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 H \alpha emission and optical continuum data retrieved from the literature .
We find an offset of \sim 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 , \sim 4 kpc offset between the peak of the H \alpha emission and that of the X-ray emission .
Optical images highlight the presence of a dust filament extending up to \sim 6 kpc in the cluster BCG , and allow us to estimate a dust mass within the central 7 kpc of 1.7 \cdot 10 ^ { 5 } M _ { \sun } .
Exploiting the dust to gas ratio and the L _ { \text { H } \alpha } - M _ { \text { mol } } relation , we argue that a significant amount ( up to 10 ^ { 9 } M _ { \sun } ) 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 _ { \text { age } } \sim 18 Myr and P _ { \text { cav } } \sim 1.2 \cdot 10 ^ { 43 } erg s ^ { -1 } , the outer one by t _ { \text { age } } \sim 53 Myr and P _ { \text { cav } } \sim 5.6 \cdot 10 ^ { 42 } erg s ^ { -1 } .
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 H \alpha 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 .