Mukai, K.; Still, M.; Corbet, R. H. D.; Kuntz, K. D. and Barnard, R.
|DOI (Digital Object Identifier) Link:||http://doi.org/10.1086/497110|
|Google Scholar:||Look up in Google Scholar|
We report our analysis of X-ray data on M101 ULX-1, concentrating on high-state Chandra and XMM-Newton observations. We find that the high state of M101 ULX-1 may have a preferred recurrence timescale. If so, the underlying clock may have periods around 160 or 190 days, or possibly around 45 days. Its short-term variations resemble those of X-ray binaries at high accretion rates. If this analogy is correct, we infer that the accretor is a 20 40 M-circle dot object. This is consistent with our spectral analysis of the high-state spectra of M101 ULX-1, from which we find no evidence for an extreme (> 10(40) ergs s(-1)) luminosity. We present our interpretation in the framework of a high-mass X-ray binary system consisting of a B supergiant mass donor and a large stellar-mass black hole.
|Item Type:||Journal Article|
|Copyright Holders:||2005 The American Astronomical Society|
|Keywords:||galaxies; x-rays; binary stars|
|Academic Unit/Department:||Faculty of Science, Technology, Engineering and Mathematics (STEM) > Physical Sciences
Faculty of Science, Technology, Engineering and Mathematics (STEM)
|Interdisciplinary Research Centre:||Centre for Earth, Planetary, Space and Astronomical Research (CEPSAR)|
|Depositing User:||Colin Smith|
|Date Deposited:||07 Sep 2009 10:09|
|Last Modified:||04 Oct 2016 10:27|
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