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Chandra ACIS-S observations of the galaxy cluster A3112 feature the presenceof an excess of X-ray emission above the contribution from the diffuse hot gas,which can be equally well modeled with an additional non-thermal power-lawmodel or with a low-temperature thermal model of low metal abundance. We showthat the excess emission cannot be due to uncertainties in the backgroundsubtraction or in the Galactic HI column density. Calibration uncertainties inthe ACIS detector that may affect our results are addressed by comparing theChandra data to XMM MOS and PN spectra. While differences between the threeinstruments remain, all detect the excess in similar amounts, providingevidence against an instrumental nature of the excess. Given the presence ofnon-thermal radio emission near the center of A3112, we argue that the excessX-ray emission is of non-thermal nature and distributed throughout the entireX-ray bandpass, from soft to hard X-rays. The excess can be explained with thepresence of a population of relativistic electrons with ~7% of the cluster'sgas pressure. We also discuss a possible thermal nature of the excess, andexamine the problems associated with such interpretation.

Soft and hard X-ray excess emission in Abell 3112 observed with Chandra