ABELL2256_P2
XRISM PV results on merging galaxy clusters show low velocity dispersion, at the lower end of cosmological simulation predictions. This raises questions on turbulence development timescales, implemented physics in the simulations, and whether the PV sample favors more relaxed clusters. To address this, we propose three Resolve pointings (510 ks total) of A2256 - a complex merger with disturbed X-ray morphology and striking radio structures. We will map gas kinematics and, supported by simulations of the A2256 analog, interpret its complexity, reconstruct merger geometry and energy partition. Correlating peculiar radio emission variations with gas motions will test cosmic ray re-acceleration models. We will constrain the velocity power spectrum, building on the first such attempt in Coma.
obsid = 202040010 / Unique Observation/Sequence Number
object = ABELL2256_P2 / Object name
pi_name = ZHURAVLEVA IRINA / Proposal Principal Investigator Name
ra = 255.790946540741 / Right Ascension (Pointing Position) (deg)
dec = 78.6609492797563 / Declination (Pointing Position) (deg)
roll_angle = 229.985305328682 / Roll Angle (deg)
start_time = 2025-10-30T13:59:04 / Start Time of the Observation
stop_time = 2025-11-02T21:16:04 / Stop Time of the Observation
exposure = 187509.34318 / Effective Total Observation Exposure (s)
public_date= 2026-11-13 / Public Date