Measuring Star Formation Histories, Distances, and Metallicities with Pixel Color-Magnitude Diagrams. I. Model Definition and Mock Tests

We present a comprehensive study of the applications of the pixel color-magnitude diagram (pCMD) technique for measuring star formation histories (SFHs) and other stellar population parameters of galaxies, and we demonstrate that the technique can also constrain distances. SFHs have previously been measured through either the modeling of resolved-star CMDs or of integrated-light spectral energy distributions, yet neither approach can easily be applied to galaxies in the "semi-resolved regime." The pCMD technique has previously been shown to have the potential to measure stellar populations and SFHs in semi-resolved galaxies. Here we present Pixel Color-Magnitude Diagrams with Python (PCMDPy), a graphics processing unit (GPU)-accelerated package that makes significant computational improvements to the original code and includes more realistic physical models. These advances include the simultaneous fitting of distance, modeling a Gaussian metallicity distribution function, and an observationally motivated dust model. GPU acceleration allows these more realistic models to be fit roughly 7x. faster than the simpler models in the original code. We present results from a suite of mock tests, showing that with proper model assumptions, the code can simultaneously recover SFH, [Fe/H], distance, and dust extinction. Our results suggest the code, applied to observations with Hubble Space Telescope-like resolution, should constrain these properties with high precision within 10 Mpc and can be applied to systems out to as far as 100 Mpc. pCMDs open a new window to studying the stellar populations of many galaxies that cannot be readily studied through other means.