Issue |
A&A
Volume 416, Number 2, March III 2004
|
|
---|---|---|
Page(s) | 529 - 536 | |
Section | Extragalactic astronomy | |
DOI | https://doi.org/10.1051/0004-6361:20034303 | |
Published online | 27 February 2004 |
XMM–Newton observations of the ultraluminous nuclear X-ray source in M 33*
1
Istituto di Astrofisica Spaziale e Fisica Cosmica (IASF) del CNR, Sezione di Bologna, Via Gobetti 101, 40129 Bologna, Italy
2
CEA Saclay, DSM/DAPNIA/SAp (CNRS FRE 2591), 91191 Gif-sur-Yvette Cedex, France
3
INTEGRAL Science Data Centre, Chemin d'Écogia 16, 1290 Versoix, Switzerland
4
The Observatories of the Carnegie Institution of Washington, 813 Santa Barbara Street, Pasadena, CA 91101, USA
5
Observatory of Geneva, 51 chemin des Maillettes, 1290 Sauverny, Switzerland
Corresponding author: L. Foschini, foschini@bo.iasf.cnr.it
Received:
10
September
2003
Accepted:
3
December
2003
We present observations with XMM-Newton of M 33 X-8, the ultraluminous
X-ray source ( erg/s) closest to the centre of the galaxy.
The best-fit model is similar to the typical model of Galactic black holes in very high state.
Comparison with previous observations indicates that the source is still in a
very high state after about 20 years of observations. No state transition has
been observed even during the present set of XMM-Newton observations.
We estimate the lower limit of the mass of the black hole >
, but
with proper parameters taking into account different effects, the best estimate becomes
. Our analysis favours the hypothesis that M 33 X–8 is a stellar mass
black hole candidate, in agreement with the findings of other authors. In addition,
we propose a different model where the high luminosity of the source
is likely to be due to orientation effects of the accretion disc and anisotropies in the
Comptonized emission.
Key words: X-rays: binaries / X-rays: galaxies / galaxies: individual: M 33 / galaxies: nuclei
© ESO, 2004
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