range; 94% of the simulated extragalactic sources are within the $2.5 < MedE < 4.5$ keV range.

2.  The observed CCCP sources span a wide range of $MedE$, from 0.6 to 7 keV, with a skewed distribution peaking at $1.4-1.5$ keV.

3.  The histograms of the observed CCCP sources and the simulated foreground stars have similar numbers of sources in the range $0.7 < MedE < 1$ keV, suggesting that nearly all the CCCP sources in this range are likely foreground stars. This also implies that our simulation did not significantly underestimate the foreground population due to an unmodeled population of MS stars in the Carina spiral arm (§ \[contaminants\_stellar\_section\]).

4.  The histograms of the observed CCCP sources and the simulated AGNs have similar numbers of sources in the range $2.5 < MedE < 4.5$ keV, suggesting that nearly all the CCCP sources in this energy range can be AGNs.

5.  The peak of the simulated background stars coincides with the peak of the observed CCCP sources, but the numbers of the CCCP and simulated background sources are drastically different. It is clearly impossible to distinguish between background stars and Carina PMS members using $MedE$.

We see that the X-ray 