This article has an erratum: [https://doi.org/10.1051/0004-6361:20035661e]
Volume 405, Number 2, July II 2003
|Page(s)||505 - 511|
|Published online||19 June 2003|
RX J0042.3+4115: A stellar mass black hole binary identified in M 31
The Department of Physics and Astronomy, The Open University, Walton Hall, Milton Keynes, MK7 6BT, UK
2 The Department of Physics and Astronomy, The University of Leicester, Leicester, LE1 7RH, UK
3 Los Alamos National Laboratory, PO Box 1663, Mail Stop D436, NIS-2, Los Alamos, MN 87545, USA
Corresponding author: R. Barnard, firstname.lastname@example.org
Accepted: 17 April 2003
Four XMM-Newton X-ray observations of the central region of the Andromeda Galaxy (M 31) have revealed an X-ray source that varies in luminosity over ~ erg s-1 between observations and also displays significant variability over time-scales of a few hundred seconds. The power density spectra of lightcurves obtained in the 0.3–10 keV energy band from the three EPIC instruments on board XMM-Newton are typical of disc-accreting X-ray binaries at low accretion rates, observed in neutron star binaries only at much lower luminosities (~ 1036 erg s-1). However X-ray binaries with massive black hole primaries have exhibited such power spectra for luminosities >1038 erg s-1. We discuss alternative possibilities where RX J0042.3+4115 may be a background AGN or foreground object in the field of view, but conclude that it is located within M 31 and hence use the observed power spectra and X-ray luminosities to identify the primary as a black hole candidate.
Key words: X-rays: general / galaxies: individual: M 31 / X-rays: binaries / black hole physics
© ESO, 2003
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