Confirmation of IGR J01363+6610 as a Be X-ray binary with very low quiescent X-ray luminosity

Details Confirmation of IGR J01363+6610 as a Be X-ray binary with very low quiescent X-ray luminosity Confirmation of IGR J01363+6610 as a Be X-ray binary with very low quiescent X-ray luminosity

2010-12-13

arxiv.org/abs/1012.2817v1

Astronomy and Astrophysics

Astrophysics

High Energy Astrophysical Phenomena

9 pages, accepted by ApJ

Scientific paper

The field containing the candidate High Mass X-ray Binary IGR J01363+6610 was observed by XMM-Newton on 2009 July 31 for 28 ks. A Be star was previously suggested as the possible counterpart of the INTEGRAL source, and although Chandra, during a 2007 observation, did not detect an X-ray source at the position of the Be star, we find a variable source (XMMU J013549.5+661243) with an average X-ray flux of 2e-13 ergs/cm2/s (0.2-12 keV, unabsorbed) at this position with XMM-Newton. The spectrum of this source is consistent with a hard power-law with a photon index of 1.4 +/- 0.3 and a column density of 1.5e22 cm^-2 (90% confidence errors). These results, along with our optical investigation of other X-ray sources in the field, makes the association with the Be star very likely, and the 2 kpc distance estimate for the Be star indicates an X-ray luminosity of 9.1e31 ergs/s. This is lower than typical for a Be X-ray binary, and the upper limit on the luminosity was even lower (<1.4e31 ergs/s assuming the same spectral model) during the Chandra observation. We discuss possible implications of the very low quiescent luminosity for the physical properties of IGR J01363+6610.

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