SS_CYGNI
SS Cygni is one of the prototypical dwarf novae, which shows transitions between an optically quiescent state and an outburst state. In the outburst state, hard X-ray emission is thought to arise from coronae over an accretion disc, but their location is unclear. We will understand the corona geometry by measuring profiles of the coronal emission lines with the Resolve. In the quiescent state, on the other hand, it is commonly understood that the hard X-ray emission emanates from the optically thin boundary layer, yet its heating mechanism and radial profile of the BL plasma are both poorly understood. We will try to make them clear by means of spectroscopy of the emission lines from the plasma and the fluorescent iron K-alpha emission line with the Resolve.
obsid = 300042010 / Unique Observation/Sequence Number
object = SS_CYGNI / Object name
pi_name = Collaboration XRISM / Proposal Principal Investigator Name
ra = 325.678044313503 / Right Ascension (Pointing Position) (deg)
dec = 43.5857375035493 / Declination (Pointing Position) (deg)
roll_angle = 60.4387760821783 / Roll Angle (deg)
start_time = 2024-06-04T10:38:04 / Start Time of the Observation
stop_time = 2024-06-09T00:17:04 / Stop Time of the Observation
exposure = 281346.2234303 / Effective Total Observation Exposure (s)
public_date= 2025-08-31 / Public Date