9572 | 278.75688601 | -34.83345845 | 297.0986 | 56021.0207986111 | 56023.6043402778 | 807008010 | 101961.4 | 100000 | 101961.4 | 101961.4 | 0 | 101961.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 99003.1 | 99003.1 | 223204 | 1 | PROCESSED | 57605.1620023148 | 56401 | 56034.2910069444 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070036 | Recently, we discovered recombining plasma (RP) from several mixed-morphology (MM) SNRs in our galaxy, which provides us a new insight into the evolution of SNRs. On the other hand, the RP has not been detected yet from extragalactic SNRs, while many MM-SNRs exist also in extra galaxies. We investigated all the X-ray spectra obtained from previous observations with Suzaku, XMM-Newton and Chandra and found a clear signal of the RP from three LMC SNRs (N49, N23 and DEM L71). Long-time observations with Suzaku XIS will provide us a first evidence of RP from extra galaxies. We propose 2-pointing observations of three SNRs for 290ks. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | UCHIDA | HIROYUKI | NULL | NULL | JAP | 7 | AO7 | FIRST INVESTIGATION OF RECOMBINING PLASMA FROM EXTRAGALACTIC SNRS | XIS | Y |
| PERSEUS F_2 | 49.9481 | 41.7834 | 150.42037818 | -13.03556783 | 257.3692 | 56324.1634259259 | 56324.4342939815 | 807019010 | 17208.6 | 15000 | 17215.6 | 17215.6 | 0 | 17208.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 18555.5 | 18555.5 | 23399.9 | 0 | PROCESSED | 57610.4952314815 | 56731 | 56365.4862731482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070056 | We propose to map the central region (R<20') of the Perseus cluster of galaxies. The cluster is the X-ray brightest one at z=0.02. This unique object along with good performance of the SUZAKU XIS and HXD provides the best quality, wide-band and spatially-resolved X-ray spectroscopy of the ICM. Using the data, we will measure ICM bulk motions around the cluster core. Based on these observation, we will understand the physics of cluster formation and the distribution of dark matter. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAMURA | TAKAYUKI | NULL | NULL | JAP | 7 | AO7 | GAS MOTION IN THE PERSEUS | XIS | Y |
| PERSEUS S1_2 | 49.8718 | 41.2522 | 150.6720925 | -13.51034913 | 256.4607 | 56333.5592939815 | 56334.2077546296 | 807020010 | 24424.5 | 25000 | 24448.5 | 24424.5 | 0 | 24448.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 23744.7 | 23744.7 | 55999.9 | 0 | PROCESSED | 57610.5627083333 | 56731 | 56365.492662037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070056 | We propose to map the central region (R<20') of the Perseus cluster of galaxies. The cluster is the X-ray brightest one at z=0.02. This unique object along with good performance of the SUZAKU XIS and HXD provides the best quality, wide-band and spatially-resolved X-ray spectroscopy of the ICM. Using the data, we will measure ICM bulk motions around the cluster core. Based on these observation, we will understand the physics of cluster formation and the distribution of dark matter. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAMURA | TAKAYUKI | NULL | NULL | JAP | 7 | AO7 | GAS MOTION IN THE PERSEUS | XIS | Y |
| PERSEUS H_2 | 50.3295 | 41.6532 | 150.73770492 | -12.98651547 | 259.0589 | 56327.8720949074 | 56328.3355092593 | 807021010 | 20345.6 | 20000 | 20363.6 | 20345.6 | 0 | 20353.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21877.6 | 21877.6 | 40034 | 0 | PROCESSED | 57610.5111921296 | 56715 | 56349.4892708333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070056 | We propose to map the central region (R<20') of the Perseus cluster of galaxies. The cluster is the X-ray brightest one at z=0.02. This unique object along with good performance of the SUZAKU XIS and HXD provides the best quality, wide-band and spatially-resolved X-ray spectroscopy of the ICM. Using the data, we will measure ICM bulk motions around the cluster core. Based on these observation, we will understand the physics of cluster formation and the distribution of dark matter. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAMURA | TAKAYUKI | NULL | NULL | JAP | 7 | AO7 | GAS MOTION IN THE PERSEUS | XIS | Y |
| PERSEUS W1_2 | 49.5978 | 41.5445 | 150.3304489 | -13.378921 | 258.3807 | 56328.3362615741 | 56329.0106018518 | 807022010 | 28949.2 | 25000 | 28949.2 | 28973.2 | 0 | 28949.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26275.1 | 26275.1 | 58255.9 | 0 | PROCESSED | 57610.5207523148 | 56715 | 56349.5185648148 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070056 | We propose to map the central region (R<20') of the Perseus cluster of galaxies. The cluster is the X-ray brightest one at z=0.02. This unique object along with good performance of the SUZAKU XIS and HXD provides the best quality, wide-band and spatially-resolved X-ray spectroscopy of the ICM. Using the data, we will measure ICM bulk motions around the cluster core. Based on these observation, we will understand the physics of cluster formation and the distribution of dark matter. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAMURA | TAKAYUKI | NULL | NULL | JAP | 7 | AO7 | GAS MOTION IN THE PERSEUS | XIS | Y |
| PERSEUS G_2 | 50.329 | 41.3745 | 150.89645322 | -13.21839457 | 259.7649 | 56325.9651157407 | 56326.3181828704 | 807023010 | 14244.5 | 15000 | 14244.5 | 14252.5 | 0 | 14252.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20582.2 | 20582.2 | 30483.9 | 0 | PROCESSED | 57610.4949074074 | 56711 | 56345.4909953704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070056 | We propose to map the central region (R<20') of the Perseus cluster of galaxies. The cluster is the X-ray brightest one at z=0.02. This unique object along with good performance of the SUZAKU XIS and HXD provides the best quality, wide-band and spatially-resolved X-ray spectroscopy of the ICM. Using the data, we will measure ICM bulk motions around the cluster core. Based on these observation, we will understand the physics of cluster formation and the distribution of dark matter. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAMURA | TAKAYUKI | NULL | NULL | JAP | 7 | AO7 | GAS MOTION IN THE PERSEUS | XIS | Y |
| A2256N | 256.1941 | 78.9961 | 111.38046428 | 31.59001765 | 219.8042 | 56234.8690625 | 56236.1877083333 | 807024010 | 62285.5 | 60000 | 62285.5 | 62285.5 | 0 | 62285.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 76536.1 | 76536.1 | 113903.9 | 0 | PROCESSED | 57607.9455555556 | 56630 | 56260.5238657407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070058 | We observe outskirts of the famous merging cluster of galaxies A2256 with 4 pointings (60ks for each), and obtain spatial distributions of temperature, electron density, pressure and entropy. In a recent study, the thermal profiles after a merger are thought to be similar to those at cluster formation age. By comparing the spatial distributions of A2256 with those of nearby relaxed clusters, we observationally study the evolution of thermal spatial properties of the ICM in the course of cluster evolution. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KAWAHARADA | MADOKA | NULL | NULL | JAP | 7 | AO7 | THERMAL EVOLUTION OF THE ICM STUDIED WITH A2256 | XIS | Y |
| A2256BKG | 259.0594 | 79.1323 | 111.31764948 | 31.03227987 | 219.8044 | 56236.1893865741 | 56237.0696875 | 807025010 | 39686.5 | 40000 | 39686.5 | 39686.5 | 0 | 39686.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48930.4 | 48930.4 | 76047.9 | 0 | PROCESSED | 57607.9668634259 | 56630 | 56264.5702199074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070058 | We observe outskirts of the famous merging cluster of galaxies A2256 with 4 pointings (60ks for each), and obtain spatial distributions of temperature, electron density, pressure and entropy. In a recent study, the thermal profiles after a merger are thought to be similar to those at cluster formation age. By comparing the spatial distributions of A2256 with those of nearby relaxed clusters, we observationally study the evolution of thermal spatial properties of the ICM in the course of cluster evolution. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | KAWAHARADA | MADOKA | NULL | NULL | JAP | 7 | AO7 | THERMAL EVOLUTION OF THE ICM STUDIED WITH A2256 | XIS | Y |
| A3581_CEN | 211.9083 | -27.0199 | 323.17769244 | 32.83870198 | 117.8993 | 56308.5541782407 | 56310.7078356482 | 807026010 | 80408 | 80000 | 80416 | 80416 | 0 | 80408 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 70171.5 | 70171.5 | 186041.9 | 1 | PROCESSED | 57608.5784259259 | 56711 | 56345.6637384259 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070064 | We propose to study the metallicity of Abell 3581 to the outer region beyond 0.5 r180. Abell 3581 is a very useful system for investigating the history of the chemical evolution of groups and clusters, because the temperature of the intra-cluster medium is about 1.7 keV, which is intermediate between groups and clusters of galaxies. Suzaku will enable us to measure for the first time the metal distributions to such outer regions of the clusters, because of the significantly lower background level and higher sensitivity below ~1 keV. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | SATO | KOSUKE | NULL | NULL | JAP | 7 | AO7 | SEARCH FOR THE METALLICITY OF ABELL 3581 TO THE OUTER REGION BEYOND 0.5 R180 | XIS | Y |
| A2061_1 | 229.9941 | 30.5295 | 47.89500096 | 57.43543483 | 120.6365 | 56306.3817939815 | 56307.4847800926 | 807029010 | 42292.3 | 40000 | 42300.6 | 42299.1 | 0 | 42292.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38183.8 | 38183.8 | 95294 | 0 | PROCESSED | 57608.511087963 | 56703 | 56337.5472222222 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070070 | We propose to conduct multi-pointing observations to cover the entire region of A2061 hosting radio relic. We discovered that the radio relic is located in the cluster outskirts of the opposite side of the filamentary large-scale structure. We found the same trend for 3 relic clusters compiling NVSS radio and SDSS optical data-sets, though the sample number is small. It suggests that an universal process to form radio relic potentially exists. We therefore aim to map out the temperature, density, pressure, and entropy of the intra-cluster medium (ICM) to understand the interplays among the large-scale structure, the ICM and radio relic. Our study provides us a comprehensive picture of the ICM in the radio relic cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | OKABE | NOBUHIRO | NULL | NULL | JAP | 7 | AO7 | SUZAKU OBSERVATION OF THE OUTSKIRTS IN RADIO RELIC CLUSTER A2061 | XIS | Y |
| A2061_2 | 230.6122 | 30.8661 | 48.57175305 | 56.92431824 | 121.1842 | 56307.485625 | 56308.5460185185 | 807030010 | 41788 | 40000 | 41788 | 41788 | 0 | 41788 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37752.9 | 37752.9 | 91601.8 | 1 | PROCESSED | 57608.5263888889 | 56707 | 56338.5482291667 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070070 | We propose to conduct multi-pointing observations to cover the entire region of A2061 hosting radio relic. We discovered that the radio relic is located in the cluster outskirts of the opposite side of the filamentary large-scale structure. We found the same trend for 3 relic clusters compiling NVSS radio and SDSS optical data-sets, though the sample number is small. It suggests that an universal process to form radio relic potentially exists. We therefore aim to map out the temperature, density, pressure, and entropy of the intra-cluster medium (ICM) to understand the interplays among the large-scale structure, the ICM and radio relic. Our study provides us a comprehensive picture of the ICM in the radio relic cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | OKABE | NOBUHIRO | NULL | NULL | JAP | 7 | AO7 | SUZAKU OBSERVATION OF THE OUTSKIRTS IN RADIO RELIC CLUSTER A2061 | XIS | Y |
| ABELL 3395 N | 96.6064 | -54.3394 | 263.07484149 | -25.27687082 | 220.9999 | 56329.4933449074 | 56330.7758564815 | 807031010 | 46975.1 | 45000 | 46980 | 46975.1 | 0 | 46986.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42008.3 | 42008.3 | 110799.8 | 2 | PROCESSED | 57610.5772337963 | 56715 | 56349.5329398148 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070072 | We propose observations of north and south regions of merging cluster Abell 3395 (A3395), which have high temperature intracluster gas, with each exposure time of 45 ks in order to obtain a detailed temperature distribution in these regions. A3395 is a very complex system, which is composed of three subclusters (A3395 NE, SW and NW) and a bridge structure which joining the A3395 NE and NW subclusters. We can obtain the information of the merging direction and the structure formation in A3395 from the detailed high-accuracy temperature distribution. In addition, it might be possible to get from this observations some information of the hot gas filling the supercluster which includes A3395. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TANAKA | NOBUHIRO | NULL | NULL | JAP | 7 | AO7 | INVESTIGATION OF TEMPERATURE DISTRIBUTION OF OUTER REGIONS IN MERGING CLUSTER ABELL 3395 | XIS | Y |
| ABELL 3395 S | 96.923 | -54.6479 | 263.45062321 | -25.16108018 | 230.2008 | 56339.3357060185 | 56340.1778703704 | 807032010 | 47184.9 | 45000 | 47184.9 | 47184.9 | 0 | 47184.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 49750.9 | 49750.9 | 72753.9 | 2 | PROCESSED | 57610.6116898148 | 56717 | 56349.6397569444 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070072 | We propose observations of north and south regions of merging cluster Abell 3395 (A3395), which have high temperature intracluster gas, with each exposure time of 45 ks in order to obtain a detailed temperature distribution in these regions. A3395 is a very complex system, which is composed of three subclusters (A3395 NE, SW and NW) and a bridge structure which joining the A3395 NE and NW subclusters. We can obtain the information of the merging direction and the structure formation in A3395 from the detailed high-accuracy temperature distribution. In addition, it might be possible to get from this observations some information of the hot gas filling the supercluster which includes A3395. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TANAKA | NOBUHIRO | NULL | NULL | JAP | 7 | AO7 | INVESTIGATION OF TEMPERATURE DISTRIBUTION OF OUTER REGIONS IN MERGING CLUSTER ABELL 3395 | XIS | Y |
| A548W | 86.2487 | -25.8437 | 230.35478522 | -25.32458233 | 240.9996 | 56337.0028819444 | 56339.3300462963 | 807033010 | 99370.7 | 100000 | 99370.7 | 99370.7 | 0 | 99370.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 85344.6 | 85344.6 | 201043.7 | 2 | PROCESSED | 57610.6626041667 | 56738 | 56372.6069444445 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070085 | Abell 548 west is a near-by (z=0.0424) poor cluster with an X-ray temperature of 3.4 keV. It has two bright radio relic emission located to the north (Feretti et al. 2006), and a candidate shock-front located near the relics (Solovyeva et al. 2008). The cluster X-ray luminosity is more than an order of magnitude dimmer when plotted in the kT-Lx relation. Combined with its too high galaxy velocity dispersion, we consider this target as a critical merger of two group-sized systems, which is a very rare case in our vicinity. Using Suzaku, we will parametrize the low surface brightness candidate shock region, to identify the temperature jump, which cannot be detected with XMM. We will also investigate the IC emission from the relics to measure the lower limit of its magnetic field. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NAKAZAWA | KAZUHIRO | NULL | NULL | JAP | 7 | AO7 | SUZAKU OBSERVATION OF A MERGING GROUP CANDIDATE ABELL 548 WEST | XIS | Y |
| NGC6946 | 308.6989 | 60.1968 | 95.74917907 | 11.70533663 | 79.9968 | 56060.7040393518 | 56063.8903935185 | 807035010 | 198879 | 200000 | 198879 | 198895.8 | 0 | 198894.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 182195.5 | 182195.5 | 275275.6 | 3 | PROCESSED | 57605.4921296296 | 56442 | 56075.3809027778 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070098 | Hot X-ray emitting interstellar medium (ISM) carries important information about the history of star formation and evolution of galaxies. However, the origin of hot ISM is still unclear. We investigate the property of hot ISM according to luminosity of infrared emission, which is good tracer of star formation rate. If the hot ISM depend on the present activity of star formation, there are correlation between hot ISM and infrared emission. We propose the observation of the spiral galaxy NGC 6946. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | KONAMI | SAORI | NULL | NULL | JAP | 7 | AO7 | CLARIFICATION OF THE ORIGIN OF HOT ISM IN SPIRAL GALAXIES | XIS | Y |
| CIZA J1358.9-4750 | 209.651 | -47.7758 | 314.45332941 | 13.58776424 | 104.5762 | 56313.755 | 56315.4835648148 | 807037010 | 61689.9 | 60000 | 61729.9 | 61689.9 | 0 | 61731 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 58949.7 | 58949.7 | 149331.8 | 1 | PROCESSED | 57608.595162037 | 56718 | 56351.6358680556 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070101 | We propose a Suzaku observation of newly found merging cluster in the Zone of Avoidance, CIZA J1358.9-4750. The cluster has double core, and apparently in an early phase of merging. Targets with this phase is rare. With this observation, we want to obtain the temperature map of the bridge region and identify the existence of heating, to understand the merging phase of this cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | NISHIDA | TERUKAZU | NULL | NULL | JAP | 7 | AO7 | OBSERVATION OF THE NEWLY DISCOVERED MERGING CLUSTER NEAR THE GALACTIC DISC; CIZA J1358.9-4750 | XIS | Y |
| FILAMENT JUNCTION A | 165.6591 | 29.2454 | 201.46002358 | 65.98539565 | 289.5 | 56086.3001041667 | 56088.1238425926 | 807038010 | 69142.8 | 70000 | 69158.8 | 69142.8 | 0 | 69158.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 62299.2 | 62299.2 | 157555.8 | 1 | PROCESSED | 57605.6780787037 | 56543 | 56176.2765046296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070105 | We propose Suzaku observations of three filamentary junctions of galaxies identified in the Sloan Digital Sky Survey spectroscopic data. Because of the strong gravitational potential, it is likely to exist groups or clusters of galaxies with X-ray halo at filamentary junctions. However, there are many filaments where X-ray emission have not been detected. We will search faint X-ray halos are now growing with accreating baryons through shock heating. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | SEKIYA | NORIO | NULL | NULL | JAP | 7 | AO7 | EXPLORING INTERNAL STRUCTURE OF HALOES AT FILAMENTARY JUNCTIONS OF GALAXIES | XIS | Y |
| FILAMENT JUNCTION B | 173.7402 | 21.0892 | 227.90630551 | 71.55824615 | 299.4979 | 56088.1275115741 | 56089.3439814815 | 807039010 | 50106.3 | 50000 | 50118.9 | 50106.3 | 0 | 50126.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 40981.8 | 40981.8 | 105095.9 | 0 | PROCESSED | 57605.6509375 | 56543 | 56176.2814236111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070105 | We propose Suzaku observations of three filamentary junctions of galaxies identified in the Sloan Digital Sky Survey spectroscopic data. Because of the strong gravitational potential, it is likely to exist groups or clusters of galaxies with X-ray halo at filamentary junctions. However, there are many filaments where X-ray emission have not been detected. We will search faint X-ray halos are now growing with accreating baryons through shock heating. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | SEKIYA | NORIO | NULL | NULL | JAP | 7 | AO7 | EXPLORING INTERNAL STRUCTURE OF HALOES AT FILAMENTARY JUNCTIONS OF GALAXIES | XIS | Y |
| CENA LOBE 1 | 201.4716 | -38.9356 | 310.226071 | 23.44775478 | 285.9999 | 56117.7018287037 | 56119.8959953704 | 807040010 | 84161 | 80000 | 84161 | 84161 | 0 | 84161 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 72283.8 | 72283.8 | 188795.5 | 3 | PROCESSED | 57606.6375347222 | 56018 | 56159.3425925926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070106 | Radio source Centaurus A is the closest active galaxy in the Universe (D=3.7 Mpc). It is surrounded by relatively poorly known giant radio lobes extending for about 600 kpc in the N-S direction. Here we propose ambitious Suzaku observations of four carefully selected regions in the Northern giant lobe of target. The primary goal of the project is to study the filamentary structure of the lobe in X-rays, in the broader context of particle acceleration and energy dissipation processes taking place in highly inhomogeneous, magnetized, rarified and multi-phase plasma. We have gathered a larger team of the researches involved in the project to assure a proper analysis of the collected dataset with extensive multi-wavelength support and in-depth theoretical modeling/interpretation. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | STAWARZ | LUKASZ | NULL | NULL | JAP | 7 | AO7 | STUDYING GIANT FILAMENTARY LOBES IN THE CENTAURUS A SYSTEM WITH SUZAKU | XIS | Y |
| CENA LOBE 2 | 201.7887 | -39.7611 | 310.35734609 | 22.59512331 | 290.5003 | 56122.1648958333 | 56122.4584490741 | 807041020 | 12946.3 | 80000 | 12946.3 | 12946.3 | 0 | 12946.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12651.8 | 12651.8 | 25351.9 | 0 | PROCESSED | 57606.6009027778 | 56018 | 56142.1626736111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070106 | Radio source Centaurus A is the closest active galaxy in the Universe (D=3.7 Mpc). It is surrounded by relatively poorly known giant radio lobes extending for about 600 kpc in the N-S direction. Here we propose ambitious Suzaku observations of four carefully selected regions in the Northern giant lobe of target. The primary goal of the project is to study the filamentary structure of the lobe in X-rays, in the broader context of particle acceleration and energy dissipation processes taking place in highly inhomogeneous, magnetized, rarified and multi-phase plasma. We have gathered a larger team of the researches involved in the project to assure a proper analysis of the collected dataset with extensive multi-wavelength support and in-depth theoretical modeling/interpretation. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | STAWARZ | LUKASZ | NULL | NULL | JAP | 7 | AO7 | STUDYING GIANT FILAMENTARY LOBES IN THE CENTAURUS A SYSTEM WITH SUZAKU | XIS | Y |
| CENA LOBE 2 | 201.7888 | -39.7615 | 310.35736359 | 22.59471631 | 296.9216 | 56141.4611921296 | 56143.2779861111 | 807041030 | 65866.6 | 65000 | 65874.6 | 65874.6 | 0 | 65866.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 57865.9 | 57865.9 | 156953.8 | 2 | PROCESSED | 57606.7677893518 | 56018 | 56162.2467013889 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070106 | Radio source Centaurus A is the closest active galaxy in the Universe (D=3.7 Mpc). It is surrounded by relatively poorly known giant radio lobes extending for about 600 kpc in the N-S direction. Here we propose ambitious Suzaku observations of four carefully selected regions in the Northern giant lobe of target. The primary goal of the project is to study the filamentary structure of the lobe in X-rays, in the broader context of particle acceleration and energy dissipation processes taking place in highly inhomogeneous, magnetized, rarified and multi-phase plasma. We have gathered a larger team of the researches involved in the project to assure a proper analysis of the collected dataset with extensive multi-wavelength support and in-depth theoretical modeling/interpretation. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | STAWARZ | LUKASZ | NULL | NULL | JAP | 7 | AO7 | STUDYING GIANT FILAMENTARY LOBES IN THE CENTAURUS A SYSTEM WITH SUZAKU | XIS | Y |
| CENA LOBE BGD1 | 205.3783 | -39.3349 | 313.38854271 | 22.51794697 | 286.0001 | 56122.4603125 | 56123.1043634259 | 807042010 | 22245.5 | 20000 | 22245.5 | 22245.5 | 0 | 22245.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18855.6 | 18855.6 | 55616 | 1 | PROCESSED | 57606.6151157407 | 56018 | 56142.2381597222 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070106 | Radio source Centaurus A is the closest active galaxy in the Universe (D=3.7 Mpc). It is surrounded by relatively poorly known giant radio lobes extending for about 600 kpc in the N-S direction. Here we propose ambitious Suzaku observations of four carefully selected regions in the Northern giant lobe of target. The primary goal of the project is to study the filamentary structure of the lobe in X-rays, in the broader context of particle acceleration and energy dissipation processes taking place in highly inhomogeneous, magnetized, rarified and multi-phase plasma. We have gathered a larger team of the researches involved in the project to assure a proper analysis of the collected dataset with extensive multi-wavelength support and in-depth theoretical modeling/interpretation. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | STAWARZ | LUKASZ | NULL | NULL | JAP | 7 | AO7 | STUDYING GIANT FILAMENTARY LOBES IN THE CENTAURUS A SYSTEM WITH SUZAKU | XIS | Y |
| CENA LOBE BGD2 | 197.06 | -39.3239 | 306.47248435 | 23.43231323 | 291.4078 | 56123.1069212963 | 56123.5835300926 | 807043010 | 21277.2 | 20000 | 21277.2 | 21277.2 | 0 | 21277.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 19472.9 | 19472.9 | 41167.9 | 0 | PROCESSED | 57606.6117476852 | 56018 | 56142.2269675926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070106 | Radio source Centaurus A is the closest active galaxy in the Universe (D=3.7 Mpc). It is surrounded by relatively poorly known giant radio lobes extending for about 600 kpc in the N-S direction. Here we propose ambitious Suzaku observations of four carefully selected regions in the Northern giant lobe of target. The primary goal of the project is to study the filamentary structure of the lobe in X-rays, in the broader context of particle acceleration and energy dissipation processes taking place in highly inhomogeneous, magnetized, rarified and multi-phase plasma. We have gathered a larger team of the researches involved in the project to assure a proper analysis of the collected dataset with extensive multi-wavelength support and in-depth theoretical modeling/interpretation. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | STAWARZ | LUKASZ | NULL | NULL | JAP | 7 | AO7 | STUDYING GIANT FILAMENTARY LOBES IN THE CENTAURUS A SYSTEM WITH SUZAKU | XIS | Y |
| DDO 120 | 185.3167 | 45.8198 | 138.73502996 | 70.37152611 | 129.0479 | 56256.0169444444 | 56258.4271990741 | 807044010 | 101741.4 | 100000 | 101741.4 | 101741.4 | 0 | 101741.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 91086.4 | 91086.4 | 208183.9 | 0 | PROCESSED | 57608.1579861111 | 56644 | 56275.7410648148 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070107 | We propose to observe an irregular dwarf galaxy DDO120 to detect a hot interstellar medium associated with the dwarf galaxy. The study of the temperature and density of the gas will give us important information about the pollution of the intergalactic medium from galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | YAMAMOTO | RYO | NULL | NULL | JAP | 7 | AO7 | SEARCH FOR HOT INTERSTELLAR MEDIUM OF AN IRREGULAR DWARF GALAXY DDO 120 | XIS | Y |
| SEGUE 1 | 151.7658 | 16.0862 | 220.47149585 | 50.42674703 | 110.8027 | 56248.0740625 | 56250.3182291667 | 807046010 | 85439.1 | 85000 | 85462.2 | 85443.1 | 0 | 85439.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 77564.5 | 77564.5 | 193841.9 | 4 | PROCESSED | 57608.0603240741 | 56641 | 56275.5584490741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071502 | Our ongoing dedicated X-ray search for dark matter targeting dwarf spheroidal galaxies set new constraints on the mass and mixing angle of the sterile neutrino -- a plausible dark matter candidate that emits an X-ray via radiative decay. We have proposed a new well-motivated candidate -- moduli dark matter, that also produces a detectable X-ray line. We propose Suzaku observations of the Segue 1 dwarf spheroidal -- the most dark matter dominated galaxy known. Its extreme nature implies that it provides the tightest constraints on sterile neutrino and moduli parameters in the event of a detection, and best limits in the absence of one. The resulting spectrum is optimal for exploring new physics, such as string theory compactification or supersymmetry breaking, and as a legacy for Astro-H. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | LOEWENSTEIN | MICHAEL | NULL | NULL | USA | 7 | AO7 | SEARCH FOR DARK MATTER WITH SUZAKU OBSERVATIONS OF THE MOST DARK MATTER DOMINATED GALAXY IN THE UNIVERSE | XIS | Y |
| NGC 7796 | 359.7407 | -55.4558 | 317.90399943 | -60.12089491 | 60.4505 | 56078.2927430556 | 56080.5001851852 | 807047010 | 161613.6 | 150000 | 161621.6 | 161621.6 | 0 | 161613.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 134043.2 | 134043.2 | 190711.8 | 0 | PROCESSED | 57605.6269328704 | 56018 | 56090.2424537037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071503 | The mass profiles of elliptical galaxies are important probes of galaxy formation and cosmology. Only a few elliptical galaxies have detailed mass measurements from X-rays because of the lack of suitable targets in terms of total mass (< ~10^{13} m_sun) and relaxed dynamical states appropriate for hydrostatic analysis. We have identified a sample of (hot) gas-rich isolated elliptical galaxies, most of which were discovered from previously awarded XMM and Chandra snapshot programs to search for optimal targets for X-ray studies of mass profiles on the galaxy scale. We request Suzaku observations to map the detailed profiles of stars, dark matter, and hot gas in two of these galaxies which have (scheduled) complementary Chandra observations. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | BUOTE | DAVID | NULL | NULL | USA | 7 | AO7 | THE MASS PROFILES OF ISOLATED ELLIPTICAL GALAXIES | XIS | Y |
| IC 5157 | 330.8663 | -34.934 | 10.02196464 | -53.45455848 | 251.1985 | 56250.3323611111 | 56251.6043287037 | 807048010 | 65541.1 | 150000 | 65541.1 | 65541.1 | 0 | 65541.1 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 67764 | 67764 | 109886.1 | 1 | PROCESSED | 57608.0722222222 | 56018 | 56275.5333333333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071503 | The mass profiles of elliptical galaxies are important probes of galaxy formation and cosmology. Only a few elliptical galaxies have detailed mass measurements from X-rays because of the lack of suitable targets in terms of total mass (< ~10^{13} m_sun) and relaxed dynamical states appropriate for hydrostatic analysis. We have identified a sample of (hot) gas-rich isolated elliptical galaxies, most of which were discovered from previously awarded XMM and Chandra snapshot programs to search for optimal targets for X-ray studies of mass profiles on the galaxy scale. We request Suzaku observations to map the detailed profiles of stars, dark matter, and hot gas in two of these galaxies which have (scheduled) complementary Chandra observations. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | BUOTE | DAVID | NULL | NULL | USA | 7 | AO7 | THE MASS PROFILES OF ISOLATED ELLIPTICAL GALAXIES | XIS | Y |
| FG25 | 234.9579 | 30.7058 | 48.772653 | 53.18955534 | 294.6599 | 56136.7541898148 | 56137.0821875 | 807049010 | 10639.3 | 10000 | 10639.3 | 10639.3 | 0 | 10639.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11074 | 11074 | 28328.1 | 0 | PROCESSED | 57606.6807523148 | 56527 | 56161.2376736111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071511 | Optical and X-ray measurements of fossil groups/clusters (FGs) suggest that they are old and relaxed systems. If FGs are assembled at higher redshift, there is enough time for intermediate-luminosity galaxies to merge, resulting in the formation of the brightest system galaxy. We carry out the first, systematic study of a large sample of FGs, the ``FOssil Group Origins'' (FOGO) based on an International Time Project at the Roque de los Muchachos Observatory. For ten FOGO FGs we propose to measure the temperature of the hot intracluster gas (ICM) and to evaluate Lx-Tx, Lopt-Tx, and sigmaV-Tx relations as compared to the non fossil systems. By combining these observations with hydrodynamical simulations we will open a new window into the study of the ICM and the nature of fossil systems. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | D'ONGHIA | ELENA | NULL | NULL | USA | 7 | AO7 | SCALING RELATIONS OF FOSSIL GALAXY SYSTEMS | XIS | Y |
| FG09 | 160.7604 | 0.8965 | 247.95154277 | 49.5505044 | 288.8833 | 56077.2212731482 | 56077.5397337963 | 807050010 | 12490 | 10000 | 12494.4 | 12490 | 0 | 12500 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10850.6 | 10850.6 | 27511.9 | 0 | PROCESSED | 57605.5584722222 | 56462 | 56096.107662037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071511 | Optical and X-ray measurements of fossil groups/clusters (FGs) suggest that they are old and relaxed systems. If FGs are assembled at higher redshift, there is enough time for intermediate-luminosity galaxies to merge, resulting in the formation of the brightest system galaxy. We carry out the first, systematic study of a large sample of FGs, the ``FOssil Group Origins'' (FOGO) based on an International Time Project at the Roque de los Muchachos Observatory. For ten FOGO FGs we propose to measure the temperature of the hot intracluster gas (ICM) and to evaluate Lx-Tx, Lopt-Tx, and sigmaV-Tx relations as compared to the non fossil systems. By combining these observations with hydrodynamical simulations we will open a new window into the study of the ICM and the nature of fossil systems. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | D'ONGHIA | ELENA | NULL | NULL | USA | 7 | AO7 | SCALING RELATIONS OF FOSSIL GALAXY SYSTEMS | XIS | Y |
| FG30 | 259.5133 | 56.677 | 84.88085465 | 35.08331599 | 38.7622 | 56049.4885532407 | 56049.7980671296 | 807051010 | 13978.7 | 10000 | 13986.7 | 13994.7 | 0 | 13978.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15579 | 15579 | 26725.9 | 0 | PROCESSED | 57605.3190856482 | 56465 | 56099.2218171296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071511 | Optical and X-ray measurements of fossil groups/clusters (FGs) suggest that they are old and relaxed systems. If FGs are assembled at higher redshift, there is enough time for intermediate-luminosity galaxies to merge, resulting in the formation of the brightest system galaxy. We carry out the first, systematic study of a large sample of FGs, the ``FOssil Group Origins'' (FOGO) based on an International Time Project at the Roque de los Muchachos Observatory. For ten FOGO FGs we propose to measure the temperature of the hot intracluster gas (ICM) and to evaluate Lx-Tx, Lopt-Tx, and sigmaV-Tx relations as compared to the non fossil systems. By combining these observations with hydrodynamical simulations we will open a new window into the study of the ICM and the nature of fossil systems. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | D'ONGHIA | ELENA | NULL | NULL | USA | 7 | AO7 | SCALING RELATIONS OF FOSSIL GALAXY SYSTEMS | XIS | Y |
| FG03 | 118.182 | 45.9572 | 173.26592635 | 29.42392711 | 92.9981 | 56228.7772453704 | 56229.1078819444 | 807052010 | 14318.5 | 10000 | 14326.5 | 14318.5 | 0 | 14334.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15365 | 15365 | 28544 | 0 | PROCESSED | 57607.868125 | 56696 | 56330.5013541667 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071511 | Optical and X-ray measurements of fossil groups/clusters (FGs) suggest that they are old and relaxed systems. If FGs are assembled at higher redshift, there is enough time for intermediate-luminosity galaxies to merge, resulting in the formation of the brightest system galaxy. We carry out the first, systematic study of a large sample of FGs, the ``FOssil Group Origins'' (FOGO) based on an International Time Project at the Roque de los Muchachos Observatory. For ten FOGO FGs we propose to measure the temperature of the hot intracluster gas (ICM) and to evaluate Lx-Tx, Lopt-Tx, and sigmaV-Tx relations as compared to the non fossil systems. By combining these observations with hydrodynamical simulations we will open a new window into the study of the ICM and the nature of fossil systems. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | D'ONGHIA | ELENA | NULL | NULL | USA | 7 | AO7 | SCALING RELATIONS OF FOSSIL GALAXY SYSTEMS | XIS | Y |
| FG04 | 121.8798 | 33.9978 | 187.39667673 | 29.69857824 | 274.999 | 56053.6835648148 | 56053.9411921296 | 807053010 | 10821 | 10000 | 10821 | 10821 | 0 | 10821 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11076.6 | 11076.6 | 22255.9 | 0 | PROCESSED | 57605.3537268518 | 56435 | 56068.6337152778 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071511 | Optical and X-ray measurements of fossil groups/clusters (FGs) suggest that they are old and relaxed systems. If FGs are assembled at higher redshift, there is enough time for intermediate-luminosity galaxies to merge, resulting in the formation of the brightest system galaxy. We carry out the first, systematic study of a large sample of FGs, the ``FOssil Group Origins'' (FOGO) based on an International Time Project at the Roque de los Muchachos Observatory. For ten FOGO FGs we propose to measure the temperature of the hot intracluster gas (ICM) and to evaluate Lx-Tx, Lopt-Tx, and sigmaV-Tx relations as compared to the non fossil systems. By combining these observations with hydrodynamical simulations we will open a new window into the study of the ICM and the nature of fossil systems. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | D'ONGHIA | ELENA | NULL | NULL | USA | 7 | AO7 | SCALING RELATIONS OF FOSSIL GALAXY SYSTEMS | XIS | Y |
| FG26 | 237.2323 | 8.8441 | 17.92603672 | 44.32356312 | 282.0742 | 56137.0874305556 | 56137.3307986111 | 807054010 | 11891.2 | 10000 | 11891.2 | 11891.2 | 0 | 11891.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8598.3 | 8598.3 | 20999.9 | 0 | PROCESSED | 57606.6870023148 | 56626 | 56260.480474537 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071511 | Optical and X-ray measurements of fossil groups/clusters (FGs) suggest that they are old and relaxed systems. If FGs are assembled at higher redshift, there is enough time for intermediate-luminosity galaxies to merge, resulting in the formation of the brightest system galaxy. We carry out the first, systematic study of a large sample of FGs, the ``FOssil Group Origins'' (FOGO) based on an International Time Project at the Roque de los Muchachos Observatory. For ten FOGO FGs we propose to measure the temperature of the hot intracluster gas (ICM) and to evaluate Lx-Tx, Lopt-Tx, and sigmaV-Tx relations as compared to the non fossil systems. By combining these observations with hydrodynamical simulations we will open a new window into the study of the ICM and the nature of fossil systems. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | D'ONGHIA | ELENA | NULL | NULL | USA | 7 | AO7 | SCALING RELATIONS OF FOSSIL GALAXY SYSTEMS | XIS | Y |
| FG14 | 176.6962 | 9.8632 | 258.4262435 | 66.96745764 | 295.6185 | 56076.7125925926 | 56077.2168171296 | 807055010 | 12492.6 | 10000 | 12500.6 | 12495 | 0 | 12492.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13535 | 13535 | 43553.9 | 1 | PROCESSED | 57605.5555671296 | 56452 | 56086.1554861111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071511 | Optical and X-ray measurements of fossil groups/clusters (FGs) suggest that they are old and relaxed systems. If FGs are assembled at higher redshift, there is enough time for intermediate-luminosity galaxies to merge, resulting in the formation of the brightest system galaxy. We carry out the first, systematic study of a large sample of FGs, the ``FOssil Group Origins'' (FOGO) based on an International Time Project at the Roque de los Muchachos Observatory. For ten FOGO FGs we propose to measure the temperature of the hot intracluster gas (ICM) and to evaluate Lx-Tx, Lopt-Tx, and sigmaV-Tx relations as compared to the non fossil systems. By combining these observations with hydrodynamical simulations we will open a new window into the study of the ICM and the nature of fossil systems. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | D'ONGHIA | ELENA | NULL | NULL | USA | 7 | AO7 | SCALING RELATIONS OF FOSSIL GALAXY SYSTEMS | XIS | Y |
| FG27 | 243.6269 | 26.7212 | 44.57695273 | 45.05698279 | 293.3995 | 56144.3018055556 | 56144.5557638889 | 807056010 | 11219.4 | 15000 | 11235 | 11219.4 | 0 | 11235 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10911.4 | 10911.4 | 21935.9 | 1 | PROCESSED | 57606.7546643518 | 56533 | 56167.1527893518 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071511 | Optical and X-ray measurements of fossil groups/clusters (FGs) suggest that they are old and relaxed systems. If FGs are assembled at higher redshift, there is enough time for intermediate-luminosity galaxies to merge, resulting in the formation of the brightest system galaxy. We carry out the first, systematic study of a large sample of FGs, the ``FOssil Group Origins'' (FOGO) based on an International Time Project at the Roque de los Muchachos Observatory. For ten FOGO FGs we propose to measure the temperature of the hot intracluster gas (ICM) and to evaluate Lx-Tx, Lopt-Tx, and sigmaV-Tx relations as compared to the non fossil systems. By combining these observations with hydrodynamical simulations we will open a new window into the study of the ICM and the nature of fossil systems. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | D'ONGHIA | ELENA | NULL | NULL | USA | 7 | AO7 | SCALING RELATIONS OF FOSSIL GALAXY SYSTEMS | XIS | Y |
| FG15 | 177.008 | 56.8964 | 139.35969999 | 58.16359998 | 300.5727 | 56073.7490856482 | 56074.0586226852 | 807057010 | 14075.7 | 15000 | 14075.7 | 14075.7 | 0 | 14075.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15603 | 15603 | 26739.9 | 1 | PROCESSED | 57605.5125578704 | 56470 | 56103.1467013889 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071511 | Optical and X-ray measurements of fossil groups/clusters (FGs) suggest that they are old and relaxed systems. If FGs are assembled at higher redshift, there is enough time for intermediate-luminosity galaxies to merge, resulting in the formation of the brightest system galaxy. We carry out the first, systematic study of a large sample of FGs, the ``FOssil Group Origins'' (FOGO) based on an International Time Project at the Roque de los Muchachos Observatory. For ten FOGO FGs we propose to measure the temperature of the hot intracluster gas (ICM) and to evaluate Lx-Tx, Lopt-Tx, and sigmaV-Tx relations as compared to the non fossil systems. By combining these observations with hydrodynamical simulations we will open a new window into the study of the ICM and the nature of fossil systems. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | D'ONGHIA | ELENA | NULL | NULL | USA | 7 | AO7 | SCALING RELATIONS OF FOSSIL GALAXY SYSTEMS | XIS | Y |
| FG24 | 233.4334 | 3.6096 | 8.88650115 | 44.69822064 | 290.4245 | 56136.3403935185 | 56136.7487152778 | 807058010 | 15823.1 | 15000 | 15823.1 | 15823.1 | 0 | 15823.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13191 | 13191 | 35275.9 | 0 | PROCESSED | 57606.6653819444 | 56527 | 56161.2328240741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071511 | Optical and X-ray measurements of fossil groups/clusters (FGs) suggest that they are old and relaxed systems. If FGs are assembled at higher redshift, there is enough time for intermediate-luminosity galaxies to merge, resulting in the formation of the brightest system galaxy. We carry out the first, systematic study of a large sample of FGs, the ``FOssil Group Origins'' (FOGO) based on an International Time Project at the Roque de los Muchachos Observatory. For ten FOGO FGs we propose to measure the temperature of the hot intracluster gas (ICM) and to evaluate Lx-Tx, Lopt-Tx, and sigmaV-Tx relations as compared to the non fossil systems. By combining these observations with hydrodynamical simulations we will open a new window into the study of the ICM and the nature of fossil systems. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | D'ONGHIA | ELENA | NULL | NULL | USA | 7 | AO7 | SCALING RELATIONS OF FOSSIL GALAXY SYSTEMS | XIS | Y |
| SDSS J0906+0301 | 136.6571 | 3.0284 | 226.89088068 | 31.22930355 | 109.9836 | 56253.2318981482 | 56253.846099537 | 807059010 | 21714.8 | 20000 | 21722.8 | 21714.8 | 0 | 21722.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20632 | 20632 | 53066 | 0 | PROCESSED | 57608.0815972222 | 56702 | 56336.4694328704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071512 | Fossil groups (FGs) are systems dominated by a single large galaxy with a cluster-scale X-ray halo. They are thought to be old, isolated galaxy groups in which the large galaxies have coalesced through dynamical friction, but recent studies reveal a more complicated picture. We propose Suzaku observations of 5 optically selected FG candidates. These targets will extend our previous survey, which identified 12 FGs; when combined with 5 FG candidates approved for the current Chandra cycle, this will create the largest uniformly-selected sample of real FGs. The L_X and T_X measured will be used with optical spectroscopy to extend FG scaling relations to low mass, and to plan deeper X-ray spectroscopic follow-up to constrain the formation epoch and evolution of these puzzling systems. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MILLER | ERIC | NULL | NULL | USA | 7 | AO7 | FINDING FOSSIL GROUPS WITH SUZAKU | XIS | Y |
| SDSS J1302+4729 | 195.5068 | 47.4831 | 117.80880843 | 69.53967787 | 316.2365 | 56076.2710648148 | 56076.7058217593 | 807060010 | 20427 | 20000 | 20427 | 20427 | 0 | 20427 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 24660 | 24660 | 37559.9 | 1 | PROCESSED | 57605.5578240741 | 56500 | 56134.0735300926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071512 | Fossil groups (FGs) are systems dominated by a single large galaxy with a cluster-scale X-ray halo. They are thought to be old, isolated galaxy groups in which the large galaxies have coalesced through dynamical friction, but recent studies reveal a more complicated picture. We propose Suzaku observations of 5 optically selected FG candidates. These targets will extend our previous survey, which identified 12 FGs; when combined with 5 FG candidates approved for the current Chandra cycle, this will create the largest uniformly-selected sample of real FGs. The L_X and T_X measured will be used with optical spectroscopy to extend FG scaling relations to low mass, and to plan deeper X-ray spectroscopic follow-up to constrain the formation epoch and evolution of these puzzling systems. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MILLER | ERIC | NULL | NULL | USA | 7 | AO7 | FINDING FOSSIL GROUPS WITH SUZAKU | XIS | Y |
| SDSS J0837+4414 | 129.4975 | 44.2566 | 176.37698799 | 37.1577345 | 110.1912 | 56213.8277083333 | 56214.3515393518 | 807061010 | 20621.9 | 20000 | 20621.9 | 20621.9 | 0 | 20621.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 20958 | 20958 | 45239.9 | 0 | PROCESSED | 57607.7583796296 | 56598 | 56232.4985185185 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071512 | Fossil groups (FGs) are systems dominated by a single large galaxy with a cluster-scale X-ray halo. They are thought to be old, isolated galaxy groups in which the large galaxies have coalesced through dynamical friction, but recent studies reveal a more complicated picture. We propose Suzaku observations of 5 optically selected FG candidates. These targets will extend our previous survey, which identified 12 FGs; when combined with 5 FG candidates approved for the current Chandra cycle, this will create the largest uniformly-selected sample of real FGs. The L_X and T_X measured will be used with optical spectroscopy to extend FG scaling relations to low mass, and to plan deeper X-ray spectroscopic follow-up to constrain the formation epoch and evolution of these puzzling systems. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MILLER | ERIC | NULL | NULL | USA | 7 | AO7 | FINDING FOSSIL GROUPS WITH SUZAKU | XIS | Y |
| SDSS J1431+0047 | 217.7608 | 0.788 | 349.30444711 | 54.43383912 | 287.7594 | 56140.9857291667 | 56141.454375 | 807062010 | 22355.3 | 20000 | 22371 | 22355.3 | 0 | 22363 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16580.9 | 16580.9 | 40479.9 | 1 | PROCESSED | 57606.7190740741 | 56528 | 56162.1265972222 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071512 | Fossil groups (FGs) are systems dominated by a single large galaxy with a cluster-scale X-ray halo. They are thought to be old, isolated galaxy groups in which the large galaxies have coalesced through dynamical friction, but recent studies reveal a more complicated picture. We propose Suzaku observations of 5 optically selected FG candidates. These targets will extend our previous survey, which identified 12 FGs; when combined with 5 FG candidates approved for the current Chandra cycle, this will create the largest uniformly-selected sample of real FGs. The L_X and T_X measured will be used with optical spectroscopy to extend FG scaling relations to low mass, and to plan deeper X-ray spectroscopic follow-up to constrain the formation epoch and evolution of these puzzling systems. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MILLER | ERIC | NULL | NULL | USA | 7 | AO7 | FINDING FOSSIL GROUPS WITH SUZAKU | XIS | Y |
| SDSS J0854+3524 | 133.7386 | 35.4192 | 188.0033984 | 39.53150085 | 111.2842 | 56214.3546527778 | 56214.8244560185 | 807063010 | 20614.8 | 20000 | 20614.8 | 20614.8 | 0 | 20614.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 18084 | 18084 | 40560 | 0 | PROCESSED | 57607.7601157407 | 56598 | 56232.4365856482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071512 | Fossil groups (FGs) are systems dominated by a single large galaxy with a cluster-scale X-ray halo. They are thought to be old, isolated galaxy groups in which the large galaxies have coalesced through dynamical friction, but recent studies reveal a more complicated picture. We propose Suzaku observations of 5 optically selected FG candidates. These targets will extend our previous survey, which identified 12 FGs; when combined with 5 FG candidates approved for the current Chandra cycle, this will create the largest uniformly-selected sample of real FGs. The L_X and T_X measured will be used with optical spectroscopy to extend FG scaling relations to low mass, and to plan deeper X-ray spectroscopic follow-up to constrain the formation epoch and evolution of these puzzling systems. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MILLER | ERIC | NULL | NULL | USA | 7 | AO7 | FINDING FOSSIL GROUPS WITH SUZAKU | XIS | Y |
| RXJ1159+5531 | 179.9637 | 55.4123 | 137.70641489 | 60.21165624 | 302.8269 | 56074.0600694445 | 56075.6800578704 | 807064010 | 82233.9 | 100000 | 82241.9 | 82241.9 | 0 | 82233.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 98601.1 | 98601.1 | 139964 | 1 | PROCESSED | 57605.5596875 | 56657 | 56086.0194328704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071513 | With Chandra and Suzaku we recently constrained the hot gas and dark matter out to the virial radius (rvir=R108) in the fossil group/cluster RXJ1159+5531. Unlike some recent observations of cluster outskirts, the gas fraction is consistent with the cosmic value, and the entropy profile at rvir is consistent with gravity-only structure formation simulations. As a fossil group, RXJ1159+5531 may be unusually relaxed at large scales. If so, the gas properties should not vary much azimuthally. We propose a complementary Suzaku observation to explore this by measuring the gas in a different azimuthal region, more than doubling the current (~27%) azimuthal coverage. Our results will help determine if gas clumping, invoked to explain the outskirts of some clusters, is ubiquitous. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | HUMPHREY | PHILIP | NULL | NULL | USA | 7 | AO7 | RELAXED GAS AT THE VIRIAL RADIUS IN A FOSSIL GROUP | XIS | Y |
| RXJ1159+5531 | 179.9812 | 55.4402 | 137.66567163 | 60.1900448 | 115.1582 | 56268.8799768518 | 56269.4140162037 | 807064020 | 21143.2 | 20000 | 21143.2 | 21151.2 | 0 | 21151.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22600.1 | 22600.1 | 46140 | 0 | PROCESSED | 57608.2013310185 | 56646 | 56279.6625925926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071513 | With Chandra and Suzaku we recently constrained the hot gas and dark matter out to the virial radius (rvir=R108) in the fossil group/cluster RXJ1159+5531. Unlike some recent observations of cluster outskirts, the gas fraction is consistent with the cosmic value, and the entropy profile at rvir is consistent with gravity-only structure formation simulations. As a fossil group, RXJ1159+5531 may be unusually relaxed at large scales. If so, the gas properties should not vary much azimuthally. We propose a complementary Suzaku observation to explore this by measuring the gas in a different azimuthal region, more than doubling the current (~27%) azimuthal coverage. Our results will help determine if gas clumping, invoked to explain the outskirts of some clusters, is ubiquitous. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | HUMPHREY | PHILIP | NULL | NULL | USA | 7 | AO7 | RELAXED GAS AT THE VIRIAL RADIUS IN A FOSSIL GROUP | XIS | Y |
| RXJ1416.4+2315 | 214.0475 | 23.1701 | 25.95045598 | 70.44211392 | 293.1172 | 56123.5919675926 | 56124.3335300926 | 807065010 | 23719.2 | 120000 | 23727.2 | 23719.2 | 0 | 23727.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 22602.8 | 22602.8 | 64063.9 | 1 | PROCESSED | 57606.624537037 | 56598 | 56144.9996180556 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071514 | Our study of the fossil group RXJ 1159+5531 does not find the gas clumping invoked to explain unexpectedly flat entropy profiles and large gas fractions near r_vir in some clusters. Instead its ICM properties at r_vir are consistent with adiabatic cluster formation, which may reflect that hydrostatic equilibrium is very accurate in this highly evolved fossil group. To examine whether these results extend to other fossils and to more massive systems, we propose to observe the fossil cluster RXJ 1416.4+2315 (M_vir ~3 x 10^14 M_sun) to constrain its entropy and gas fraction out to r_vir (r_112). Since it is located at a redshift of 0.137, this target provides an efficient means to explore the outer ICM, where a large azimuthal portion (~80%) of r_vir can be observed in a single Suzaku field. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | BUOTE | DAVID | NULL | NULL | USA | 7 | AO7 | RXJ1416.4+2315: A MASSIVE FOSSIL CLUSTER | XIS | Y |
| RXJ1416.4+2315 | 214.0491 | 23.1704 | 25.95253376 | 70.44078356 | 293.1179 | 56125.9101736111 | 56128.5008796296 | 807065020 | 101693.8 | 100000 | 101701.8 | 101693.8 | 0 | 101701.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 99676.3 | 99676.3 | 223820.9 | 2 | PROCESSED | 57606.7012037037 | 56598 | 56232.6190740741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071514 | Our study of the fossil group RXJ 1159+5531 does not find the gas clumping invoked to explain unexpectedly flat entropy profiles and large gas fractions near r_vir in some clusters. Instead its ICM properties at r_vir are consistent with adiabatic cluster formation, which may reflect that hydrostatic equilibrium is very accurate in this highly evolved fossil group. To examine whether these results extend to other fossils and to more massive systems, we propose to observe the fossil cluster RXJ 1416.4+2315 (M_vir ~3 x 10^14 M_sun) to constrain its entropy and gas fraction out to r_vir (r_112). Since it is located at a redshift of 0.137, this target provides an efficient means to explore the outer ICM, where a large azimuthal portion (~80%) of r_vir can be observed in a single Suzaku field. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | BUOTE | DAVID | NULL | NULL | USA | 7 | AO7 | RXJ1416.4+2315: A MASSIVE FOSSIL CLUSTER | XIS | Y |
| ANTLIA E1 | 157.8782 | -35.3295 | 273.21530285 | 19.3432713 | 277.4995 | 56091.5629398148 | 56092.2633912037 | 807066010 | 25747 | 23000 | 25755 | 25747 | 0 | 25755 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22929.1 | 22929.1 | 60513.9 | 1 | PROCESSED | 57605.6597106482 | 56473 | 56107.272650463 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071521 | We propose to carry out mosaic observations (204 ks total) of the Antlia cluster, the third closest galaxy cluster highly ignored in X-ray, out to R200. It is the nearest non-cool core cluster with a similar low temperature as the cool core Virgo Cluster, allowing us to make a direct comparison to the cool core counterpart in our neighborhood. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will test models for clumping, electron-ion equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | WONG | KA-WAH | NULL | NULL | USA | 7 | AO7 | MAPPING THE NEAREST NON-COOL CORE CLUSTER OUT TO R200 | XIS | Y |
| ANTLIA E2 | 158.2496 | -35.3292 | 273.48585529 | 19.50669913 | 277.9997 | 56092.2642361111 | 56093.0181944444 | 807067010 | 24174.1 | 23000 | 24182.1 | 24174.1 | 0 | 24190.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22853.4 | 22853.4 | 65135.9 | 3 | PROCESSED | 57605.6727546296 | 56476 | 56110.5259027778 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071521 | We propose to carry out mosaic observations (204 ks total) of the Antlia cluster, the third closest galaxy cluster highly ignored in X-ray, out to R200. It is the nearest non-cool core cluster with a similar low temperature as the cool core Virgo Cluster, allowing us to make a direct comparison to the cool core counterpart in our neighborhood. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will test models for clumping, electron-ion equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | WONG | KA-WAH | NULL | NULL | USA | 7 | AO7 | MAPPING THE NEAREST NON-COOL CORE CLUSTER OUT TO R200 | XIS | Y |
| ANTLIA E3 | 158.6143 | -35.3303 | 273.75347644 | 19.66467309 | 278.5008 | 56093.5404166667 | 56094.1877546296 | 807068010 | 23486.1 | 23000 | 23502.1 | 23486.1 | 0 | 23502.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20686.2 | 20686.2 | 55926 | 1 | PROCESSED | 57605.6943287037 | 56476 | 56110.5216550926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071521 | We propose to carry out mosaic observations (204 ks total) of the Antlia cluster, the third closest galaxy cluster highly ignored in X-ray, out to R200. It is the nearest non-cool core cluster with a similar low temperature as the cool core Virgo Cluster, allowing us to make a direct comparison to the cool core counterpart in our neighborhood. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will test models for clumping, electron-ion equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | WONG | KA-WAH | NULL | NULL | USA | 7 | AO7 | MAPPING THE NEAREST NON-COOL CORE CLUSTER OUT TO R200 | XIS | Y |
| ANTLIA E4 | 158.9815 | -35.3293 | 274.02289995 | 19.82417732 | 279.0004 | 56094.1885532407 | 56095.3688888889 | 807069010 | 46503.1 | 45000 | 46503.1 | 46519.5 | 0 | 46511.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38618.5 | 38618.5 | 101969.9 | 0 | PROCESSED | 57605.7108564815 | 56477 | 56111.0445023148 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071521 | We propose to carry out mosaic observations (204 ks total) of the Antlia cluster, the third closest galaxy cluster highly ignored in X-ray, out to R200. It is the nearest non-cool core cluster with a similar low temperature as the cool core Virgo Cluster, allowing us to make a direct comparison to the cool core counterpart in our neighborhood. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will test models for clumping, electron-ion equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | WONG | KA-WAH | NULL | NULL | USA | 7 | AO7 | MAPPING THE NEAREST NON-COOL CORE CLUSTER OUT TO R200 | XIS | Y |
| ANTLIA E5 | 159.3469 | -35.3315 | 274.29394045 | 19.97884062 | 279.4997 | 56095.3697337963 | 56096.5972916667 | 807070010 | 46781.4 | 45000 | 46789.4 | 46781.4 | 0 | 46797.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41061.7 | 41061.7 | 106057.9 | 2 | PROCESSED | 57605.7158333333 | 56590 | 56219.6892361111 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071521 | We propose to carry out mosaic observations (204 ks total) of the Antlia cluster, the third closest galaxy cluster highly ignored in X-ray, out to R200. It is the nearest non-cool core cluster with a similar low temperature as the cool core Virgo Cluster, allowing us to make a direct comparison to the cool core counterpart in our neighborhood. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will test models for clumping, electron-ion equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | WONG | KA-WAH | NULL | NULL | USA | 7 | AO7 | MAPPING THE NEAREST NON-COOL CORE CLUSTER OUT TO R200 | XIS | Y |
| ANTLIA EB | 160.0852 | -35.3304 | 274.84198608 | 20.29194272 | 279.6006 | 56096.5981828704 | 56097.8197106482 | 807071010 | 45747.5 | 45000 | 45763.5 | 45747.5 | 0 | 45763.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40361.9 | 40361.9 | 105536 | 1 | PROCESSED | 57605.7231481482 | 56477 | 56111.1019328704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071521 | We propose to carry out mosaic observations (204 ks total) of the Antlia cluster, the third closest galaxy cluster highly ignored in X-ray, out to R200. It is the nearest non-cool core cluster with a similar low temperature as the cool core Virgo Cluster, allowing us to make a direct comparison to the cool core counterpart in our neighborhood. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will test models for clumping, electron-ion equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | WONG | KA-WAH | NULL | NULL | USA | 7 | AO7 | MAPPING THE NEAREST NON-COOL CORE CLUSTER OUT TO R200 | XIS | Y |
| ABELL 665 | 128.154 | 65.9045 | 149.6634974 | 34.85484411 | 289.999 | 56026.3998958333 | 56027.1251967593 | 807072010 | 50431 | 50000 | 50431 | 50431 | 0 | 50431 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41011.1 | 41011.1 | 62659.9 | 1 | PROCESSED | 57605.1298958333 | 56018 | 56044.1528240741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071522 | We propose observations of 2 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in previous cycles, and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MILLER | ERIC | NULL | NULL | USA | 7 | AO7 | COMPLETING THE SUZAKU CLUSTER OUTSKIRTS PROJECT | XIS | Y |
| ABELL 665 | 127.5519 | 65.9953 | 149.61230509 | 34.59661242 | 290.0005 | 56027.1259953704 | 56027.8057638889 | 807072020 | 51446 | 50000 | 51446 | 51446 | 0 | 51446 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 43276.9 | 43276.9 | 58728 | 1 | PROCESSED | 57605.1345717593 | 56018 | 56044.1899537037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071522 | We propose observations of 2 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in previous cycles, and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MILLER | ERIC | NULL | NULL | USA | 7 | AO7 | COMPLETING THE SUZAKU CLUSTER OUTSKIRTS PROJECT | XIS | Y |
| ABELL 665 | 127.3329 | 65.7462 | 149.92967896 | 34.55444535 | 289.9972 | 56027.8062847222 | 56028.5592476852 | 807072030 | 50348.6 | 50000 | 50352.6 | 50348.6 | 0 | 50356.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47385.6 | 47385.6 | 65049 | 0 | PROCESSED | 57605.1517939815 | 56018 | 56044.1669791667 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071522 | We propose observations of 2 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in previous cycles, and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MILLER | ERIC | NULL | NULL | USA | 7 | AO7 | COMPLETING THE SUZAKU CLUSTER OUTSKIRTS PROJECT | XIS | Y |
| ABELL 665 | 127.933 | 65.6581 | 149.97935617 | 34.81341699 | 289.9968 | 56028.5599537037 | 56029.4036226852 | 807072040 | 52791 | 50000 | 52791 | 52799 | 0 | 52799 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51667.1 | 51667.1 | 72885.9 | 0 | PROCESSED | 57605.1597569444 | 56018 | 56044.1843518518 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071522 | We propose observations of 2 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in previous cycles, and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MILLER | ERIC | NULL | NULL | USA | 7 | AO7 | COMPLETING THE SUZAKU CLUSTER OUTSKIRTS PROJECT | XIS | Y |
| ABELL 2597 | 351.4175 | -11.9496 | 65.78537526 | -64.80325971 | 249.1017 | 56261.057650463 | 56262.3299768518 | 807073010 | 51052.6 | 50000 | 51056.6 | 51067.4 | 0 | 51052.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46361.3 | 46361.3 | 109913.9 | 1 | PROCESSED | 57608.180462963 | 56018 | 56278.743587963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071522 | We propose observations of 2 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in previous cycles, and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MILLER | ERIC | NULL | NULL | USA | 7 | AO7 | COMPLETING THE SUZAKU CLUSTER OUTSKIRTS PROJECT | XIS | Y |
| ABELL 2597 | 351.1561 | -12.0446 | 65.23010074 | -64.66820365 | 250.0003 | 56262.3308680556 | 56263.5369212963 | 807073020 | 50034.5 | 50000 | 50058.5 | 50042.5 | 0 | 50034.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 44785 | 44785 | 104191.9 | 0 | PROCESSED | 57608.1666319444 | 56018 | 56336.4705902778 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071522 | We propose observations of 2 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in previous cycles, and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MILLER | ERIC | NULL | NULL | USA | 7 | AO7 | COMPLETING THE SUZAKU CLUSTER OUTSKIRTS PROJECT | XIS | Y |
| ABELL 2597 | 351.5123 | -12.2071 | 65.46064183 | -65.03980804 | 250.0004 | 56263.5374884259 | 56264.7744907407 | 807073030 | 50298.3 | 50000 | 50306.3 | 50298.3 | 0 | 50298.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42336.4 | 42336.4 | 106855.8 | 0 | PROCESSED | 57608.190625 | 56018 | 56279.6896180556 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071522 | We propose observations of 2 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in previous cycles, and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MILLER | ERIC | NULL | NULL | USA | 7 | AO7 | COMPLETING THE SUZAKU CLUSTER OUTSKIRTS PROJECT | XIS | Y |
| ABELL 2597 | 351.2512 | -12.298 | 64.91051751 | -64.90126459 | 250.0013 | 56264.7750115741 | 56266.2606134259 | 807073040 | 54718.7 | 50000 | 54718.7 | 54742.7 | 0 | 54726.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47919 | 47919 | 128327.8 | 1 | PROCESSED | 57608.2146759259 | 56018 | 56279.7033912037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071522 | We propose observations of 2 clusters of galaxies to probe the cluster environment out to r200 in order to (1) determine the temperature and density profiles for a representative sample of clusters; (2) search for azimuthal variations at these scales which may be indicative of the ongoing cluster accretion process; (3) construct the largest sample to date of clusters with accurate X-ray temperature and pressure determination out to r200; and (4) provide a fiducial data set for detailed comparison with high resolution numerical simulations. These targets capitalize on our large sample of clusters surveyed with XMM, expanding on a project started in previous cycles, and will provide a large enough data set to truly sample the properties of clusters at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MILLER | ERIC | NULL | NULL | USA | 7 | AO7 | COMPLETING THE SUZAKU CLUSTER OUTSKIRTS PROJECT | XIS | Y |
| RCS110619-0423.6 | 166.5769 | -4.3915 | 260.07293798 | 49.52807614 | 109.9541 | 56253.8521296296 | 56256.0092476852 | 807075010 | 77076.5 | 75000 | 77092.5 | 77076.5 | 0 | 77100.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 69380.5 | 69380.5 | 186345.8 | 4 | PROCESSED | 57608.1296875 | 56641 | 56275.577025463 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071525 | Accurate relationships between baryons in galaxy clusters and underlying dark matter distributions are crucial for using clusters as cosmological probes. Understanding the gamut of ICM properties, however, requires X-ray observations of samples chosen independently of their X-ray characteristics; likewise, such samples provide a powerful tool for quantifying redshift evolution in cluster properties. We have amassed X-ray observations of 24 optically-selected clusters of galaxies out to z~1. Here we propose 5 additional observations in order to uniformly span our total mass-redshift space over the range 0.15<z<0.9, for the purposes of constraining cluster evolution with a wholly unbiased sample. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | HICKS | AMALIA | NULL | NULL | USA | 7 | AO7 | AN UNBIASED SAMPLE: CONSTRAINING REDSHIFT EVOLUTION WITH OPTICALLY-SELECTED CLUSTERS OF GALAXIES II | XIS | Y |
| RCS110104-0351.3 | 165.266 | -3.8543 | 257.98650762 | 49.14106345 | 115.7008 | 56286.1353587963 | 56287.8716898148 | 807076010 | 76137.9 | 75000 | 76153.9 | 76137.9 | 0 | 76153.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 67441.1 | 67441.1 | 150001.8 | 0 | PROCESSED | 57608.3704050926 | 56690 | 56324.5102314815 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071525 | Accurate relationships between baryons in galaxy clusters and underlying dark matter distributions are crucial for using clusters as cosmological probes. Understanding the gamut of ICM properties, however, requires X-ray observations of samples chosen independently of their X-ray characteristics; likewise, such samples provide a powerful tool for quantifying redshift evolution in cluster properties. We have amassed X-ray observations of 24 optically-selected clusters of galaxies out to z~1. Here we propose 5 additional observations in order to uniformly span our total mass-redshift space over the range 0.15<z<0.9, for the purposes of constraining cluster evolution with a wholly unbiased sample. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | HICKS | AMALIA | NULL | NULL | USA | 7 | AO7 | AN UNBIASED SAMPLE: CONSTRAINING REDSHIFT EVOLUTION WITH OPTICALLY-SELECTED CLUSTERS OF GALAXIES II | XIS | Y |
| RCS022456-0348.8 | 36.2382 | -3.8143 | 170.77871975 | -57.71972182 | 253.341 | 56324.4414814815 | 56325.9579282407 | 807078010 | 50811.8 | 49000 | 50822.7 | 50814.7 | 0 | 50811.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46195 | 46195 | 131007.8 | 0 | PROCESSED | 57610.5290509259 | 56711 | 56345.5401967593 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071525 | Accurate relationships between baryons in galaxy clusters and underlying dark matter distributions are crucial for using clusters as cosmological probes. Understanding the gamut of ICM properties, however, requires X-ray observations of samples chosen independently of their X-ray characteristics; likewise, such samples provide a powerful tool for quantifying redshift evolution in cluster properties. We have amassed X-ray observations of 24 optically-selected clusters of galaxies out to z~1. Here we propose 5 additional observations in order to uniformly span our total mass-redshift space over the range 0.15<z<0.9, for the purposes of constraining cluster evolution with a wholly unbiased sample. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | HICKS | AMALIA | NULL | NULL | USA | 7 | AO7 | AN UNBIASED SAMPLE: CONSTRAINING REDSHIFT EVOLUTION WITH OPTICALLY-SELECTED CLUSTERS OF GALAXIES II | XIS | Y |
| SWCL J1403+3212 | 210.8847 | 32.2142 | 55.27159844 | 73.55798506 | 128.2493 | 56289.1009837963 | 56290.2578587963 | 807081010 | 52137.4 | 45000 | 52137.4 | 52143 | 0 | 52145.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42986.8 | 42986.8 | 99935.8 | 0 | PROCESSED | 57608.4054050926 | 56690 | 56324.4837152778 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071526 | The evolution of X-ray properties of galaxy clusters with redshift provides important constraints on the formation and evolution of the hot gaseous halos. The scaling relations and their deviations from self-similar model predictions due to non-gravitational processes are also important for modeling the cluster selection function for cosmology. We propose to observe a uniform sample of z~0.6 galaxy clusters, selected from the Swift archival data and confirmed by multi-band optical data, using Suzaku to better characterize their X-ray properties such the X-ray luminosity and temperature. With this sample, we are able to model the selection functions relatively easily and place cleaner and tighter constraints on the evolution of X-ray properties of galaxy clusters. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | DAI | XINYU | NULL | NULL | USA | 7 | AO7 | X-RAY PROPERTIES OF A UNIFORMLY SELECTED SAMPLE OF Z ~ 0.6 CLUSTERS | XIS | Y |
| J2218.2-0350 | 334.573 | -3.8385 | 58.63251599 | -46.67973864 | 268.0005 | 56260.6621527778 | 56261.0523148148 | 807084010 | 15767.1 | 15000 | 15775.1 | 15767.1 | 0 | 15783.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11914.5 | 11914.5 | 33707.9 | 0 | PROCESSED | 57608.1412384259 | 56644 | 56275.6610300926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 072018 | We propose to observe the three clusters of galaxies J2218.2-0350, J2218.6-0346 and J2218.8-0258 with exposure times of 15, 25 and 35 ks respectively. These clusters are part of a structure of four linearly aligned clusters, separated from each other by 4 to 10 Mpc. We will accurately determine their masses and orientation. This will allow us to fully map the tidal force field of the structure, which is the prime force behind the formation of filaments in the cosmic web. We will study the effects of cluster mass, separation and mutual orientation on the filamentary structure of the cosmic web and on the evolution of galaxies therein. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | BOS | E.G. PATRICK | NULL | NULL | EUR | 7 | AO7 | CLUSTERS AND THE COSMIC WEB | XIS | Y |
| J2218.6-0346 | 334.6629 | -3.7693 | 58.79146355 | -46.71055995 | 71.7798 | 56063.8991550926 | 56064.7196875 | 807085010 | 28629 | 25000 | 28629 | 28629 | 0 | 28629 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26832.7 | 26832.7 | 70883.9 | 1 | PROCESSED | 57605.4341550926 | 56442 | 56076.0273726852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 072018 | We propose to observe the three clusters of galaxies J2218.2-0350, J2218.6-0346 and J2218.8-0258 with exposure times of 15, 25 and 35 ks respectively. These clusters are part of a structure of four linearly aligned clusters, separated from each other by 4 to 10 Mpc. We will accurately determine their masses and orientation. This will allow us to fully map the tidal force field of the structure, which is the prime force behind the formation of filaments in the cosmic web. We will study the effects of cluster mass, separation and mutual orientation on the filamentary structure of the cosmic web and on the evolution of galaxies therein. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | BOS | E.G. PATRICK | NULL | NULL | EUR | 7 | AO7 | CLUSTERS AND THE COSMIC WEB | XIS | Y |
| J2218.8-0258 | 334.694 | -2.9598 | 59.75779093 | -46.24852305 | 49.9996 | 56072.7972685185 | 56073.7370833333 | 807086010 | 38398.1 | 35000 | 38406.1 | 38398.1 | 0 | 38406.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 36973.9 | 36973.9 | 81195.8 | 1 | PROCESSED | 57605.5228703704 | 56500 | 56134.0402199074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 072018 | We propose to observe the three clusters of galaxies J2218.2-0350, J2218.6-0346 and J2218.8-0258 with exposure times of 15, 25 and 35 ks respectively. These clusters are part of a structure of four linearly aligned clusters, separated from each other by 4 to 10 Mpc. We will accurately determine their masses and orientation. This will allow us to fully map the tidal force field of the structure, which is the prime force behind the formation of filaments in the cosmic web. We will study the effects of cluster mass, separation and mutual orientation on the filamentary structure of the cosmic web and on the evolution of galaxies therein. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | BOS | E.G. PATRICK | NULL | NULL | EUR | 7 | AO7 | CLUSTERS AND THE COSMIC WEB | XIS | Y |
| HYDRA A SE | 139.5641 | -12.2366 | 243.07517911 | 25.03717361 | 300.0006 | 56085.6674421296 | 56086.2926388889 | 807087010 | 21489.8 | 20000 | 21489.8 | 21489.8 | 0 | 21489.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20365.1 | 20365.1 | 54012 | 0 | PROCESSED | 57605.6279976852 | 56465 | 56099.0036921296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 072020 | Galaxy cluster outskirts are the regions where structure formation occurs through the accretion of smaller structures along large-scale filaments. Thanks to its low background, Suzaku has allowed for the first time to measure the thermodynamical properties of the ICM out to the virial radius. Recently, we used archival ROSAT observations to detect cluster emission out to large radii and quantify the deviations from spherical symmetry. Based on this work, we propose to map the outskirts of Hydra A, which was found to have the highest azimuthal scatter. This will allow us to measure the temperature profiles out to the virial radius and infer the bias on the mean thermodynamical properties and the mass reconstruction when clusters are observed along preferential directions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | ECKERT | DOMINIQUE | NULL | NULL | EUR | 7 | AO7 | MAPPING THE OUTSKIRTS OF HYDRA A WITH SUZAKU | XIS | Y |
| HYDRA A FAR SE | 139.7 | -12.375 | 243.28582967 | 25.05625041 | 300 | 56082.6736342593 | 56083.9368981482 | 807088010 | 40939 | 40000 | 40947 | 40939 | 0 | 40947 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 37914.3 | 37914.3 | 109135.8 | 0 | PROCESSED | 57605.5894444444 | 56464 | 56096.2405208333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 072020 | Galaxy cluster outskirts are the regions where structure formation occurs through the accretion of smaller structures along large-scale filaments. Thanks to its low background, Suzaku has allowed for the first time to measure the thermodynamical properties of the ICM out to the virial radius. Recently, we used archival ROSAT observations to detect cluster emission out to large radii and quantify the deviations from spherical symmetry. Based on this work, we propose to map the outskirts of Hydra A, which was found to have the highest azimuthal scatter. This will allow us to measure the temperature profiles out to the virial radius and infer the bias on the mean thermodynamical properties and the mass reconstruction when clusters are observed along preferential directions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | ECKERT | DOMINIQUE | NULL | NULL | EUR | 7 | AO7 | MAPPING THE OUTSKIRTS OF HYDRA A WITH SUZAKU | XIS | Y |
| HYDRA A FAR N | 139.5397 | -11.7599 | 242.64361193 | 25.31151573 | 300.0007 | 56083.9377430556 | 56085.1452662037 | 807089010 | 41276 | 40000 | 41284 | 41284 | 0 | 41276 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38172.7 | 38172.7 | 104311.7 | 1 | PROCESSED | 57605.6201851852 | 56465 | 56098.4661689815 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 072020 | Galaxy cluster outskirts are the regions where structure formation occurs through the accretion of smaller structures along large-scale filaments. Thanks to its low background, Suzaku has allowed for the first time to measure the thermodynamical properties of the ICM out to the virial radius. Recently, we used archival ROSAT observations to detect cluster emission out to large radii and quantify the deviations from spherical symmetry. Based on this work, we propose to map the outskirts of Hydra A, which was found to have the highest azimuthal scatter. This will allow us to measure the temperature profiles out to the virial radius and infer the bias on the mean thermodynamical properties and the mass reconstruction when clusters are observed along preferential directions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | ECKERT | DOMINIQUE | NULL | NULL | EUR | 7 | AO7 | MAPPING THE OUTSKIRTS OF HYDRA A WITH SUZAKU | XIS | Y |
| HYDRA A SW | 139.253 | -12.251 | 242.88145003 | 24.78864489 | 106.4205 | 56241.8334490741 | 56242.8342708333 | 807090010 | 39839.9 | 40000 | 39847.9 | 39855.9 | 0 | 39839.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 33708.5 | 33708.5 | 86463.9 | 0 | PROCESSED | 57607.9882407407 | 56631 | 56265.6332986111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 072020 | Galaxy cluster outskirts are the regions where structure formation occurs through the accretion of smaller structures along large-scale filaments. Thanks to its low background, Suzaku has allowed for the first time to measure the thermodynamical properties of the ICM out to the virial radius. Recently, we used archival ROSAT observations to detect cluster emission out to large radii and quantify the deviations from spherical symmetry. Based on this work, we propose to map the outskirts of Hydra A, which was found to have the highest azimuthal scatter. This will allow us to measure the temperature profiles out to the virial radius and infer the bias on the mean thermodynamical properties and the mass reconstruction when clusters are observed along preferential directions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | ECKERT | DOMINIQUE | NULL | NULL | EUR | 7 | AO7 | MAPPING THE OUTSKIRTS OF HYDRA A WITH SUZAKU | XIS | Y |
| HYDRA A OUT | 139.8502 | -12.6235 | 243.60142222 | 25.01758475 | 300.0034 | 56085.1461574074 | 56085.6667824074 | 807091010 | 20327.6 | 20000 | 20351.6 | 20343.6 | 0 | 20327.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16540.3 | 16540.3 | 44977.9 | 0 | PROCESSED | 57605.607349537 | 56491 | 56120.2321296296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 072020 | Galaxy cluster outskirts are the regions where structure formation occurs through the accretion of smaller structures along large-scale filaments. Thanks to its low background, Suzaku has allowed for the first time to measure the thermodynamical properties of the ICM out to the virial radius. Recently, we used archival ROSAT observations to detect cluster emission out to large radii and quantify the deviations from spherical symmetry. Based on this work, we propose to map the outskirts of Hydra A, which was found to have the highest azimuthal scatter. This will allow us to measure the temperature profiles out to the virial radius and infer the bias on the mean thermodynamical properties and the mass reconstruction when clusters are observed along preferential directions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | ECKERT | DOMINIQUE | NULL | NULL | EUR | 7 | AO7 | MAPPING THE OUTSKIRTS OF HYDRA A WITH SUZAKU | XIS | Y |
| G171.9-40.7 | 48.2433 | 8.3685 | 171.97024112 | -40.65556769 | 252.8031 | 56320.012025463 | 56322.7126967593 | 807092010 | 100982.5 | 100000 | 100990.5 | 100982.5 | 0 | 100984.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 93161.7 | 93161.7 | 233295.7 | 0 | PROCESSED | 57608.6871527778 | 56749 | 56365.6023263889 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 072021 | We propose to observe 4 galaxy clusters from the first all-sky blind Sunyaev Zeldovich (SZ) effect cluster catalogue produced by the Planck satellite. This catalogue has revealed a new population of clusters previously undetected by X-ray surveys. The Planck SZ selected cluster sample consists of hot, massive, morphologically disturbed clusters that are under-luminous in the soft X-ray band. This exciting population has implications not only for understanding the thermodynamic state of the intracluster medium, but also for cluster cosmology where it represents an important area of phase space in the cluster mass function; it is a pointer to the dynamics of how clusters form through mergers, and to the true spatial density of cluster-mass structures not represented in X-ray surveys. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | SCAIFE | ANNA | NULL | NULL | EUR | 7 | AO7 | CONSTRAINING THE THERMODYNAMIC STATE OF NEW PLANCK GALAXY CLUSTERS WITH SUZAKU | XIS | Y |
| G115.7+17.5 | 336.6801 | 78.3035 | 115.72297849 | 17.51053762 | 214.3075 | 56311.7506712963 | 56313.7419328704 | 807093010 | 97873.2 | 100000 | 97889.2 | 97873.2 | 0 | 97889.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 94397.7 | 94397.7 | 172007.9 | 1 | PROCESSED | 57608.5818634259 | 56708 | 56342.5694097222 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 072021 | We propose to observe 4 galaxy clusters from the first all-sky blind Sunyaev Zeldovich (SZ) effect cluster catalogue produced by the Planck satellite. This catalogue has revealed a new population of clusters previously undetected by X-ray surveys. The Planck SZ selected cluster sample consists of hot, massive, morphologically disturbed clusters that are under-luminous in the soft X-ray band. This exciting population has implications not only for understanding the thermodynamic state of the intracluster medium, but also for cluster cosmology where it represents an important area of phase space in the cluster mass function; it is a pointer to the dynamics of how clusters form through mergers, and to the true spatial density of cluster-mass structures not represented in X-ray surveys. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | SCAIFE | ANNA | NULL | NULL | EUR | 7 | AO7 | CONSTRAINING THE THERMODYNAMIC STATE OF NEW PLANCK GALAXY CLUSTERS WITH SUZAKU | XIS | Y |
| VIRGO W1 | 187.5107 | 12.2426 | 283.26919479 | 74.29186005 | 291.9999 | 56110.6712847222 | 56110.9370138889 | 807094010 | 12785.9 | 10000 | 12793.9 | 12793.9 | 0 | 12785.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10542.9 | 10542.9 | 22951.9 | 0 | PROCESSED | 57606.5451157407 | 56018 | 56127.137662037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076004 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 7 | AO7 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO W2 | 187.236 | 12.0886 | 282.50975725 | 74.06175724 | 285.4993 | 56110.9396180556 | 56111.2640509259 | 807095010 | 12484.7 | 10000 | 12492.7 | 12484.7 | 0 | 12500.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12333.5 | 12333.5 | 28025.9 | 1 | PROCESSED | 57606.5414583333 | 56018 | 56139.0870717593 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076004 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 7 | AO7 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO W3 | 186.9593 | 11.946 | 281.75004157 | 73.83934761 | 99.9993 | 56273.4086921296 | 56273.6403472222 | 807096010 | 10842.4 | 10000 | 10850.4 | 10850.4 | 0 | 10842.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9092.1 | 9092.1 | 20007.9 | 0 | PROCESSED | 57608.2529282407 | 56018 | 56342.4989699074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076004 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 7 | AO7 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO W4 | 186.6838 | 11.7876 | 281.0321598 | 73.60000956 | 100.001 | 56273.6409143518 | 56273.9264699074 | 807097010 | 14512 | 11000 | 14512 | 14536 | 0 | 14520 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13737.9 | 13737.9 | 24665.9 | 0 | PROCESSED | 57608.2576388889 | 56018 | 56342.5158680556 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076004 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 7 | AO7 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO W5 | 186.3906 | 11.6158 | 280.29277845 | 73.33982916 | 99.9992 | 56273.927037037 | 56274.3467476852 | 807098010 | 16614.4 | 15000 | 16626.1 | 16622.4 | 0 | 16614.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18174 | 18174 | 36256 | 0 | PROCESSED | 57608.2663078704 | 56018 | 56303.5207407407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076004 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 7 | AO7 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO W6 | 186.0979 | 11.4464 | 279.57270772 | 73.07967034 | 99.9988 | 56274.3472685185 | 56274.8098726852 | 807099010 | 22421.7 | 19000 | 22421.7 | 22421.7 | 0 | 22421.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19182 | 19182 | 39949.9 | 1 | PROCESSED | 57608.269224537 | 56018 | 56342.6277893518 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076004 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 7 | AO7 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO W7 | 185.8245 | 11.2655 | 278.94638045 | 72.81351487 | 99.9999 | 56274.8104398148 | 56275.3217013889 | 807100010 | 23444.9 | 20000 | 23452.9 | 23452.9 | 0 | 23444.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25035.3 | 25035.3 | 44169.9 | 0 | PROCESSED | 57608.2724652778 | 56018 | 56338.5069560185 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076004 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 7 | AO7 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO W8 | 185.551 | 11.0911 | 278.32881118 | 72.55156974 | 99.4998 | 56275.3224074074 | 56275.8078240741 | 807101010 | 22170.3 | 21000 | 22178.3 | 22170.3 | 0 | 22186.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18858.5 | 18858.5 | 41918 | 0 | PROCESSED | 57608.2782291667 | 56018 | 56315.5145023148 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076004 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 7 | AO7 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO W9 | 185.2783 | 10.9356 | 277.70610968 | 72.30561596 | 99.9989 | 56275.8085763889 | 56276.4093055556 | 807102010 | 27105.7 | 23000 | 27105.7 | 27105.7 | 0 | 27105.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28479.1 | 28479.1 | 51896 | 0 | PROCESSED | 57608.2880092593 | 56018 | 56315.5260300926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076004 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 7 | AO7 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO W10 | 185.0059 | 10.7782 | 277.10217205 | 72.05623626 | 99.9987 | 56276.4098263889 | 56276.9828935185 | 807103010 | 27967.7 | 24000 | 27967.7 | 27967.7 | 0 | 27967.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25760.4 | 25760.4 | 49503.9 | 0 | PROCESSED | 57608.287974537 | 56018 | 56315.5187037037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076004 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 7 | AO7 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO W11 | 184.734 | 10.623 | 276.51178499 | 71.80735655 | 99.9988 | 56276.9834143518 | 56277.5397337963 | 807104010 | 24308.7 | 24000 | 24308.7 | 24311 | 0 | 24312.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 23509.5 | 23509.5 | 48038.1 | 0 | PROCESSED | 57608.2867361111 | 56018 | 56338.5029050926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076004 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 7 | AO7 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO W12 | 184.4921 | 10.4589 | 276.03236295 | 71.56080365 | 100 | 56277.5402546296 | 56278.125150463 | 807105010 | 27091.5 | 24000 | 27099.5 | 27091.5 | 0 | 27099.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 26852.8 | 26852.8 | 50488 | 1 | PROCESSED | 57608.2964930556 | 56018 | 56344.6765162037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076004 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 7 | AO7 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO N1 | 187.7027 | 13.2607 | 282.74012713 | 75.31771863 | 314.0012 | 56097.8290740741 | 56098.0419328704 | 807106010 | 9931.9 | 10000 | 9931.9 | 9939.9 | 0 | 9939.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9542 | 9542 | 18383.9 | 0 | PROCESSED | 57605.7042592593 | 56018 | 56225.4789699074 | 3.0.22.44 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076004 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 7 | AO7 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO N2 | 187.703 | 13.5671 | 282.35217615 | 75.60823465 | 313.9984 | 56098.0424074074 | 56098.2606828704 | 807107010 | 10706.8 | 10000 | 10706.8 | 10730.8 | 0 | 10714.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8659 | 8659 | 18848 | 1 | PROCESSED | 57605.7127777778 | 56018 | 56214.9560763889 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076004 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 7 | AO7 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO N3 | 187.7014 | 13.8904 | 281.91864672 | 75.91344863 | 313.997 | 56098.2612037037 | 56098.5176388889 | 807108010 | 12266 | 10000 | 12266 | 12266 | 0 | 12266 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12699.7 | 12699.7 | 22139.9 | 1 | PROCESSED | 57605.7217013889 | 56018 | 56214.9569907407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076004 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 7 | AO7 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO N4 | 187.7041 | 14.2061 | 281.49354158 | 76.21209693 | 310.9981 | 56104.178900463 | 56104.463275463 | 807109010 | 12757.7 | 12000 | 12757.7 | 12757.7 | 0 | 12757.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13291 | 13291 | 24561.9 | 0 | PROCESSED | 57606.4838541667 | 56018 | 56219.6559953704 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076004 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 7 | AO7 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO N5 | 187.7004 | 14.5243 | 281.02135681 | 76.51020537 | 313.9964 | 56098.5183449074 | 56098.9203125 | 807110010 | 15778.9 | 13000 | 15778.9 | 15789.4 | 0 | 15782.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16072.8 | 16072.8 | 34728 | 0 | PROCESSED | 57605.7329166667 | 56018 | 56214.963587963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076004 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 7 | AO7 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO N6 | 187.706 | 14.8589 | 280.53999282 | 76.82590701 | 310.9995 | 56104.4640740741 | 56104.8946296296 | 807111010 | 20488 | 15000 | 20488 | 20496 | 0 | 20496 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19902.5 | 19902.5 | 37198 | 1 | PROCESSED | 57606.4880555556 | 56018 | 56117.9917361111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076004 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 7 | AO7 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO N7 | 187.7068 | 15.1871 | 280.02627988 | 77.13302603 | 311 | 56104.895150463 | 56105.2924768518 | 807112010 | 18182.8 | 16000 | 18182.8 | 18205.9 | 0 | 18190.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16604 | 16604 | 34327.9 | 0 | PROCESSED | 57606.4965393518 | 56018 | 56117.9967013889 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076004 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 7 | AO7 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO N8 | 187.7075 | 15.4944 | 279.52276063 | 77.41962086 | 310.9997 | 56105.2930439815 | 56105.7028703704 | 807113010 | 18701.8 | 18000 | 18705.7 | 18701.8 | 0 | 18709.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18750.4 | 18750.4 | 35400 | 0 | PROCESSED | 57606.4979050926 | 56018 | 56118.0144097222 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076004 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 7 | AO7 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO N9 | 187.7056 | 15.8164 | 278.95935226 | 77.71791573 | 310.4995 | 56106.6618171296 | 56107.1398611111 | 807114010 | 22978.8 | 19000 | 22978.8 | 23005.9 | 0 | 22978.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 20681.9 | 20681.9 | 41295.9 | 1 | PROCESSED | 57606.5125578704 | 56018 | 56118.0912037037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076004 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 7 | AO7 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO S1 | 187.7666 | 12.1106 | 284.29495534 | 74.24059367 | 308.501 | 56111.2691087963 | 56111.5314583333 | 807115010 | 12521.6 | 10000 | 12533.6 | 12521.6 | 0 | 12536.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13182 | 13182 | 22642 | 0 | PROCESSED | 57606.5476736111 | 56018 | 56226.6475 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076004 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 7 | AO7 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO S2 | 187.7262 | 11.7827 | 284.50264567 | 73.91527115 | 308.5008 | 56111.5319791667 | 56111.8286805556 | 807116010 | 14040.8 | 10000 | 14048.8 | 14040.8 | 0 | 14056.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13163.1 | 13163.1 | 25631.9 | 0 | PROCESSED | 57606.5448611111 | 56018 | 56139.1771180556 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076004 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 7 | AO7 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO S3 | 187.7051 | 11.4733 | 284.74763768 | 73.61284119 | 308.498 | 56111.8292013889 | 56112.2224189815 | 807117010 | 15063 | 10000 | 15063 | 15063 | 0 | 15063 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13396 | 13396 | 33961.9 | 0 | PROCESSED | 57606.5537384259 | 56018 | 56139.230787037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076004 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 7 | AO7 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO S4 | 187.668 | 11.1668 | 284.92853674 | 73.30851588 | 308.5011 | 56112.2229861111 | 56112.5056828704 | 807118010 | 12852 | 10000 | 12852 | 12852 | 0 | 12852 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13862.2 | 13862.2 | 24417.9 | 0 | PROCESSED | 57606.5554282407 | 56018 | 56141.1138194445 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076004 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 7 | AO7 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO S5 | 187.6482 | 10.8577 | 285.16119801 | 73.00623042 | 308.4993 | 56112.5062037037 | 56112.7681828704 | 807119010 | 12773.2 | 10000 | 12781.2 | 12773.2 | 0 | 12789.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12087 | 12087 | 22623.9 | 0 | PROCESSED | 57606.5630439815 | 56018 | 56141.1590625 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076004 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 7 | AO7 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO S6 | 187.6479 | 10.5513 | 285.44540552 | 72.71150131 | 308.4999 | 56112.7686574074 | 56113.0799421296 | 807120010 | 12701.4 | 10000 | 12701.4 | 12701.4 | 0 | 12701.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10500.5 | 10500.5 | 26887.9 | 1 | PROCESSED | 57606.5642361111 | 56018 | 56141.2151388889 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076004 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 7 | AO7 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO S7 | 187.6096 | 10.2244 | 285.61941254 | 72.38660135 | 308.5009 | 56113.0805092593 | 56113.4293518518 | 807121010 | 14997.9 | 13000 | 14997.9 | 14997.9 | 0 | 14997.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15746 | 15746 | 30135.9 | 0 | PROCESSED | 57606.5659606482 | 56018 | 56141.9783101852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076004 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 7 | AO7 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO S8 | 187.5886 | 9.916 | 285.82444468 | 72.08390522 | 307.999 | 56113.4301041667 | 56113.7523148148 | 807122010 | 16053 | 13000 | 16053 | 16053 | 0 | 16053 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 15150 | 15150 | 27831.9 | 1 | PROCESSED | 57606.5675578704 | 56018 | 56226.5896296296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076004 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 7 | AO7 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO S9 | 187.5697 | 9.5888 | 286.04491696 | 71.76339412 | 306.8996 | 56115.2917361111 | 56115.6641319444 | 807123010 | 18917.9 | 14000 | 18933.9 | 18917.9 | 0 | 18933.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18618.5 | 18618.5 | 32168 | 0 | PROCESSED | 57606.5741087963 | 56018 | 56142.0874884259 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076004 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 7 | AO7 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO S10 | 187.554 | 9.2735 | 286.25782629 | 71.4549429 | 121.999 | 56269.421712963 | 56269.7570717593 | 807124010 | 16098 | 16000 | 16098 | 16098 | 0 | 16098 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 13413 | 13413 | 28952 | 0 | PROCESSED | 57608.2049074074 | 56018 | 56336.4667824074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076004 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 7 | AO7 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO S11 | 187.5325 | 8.9432 | 286.45864166 | 71.13028831 | 122.0016 | 56269.7576851852 | 56270.1612384259 | 807125010 | 17282.3 | 16000 | 17282.3 | 17282.3 | 0 | 17282.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18562.7 | 18562.7 | 34820 | 0 | PROCESSED | 57608.2142013889 | 56018 | 56336.4686111111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076004 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 7 | AO7 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO S12 | 187.4953 | 8.619 | 286.60241823 | 70.80739613 | 122.0035 | 56270.1617592593 | 56270.5772106482 | 807126010 | 16427.5 | 16000 | 16427.5 | 16427.5 | 0 | 16427.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16183.7 | 16183.7 | 35863.9 | 0 | PROCESSED | 57608.2146527778 | 56018 | 56338.4929166667 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076004 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 7 | AO7 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO S13 | 187.4758 | 8.312 | 286.77930619 | 70.50542211 | 122.0007 | 56270.5777314815 | 56270.8459606482 | 807127010 | 13066.6 | 12000 | 13098.4 | 13090.6 | 0 | 13066.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11541.1 | 11541.1 | 23167.9 | 0 | PROCESSED | 57608.2217824074 | 56018 | 56291.6901273148 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076004 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 7 | AO7 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO S14 | 187.4376 | 7.6823 | 287.13089499 | 69.88593318 | 122 | 56270.8466666667 | 56271.2320717593 | 807128010 | 15420.4 | 12000 | 15436.4 | 15420.4 | 0 | 15444.4 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16741.7 | 16741.7 | 33287.9 | 0 | PROCESSED | 57608.2246643518 | 56018 | 56291.692349537 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076004 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 7 | AO7 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO S15 | 187.3986 | 7.3548 | 287.25281516 | 69.55887671 | 122.0016 | 56271.2325925926 | 56271.6272106482 | 807129010 | 18213.6 | 16000 | 18229.6 | 18213.6 | 0 | 18229.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17321.8 | 17321.8 | 34056 | 0 | PROCESSED | 57608.2302430556 | 56018 | 56291.7069328704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076004 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 7 | AO7 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO S16 | 187.3813 | 7.0531 | 287.41240339 | 69.26194594 | 122.0008 | 56271.6277314815 | 56272.0709722222 | 807130010 | 21648.2 | 18000 | 21648.2 | 21648.2 | 0 | 21648.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21308.1 | 21308.1 | 38267.9 | 1 | PROCESSED | 57608.2349652778 | 56018 | 56330.5084837963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076004 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 7 | AO7 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO S17 | 187.3614 | 6.7452 | 287.56473465 | 68.95823146 | 122.4996 | 56272.071724537 | 56272.5258796296 | 807131010 | 18943.2 | 18000 | 18951.2 | 18943.2 | 0 | 18951.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 18614.5 | 18614.5 | 39231.9 | 1 | PROCESSED | 57608.241712963 | 56018 | 56291.7338773148 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076004 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 7 | AO7 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO S18 | 187.3413 | 6.4206 | 287.72310531 | 68.63810092 | 122.5021 | 56272.526400463 | 56272.9307175926 | 807132010 | 19867.6 | 18000 | 19875.6 | 19867.6 | 0 | 19883.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18825.1 | 18825.1 | 34931.9 | 0 | PROCESSED | 57608.2443055556 | 56018 | 56291.7121296296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076004 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 7 | AO7 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO S19 | 187.324 | 6.1182 | 287.8702994 | 68.34005974 | 122.7988 | 56272.9313310185 | 56273.403587963 | 807133010 | 19348.4 | 19000 | 19360.1 | 19356.4 | 0 | 19348.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20709.9 | 20709.9 | 40798 | 0 | PROCESSED | 57608.2512384259 | 56018 | 56338.5094907407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 076004 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 7 | AO7 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| CENA N LOBE 3 | 201.1567 | -39.315 | 309.90401242 | 23.10702351 | 110.949 | 56316.327349537 | 56318.4140046296 | 807134010 | 81984 | 75000 | 81992 | 81992 | 0 | 81984 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 73883.8 | 73883.8 | 180247.8 | 2 | PROCESSED | 57608.6528356482 | 56708 | 56342.7001157407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 070127 | Radio source Centaurus A is the closest active galaxy in the Universe (3.7 Mpc). It is surrounded by poorly known giant radio lobes extending for about 600 kpc in the N-S direction. Here we propose Chandra follow-up of four regions in the Southern and Northern lobes where Suzaku time was allocated. We also propose joint Chandra-Suzaku observation toward interacting filamentary region where ASCA found a hint of X-ray emission. The primary goal of the project is to study the filamentary structure of the lobe in X-rays, in the broader context of particle acceleration and energy dissipation processes taking place in inhomogeneous and multi-phase plasma. The obtained results are guaranteed to improve our knowledge regarding not only the Centaurus A, but all jetted active galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | S | TANAKA | YASUYUKI | NULL | NULL | JAP | 7 | AO7 | STUDYING GIANT FILAMENTARY LOBES OF CENTAURUS A | XIS | Y |
| ABELL 85 S1 | 10.6021 | -9.9841 | 115.42621428 | -72.72412936 | 230 | 56292.2572800926 | 56295.6314583333 | 807135010 | 139998.2 | 50000 | 139998.2 | 139998.2 | 0 | 139998.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11820 | 11820 | 25477.9 | 0 | PROCESSED | 57608.4068402778 | 56703 | 56337.496875 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071791 | We propose exposures with CHandra and Suzaku in Abell 85 to trace the impact of a galaxy group merging with a galaxy cluster at multiple scales. Existing observations of Abell 85 reveal an infalling galaxy group ~300 kpc to the south of the main cluster moving supersonically through the ICM. Stripped gas is observed trailing behind this group to distances of 2 Mpc. We will investigate interactions between this group and the main cluster by observing the shocks associated with the group's motion and the properties of stripped gas. We will be able to measure the properties of the stripped gas from the group's current location out to the virial radius by combining the data from both telescopes. These observations will provide key insights into how the largest structures form. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | S | ALLEN | STEVEN | NULL | NULL | USA | 7 | AO7 | TRACING A MERGER FROM START TO FINISH IN ABELL 85 | XIS | Y |
| ABELL 85 S2 | 10.6249 | -9.681 | 115.61862408 | -72.42570917 | 230.5003 | 56295.6322106482 | 56296.8696064815 | 807136010 | 53603 | 50000 | 53611 | 53611 | 0 | 53603 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 51842.6 | 51842.6 | 106895.7 | 2 | PROCESSED | 57608.4325347222 | 56702 | 56336.5803240741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071791 | We propose exposures with CHandra and Suzaku in Abell 85 to trace the impact of a galaxy group merging with a galaxy cluster at multiple scales. Existing observations of Abell 85 reveal an infalling galaxy group ~300 kpc to the south of the main cluster moving supersonically through the ICM. Stripped gas is observed trailing behind this group to distances of 2 Mpc. We will investigate interactions between this group and the main cluster by observing the shocks associated with the group's motion and the properties of stripped gas. We will be able to measure the properties of the stripped gas from the group's current location out to the virial radius by combining the data from both telescopes. These observations will provide key insights into how the largest structures form. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | S | ALLEN | STEVEN | NULL | NULL | USA | 7 | AO7 | TRACING A MERGER FROM START TO FINISH IN ABELL 85 | XIS | Y |
| SHAPLEY B | 201.6375 | -31.8605 | 311.5766773 | 30.42117615 | 110.7883 | 56315.4877893518 | 56316.3245138889 | 807137010 | 30505.2 | 30000 | 30513.2 | 30505.2 | 0 | 30520.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 26139.5 | 26139.5 | 72291.9 | 2 | PROCESSED | 57608.5939814815 | 56709 | 56342.5463888889 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071848 | 29% of the baryon density measured at high redshift are unaccounted for at the present epoch. Since a persistent deficit would challenge our current understanding of the thermodynamics of structure formation and the effects of shocks and galactic outflows on the surrounding gas, resolving this deficit is critical for understanding low-redshift cosmology and galaxy formation. Simulations suggest these baryons emit soft X-rays and should reside along low density filaments in the cosmic web, the WHIM. We propose to combine Chandra ACIS-I with Suzaku XIS observations for 3 large scale filaments in the Shapley Supercluster, the largest overdensity of galaxies and clusters in the z<0.1 Universe, to identify galaxy groups in these filaments and search for X-ray emission from the WHIM. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | S | MACHACEK | MARIE | NULL | NULL | USA | 7 | AO7 | MAPPING GALAXY GROUPS AND THE HOT WHIM IN SHAPLEY SUPERCLUSTER FILAMENTS WITH CHANDRA AND SUZAKU | XIS | Y |
| SHAPLEY C | 202.085 | -31.0332 | 312.17140577 | 31.17563268 | 109.0374 | 56330.7851273148 | 56331.4147453704 | 807138010 | 30874.4 | 30000 | 30890.4 | 30874.4 | 0 | 30890.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 31966 | 31966 | 54392 | 0 | PROCESSED | 57610.5475694444 | 56715 | 56349.523287037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 071848 | 29% of the baryon density measured at high redshift are unaccounted for at the present epoch. Since a persistent deficit would challenge our current understanding of the thermodynamics of structure formation and the effects of shocks and galactic outflows on the surrounding gas, resolving this deficit is critical for understanding low-redshift cosmology and galaxy formation. Simulations suggest these baryons emit soft X-rays and should reside along low density filaments in the cosmic web, the WHIM. We propose to combine Chandra ACIS-I with Suzaku XIS observations for 3 large scale filaments in the Shapley Supercluster, the largest overdensity of galaxies and clusters in the z<0.1 Universe, to identify galaxy groups in these filaments and search for X-ray emission from the WHIM. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | S | MACHACEK | MARIE | NULL | NULL | USA | 7 | AO7 | MAPPING GALAXY GROUPS AND THE HOT WHIM IN SHAPLEY SUPERCLUSTER FILAMENTS WITH CHANDRA AND SUZAKU | XIS | Y |
| A399&A401 FILAMENT | 44.5739 | 13.3044 | 164.23302583 | -39.1861165 | 71.9992 | 56522.5065972222 | 56523.421724537 | 808005010 | 42165.5 | 40000 | 42165.5 | 42165.5 | 0 | 42165.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 40981 | 40981 | 79063.8 | 2 | PROCESSED | 57612.3602083333 | 56956 | 56587.6829398148 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080004 | To investigate (i)the influence of the merging event on IntraCluster Medium (ICM), We propose 40 ks+50 ks ~2 =140 ks observations of the linked region between Abell 399 and Abell 401. A399 (z=0.0724) and A401 (z=0.0737) are expected be in the initial phase of a cluster merger. With Suzaku fs high sensitivity observations, we will (i)determine the ICM physical conditions by measuring the temperature and density distribution, (ii) characterize the dynamical state of the cluster linked region, (iii) confirm the presence of a shock front predicted by numerical simulations. Our study will reveal the nature of initial phase of merging event of clusters of galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ISHISAKI | YOSHITAKA | NULL | NULL | JAP | 8 | AO8 | MORPHOLOGY AND PHYSICAL PROPERTIES OF SHOCKED GAS BY MAJOR MERGER IN THE LINKED REGION OF ABELL 399 AND ABELL 401 | XIS | Y |
| A401EAST | 45.0348 | 13.3366 | 164.66710088 | -38.88860633 | 71.9996 | 56530.5043055556 | 56531.6841782407 | 808006010 | 51662.8 | 50000 | 51686.8 | 51662.8 | 0 | 51686.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47809.9 | 47809.9 | 101923.8 | 1 | PROCESSED | 57612.4270138889 | 56956 | 56587.515474537 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080004 | To investigate (i)the influence of the merging event on IntraCluster Medium (ICM), We propose 40 ks+50 ks ~2 =140 ks observations of the linked region between Abell 399 and Abell 401. A399 (z=0.0724) and A401 (z=0.0737) are expected be in the initial phase of a cluster merger. With Suzaku fs high sensitivity observations, we will (i)determine the ICM physical conditions by measuring the temperature and density distribution, (ii) characterize the dynamical state of the cluster linked region, (iii) confirm the presence of a shock front predicted by numerical simulations. Our study will reveal the nature of initial phase of merging event of clusters of galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ISHISAKI | YOSHITAKA | NULL | NULL | JAP | 8 | AO8 | MORPHOLOGY AND PHYSICAL PROPERTIES OF SHOCKED GAS BY MAJOR MERGER IN THE LINKED REGION OF ABELL 399 AND ABELL 401 | XIS | Y |
| A399EAST | 44.8284 | 12.9677 | 164.75111172 | -39.30361408 | 72.1818 | 56529.3727777778 | 56530.5036921296 | 808007010 | 50276.8 | 50000 | 50292.8 | 50276.8 | 0 | 50300.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46303.9 | 46303.9 | 97684 | 0 | PROCESSED | 57612.4010069444 | 56956 | 56587.522349537 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080004 | To investigate (i)the influence of the merging event on IntraCluster Medium (ICM), We propose 40 ks+50 ks ~2 =140 ks observations of the linked region between Abell 399 and Abell 401. A399 (z=0.0724) and A401 (z=0.0737) are expected be in the initial phase of a cluster merger. With Suzaku fs high sensitivity observations, we will (i)determine the ICM physical conditions by measuring the temperature and density distribution, (ii) characterize the dynamical state of the cluster linked region, (iii) confirm the presence of a shock front predicted by numerical simulations. Our study will reveal the nature of initial phase of merging event of clusters of galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | ISHISAKI | YOSHITAKA | NULL | NULL | JAP | 8 | AO8 | MORPHOLOGY AND PHYSICAL PROPERTIES OF SHOCKED GAS BY MAJOR MERGER IN THE LINKED REGION OF ABELL 399 AND ABELL 401 | XIS | Y |
| A2744_NE | 3.7189 | -30.3078 | 9.14048559 | -81.37985976 | 233.5002 | 56616.3325694445 | 56618.5994791667 | 808008010 | 82773 | 80000 | 82781 | 82781 | 0 | 82773 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 71736.5 | 71736.5 | 195837.7 | 2 | PROCESSED | 57613.443900463 | 56995 | 56629.7456481482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080005 | We propose an additional 80ks pointing to complete our mapping of A2744 out to large radii and constrain the thermodynamical history of the cluster growth. A2744 is a multiple merger, nicknamed Pandora's cluster. Our analysis of existing Suzaku data suggest that this cluster has an anisotropic temperature structure near the virial radius and there is not a simple correlation between temperature and surface mass density of member galaxies. With proposed observations, we can determine, for the first time, the temperature and entropy profiles near the radio relic in the northeast and further test a scenario of gas heating and shock propagation in the cluster outskirts. Suzaku is most suited for this study because of the lowest background and excellent sensitivity. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | OTA | NAOMI | NULL | NULL | JAP | 8 | AO8 | REVEALING THE THERMODYNAMICAL EVOLUTION IN THE PANDORA'S CLUSTER | XIS | Y |
| CYGNUS A SUB | 299.7227 | 40.8585 | 76.23979532 | 5.91406977 | 241.0006 | 56615.3145717593 | 56616.3224189815 | 808016010 | 42520.4 | 40000 | 42528.4 | 42528.4 | 0 | 42520.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38917.3 | 38917.3 | 87071.9 | 1 | PROCESSED | 57613.3640625 | 56995 | 56629.6679050926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080018 | We have observed a merging cluster Cygnus A in the Suzaku GO-3 with 45ks. This observation confirmed a hot region between the main and sub components. Furthermore, we found a gas velocity shift between the main and sub by about 2500 km/s. We believe that these are colliding with each other. The current result are limited by statistics and systematic uncertainty. To improve the accurary of the measurement and complete our study, we propose two additional observations located the main and sub components at the center of the FOV. These will provide the best chance to look into a merging cluster "in motion". | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | TAMURA | TAKAYUKI | NULL | NULL | JAP | 8 | AO8 | CYGNUS A CLUSTER: THE BEST MERGING SYSTEM FOR THE SUZAKU | XIS | Y |
| COMA SUBHALO1 | 195.4003 | 29.028 | 73.80298118 | 87.06170231 | 296.7987 | 56451.3782638889 | 56452.0681712963 | 808018010 | 31182.6 | 30000 | 31190.6 | 31182.6 | 0 | 31190.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28819.7 | 28819.7 | 59604 | 1 | PROCESSED | 57611.5003935185 | 56869 | 56503.6225462963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080023 | We propose to conduct multi-pointing observations of Coma cluster to cover massive dark matter subhalos, which are unveiled by weak gravitational lensing analysis. We aim to detect X-ray emission from the gas associated with the massive subhalos and measure these quantities with Suzaku/XIS. Large apparent size of the cluster enables us to clearly resolve X-ray emission from subhalo regions. Compared with our X-ray data around non-subhalo regions, we investigate the systematic effect of gas clumpiness on X-ray observables in the outskirts, which is of prime importance to conclude the universality of the entropy flatness in cluster outskirts. Therefore, our observation is a benefit for all public Suzaku/XIS data of cluster outskirts. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | OKABE | NOBUHIRO | NULL | NULL | JAP | 8 | AO8 | SUZAKU FOLLOW-UP OBSERVATION OF DARK MATTER SUBHALOS IN COMA CLUSTER | XIS | Y |
| COMA SUBHALO1 S | 195.2527 | 28.7629 | 71.19878606 | 87.32773157 | 296.8003 | 56452.0686458333 | 56452.5459490741 | 808019010 | 20480.8 | 20000 | 20488.8 | 20480.8 | 0 | 20496.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 21496.8 | 21496.8 | 41231.9 | 0 | PROCESSED | 57611.4938541667 | 56869 | 56503.6109606482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080023 | We propose to conduct multi-pointing observations of Coma cluster to cover massive dark matter subhalos, which are unveiled by weak gravitational lensing analysis. We aim to detect X-ray emission from the gas associated with the massive subhalos and measure these quantities with Suzaku/XIS. Large apparent size of the cluster enables us to clearly resolve X-ray emission from subhalo regions. Compared with our X-ray data around non-subhalo regions, we investigate the systematic effect of gas clumpiness on X-ray observables in the outskirts, which is of prime importance to conclude the universality of the entropy flatness in cluster outskirts. Therefore, our observation is a benefit for all public Suzaku/XIS data of cluster outskirts. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | OKABE | NOBUHIRO | NULL | NULL | JAP | 8 | AO8 | SUZAKU FOLLOW-UP OBSERVATION OF DARK MATTER SUBHALOS IN COMA CLUSTER | XIS | Y |
| COMA SUBHALO2 | 194.5069 | 27.3689 | 42.63932899 | 88.51577103 | 315.0001 | 56452.5504976852 | 56453.0265046296 | 808020010 | 21156.3 | 20000 | 21156.3 | 21156.3 | 0 | 21156.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17608 | 17608 | 41119.9 | 1 | PROCESSED | 57611.5058564815 | 56872 | 56506.7547222222 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080023 | We propose to conduct multi-pointing observations of Coma cluster to cover massive dark matter subhalos, which are unveiled by weak gravitational lensing analysis. We aim to detect X-ray emission from the gas associated with the massive subhalos and measure these quantities with Suzaku/XIS. Large apparent size of the cluster enables us to clearly resolve X-ray emission from subhalo regions. Compared with our X-ray data around non-subhalo regions, we investigate the systematic effect of gas clumpiness on X-ray observables in the outskirts, which is of prime importance to conclude the universality of the entropy flatness in cluster outskirts. Therefore, our observation is a benefit for all public Suzaku/XIS data of cluster outskirts. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | OKABE | NOBUHIRO | NULL | NULL | JAP | 8 | AO8 | SUZAKU FOLLOW-UP OBSERVATION OF DARK MATTER SUBHALOS IN COMA CLUSTER | XIS | Y |
| COMA SUBHALO3 | 193.9804 | 27.7549 | 65.39722549 | 88.82429581 | 314.9967 | 56453.0272569444 | 56453.5912384259 | 808021010 | 24044.1 | 20000 | 24052.1 | 24044.1 | 0 | 24052.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 25533.4 | 25533.4 | 48697.9 | 0 | PROCESSED | 57611.5202199074 | 56872 | 56506.7633101852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080023 | We propose to conduct multi-pointing observations of Coma cluster to cover massive dark matter subhalos, which are unveiled by weak gravitational lensing analysis. We aim to detect X-ray emission from the gas associated with the massive subhalos and measure these quantities with Suzaku/XIS. Large apparent size of the cluster enables us to clearly resolve X-ray emission from subhalo regions. Compared with our X-ray data around non-subhalo regions, we investigate the systematic effect of gas clumpiness on X-ray observables in the outskirts, which is of prime importance to conclude the universality of the entropy flatness in cluster outskirts. Therefore, our observation is a benefit for all public Suzaku/XIS data of cluster outskirts. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | OKABE | NOBUHIRO | NULL | NULL | JAP | 8 | AO8 | SUZAKU FOLLOW-UP OBSERVATION OF DARK MATTER SUBHALOS IN COMA CLUSTER | XIS | Y |
| COMA SUBHALO4 | 193.8668 | 27.5167 | 56.62578598 | 89.02439779 | 314.9971 | 56453.5916666667 | 56454.1370717593 | 808022010 | 23809.1 | 20000 | 23809.1 | 23833.1 | 0 | 23817.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19619.5 | 19619.5 | 47113.9 | 0 | PROCESSED | 57611.5223958333 | 56830 | 56464.6326041667 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080023 | We propose to conduct multi-pointing observations of Coma cluster to cover massive dark matter subhalos, which are unveiled by weak gravitational lensing analysis. We aim to detect X-ray emission from the gas associated with the massive subhalos and measure these quantities with Suzaku/XIS. Large apparent size of the cluster enables us to clearly resolve X-ray emission from subhalo regions. Compared with our X-ray data around non-subhalo regions, we investigate the systematic effect of gas clumpiness on X-ray observables in the outskirts, which is of prime importance to conclude the universality of the entropy flatness in cluster outskirts. Therefore, our observation is a benefit for all public Suzaku/XIS data of cluster outskirts. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | OKABE | NOBUHIRO | NULL | NULL | JAP | 8 | AO8 | SUZAKU FOLLOW-UP OBSERVATION OF DARK MATTER SUBHALOS IN COMA CLUSTER | XIS | Y |
| AWM7 NW1 | 42.8658 | 41.9211 | 145.6578115 | -15.59334332 | 257 | 56705.5358680556 | 56705.8668287037 | 808023010 | 14857.6 | 15000 | 14889.6 | 14857.6 | 0 | 14873.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11008.8 | 11008.8 | 28583.9 | 1 | PROCESSED | 57613.8366550926 | 57085 | 56719.7185532407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080034 | We propose to observe AWM 7 cluster at 0.4--0.9 r180 toward northwest and southeast with 4 pointing observations (15 ks x 2+35 ks x 2) and a background field with 20 ks exposure. These directions are between a filament and a void directions and free from systematic errors caused by stray light. The objective is to derive metal-mass-to-light ratios out to the virial radius, and constrain the slope of the initial mass function of stars in early-type galaxies in clusters of galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MATSUSHITA | KYOKO | NULL | NULL | JAP | 8 | AO8 | METAL-MASS-TO-LIGHT RATIOS OUT TO THE VIRIAL RADIUS OF THE AWM 7 CLUSTER | XIS | Y |
| AWM7 NW2 | 42.4678 | 42.1132 | 145.29354682 | -15.55850289 | 257.0018 | 56705.8674421296 | 56706.6667824074 | 808024010 | 35333 | 35000 | 35341 | 35333 | 0 | 35349 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30059.6 | 30059.6 | 69055.9 | 0 | PROCESSED | 57613.8687268518 | 57130 | 56764.8062847222 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080034 | We propose to observe AWM 7 cluster at 0.4--0.9 r180 toward northwest and southeast with 4 pointing observations (15 ks x 2+35 ks x 2) and a background field with 20 ks exposure. These directions are between a filament and a void directions and free from systematic errors caused by stray light. The objective is to derive metal-mass-to-light ratios out to the virial radius, and constrain the slope of the initial mass function of stars in early-type galaxies in clusters of galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MATSUSHITA | KYOKO | NULL | NULL | JAP | 8 | AO8 | METAL-MASS-TO-LIGHT RATIOS OUT TO THE VIRIAL RADIUS OF THE AWM 7 CLUSTER | XIS | Y |
| AWM7 SE1 | 44.3556 | 41.1876 | 147.03812428 | -15.71286613 | 256.9997 | 56706.6681828704 | 56707.1284953704 | 808025010 | 16819.4 | 15000 | 16819.4 | 16843.4 | 0 | 16827.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15321 | 15321 | 39761.9 | 0 | PROCESSED | 57613.8533912037 | 57085 | 56719.747662037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080034 | We propose to observe AWM 7 cluster at 0.4--0.9 r180 toward northwest and southeast with 4 pointing observations (15 ks x 2+35 ks x 2) and a background field with 20 ks exposure. These directions are between a filament and a void directions and free from systematic errors caused by stray light. The objective is to derive metal-mass-to-light ratios out to the virial radius, and constrain the slope of the initial mass function of stars in early-type galaxies in clusters of galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MATSUSHITA | KYOKO | NULL | NULL | JAP | 8 | AO8 | METAL-MASS-TO-LIGHT RATIOS OUT TO THE VIRIAL RADIUS OF THE AWM 7 CLUSTER | XIS | Y |
| AWM7 SE2 | 44.7376 | 40.9954 | 147.39655193 | -15.74105021 | 257.0003 | 56707.1291319444 | 56707.9132407407 | 808026010 | 35304 | 35000 | 35304 | 35316 | 0 | 35308 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 31177.8 | 31177.8 | 67742 | 4 | PROCESSED | 57613.8746064815 | 57085 | 56719.7754398148 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080034 | We propose to observe AWM 7 cluster at 0.4--0.9 r180 toward northwest and southeast with 4 pointing observations (15 ks x 2+35 ks x 2) and a background field with 20 ks exposure. These directions are between a filament and a void directions and free from systematic errors caused by stray light. The objective is to derive metal-mass-to-light ratios out to the virial radius, and constrain the slope of the initial mass function of stars in early-type galaxies in clusters of galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MATSUSHITA | KYOKO | NULL | NULL | JAP | 8 | AO8 | METAL-MASS-TO-LIGHT RATIOS OUT TO THE VIRIAL RADIUS OF THE AWM 7 CLUSTER | XIS | Y |
| AWM7 BGD | 41.6937 | 42.4876 | 144.58796377 | -15.48250354 | 257.001 | 56707.9150810185 | 56708.3828587963 | 808027010 | 20497.1 | 20000 | 20501.1 | 20505.1 | 0 | 20497.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 22116 | 22116 | 40410 | 0 | PROCESSED | 57613.8622106482 | 57086 | 56720.6154976852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080034 | We propose to observe AWM 7 cluster at 0.4--0.9 r180 toward northwest and southeast with 4 pointing observations (15 ks x 2+35 ks x 2) and a background field with 20 ks exposure. These directions are between a filament and a void directions and free from systematic errors caused by stray light. The objective is to derive metal-mass-to-light ratios out to the virial radius, and constrain the slope of the initial mass function of stars in early-type galaxies in clusters of galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MATSUSHITA | KYOKO | NULL | NULL | JAP | 8 | AO8 | METAL-MASS-TO-LIGHT RATIOS OUT TO THE VIRIAL RADIUS OF THE AWM 7 CLUSTER | XIS | Y |
| A3376 EAST | 90.8243 | -39.9606 | 246.56739968 | -25.79165375 | 80.8001 | 56549.3239699074 | 56551.6953472222 | 808028010 | 81573.4 | 81000 | 81573.4 | 81573.4 | 0 | 81573.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 75181.4 | 75181.4 | 204857.8 | 2 | PROCESSED | 57612.6739467593 | 56956 | 56588.6883449074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080037 | Abell 3376 (z=0.046) is a peculiar merging cluster with giant double radio relics. High sensitivity of the XIS will enable us (i) to determine the temperature and density distributions around the shock accompanying the east relic, and (ii) to examine how thermal and non-thermal energies separate and go into the respective particles. Wide coverage will allow us to compare the ICM properties along the shock and non-shock directions. The low redshift of the source will allow XIS data to resolve detailed shock-related structures. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | OHASHI | TAKAYA | NULL | NULL | JAP | 8 | AO8 | SUZAKU OBSERVATION OF THE EAST MERGER SHOCK AND RADIO RELIC IN ABELL 3376 | XIS | Y |
| A3376 NORTH | 90.6541 | -39.7108 | 246.26196714 | -25.85404299 | 80.8001 | 56553.3109143518 | 56554.8453935185 | 808029010 | 57691.2 | 57000 | 57691.2 | 57699.2 | 0 | 57707.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 50818.5 | 50818.5 | 132570 | 0 | PROCESSED | 57612.703275463 | 56956 | 56588.7436689815 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080037 | Abell 3376 (z=0.046) is a peculiar merging cluster with giant double radio relics. High sensitivity of the XIS will enable us (i) to determine the temperature and density distributions around the shock accompanying the east relic, and (ii) to examine how thermal and non-thermal energies separate and go into the respective particles. Wide coverage will allow us to compare the ICM properties along the shock and non-shock directions. The low redshift of the source will allow XIS data to resolve detailed shock-related structures. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | OHASHI | TAKAYA | NULL | NULL | JAP | 8 | AO8 | SUZAKU OBSERVATION OF THE EAST MERGER SHOCK AND RADIO RELIC IN ABELL 3376 | XIS | Y |
| A3376 SOUTH | 90.6172 | -40.196 | 246.775776 | -26.0046965 | 124.8629 | 56580.8395486111 | 56582.2918055556 | 808030010 | 66534.6 | 57000 | 66534.7 | 66534.6 | 0 | 66534.6 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 56977.1 | 56977.1 | 125450 | 1 | PROCESSED | 57613.0188541667 | 57004 | 56637.6639351852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080037 | Abell 3376 (z=0.046) is a peculiar merging cluster with giant double radio relics. High sensitivity of the XIS will enable us (i) to determine the temperature and density distributions around the shock accompanying the east relic, and (ii) to examine how thermal and non-thermal energies separate and go into the respective particles. Wide coverage will allow us to compare the ICM properties along the shock and non-shock directions. The low redshift of the source will allow XIS data to resolve detailed shock-related structures. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | OHASHI | TAKAYA | NULL | NULL | JAP | 8 | AO8 | SUZAKU OBSERVATION OF THE EAST MERGER SHOCK AND RADIO RELIC IN ABELL 3376 | XIS | Y |
| A2255_NW | 258.0206 | 64.3236 | 94.26240936 | 34.95584628 | 200.0017 | 56613.0157060185 | 56613.9467476852 | 808039010 | 43768.8 | 40000 | 43768.8 | 43768.8 | 0 | 43768.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 41855.7 | 41855.7 | 80412.1 | 0 | PROCESSED | 57613.3414814815 | 56991 | 56625.6806481482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080047 | We propose to obtain high-quality X-ray spectra of two subcluster regions in A2255 aiming at detection of supersonic motion of the intracluster gas. Previous optical and X-ray observations suggest that A2255 is indeed in the process of merging and subclusters have high velocities relative to the main cluster. Utilizing the high-sensitivity Suzaku spectroscopy, the line-of-sight velocity of the X-ray emitting gas can be measured from the Doppler shift of iron-K lines. With additional 40ks/80ks observations of the NW/SE subclusters, we expect to detect significant bulk velocities for the first time in this cluster. This will enhance our understanding of the 3-dimensional structure of the object including line-of-sight gas velocities and the cluster dynamical evolution. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | YOSHIDA | HIROKO | NULL | NULL | JAP | 8 | AO8 | MAPPING GAS MOTIONS IN THE MERGING CLUSTER A2255 | XIS | Y |
| A2255_SE | 258.2963 | 63.8192 | 93.63129587 | 34.92006939 | 200.0025 | 56613.9474537037 | 56615.3084953704 | 808040010 | 64733 | 60000 | 64741 | 64741 | 0 | 64733 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 64886.5 | 64886.5 | 117587.9 | 1 | PROCESSED | 57613.3519097222 | 57029 | 56653.6890046296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080047 | We propose to obtain high-quality X-ray spectra of two subcluster regions in A2255 aiming at detection of supersonic motion of the intracluster gas. Previous optical and X-ray observations suggest that A2255 is indeed in the process of merging and subclusters have high velocities relative to the main cluster. Utilizing the high-sensitivity Suzaku spectroscopy, the line-of-sight velocity of the X-ray emitting gas can be measured from the Doppler shift of iron-K lines. With additional 40ks/80ks observations of the NW/SE subclusters, we expect to detect significant bulk velocities for the first time in this cluster. This will enhance our understanding of the 3-dimensional structure of the object including line-of-sight gas velocities and the cluster dynamical evolution. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | YOSHIDA | HIROKO | NULL | NULL | JAP | 8 | AO8 | MAPPING GAS MOTIONS IN THE MERGING CLUSTER A2255 | XIS | Y |
| FJ1 | 238.114 | 22.5674 | 36.86878642 | 48.89749971 | 115.0005 | 56698.0557638889 | 56701.0001851852 | 808041010 | 111845.7 | 100000 | 111853.7 | 111845.7 | 0 | 111853.7 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57613.8229166667 | 57130 | 56765.6012152778 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080054 | Filament Junctions are known to be the most active regions in structure formation in the Universe. These regions can be identified using our original method based on galaxy distribution. In AO8, we try to detect (1) a galaxy-scale halo with a radio relic structure often observed after merger and (2) a galaxy-scale halo just before merger at the Filament Junction. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MITSUISHI | IKUYUKI | NULL | NULL | JAP | 8 | AO8 | EXPLORING EVOLUTION OF GROUPS AT FILAMENT JUNCTIONS OF GALAXIES | XIS | Y |
| FORNAX A EAST LOBE | 51.0149 | -37.2799 | 240.23704173 | -56.41225665 | 91.5022 | 56506.6358564815 | 56510.623125 | 808043010 | 151462.6 | 150000 | 151486.6 | 151462.6 | 0 | 151494.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 134094.2 | 134094.2 | 344435.3 | 3 | PROCESSED | 57612.2277777778 | 56955 | 56587.7734259259 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080056 | We propose Suzaku observations of the Fornax A east radio lobe and the background region. In previous cycles, we observed the west lobe and detected thermal extended gas for the first time, in addition to the non-thermal emission known for decades (Seta PhD thesis, 2012). In order to reveal the relation between the AGN jet and the thermal gas, the additional data in the opposite side of the lobe is critically important. We aim to detect the thermal gas in the eastern lobe, too, and investigate the spatial difference of its temperature and surface brightness. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SETA | HIROMI | NULL | NULL | JAP | 8 | AO8 | COMPLETING THE MAPPING OBSERVATION OF FORNAX A RADIO LOBE | XIS | Y |
| FORNAX A LOBE BKG | 50.9375 | -37.5569 | 240.74738045 | -56.44161041 | 91.6954 | 56510.6236458333 | 56511.9333912037 | 808044010 | 54454.5 | 50000 | 54462.5 | 54454.5 | 0 | 54470.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46892.5 | 46892.5 | 113147.8 | 1 | PROCESSED | 57612.1934837963 | 56955 | 56587.7940046296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080056 | We propose Suzaku observations of the Fornax A east radio lobe and the background region. In previous cycles, we observed the west lobe and detected thermal extended gas for the first time, in addition to the non-thermal emission known for decades (Seta PhD thesis, 2012). In order to reveal the relation between the AGN jet and the thermal gas, the additional data in the opposite side of the lobe is critically important. We aim to detect the thermal gas in the eastern lobe, too, and investigate the spatial difference of its temperature and surface brightness. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SETA | HIROMI | NULL | NULL | JAP | 8 | AO8 | COMPLETING THE MAPPING OBSERVATION OF FORNAX A RADIO LOBE | XIS | Y |
| N4438 TAIL | 186.7653 | 12.9509 | 279.81897455 | 74.71807646 | 119.2941 | 56636.4959259259 | 56639.0884259259 | 808045010 | 102773.8 | 100000 | 102773.8 | 102773.8 | 0 | 102773.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 92834.2 | 92834.2 | 223962 | 2 | PROCESSED | 57613.6203587963 | 57016 | 56650.8089583333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080059 | We propose a 100 ks XIS observation to the Halpha/X-ray filament connecting N4438 and M86 in the Virgo cluster. Our main objective is to probe conclusively the OVII line which is marginally detected with the XMM-Newton. If established, by employing line diagnostic and non-equilibrium ionization analysis, we will be able to determine the ionization temperature and elapsed timescale of the multi-phase ISM stripped from N4438, and give constraint on the thermal conductivity and metal enrichment of the ICM. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | GU | LIYI | NULL | NULL | JAP | 8 | AO8 | A SUZAKU OBSERVATION OF ONGOING IONIZATION OF ISM IN THE VIRGO CLUSTER ICM | XIS | Y |
| 3C390.3_VICINITY_1 | 276.9861 | 79.7253 | 111.37115096 | 27.70478895 | 240.0064 | 56607.4234953704 | 56608.4910648148 | 808046010 | 57710 | 50000 | 57710 | 57720 | 0 | 57714.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 52940.8 | 52940.8 | 92231.9 | 1 | PROCESSED | 57613.2938425926 | 56991 | 56625.6961458333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080060 | We propose for observations of the vicinities of 3C 390.3 and Fairall 9, in order to constrain the origins of 'excess' emission in the soft X-ray diffuse background observed with Suzaku and to confirm its possible relation to high velocity clouds (HVCs). We have been observing blank-skies in many directions and studying a oxygen emission from the Galactic halo. Intensities of the emission show a uniform value in most of directions; however in some directions we can see an excess, which possibly originate to a blob-like high density gas and/or a distribution of HVCs. By conducting a joint analysis of absorption and emission lines, we can characterize the roots of the excess emission. Moreover, the joint analysis even constraints a density of the origins, which has never been done until now. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | SAKAI | KAZUHIRO | NULL | NULL | JAP | 8 | AO8 | DO HIGH VELOCITY CLOUDS HEAT THE HALO OF OUR GALAXY? | XIS | Y |
| 3C390.3_VICINITY_2 | 284.1264 | 79.7065 | 111.42410994 | 26.43157038 | 239.9994 | 56608.493900463 | 56609.4897222222 | 808047010 | 52885.6 | 50000 | 52906.6 | 52893.6 | 0 | 52885.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48401.3 | 48401.3 | 86031.9 | 0 | PROCESSED | 57613.3036111111 | 56991 | 56625.7010648148 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080060 | We propose for observations of the vicinities of 3C 390.3 and Fairall 9, in order to constrain the origins of 'excess' emission in the soft X-ray diffuse background observed with Suzaku and to confirm its possible relation to high velocity clouds (HVCs). We have been observing blank-skies in many directions and studying a oxygen emission from the Galactic halo. Intensities of the emission show a uniform value in most of directions; however in some directions we can see an excess, which possibly originate to a blob-like high density gas and/or a distribution of HVCs. By conducting a joint analysis of absorption and emission lines, we can characterize the roots of the excess emission. Moreover, the joint analysis even constraints a density of the origins, which has never been done until now. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | SAKAI | KAZUHIRO | NULL | NULL | JAP | 8 | AO8 | DO HIGH VELOCITY CLOUDS HEAT THE HALO OF OUR GALAXY? | XIS | Y |
| A2199_NE | 247.516 | 39.7841 | 63.26645529 | 43.42583068 | 143.5992 | 56661.6024074074 | 56662.5572222222 | 808050010 | 44163.1 | 40000 | 44171.1 | 44163.1 | 0 | 44171.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42353.1 | 42353.1 | 82491.9 | 1 | PROCESSED | 57613.7484953704 | 57079 | 56713.7287037037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080067 | We propose to complete pointing observations to cover the entire region of Abell 2199 cluster. Suzaku has performed 21 pointing observations of Abell 2199 cluster (z=0.03), showing remarkable features in the temperature and entropy distributions with high physical resolution, as ``Suzaku AO-6 keyproject'' we proposed. Our target is the only cluster to cover the whole region, achieved solely by Suzaku/XIS among currently available facilities. Therefore, this project can provide us an exquisite, complete information of the cluster gas with the high physical resolution, which would be used as unsurpassed, legacy-type dataset in the X-ray cluster community. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | SATO | KOSUKE | NULL | NULL | JAP | 8 | AO8 | COMPLETING THE SUZAKU LEGACY MOSAIC OF ABELL 2199 CLUSTER TO THE VIRIAL RADIUS | XIS | Y |
| A2199_FE | 248.2855 | 39.6383 | 63.09452591 | 42.82923772 | 143.2418 | 56662.5581597222 | 56663.4606944444 | 808051010 | 40354.8 | 40000 | 40370.8 | 40354.8 | 0 | 40371.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 39811.9 | 39811.9 | 77967.9 | 1 | PROCESSED | 57613.7559490741 | 57085 | 56719.7506597222 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080067 | We propose to complete pointing observations to cover the entire region of Abell 2199 cluster. Suzaku has performed 21 pointing observations of Abell 2199 cluster (z=0.03), showing remarkable features in the temperature and entropy distributions with high physical resolution, as ``Suzaku AO-6 keyproject'' we proposed. Our target is the only cluster to cover the whole region, achieved solely by Suzaku/XIS among currently available facilities. Therefore, this project can provide us an exquisite, complete information of the cluster gas with the high physical resolution, which would be used as unsurpassed, legacy-type dataset in the X-ray cluster community. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | SATO | KOSUKE | NULL | NULL | JAP | 8 | AO8 | COMPLETING THE SUZAKU LEGACY MOSAIC OF ABELL 2199 CLUSTER TO THE VIRIAL RADIUS | XIS | Y |
| NGC 253 | 11.9272 | -25.3509 | 97.52826827 | -88.03578801 | 242.9951 | 56643.3716203704 | 56645.502962963 | 808053010 | 99686.4 | 100000 | 99686.4 | 99686.4 | 0 | 99686.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 98564.2 | 98564.2 | 184103.8 | 0 | PROCESSED | 57613.6331481482 | 57031 | 56664.7662962963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080070 | We propose the observation of edge-on starburst galaxies NGC253 and NGC 2146 for 150 ks and 100 ks, respectively. One of the mechanisms that promote the chemical evolution of the universe, starburst outflows have been studied from both aspects of multi-wavelength observations and theory so far. Suzaku original attempts focusing on the abundance patterns has given new insights for a starburst-driven outflow scenario. In AO8, we try to extract the abundance pattern from the south region in NGC 253 and the central region in NGC 2146. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | SATO | TOSHIKI | NULL | NULL | JAP | 8 | AO8 | OBSERVATION OF EDGE-ON STARBURST GALAXIES NGC 253 & NGC 2146 | XIS | Y |
| BULLET-OFFSET1 | 104.8831 | -55.8434 | 265.96507608 | -21.0808269 | 287.0003 | 56416.3315277778 | 56419.0787037037 | 808055010 | 102917.2 | 100000 | 102941.2 | 102917.2 | 0 | 102941.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 93439.5 | 93439.5 | 237316.7 | 4 | PROCESSED | 57611.2833564815 | 56795 | 56429.7533101852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080080 | We propose two offset pointings of the bullet cluster with one adjacent blank-sky pointing. By detecting a very hot component in the ICM and mapping temperature/entropy out to the outskirts, we study thermodynamical evolution of the ICM in the course of cluster merger. More specifically, we estimate the fraction of energy injected to the ICM from the energy released by the merger, and the amount of energy heating the ICM through the shock, irreversible process. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KAWAHARADA | MADOKA | NULL | NULL | JAP | 8 | AO8 | THERMODYNAMICAL EVOLUTION OF THE ICM IN THE BULLET CLUSTER | XIS | Y |
| BULLET-OFFSET2 | 104.4232 | -55.8309 | 265.86935635 | -21.32349548 | 287.0017 | 56419.6209722222 | 56422.4605439815 | 808056010 | 101385.5 | 100000 | 101393.5 | 101393.5 | 0 | 101385.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 93676.7 | 93676.7 | 245305.8 | 2 | PROCESSED | 57611.3171643518 | 56799 | 56433.6998958333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080080 | We propose two offset pointings of the bullet cluster with one adjacent blank-sky pointing. By detecting a very hot component in the ICM and mapping temperature/entropy out to the outskirts, we study thermodynamical evolution of the ICM in the course of cluster merger. More specifically, we estimate the fraction of energy injected to the ICM from the energy released by the merger, and the amount of energy heating the ICM through the shock, irreversible process. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KAWAHARADA | MADOKA | NULL | NULL | JAP | 8 | AO8 | THERMODYNAMICAL EVOLUTION OF THE ICM IN THE BULLET CLUSTER | XIS | Y |
| BULLET-BKG | 105.498 | -55.9182 | 266.15428465 | -20.7753384 | 287.5121 | 56422.4617592593 | 56424.0029976852 | 808057010 | 51090.7 | 50000 | 51098.7 | 51090.7 | 0 | 51106.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46693.8 | 46693.8 | 133149.6 | 0 | PROCESSED | 57611.3081365741 | 56799 | 56433.6980208333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080080 | We propose two offset pointings of the bullet cluster with one adjacent blank-sky pointing. By detecting a very hot component in the ICM and mapping temperature/entropy out to the outskirts, we study thermodynamical evolution of the ICM in the course of cluster merger. More specifically, we estimate the fraction of energy injected to the ICM from the energy released by the merger, and the amount of energy heating the ICM through the shock, irreversible process. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | KAWAHARADA | MADOKA | NULL | NULL | JAP | 8 | AO8 | THERMODYNAMICAL EVOLUTION OF THE ICM IN THE BULLET CLUSTER | XIS | Y |
| A3627_NORTH | 243.656 | -60.6115 | 325.45745985 | -6.96421785 | 306.0001 | 56545.808912037 | 56546.5556828704 | 808058010 | 51899.6 | 50000 | 51931.6 | 51923.6 | 0 | 51899.6 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 43028.4 | 43028.4 | 64511.9 | 1 | PROCESSED | 57612.6119097222 | 56956 | 56588.8328935185 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080097 | We propose to observe the north-west region in nearby merging cluster Abell 3627. Suzaku observation in AO-3 found a subcluster colliding into the main body from the south-east direction and a hard X-ray component above 12 keV probably originated from the north-west region. The region has also peculiar structures such as long X-ray/radio tails, suggesting a relation with the cluster merging. In order to understand the process of cluster merging taking into accout the hard X-ray component and these peculiar structures, we will measure the temperature and pressure distributions in the north-west region using the low background of XIS. We will also study the non-thermal emission using HXD and investigate a possibililty of the particle acceleration in Abell 3627. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | HAYASHI | KATSUHIRO | NULL | NULL | JAP | 8 | AO8 | OBSERVATION OF THE NORTH-WEST REGION IN NEARBY MERGING CLUSTER ABELL 3627 | XIS | Y |
| A3627_WEST | 243.1701 | -60.6984 | 325.22376786 | -6.86207305 | 306.0002 | 56546.5563425926 | 56547.2535185185 | 808059010 | 52799.8 | 50000 | 52799.8 | 52823.7 | 0 | 52807.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42896.8 | 42896.8 | 60231.9 | 0 | PROCESSED | 57612.5956481482 | 56956 | 56588.7134837963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080097 | We propose to observe the north-west region in nearby merging cluster Abell 3627. Suzaku observation in AO-3 found a subcluster colliding into the main body from the south-east direction and a hard X-ray component above 12 keV probably originated from the north-west region. The region has also peculiar structures such as long X-ray/radio tails, suggesting a relation with the cluster merging. In order to understand the process of cluster merging taking into accout the hard X-ray component and these peculiar structures, we will measure the temperature and pressure distributions in the north-west region using the low background of XIS. We will also study the non-thermal emission using HXD and investigate a possibililty of the particle acceleration in Abell 3627. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | HAYASHI | KATSUHIRO | NULL | NULL | JAP | 8 | AO8 | OBSERVATION OF THE NORTH-WEST REGION IN NEARBY MERGING CLUSTER ABELL 3627 | XIS | Y |
| NGC1550_45OFFSET_E | 65.5544 | 2.4106 | 191.40103429 | -31.31407553 | 260.0002 | 56696.1115393518 | 56697.3543634259 | 808060010 | 53049.6 | 50000 | 53049.6 | 53049.6 | 0 | 53049.6 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57613.8049421296 | 57075 | 56709.7114351852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080110 | We propose to study the entropy profile and the metal enrichment process of the fossil group, NGC 1550 with total 170 ksec observations. NGC 1550 is a bright nearby group (z=0.0124), and classified as a fossil group which has no bright galaxies except for a central elliptical galaxy. Fossil groups, therefore, are a very useful system for investigating how the ICM metals have been enriched from galaxies. On the other hand, it is known that the entropy of groups has a several times larger than that of clusters within ~0.2 r180, and has similar value to clusters at 0.5 r180. However, in r > 0.5 r180 region, the entropy profile of groups has not been observed yet, while those of clusters have shown a flatter slope than the expected value from simulations in the Suzaku results. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | SASAKI | TORU | NULL | NULL | JAP | 8 | AO8 | STUDY OF THE ENTROPY PROFILE AND THE METAL ENRICHMENT PROCESS IN THE FOSSIL GROUP, NGC~1550 | XIS | Y |
| NGC1550_BGD | 66.1553 | 2.4144 | 191.78857248 | -30.8138174 | 260.0006 | 56697.3550694444 | 56698.0418634259 | 808061010 | 31145.6 | 30000 | 31153.6 | 31153.6 | 0 | 31145.6 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57613.8043171296 | 57102 | 56736.7213425926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 080110 | We propose to study the entropy profile and the metal enrichment process of the fossil group, NGC 1550 with total 170 ksec observations. NGC 1550 is a bright nearby group (z=0.0124), and classified as a fossil group which has no bright galaxies except for a central elliptical galaxy. Fossil groups, therefore, are a very useful system for investigating how the ICM metals have been enriched from galaxies. On the other hand, it is known that the entropy of groups has a several times larger than that of clusters within ~0.2 r180, and has similar value to clusters at 0.5 r180. However, in r > 0.5 r180 region, the entropy profile of groups has not been observed yet, while those of clusters have shown a flatter slope than the expected value from simulations in the Suzaku results. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | SASAKI | TORU | NULL | NULL | JAP | 8 | AO8 | STUDY OF THE ENTROPY PROFILE AND THE METAL ENRICHMENT PROCESS IN THE FOSSIL GROUP, NGC~1550 | XIS | Y |
| ESO318-021 | 163.2697 | -40.3328 | 279.73310675 | 17.14745123 | 111.1499 | 56639.0964467593 | 56643.3605902778 | 808063010 | 152219.8 | 150000 | 152219.8 | 152219.8 | 0 | 152219.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 132973.3 | 132973.3 | 368377.7 | 4 | PROCESSED | 57613.6558101852 | 57050 | 56680.7667476852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081503 | The mass profiles of elliptical galaxies are important probes of galaxy formation and cosmology. Only a few elliptical galaxies have detailed mass measurements from X-rays because of the lack of suitable targets in terms of total mass (< ~10^{13} m_sun) and relaxed dynamical states appropriate for hydrostatic analysis. We have identified a sample of (hot) gas-rich isolated elliptical galaxies, most of which were discovered from previously awarded XMM and Chandra snapshot programs to search for optimal targets for X-ray studies of mass profiles on the galaxy scale. We request Suzaku observations to map the detailed profiles of stars, dark matter, and hot gas in two of these galaxies which have (scheduled) complementary Chandra observations. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | BUOTE | DAVID | NULL | NULL | USA | 8 | AO8 | THE DARK MATTER AND BARYON PROFILES OF ISOLATED ELLIPTICAL GALAXIES | XIS | Y |
| RXJ1416.4+2315 | 214.0623 | 23.3458 | 26.46691952 | 70.47697816 | 292.671 | 56496.6431712963 | 56499.3349074074 | 808064010 | 122931.7 | 120000 | 122931.7 | 122931.7 | 0 | 122931.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 116822.6 | 116822.6 | 232547.4 | 2 | PROCESSED | 57612.032650463 | 56953 | 56587.4880671296 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081511 | Our preliminary analysis of AO7 XIS data of the fossil cluster RXJ 1416.4+2315 does not find evidence for the gas clumping invoked to explain the flat entropy profiles and large gas fractions found near r_vir in several nearby clusters. Instead its ICM properties at r_vir are consistent with adiabatic cluster formation as we found previously for the fossil group/cluster RXJ 1159+5531, which may reflect that hydrostatic equilibrium is very accurate in these highly evolved fossil systems. Therefore, we propose a Suzaku observation in a different azimuthal direction to double the azimuthal coverage at r_vir (from ~30% to ~60%) in order to test for the presence of azimuthal ICM variations expected for clusters that grow by accretion along large-scale filaments. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | BUOTE | DAVID | NULL | NULL | USA | 8 | AO8 | VERIFYING RELAXED ICM AT THE VIRIAL RADIUS IN A FOSSIL GALAXY CLUSTER | XIS | Y |
| MKW4-W2 | 181.7129 | 1.8545 | 278.14148217 | 62.56052834 | 136.8029 | 56652.6158217593 | 56655.3919097222 | 808065010 | 102601.1 | 100000 | 102601.1 | 102601.1 | 0 | 102601.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 88697.7 | 88697.7 | 239825.8 | 1 | PROCESSED | 57613.7424421296 | 57079 | 56700.7408449074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081512 | We propose to observe the MKW4 group by leveraging existing observations to provide coverage from its center to its virial radius in two orthogonal directions. Three additional pointings, totaling 230 ksec, combined with two existing pointings, will allow us to determine radial profiles of gas temperature, density, entropy, pressure, and gas mass fraction, as well as their azimuthal variations. Comparing these properties to those of clusters will allow us to probe the role played by baryonic physics and assess the imprints of hierarchical structure formation. The stable and low background of the Suzaku XIS is crucial for the study of galaxy groups to their virial radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | SU | YUANYUAN | NULL | NULL | USA | 8 | AO8 | PROBING A TYPICAL GALAXY GROUP TO ITS VIRAL RADIUS | XIS | Y |
| MKW4 | 181.137 | 1.9141 | 276.9409609 | 62.39583381 | 136.3986 | 56655.392662037 | 56656.271099537 | 808066010 | 34570 | 30000 | 34570 | 34570 | 0 | 34570 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30143.5 | 30143.5 | 75887.9 | 0 | PROCESSED | 57613.7104861111 | 57033 | 56667.6362268518 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081512 | We propose to observe the MKW4 group by leveraging existing observations to provide coverage from its center to its virial radius in two orthogonal directions. Three additional pointings, totaling 230 ksec, combined with two existing pointings, will allow us to determine radial profiles of gas temperature, density, entropy, pressure, and gas mass fraction, as well as their azimuthal variations. Comparing these properties to those of clusters will allow us to probe the role played by baryonic physics and assess the imprints of hierarchical structure formation. The stable and low background of the Suzaku XIS is crucial for the study of galaxy groups to their virial radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | SU | YUANYUAN | NULL | NULL | USA | 8 | AO8 | PROBING A TYPICAL GALAXY GROUP TO ITS VIRAL RADIUS | XIS | Y |
| MKW-N2 | 181.1507 | 2.5267 | 276.44275792 | 62.96433079 | 120.2659 | 56663.6701967593 | 56666.0195023148 | 808067010 | 99788.3 | 100000 | 99788.3 | 99788.3 | 0 | 99788.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 99936.2 | 99936.2 | 202953.7 | 4 | PROCESSED | 57613.8221643518 | 57096 | 56730.5704166667 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081512 | We propose to observe the MKW4 group by leveraging existing observations to provide coverage from its center to its virial radius in two orthogonal directions. Three additional pointings, totaling 230 ksec, combined with two existing pointings, will allow us to determine radial profiles of gas temperature, density, entropy, pressure, and gas mass fraction, as well as their azimuthal variations. Comparing these properties to those of clusters will allow us to probe the role played by baryonic physics and assess the imprints of hierarchical structure formation. The stable and low background of the Suzaku XIS is crucial for the study of galaxy groups to their virial radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | SU | YUANYUAN | NULL | NULL | USA | 8 | AO8 | PROBING A TYPICAL GALAXY GROUP TO ITS VIRAL RADIUS | XIS | Y |
| ABELL 3112 | 49.4982 | -44.2507 | 252.95298598 | -56.06981795 | 43.5004 | 56466.5743634259 | 56468.5418055556 | 808068010 | 119124.7 | 200000 | 119124.7 | 119124.7 | 0 | 119124.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 114561.8 | 114561.8 | 169941.8 | 0 | PROCESSED | 57611.6340856482 | 56848 | 56481.8003356482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081522 | The hot X-ray emitting gas in clusters of galaxies is a very large repository of metals produced by stars and galaxies. These metals enter the intra-cluster medium (ICM) via strong galactic winds, supernovae explosions, and ram-pressure stripping. However, the details of the mechanisms that transport metals to the ICM and the origin of these metals remain still unclear. We aim to accurately measure the temperature and abundance patterns of a bright nearby galaxy cluster A3112 out to the virial radius and compare these data with metal abundance yields produced by supernovae. Our proposed observation will provide information about how these metals are created, as well as how and when the metals were transported to the ICM. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | BULBUL | ESRA | NULL | NULL | USA | 8 | AO8 | CHEMICAL EVOLUTION HISTORY OF A COOL CORE CLUSTER A3112 OUT TO THE VIRIAL RADIUS | XIS | Y |
| ABELL 3112 | 49.4972 | -44.2507 | 252.95338075 | -56.0704995 | 43.5006 | 56468.5418171296 | 56469.5834259259 | 808068020 | 65397.7 | 200000 | 65405.7 | 65405.7 | 0 | 65397.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 54074.4 | 54074.4 | 89983.8 | 1 | PROCESSED | 57611.633912037 | 56848 | 56481.7677083333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081522 | The hot X-ray emitting gas in clusters of galaxies is a very large repository of metals produced by stars and galaxies. These metals enter the intra-cluster medium (ICM) via strong galactic winds, supernovae explosions, and ram-pressure stripping. However, the details of the mechanisms that transport metals to the ICM and the origin of these metals remain still unclear. We aim to accurately measure the temperature and abundance patterns of a bright nearby galaxy cluster A3112 out to the virial radius and compare these data with metal abundance yields produced by supernovae. Our proposed observation will provide information about how these metals are created, as well as how and when the metals were transported to the ICM. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | BULBUL | ESRA | NULL | NULL | USA | 8 | AO8 | CHEMICAL EVOLUTION HISTORY OF A COOL CORE CLUSTER A3112 OUT TO THE VIRIAL RADIUS | XIS | Y |
| A133_FIELD_1 | 15.9453 | -21.6335 | 150.67449532 | -83.82895318 | 231.9994 | 56645.5063078704 | 56646.6683449074 | 808081010 | 53648.3 | 50000 | 53664.3 | 53648.3 | 0 | 53664.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 52651.2 | 52651.2 | 100387.9 | 1 | PROCESSED | 57613.6155439815 | 57061 | 56695.6487152778 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081525 | We propose observations of the outskirts of Abell 133, a relaxed galaxy cluster that is the target of a Chandra X-ray Visionary Project. These modest Suzaku observations will leverage the 2.4 Msec of Chandra time spent deeply imaging the region beyond r_500 to search for ICM clumping. Such clumping has been invoked to explain the flat entropy profiles and excess inferred gas fraction beyond r_500 in several clusters observed recently with Suzaku. The proposed Suzaku observations combined with the unprecedented Chandra depth will create a fiducial dataset to compare to the existing Suzaku cluster outskirts data, and they will definitely determine whether the excess inferred gas fractions seen with Suzaku arise from gas clumping. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MILLER | ERIC | NULL | NULL | USA | 8 | AO8 | A DEFINITIVE STUDY OF GALAXY CLUSTER OUTSKIRTS WITH SUZAKU AND CHANDRA | XIS | Y |
| A133_FIELD_2 | 15.4723 | -21.5865 | 146.72727626 | -83.96930246 | 231.9996 | 56646.6689583333 | 56647.8294212963 | 808082010 | 50640.6 | 50000 | 50664.6 | 50656.6 | 0 | 50640.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46433.8 | 46433.8 | 100255.9 | 1 | PROCESSED | 57613.6561921296 | 57061 | 56695.6286689815 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081525 | We propose observations of the outskirts of Abell 133, a relaxed galaxy cluster that is the target of a Chandra X-ray Visionary Project. These modest Suzaku observations will leverage the 2.4 Msec of Chandra time spent deeply imaging the region beyond r_500 to search for ICM clumping. Such clumping has been invoked to explain the flat entropy profiles and excess inferred gas fraction beyond r_500 in several clusters observed recently with Suzaku. The proposed Suzaku observations combined with the unprecedented Chandra depth will create a fiducial dataset to compare to the existing Suzaku cluster outskirts data, and they will definitely determine whether the excess inferred gas fractions seen with Suzaku arise from gas clumping. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | MILLER | ERIC | NULL | NULL | USA | 8 | AO8 | A DEFINITIVE STUDY OF GALAXY CLUSTER OUTSKIRTS WITH SUZAKU AND CHANDRA | XIS | Y |
| A133_FIELD_3 | 15.3292 | -22.0955 | 147.50079252 | -84.48957915 | 231.9998 | 56631.4102314815 | 56632.6168981482 | 808083010 | 51856.8 | 50000 | 51856.8 | 51856.8 | 0 | 51856.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 47956.9 | 47956.9 | 104241.8 | 0 | PROCESSED | 57613.5483217593 | 57009 | 56643.7003587963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081525 | We propose observations of the outskirts of Abell 133, a relaxed galaxy cluster that is the target of a Chandra X-ray Visionary Project. These modest Suzaku observations will leverage the 2.4 Msec of Chandra time spent deeply imaging the region beyond r_500 to search for ICM clumping. Such clumping has been invoked to explain the flat entropy profiles and excess inferred gas fraction beyond r_500 in several clusters observed recently with Suzaku. The proposed Suzaku observations combined with the unprecedented Chandra depth will create a fiducial dataset to compare to the existing Suzaku cluster outskirts data, and they will definitely determine whether the excess inferred gas fractions seen with Suzaku arise from gas clumping. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MILLER | ERIC | NULL | NULL | USA | 8 | AO8 | A DEFINITIVE STUDY OF GALAXY CLUSTER OUTSKIRTS WITH SUZAKU AND CHANDRA | XIS | Y |
| A133_FIELD_4 | 16.0019 | -22.0663 | 153.04375578 | -84.18809016 | 231.9997 | 56632.6176967593 | 56633.8716666667 | 808084010 | 52528.2 | 50000 | 52528.2 | 52528.2 | 0 | 52528.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 49912 | 49912 | 108328.1 | 0 | PROCESSED | 57613.5467013889 | 57061 | 56695.6415046296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081525 | We propose observations of the outskirts of Abell 133, a relaxed galaxy cluster that is the target of a Chandra X-ray Visionary Project. These modest Suzaku observations will leverage the 2.4 Msec of Chandra time spent deeply imaging the region beyond r_500 to search for ICM clumping. Such clumping has been invoked to explain the flat entropy profiles and excess inferred gas fraction beyond r_500 in several clusters observed recently with Suzaku. The proposed Suzaku observations combined with the unprecedented Chandra depth will create a fiducial dataset to compare to the existing Suzaku cluster outskirts data, and they will definitely determine whether the excess inferred gas fractions seen with Suzaku arise from gas clumping. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MILLER | ERIC | NULL | NULL | USA | 8 | AO8 | A DEFINITIVE STUDY OF GALAXY CLUSTER OUTSKIRTS WITH SUZAKU AND CHANDRA | XIS | Y |
| A426VIR S | 48.9041 | 42.4908 | 149.35896709 | -12.86322568 | 271.5007 | 56708.3862962963 | 56709.0453009259 | 808085010 | 26260 | 25000 | 26284 | 26276 | 0 | 26260 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21026.7 | 21026.7 | 56933.9 | 1 | PROCESSED | 57613.8719560185 | 57086 | 56720.6405902778 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081526 | Our analysis of Suzaku Key Project data of the Perseus Cluster of galaxies has uncovered a significant drop in temperature, density and derived thermodynamic properties of the intra-cluster medium in the NW direction at the cluster's virial radius, suggesting the presence of a strong shock. In order to firmly confirm and further explore this feature we propose to expand upon the observation of this region. Confirmation of a shock at the virial radius will provide the first ever direct observation of the formation of a galaxy cluster and virialization of the in-falling hot gas. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | URBAN | ONDREJ | NULL | NULL | USA | 8 | AO8 | SHOCK FRONT AT THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| A426VIR E | 49.1256 | 42.621 | 149.42807458 | -12.66566367 | 271.4976 | 56709.0457986111 | 56709.5683101852 | 808086010 | 25370.3 | 25000 | 25382.3 | 25370.3 | 0 | 25370.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 24322 | 24322 | 45140 | 1 | PROCESSED | 57613.8778935185 | 57141 | 56764.7643171296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081526 | Our analysis of Suzaku Key Project data of the Perseus Cluster of galaxies has uncovered a significant drop in temperature, density and derived thermodynamic properties of the intra-cluster medium in the NW direction at the cluster's virial radius, suggesting the presence of a strong shock. In order to firmly confirm and further explore this feature we propose to expand upon the observation of this region. Confirmation of a shock at the virial radius will provide the first ever direct observation of the formation of a galaxy cluster and virialization of the in-falling hot gas. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | URBAN | ONDREJ | NULL | NULL | USA | 8 | AO8 | SHOCK FRONT AT THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| A426VIR N | 48.9538 | 42.7811 | 149.23070312 | -12.5987294 | 270.5957 | 56710.5023726852 | 56711.155775463 | 808087010 | 23377.6 | 25000 | 23385.6 | 23385.6 | 0 | 23377.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 20561.2 | 20561.2 | 56441.9 | 0 | PROCESSED | 57613.8896296296 | 57089 | 56723.6141898148 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081526 | Our analysis of Suzaku Key Project data of the Perseus Cluster of galaxies has uncovered a significant drop in temperature, density and derived thermodynamic properties of the intra-cluster medium in the NW direction at the cluster's virial radius, suggesting the presence of a strong shock. In order to firmly confirm and further explore this feature we propose to expand upon the observation of this region. Confirmation of a shock at the virial radius will provide the first ever direct observation of the formation of a galaxy cluster and virialization of the in-falling hot gas. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | URBAN | ONDREJ | NULL | NULL | USA | 8 | AO8 | SHOCK FRONT AT THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| A426VIR W | 48.7321 | 42.6495 | 149.16205221 | -12.79713949 | 270.0001 | 56711.1564351852 | 56711.6279976852 | 808088010 | 24742.8 | 25000 | 24758.7 | 24742.8 | 0 | 24766.7 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 22016.8 | 22016.8 | 40735.9 | 0 | PROCESSED | 57613.8909259259 | 57141 | 56764.7613657407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081526 | Our analysis of Suzaku Key Project data of the Perseus Cluster of galaxies has uncovered a significant drop in temperature, density and derived thermodynamic properties of the intra-cluster medium in the NW direction at the cluster's virial radius, suggesting the presence of a strong shock. In order to firmly confirm and further explore this feature we propose to expand upon the observation of this region. Confirmation of a shock at the virial radius will provide the first ever direct observation of the formation of a galaxy cluster and virialization of the in-falling hot gas. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | URBAN | ONDREJ | NULL | NULL | USA | 8 | AO8 | SHOCK FRONT AT THE VIRIAL RADIUS OF THE X-RAY BRIGHTEST GALAXY CLUSTER | XIS | Y |
| ABELL 1689 (OFFSET) | 198.1816 | -1.2688 | 314.01012466 | 61.14421574 | 293.5484 | 56470.3775578704 | 56473.3751273148 | 808089010 | 105751.8 | 396000 | 105759.8 | 105751.8 | 0 | 105751.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 95047.7 | 95047.7 | 258955.6 | 4 | PROCESSED | 57611.7314930556 | 56383 | 56523.7467708333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081528 | Recent Suzaku results suggest that the surface brightness in galaxy cluster outskirts is higher than the predictions by self-similar models, indicating that the gas may be clumpy or may not be in collisional equilibrium near and beyond the virial radius. If this is the case, gas emission near cosmological accretion shocks should readily be detected. We propose to search for emission near the accretion shock radius where it is the only region unexplored in galaxy cluster studies in X-ray. These data can place important constraints on accretion models and large-scale structure formation theory. Physical properties at the true virial radius (R100) will also be measured to the highest precision to date. A very deep exposure and the low Suzaku background allow this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | WONG | KA-WAH | NULL | NULL | USA | 8 | AO8 | SEARCH FOR ACCRETION SHOCK IN A MASSIVE GALAXY CLUSTER | XIS | Y |
| ABELL 1689 (OFFSET) | 198.1818 | -1.2687 | 314.01056832 | 61.14428006 | 293.5484 | 56473.3751388889 | 56475.3022916667 | 808089020 | 67800.3 | 396000 | 67808.3 | 67800.3 | 0 | 67808.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 60964.9 | 60964.9 | 166469.8 | 5 | PROCESSED | 57611.6944907407 | 56383 | 56491.6594675926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081528 | Recent Suzaku results suggest that the surface brightness in galaxy cluster outskirts is higher than the predictions by self-similar models, indicating that the gas may be clumpy or may not be in collisional equilibrium near and beyond the virial radius. If this is the case, gas emission near cosmological accretion shocks should readily be detected. We propose to search for emission near the accretion shock radius where it is the only region unexplored in galaxy cluster studies in X-ray. These data can place important constraints on accretion models and large-scale structure formation theory. Physical properties at the true virial radius (R100) will also be measured to the highest precision to date. A very deep exposure and the low Suzaku background allow this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | WONG | KA-WAH | NULL | NULL | USA | 8 | AO8 | SEARCH FOR ACCRETION SHOCK IN A MASSIVE GALAXY CLUSTER | XIS | Y |
| ABELL 1689 (OFFSET) | 198.1886 | -1.1923 | 314.05162405 | 61.21838483 | 111.865 | 56657.0769444444 | 56660.6460069445 | 808089030 | 53227.2 | 130000 | 53227.2 | 53227.2 | 0 | 53227.2 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 3327.9 | 0 | PROCESSED | 57613.7319791667 | 56383 | 56713.6636342593 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081528 | Recent Suzaku results suggest that the surface brightness in galaxy cluster outskirts is higher than the predictions by self-similar models, indicating that the gas may be clumpy or may not be in collisional equilibrium near and beyond the virial radius. If this is the case, gas emission near cosmological accretion shocks should readily be detected. We propose to search for emission near the accretion shock radius where it is the only region unexplored in galaxy cluster studies in X-ray. These data can place important constraints on accretion models and large-scale structure formation theory. Physical properties at the true virial radius (R100) will also be measured to the highest precision to date. A very deep exposure and the low Suzaku background allow this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | WONG | KA-WAH | NULL | NULL | USA | 8 | AO8 | SEARCH FOR ACCRETION SHOCK IN A MASSIVE GALAXY CLUSTER | XIS | Y |
| ABELL 1689 (OFFSET) | 198.1809 | -1.2604 | 314.01167358 | 61.15261163 | 111.9001 | 56670.9898148148 | 56672.9376388889 | 808089040 | 37466.7 | 90000 | 37466.7 | 37466.7 | 0 | 37466.7 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57613.7681134259 | 56383 | 56687.7783564815 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081528 | Recent Suzaku results suggest that the surface brightness in galaxy cluster outskirts is higher than the predictions by self-similar models, indicating that the gas may be clumpy or may not be in collisional equilibrium near and beyond the virial radius. If this is the case, gas emission near cosmological accretion shocks should readily be detected. We propose to search for emission near the accretion shock radius where it is the only region unexplored in galaxy cluster studies in X-ray. These data can place important constraints on accretion models and large-scale structure formation theory. Physical properties at the true virial radius (R100) will also be measured to the highest precision to date. A very deep exposure and the low Suzaku background allow this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | WONG | KA-WAH | NULL | NULL | USA | 8 | AO8 | SEARCH FOR ACCRETION SHOCK IN A MASSIVE GALAXY CLUSTER | XIS | Y |
| COMA W SHOCK1 | 194.1832 | 28.2738 | 77.58391557 | 88.36116739 | 275.406 | 56475.3084143518 | 56475.66125 | 808090010 | 16692 | 15000 | 16692 | 16716 | 0 | 16700 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 13638 | 13638 | 30475.9 | 1 | PROCESSED | 57611.6582407407 | 56897 | 56524.6518518518 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081529 | Our analysis of Suzaku data of the Coma Cluster revealed an intriguing correlation between the outer edge of its radio halo and the thermodynamic properties of the gas. This correlation seems to be the most pronounced in the western direction where the temperature drops from about 10keV in the annulus spanning 35'-41' to only 1.7keV in the annulus spanning 50'-60'. The Planck Collaboration found a marked local steepening of the radial gradient of the SZ signal at this location and interpret this feature as a shock with a Mach number of about 2. Unfortunately, we currently lack X-ray coverage towards the W in this critical range of 41'-50'. We therefore propose two additional pointings with a total exposure time of 30ks, that will allow us to resolve the temperature gradient in this region. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | SIMIONESCU | AURORA | NULL | NULL | USA | 8 | AO8 | THE MISSING PUZZLE PIECE IN THE COMA SHOCK FRONT | XIS | Y |
| COMA W SHOCK2 | 194.0639 | 28.3374 | 81.80911298 | 88.38803012 | 275.4001 | 56475.6616782407 | 56476.1674884259 | 808091010 | 15693.4 | 15000 | 15709.4 | 15693.4 | 0 | 15709.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16625.4 | 16625.4 | 43694 | 0 | PROCESSED | 57611.6755902778 | 56858 | 56492.6168865741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081529 | Our analysis of Suzaku data of the Coma Cluster revealed an intriguing correlation between the outer edge of its radio halo and the thermodynamic properties of the gas. This correlation seems to be the most pronounced in the western direction where the temperature drops from about 10keV in the annulus spanning 35'-41' to only 1.7keV in the annulus spanning 50'-60'. The Planck Collaboration found a marked local steepening of the radial gradient of the SZ signal at this location and interpret this feature as a shock with a Mach number of about 2. Unfortunately, we currently lack X-ray coverage towards the W in this critical range of 41'-50'. We therefore propose two additional pointings with a total exposure time of 30ks, that will allow us to resolve the temperature gradient in this region. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | SIMIONESCU | AURORA | NULL | NULL | USA | 8 | AO8 | THE MISSING PUZZLE PIECE IN THE COMA SHOCK FRONT | XIS | Y |
| CIZASOUTHPE | 340.7756 | 52.9173 | 104.17197619 | -5.21572392 | 71.9989 | 56461.8747800926 | 56464.2467361111 | 808092010 | 92959.5 | 99000 | 92967.5 | 92967.5 | 0 | 92959.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 96312.5 | 96312.5 | 204921.6 | 2 | PROCESSED | 57611.5762268518 | 56848 | 56481.818287037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081530 | The Sausage Cluster is a violent merging galaxy cluster that offers unique opportunities to study the physics of particle acceleration and shocks in the ICM. We propose Suzaku observations of the southern part of the Sausage Cluster to (i) measure the Mach number of a merger related shock and (ii) determine the temperature distribution in the entire cluster outskirts. These observations will provide the first complete view of a system of merger-induced radio shocks and therefore play a crucial role in (1) understanding the impacts of such shocks on the evolution of galaxy clusters, (2) determining the physics of particle acceleration at low Mach number shocks, and (3) providing vital input for modeling the merger event in detail. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | VAN WEEREN | REINOUT | NULL | NULL | USA | 8 | AO8 | SHOCK AND AWE: PARTICLE ACCELERATION IN THE SAUSAGE CLUSTER | XIS | Y |
| CIZASOUTHPW | 340.5329 | 52.9469 | 104.05697228 | -5.12002469 | 72.9252 | 56464.2477662037 | 56466.5627777778 | 808093010 | 98420.7 | 99000 | 98428.7 | 98420.7 | 0 | 98428.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 99100.6 | 99100.6 | 200005.6 | 0 | PROCESSED | 57611.6015277778 | 56848 | 56481.8295486111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081530 | The Sausage Cluster is a violent merging galaxy cluster that offers unique opportunities to study the physics of particle acceleration and shocks in the ICM. We propose Suzaku observations of the southern part of the Sausage Cluster to (i) measure the Mach number of a merger related shock and (ii) determine the temperature distribution in the entire cluster outskirts. These observations will provide the first complete view of a system of merger-induced radio shocks and therefore play a crucial role in (1) understanding the impacts of such shocks on the evolution of galaxy clusters, (2) determining the physics of particle acceleration at low Mach number shocks, and (3) providing vital input for modeling the merger event in detail. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | VAN WEEREN | REINOUT | NULL | NULL | USA | 8 | AO8 | SHOCK AND AWE: PARTICLE ACCELERATION IN THE SAUSAGE CLUSTER | XIS | Y |
| ABELL 3571 | 206.8624 | -32.8524 | 316.31343933 | 28.55973438 | 103.8412 | 56666.0275 | 56666.7772453704 | 808094010 | 38279 | 60000 | 38279 | 38279 | 0 | 38279 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39004.7 | 39004.7 | 64776 | 0 | PROCESSED | 57613.7763425926 | 57096 | 56730.4916435185 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 081531 | Abell 3571 is one of the brightest cluster in the X-ray sky and one of the main clusters in the Shapley supercluster. We have recently found evidence that it may be passing through a violent (~2000 km/s) merger in the line of sight (los). If corroborated it would be the closest template for the systems of this kind allowing us to study and characterize los mergers. We request a short observation of 60 ksec to corroborate the velocity gradients found with Chandra for this cluster, using the improved spectral resolution and gain stability of Suzaku s XISs. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | DUPKE | RENATO | NULL | NULL | USA | 8 | AO8 | ABELL 3571. THE CLOSEST LINE OF SIGHT MERGER? | XIS | Y |
| PLCK G214.6-37.0 | 137.1752 | 14.6923 | 214.5759479 | 36.9399481 | 287 | 56413.2455439815 | 56416.322349537 | 808101010 | 119263.7 | 120000 | 119263.7 | 119263.7 | 0 | 119263.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 106312.7 | 106312.7 | 265803.9 | 5 | PROCESSED | 57611.2793981482 | 56795 | 56429.7933217593 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 082007 | We propose a detailed investigation of the nature of PLCK G214.6-37.0, discovered in the Planck survey. We aim at constraining the presence and properties of filamentary structures connecting and surrounding the clusters. We will unveil the overall dynamics of this complex structure and establish its detailed pressure distribution that can be used for a better estimation of YX to be compared with YSZ. Thus, we will perform a direct search for structures in between identified supercluster components from a careful comparison with the Planck results. Furthermore, the distribution of the PLCK G214.6-37.0 components suggest that it is evolving accreting sub-clusters along the filaments. That makes this supercluster one of the to search for the WHIM. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | LOVISARI | LORENZO | NULL | NULL | EUR | 8 | AO8 | TRACKING DOWN THE PLANCK SUPERCLUSTER PLCK G214.6-37.0 | XIS | Y |
| A2877-NORTH | 17.5135 | -45.1865 | 292.51418745 | -71.56330592 | 266.5006 | 56649.9225810185 | 56651.7884027778 | 808102010 | 72629 | 70000 | 72637 | 72629 | 0 | 72645 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 69264.1 | 69264.1 | 161185.7 | 0 | PROCESSED | 57613.7012615741 | 57033 | 56665.7969097222 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 082014 | We propose to observe the galaxy group A2877 for a combine observation time of 150 ks, with two different pointings. The aim of the project is to obtain temperature and surface brightness profiles out to large radii to constrain entropies. We aim to see if the entropy profile flattens at large radii, which could indicate gas clumping and/or other processes. This would possibly be the first unrelaxed galaxy group whose entropy profile would have been studied in the outskirts. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | VIJAYSARATHY | BHARADWAJ | NULL | NULL | EUR | 8 | AO8 | INVESTIGATING THE OUTSKIRTS OF THE UNRELAXED GALAXY GROUP A2877 | XIS | Y |
| A2877-SOUTH | 17.378 | -46.6527 | 293.76700694 | -70.15260223 | 237.9995 | 56647.8346643518 | 56649.916875 | 808103010 | 83517.2 | 80000 | 83517.2 | 83525.2 | 0 | 83533.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 81299.3 | 81299.3 | 179897.9 | 4 | PROCESSED | 57613.6802199074 | 57033 | 56665.8173263889 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 082014 | We propose to observe the galaxy group A2877 for a combine observation time of 150 ks, with two different pointings. The aim of the project is to obtain temperature and surface brightness profiles out to large radii to constrain entropies. We aim to see if the entropy profile flattens at large radii, which could indicate gas clumping and/or other processes. This would possibly be the first unrelaxed galaxy group whose entropy profile would have been studied in the outskirts. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | VIJAYSARATHY | BHARADWAJ | NULL | NULL | EUR | 8 | AO8 | INVESTIGATING THE OUTSKIRTS OF THE UNRELAXED GALAXY GROUP A2877 | XIS | Y |
| A3528-S OFFSET 1 | 193.8801 | -29.4768 | 303.99602967 | 33.38651365 | 289.4829 | 56500.4359953704 | 56501.528587963 | 808104010 | 40341.1 | 50000 | 40349.1 | 40349.1 | 0 | 40341.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40862.3 | 40862.3 | 94384 | 2 | PROCESSED | 57612.0687037037 | 56955 | 56587.7834490741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 082018 | We propose to observe, for a total of 180 ks, the region between the galaxy cluster A3528 and the complex A3530-A3532, in which we expect to find the filament connecting the clusters. With the requested time we aim to detect the Warm Hot Intergalactic Medium (WHIM) by its thermal soft-Xray emission, to resolve one of the major problems of modern astrophysics - the missing baryons , which are now thought to reside in the filaments connecting clusters. In addition to a full understanding of the typical baryon fraction, the proposed observations will allow us to study the gas clumping in the cluster outskirts. Furthermore, a combined analysis of X-ray and optical data will enable us to shed light on the influence of the environments on galaxy evolution. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | LOVISARI | LORENZO | NULL | NULL | EUR | 8 | AO8 | TRACING A FILAMENT IN THE OUTSKIRTS OF THE SHAPLEY SUPERCLUSTER | XIS | Y |
| A3528-S OFFSET 2 | 193.9782 | -29.6501 | 304.09397791 | 33.21155179 | 289.0026 | 56501.5292476852 | 56502.3981481482 | 808105010 | 42300 | 40000 | 42300 | 42307.8 | 0 | 42316 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42525.8 | 42525.8 | 75065.9 | 2 | PROCESSED | 57612.0639583333 | 56955 | 56587.7982523148 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 082018 | We propose to observe, for a total of 180 ks, the region between the galaxy cluster A3528 and the complex A3530-A3532, in which we expect to find the filament connecting the clusters. With the requested time we aim to detect the Warm Hot Intergalactic Medium (WHIM) by its thermal soft-Xray emission, to resolve one of the major problems of modern astrophysics - the missing baryons , which are now thought to reside in the filaments connecting clusters. In addition to a full understanding of the typical baryon fraction, the proposed observations will allow us to study the gas clumping in the cluster outskirts. Furthermore, a combined analysis of X-ray and optical data will enable us to shed light on the influence of the environments on galaxy evolution. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | LOVISARI | LORENZO | NULL | NULL | EUR | 8 | AO8 | TRACING A FILAMENT IN THE OUTSKIRTS OF THE SHAPLEY SUPERCLUSTER | XIS | Y |
| A3528-S OFFSET 3 | 194.0873 | -29.8404 | 304.20210274 | 33.01923597 | 288.9994 | 56502.3985300926 | 56503.6522453704 | 808106010 | 61233.9 | 60000 | 61257.9 | 61249.9 | 0 | 61233.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 61647.4 | 61647.4 | 108309.7 | 2 | PROCESSED | 57612.1235763889 | 56955 | 56587.4691782407 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 082018 | We propose to observe, for a total of 180 ks, the region between the galaxy cluster A3528 and the complex A3530-A3532, in which we expect to find the filament connecting the clusters. With the requested time we aim to detect the Warm Hot Intergalactic Medium (WHIM) by its thermal soft-Xray emission, to resolve one of the major problems of modern astrophysics - the missing baryons , which are now thought to reside in the filaments connecting clusters. In addition to a full understanding of the typical baryon fraction, the proposed observations will allow us to study the gas clumping in the cluster outskirts. Furthermore, a combined analysis of X-ray and optical data will enable us to shed light on the influence of the environments on galaxy evolution. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | LOVISARI | LORENZO | NULL | NULL | EUR | 8 | AO8 | TRACING A FILAMENT IN THE OUTSKIRTS OF THE SHAPLEY SUPERCLUSTER | XIS | Y |
| A3528-S OFFSET 4 | 194.1847 | -30.0435 | 304.29690153 | 32.8141993 | 288.9992 | 56503.6527199074 | 56504.4071064815 | 808107010 | 32775.2 | 30000 | 32783.2 | 32775.2 | 0 | 32791.2 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 31258.5 | 31258.5 | 65159.9 | 0 | PROCESSED | 57612.0918634259 | 56955 | 56587.7238310185 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 082018 | We propose to observe, for a total of 180 ks, the region between the galaxy cluster A3528 and the complex A3530-A3532, in which we expect to find the filament connecting the clusters. With the requested time we aim to detect the Warm Hot Intergalactic Medium (WHIM) by its thermal soft-Xray emission, to resolve one of the major problems of modern astrophysics - the missing baryons , which are now thought to reside in the filaments connecting clusters. In addition to a full understanding of the typical baryon fraction, the proposed observations will allow us to study the gas clumping in the cluster outskirts. Furthermore, a combined analysis of X-ray and optical data will enable us to shed light on the influence of the environments on galaxy evolution. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | LOVISARI | LORENZO | NULL | NULL | EUR | 8 | AO8 | TRACING A FILAMENT IN THE OUTSKIRTS OF THE SHAPLEY SUPERCLUSTER | XIS | Y |
| A262 NE1 | 28.4051 | 36.5019 | 136.64990456 | -24.70790073 | 250 | 56702.5986342593 | 56703.187662037 | 808108010 | 25610.2 | 24000 | 25610.2 | 25610.2 | 0 | 25610.2 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57613.8178472222 | 57080 | 56714.742037037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 083002 | We propose to observe a poor cluster, Abell 262 (kT=2.2 keV, z=0.017), out to 0.9 r180 toward directions of a filament and void. The objectives are to derive gas-mass and fe-mass-to-light ratios and entropy profiles out the virial radius and study their dependence of the system mass, and to study azimuthal dependence of the temperature, density and entropy. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MATSUSHITA | KYOKO | WERNER | NORBERT | JUS | 8 | AO8 | OBSERVATIONS OF AN POOR CLUSTER OUT TO THE VIRIAL RADIUS | XIS | Y |
| A262 NE2 | 28.537 | 36.7219 | 136.69850182 | -24.46778258 | 249.9995 | 56703.1881712963 | 56703.8821643518 | 808109010 | 32944.7 | 32000 | 32952.7 | 32960.7 | 0 | 32944.7 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57613.8208564815 | 57080 | 56714.743275463 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 083002 | We propose to observe a poor cluster, Abell 262 (kT=2.2 keV, z=0.017), out to 0.9 r180 toward directions of a filament and void. The objectives are to derive gas-mass and fe-mass-to-light ratios and entropy profiles out the virial radius and study their dependence of the system mass, and to study azimuthal dependence of the temperature, density and entropy. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MATSUSHITA | KYOKO | WERNER | NORBERT | JUS | 8 | AO8 | OBSERVATIONS OF AN POOR CLUSTER OUT TO THE VIRIAL RADIUS | XIS | Y |
| A262 NE3 | 28.6712 | 36.9514 | 136.74540455 | -24.21802206 | 250.0003 | 56703.8826388889 | 56704.7987731482 | 808110010 | 40490.3 | 40000 | 40513.4 | 40490.3 | 0 | 40496.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34262.4 | 34262.4 | 69899 | 1 | PROCESSED | 57613.8476041667 | 57081 | 56715.76 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 083002 | We propose to observe a poor cluster, Abell 262 (kT=2.2 keV, z=0.017), out to 0.9 r180 toward directions of a filament and void. The objectives are to derive gas-mass and fe-mass-to-light ratios and entropy profiles out the virial radius and study their dependence of the system mass, and to study azimuthal dependence of the temperature, density and entropy. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MATSUSHITA | KYOKO | WERNER | NORBERT | JUS | 8 | AO8 | OBSERVATIONS OF AN POOR CLUSTER OUT TO THE VIRIAL RADIUS | XIS | Y |
| A262 NE4 | 28.8115 | 37.1901 | 136.79382783 | -23.95810874 | 249.9999 | 56704.7992476852 | 56705.5321064815 | 808111010 | 30930.5 | 30000 | 30962.5 | 30930.5 | 0 | 30962.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 27802.7 | 27802.7 | 63311.9 | 2 | PROCESSED | 57613.8474652778 | 57085 | 56719.7343981482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 083002 | We propose to observe a poor cluster, Abell 262 (kT=2.2 keV, z=0.017), out to 0.9 r180 toward directions of a filament and void. The objectives are to derive gas-mass and fe-mass-to-light ratios and entropy profiles out the virial radius and study their dependence of the system mass, and to study azimuthal dependence of the temperature, density and entropy. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MATSUSHITA | KYOKO | WERNER | NORBERT | JUS | 8 | AO8 | OBSERVATIONS OF AN POOR CLUSTER OUT TO THE VIRIAL RADIUS | XIS | Y |
| A262 E1 | 28.6322 | 35.9862 | 136.99532529 | -25.15665513 | 249.9998 | 56694.7928935185 | 56695.3750694444 | 808112010 | 25946.6 | 24000 | 25954.6 | 25946.6 | 0 | 25962.6 | 3 | 3 | 0 | 3 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57613.7986226852 | 57074 | 56709.7127893518 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 083002 | We propose to observe a poor cluster, Abell 262 (kT=2.2 keV, z=0.017), out to 0.9 r180 toward directions of a filament and void. The objectives are to derive gas-mass and fe-mass-to-light ratios and entropy profiles out the virial radius and study their dependence of the system mass, and to study azimuthal dependence of the temperature, density and entropy. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MATSUSHITA | KYOKO | WERNER | NORBERT | JUS | 8 | AO8 | OBSERVATIONS OF AN POOR CLUSTER OUT TO THE VIRIAL RADIUS | XIS | Y |
| A262 E2 | 28.9415 | 35.8688 | 137.29682221 | -25.20210685 | 249.9999 | 56695.375625 | 56696.1043518518 | 808113010 | 33056.9 | 32000 | 33060.9 | 33056.9 | 0 | 33064.9 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57613.8024884259 | 57074 | 56709.7139814815 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 083002 | We propose to observe a poor cluster, Abell 262 (kT=2.2 keV, z=0.017), out to 0.9 r180 toward directions of a filament and void. The objectives are to derive gas-mass and fe-mass-to-light ratios and entropy profiles out the virial radius and study their dependence of the system mass, and to study azimuthal dependence of the temperature, density and entropy. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MATSUSHITA | KYOKO | WERNER | NORBERT | JUS | 8 | AO8 | OBSERVATIONS OF AN POOR CLUSTER OUT TO THE VIRIAL RADIUS | XIS | Y |
| A262 E3 | 29.2513 | 35.7586 | 137.59731231 | -25.23895106 | 250.0003 | 56701.0116319444 | 56701.8717939815 | 808114010 | 38568.1 | 40000 | 38576.1 | 38568.1 | 0 | 38576.1 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57613.8129861111 | 57080 | 56714.7407986111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 083002 | We propose to observe a poor cluster, Abell 262 (kT=2.2 keV, z=0.017), out to 0.9 r180 toward directions of a filament and void. The objectives are to derive gas-mass and fe-mass-to-light ratios and entropy profiles out the virial radius and study their dependence of the system mass, and to study azimuthal dependence of the temperature, density and entropy. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MATSUSHITA | KYOKO | WERNER | NORBERT | JUS | 8 | AO8 | OBSERVATIONS OF AN POOR CLUSTER OUT TO THE VIRIAL RADIUS | XIS | Y |
| A262 E4 | 29.5568 | 35.6351 | 137.89892988 | -25.28797491 | 250 | 56701.8723148148 | 56702.5974652778 | 808115010 | 31938.9 | 30000 | 31946.9 | 31938.9 | 0 | 31954.9 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57613.8117361111 | 57080 | 56714.739525463 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 083002 | We propose to observe a poor cluster, Abell 262 (kT=2.2 keV, z=0.017), out to 0.9 r180 toward directions of a filament and void. The objectives are to derive gas-mass and fe-mass-to-light ratios and entropy profiles out the virial radius and study their dependence of the system mass, and to study azimuthal dependence of the temperature, density and entropy. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MATSUSHITA | KYOKO | WERNER | NORBERT | JUS | 8 | AO8 | OBSERVATIONS OF AN POOR CLUSTER OUT TO THE VIRIAL RADIUS | XIS | Y |
| VIRGO E1 | 188.0634 | 12.5322 | 284.88156742 | 74.72763223 | 285 | 56481.2981828704 | 56481.5626736111 | 808116010 | 10335.3 | 10000 | 10335.3 | 10335.3 | 0 | 10335.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 8832.3 | 8832.3 | 22845.9 | 0 | PROCESSED | 57611.7060416667 | 56383 | 56524.6432407407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 086003 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 8 | AO8 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO E2 | 188.3405 | 12.688 | 285.71074231 | 74.9520878 | 284.9998 | 56481.5631944444 | 56481.9592824074 | 808117010 | 10659.8 | 10000 | 10659.8 | 10659.8 | 0 | 10659.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10698.2 | 10698.2 | 34220 | 0 | PROCESSED | 57611.7227199074 | 56383 | 56524.654212963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 086003 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 8 | AO8 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO E3 | 188.6166 | 12.8387 | 286.56417369 | 75.16845975 | 284.999 | 56481.9598032407 | 56482.2154861111 | 808118010 | 12327.5 | 10000 | 12335.5 | 12335.5 | 0 | 12327.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10334 | 10334 | 22087.9 | 0 | PROCESSED | 57611.7501851852 | 56383 | 56495.6160185185 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 086003 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 8 | AO8 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO E4 | 188.894 | 12.9933 | 287.44169131 | 75.38588793 | 285.0007 | 56482.2160069445 | 56482.4926157407 | 808119010 | 12968.7 | 11000 | 12992.7 | 12984.7 | 0 | 12968.7 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 9283 | 9283 | 23895.9 | 0 | PROCESSED | 57611.7741319444 | 56383 | 56496.5935185185 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 086003 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 8 | AO8 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO E5 | 189.1714 | 13.1819 | 288.31179147 | 75.63323247 | 284.9999 | 56482.4931365741 | 56482.9348726852 | 808120010 | 12298.6 | 12000 | 12298.6 | 12298.6 | 0 | 12298.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 12267.1 | 12267.1 | 38161.9 | 0 | PROCESSED | 57611.7660300926 | 56383 | 56496.6035416667 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 086003 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 8 | AO8 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO E6 | 189.4489 | 13.3515 | 289.22685608 | 75.85896695 | 284.9998 | 56482.9353935185 | 56483.2543171296 | 808121010 | 14633 | 14000 | 14641 | 14641 | 0 | 14633 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 11044.1 | 11044.1 | 27551.9 | 0 | PROCESSED | 57611.7799421296 | 56383 | 56496.5976157407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 086003 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 8 | AO8 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO E7 | 189.7478 | 13.5221 | 290.25286309 | 76.08652265 | 285.0003 | 56483.2548842593 | 56483.6994560185 | 808122010 | 18166.5 | 17000 | 18166.5 | 18190.5 | 0 | 18174.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15691.7 | 15691.7 | 38403.9 | 2 | PROCESSED | 57611.7926273148 | 56383 | 56496.6013657407 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 086003 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 8 | AO8 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO E8 | 190.0457 | 13.6937 | 291.30515449 | 76.31072684 | 284.9998 | 56483.6999768518 | 56484.1918634259 | 808123010 | 18448.2 | 18000 | 18448.2 | 18448.2 | 0 | 18448.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 16212.2 | 16212.2 | 42492 | 0 | PROCESSED | 57611.7962268518 | 56383 | 56498.6264351852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 086003 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 8 | AO8 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO E9 | 190.3236 | 13.8446 | 292.32223865 | 76.50695206 | 284.9995 | 56484.1924305556 | 56484.6162268518 | 808124010 | 18871.9 | 18000 | 18895.1 | 18887.9 | 0 | 18871.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15367.4 | 15367.4 | 36611.9 | 0 | PROCESSED | 57611.8197106482 | 56383 | 56498.6214930556 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 086003 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 8 | AO8 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO E10 | 190.6018 | 13.9952 | 293.36819262 | 76.69896749 | 284.9995 | 56484.6167476852 | 56485.1960416667 | 808125010 | 21443.5 | 20000 | 21443.5 | 21443.5 | 0 | 21443.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19152 | 19152 | 50044 | 1 | PROCESSED | 57611.8325115741 | 56383 | 56498.6333796296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 086003 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 8 | AO8 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO E11 | 190.8574 | 14.15 | 294.34392528 | 76.88802661 | 285 | 56485.1965162037 | 56485.8154513889 | 808126010 | 23359.1 | 21000 | 23367.1 | 23359.1 | 0 | 23373.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19993.7 | 19993.7 | 53469.9 | 1 | PROCESSED | 57611.8143171296 | 56383 | 56498.6447106482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 086003 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 8 | AO8 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO E12 | 191.1366 | 14.3009 | 295.44935056 | 77.07241976 | 285.0012 | 56485.8160185185 | 56486.2634143518 | 808127010 | 20597.9 | 20000 | 20613.9 | 20597.9 | 0 | 20613.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17420 | 17420 | 38647.9 | 0 | PROCESSED | 57611.9024768518 | 56383 | 56498.6479976852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 086003 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 8 | AO8 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| VIRGO E13 | 191.4157 | 14.448 | 296.58532586 | 77.24852866 | 284.9997 | 56486.2639351852 | 56486.8515856482 | 808128010 | 20481.7 | 20000 | 20489.7 | 20481.7 | 0 | 20489.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18787 | 18787 | 50759.9 | 0 | PROCESSED | 57611.9056134259 | 56383 | 56503.6194444444 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 086003 | We propose a legacy-class study of the outskirts of the Virgo Cluster, the nearest, second brightest galaxy cluster in the X-ray sky. This will provide the first detailed study of the outer parts of a low-mass system, with unparalleled signal-to-noise and spatial resolution. We will observe along four distinct directions which will provide unique insight into the ongoing virialization and equilibration processes that occur during large-scale structure formation. The Virgo Cluster is dynamically complex, with clear differences in its X-ray and optical properties along the chosen axes. This, its proximity and brightness, and the unrivaled multi-wavelength follow-up data make it the ideal system for studying the effects that different accretion rates have in shaping the ICM at large radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SIMIONESCU | AURORA | NULL | NULL | USA | 8 | AO8 | WITNESSING THE GROWTH OF THE NEAREST GALAXY CLUSTER | XIS | Y |
| THE MOON | 131.4647 | 12.9515 | 213.82172975 | 31.16197152 | 285.4003 | 56783.5475578704 | 56783.6842361111 | 809001010 | 4642.4 | 45000 | 4646.4 | 4642.4 | 0 | 4650.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 4564.7 | 4564.7 | 11806 | 0 | PROCESSED | 57615.0366898148 | 57162 | 56793.5228125 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y |
| THE MOON | 132.8593 | 12.3218 | 215.15290673 | 32.14399459 | 282.2504 | 56783.6861921296 | 56783.8127083333 | 809001020 | 4644.5 | 45000 | 4644.5 | 4644.5 | 0 | 4660.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 4929.9 | 4929.9 | 10919.9 | 0 | PROCESSED | 57615.0434143518 | 57162 | 56793.5180324074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y |
| THE MOON | 134.2483 | 11.6812 | 216.51758385 | 33.11115118 | 281.9606 | 56783.8139699074 | 56783.948125 | 809001030 | 6489.9 | 45000 | 6497.9 | 6489.9 | 0 | 6497.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 7020 | 7020 | 11583.9 | 0 | PROCESSED | 57615.0497222222 | 57162 | 56793.5289930556 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y |
| THE MOON | 135.7323 | 11.3866 | 217.57839096 | 34.30376044 | 284.6998 | 56783.949849537 | 56784.073125 | 809001040 | 5555.6 | 45000 | 5555.6 | 5571.4 | 0 | 5563.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 4574 | 4574 | 10647.9 | 0 | PROCESSED | 57615.0559606482 | 57162 | 56796.5928240741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y |
| THE MOON | 137.2637 | 11.2624 | 218.49853071 | 35.60818154 | 285.3989 | 56784.0743402778 | 56784.198125 | 809001050 | 5762.5 | 45000 | 5770.5 | 5762.5 | 0 | 5778.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 4371 | 4371 | 10687.9 | 1 | PROCESSED | 57615.062337963 | 57218 | 56852.5744328704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y |
| THE MOON | 138.793 | 11.1278 | 219.45159127 | 36.90361182 | 285.3988 | 56784.1992939815 | 56784.3233101852 | 809001060 | 6400 | 45000 | 6400 | 6400 | 0 | 6400 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 6276.2 | 6276.2 | 10711.9 | 0 | PROCESSED | 57615.0611805556 | 57218 | 56852.5717708333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y |
| THE MOON | 140.1926 | 10.5514 | 220.86178985 | 37.88683751 | 291.2213 | 56784.325775463 | 56784.4480555556 | 809001070 | 6405 | 45000 | 6405 | 6405 | 0 | 6405 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 6677 | 6677 | 10553.9 | 0 | PROCESSED | 57615.0674074074 | 57218 | 56852.581875 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y |
| THE MOON | 141.5744 | 9.879 | 222.40545014 | 38.80103529 | 285.4041 | 56784.4506712963 | 56784.5827662037 | 809001080 | 5610.7 | 45000 | 5610.7 | 5610.7 | 0 | 5610.7 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 5507 | 5507 | 11391.9 | 0 | PROCESSED | 57615.0708217593 | 57220 | 56854.5770717593 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y |
| THE MOON | 142.9426 | 9.1926 | 223.99367078 | 39.68355518 | 285.4008 | 56784.5840162037 | 56784.7155555556 | 809001090 | 4755.8 | 45000 | 4755.8 | 4755.8 | 0 | 4755.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 4667.4 | 4667.4 | 11358 | 0 | PROCESSED | 57615.0740277778 | 57162 | 56796.5977546296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y |
| THE MOON | 17.8678 | 7.6685 | 131.57870726 | -54.86656285 | 73.8004 | 56856.4839814815 | 56856.6565162037 | 809001100 | 8248.2 | 45000 | 8264.2 | 8248.2 | 0 | 8264.2 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.3962962963 | 57233 | 56867.7358912037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y |
| THE MOON | 19.4299 | 8.4288 | 134.00151394 | -53.87712274 | 73.8016 | 56856.6577777778 | 56856.7905439815 | 809001110 | 6369.6 | 45000 | 6385.6 | 6369.6 | 0 | 6393.6 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.3999305556 | 57233 | 56867.740474537 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y |
| THE MOON | 20.9888 | 9.1871 | 136.29340358 | -52.83899755 | 73.8 | 56856.7918055556 | 56856.8877662037 | 809001120 | 4262.3 | 45000 | 4270.3 | 4262.3 | 0 | 4278.3 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.400775463 | 57233 | 56867.7339930556 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y |
| THE MOON | 22.6503 | 9.5807 | 138.76659478 | -52.08288303 | 73.7999 | 56856.8890277778 | 56857.0196412037 | 809001130 | 5301.7 | 45000 | 5301.7 | 5301.7 | 0 | 5301.7 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.4036574074 | 57267 | 56902.5802314815 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y |
| THE MOON | 24.3624 | 9.7895 | 141.30582848 | -51.43331262 | 73.7995 | 56857.0209259259 | 56857.1515856482 | 809001140 | 4290.7 | 45000 | 4290.7 | 4290.7 | 0 | 4290.7 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.4055439815 | 57267 | 56902.7022685185 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y |
| THE MOON | 26.0744 | 9.9879 | 143.76867514 | -50.73288629 | 73.7996 | 56857.1528472222 | 56857.2765856482 | 809001150 | 3916.9 | 45000 | 3916.9 | 3916.9 | 0 | 3916.9 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.4069097222 | 57235 | 56869.6125925926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y |
| THE MOON | 27.6562 | 10.6142 | 145.72862444 | -49.61972993 | 73.8014 | 56857.2778935185 | 56857.4015856482 | 809001160 | 6333.1 | 45000 | 6341.1 | 6341.1 | 0 | 6333.1 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.4093287037 | 57267 | 56902.690775463 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y |
| THE MOON | 29.2087 | 11.3221 | 147.49986562 | -48.40533826 | 73.8007 | 56857.4028472222 | 56857.5265856482 | 809001170 | 5662.1 | 45000 | 5670.1 | 5662.1 | 0 | 5670.1 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.4102314815 | 57239 | 56869.612974537 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y |
| THE MOON | 30.7597 | 12.0224 | 149.17525918 | -47.16814979 | 73.8003 | 56857.5278009259 | 56857.5974189815 | 809001180 | 3438.6 | 45000 | 3446.6 | 3438.6 | 0 | 3454.6 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.4120601852 | 57239 | 56869.6134953704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y |
| THE MOON | 137.1548 | 11.8786 | 217.75615417 | 35.77416951 | 105.7184 | 56975.0809490741 | 56975.1987615741 | 809001190 | 6413 | 45000 | 6413 | 6413 | 0 | 6413 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.77 | 57358 | 56992.4097916667 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y |
| THE MOON | 138.5418 | 11.2369 | 219.19555273 | 36.72863641 | 105.699 | 56975.1999768518 | 56975.3237615741 | 809001200 | 3379.6 | 45000 | 3379.6 | 3379.6 | 0 | 3379.6 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7701041667 | 57358 | 56992.4114699074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y |
| THE MOON | 139.925 | 10.5889 | 220.6720528 | 37.66748388 | 105.6998 | 56975.3249305556 | 56975.4487615741 | 809001210 | 3524.6 | 45000 | 3524.6 | 3524.6 | 0 | 3524.6 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.771412037 | 57358 | 56992.4131018518 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y |
| THE MOON | 141.4013 | 10.2837 | 221.84323525 | 38.83162783 | 105.6986 | 56975.4499305556 | 56975.5834143518 | 809001220 | 4255.2 | 45000 | 4255.2 | 4263.2 | 0 | 4263.2 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7742592593 | 57358 | 56992.4140625 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y |
| THE MOON | 142.9239 | 10.1507 | 222.87402657 | 40.10832518 | 105.6986 | 56975.5846296296 | 56975.7154166667 | 809001230 | 5184.8 | 45000 | 5184.8 | 5212.8 | 0 | 5220.8 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7753009259 | 57358 | 56992.4173148148 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y |
| THE MOON | 144.4436 | 10.011 | 223.94276709 | 41.37428155 | 105.6999 | 56975.7165856482 | 56975.8473611111 | 809001240 | 6219.2 | 45000 | 6219.2 | 6227.2 | 0 | 6251.2 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7771412037 | 57358 | 56992.4178703704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y |
| THE MOON | 145.8331 | 9.4283 | 225.49397113 | 42.31232043 | 105.6985 | 56975.8485300926 | 56975.9376388889 | 809001250 | 4244 | 45000 | 4244 | 4308 | 0 | 4324 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7786574074 | 57358 | 56992.4181828704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y |
| THE MOON | 147.1957 | 8.7504 | 227.18440299 | 43.16589995 | 105.6994 | 56975.9388541667 | 56976.0626388889 | 809001260 | 6330 | 45000 | 6330 | 6442 | 0 | 6442 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7804513889 | 57359 | 56992.418587963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y |
| THE MOON | 148.554 | 8.0651 | 228.92553687 | 43.99318882 | 105.699 | 56976.0638541667 | 56976.1876388889 | 809001270 | 5953.6 | 45000 | 5953.6 | 5961.6 | 0 | 5961.6 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7826967593 | 57359 | 56992.4196527778 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y |
| THE MOON | 330.3821 | -8.1914 | 50.06648816 | -45.61675095 | 252.3 | 56989.8522685185 | 56989.9654976852 | 809001280 | 4727.2 | 45000 | 4727.2 | 4727.2 | 0 | 4727.2 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.401712963 | 57415 | 57002.4419444445 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y |
| THE MOON | 332.0733 | -7.3936 | 52.31004503 | -46.62982693 | 251.0013 | 56989.9669444444 | 56990.1008449074 | 809001290 | 4227 | 45000 | 4227 | 4250.6 | 0 | 4235 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.4062962963 | 57415 | 57002.4422453704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y |
| THE MOON | 333.6436 | -6.6185 | 54.50784287 | -47.51853169 | 249.2061 | 56990.1023958333 | 56990.2084837963 | 809001300 | 3878.8 | 45000 | 3882.8 | 3878.8 | 0 | 3886.8 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.4075115741 | 57415 | 57049.4536805556 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y |
| THE MOON | 335.3702 | -6.281 | 56.37004308 | -48.74864005 | 248.3898 | 56990.2098148148 | 56990.3474768518 | 809001310 | 6224.2 | 45000 | 6224.2 | 6224.2 | 0 | 6224.2 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.4106481482 | 57415 | 57002.4438541667 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y |
| THE MOON | 337.3918 | -5.9294 | 58.6068568 | -50.1809823 | 252.3009 | 56990.3496643518 | 56990.483587963 | 809001320 | 6386.8 | 45000 | 6386.8 | 6386.8 | 0 | 6386.8 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.4101851852 | 57415 | 57006.395 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y |
| THE MOON | 339.1671 | -5.6557 | 60.63287277 | -51.42821416 | 248.2317 | 56990.4856828704 | 56990.608587963 | 809001330 | 6364.6 | 45000 | 6364.6 | 6364.6 | 0 | 6364.6 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.4115856482 | 57415 | 57006.4031018518 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y |
| THE MOON | 340.8235 | -5.0226 | 63.09935011 | -52.32405661 | 251.0714 | 56990.6104513889 | 56990.733587963 | 809001340 | 6356.6 | 45000 | 6356.6 | 6356.6 | 0 | 6356.6 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.4124537037 | 57415 | 57007.4026041667 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y |
| THE MOON | 342.4216 | -4.2139 | 65.81829296 | -53.01188957 | 247.9474 | 56990.7354513889 | 56990.8683101852 | 809001350 | 6319.6 | 45000 | 6319.6 | 6319.6 | 0 | 6319.6 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.4131018518 | 57415 | 57006.4014699074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y |
| THE MOON | 344.0153 | -3.4 | 68.62224539 | -53.63365394 | 247.8502 | 56990.8695717593 | 56991.0002546296 | 809001360 | 4899.8 | 45000 | 4899.8 | 4899.8 | 0 | 4899.8 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.4137615741 | 57415 | 57007.4035648148 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090016 | The Cosmic X-ray Background (CXB) was discovered almost 50 years ago. Despite many attempts to measure its spectrum, the normalization of the spectrum of the CXB in the 2-10 keV band has considerable uncertainty, of the order of 30% or more. The CXB represents an important integral of the total accretion power of supermassive black holes. We propose to use the dark side of the Moon as a shutter, thereby enabling a clear and unambiguous measurement of the CXB to be made with Suzaku. The motion of the Moon during a 45 ks observation extends over 5 deg, so by tracking the Moon we shall obtain an angle-averaged spectrum. Data from the Moon itself will be analysed and mosaicked to form an X-ray colour image highlighting different fluorescent lines from the bright side. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | UEDA | YOSHIHIRO | NULL | NULL | JAP | 9 | AO9 | USING THE MOON TO DETERMINE THE NORMALIZATION OF THE COSMIC X-RAY BACKGROUND | XIS | Y |
| CEN_A_LOBE_N1 | 201.8136 | -42.0782 | 310.00727378 | 20.30096505 | 292.0832 | 56859.7082060185 | 56861.2571990741 | 809002010 | 50380.1 | 50000 | 50388.1 | 50388.1 | 0 | 50380.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11477.5 | 11477.5 | 24471.9 | 0 | PROCESSED | 57615.4533333333 | 57242 | 56875.1360185185 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090021 | In AO1 and AO4, we conducted mapping observations of the western radio lobe of Fornax A, from which we disconvered thermal plasma pervasive in the lobe (Seta et al. 2013). Such a plasma may trace the AGN feedback activities influencing the evolution of the host galaxy and the cluster of galaxies, but much remains to be unveiled about its observational properties. In order to derive the surface brightness profile and the matalicity of the thermal plasma, we propose a 50 ks x 5 mapping observations of the northern radio lobe of Cen A, which is the largest radio lobe in appearance in the entire whole sky. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SETA | HIROMI | NULL | NULL | JAP | 9 | AO9 | MAPPING OBSERVATIONS OF THE NORTHERN RADIO LOBE OF THE CENTAURUS A | XIS | Y |
| CEN_A_LOBE_N2 | 201.2142 | -42.0778 | 309.53774085 | 20.36490033 | 292.2294 | 56861.2578587963 | 56862.6946990741 | 809003010 | 52142.7 | 50000 | 52150.7 | 52142.7 | 0 | 52158.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 19310.7 | 19310.7 | 40071.9 | 0 | PROCESSED | 57615.4510648148 | 57242 | 56875.1594560185 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090021 | In AO1 and AO4, we conducted mapping observations of the western radio lobe of Fornax A, from which we disconvered thermal plasma pervasive in the lobe (Seta et al. 2013). Such a plasma may trace the AGN feedback activities influencing the evolution of the host galaxy and the cluster of galaxies, but much remains to be unveiled about its observational properties. In order to derive the surface brightness profile and the matalicity of the thermal plasma, we propose a 50 ks x 5 mapping observations of the northern radio lobe of Cen A, which is the largest radio lobe in appearance in the entire whole sky. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SETA | HIROMI | NULL | NULL | JAP | 9 | AO9 | MAPPING OBSERVATIONS OF THE NORTHERN RADIO LOBE OF THE CENTAURUS A | XIS | Y |
| CEN_A_LOBE_N3 | 200.614 | -42.0794 | 309.06646515 | 20.4225822 | 293.3211 | 56862.6955439815 | 56864.2709722222 | 809004010 | 51489.4 | 50000 | 51489.4 | 51489.4 | 0 | 51489.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10638.4 | 10638.4 | 21480 | 0 | PROCESSED | 57615.4562384259 | 57242 | 56875.2082175926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090021 | In AO1 and AO4, we conducted mapping observations of the western radio lobe of Fornax A, from which we disconvered thermal plasma pervasive in the lobe (Seta et al. 2013). Such a plasma may trace the AGN feedback activities influencing the evolution of the host galaxy and the cluster of galaxies, but much remains to be unveiled about its observational properties. In order to derive the surface brightness profile and the matalicity of the thermal plasma, we propose a 50 ks x 5 mapping observations of the northern radio lobe of Cen A, which is the largest radio lobe in appearance in the entire whole sky. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SETA | HIROMI | NULL | NULL | JAP | 9 | AO9 | MAPPING OBSERVATIONS OF THE NORTHERN RADIO LOBE OF THE CENTAURUS A | XIS | Y |
| CEN_A_LOBE_N4 | 200.0149 | -42.0781 | 308.59567712 | 20.47867303 | 294.4884 | 56864.2718634259 | 56865.6863194444 | 809005010 | 49421.5 | 50000 | 49421.5 | 50309.3 | 0 | 50309.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14771.1 | 14771.1 | 31051.9 | 0 | PROCESSED | 57615.4593055556 | 57242 | 56875.2119675926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090021 | In AO1 and AO4, we conducted mapping observations of the western radio lobe of Fornax A, from which we disconvered thermal plasma pervasive in the lobe (Seta et al. 2013). Such a plasma may trace the AGN feedback activities influencing the evolution of the host galaxy and the cluster of galaxies, but much remains to be unveiled about its observational properties. In order to derive the surface brightness profile and the matalicity of the thermal plasma, we propose a 50 ks x 5 mapping observations of the northern radio lobe of Cen A, which is the largest radio lobe in appearance in the entire whole sky. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SETA | HIROMI | NULL | NULL | JAP | 9 | AO9 | MAPPING OBSERVATIONS OF THE NORTHERN RADIO LOBE OF THE CENTAURUS A | XIS | Y |
| CEN_A_LOBE_N5 | 198.8206 | -42.0777 | 307.6547721 | 20.57528449 | 295.9847 | 56865.6873032407 | 56867.2502430556 | 809006010 | 51939.2 | 50000 | 51939.2 | 52574.6 | 0 | 52574.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 10658.6 | 10658.6 | 20936 | 0 | PROCESSED | 57615.4722916667 | 57267 | 56898.3358449074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090021 | In AO1 and AO4, we conducted mapping observations of the western radio lobe of Fornax A, from which we disconvered thermal plasma pervasive in the lobe (Seta et al. 2013). Such a plasma may trace the AGN feedback activities influencing the evolution of the host galaxy and the cluster of galaxies, but much remains to be unveiled about its observational properties. In order to derive the surface brightness profile and the matalicity of the thermal plasma, we propose a 50 ks x 5 mapping observations of the northern radio lobe of Cen A, which is the largest radio lobe in appearance in the entire whole sky. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | SETA | HIROMI | NULL | NULL | JAP | 9 | AO9 | MAPPING OBSERVATIONS OF THE NORTHERN RADIO LOBE OF THE CENTAURUS A | XIS | Y |
| CENTAURUS CLUSTER NW | 191.8913 | -40.8227 | 302.14149361 | 22.04310508 | 292.0001 | 56850.5075462963 | 56854.4064236111 | 809007010 | 147888.9 | 150000 | 147888.9 | 148568.9 | 0 | 148568.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 14662.5 | 14662.5 | 46016 | 1 | PROCESSED | 57615.4267476852 | 57283 | 56917.6316666667 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090031 | We propose to observe the north-west offset (20'--40' or 0.4--0.8 r500) of the Centaurus cluster with a 150 ks exposure. A previous Suzaku observation with a 10 ks exposure yielded a very low Fe abundance (0.0-0.1 solar) in the ICM. With a 150 ks exposure, we will detect the Fe-K line of He-like Fe and derive Fe abundance with an accuracy of 0.05 solar. Then, we will be able to study the validity of the Fe abundance derived from the Fe L lines from cluster outskirts. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MATSUSHITA | KYOKO | NULL | NULL | JAP | 9 | AO9 | COMPARISON OF THE FE ABUNDANCES FROM THE L AND K LINES FROM THE CLUSTER OUTSKIRTS | XIS | Y |
| A2163NW | 243.7926 | -5.9349 | 6.85972512 | 30.71314923 | 93.93 | 57075.8011574074 | 57077.0558333333 | 809008010 | 48063.4 | 50000 | 48063.4 | 49733.9 | 0 | 49719.4 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.6490046296 | 57454 | 57087.4664467593 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090032 | Suzaku and Planck are complementary in the study of the cluster outskirts. We propose to cover Abell 2163 cluster which have the most accurate pressure with Planck out to the virial radius with two pointings (50 ks x 2) and background regions (30 ks x 2). The immediate objectives are to constrain the physical status of the intracluster medium such as clumping and bulk motions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MATSUSHITA | KYOKO | NULL | NULL | JAP | 9 | AO9 | SUZAKU AND PLANCK PRESSURE PROFILES OUT TO THE VIRIAL RADIUS OF THE HOTTEST CLUSTER, ABELL 2163 | XIS | Y |
| A2163SE | 244.1024 | -6.3096 | 6.72311865 | 30.24259241 | 94.6291 | 57074.4179282407 | 57075.8002662037 | 809009010 | 43294.5 | 50000 | 43294.5 | 51062.3 | 0 | 51094.3 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.6399421296 | 57453 | 57087.4694212963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090032 | Suzaku and Planck are complementary in the study of the cluster outskirts. We propose to cover Abell 2163 cluster which have the most accurate pressure with Planck out to the virial radius with two pointings (50 ks x 2) and background regions (30 ks x 2). The immediate objectives are to constrain the physical status of the intracluster medium such as clumping and bulk motions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MATSUSHITA | KYOKO | NULL | NULL | JAP | 9 | AO9 | SUZAKU AND PLANCK PRESSURE PROFILES OUT TO THE VIRIAL RADIUS OF THE HOTTEST CLUSTER, ABELL 2163 | XIS | Y |
| A2163BGD1 | 244.2972 | -6.0675 | 7.08170195 | 30.23063611 | 97.9997 | 57078.1207523148 | 57078.9737384259 | 809010010 | 28653.9 | 30000 | 28653.9 | 28661.9 | 0 | 28669.9 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.6666782407 | 57454 | 57087.4740393518 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090032 | Suzaku and Planck are complementary in the study of the cluster outskirts. We propose to cover Abell 2163 cluster which have the most accurate pressure with Planck out to the virial radius with two pointings (50 ks x 2) and background regions (30 ks x 2). The immediate objectives are to constrain the physical status of the intracluster medium such as clumping and bulk motions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MATSUSHITA | KYOKO | NULL | NULL | JAP | 9 | AO9 | SUZAKU AND PLANCK PRESSURE PROFILES OUT TO THE VIRIAL RADIUS OF THE HOTTEST CLUSTER, ABELL 2163 | XIS | Y |
| A2163BGD2 | 243.9063 | -6.5323 | 6.38161233 | 30.26602519 | 93.9997 | 57078.975787037 | 57079.8335763889 | 809011010 | 28816.6 | 30000 | 28832.6 | 28816.6 | 0 | 28840.6 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.6710763889 | 57458 | 57091.463587963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090032 | Suzaku and Planck are complementary in the study of the cluster outskirts. We propose to cover Abell 2163 cluster which have the most accurate pressure with Planck out to the virial radius with two pointings (50 ks x 2) and background regions (30 ks x 2). The immediate objectives are to constrain the physical status of the intracluster medium such as clumping and bulk motions. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | MATSUSHITA | KYOKO | NULL | NULL | JAP | 9 | AO9 | SUZAKU AND PLANCK PRESSURE PROFILES OUT TO THE VIRIAL RADIUS OF THE HOTTEST CLUSTER, ABELL 2163 | XIS | Y |
| RXCJ2157.4-0747 NW | 329.1863 | -7.8673 | 49.60582387 | -44.43308021 | 249.9998 | 56972.0423726852 | 56972.5418171296 | 809020010 | 23130.7 | 20000 | 23130.7 | 23130.7 | 0 | 23130.7 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7608101852 | 57352 | 56986.4053819444 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090049 | About 5-10% of galaxy clusters in the ROSAT survey have a very diffuse, low X-ray surface brightness (hereafter, LSB clusters). There are only 5 LSB clusters in the nearby universe, but it is no surprise that the majority of them may have been missed in existing X-ray surveys. Revealing gas and mass profiles of this unexplored population is critical not only for understanding its nature but cluster cosmology. Our Suzaku study of 2 LSB clusters indicated that their gas profiles deviate from self-similar expectations. We thus aim at establishing our findings by observing 3 remaining LSB clusters, clarifying whether they follow a similar trend, and inferring their mean gas profiles and dispersions. This study can only be achieved by the Suzaku's high sensitivity for diffuse emission. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | OTA | NAOMI | NULL | NULL | JAP | 9 | AO9 | PROBING THE NATURE OF VERY LOW SURFACE BRIGHTNESS CLUSTERS | XIS | Y |
| RXCJ2157.4-0747 NE | 329.3742 | -7.8003 | 49.81973283 | -44.55901105 | 250.0004 | 56972.5422453704 | 56973.0835069445 | 809021010 | 18630 | 20000 | 18646 | 18630 | 0 | 18646 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.764375 | 57352 | 56986.4078240741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090049 | About 5-10% of galaxy clusters in the ROSAT survey have a very diffuse, low X-ray surface brightness (hereafter, LSB clusters). There are only 5 LSB clusters in the nearby universe, but it is no surprise that the majority of them may have been missed in existing X-ray surveys. Revealing gas and mass profiles of this unexplored population is critical not only for understanding its nature but cluster cosmology. Our Suzaku study of 2 LSB clusters indicated that their gas profiles deviate from self-similar expectations. We thus aim at establishing our findings by observing 3 remaining LSB clusters, clarifying whether they follow a similar trend, and inferring their mean gas profiles and dispersions. This study can only be achieved by the Suzaku's high sensitivity for diffuse emission. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | OTA | NAOMI | NULL | NULL | JAP | 9 | AO9 | PROBING THE NATURE OF VERY LOW SURFACE BRIGHTNESS CLUSTERS | XIS | Y |
| RXCJ2157.4-0747 SE | 329.2877 | -7.568 | 50.03773919 | -44.36639016 | 250.0002 | 56973.0839351852 | 56973.6668055556 | 809022010 | 25958.4 | 20000 | 25974.4 | 25958.4 | 0 | 25982.4 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7636111111 | 57352 | 56986.4089351852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090049 | About 5-10% of galaxy clusters in the ROSAT survey have a very diffuse, low X-ray surface brightness (hereafter, LSB clusters). There are only 5 LSB clusters in the nearby universe, but it is no surprise that the majority of them may have been missed in existing X-ray surveys. Revealing gas and mass profiles of this unexplored population is critical not only for understanding its nature but cluster cosmology. Our Suzaku study of 2 LSB clusters indicated that their gas profiles deviate from self-similar expectations. We thus aim at establishing our findings by observing 3 remaining LSB clusters, clarifying whether they follow a similar trend, and inferring their mean gas profiles and dispersions. This study can only be achieved by the Suzaku's high sensitivity for diffuse emission. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | OTA | NAOMI | NULL | NULL | JAP | 9 | AO9 | PROBING THE NATURE OF VERY LOW SURFACE BRIGHTNESS CLUSTERS | XIS | Y |
| RXCJ2157.4-0747 SW | 329.5619 | -7.7328 | 50.03497203 | -44.68420804 | 250.0004 | 56976.2027893518 | 56976.7307175926 | 809023010 | 20918.8 | 20000 | 20918.8 | 20918.8 | 0 | 20918.8 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.786099537 | 57361 | 56993.4286921296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090049 | About 5-10% of galaxy clusters in the ROSAT survey have a very diffuse, low X-ray surface brightness (hereafter, LSB clusters). There are only 5 LSB clusters in the nearby universe, but it is no surprise that the majority of them may have been missed in existing X-ray surveys. Revealing gas and mass profiles of this unexplored population is critical not only for understanding its nature but cluster cosmology. Our Suzaku study of 2 LSB clusters indicated that their gas profiles deviate from self-similar expectations. We thus aim at establishing our findings by observing 3 remaining LSB clusters, clarifying whether they follow a similar trend, and inferring their mean gas profiles and dispersions. This study can only be achieved by the Suzaku's high sensitivity for diffuse emission. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | OTA | NAOMI | NULL | NULL | JAP | 9 | AO9 | PROBING THE NATURE OF VERY LOW SURFACE BRIGHTNESS CLUSTERS | XIS | Y |
| A3112E | 49.9177 | -44.1055 | 252.54334877 | -55.82694751 | 25.0007 | 56829.3656134259 | 56830.3266435185 | 809024010 | 33435 | 45000 | 33435 | 34195 | 0 | 34219 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 30293 | 30293 | 82991.8 | 1 | PROCESSED | 57615.3104398148 | 57239 | 56873.1925 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090061 | We propose to confirm the difference of the entropy profiles to the virial radius derived from Suzaku and Planck by 255 ksec Suzaku observations. Combination of X-ray and the Sunyuaev-Zel'dvitch effect observations play key roles for investigating not only cluster evolutions but also determining cosmological parameters because those observations are important complementary probe. While Suzaku observations found the flatter entropy slope than that expected from the numerical simulation in the outer region of the clusters, the entropy profile from the Planck observations agreed with the expected one well. This proposed observations would give hints in investigating the difference between the Suzaku and Planck results. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | SATO | KOSUKE | NULL | NULL | JAP | 9 | AO9 | ENTROPY PROFILE OF ABELL 3112 TO THE VIRIAL RADIUS FOR COMPARING TO PLANCK RESULTS | XIS | Y |
| A3112W | 49.1257 | -44.1666 | 252.9579492 | -56.34974536 | 40.0005 | 56834.0356481482 | 56835.5486458333 | 809025010 | 48949 | 45000 | 48949 | 48949 | 0 | 48949 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 11966 | 11966 | 40606.9 | 2 | PROCESSED | 57615.3397685185 | 57249 | 56881.2363078704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090061 | We propose to confirm the difference of the entropy profiles to the virial radius derived from Suzaku and Planck by 255 ksec Suzaku observations. Combination of X-ray and the Sunyuaev-Zel'dvitch effect observations play key roles for investigating not only cluster evolutions but also determining cosmological parameters because those observations are important complementary probe. While Suzaku observations found the flatter entropy slope than that expected from the numerical simulation in the outer region of the clusters, the entropy profile from the Planck observations agreed with the expected one well. This proposed observations would give hints in investigating the difference between the Suzaku and Planck results. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | SATO | KOSUKE | NULL | NULL | JAP | 9 | AO9 | ENTROPY PROFILE OF ABELL 3112 TO THE VIRIAL RADIUS FOR COMPARING TO PLANCK RESULTS | XIS | Y |
| A3112SE | 49.8254 | -44.4068 | 253.09009544 | -55.79916534 | 40.0009 | 56832.6869791667 | 56834.034849537 | 809026010 | 49844.3 | 45000 | 49852.3 | 49844.3 | 0 | 49860.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44224.6 | 44224.6 | 116441.8 | 0 | PROCESSED | 57615.347662037 | 57212 | 56846.5576273148 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090061 | We propose to confirm the difference of the entropy profiles to the virial radius derived from Suzaku and Planck by 255 ksec Suzaku observations. Combination of X-ray and the Sunyuaev-Zel'dvitch effect observations play key roles for investigating not only cluster evolutions but also determining cosmological parameters because those observations are important complementary probe. While Suzaku observations found the flatter entropy slope than that expected from the numerical simulation in the outer region of the clusters, the entropy profile from the Planck observations agreed with the expected one well. This proposed observations would give hints in investigating the difference between the Suzaku and Planck results. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | SATO | KOSUKE | NULL | NULL | JAP | 9 | AO9 | ENTROPY PROFILE OF ABELL 3112 TO THE VIRIAL RADIUS FOR COMPARING TO PLANCK RESULTS | XIS | Y |
| A3112N | 49.535 | -43.9764 | 252.47008016 | -56.12805661 | 40.0008 | 56831.1105439815 | 56832.6863194444 | 809027010 | 49532.3 | 45000 | 49532.3 | 49892.3 | 0 | 49892.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44240.5 | 44240.5 | 136135.6 | 2 | PROCESSED | 57615.3567476852 | 57212 | 56846.5678703704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090061 | We propose to confirm the difference of the entropy profiles to the virial radius derived from Suzaku and Planck by 255 ksec Suzaku observations. Combination of X-ray and the Sunyuaev-Zel'dvitch effect observations play key roles for investigating not only cluster evolutions but also determining cosmological parameters because those observations are important complementary probe. While Suzaku observations found the flatter entropy slope than that expected from the numerical simulation in the outer region of the clusters, the entropy profile from the Planck observations agreed with the expected one well. This proposed observations would give hints in investigating the difference between the Suzaku and Planck results. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | SATO | KOSUKE | NULL | NULL | JAP | 9 | AO9 | ENTROPY PROFILE OF ABELL 3112 TO THE VIRIAL RADIUS FOR COMPARING TO PLANCK RESULTS | XIS | Y |
| A3112BG | 50.3312 | -44.7001 | 253.38993788 | -55.36648392 | 25.002 | 56828.7830208333 | 56829.3648611111 | 809028010 | 13041 | 30000 | 13041 | 13041 | 0 | 24268 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 20199 | 20199 | 50255.9 | 0 | PROCESSED | 57615.2871064815 | 57394 | 56873.1992824074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090061 | We propose to confirm the difference of the entropy profiles to the virial radius derived from Suzaku and Planck by 255 ksec Suzaku observations. Combination of X-ray and the Sunyuaev-Zel'dvitch effect observations play key roles for investigating not only cluster evolutions but also determining cosmological parameters because those observations are important complementary probe. While Suzaku observations found the flatter entropy slope than that expected from the numerical simulation in the outer region of the clusters, the entropy profile from the Planck observations agreed with the expected one well. This proposed observations would give hints in investigating the difference between the Suzaku and Planck results. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | SATO | KOSUKE | NULL | NULL | JAP | 9 | AO9 | ENTROPY PROFILE OF ABELL 3112 TO THE VIRIAL RADIUS FOR COMPARING TO PLANCK RESULTS | XIS | Y |
| A3112BG | 50.3198 | -44.6958 | 253.38706356 | -55.37551095 | 204.9994 | 57009.69125 | 57010.2550462963 | 809028020 | 18354.5 | 15000 | 18354.5 | 18354.5 | 0 | 18354.5 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.5354166667 | 57394 | 57027.3975 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090061 | We propose to confirm the difference of the entropy profiles to the virial radius derived from Suzaku and Planck by 255 ksec Suzaku observations. Combination of X-ray and the Sunyuaev-Zel'dvitch effect observations play key roles for investigating not only cluster evolutions but also determining cosmological parameters because those observations are important complementary probe. While Suzaku observations found the flatter entropy slope than that expected from the numerical simulation in the outer region of the clusters, the entropy profile from the Planck observations agreed with the expected one well. This proposed observations would give hints in investigating the difference between the Suzaku and Planck results. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | SATO | KOSUKE | NULL | NULL | JAP | 9 | AO9 | ENTROPY PROFILE OF ABELL 3112 TO THE VIRIAL RADIUS FOR COMPARING TO PLANCK RESULTS | XIS | Y |
| A3391&A3395 FILAMENT | 96.6913 | -54.1225 | 262.85175229 | -25.18315788 | 316.4875 | 56791.0860532407 | 56792.4794328704 | 809033010 | 88613.4 | 92000 | 88613.4 | 88613.4 | 0 | 88613.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15244.8 | 15244.8 | 23346 | 0 | PROCESSED | 57615.0916319445 | 57227 | 56861.4967361111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090082 | To investigate hot gas properties of a large scale filament, we propose Suzaku observation (92 ks) of a filamentary structure between Abell 3391 and Abell 3395. A3391 and A3395 are located in Horologium supercluster and expected to be in an initial phase of a cluster merger. With Suzaku fs high sensitivity observation, we will (i) determine the physical conditions of IntraCluster Medium by measuring the temperature and density distribution, (ii) unveil the origin of the filamentary structure from distribution of abundance, pressure and entropy. Our study will reveal the formation history of the filament and provide a useful information for the future Sunyaev-Zeldovich effect observations. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | ISHISAKI | YOSHITAKA | NULL | NULL | JAP | 9 | AO9 | INVESTIGATION OF THE ORIGIN OF THE FILAMENTARY STRUCTURE BETWEEN ABELL 3391 AND ABELL 3395 | XIS | Y |
| PKS 0558-504 VIC 1 | 90.9582 | -50.6414 | 258.29690544 | -27.96668923 | 6.4262 | 56825.0805208333 | 56826.8543518518 | 809034010 | 52013.2 | 60000 | 52013.2 | 52013.2 | 0 | 52013.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 50487.4 | 50487.4 | 153247.9 | 0 | PROCESSED | 57615.2996180556 | 57233 | 56867.5608912037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090086 | We have conducted joint analysis of absorption and emission lines toward several targets and successfully constrained temperatures, extents, and densities of the hot gas for each directions. The results are all consistent and indicate the disk-like hot gas with its height of a few kpc from the Galactic plane. However, other research group claimed that the hot gas extends to > 100 kpc and can be a reservoir of the missing baryon. We propose for an observation of the vicinities of PKS 0558-504 in order to limit an extent of the hot gas surrounding our Galaxy and to clinch an argument that the hot gas can be a huge reservoir of the missing baryon. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | SAKAI | KAZUHIRO | NULL | NULL | JAP | 9 | AO9 | IS GALACTIC HOT GAS REALLY A HUGE RESERVOIR FOR THE MISSING BARYON? | XIS | Y |
| PKS 0558-504 VIC 2 | 88.9376 | -50.5474 | 257.96524127 | -29.21937587 | 349.9999 | 56822.2473148148 | 56824.093900463 | 809035010 | 60152.3 | 60000 | 60152.3 | 62172.8 | 0 | 62188.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 56747.6 | 56747.6 | 159531.8 | 2 | PROCESSED | 57615.2572800926 | 57204 | 56835.7714236111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090086 | We have conducted joint analysis of absorption and emission lines toward several targets and successfully constrained temperatures, extents, and densities of the hot gas for each directions. The results are all consistent and indicate the disk-like hot gas with its height of a few kpc from the Galactic plane. However, other research group claimed that the hot gas extends to > 100 kpc and can be a reservoir of the missing baryon. We propose for an observation of the vicinities of PKS 0558-504 in order to limit an extent of the hot gas surrounding our Galaxy and to clinch an argument that the hot gas can be a huge reservoir of the missing baryon. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | SAKAI | KAZUHIRO | NULL | NULL | JAP | 9 | AO9 | IS GALACTIC HOT GAS REALLY A HUGE RESERVOIR FOR THE MISSING BARYON? | XIS | Y |
| FJ1145+6430 | 176.4302 | 64.5188 | 134.11889935 | 51.15827028 | 157.0241 | 56940.8652199074 | 56941.847337963 | 809036010 | 44555.5 | 45000 | 44555.5 | 44915.5 | 0 | 44923.5 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.6416435185 | 57345 | 56979.4120949074 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090090 | Junctions of galaxy filaments are known to be the most active regions in structure formation in the Universe. These regions can be identified by using our original method based on SDSS galaxy distribution. We detected three merging groups of galaxies in such active regions. In AO9, we try to detect group-scale halos associated with merging phenomena in the final phase of a group evolution towards a cluster of galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MITSUISHI | IKUYUKI | NULL | NULL | JAP | 9 | AO9 | EXPLORING HOT GAS ASSOCIATED WITH MERGING GROUPS AT FILAMENT JUNCTIONS OF GALAXIES | XIS | Y |
| FJ0846+5326 | 131.5564 | 53.4343 | 164.73615985 | 38.37651034 | 277.0006 | 56764.8665393518 | 56766.1148032407 | 809037010 | 44716.6 | 45000 | 44716.6 | 44716.6 | 0 | 44716.6 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57614.9585416667 | 57145 | 56782.5079976852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090090 | Junctions of galaxy filaments are known to be the most active regions in structure formation in the Universe. These regions can be identified by using our original method based on SDSS galaxy distribution. We detected three merging groups of galaxies in such active regions. In AO9, we try to detect group-scale halos associated with merging phenomena in the final phase of a group evolution towards a cluster of galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MITSUISHI | IKUYUKI | NULL | NULL | JAP | 9 | AO9 | EXPLORING HOT GAS ASSOCIATED WITH MERGING GROUPS AT FILAMENT JUNCTIONS OF GALAXIES | XIS | Y |
| FJ0854+4908 | 133.7471 | 49.1347 | 170.1345398 | 40.07327965 | 275.4931 | 56775.9268865741 | 56776.9669328704 | 809038010 | 43471.3 | 45000 | 43471.3 | 43471.3 | 0 | 43471.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 40211.9 | 40211.9 | 89847.9 | 1 | PROCESSED | 57615.0216666667 | 57214 | 56848.6454166667 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090090 | Junctions of galaxy filaments are known to be the most active regions in structure formation in the Universe. These regions can be identified by using our original method based on SDSS galaxy distribution. We detected three merging groups of galaxies in such active regions. In AO9, we try to detect group-scale halos associated with merging phenomena in the final phase of a group evolution towards a cluster of galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MITSUISHI | IKUYUKI | NULL | NULL | JAP | 9 | AO9 | EXPLORING HOT GAS ASSOCIATED WITH MERGING GROUPS AT FILAMENT JUNCTIONS OF GALAXIES | XIS | Y |
| FJ0854+4908_OFFSET | 133.7467 | 48.8373 | 170.52256786 | 40.09070343 | 275.4911 | 56776.9674074074 | 56777.6286805556 | 809039010 | 31915.5 | 30000 | 31915.5 | 31915.5 | 0 | 31915.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28928 | 28928 | 57125.9 | 0 | PROCESSED | 57615.0205555556 | 57218 | 56852.6002546296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090090 | Junctions of galaxy filaments are known to be the most active regions in structure formation in the Universe. These regions can be identified by using our original method based on SDSS galaxy distribution. We detected three merging groups of galaxies in such active regions. In AO9, we try to detect group-scale halos associated with merging phenomena in the final phase of a group evolution towards a cluster of galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MITSUISHI | IKUYUKI | NULL | NULL | JAP | 9 | AO9 | EXPLORING HOT GAS ASSOCIATED WITH MERGING GROUPS AT FILAMENT JUNCTIONS OF GALAXIES | XIS | Y |
| FJ1336+3553 | 203.9051 | 36.0067 | 79.05269341 | 77.07938329 | 299.9994 | 56835.5627546296 | 56836.6564814815 | 809040010 | 49846.4 | 50000 | 49846.4 | 49846.4 | 0 | 49846.4 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.3306828704 | 57212 | 56846.5971180556 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090090 | Junctions of galaxy filaments are known to be the most active regions in structure formation in the Universe. These regions can be identified by using our original method based on SDSS galaxy distribution. We detected three merging groups of galaxies in such active regions. In AO9, we try to detect group-scale halos associated with merging phenomena in the final phase of a group evolution towards a cluster of galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MITSUISHI | IKUYUKI | NULL | NULL | JAP | 9 | AO9 | EXPLORING HOT GAS ASSOCIATED WITH MERGING GROUPS AT FILAMENT JUNCTIONS OF GALAXIES | XIS | Y |
| FJ1336+3553_OFFSET | 203.9396 | 35.8517 | 78.4395295 | 77.15761363 | 299.9998 | 56836.6568171296 | 56837.6530092593 | 809041010 | 43307 | 45000 | 43307 | 45501.9 | 0 | 45517.9 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.3386458333 | 57212 | 56846.5938425926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090090 | Junctions of galaxy filaments are known to be the most active regions in structure formation in the Universe. These regions can be identified by using our original method based on SDSS galaxy distribution. We detected three merging groups of galaxies in such active regions. In AO9, we try to detect group-scale halos associated with merging phenomena in the final phase of a group evolution towards a cluster of galaxies. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | MITSUISHI | IKUYUKI | NULL | NULL | JAP | 9 | AO9 | EXPLORING HOT GAS ASSOCIATED WITH MERGING GROUPS AT FILAMENT JUNCTIONS OF GALAXIES | XIS | Y |
| A1674_NE | 196.3328 | 67.5805 | 120.89335151 | 49.49272287 | 327.6637 | 56799.3349189815 | 56800.5487962963 | 809042010 | 60530.3 | 40000 | 0 | 60530.3 | 0 | 0 | 0 | 3 | 0 | 0 | 1 | 0 | 0 | 61651.2 | 61651.2 | 104859.7 | 2 | PROCESSED | 57615.1320023148 | 57626 | 56818.712650463 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090114 | A1674 is a nearby cluster of galaxies, cataloged as richness class 3. Regardless of this extreme richness, its X-ray luminosity is as low as 5e43 erg/s. Our Suzaku AO1 observation revealed that A1674 consists of at least two clusters, one at z~0.2 and the other at z~0.1. Moreover, excess hard X-ray emission was detected with an intensity exceeding the 90% confidence range of the NXB modeling uncertainty. We aim to confirm this hard X-ray emission and to localize that component (really diffuse or point-like) by performing 4 pointings during the AO9 phase. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | HAYASHIDA | KIYOSHI | NULL | NULL | JAP | 9 | AO9 | HARD X-RAY EMISSION IN THE CLUSTER OF GALAXIES A1674 | XIS | Y |
| A1674_Center | 195.9709 | 67.5098 | 121.09709791 | 49.57408901 | 327.6687 | 56800.5493171296 | 56801.6251736111 | 809042020 | 56039.5 | 40000 | 0 | 56039.5 | 0 | 0 | 0 | 2 | 0 | 0 | 1 | 0 | 0 | 56029.6 | 56029.6 | 92937.6 | 0 | PROCESSED | 57615.1546180556 | 57626 | 56862.7934837963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090114 | A1674 is a nearby cluster of galaxies, cataloged as richness class 3. Regardless of this extreme richness, its X-ray luminosity is as low as 5e43 erg/s. Our Suzaku AO1 observation revealed that A1674 consists of at least two clusters, one at z~0.2 and the other at z~0.1. Moreover, excess hard X-ray emission was detected with an intensity exceeding the 90% confidence range of the NXB modeling uncertainty. We aim to confirm this hard X-ray emission and to localize that component (really diffuse or point-like) by performing 4 pointings during the AO9 phase. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | HAYASHIDA | KIYOSHI | NULL | NULL | JAP | 9 | AO9 | HARD X-RAY EMISSION IN THE CLUSTER OF GALAXIES A1674 | XIS | Y |
| A1674_Offset | 196.9691 | 67.2995 | 120.47867852 | 49.75037622 | 328.362 | 56801.6258333333 | 56802.7363541667 | 809042030 | 67475.6 | 40000 | 0 | 67475.6 | 0 | 0 | 0 | 2 | 0 | 0 | 1 | 0 | 0 | 63453.5 | 63453.5 | 95941.8 | 0 | PROCESSED | 57615.1567013889 | 57626 | 56818.7013541667 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090114 | A1674 is a nearby cluster of galaxies, cataloged as richness class 3. Regardless of this extreme richness, its X-ray luminosity is as low as 5e43 erg/s. Our Suzaku AO1 observation revealed that A1674 consists of at least two clusters, one at z~0.2 and the other at z~0.1. Moreover, excess hard X-ray emission was detected with an intensity exceeding the 90% confidence range of the NXB modeling uncertainty. We aim to confirm this hard X-ray emission and to localize that component (really diffuse or point-like) by performing 4 pointings during the AO9 phase. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | HAYASHIDA | KIYOSHI | NULL | NULL | JAP | 9 | AO9 | HARD X-RAY EMISSION IN THE CLUSTER OF GALAXIES A1674 | XIS | Y |
| A1674_SW | 195.6324 | 67.4673 | 121.29194244 | 49.62561755 | 325.0183 | 56802.7378472222 | 56804.2224537037 | 809042040 | 6377.2 | 40000 | 6377.2 | 90849.8 | 0 | 6377.2 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 71076.8 | 71076.8 | 103078.8 | 1 | PROCESSED | 57615.185787037 | 57626 | 56818.7191203704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 090114 | A1674 is a nearby cluster of galaxies, cataloged as richness class 3. Regardless of this extreme richness, its X-ray luminosity is as low as 5e43 erg/s. Our Suzaku AO1 observation revealed that A1674 consists of at least two clusters, one at z~0.2 and the other at z~0.1. Moreover, excess hard X-ray emission was detected with an intensity exceeding the 90% confidence range of the NXB modeling uncertainty. We aim to confirm this hard X-ray emission and to localize that component (really diffuse or point-like) by performing 4 pointings during the AO9 phase. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | HAYASHIDA | KIYOSHI | NULL | NULL | JAP | 9 | AO9 | HARD X-RAY EMISSION IN THE CLUSTER OF GALAXIES A1674 | XIS | Y |
| NGC3221 | 155.5344 | 21.5594 | 213.96748211 | 55.66659318 | 113.4999 | 56977.5304513889 | 56980.5453125 | 809051010 | 121245.9 | 120000 | 121245.9 | 121245.9 | 0 | 121245.9 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.8106018518 | 57362 | 56995.6190162037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091501 | Late-type galaxies in the Local Universe are missing over 70% of their baryonic mass, a large fraction of which is likely embedded in the extended, low density warm-hot gaseous halo. However, searches of hot diffuse halos around massive spiral galaxies found them to be relatively small and not very massive. The UV observations have shown that the baryonic halo mass depends on the specific star formation rate (sSFR) and not on the total mass of the galaxy. We propose to observe the halo emission of NGC3221 with very high sSFR. Detection and characterization of the hot halo around this galaxy will expand our understanding of the dependence of halo properties on galaxy properties, and advance our understanding of galaxy formation, feedback and metal enrichment proposed by theoretical models. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | GUPTA | ANJALI | NULL | NULL | USA | 9 | AO9 | SEARCH FOR THE HOT GASEOUS HALO AROUND THE NEARBY SPIRAL GALAXY NGC3221 | XIS | Y |
| OFF-FIELD1 | 154.5616 | 22.312 | 212.25034337 | 55.01303699 | 298.5999 | 56782.6031712963 | 56783.5417939815 | 809052010 | 41103 | 40000 | 41103 | 41103 | 0 | 41103 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39028.3 | 39028.3 | 81071.9 | 1 | PROCESSED | 57615.0526388889 | 57162 | 56793.5659490741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091501 | Late-type galaxies in the Local Universe are missing over 70% of their baryonic mass, a large fraction of which is likely embedded in the extended, low density warm-hot gaseous halo. However, searches of hot diffuse halos around massive spiral galaxies found them to be relatively small and not very massive. The UV observations have shown that the baryonic halo mass depends on the specific star formation rate (sSFR) and not on the total mass of the galaxy. We propose to observe the halo emission of NGC3221 with very high sSFR. Detection and characterization of the hot halo around this galaxy will expand our understanding of the dependence of halo properties on galaxy properties, and advance our understanding of galaxy formation, feedback and metal enrichment proposed by theoretical models. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | GUPTA | ANJALI | NULL | NULL | USA | 9 | AO9 | SEARCH FOR THE HOT GASEOUS HALO AROUND THE NEARBY SPIRAL GALAXY NGC3221 | XIS | Y |
| OFF-FIELD2 | 156.3941 | 20.5095 | 216.1857144 | 56.11255364 | 112.0717 | 56982.1681018518 | 56983.2640046296 | 809053010 | 39828.7 | 40000 | 39828.7 | 39828.7 | 0 | 39828.7 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.8087847222 | 57377 | 57009.4169444444 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091501 | Late-type galaxies in the Local Universe are missing over 70% of their baryonic mass, a large fraction of which is likely embedded in the extended, low density warm-hot gaseous halo. However, searches of hot diffuse halos around massive spiral galaxies found them to be relatively small and not very massive. The UV observations have shown that the baryonic halo mass depends on the specific star formation rate (sSFR) and not on the total mass of the galaxy. We propose to observe the halo emission of NGC3221 with very high sSFR. Detection and characterization of the hot halo around this galaxy will expand our understanding of the dependence of halo properties on galaxy properties, and advance our understanding of galaxy formation, feedback and metal enrichment proposed by theoretical models. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | GUPTA | ANJALI | NULL | NULL | USA | 9 | AO9 | SEARCH FOR THE HOT GASEOUS HALO AROUND THE NEARBY SPIRAL GALAXY NGC3221 | XIS | Y |
| NGC 891 | 35.645 | 42.3416 | 140.39047988 | -17.41940889 | 243.1772 | 57072.5035300926 | 57073.2222916667 | 809054010 | 28873.8 | 100000 | 28873.8 | 28873.8 | 0 | 28873.8 | 3 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.6291550926 | 57626 | 57087.4767013889 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091502 | The metallicity of the hot gas in the halos of isolated galaxies distinguishes between two models of galaxy formation, but few galaxies have bright enough halos to make this measurement. Metallicities measured in these systems are applied broadly and used in models, so it is important to understand the limits of the measurement. We address two ilimitations: we estimate the systematic error in the metallicity by comparing Suzaku and XMM-Newton observations, and we determine whether the bright, metal-enriched gas around starburst galaxies represents most of their mass. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | HODGES-KLUCK | EDMUND | NULL | NULL | USA | 9 | AO9 | MEASURING SYSTEMATIC UNCERTAINTY IN THE HALO METALLICITY OF NGC 891 AND NGC 4631 | XIS | Y |
| NGC 953 | 37.7955 | 29.584 | 147.58231113 | -28.46974369 | 250.5565 | 57059.5397222222 | 57063.4376157407 | 809055010 | 150819.1 | 150000 | 150819.1 | 150867.1 | 0 | 150867.1 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.6137037037 | 56748 | 57107.4400578704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091503 | The mass profiles of elliptical galaxies are important probes of galaxy formation and cosmology. Only a few elliptical galaxies have detailed mass measurements from X-rays because of the lack of suitable targets in terms of total mass (< ~10^13 m_sun) and relaxed dynamical states appropriate for hydrostatic analysis. We have identified a sample of (hot) gas-rich isolated elliptical galaxies, most of which were discovered from previously awarded XMM and Chandra snapshot programs to search for optimal targets for X-ray studies of mass profiles on the galaxy scale. We request Suzaku observations to map the detailed profiles of stars, dark matter, and hot gas in two of these galaxies which have complementary Chandra observations. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | BUOTE | DAVID | NULL | NULL | USA | 9 | AO9 | THE DARK MATTER AND BARYON PROFILES OF ISOLATED ELLIPTICAL GALAXIES | XIS | Y |
| FG23 | 232.4567 | 44.1429 | 71.72776372 | 54.06523853 | 150.3369 | 57007.3108101852 | 57008.1494791667 | 809058010 | 38441.5 | 40000 | 38441.5 | 38441.5 | 0 | 38441.5 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.5220601852 | 57482 | 57114.5765972222 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091512 | Optical and X-ray measurements of fossil galaxy systems (FGs) suggest that they are old and relaxed. If FGs are assembled at higher redshifts, there is enough time for intermediate-luminosity galaxies to merge, resulting in the formation of the brightest group galaxy (BGG). We carry out the first systematic and multiwavelength study of a large sample of FGs, the FOssil Group Origins (FOGO) project. We propose to observe four bona fide fossil groups, most with T< 2 keV measuring Tx and Lx for objects at the mass scale of groups, which are rather unexplored. We will evaluate Lx-Tx, Lopt-Tx, and sigmaV-Tx relations as compared to our sample of fossil clusters completing the first X-ray selected sample of fossil systems ranging from the cluster to galaxy group scale. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | D'ONGHIA | ELENA | NULL | NULL | USA | 9 | AO9 | SCALING RELATIONS OF FOSSIL GALAXY GROUPS | XIS | Y |
| FG34 | 359.5671 | 15.0896 | 104.34552863 | -45.85455759 | 250.6856 | 56999.6725115741 | 57000.6669328704 | 809060010 | 38506.2 | 40000 | 38506.2 | 38506.2 | 0 | 38506.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35058.4 | 35058.4 | 85895.8 | 1 | PROCESSED | 57617.4968634259 | 57377 | 57010.1825925926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091512 | Optical and X-ray measurements of fossil galaxy systems (FGs) suggest that they are old and relaxed. If FGs are assembled at higher redshifts, there is enough time for intermediate-luminosity galaxies to merge, resulting in the formation of the brightest group galaxy (BGG). We carry out the first systematic and multiwavelength study of a large sample of FGs, the FOssil Group Origins (FOGO) project. We propose to observe four bona fide fossil groups, most with T< 2 keV measuring Tx and Lx for objects at the mass scale of groups, which are rather unexplored. We will evaluate Lx-Tx, Lopt-Tx, and sigmaV-Tx relations as compared to our sample of fossil clusters completing the first X-ray selected sample of fossil systems ranging from the cluster to galaxy group scale. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | D'ONGHIA | ELENA | NULL | NULL | USA | 9 | AO9 | SCALING RELATIONS OF FOSSIL GALAXY GROUPS | XIS | Y |
| FG10 | 163.7228 | 55.3656 | 151.60913312 | 54.78459511 | 121.1085 | 56973.8939467593 | 56975.0737615741 | 809061010 | 61108.5 | 60000 | 61108.5 | 61297.8 | 0 | 61297.8 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7792361111 | 57444 | 57076.4143865741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091512 | Optical and X-ray measurements of fossil galaxy systems (FGs) suggest that they are old and relaxed. If FGs are assembled at higher redshifts, there is enough time for intermediate-luminosity galaxies to merge, resulting in the formation of the brightest group galaxy (BGG). We carry out the first systematic and multiwavelength study of a large sample of FGs, the FOssil Group Origins (FOGO) project. We propose to observe four bona fide fossil groups, most with T< 2 keV measuring Tx and Lx for objects at the mass scale of groups, which are rather unexplored. We will evaluate Lx-Tx, Lopt-Tx, and sigmaV-Tx relations as compared to our sample of fossil clusters completing the first X-ray selected sample of fossil systems ranging from the cluster to galaxy group scale. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | D'ONGHIA | ELENA | NULL | NULL | USA | 9 | AO9 | SCALING RELATIONS OF FOSSIL GALAXY GROUPS | XIS | Y |
| MKW4-WN | 181.4571 | 2.3391 | 277.2234025 | 62.91169747 | 110.2998 | 56994.5218865741 | 56996.9723842593 | 809062010 | 90365.2 | 100000 | 90365.2 | 91517.2 | 0 | 91517.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 88738.5 | 88738.5 | 211705.7 | 1 | PROCESSED | 57617.4717361111 | 56748 | 57007.0908912037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091513 | We propose to observe the nearby group MKW4 by leveraging existing observations to provide coverage from its center to its virial radius in two orthogonal directions. Four additional pointings, combined with two existing pointings, will allow us to determine radial profiles of gas temperature, density, entropy, pressure, and gas mass fraction, as well as their azimuthal variation. Comparing these properties to those of clusters will allow us to probe the role played by baryonic physics and assess the imprints of hierarchical structure formation. The stable and low background of the Suzaku XIS is crucial for the study of galaxy groups to their virial radii. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | SU | YUANYUAN | NULL | NULL | USA | 9 | AO9 | PROBING A TYPICAL GALAXY GROUP TO ITS VIRIAL RADIUS | XIS | Y |
| RXJ1159+5531 E | 180.1946 | 55.5211 | 137.37799324 | 60.16358606 | 301.575 | 56806.5416550926 | 56808.2502430556 | 809063010 | 99161.8 | 100000 | 99177.8 | 99161.8 | 0 | 99177.8 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.1713657407 | 57234 | 56866.7150925926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091521 | In contrast to some recent observations of cluster outskirts, for RXJ1159+5531, we obtain measurements of the gas fraction and entropy at the virial radius that are fully consistent with gravity-only structure formation simulations. Our preliminary Suzaku analysis of an opposite direction shows similar results. This encouraging consistency suggests that we may see little azimuthal variation in the gas properties for this unusually relaxed system. To verify and also benefit from the relaxed state of this benchmark system, we propose complementary Suzaku observations of RXJ1159+5531 in the other two directions. Simultaneously fitting these pointings would provide us the metal abundance ratios at large radii in order to place broad constrains on the enrichment history of group scale systems. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | SU | YUANYUAN | NULL | NULL | USA | 9 | AO9 | MAPPING A BENCHMARK RELAXED POOR CLUSTER OUT TO ITS VIRIAL RADIUS WITH SUZAKU | XIS | Y |
| RXJ1159+5531 W | 179.7493 | 55.5442 | 137.82331154 | 60.04203639 | 299.9575 | 56808.2513657407 | 56809.8959490741 | 809064010 | 95109 | 100000 | 95109 | 96041 | 0 | 96033 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.1837731482 | 57194 | 56828.5942592593 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091521 | In contrast to some recent observations of cluster outskirts, for RXJ1159+5531, we obtain measurements of the gas fraction and entropy at the virial radius that are fully consistent with gravity-only structure formation simulations. Our preliminary Suzaku analysis of an opposite direction shows similar results. This encouraging consistency suggests that we may see little azimuthal variation in the gas properties for this unusually relaxed system. To verify and also benefit from the relaxed state of this benchmark system, we propose complementary Suzaku observations of RXJ1159+5531 in the other two directions. Simultaneously fitting these pointings would provide us the metal abundance ratios at large radii in order to place broad constrains on the enrichment history of group scale systems. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | SU | YUANYUAN | NULL | NULL | USA | 9 | AO9 | MAPPING A BENCHMARK RELAXED POOR CLUSTER OUT TO ITS VIRIAL RADIUS WITH SUZAKU | XIS | Y |
| CENTAURUS SE4 | 192.8602 | -42.5262 | 302.93248329 | 20.34554874 | 294.0685 | 56854.4082407407 | 56854.9480092593 | 809068010 | 20659 | 20000 | 20659 | 20659 | 0 | 20659 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 10395 | 10395 | 22031.9 | 0 | PROCESSED | 57615.3959606482 | 57250 | 56883.1729050926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091522 | We propose here to observe the outskirts of the X-ray bright, nearby Centaurus cluster with good azimuthal coverage by adding 3 new arms with total exposure 204ks. This will extend our initial analysis in one direction to the north-west which has allowed our team to obtain high spatial resolution profiles of temperature, density and entropy. The XMM temperature map of the central 30 arcmins shows a complex temperature environment and deviations from spherical symmetry, and good azimuthal coverage is important to obtain an accurate understanding of the outskirts.Observations of the Perseus cluster have shown significant azimuthal variations in the ICM temperature and entropy. Centaurus is the best target for understanding the ICM in the outskirts of a relaxed, intermediate mass cluster. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | REYNOLDS | CHRISTOPHER | NULL | NULL | USA | 9 | AO9 | OBSERVATIONS OF THE X-RAY BRIGHT, NEARBY CENTAURUS CLUSTER TO THE VIRIAL RADIUS | XIS | Y |
| ABELL 98-CENTER | 11.6247 | 20.5572 | 121.3687084 | -42.29955696 | 80.8972 | 56837.6648726852 | 56839.2014236111 | 809077010 | 60781 | 60000 | 60781 | 60917 | 0 | 60925 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.3554282407 | 56748 | 56854.7844212963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091525 | We propose to observe the outskirts of the strongly merging cluster Abell 98 both along and perpendicular to the large scale structure filament implied by the orientation of its three merging subclusters. This is the only remaining one of the four bright, strongly merging "double" clusters originally identified from Einstein observations that has not been observed with Suzaku. A comparison of the extended atmosphere in the filament and off-filament pointings will allow us to test for the presence of unresolved gas clumps, which should be more abundant along the filament, invoked to explain anomalously high (above cosmic) baryon fractions observed in some other clusters. If this "unresolved clumps" hypothesis is correct, then we should find higher baryon fractions along the filament. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | RANDALL | SCOTT | NULL | NULL | USA | 9 | AO9 | EXPLORING THE EXTENDED ATMOSPHERE OF THE STRONGLY MERGING CLUSTER ABELL 98 | XIS | Y |
| ABELL 98-NORTH | 11.5755 | 20.8389 | 121.31667052 | -42.01674062 | 67.4405 | 56840.5909259259 | 56841.1634375 | 809078010 | 25058.2 | 100000 | 0 | 0 | 0 | 25058.2 | 0 | 0 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.3531481482 | 56748 | 56855.7487268518 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091525 | We propose to observe the outskirts of the strongly merging cluster Abell 98 both along and perpendicular to the large scale structure filament implied by the orientation of its three merging subclusters. This is the only remaining one of the four bright, strongly merging "double" clusters originally identified from Einstein observations that has not been observed with Suzaku. A comparison of the extended atmosphere in the filament and off-filament pointings will allow us to test for the presence of unresolved gas clumps, which should be more abundant along the filament, invoked to explain anomalously high (above cosmic) baryon fractions observed in some other clusters. If this "unresolved clumps" hypothesis is correct, then we should find higher baryon fractions along the filament. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | RANDALL | SCOTT | NULL | NULL | USA | 9 | AO9 | EXPLORING THE EXTENDED ATMOSPHERE OF THE STRONGLY MERGING CLUSTER ABELL 98 | XIS | Y |
| ABELL 98-NORTH | 11.5751 | 20.8392 | 121.31617836 | -42.01643069 | 67.4405 | 56841.1634490741 | 56841.958599537 | 809078020 | 23888 | 100000 | 24680 | 23888 | 0 | 24939.6 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.3618865741 | 56748 | 56875.6040393518 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091525 | We propose to observe the outskirts of the strongly merging cluster Abell 98 both along and perpendicular to the large scale structure filament implied by the orientation of its three merging subclusters. This is the only remaining one of the four bright, strongly merging "double" clusters originally identified from Einstein observations that has not been observed with Suzaku. A comparison of the extended atmosphere in the filament and off-filament pointings will allow us to test for the presence of unresolved gas clumps, which should be more abundant along the filament, invoked to explain anomalously high (above cosmic) baryon fractions observed in some other clusters. If this "unresolved clumps" hypothesis is correct, then we should find higher baryon fractions along the filament. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | RANDALL | SCOTT | NULL | NULL | USA | 9 | AO9 | EXPLORING THE EXTENDED ATMOSPHERE OF THE STRONGLY MERGING CLUSTER ABELL 98 | XIS | Y |
| ABELL 98-NORTH | 11.5799 | 20.8287 | 121.32183614 | -42.02704716 | 251.2557 | 57012.9175231482 | 57014.2377430556 | 809078030 | 49538.1 | 50000 | 49538.1 | 51792.5 | 0 | 51808.5 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.5690509259 | 56748 | 57107.4424305556 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091525 | We propose to observe the outskirts of the strongly merging cluster Abell 98 both along and perpendicular to the large scale structure filament implied by the orientation of its three merging subclusters. This is the only remaining one of the four bright, strongly merging "double" clusters originally identified from Einstein observations that has not been observed with Suzaku. A comparison of the extended atmosphere in the filament and off-filament pointings will allow us to test for the presence of unresolved gas clumps, which should be more abundant along the filament, invoked to explain anomalously high (above cosmic) baryon fractions observed in some other clusters. If this "unresolved clumps" hypothesis is correct, then we should find higher baryon fractions along the filament. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | RANDALL | SCOTT | NULL | NULL | USA | 9 | AO9 | EXPLORING THE EXTENDED ATMOSPHERE OF THE STRONGLY MERGING CLUSTER ABELL 98 | XIS | Y |
| ABELL 98-WEST | 11.3131 | 20.6695 | 120.97936172 | -42.17879703 | 80.8359 | 56841.9624537037 | 56844.7606712963 | 809079010 | 96692.4 | 100000 | 96692.4 | 100643.8 | 0 | 100659.8 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.3882638889 | 56748 | 56881.441724537 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091525 | We propose to observe the outskirts of the strongly merging cluster Abell 98 both along and perpendicular to the large scale structure filament implied by the orientation of its three merging subclusters. This is the only remaining one of the four bright, strongly merging "double" clusters originally identified from Einstein observations that has not been observed with Suzaku. A comparison of the extended atmosphere in the filament and off-filament pointings will allow us to test for the presence of unresolved gas clumps, which should be more abundant along the filament, invoked to explain anomalously high (above cosmic) baryon fractions observed in some other clusters. If this "unresolved clumps" hypothesis is correct, then we should find higher baryon fractions along the filament. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | RANDALL | SCOTT | NULL | NULL | USA | 9 | AO9 | EXPLORING THE EXTENDED ATMOSPHERE OF THE STRONGLY MERGING CLUSTER ABELL 98 | XIS | Y |
| ABELL 98-SOUTH | 11.6766 | 20.275 | 121.42486866 | -42.58290308 | 251.4904 | 57011.5401736111 | 57012.9168171296 | 809080010 | 48257.9 | 100000 | 48257.9 | 49054.4 | 0 | 49110.4 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.5485532407 | 56748 | 57107.4443171296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091525 | We propose to observe the outskirts of the strongly merging cluster Abell 98 both along and perpendicular to the large scale structure filament implied by the orientation of its three merging subclusters. This is the only remaining one of the four bright, strongly merging "double" clusters originally identified from Einstein observations that has not been observed with Suzaku. A comparison of the extended atmosphere in the filament and off-filament pointings will allow us to test for the presence of unresolved gas clumps, which should be more abundant along the filament, invoked to explain anomalously high (above cosmic) baryon fractions observed in some other clusters. If this "unresolved clumps" hypothesis is correct, then we should find higher baryon fractions along the filament. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | RANDALL | SCOTT | NULL | NULL | USA | 9 | AO9 | EXPLORING THE EXTENDED ATMOSPHERE OF THE STRONGLY MERGING CLUSTER ABELL 98 | XIS | Y |
| ABELL 2259 | 259.9722 | 27.8097 | 50.52312942 | 31.25775464 | 109.9997 | 57081.1636458333 | 57082.4113194445 | 809081010 | 42220.3 | 42500 | 42220.3 | 43044.3 | 0 | 43100.3 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.6840509259 | 57465 | 57091.4611226852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091526 | Precision cosmology studies with regular galaxy clusters require a full understanding of cluster physics with a few percent systematic uncertainty. Most of the studies on regular cluster outskirts are limited to cool core clusters but not many were studied for "regular" non-cool core clusters. We propose a 170 ks Suzaku observation of a regular non-cool core cluster Abell 2259. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will compare results to cool core clusters and test models for pre-heating, shock heating, thermal conduction, e-p equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | WONG | KA-WAH | NULL | NULL | USA | 9 | AO9 | REGULAR NON-COOL CORE GALAXY CLUSTER OUT TO THE VIRIAL RADIUS | XIS | Y |
| ABELL 2259 | 260.1834 | 27.7413 | 50.50845469 | 31.05916058 | 109.9997 | 57082.4117476852 | 57083.6002199074 | 809081020 | 42592.8 | 42500 | 42592.8 | 43016.8 | 0 | 43056.8 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.687650463 | 57465 | 57097.407037037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091526 | Precision cosmology studies with regular galaxy clusters require a full understanding of cluster physics with a few percent systematic uncertainty. Most of the studies on regular cluster outskirts are limited to cool core clusters but not many were studied for "regular" non-cool core clusters. We propose a 170 ks Suzaku observation of a regular non-cool core cluster Abell 2259. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will compare results to cool core clusters and test models for pre-heating, shock heating, thermal conduction, e-p equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | WONG | KA-WAH | NULL | NULL | USA | 9 | AO9 | REGULAR NON-COOL CORE GALAXY CLUSTER OUT TO THE VIRIAL RADIUS | XIS | Y |
| ABELL 2259 | 260.1067 | 27.5543 | 50.27658806 | 31.07091189 | 109.9997 | 57083.6006018518 | 57084.7258564815 | 809081030 | 44246.8 | 42500 | 44246.8 | 44254.8 | 0 | 44254.8 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.7027314815 | 57475 | 57107.4892476852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091526 | Precision cosmology studies with regular galaxy clusters require a full understanding of cluster physics with a few percent systematic uncertainty. Most of the studies on regular cluster outskirts are limited to cool core clusters but not many were studied for "regular" non-cool core clusters. We propose a 170 ks Suzaku observation of a regular non-cool core cluster Abell 2259. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will compare results to cool core clusters and test models for pre-heating, shock heating, thermal conduction, e-p equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | WONG | KA-WAH | NULL | NULL | USA | 9 | AO9 | REGULAR NON-COOL CORE GALAXY CLUSTER OUT TO THE VIRIAL RADIUS | XIS | Y |
| ABELL 2259 | 259.8931 | 27.621 | 50.28820146 | 31.27138653 | 102.8681 | 57093.1224305556 | 57094.3141203704 | 809081040 | 43027 | 42500 | 43027 | 43027 | 0 | 43526.6 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.7751736111 | 57475 | 57108.4150578704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091526 | Precision cosmology studies with regular galaxy clusters require a full understanding of cluster physics with a few percent systematic uncertainty. Most of the studies on regular cluster outskirts are limited to cool core clusters but not many were studied for "regular" non-cool core clusters. We propose a 170 ks Suzaku observation of a regular non-cool core cluster Abell 2259. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will compare results to cool core clusters and test models for pre-heating, shock heating, thermal conduction, e-p equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | WONG | KA-WAH | NULL | NULL | USA | 9 | AO9 | REGULAR NON-COOL CORE GALAXY CLUSTER OUT TO THE VIRIAL RADIUS | XIS | Y |
| ABELL 3411 | 130.503 | -17.558 | 242.03718903 | 14.84069283 | 105.0003 | 56964.4121759259 | 56967.3091898148 | 809082010 | 126679.2 | 130000 | 126679.2 | 131271.2 | 0 | 131263.2 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.749525463 | 57358 | 56982.4526273148 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091528 | Galaxy cluster mergers trigger Mpc-scale shocks in the ICM, which can accelerate particles to relativistic energies to form arc-shaped radio relics. Last year, we discovered a spectacular radio relic in the Planck cluster A3411. The relic has a complex, fragmentary morphology, at odds with the arc-shaped shocks predicted by hydrodynamical simulations. In light of this unexpected discovery, we propose for a 169-ks Suzaku observation to characterize the ICM properties at the radio relic in A3411. The combination of high-quality X-ray and radio data will provide a unique opportunity to (1) measure the shock properties and relate them to the radio structures; (2) explore the reason for the fragmentation of the relic; (3) model the merger event; and (4) test different shock acceleration models. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | VAN WEEREN | REINOUT | NULL | NULL | USA | 9 | AO9 | ABELL 3411: PARTICLE RE-ACCELERATION AND A COMPLEX SHOCK GEOMETRY? | XIS | Y |
| ABELL 3411 OFFSET | 130.7649 | -17.3143 | 241.9812862 | 15.18552207 | 105.3327 | 56967.309849537 | 56968.1939467593 | 809083010 | 38952 | 39000 | 38952 | 39272 | 0 | 39288 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7398263889 | 57358 | 56982.4550231482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091528 | Galaxy cluster mergers trigger Mpc-scale shocks in the ICM, which can accelerate particles to relativistic energies to form arc-shaped radio relics. Last year, we discovered a spectacular radio relic in the Planck cluster A3411. The relic has a complex, fragmentary morphology, at odds with the arc-shaped shocks predicted by hydrodynamical simulations. In light of this unexpected discovery, we propose for a 169-ks Suzaku observation to characterize the ICM properties at the radio relic in A3411. The combination of high-quality X-ray and radio data will provide a unique opportunity to (1) measure the shock properties and relate them to the radio structures; (2) explore the reason for the fragmentation of the relic; (3) model the merger event; and (4) test different shock acceleration models. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | VAN WEEREN | REINOUT | NULL | NULL | USA | 9 | AO9 | ABELL 3411: PARTICLE RE-ACCELERATION AND A COMPLEX SHOCK GEOMETRY? | XIS | Y |
| SWCL0759+3244 | 119.7517 | 32.7514 | 188.23731341 | 27.65711067 | 99.0622 | 56961.3067708333 | 56962.2286574074 | 809085010 | 42303.9 | 41000 | 42303.9 | 42303.9 | 0 | 42303.9 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7390277778 | 57345 | 56979.4492708333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091531 | The evolution of X-ray properties of galaxy clusters with redshift provides important constraints on the self-similar models of cluster evolution. The scaling relations and their deviations from self-similar models due to non-gravitational processes are important for modeling the cluster selection function for cosmology. We propose to observe a uniform sample of z ~ 0.6 galaxy clusters, selected from Swift archival data and confirmed by multi-band optical data, using Suzaku to better characterize their X-ray properties such as the X-ray luminosity and temperature. With this uniformly selected sample from a narrow redshift bin, we are able to independently constrain the self-similar evolution of cluster properties with redshift. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | DAI | XINYU | NULL | NULL | USA | 9 | AO9 | X-RAY PROPERTIES OF A UNIFORMLY SELECTED SAMPLE OF Z ~ 0.6 CLUSTERS | XIS | Y |
| SWCL1313+0802 | 198.2492 | 8.0414 | 318.90135946 | 70.24184099 | 291.5304 | 56850.0041435185 | 56850.5002199074 | 809087010 | 20270.5 | 20000 | 20270.5 | 20270.5 | 0 | 20270.5 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.3782986111 | 57229 | 56861.6452083333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091531 | The evolution of X-ray properties of galaxy clusters with redshift provides important constraints on the self-similar models of cluster evolution. The scaling relations and their deviations from self-similar models due to non-gravitational processes are important for modeling the cluster selection function for cosmology. We propose to observe a uniform sample of z ~ 0.6 galaxy clusters, selected from Swift archival data and confirmed by multi-band optical data, using Suzaku to better characterize their X-ray properties such as the X-ray luminosity and temperature. With this uniformly selected sample from a narrow redshift bin, we are able to independently constrain the self-similar evolution of cluster properties with redshift. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | DAI | XINYU | NULL | NULL | USA | 9 | AO9 | X-RAY PROPERTIES OF A UNIFORMLY SELECTED SAMPLE OF Z ~ 0.6 CLUSTERS | XIS | Y |
| SWCL1330+4206 | 202.7226 | 42.119 | 97.20252966 | 72.98152353 | 144.6477 | 56984.0225347222 | 56985.3840740741 | 809088010 | 15861.2 | 49000 | 15861.2 | 15877.6 | 0 | 15869.2 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.8069212963 | 57548 | 57009.4143981482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091531 | The evolution of X-ray properties of galaxy clusters with redshift provides important constraints on the self-similar models of cluster evolution. The scaling relations and their deviations from self-similar models due to non-gravitational processes are important for modeling the cluster selection function for cosmology. We propose to observe a uniform sample of z ~ 0.6 galaxy clusters, selected from Swift archival data and confirmed by multi-band optical data, using Suzaku to better characterize their X-ray properties such as the X-ray luminosity and temperature. With this uniformly selected sample from a narrow redshift bin, we are able to independently constrain the self-similar evolution of cluster properties with redshift. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | DAI | XINYU | NULL | NULL | USA | 9 | AO9 | X-RAY PROPERTIES OF A UNIFORMLY SELECTED SAMPLE OF Z ~ 0.6 CLUSTERS | XIS | Y |
| SWCL1330+4206 | 202.7007 | 42.1031 | 97.22165079 | 73.00355707 | 325.866 | 57166.2929166667 | 57167.0793171296 | 809088020 | 34779.6 | 34000 | 34779.6 | 34787.6 | 0 | 34779.6 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 21068.6 | 21068.6 | 53048 | 1 | PROCESSED | 57618.72625 | 57548 | 57178.157025463 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091531 | The evolution of X-ray properties of galaxy clusters with redshift provides important constraints on the self-similar models of cluster evolution. The scaling relations and their deviations from self-similar models due to non-gravitational processes are important for modeling the cluster selection function for cosmology. We propose to observe a uniform sample of z ~ 0.6 galaxy clusters, selected from Swift archival data and confirmed by multi-band optical data, using Suzaku to better characterize their X-ray properties such as the X-ray luminosity and temperature. With this uniformly selected sample from a narrow redshift bin, we are able to independently constrain the self-similar evolution of cluster properties with redshift. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | DAI | XINYU | NULL | NULL | USA | 9 | AO9 | X-RAY PROPERTIES OF A UNIFORMLY SELECTED SAMPLE OF Z ~ 0.6 CLUSTERS | XIS | Y |
| ABELL 2151A | 241.1446 | 17.7141 | 31.46236827 | 44.65865226 | 285.8808 | 56883.5616898148 | 56883.843900463 | 809098010 | 11026.8 | 10000 | 11034.8 | 11034.8 | 0 | 11026.8 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.4947569444 | 57270 | 56910.6327893518 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 092015 | Upcoming X-ray surveys like eROSITA, require precise calibration between X-ray observables (e.g. luminosity and temperature) and mass, down to the low mass regime to set tight constraints on the fundamental cosmological parameters. We propose to observe 19 galaxy groups with a total exposure time of 230 ks to complete observations for a flux limited sample. We will use this complete sample to study the scaling law properties of the low mass systems with a view to the eROSITA survey, which is expected to detect 100,000 objects, most of them in the low mass regime. Furthermore, we will investigate the relative importance of gravitational and non-gravitational processes by studying their thermodynamical properties beyond R500. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | LOVISARI | LORENZO | NULL | NULL | EUR | 9 | AO9 | SCALING PROPERTIES AND THE EFFECTS OF FEEDBACK FOR A COMPLETE SAMPLE OF GALAXY GROUPS | XIS | Y |
| NGC 6338 | 258.8129 | 57.4208 | 85.8195722 | 35.41601483 | 46.4308 | 56771.4831712963 | 56771.8058333333 | 809099010 | 15475.6 | 10000 | 15475.6 | 15475.6 | 0 | 15475.6 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 14525.9 | 14525.9 | 26044.9 | 0 | PROCESSED | 57614.9892708333 | 57155 | 56789.6384722222 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 092015 | Upcoming X-ray surveys like eROSITA, require precise calibration between X-ray observables (e.g. luminosity and temperature) and mass, down to the low mass regime to set tight constraints on the fundamental cosmological parameters. We propose to observe 19 galaxy groups with a total exposure time of 230 ks to complete observations for a flux limited sample. We will use this complete sample to study the scaling law properties of the low mass systems with a view to the eROSITA survey, which is expected to detect 100,000 objects, most of them in the low mass regime. Furthermore, we will investigate the relative importance of gravitational and non-gravitational processes by studying their thermodynamical properties beyond R500. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | LOVISARI | LORENZO | NULL | NULL | EUR | 9 | AO9 | SCALING PROPERTIES AND THE EFFECTS OF FEEDBACK FOR A COMPLETE SAMPLE OF GALAXY GROUPS | XIS | Y |
| ABELL 2877 | 17.5065 | -45.9303 | 293.04607396 | -70.83949903 | 47.4208 | 56809.9110532407 | 56810.1181712963 | 809100010 | 11908 | 10000 | 11916 | 11908 | 0 | 11930.6 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.1778240741 | 57197 | 56828.5915856482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 092015 | Upcoming X-ray surveys like eROSITA, require precise calibration between X-ray observables (e.g. luminosity and temperature) and mass, down to the low mass regime to set tight constraints on the fundamental cosmological parameters. We propose to observe 19 galaxy groups with a total exposure time of 230 ks to complete observations for a flux limited sample. We will use this complete sample to study the scaling law properties of the low mass systems with a view to the eROSITA survey, which is expected to detect 100,000 objects, most of them in the low mass regime. Furthermore, we will investigate the relative importance of gravitational and non-gravitational processes by studying their thermodynamical properties beyond R500. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | LOVISARI | LORENZO | NULL | NULL | EUR | 9 | AO9 | SCALING PROPERTIES AND THE EFFECTS OF FEEDBACK FOR A COMPLETE SAMPLE OF GALAXY GROUPS | XIS | Y |
| MKW8 | 220.1793 | 3.4582 | 355.49716412 | 54.76401984 | 291.2239 | 56859.4682986111 | 56859.7009259259 | 809101010 | 10412 | 10000 | 10412 | 10488 | 0 | 10495.6 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.4174305556 | 57239 | 56873.5532523148 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 092015 | Upcoming X-ray surveys like eROSITA, require precise calibration between X-ray observables (e.g. luminosity and temperature) and mass, down to the low mass regime to set tight constraints on the fundamental cosmological parameters. We propose to observe 19 galaxy groups with a total exposure time of 230 ks to complete observations for a flux limited sample. We will use this complete sample to study the scaling law properties of the low mass systems with a view to the eROSITA survey, which is expected to detect 100,000 objects, most of them in the low mass regime. Furthermore, we will investigate the relative importance of gravitational and non-gravitational processes by studying their thermodynamical properties beyond R500. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | LOVISARI | LORENZO | NULL | NULL | EUR | 9 | AO9 | SCALING PROPERTIES AND THE EFFECTS OF FEEDBACK FOR A COMPLETE SAMPLE OF GALAXY GROUPS | XIS | Y |
| AWM4 | 241.2331 | 23.9108 | 39.92527821 | 46.49145981 | 302.6954 | 56859.2473263889 | 56859.4627314815 | 809102010 | 9310 | 11000 | 9310 | 9438 | 0 | 9438 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.4155092593 | 57239 | 56873.5548958333 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 092015 | Upcoming X-ray surveys like eROSITA, require precise calibration between X-ray observables (e.g. luminosity and temperature) and mass, down to the low mass regime to set tight constraints on the fundamental cosmological parameters. We propose to observe 19 galaxy groups with a total exposure time of 230 ks to complete observations for a flux limited sample. We will use this complete sample to study the scaling law properties of the low mass systems with a view to the eROSITA survey, which is expected to detect 100,000 objects, most of them in the low mass regime. Furthermore, we will investigate the relative importance of gravitational and non-gravitational processes by studying their thermodynamical properties beyond R500. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | LOVISARI | LORENZO | NULL | NULL | EUR | 9 | AO9 | SCALING PROPERTIES AND THE EFFECTS OF FEEDBACK FOR A COMPLETE SAMPLE OF GALAXY GROUPS | XIS | Y |
| IC1262 | 263.2444 | 43.7719 | 69.53148075 | 32.08557503 | 39.6325 | 56784.7266319444 | 56784.9377777778 | 809103010 | 8569 | 10000 | 8569 | 8569 | 0 | 8569 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 8943 | 8943 | 18231.9 | 0 | PROCESSED | 57615.0791898148 | 57166 | 56800.6274537037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 092015 | Upcoming X-ray surveys like eROSITA, require precise calibration between X-ray observables (e.g. luminosity and temperature) and mass, down to the low mass regime to set tight constraints on the fundamental cosmological parameters. We propose to observe 19 galaxy groups with a total exposure time of 230 ks to complete observations for a flux limited sample. We will use this complete sample to study the scaling law properties of the low mass systems with a view to the eROSITA survey, which is expected to detect 100,000 objects, most of them in the low mass regime. Furthermore, we will investigate the relative importance of gravitational and non-gravitational processes by studying their thermodynamical properties beyond R500. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | LOVISARI | LORENZO | NULL | NULL | EUR | 9 | AO9 | SCALING PROPERTIES AND THE EFFECTS OF FEEDBACK FOR A COMPLETE SAMPLE OF GALAXY GROUPS | XIS | Y |
| ABELL 3341 | 81.3893 | -31.5876 | 235.16288585 | -31.086571 | 266.8997 | 57094.3290393518 | 57094.5780092593 | 809104010 | 11439 | 10000 | 11439 | 11439 | 0 | 11439 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.7607407407 | 57478 | 57108.4097685185 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 092015 | Upcoming X-ray surveys like eROSITA, require precise calibration between X-ray observables (e.g. luminosity and temperature) and mass, down to the low mass regime to set tight constraints on the fundamental cosmological parameters. We propose to observe 19 galaxy groups with a total exposure time of 230 ks to complete observations for a flux limited sample. We will use this complete sample to study the scaling law properties of the low mass systems with a view to the eROSITA survey, which is expected to detect 100,000 objects, most of them in the low mass regime. Furthermore, we will investigate the relative importance of gravitational and non-gravitational processes by studying their thermodynamical properties beyond R500. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | LOVISARI | LORENZO | NULL | NULL | EUR | 9 | AO9 | SCALING PROPERTIES AND THE EFFECTS OF FEEDBACK FOR A COMPLETE SAMPLE OF GALAXY GROUPS | XIS | Y |
| RBS1066 | 181.3063 | 39.3578 | 158.19944471 | 74.44309108 | 133.5252 | 56973.6795486111 | 56973.8890277778 | 809105010 | 10237.6 | 12000 | 10237.6 | 10525.6 | 0 | 10525.6 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7665509259 | 57358 | 56992.4200810185 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 092015 | Upcoming X-ray surveys like eROSITA, require precise calibration between X-ray observables (e.g. luminosity and temperature) and mass, down to the low mass regime to set tight constraints on the fundamental cosmological parameters. We propose to observe 19 galaxy groups with a total exposure time of 230 ks to complete observations for a flux limited sample. We will use this complete sample to study the scaling law properties of the low mass systems with a view to the eROSITA survey, which is expected to detect 100,000 objects, most of them in the low mass regime. Furthermore, we will investigate the relative importance of gravitational and non-gravitational processes by studying their thermodynamical properties beyond R500. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | LOVISARI | LORENZO | NULL | NULL | EUR | 9 | AO9 | SCALING PROPERTIES AND THE EFFECTS OF FEEDBACK FOR A COMPLETE SAMPLE OF GALAXY GROUPS | XIS | Y |
| ABELL 3733 | 315.4567 | -28.0341 | 17.77333082 | -39.60697798 | 260.2652 | 56981.8706481482 | 56982.1530439815 | 809108010 | 14588.4 | 15000 | 14596.4 | 14604.4 | 0 | 14588.4 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7988541667 | 57362 | 56996.4060300926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 092015 | Upcoming X-ray surveys like eROSITA, require precise calibration between X-ray observables (e.g. luminosity and temperature) and mass, down to the low mass regime to set tight constraints on the fundamental cosmological parameters. We propose to observe 19 galaxy groups with a total exposure time of 230 ks to complete observations for a flux limited sample. We will use this complete sample to study the scaling law properties of the low mass systems with a view to the eROSITA survey, which is expected to detect 100,000 objects, most of them in the low mass regime. Furthermore, we will investigate the relative importance of gravitational and non-gravitational processes by studying their thermodynamical properties beyond R500. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | LOVISARI | LORENZO | NULL | NULL | EUR | 9 | AO9 | SCALING PROPERTIES AND THE EFFECTS OF FEEDBACK FOR A COMPLETE SAMPLE OF GALAXY GROUPS | XIS | Y |
| NGC 7556 | 348.9407 | -2.3789 | 76.06549974 | -56.282291 | 247.7522 | 56983.6865972222 | 56984.009837963 | 809109010 | 15119 | 15000 | 15119 | 15119 | 0 | 15119 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.8029861111 | 57365 | 57009.4127777778 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 092015 | Upcoming X-ray surveys like eROSITA, require precise calibration between X-ray observables (e.g. luminosity and temperature) and mass, down to the low mass regime to set tight constraints on the fundamental cosmological parameters. We propose to observe 19 galaxy groups with a total exposure time of 230 ks to complete observations for a flux limited sample. We will use this complete sample to study the scaling law properties of the low mass systems with a view to the eROSITA survey, which is expected to detect 100,000 objects, most of them in the low mass regime. Furthermore, we will investigate the relative importance of gravitational and non-gravitational processes by studying their thermodynamical properties beyond R500. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | LOVISARI | LORENZO | NULL | NULL | EUR | 9 | AO9 | SCALING PROPERTIES AND THE EFFECTS OF FEEDBACK FOR A COMPLETE SAMPLE OF GALAXY GROUPS | XIS | Y |
| NGC4325 | 185.7751 | 10.6242 | 279.57257446 | 72.19853871 | 120.2615 | 56997.2271990741 | 56997.680775463 | 809110010 | 17468.1 | 15000 | 17476.1 | 17468.1 | 0 | 17476.1 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 16809.3 | 16809.3 | 39184 | 0 | PROCESSED | 57617.4727083333 | 57376 | 57010.1165162037 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 092015 | Upcoming X-ray surveys like eROSITA, require precise calibration between X-ray observables (e.g. luminosity and temperature) and mass, down to the low mass regime to set tight constraints on the fundamental cosmological parameters. We propose to observe 19 galaxy groups with a total exposure time of 230 ks to complete observations for a flux limited sample. We will use this complete sample to study the scaling law properties of the low mass systems with a view to the eROSITA survey, which is expected to detect 100,000 objects, most of them in the low mass regime. Furthermore, we will investigate the relative importance of gravitational and non-gravitational processes by studying their thermodynamical properties beyond R500. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | LOVISARI | LORENZO | NULL | NULL | EUR | 9 | AO9 | SCALING PROPERTIES AND THE EFFECTS OF FEEDBACK FOR A COMPLETE SAMPLE OF GALAXY GROUPS | XIS | Y |
| A3112 | 49.3536 | -44.4489 | 253.34827073 | -56.10640985 | 209.0009 | 57000.6762037037 | 57003.8439351852 | 809116010 | 107965.1 | 200000 | 107965.1 | 107965.1 | 0 | 107965.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 8148.7 | 8148.7 | 33907.9 | 1 | PROCESSED | 57617.53125 | 57387 | 57016.2346180556 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 094527 | The hot X-ray emitting gas in clusters of galaxies is a very large repository of metals produced by stars and galaxies. These metals enter the intra-cluster medium (ICM) via strong galactic winds, supernovae explosions, and ram-pressure stripping. However, the details of the mechanisms that transport metals to the ICM and the origin of these metals remain still unclear. We aim to accurately measure the temperature and abundance patterns of a bright nearby galaxy cluster A3112 out to the virial radius and compare these data with metal abundance yields produced by supernovae. Our proposed observation will provide information about how these metals are created, as well as how and when the metals were transported to the ICM. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | BULBUL | ESRA | SATO | KOSUKE | USJ | 9 | AO9 | A DETAILED STUDY OF CHEMICAL ENRICHMENT OF A3112 OUT TO THE VIRIAL RADIUS | XIS | Y |
| A3112 | 49.3542 | -44.4494 | 253.34888003 | -56.10584592 | 209.0003 | 57003.8439467593 | 57006.6182407407 | 809116020 | 97989 | 200000 | 97989 | 97989 | 0 | 97989 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57617.5061458333 | 57387 | 57017.4238425926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 094527 | The hot X-ray emitting gas in clusters of galaxies is a very large repository of metals produced by stars and galaxies. These metals enter the intra-cluster medium (ICM) via strong galactic winds, supernovae explosions, and ram-pressure stripping. However, the details of the mechanisms that transport metals to the ICM and the origin of these metals remain still unclear. We aim to accurately measure the temperature and abundance patterns of a bright nearby galaxy cluster A3112 out to the virial radius and compare these data with metal abundance yields produced by supernovae. Our proposed observation will provide information about how these metals are created, as well as how and when the metals were transported to the ICM. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | BULBUL | ESRA | NULL | NULL | USJ | 9 | AO9 | A DETAILED STUDY OF CHEMICAL ENRICHMENT OF A3112 OUT TO THE VIRIAL RADIUS | XIS | Y |
| ZWCL0008.8+5215 WEST | 2.7765 | 52.5416 | 116.7279282 | -9.84363991 | 63.9984 | 56847.5889351852 | 56849.9925115741 | 809117010 | 102373.6 | 100000 | 102381.6 | 102373.6 | 0 | 102389.6 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.3796643518 | 56748 | 56861.6478703704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 096003 | Radio relics in merging galaxy clusters trace low-Mach number shocks where particles are accelerated to extreme energies. Suzaku revealed temperature jumps at several relics. However the Mach numbers derived by X-ray observations are significantly lower than those from the radio spectra, and simple shock acceleration models need to be re-examined. We propose Suzaku key project observations of 12 radio relics to establish the shock properties, by combining with new radio data. These data will advance our understanding of (i) particle acceleration at the shocks and (ii) spatial distribution of the thermal and non-thermal components. We will make a breakthrough shocks and (ii) spatial distribution of the thermal and non-thermal components. We will make a breakthrough in our understand. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | AKAMATSU | HIROKI | NULL | NULL | EUR | 9 | AO9 | EXPLORING ENERGETICS AT THE LARGEST SHOCK STRUCTURES IN THE UNIVERSE | XIS | Y |
| ZWCL0008.8+5215 EAST | 3.1134 | 52.6387 | 116.94843434 | -9.77955026 | 65.9987 | 56844.7667939815 | 56847.5876273148 | 809118010 | 117847.3 | 120000 | 117847.3 | 119909.4 | 0 | 119933.4 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.3793518518 | 56748 | 56859.7336111111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 096003 | Radio relics in merging galaxy clusters trace low-Mach number shocks where particles are accelerated to extreme energies. Suzaku revealed temperature jumps at several relics. However the Mach numbers derived by X-ray observations are significantly lower than those from the radio spectra, and simple shock acceleration models need to be re-examined. We propose Suzaku key project observations of 12 radio relics to establish the shock properties, by combining with new radio data. These data will advance our understanding of (i) particle acceleration at the shocks and (ii) spatial distribution of the thermal and non-thermal components. We will make a breakthrough shocks and (ii) spatial distribution of the thermal and non-thermal components. We will make a breakthrough in our understand. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | AKAMATSU | HIROKI | NULL | NULL | EUR | 9 | AO9 | EXPLORING ENERGETICS AT THE LARGEST SHOCK STRUCTURES IN THE UNIVERSE | XIS | Y |
| ABELL2345EAST | 321.8675 | -12.1557 | 39.92441578 | -40.06382879 | 77.2002 | 56777.6418402778 | 56780.1466550926 | 809119010 | 101300.9 | 100000 | 101316.9 | 101300.9 | 0 | 101316.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 88088.5 | 88088.5 | 216380 | 1 | PROCESSED | 57615.0703935185 | 56748 | 56790.7271759259 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 096003 | Radio relics in merging galaxy clusters trace low-Mach number shocks where particles are accelerated to extreme energies. Suzaku revealed temperature jumps at several relics. However the Mach numbers derived by X-ray observations are significantly lower than those from the radio spectra, and simple shock acceleration models need to be re-examined. We propose Suzaku key project observations of 12 radio relics to establish the shock properties, by combining with new radio data. These data will advance our understanding of (i) particle acceleration at the shocks and (ii) spatial distribution of the thermal and non-thermal components. We will make a breakthrough shocks and (ii) spatial distribution of the thermal and non-thermal components. We will make a breakthrough in our understand. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | AKAMATSU | HIROKI | NULL | NULL | EUR | 9 | AO9 | EXPLORING ENERGETICS AT THE LARGEST SHOCK STRUCTURES IN THE UNIVERSE | XIS | Y |
| RXCJ1053.7+5453 | 163.1919 | 54.9274 | 152.52898808 | 54.84022784 | 128.7233 | 56962.235150463 | 56964.4029513889 | 809120010 | 87084.7 | 100000 | 87084.7 | 101552.9 | 0 | 101552.9 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.7267708333 | 56748 | 57071.4205671296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 096003 | Radio relics in merging galaxy clusters trace low-Mach number shocks where particles are accelerated to extreme energies. Suzaku revealed temperature jumps at several relics. However the Mach numbers derived by X-ray observations are significantly lower than those from the radio spectra, and simple shock acceleration models need to be re-examined. We propose Suzaku key project observations of 12 radio relics to establish the shock properties, by combining with new radio data. These data will advance our understanding of (i) particle acceleration at the shocks and (ii) spatial distribution of the thermal and non-thermal components. We will make a breakthrough shocks and (ii) spatial distribution of the thermal and non-thermal components. We will make a breakthrough in our understand. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | AKAMATSU | HIROKI | NULL | NULL | EUR | 9 | AO9 | EXPLORING ENERGETICS AT THE LARGEST SHOCK STRUCTURES IN THE UNIVERSE | XIS | Y |
| ABELL2255_RELIC | 258.3088 | 64.2709 | 94.17355304 | 34.84143708 | 3.193 | 56810.1311458333 | 56812.4147569444 | 809121010 | 100604.5 | 100000 | 100604.5 | 100812.5 | 0 | 100804.5 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57615.1987731482 | 56748 | 56867.7458217593 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 096003 | Radio relics in merging galaxy clusters trace low-Mach number shocks where particles are accelerated to extreme energies. Suzaku revealed temperature jumps at several relics. However the Mach numbers derived by X-ray observations are significantly lower than those from the radio spectra, and simple shock acceleration models need to be re-examined. We propose Suzaku key project observations of 12 radio relics to establish the shock properties, by combining with new radio data. These data will advance our understanding of (i) particle acceleration at the shocks and (ii) spatial distribution of the thermal and non-thermal components. We will make a breakthrough shocks and (ii) spatial distribution of the thermal and non-thermal components. We will make a breakthrough in our understand. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | A | AKAMATSU | HIROKI | NULL | NULL | EUR | 9 | AO9 | EXPLORING ENERGETICS AT THE LARGEST SHOCK STRUCTURES IN THE UNIVERSE | XIS | Y |
| M82 N1 | 148.6748 | 70.0409 | 141.10131259 | 40.27429686 | 283.7057 | 57159.0836921296 | 57160.4702546296 | 809122010 | 59505.5 | 60000 | 59505.5 | 59505.5 | 0 | 59513.5 | 1 | 1 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57618.6721759259 | 57538 | 57171.5244212963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 091701 | We propose to carry out joint Chandra and Suzaku observations of the starburst galaxy M82. We will search for extended clumps similar to the Northern Cap out to 45 kpc. We will also constrain the density and temperature profiles of the tenuous wind emission out to large radii. These data can place important constraints on theoretical models of starburst galaxies and their environments. We will test models such as the Chevalier & Clegg adiabatic wind model, hydrostatic halo model, shocked clouds in a wind, etc. The excellent Chandra spatial resolution combining with the low Suzaku background allows this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | S | WONG | KA-WAH | NULL | NULL | USA | 9 | AO9 | SEARCH FOR THE OUTER BOUNDARY OF THE STARBURST GALAXY: M82 | XIS | Y |
| M82 N2 | 148.2738 | 70.273 | 140.95732372 | 40.02876632 | 282.8972 | 57162.9827546296 | 57164.434224537 | 810043010 | 59808.4 | 60000 | 59808.4 | 61902.1 | 0 | 61902.1 | 2 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 34130 | 0 | PROCESSED | 57618.7218287037 | 57548 | 57177.3762847222 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 101442 | We propose to carry out Suzaku observations of the starburst galaxy M82. We will search for X-ray emission from winds and shock heated clouds out to its possible outer boundary of ~45 kpc. We will also constrain the density and temperature profiles of the gas/wind emission out to large radii. These data can place important constraints on theoretical models of starburst galaxies and their environments. We will test models such as the Chevalier & Clegg adiabatic wind model, shocked clouds in a wind, etc. The low Suzaku background allows this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | B | WONG | KA-WAH | NULL | NULL | USA | 10 | AO10 | SEARCH FOR THE OUTER BOUNDARY OF THE STARBURST GALAXY: M82 | XIS | Y |
| ANTLIA NW4 | 156.477 | -34.4731 | 271.69853818 | 19.42589093 | 299.2985 | 57168.4177546296 | 57169.4605902778 | 810066010 | 6359.6 | 40000 | 6359.6 | 6863.5 | 0 | 6863.5 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 6734.1 | 6734.1 | 78062.1 | 0 | PROCESSED | 57618.7963657407 | 57626 | 57178.2408101852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 101522 | We have measured hot gas properties of the nearest non-cool core cluster, Antlia, in the eastern direction out to R200. Our initial results suggest that its density profile is more consistent with some massive clusters, but significantly steeper than its cool core counterpart with a similar temperature (mass), Virgo. We propose to extend our program to observe two other directions to test azimuthal variation, which is likely to be significant. Physical properties such as density and temperature will be studied around the virial radius. These data can place important constraints on theoretical models of clusters and their environments. We will test models for clumping, electron-ion equipartition, and non-equilibrium ionization. The low Suzaku background allows this measurement. | EXTRAGALACTIC DIFFUSE SOURCES | 8 | C | WONG | KA-WAH | NULL | NULL | USA | 10 | AO10 | MAPPING THE NEAREST NON-COOL CORE CLUSTER OUT TO R200 | XIS | Y |
| GRB060105 | 297.6095 | 46.3384 | 80.2506255 | 9.98748628 | 191.1906 | 53740.5089351852 | 53741.5002083333 | 900001010 | 42220.8 | 40000 | 42220.8 | 42220.8 | 42220.8 | 42220.8 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 37718 | 37718 | 85641.9 | 2 | PROCESSED | 57532.6415856482 | 54247 | 54039.776712963 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 001008 | (i) Early break in lightcurve of X-ray afterglows using HXD. Recent Swift/XRT observations reveal that early X-ray afterglows of GRB has flat portion with very shallow decay. It may suggest continuous energy input from the central engine. The transition from its phase to general afterglow may display hard-to-soft evolution reflecting the cooling frequency. Thus multi wavelength observation will provide a key to the physics of central engine activity. (ii) Emission lines in the afterglows. The confirmation of line existence should be a matter of great importance because there remains unanswered questions. Some data may indicate a prominent iron line but others seem to suggest significant lower energy lines instead without iron lines. | EXTRAGALACTIC COMPACT SOURCES | 9 | A | MURAKAMI | TOSHIO | NULL | NULL | JAP | 0 | SWG-TOO | TOO OBSERVATIONS OF GAMMA-RAY BURSTS | HXD | N |
| GRB060904A | 237.7429 | 44.914 | 71.57699476 | 50.22047754 | 264.197 | 53982.4478935185 | 53983.2113888889 | 901001010 | 30336.3 | 30000 | 30344.3 | 30336.3 | 30344.3 | 30344.3 | 2 | 2 | 2 | 2 | 1 | 0 | 0 | 28347 | 28347 | 65966 | 0 | PROCESSED | 57535.45125 | 53982 | 54026.4650462963 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 017001 | N/A | EXTRAGALACTIC COMPACT SOURCES | 9 | A | SWG GRB TEAM | N/A | NULL | NULL | JAP | 1 | TOO | TOO OBSERVATION OF GRB060904A | HXD | N |
| CXOU J164710.2-455216 | 251.7964 | -45.87 | 339.54853507 | -0.43200811 | 286.2915 | 54001.2911689815 | 54002.205775463 | 901002010 | 38679.4 | 40000 | 38687.4 | 38695.4 | 38696.1 | 38679.4 | 1 | 1 | 1 | 1 | 1 | 0 | 0 | 35079.9 | 35079.9 | 79015.9 | 1 | PROCESSED | 57535.6726851852 | 54002 | 54026.4631134259 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 017002 | N/A | GALACTIC COMPACT OBJECT | 9 | A | SWG | NULL | NULL | NULL | JAP | 1 | TOO | TOO OBSERVATION OF CXOU J164710.2-455216 | XIS | N |
| IGR J17497-2821 | 267.404 | -28.4152 | 0.89934627 | -0.48041902 | 271.4056 | 54003.2926967593 | 54004.593275463 | 901003010 | 53317.8 | 60000 | 53333.8 | 53333.8 | 53333.8 | 53317.8 | 3 | 2 | 3 | 3 | 1 | 0 | 0 | 47947.6 | 47947.6 | 112359.9 | 1 | PROCESSED | 57535.7125925926 | 54004 | 54026.5016898148 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 017003 | N/A | GALACTIC COMPACT OBJECT | 9 | A | SWG | NULL | NULL | NULL | JAP | 1 | TOO | OBSERVATION OF IGR J17497-2821 | HXD | Y |
| XTE J1856+053 | 284.159 | 5.396 | 38.32644604 | 1.30563349 | 89.2928 | 54178.8141666667 | 54179.4321643518 | 901004010 | 24476 | 25000 | 24476 | 24476 | 0 | 24476 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 20110.8 | 20110.8 | 53391.9 | 0 | PROCESSED | 57537.7386805556 | 54171 | 54185.38 | 3.0.22.43 | 4 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 017020 | Observation for a outburst of XTE J1856+053 (ATEL #1024) | GALACTIC POINT SOURCES | 9 | A | SWG | NULL | NULL | NULL | JAP | 1 | TOO | TOO OBSERVATION OF XTE J1856+053 | HXD | Y |
| GRB070328 | 65.0965 | -34.1127 | 235.19366633 | -44.98909931 | 291.3415 | 54187.3163773148 | 54188.4585416667 | 901005010 | 52565.3 | 40000 | 52565.3 | 52565.3 | 0 | 52565.3 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 48242.8 | 48242.8 | 98681.9 | 2 | PROCESSED | 57538.0113888889 | 54187 | 54209.5955324074 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 017004 | TOO Observation of GRB 070328, REPORTED BY GCN 6224 | EXTRAGALACTIC COMPACT SOURCES | 9 | A | SUZAKU GRB TEAM | N/A | NULL | NULL | JAP | 1 | TOO | TOO OBSERVATION OF GRB 070328 | HXD | Y |
| NOVA VUL 2007 | 298.607 | 20.8689 | 58.62463604 | -3.62698433 | 252.0478 | 54408.3270023148 | 54408.8752777778 | 902001010 | 19586.9 | 20000 | 19586.9 | 19586.9 | 0 | 19586.9 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 17153 | 17153 | 47359.9 | 1 | PROCESSED | 57540.4186342593 | 54408 | 54418.4242361111 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 027001 | Observation for NOVA Vul | GALACTIC POINT SOURCES | 9 | A | SWG | NULL | NULL | NULL | JAP | 2 | TOO | TOO OBSERVATION OF NOVA VUL | XIS | Y |
| 3C454.3 | 343.4944 | 16.1419 | 86.11044475 | -38.19108399 | 249.0674 | 54439.2068865741 | 54440.1112731482 | 902002010 | 39889.5 | 40000 | 39889.5 | 39889.5 | 0 | 39889.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38041.2 | 38041.2 | 78131.9 | 1 | PROCESSED | 57540.8195023148 | 54431 | 54448.1589351852 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 027002 | We propose a 40 ksec Suzaku ToO observation of 3C 454.3, which is exhibiting ultra-high flaring activity in GeV gamma-ray band. 3C454.3 is a quasar hosted blazar (QHB) located at z =0.86. Daily monitoring of AGILE records E>100 MeV flux of 2x10^(-6) photons/cm^2/s or even greater. At present (Nov.23, 2007) flux is still increasing in both GeV and R-band, and this high state is expected to continue for typical flaring time scale of 1 month. Note this level of giant flare is recorded only 4-times through the entire life of EGRET onboard CGRO (3C279,1407-076,0528+134,1622-297). We propose to take a 40 ksec snapshot X-ray spectrum that is simultaneous with AGILE and world-wide ground-based radio-to-optical telescopes. | EXTRAGALACTIC COMPACT SOURCES | 9 | A | SWG | NULL | NULL | NULL | JAP | 2 | TOO | SUZAKU TOO OBSERVATION OF GIANT FLARE IN 3C454.3 TRIGGERED BY AGILE | XIS | Y |
| GRO J1008-57 | 152.4324 | -58.2988 | 282.99756699 | -1.83025918 | 104.6149 | 54434.481087963 | 54435.8023032407 | 902003010 | 47746 | 40000 | 47746 | 47765.4 | 0 | 47781.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 42370.1 | 42370.1 | 114146 | 1 | PROCESSED | 57540.795462963 | 54434 | 54441.1193171296 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 027003 | The cyclotron resonance is a direct method to know the surface magnetic field of X-ray binary pulsars. It was measured from a little more than ten X-ray pulsars. The flares of the Be transient pulsars are rare occasions that we can measure it. For this X-ray binary pulsar GRO J1008-57, Suzaku HXD GSO is the only useful detector. The inferred resonance energy of 90 keV will be the highest resonance energy. It locates at the higher end of the resonance energy distribution. Considering the span of the flares, this will be the first and the last chance for Suzaku to observe GRO J1008-57, and generally speaking, a feature at ~100keV. | GALACTIC POINT SOURCES | 9 | A | SWG | NULL | NULL | NULL | JAP | 2 | TOO | SUZAKU TOO PROPOSAL OF GRO J1008-57 | XIS | Y |
| V2491 CYGNI | 295.754 | 32.3324 | 67.23737764 | 4.36207752 | 79.2996 | 54575.6396990741 | 54576.0834953704 | 903001010 | 21115 | 20000 | 21139 | 21115 | 0 | 21139 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 19573.8 | 19573.8 | 38335.9 | 0 | PROCESSED | 57542.3459027778 | 54557 | 54587.0072569444 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 037001 | WE PROPOSE TO OBSERVE A CLASSICAL NOVA V2941 CYBNI REPORTED IN IAUC 8394. | GALACTIC POINT SOURCES | 9 | A | SWG | NULL | NULL | NULL | JAP | 3 | TOO | SUZAKU TOO OBSERVATION OF CLASSICAL NOVA V2941 CYGNI | XIS | Y |
| V2491 CYGNI | 295.7499 | 32.3313 | 67.23470516 | 4.36454955 | 64.0391 | 54595.360462963 | 54595.8960532407 | 903001020 | 25493.2 | 20000 | 25493.2 | 25493.2 | 0 | 25502 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 20388 | 20388 | 46263.9 | 0 | PROCESSED | 57542.4680902778 | 54557 | 54605.9972569445 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 037001 | WE PROPOSE TO OBSERVE A CLASSICAL NOVA V2941 CYBNI REPORTED IN IAUC 8394. | GALACTIC POINT SOURCES | 9 | A | SWG | NULL | NULL | NULL | JAP | 3 | TOO | SUZAKU TOO OBSERVATION OF CLASSICAL NOVA V2941 CYGNI | XIS | Y |
| SGR 0501+4516 | 75.2752 | 45.2826 | 161.54026234 | 1.95127535 | 91.8929 | 54704.0171527778 | 54705.3508564815 | 903002010 | 60105.2 | 40000 | 60105.2 | 60105.2 | 0 | 60105.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 54543.5 | 54543.5 | 115226 | 2 | PROCESSED | 57543.4292592593 | 54557 | 54780.5144791667 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 037002 | WE PROPOSE TO OBSERVE A NEW GAMMA-RAY REPEATER SGR 0501+4516. | GALACTIC POINT SOURCES | 9 | A | SWG | NULL | NULL | NULL | JAP | 3 | TOO | SUZAKU TOO OBSERVATION OF A NEW GAMMA-RAY REPEATER SGR 0501+4516 | XIS | Y |
| SAX J1808.4-3658 | 272.1154 | -37.0378 | 355.33274875 | -8.17628857 | 271.0151 | 54741.6891319444 | 54742.7502777778 | 903003010 | 42511.8 | 40000 | 42511.8 | 42511.8 | 0 | 42511.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34186.3 | 34186.3 | 91664 | 1 | PROCESSED | 57544.0368634259 | 54740 | 54780.6461921296 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 037003 | WE PROPOSE A TOO OBSERVATION OF AN OUTBURST OF AN ACCRETING MILLISECOND X-RAY PULSAR SAX J1808.4-3658 | GALACTIC POINT SOURCES | 9 | A | SWG | NULL | NULL | NULL | JAP | 3 | TOO | SUZAKU TOO OBSERVATION OF SAX J1808.4-3658 | HXD | Y |
| H 1743-322 | 266.567 | -32.2347 | 357.2549954 | -1.83500757 | 279.1655 | 54746.6801041667 | 54747.5404976852 | 903004010 | 31677.7 | 30000 | 31677.7 | 31677.7 | 0 | 31677.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 28708 | 28708 | 74331.9 | 2 | PROCESSED | 57544.0736226852 | 54740 | 54780.6318287037 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 037004 | WE PROPOSE A TOO OBSERVATION OF AN OUTBURST OF A BHC H1743-322 | GALACTIC POINT SOURCES | 9 | A | SWG | NULL | NULL | NULL | JAP | 3 | TOO | SUZAKU TOO OBSERVATION OF H 1743-322 | XIS | Y |
| V1647 ORI | 86.5523 | -0.1044 | 205.42860153 | -14.52056763 | 103.4312 | 54747.5550925926 | 54748.5939699074 | 903005010 | 40445.9 | 40000 | 40445.9 | 40453.9 | 0 | 40453.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35793.7 | 35793.7 | 89743.8 | 1 | PROCESSED | 57544.0905092593 | 54740 | 54780.6375231482 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 037005 | WE PROPOSE A TOO OBSERVATION OF AN OUTBURST OF A YSO V1647 ORI | GALACTIC POINT SOURCES | 9 | A | SWG | NULL | NULL | NULL | JAP | 3 | TOO | SUZAKU TOO OBSERVATION OF V1647 ORI | XIS | Y |
| 1E1547-5408 | 237.7125 | -54.2535 | 327.26441624 | -0.08549264 | 84.7106 | 54859.89875 | 54860.8973842593 | 903006010 | 42597 | 40000 | 42597 | 42709.2 | 0 | 42661.2 | 1 | 1 | 0 | 2 | 1 | 0 | 0 | 33477.4 | 33477.4 | 86267.8 | 1 | PROCESSED | 57545.414537037 | 54857 | 54880.5653009259 | 3.0.22.43 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 037006 | WE PROPOSE A TOO OBSERVATION OF AN OUTBURST OF AN AXP 1E1547-5408 | GALACTIC POINT SOURCES | 9 | A | SWG | NULL | NULL | NULL | JAP | 3 | TOO | SUZAKU TOO OBSERVATION OF 1E1547-5408 | HXD | Y |
| GRB 090709A | 289.7685 | 60.7348 | 91.79137258 | 20.20918409 | 7.97 | 55021.552974537 | 55022.8975 | 904001010 | 61874.1 | 40000 | 61874.1 | 62146.1 | 0 | 62146.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 58221.6 | 58221.6 | 116156 | 0 | PROCESSED | 57547.8308796296 | 54922 | 55036.0450462963 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 047001 | WE PROPOSE TO OBSERVE GRB090709A | EXTRAGALACTIC POINT SOURCES | 9 | A | SWG | NULL | NULL | NULL | JAP | 4 | TOO | SUZAKU TOO OBSERVATION OF GRB090709A | HXD | Y |
| V2672 OPH | 264.5843 | -26.7394 | 1.0178963 | 2.52622489 | 269.0005 | 55071.5142476852 | 55072.0002777778 | 904002010 | 23133.6 | 20000 | 23141.6 | 23141.6 | 0 | 23133.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 21852.7 | 21852.7 | 41984 | 0 | PROCESSED | 57548.37125 | 55071 | 55109.4163541667 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 047002 | WE PROPOSE TO OBSERVE NOVA OPH 2009. | GALACTIC POINT SOURCES | 9 | A | SWG | NULL | NULL | NULL | JAP | 4 | TOO | SUZAKU TOO OBSERVATION OF NOVA OPH 2009 | XIS | Y |
| V2672 OPH | 264.5839 | -26.74 | 1.01719756 | 2.52620709 | 269 | 55080.8184259259 | 55081.479375 | 904002020 | 25099.8 | 20000 | 25115.8 | 25099.8 | 0 | 25115.8 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 18846.3 | 18846.3 | 57099.9 | 1 | PROCESSED | 57548.4140740741 | 55071 | 55092.1389699074 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 047002 | WE PROPOSE TO OBSERVE NOVA OPH 2009. | GALACTIC POINT SOURCES | 9 | A | SWG | NULL | NULL | NULL | JAP | 4 | TOO | SUZAKU TOO OBSERVATION OF NOVA OPH 2009 | XIS | Y |
| 3C 454.3 | 343.5181 | 16.0882 | 86.09659145 | -38.24838712 | 247.431 | 55174.1116087963 | 55174.9801388889 | 904003010 | 40477.2 | 40000 | 40485.2 | 40485.2 | 0 | 40477.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 33149.8 | 33149.8 | 75021.8 | 0 | PROCESSED | 57549.7589351852 | 55172 | 55195.4345833333 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 047003 | NULL | EXTRAGALACTIC COMPACT SOURCES | 9 | A | SWG | NULL | NULL | NULL | JAP | 4 | TOO | SUZAKU TOO OBSERVATION OF UNPRECEDENTED GEV FLARE IN 3C454.3 TRIGGERED BY FERMI | HXD | Y |
| X0331+53 | 53.7787 | 53.1056 | 146.10568234 | -2.23871929 | 257.9878 | 55243.264537037 | 55243.7141087963 | 904004010 | 31452.2 | 20000 | 32188.2 | 32182.5 | 0 | 31452.2 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 22673.3 | 22673.3 | 38831.9 | 0 | PROCESSED | 57550.5986342593 | 55243 | 55253.2754398148 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 047004 | NULL | GALACTIC POINT SOURCES | 9 | A | SWG | NULL | NULL | NULL | JAP | 4 | TOO | SUZAKU TOO OBSERVATION OF X0331+53 | HXD | Y |
| XTE J1752-223 | 268.0589 | -22.2786 | 6.47621976 | 2.14981725 | 88.2297 | 55251.2069444444 | 55252.1856944444 | 904005010 | 41291 | 40000 | 41312.3 | 41291 | 0 | 41312.3 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 29227.2 | 29227.2 | 84540 | 1 | PROCESSED | 57550.7198032407 | 55250 | 55264.3570601852 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 047005 | NULL | GALACTIC POINT SOURCES | 9 | A | SWG | NULL | NULL | NULL | JAP | 4 | TOO | SUZAKU TOO OBSERVATION OF XTE J1752-223 | HXD | Y |
| SGR 1833-0832 | 278.4476 | -8.4549 | 23.40264755 | 0.03869006 | 103.0954 | 55282.3774537037 | 55283.4841666667 | 904006010 | 42341.4 | 40000 | 42341.4 | 42381.6 | 0 | 42373.6 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 10768.9 | 10768.9 | 95603.8 | 0 | PROCESSED | 57551.0356018518 | 55278 | 55301.3363773148 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 047006 | NULL | GALACTIC POINT SOURCES | 9 | A | SWG | NULL | NULL | NULL | JAP | 4 | TOO | SUZAKU TOO OBSERVATION OF SGR 1833-832 | HXD | Y |
| V407 CYG | 315.5407 | 45.7909 | 86.99380151 | -0.47192729 | 99.0556 | 55295.8967708333 | 55296.812662037 | 905001010 | 42196.7 | 40000 | 42196.7 | 42196.7 | 0 | 42196.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 35195.8 | 35195.8 | 79113.9 | 1 | PROCESSED | 57551.1952199074 | 55287 | 55309.3796643518 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 057001 | NULL | GALACTIC POINT SOURCES | 9 | A | SWG | NULL | NULL | NULL | JAP | 5 | TOO | SUZAKU TOO OBSERVATION OF V407 CYG | XIS | Y |
| GX 304-1 | 195.2392 | -61.6525 | 304.06184706 | 1.19836327 | 310.0255 | 55421.6797337963 | 55421.9584722222 | 905002010 | 5104.5 | 20000 | 5125 | 5104.5 | 0 | 5124.5 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 12874.7 | 12874.7 | 24071.9 | 0 | PROCESSED | 57553.0697800926 | 55287 | 55435.189537037 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 057002 | MAXI TRRIGERED TOO, TO SURVEY CYCLOTRON RESONANCE FEATURE AT 60-90 KEV. | GALACTIC POINT SOURCES | 9 | A | SWG | NULL | NULL | NULL | JAP | 5 | TOO | SUZAKU TOO OBSERVATION OF GX304-1 | HXD | Y |
| MAXI J1659-152 | 254.7552 | -15.3386 | 5.44552714 | 16.48124356 | 273.2778 | 55468.2441319444 | 55468.6925925926 | 905003010 | 18131.6 | 20000 | 18131.6 | 18368.9 | 0 | 18131.6 | 3 | 1 | 0 | 2 | 1 | 0 | 0 | 16310.7 | 16310.7 | 38745.9 | 1 | PROCESSED | 57553.5869212963 | 55287 | 55483.5344328704 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 057003 | MAXI TRRIGERED TOO FOR MAXJ J1659-152 | GALACTIC POINT SOURCES | 9 | A | SWG | NULL | NULL | NULL | JAP | 5 | TOO | SUZAKU TOO OBSERVATION OF MAXI J1659-152 | HXD | Y |
| MAXI J1659-152 | 254.7478 | -15.3578 | 5.42486205 | 16.47605908 | 273.1379 | 55469.2336805556 | 55469.9794212963 | 905004010 | 14947.2 | 20000 | 15016.5 | 18262.5 | 0 | 14947.2 | 2 | 1 | 0 | 2 | 1 | 0 | 0 | 23509.9 | 23509.9 | 64415.8 | 0 | PROCESSED | 57553.626712963 | 55287 | 55483.5420023148 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 057003 | MAXI TRRIGERED TOO FOR MAXJ J1659-152 | GALACTIC POINT SOURCES | 9 | A | SWG | NULL | NULL | NULL | JAP | 5 | TOO | SUZAKU TOO OBSERVATION OF MAXI J1659-152 | HXD | Y |
| MAXI J1659-152 | 254.7575 | -15.3514 | 5.43592755 | 16.4720773 | 272.9914 | 55470.3714930556 | 55471.2801157407 | 905005010 | 4880.8 | 20000 | 4924.5 | 4880.8 | 0 | 4909.1 | 3 | 1 | 0 | 2 | 1 | 0 | 0 | 30666.9 | 30666.9 | 67620.9 | 1 | PROCESSED | 57553.626875 | 55287 | 55483.5484143518 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 057003 | MAXI TRRIGERED TOO FOR MAXJ J1659-152 | GALACTIC POINT SOURCES | 9 | A | SWG | NULL | NULL | NULL | JAP | 5 | TOO | SUZAKU TOO OBSERVATION OF MAXI J1659-152 | HXD | Y |
| CYG X-1 | 299.6054 | 35.1955 | 71.33620274 | 3.05313329 | 215.1197 | 55546.9562268518 | 55547.7842824074 | 905006010 | 461.2 | 40000 | 5495.2 | 461.2 | 0 | 5476.8 | 1 | 1 | 0 | 1 | 1 | 0 | 0 | 35496.1 | 35496.1 | 71537.9 | 1 | PROCESSED | 57554.4516087963 | 55287 | 55593.1461805556 | 3.0.22.43 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 057004 | MAXI TRRIGERED TOO FOR CYG X-1 | GALACTIC POINT SOURCES | 9 | A | SWG | NULL | NULL | NULL | JAP | 5 | TOO | SUZAKU TOO OBSERVATION OF CYG X-1 | XIS | Y |
| PSR B1259-63 | 195.695 | -63.834 | 304.18208178 | -0.98978615 | 116.7512 | 55585.6366087963 | 55586.7084490741 | 905007010 | 40296.5 | 40000 | 40312.5 | 40296.5 | 0 | 40312.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 46881.9 | 46881.9 | 92589.8 | 2 | PROCESSED | 57600.7364467593 | 55287 | 55599.2215046296 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 057005 | TOO FOR PSR B1259-63 | GALACTIC POINT SOURCES | 9 | A | SWG | NULL | NULL | NULL | JAP | 5 | TOO | SUZAKU TOO OBSERVATION OF PSR B1259-63 | XIS | Y |
| PSR B1259-63 BG | 195.4936 | -63.9722 | 304.08768216 | -1.12409855 | 117.786 | 55586.7093402778 | 55587.0836111111 | 905007020 | 10129.9 | 10000 | 10129.9 | 10129.9 | 0 | 10129.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 15475.5 | 15475.5 | 32306 | 0 | PROCESSED | 57600.7438773148 | 55287 | 55609.0653356482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 057005 | TOO FOR PSR B1259-63 | GALACTIC POINT SOURCES | 9 | A | SWG | NULL | NULL | NULL | JAP | 5 | TOO | SUZAKU TOO OBSERVATION OF PSR B1259-63 | XIS | Y |
| J164449.3+573451 | 251.1787 | 57.6052 | 86.74307158 | 39.45238362 | 57.9841 | 55657.1004976852 | 55658.0224189815 | 906001010 | 38317.4 | 40000 | 38317.4 | 38317.4 | 0 | 38317.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39171.8 | 39171.8 | 79639.8 | 1 | PROCESSED | 57601.4020601852 | 55652 | 55680.8027199074 | 3.0.22.44 | 3 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 067001 | TOO FOR J164449.3+573451 | GALACTIC POINT SOURCES | 9 | A | SWG | NULL | NULL | NULL | JAP | 6 | TOO | SUZAKU TOO OBSERVATION OF SWIFT J164449.3+573451 | XIS | Y |
| SWIFT J1822.3-1606 | 275.5777 | -16.1399 | 15.29578033 | -1.05412412 | 269.7491 | 55817.4160532407 | 55818.4231712963 | 906002010 | 40688.3 | 40000 | 40710.2 | 40688.3 | 0 | 40688.3 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 36153.5 | 36153.5 | 86997.8 | 0 | PROCESSED | 57603.1544791667 | 55652 | 55851.4582060185 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 067002 | TOO FOR J1822.3-1606 | GALACTIC POINT SOURCES | 9 | A | SWG | NULL | NULL | NULL | JAP | 6 | TOO | SUZAKU TOO OBSERVATION OF SWIFT J1822.3-1606 | HXD | Y |
| MAXI J 1836-194 | 278.9329 | -19.331 | 13.93624891 | -5.36115055 | 267.6561 | 55818.4252662037 | 55819.4515509259 | 906003010 | 10687.7 | 40000 | 10687.7 | 10687.7 | 0 | 10687.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38132.1 | 38132.1 | 88655.9 | 1 | PROCESSED | 57603.1781597222 | 55652 | 55851.4491550926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 067003 | TOO FOR MAXI J 1836-194 | GALACTIC POINT SOURCES | 9 | A | SUZAKU/MAXI TEAM | N/A | NULL | NULL | JAP | 6 | TOO | SUZAKU TOO OBSERVATION OF MAXI J 1836-194 | XIS | Y |
| M81 | 148.9169 | 69.0743 | 142.07426799 | 40.9032395 | 154.1516 | 55819.4638773148 | 55820.4543634259 | 906004010 | 45675.9 | 45000 | 45917.9 | 45675.9 | 0 | 45917.9 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 44736.5 | 44736.5 | 85561.8 | 0 | PROCESSED | 57603.1615509259 | 55652 | 55865.2169212963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 067004 | TOO FOR M81 | EXTRAGALACTIC COMPACT SOURCES | 9 | A | SWG | NULL | NULL | NULL | JAP | 6 | TOO | FOLLOW UP WITH SUZAKU TO M81 15 GHZ FLARE | XIS | Y |
| T PYX | 136.1688 | -32.3772 | 257.20280397 | 9.70584313 | 98.5003 | 55859.5926388889 | 55860.6926041667 | 906005010 | 38586.2 | 40000 | 38588.1 | 38588.1 | 0 | 38586.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34232.3 | 34232.3 | 95029.9 | 2 | PROCESSED | 57603.6166550926 | 55652 | 55874.0433217593 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 067005 | TOO FOR T PYX | GALACTIC COMPACT OBJECT | 9 | A | SWG | NULL | NULL | NULL | JAP | 6 | TOO | TOO OBSERVATION OF A RECURRENT NOVA T PYX | XIS | Y |
| NGC 4151 | 182.6443 | 39.4154 | 155.03407583 | 75.0595692 | 131.5185 | 55882.6359606482 | 55883.9793055556 | 906006010 | 61664.6 | 60000 | 61664.6 | 61664.6 | 0 | 61664.6 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 59013.8 | 59013.8 | 116049.8 | 0 | PROCESSED | 57603.8274074074 | 55652 | 55895.1682638889 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 067006 | TOO FOR NGC 4151 | EXTRAGALACTIC COMPACT SOURCES | 9 | A | SWG | NULL | NULL | NULL | JAP | 6 | TOO | TOO OBSERVATION OF NGC 4151 | XIS | Y |
| NGC 4151 | 182.6422 | 39.4254 | 155.0153158 | 75.05066834 | 112.4213 | 55913.6264814815 | 55915.0467708333 | 906006020 | 60596.5 | 60000 | 60596.5 | 60596.5 | 0 | 60596.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 50695.3 | 50695.3 | 122695.8 | 0 | PROCESSED | 57604.1906944444 | 55652 | 55970.2466203704 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 067006 | TOO FOR NGC 4151 | EXTRAGALACTIC COMPACT SOURCES | 9 | A | SWG | NULL | NULL | NULL | JAP | 6 | TOO | TOO OBSERVATION OF NGC 4151 | XIS | Y |
| RT CRU | 188.717 | -64.5661 | 301.15328171 | -1.75159028 | 124.9936 | 55963.7621064815 | 55964.8335763889 | 906007010 | 39428.4 | 40000 | 39428.4 | 39428.4 | 0 | 39428.4 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 34657.5 | 34657.5 | 92561.8 | 1 | PROCESSED | 57604.5932291667 | 55652 | 56016.6693865741 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 067007 | TOO FOR RT CRU | GALACTIC COMPACT OBJECT | 9 | A | SWG | NULL | NULL | NULL | JAP | 6 | TOO | TOO OBSERVATION OF A SYMBIOTIC STAR RT CRU | XIS | Y |
| 4U 1630-47 | 248.5051 | -47.3855 | 336.9160416 | 0.25611882 | 88.0013 | 55970.8879050926 | 55971.7356134259 | 906008010 | 7712.6 | 30000 | 7790.5 | 7712.6 | 0 | 7790.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 27940.3 | 27940.3 | 73239.9 | 0 | PROCESSED | 57604.6234490741 | 55652 | 55985.1625462963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 067008 | TOO FOR 4U1630-47 | GALACTIC COMPACT OBJECT | 9 | A | SWG | NULL | NULL | NULL | JAP | 6 | TOO | TOO OBSERVATION OF 4U 1630-47 | XIS | Y |
| MAXI J 1305-704 | 196.7435 | -70.4445 | 304.24264532 | -7.61230009 | 289.6357 | 56128.7572800926 | 56130.021099537 | 907001010 | 41909.7 | 40000 | 41909.7 | 41933.7 | 0 | 41917.7 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 39977.6 | 39977.6 | 109181.7 | 2 | PROCESSED | 57606.6770138889 | 56018 | 56146.1252777778 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 077001 | TOO FOR MAXI J 1305-704 | GALACTIC POINT SOURCES | 9 | A | SUZAKU/MAXI TEAM | N/A | NULL | NULL | JAP | 7 | TOO | SUZAKU TOO OBSERVATION OF MAXI J 1305-704 | XIS | Y |
| NOVA MON 2012 | 99.9089 | 5.8978 | 206.3399685 | 0.07362696 | 91.6997 | 56195.0768518518 | 56196.2278472222 | 907002010 | 46870.2 | 40000 | 46878.2 | 46886.2 | 0 | 46870.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 38818.5 | 38818.5 | 99427.8 | 1 | PROCESSED | 57607.2000694445 | 56018 | 56323.5232986111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 077002 | TOO FOR NOVA MON 2012 | GALACTIC COMPACT OBJECT | 9 | A | SWG | NULL | NULL | NULL | JAP | 7 | TOO | TOO OBSERVATION OF NOVA MON 2012 | XIS | Y |
| 4U 1630-47 | 248.5119 | -47.3916 | 336.9146822 | 0.2485984 | 290.4332 | 56202.017349537 | 56202.86 | 907003010 | 533.4 | 40000 | 2879.3 | 2879.4 | 0 | 533.4 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 39489.1 | 39489.1 | 72799.9 | 0 | PROCESSED | 57607.2690509259 | 56018 | 56226.6735300926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 077003 | TOO FOR 4U 1630-47 | GALACTIC COMPACT OBJECT | 9 | A | SWG | NULL | NULL | NULL | JAP | 7 | TOO | TOO OBSERVATION OF NOVA MON 2012 | XIS | Y |
| Swift J174510-262411 | 266.2968 | -26.405 | 2.11032862 | 1.40121804 | 268.6775 | 56211.5891087963 | 56212.4015509259 | 907004010 | 425.9 | 30000 | 2301.3 | 2301.8 | 0 | 425.9 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 32217 | 32217 | 70187.9 | 3 | PROCESSED | 57607.7432291667 | 56018 | 56232.5389351852 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 077004 | TOO FOR SWIFT J174510.8-262411 | GALACTIC COMPACT OBJECT | 9 | A | SWG | NULL | NULL | NULL | JAP | 7 | TOO | TOO OBSERVATION OF SWIFT J174510.8-262411 | XIS | Y |
| 4U 1954+319 | 298.9324 | 32.0855 | 68.38478458 | 1.91662885 | 255.7666 | 56232.1109837963 | 56233.5016087963 | 907005010 | 60828.2 | 60000 | 60836.2 | 60828.2 | 0 | 60836.2 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 53911 | 53911 | 120137.8 | 1 | PROCESSED | 57607.9528125 | 56018 | 56245.5032175926 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 077005 | TOO FOR 4U 1954+319 | GALACTIC COMPACT OBJECT | 9 | A | SWG | NULL | NULL | NULL | JAP | 7 | TOO | TOO OBSERVATION OF 4U 1954+319 | XIS | Y |
| GRO J1008-57 | 152.4258 | -58.3025 | 282.99687194 | -1.8352826 | 95.6263 | 56251.6142476852 | 56253.2231365741 | 907006010 | 9030.1 | 60000 | 9060.6 | 9030.1 | 0 | 9030.1 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 53478.5 | 53478.5 | 138989.8 | 0 | PROCESSED | 57608.1244444444 | 56018 | 56275.5913773148 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 077006 | TOO FOR GRO J1008057 | GALACTIC COMPACT OBJECT | 9 | A | SWG | NULL | NULL | NULL | JAP | 7 | TOO | TOO OBSERVATION OF GRO J1008-57 | XIS | Y |
| KS 1947+300 | 297.404 | 30.1954 | 66.09009729 | 2.0722008 | 260.7614 | 56587.2172685185 | 56587.9377546296 | 908001010 | 28997.2 | 30000 | 28997.2 | 29005 | 0 | 29011 | 3 | 3 | 0 | 3 | 1 | 0 | 0 | 29506.9 | 29506.9 | 62243.9 | 0 | PROCESSED | 57613.0578240741 | 56383 | 56601.6225462963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 087001 | TOO FOR KS 1947+300 | GALACTIC COMPACT OBJECT | 9 | A | SWG | NULL | NULL | NULL | JAP | 8 | TOO | TOO OBSERVATION OF KS 1947+300 | XIS | Y |
| KS 1947+300 | 297.4027 | 30.2054 | 66.09815344 | 2.07823784 | 229.248 | 56618.6106944444 | 56619.4287152778 | 908001020 | 7639.8 | 30000 | 7715 | 7639.8 | 0 | 7715.5 | 2 | 2 | 0 | 2 | 1 | 0 | 0 | 31861.4 | 31861.4 | 70669.9 | 2 | PROCESSED | 57613.3854050926 | 56383 | 56663.5779861111 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 087001 | TOO FOR KS 1947+300 | GALACTIC COMPACT OBJECT | 9 | A | SWG | NULL | NULL | NULL | JAP | 8 | TOO | TOO OBSERVATION OF KS 1947+300 | XIS | Y |
| MAXI J1828-249 | 277.2439 | -25.0316 | 8.11397411 | -6.54746759 | 267.8065 | 56586.2141435185 | 56587.2084606482 | 908002010 | 2569.7 | 40000 | 2620.9 | 2569.7 | 0 | 2670.6 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 33752.7 | 33752.7 | 85897.8 | 1 | PROCESSED | 57613.0608564815 | 56383 | 56644.5925462963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 087002 | TOO FOR MAXI J1828-249 | GALACTIC COMPACT OBJECT | 9 | A | SWG | NULL | NULL | NULL | JAP | 8 | TOO | TOO OBSERVATION OF MAXI J1828-249 | XIS | Y |
| MAXI J1421-613 | 215.3958 | -61.6121 | 313.4316269 | -0.5917999 | 105.0013 | 56688.5143518518 | 56691.5835300926 | 908003010 | 47202 | 40000 | 48786 | 47202 | 0 | 48834 | 3 | 2 | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57613.7880671296 | 56383 | 56726.6097337963 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 087003 | TOO FOR MAXI J1421-613 | GALACTIC COMPACT OBJECT | 9 | A | SWG | NULL | NULL | NULL | JAP | 8 | TOO | TOO OBSERVATION OF MAXI J1828-249 | XIS | Y |
| GRO J1744-28 | 266.1354 | -28.739 | 0.04490036 | 0.30435827 | 106.5003 | 56740.1835300926 | 56741.9688888889 | 908004010 | 4134.8 | 60000 | 4290 | 4134.8 | 0 | 4290 | 3 | 2 | 0 | 3 | 1 | 0 | 0 | 55441.7 | 55441.7 | 154225.7 | 1 | PROCESSED | 57614.1493402778 | 56383 | 56754.771875 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 087004 | TOO FOR GRO J1744-28 | GALACTIC COMPACT OBJECT | 9 | A | SWG | NULL | NULL | NULL | JAP | 8 | TOO | TOO OBSERVATION OF GRO J1744-28 | XIS | Y |
| SN 2014J | 148.9097 | 69.6625 | 141.44352166 | 40.56039664 | 303.2002 | 56746.5128009259 | 56750.7244560185 | 908005010 | 205780.2 | 100000 | 205788.2 | 205780.2 | 0 | 205788.2 | 3 | 2 | 0 | 2 | 1 | 0 | 0 | 205928.8 | 205928.8 | 355358 | 1 | PROCESSED | 57614.2687615741 | 56383 | 56821.9350231482 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 087005 | TOO FOR SN2014J | GALACTIC COMPACT OBJECT | 9 | A | SWG | NULL | NULL | NULL | JAP | 8 | TOO | TOO OBSERVATION OF SN2014J | XIS | Y |
| CEP X-4 | 324.8564 | 56.9938 | 99.00846722 | 3.32594824 | 40.5604 | 56839.2088888889 | 56840.5835069445 | 909001010 | 85 | 60000 | 85 | 85 | 0 | 60416.9 | 2 | 2 | 0 | 3 | 1 | 0 | 0 | 80570.1 | 80570.1 | 115385.9 | 1 | PROCESSED | 57615.3696180556 | 56748 | 56854.6169097222 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 097001 | TOO FOR CEP X-4 | GALACTIC COMPACT OBJECT | 9 | A | SWG | NULL | NULL | NULL | JAP | 9 | TOO | TOO OBSERVATION OF CEP X-4 | XIS | Y |
| IGR J17451-3022 | 266.2833 | -30.3797 | 358.71308213 | -0.66247404 | 266.8863 | 56923.3688541667 | 56924.2918287037 | 909002010 | 33872 | 35000 | 33884.4 | 33884.4 | 0 | 33872 | 2 | 2 | 0 | 1 | 0 | 0 | 0 | 0 | 0 | 0 | 0 | PROCESSED | 57616.5792361111 | 56748 | 56940.6741898148 | 3.0.22.44 | 2 | Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 | 097002 | TOO FOR IGR J17451-3022 | GALACTIC COMPACT OBJECT | 9 | A | SWG | NULL | NULL | NULL | JAP | 9 | TOO | TOO OBSERVATION OF IGR J17451-3022 | XIS | Y |