Barnard, R.; Osborne, J.P.; Kolb, U. and Borozdin, K.N.
|DOI (Digital Object Identifier) Link:||http://dx.doi.org/10.1051/0004-6361:20030638|
|Google Scholar:||Look up in Google Scholar|
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 ~1-3x1038 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 >10 38 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.
|Item Type:||Journal Article|
|Copyright Holders:||2003 Royal Astronomical Society|
|Keywords:||X-rays; galaxies; M 31; binaries; black hole physics|
|Academic Unit/Department:||Science > Physical Sciences
|Interdisciplinary Research Centre:||Centre for Earth, Planetary, Space and Astronomical Research (CEPSAR)|
|Depositing User:||Users 6041 not found.|
|Date Deposited:||17 Jul 2006|
|Last Modified:||14 Jan 2016 16:09|
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