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We present deep ($205 \rm ks$), \Chandra observations of the \ab295 binarymerging cluster ($z=0.30$). In the X-ray image, the secondary component isclearly visible as a surface brightness peak, while the primary cluster has aflatter distribution. We found cool gas ($\sim 6 \rm keV$) associated with thesecondary, while the central temperature of the primary does not deviatesignificantly 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 thecluster accompanied by a surface brightness discontinuity. We propose that thisregion 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 ofcool gas emerging from the primary cluster and a cold front and a possible bowshock (Mach number of $1.74_{-0.74}^{+1.02}$) leading the secondary cluster.Based on the observed properties in comparison to binary merger simulationsfrom the literature we propose for \ab295 a low mass ratio, off-axis mergingscenario, with secondary close to first apocentre. Comparison of our resultswith strong lensing observations of \ab295 from \cite{Cibirka2018} shows anoffset between the total mass peak and the bulk of the gas distribution in theprimary cluster. The properties of the merger and the existence of the offsetbetween mass peak and gas make \ab295 a promising candidate for the study ofmergers involving non-cool core clusters and the nature of dark matter.

Chandra observations of the Abell S0295 cluster