Galactic Plane in three stages. First, Monte Carlo simulations of the Galactic stellar population expected within the CCCP field are constructed based on the ‘Besançon model’ of stellar populations [@Robin03]. The simulations are computed by the Web service provided by the Besançon group[^3]. Using models of Galactic structure, stellar mass function, and star formation history, the calculation gives the number distribution of stars along a chosen line-of-sight including individual spectral types, optical and near-infrared magnitudes, ages, distances, and source extinctions. An additional position-dependent absorption representing the Carina molecular clouds was added for stars behind Carina ($D > 2.3$ kpc). Besançon model limitations include a simplistic assumption of uniform extinction throughout the Galactic Plane and omission of spiral arms. We run the Galactic population model with an unrealistically deep $V=28$ mag detection limit, as the faint stars are later omitted by X-ray selection.

Second, X-ray luminosities for each star obtained from a Besançon model simulation are then estimated by Monte Carlo sampling of X-ray luminosity functions (XLFs) of MS stars measured in the solar neighborhood from [*ROSAT*]{} surveys [@Schmitt95; @Schmitt97; @Hunsch99]. Based on these studies, we adopt the following lognormal XLFs with the following means and standard deviations in $\log L_X$ 