view[^9] (ignoring the “egg-crate effect”, due to variations in sensitivity with off-axis angle [@Broos11a]). In contrast to panel $a$, 70% of the sources in panel $b$ ($1.1< MedE <1.5$ keV) and 80% of the sources in panel $c$ ($1.5< MedE <2.0$ keV) are seen in projection against the chain of Carina clusters. Figure \[fig\_acisno2mass\] presents all CCCP sources without 2MASS counterparts. Panels $a$ ($MedE <1.1$ keV), $b$ ($1.1< MedE <1.5$ keV), and $c$ ($1.5< MedE <2.0$ keV) show that approximately 80%, 50%, and 50% of sources, respectively, are evenly distributed across the CCCP field.

Thus, based simply on their uniform spatial distributions, as many as $700$ ($+1400$) with $MedE<1.1$ keV, $800$ ($+1100$) with $1.1<MedE<1.5$ keV, and $300$ ($+700$) with $1.5<MedE<2.0$ keV sources with (without) 2MASS counterparts could be potential Galactic stellar contaminants. Further consideration of the expected $MedE$ and $J$-band properties for the simulated stellar contaminants (§\[contamination\_properties\_section\]) suggests that indeed, most of the $700+1400 = 2100$ sources with $MedE<1.1$ keV could be foreground stars, and roughly half of the $800+1100=1900$ sources with $1.1<MedE<1.5$ keV could be background stars. Therefore, this leaves us with at least $\sim300$ ($MedE<1.1$ keV), $\sim1000$ ($1.1<MedE<1.5$ keV), and $\sim1000$ ($1.5<MedE<2.0$ keV) CCCP sources evenly distributed across 