Chandra observations of the Abell S0295 cluster
  We present deep ($205 \rm ks$), \Chandra observations of the \ab295 binary
merging cluster ($z=0.30$). In the X-ray image, the secondary component is
clearly visible as a surface brightness peak, while the primary cluster has a
flatter distribution. We found cool gas ($\sim 6 \rm keV$) associated with the
secondary, while the central temperature of the primary does not deviate
significantly from the mean temperature of the cluster of $\sim 9.5 \rm keV$.
In the vicinity of the primary's core we found the hottest region in the
cluster accompanied by a surface brightness discontinuity. We propose that this
region corresponds to a shock, for which we estimate a Mach number of
$1.24_{-0.22}^{+0.30}$. We found other merger signatures such as a plume of
cool gas emerging from the primary cluster and a cold front and a possible bow
shock (Mach number of $1.74_{-0.74}^{+1.02}$) leading the secondary cluster.
Based on the observed properties in comparison to binary merger simulations
from the literature we propose for \ab295 a low mass ratio, off-axis merging
scenario, with secondary close to first apocentre. Comparison of our results
with strong lensing observations of \ab295 from \cite{Cibirka2018} shows an
offset between the total mass peak and the bulk of the gas distribution in the
primary cluster. The properties of the merger and the existence of the offset
between mass peak and gas make \ab295 a promising candidate for the study of
mergers involving non-cool core clusters and the nature of dark matter.
