EX_HYA
The mass of white dwarfs (WDs) within binary systems is a crucial parameter for understanding their evolution into type-Ia supernovae. Among WD binary systems, we focus on the X-ray luminous object, the intermediate polars (IPs) for XRISM observations. The measurement of gravitational redshifts and the bulk Doppler shifts of atomic lines have proven to be robust tools for mass determination, as demonstrated by Hayashi et al.(2023) with Chandra HETG data. We propose a 75 ksec XRISM observation of the IP system EX Hya, to which we already applied the method for lighter elements, to ascertain the WD mass with 10% accuracy with Fe-K lines.
obsid = 201058010 / Unique Observation/Sequence Number
object = EX_HYA / Object name
pi_name = ICHIKAWA TAICHI / Proposal Principal Investigator Name
ra = 193.101334499172 / Right Ascension (Pointing Position) (deg)
dec = -29.2489232954401 / Declination (Pointing Position) (deg)
roll_angle = 294.100314904517 / Roll Angle (deg)
start_time = 2025-07-12T18:25:04 / Start Time of the Observation
stop_time = 2025-07-14T17:16:04 / Stop Time of the Observation
exposure = 83009.362692 / Effective Total Observation Exposure (s)
public_date= 2026-07-23 / Public Date