detections include: 100 F stars, 500 G stars, 10 K stars, 40 M stars, and 250 giants. Approximately 35%, 35%, and 30% of the simulated background detections have distances in the ranges $2.3-3.0$ kpc, $3.0-4.0$ kpc, and $4.0-5.0$ kpc, respectively.

Several caveats pertain to the simulation. First, the line of sight towards the Carina complex is tangent to the Sagittarius-Carina spiral arm, but the Besançon model of the Galactic disk population (which our simulations rely on) lacks spiral arm modeling [@Robin03]. Second, X-ray luminosities of stars with ages $<1$ Gyr might be even higher than those of stars from the solar neighborhood [@Preibisch05]. Roughly $1/4$ of the simulated Besançon stars have ages $<1$ Gyr. Third, due to computational reasons, the simulations of Galactic background stars were truncated at a distance of $5$ kpc. Due to these three factors, we might expect even larger stellar contamination populations. Fourth, on the other hand, a possible decrease in X-ray activity with mass and age in giant stars [@Pizzolato00] is ignored in our simulations. If one considers only the most plausible class of X-ray emitting giants, F and G giants with ages $<1$ Gyr, the expected number of detected giants in the CCCP field 