Astronomy and Astrophysics – Astrophysics
Scientific paper
2003-06-22
Astrophys.J.599:1067-1081,2003
Astronomy and Astrophysics
Astrophysics
13 pages, 7 figures. ApJ submitted
Scientific paper
10.1086/379245
We report on the population of point sources discovered during an 18.5 ksec Chandra ACIS-S observation of the Sombrero Galaxy. We present the luminosity function, the spectra of the 6 brightest sources, consider correlations with globular clusters (GCs) and with planetary nebulae (PNe), and study the galaxy's population of SSSs. We detected 122 sources, 22 of them are identified as luminous supersoft X-ray sources (SSSs). There is an over density of SSSs within 1.5 kpc of the nucleus, which is itself the brightest X-ray source. SSSs are also found in the disk and halo, with 1 SSS in a globular cluster (GC). Several sources in Sombrero's halo are good candidates for SSS models in which the accretor is a nuclear-burning white dwarf. In total, 32 X-ray sources are associated with GCs. The majority of sources with luminosity > 1e38 erg/s are in GCs. These results for M104, an Sa galaxy, are similar to what has been found for elliptical galaxies and for the late-type spiral M31. We find that those optically bright GCs with X-ray sources house only the brightest X-ray sources. We find that, in common with other galaxies, there appears to be a positive connection between young (metal-rich) GCs and X-ray sources, but that the brightest X-ray sources are equally likely to be in metal-poor GCs. We propose a model which can explain the trends seen in the data sets from the Sombrero and other galaxies. Thermal-time scale mass transfer can occur in some of the the younger clusters in which the turn-off mass is slightly greater than $0.8 M_\odot$; multiplicity may play a role in some of the most massive clusters; accretion from giant stars may be the dominant mechanism in some older, less massive and less centrally concentrated clusters.
Delain Kisha M.
Di Stefano Rosanne
Harris William E.
Kong Albert K. H.
Murray Stephen S.
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