R. Barnard, M. Garcia, S. S. Murray
XMM J004243.6+412519 is a transient X-ray source in M31, first discovered 2012 January 15. Different approaches to fitting the brightest follow-up observation gave luminosities 1.3--2.5E+39 erg/s, making it the second ultraluminous X-ray source (ULX) in M31, with a probable black hole accretor. These different models represent different scenarios for the corona: optically thick and compact, or optically thin and extended. We obtained Chandra ACIS and {\em HST} ACS observations of this object as part of our transient monitoring program, and also observed it serendipitously in a 120 ks XMM-Newton observation. We identify an optical counterpart at J2000 position 00:42:43.70 +41:25:18.54; its F435W (~ B band) magnitude was 25.97+/-0.03 in the 2012 March 7 observation, and >28.4 at the 4 sigma level during the 2012 September 7 observation, indicating a low mass donor. We created two alternative lightcurves, using the different corona scenarios, finding linear decay for the compact corona and exponential decay for the extended corona; linear decay implies a disk that is >5 magnitudes brighter than we observed. We therefore favor the extended corona scenario, but caution that there is no statistical preference for this model in the X-ray spectra alone. Using two empirical relations between the X-ray to optical ratio and the orbital period, we estimate a period of ~9--30 hr; this period is consistent with that of the first ULX in M31 (18 +5 -6 hr).
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http://arxiv.org/abs/1305.1302
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