the line-of-sight material, and convolving the results with the $Chandra$ mirror and ACIS detector response. Typical on-axis CCCP calibration redistribution matrix and auxiliary response calibration files were used [@Broos11a]. After applying local background levels found in the CCCP data, we then remove very weak extragalactic sources that would have fallen below the CCCP source detection threshold[^2].

Our simulations predict that $\sim2500$ extragalactic sources should be detected in the CCCP observation.

Galactic Sources \[contaminants\_stellar\_section\]
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It has been argued that the point source component of the hard “Galactic ridge emission”, which stretches over 90 degrees in Galactic longitude and only 2 degrees in latitude around the Galactic Center, is mainly composed of cataclysmic variables [e.g @Ebisawa05; @Revnivtsev07; @Hong09]. The current version of our simulation omits the distribution of hard ($\ge3$ keV) X-ray sources in the Galactic plane attributed to cataclysmic variables and other classes of accretion-driven X-ray binary systems. However, this population and its X-ray emission should be unimportant in the Carina star forming region because it is located 72 degrees away from the Galactic Center where the Galactic Ridge emission is weak [see Figure 1 in @Revnivtsev06].

We simulate the stellar contamination from main sequence and giant stars in the 