CYGNUS_A
The core region of Cygnus A hosts a remarkably powerful, high-Mach number cocoon shock with an energy up to 10^61 erg. This is clearly a very dynamical example of interaction between the central SMBH and the surrounding gas that should leave unique imprints on the velocity of the ICM. Owing to the high X-ray temperature and brightness of this source, a relatively short 45 ks XRISM observation is sufficient to provide a wealth of velocity diagnostics, including line shifts, widths, shapes, and line strengths which will constrain the resonant scattering effect. These complementary probes of the gas kinematics, sensitive to motions on different scales and their anisotropy, will allow us to study both the small-scale turbulence, and the large-scale motions due to the cocoon shock's expansion.
obsid = 201120010 / Unique Observation/Sequence Number
object = CYGNUS_A / Object name
pi_name = MAJUMDER ANWESH / Proposal Principal Investigator Name
ra = 299.866945238504 / Right Ascension (Pointing Position) (deg)
dec = 40.7336880725884 / Declination (Pointing Position) (deg)
roll_angle = 275.391151825496 / Roll Angle (deg)
start_time = 2024-10-06T22:19:04 / Start Time of the Observation
stop_time = 2024-10-10T00:41:04 / Stop Time of the Observation
exposure = 179372.47819819 / Effective Total Observation Exposure (s)
public_date= 2025-10-19 / Public Date