Volume 526, February 2011
|Number of page(s)||5|
|Section||Stellar structure and evolution|
|Published online||21 December 2010|
Observations of the recurrent M 31 transient XMMU J004215.8+411924 with Swift, Chandra, HST, and Einstein
Harvard-Smithsonian Center for Astrophysics,
60 Garden Street,
2 Dublin Institute for Advanced Studies, Dublin, Republic of Ireland
3 Max-Planck-Institut für extraterrestrische Physik, Garching, Germany
Accepted: 9 November 2010
Context. The transient X-ray source XMMU J004215.8+411924 within M 31 was found to be in outburst again in the 2010 May 27 Chandra observation. We present results from our four Chandra and seven Swift observations that covered this outburst.
Aims. X-ray transient behaviour is generally caused by one of two things: mass accretion from a high mass companion during some restricted phase range in the orbital cycle, or disc instability in a low mass system. We aim to exploit Einstein, HST, Chandra and Swift observations to determine the nature of XMMU J004215.8+411924.
Methods. We model the 2010 May spectrum, and use the results to convert from intensity to counts in the fainter Chandra observations, as well as the Swift observations; these data are used to create a lightcurve. We also estimate the flux in the 1979 January 13 Einstein observation. Additionally, we search for an optical counterpart in HST data.
Results. Our best X-ray positions from the 2006 and 2010 outbursts are 0.3′′ apart, and 1.6′′ from the Einstein source; these outbursts are likely to come from the same star system. We see no evidence for an optical counterpart with mB ≲ 25.5; this new limit is 3.5 mag fainter than the existing one. Furthermore, we see no V band counterpart with mV ≲ 26. The local absorption is ~7 times higher than the Galactic line-of-sight, and provides ~2 mag of extinction in the V band. Hence MV ≳ −0.5. Fits to the X-ray emission spectrum suggest a black hole primary.
Conclusions. We find that XMMU J004215.8+411924 is most likely to be a transient LMXB, rather than a HMXB as originaly proposed. The nature of the primary is unclear, although we argue that a black hole is likely.
Key words: X-rays: general / X-rays: binaries / galaxies: individual: M 31
© ESO, 2010
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