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The TeV gamma-ray point source HESSJ1832-093 remains unidentified despiteextensive multi-wavelength studies. The gamma-ray emission could originate in avery compact pulsar wind nebula or an X-ray binary system composed of the X-raysource XMMU J183245-0921539 and a companion star (2MASS J18324516-0921545). Tounveil the nature of XMMUJ183245-0921539 and its relation to HESSJ1832-093, weperformed deeper follow-up observations in X-rays with Chandra and Swift toimprove source localisation and to investigate time variability. We observed anincrease of the X-ray flux by a factor ~6 in the Chandra data compared toprevious observations. The source is point-like for Chandra and its updatedposition is only 0.3" offset from 2MASS J18324516-0921545, confirming theassociation with this infrared source. Subsequent Swift ToO observationsresulted in a lower flux, again compatible with the one previously measuredwith XMM-Newton, indicating a variability timescale of the order of two monthsor shorter. The now established association of XMMU J183245-0921539 and 2MASSJ18324516-0921545 and the observed variability in X-rays are strong evidencefor binary nature of HESS J1832-093. Further observations to characterise theoptical counterpart as well as to search for orbital periodicity are needed toconfirm this scenario.

Discovery of a variable X-ray counterpart to HESS J1832-093: A new gamma-ray binary?