Resolving the Galactic X-ray background

Details Resolving the Galactic X-ray background Resolving the Galactic X-ray background

2006-11-30

arxiv.org/abs/astro-ph/0611952v2

Astronomy and Astrophysics

Astrophysics

Submitted to A&A

Scientific paper

10.1051/0004-6361:20066850

We use Chandra deep observations of the Galactic Center (GC) region to improve the constraints on the unresolved fraction of the Galactic X-ray background (also known as the Galactic ridge X-ray emission). We emphasize the importance of correcting the measured source counts at low fluxes for bias associated with Poisson noise. We find that at distances of 2'-4' from Sgr A* at least ~40% of the total X-ray emission in the energy band 4-8 keV originates from point sources with luminosities L(2-10 keV)> 10^{31} erg/sec. From a comparison of the source number-flux function in the GC region with the known luminosity function of faint X-ray sources in the Solar vicinity, we infer that Chandra has already resolved a large fraction of the cumulative contribution of cataclysmic variables to the total X-ray flux from the GC region. This comparison further indicates that most of the yet unresolved ~60% of the X-ray flux from the GC region is likely produced by weak cataclysmic variables and coronally active stars with L(2-10 keV)<10^{31} erg/sec. We conclude that the bulk of the Galactic X-ray background is produced by discrete sources.

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