Suzaku Observation : 402071010
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Fits Header
TELESCOP= 'SUZAKU ' / Telescope (mission) name
OBS_ID = '402071010' / Observation identification string
OBSERVER= 'JON MILLER' / Principal Investigator
OBJECT = 'GRS 1915+105' / Name of observed object
OBS_REM = ' ' / remark on observation
RA_OBJ = 288.7983 / planned target R.A.(deg)
DEC_OBJ = 10.9456 / planned target DEC.(deg)
RA_NOM = 2.887933000000000E+02 / Right Ascension of target (deci. deg)
DEC_NOM = 1.095350000000000E+01 / Declination of target (deci. deg)
PA_NOM = 67.3540 / nominal position angle from north to DETY(deg)
MEAN_EA1= 288.793268524694 / mean of the 1st ZYZ-Euler angle (deg)
MEAN_EA2= 79.046464293841 / mean of the 2nd ZYZ-Euler angle (deg)
MEAN_EA3= 22.646008614276 / mean of the 3rd ZYZ-Euler angle (deg)
DATE-OBS= '2007-05-07T14:40:22' / Start date of observations
DATE-END= '2007-05-09T01:43:19' / End date of observations
TSTART = 2.318642539618631E+08 / time start
TSTOP = 2.319883060000000E+08 / time stop
TELAPSE = 1.240520381368697E+05 / elapsed time
ONTIME = 3.267076992917061E+04 / On-source time
EXPOSURE= 3.267076992917061E+04 / Exposure time
MJD-OBS = 5.422761479335489E+04 / MJD of data start time
FILIN001= 'ae402071010xi1_0_3x3b094b_cl.evt.gz' / Input file name
SEQPNUM = 3 / Number of times this dataset processed
PROCVER = '3.0.22.43' / Processing script version
MK1STVER= 'mk1stfits20120530' / Version of mk1stfits used
SOFTVER = 'Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22' / Version of HEADAS used
CALDBVER= 'hxd20110913_xis20151005_xrt20110630_xrs20060410' / Version of CALDB u
FILIN002= 'ae402071010xi1_0_5x5b094b_cl.evt.gz' / Input file name
COMMENT -------------------------
COMMENT BITPIX compressed from 32 to 8.
COMMENT Pixel values greater than 255 was set to 255.
COMMENT This file was made for JUDO-Suzaku.
COMMENT -------------------------
COMMENT FITS (Flexible Image Transport System) format is defined in 'Astronomy
Abstract:
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.