A BCG with offset cooling: is the AGN feedback cycle broken in A2495?
  We present a combined radio/X-ray analysis of the poorly studied galaxy
cluster Abell 2495 (z=0.07923) based on new EVLA and Chandra data. We also
analyze and discuss Halpha emission and optical continuum data retrieved from
the literature. We find an offset of 6 kpc between the cluster BCG
(MCG+02-58-021) and the peak of the X-ray emission, suggesting that the cooling
process is not taking place on the central galaxy nucleus. We propose that
sloshing of the ICM could be responsible for this separation. Furthermore, we
detect a second, 4 kpc offset between the peak of the Halpha emission and that
of the X-ray emission. Optical images highlight the presence of a dust filament
extending up to 6 kpc in the cluster BCG, and allow us to estimate a dust mass
within the central 7 kpc of 1.7e+5 Msun. Exploiting the dust to gas ratio and
the L_Halpha-M_mol relation, we argue that a significant amount (up to 10^9
Msun) of molecular gas should be present in the BCG of this cluster. We also
investigate the presence of ICM depressions, finding two putative systems of
cavities; the inner pair is characterized by t age = 18 Myr and P cav = 1.2e+43
erg/s, the outer one by t age = 53 Myr and P cav = 5.6e+42 erg/s. Their age
difference appears to be consistent with the free-fall time of the central
cooling gas and with the offset timescale estimated with the Halpha kinematic
data, suggesting that sloshing is likely playing a key role in this
environment. Furthermore, the cavities' power analysis shows that the AGN
energy injection is able to sustain the feedback cycle, despite cooling being
offset from the BCG nucleus.
