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Issue A&A
Volume 391, Number 3, September I 2002
Page(s) 993 - 997
Section Formation, structure and evolution of stars
DOI http://dx.doi.org/10.1051/0004-6361:20020842



A&A 391, 993-997 (2002)
DOI: 10.1051/0004-6361:20020842

XMM-Newton detection of Nova Muscae 1991 in quiescence

F. K. Sutaria1, U. Kolb1, P. Charles2, J. P. Osborne3, E. Kuulkers4, J. Casares5, E. T. Harlaftis6, T. Shahbaz7, M. Still8 and P. Wheatley3

1  The Open University, Milton Keynes, UK
2  University of Southampton, UK
3  X-ray Astronomy Group, Dept of Physics and Astronomy, University of Leicester, University Rd, Leicester LE1 7RH, UK
4  SRON, Utrecht, The Netherlands
5  IAC, La Laguna, Tenerife, Spain
6  Institute of Astronomy and Astrophysics, National Observatory of Athens, PO Box 20048, Athens 11810, Greece
7  Dept. of Astrophysics, Oxford University, UK
8  NASA/GSFC, Maryland, USA

(Received 19 March 2002 / Accepted 4 June 2002 )

Abstract
The soft X-ray transient GU Mus has been detected by XMM-Newton in the quiescent state. The source is very faint, with a 0.5-10.0 keV unabsorbed flux of $\simeq $ $1.1 \times 10^{-14}$  ergs cm -2 s -1. The spectra is well fit by an absorbed powerlaw with a photon index of $ \alpha = 1.6 \pm 0.4$, close to the value seen when the source was in the low/hard state in Aug. 1991. From our observed luminosity, it seems unlikely that the quiescent state emission is dominated by coronal X-rays from the secondary. The flux also appears to be in agreement with the ADAF model of BH-transients in quiescence.


Key words: X-rays: binaries -- X-rays: individuals: GU Mus -- black hole physics -- accretion, accretion disks

Offprint request: F. K. Sutaria, F.K.Sutaria@open.ac.uk

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