Abstract. 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 L2−10 keV> 10 31 erg s −1. 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 L2−10 keV < 10 31 erg s −1. We conclude that the bulk of the Galactic X-ray background is produced by discrete sources
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