Photometric determinations of photospheric parameters of white dwarfs

White dwarf stars are the final end point in the evolution of more than 95% of all single stars that are born in the universe. Therefore, their understanding places important constraints in stellar evolution as a whole. The goal of our project is to compare the photometric and astrometric measurements of pulsating white dwarfs discovered by the Transiting Exoplanet Survey Satellite
(TESS) to derive effective temperature (Teff) and surface gravity (log g). We have compared the photometric measurements in the u, g, r, i, and z bands from the Sloan Digital Sky Survey (SDSS) and parallax and apparent magnitude (g_mean) from Gaia to a model grid using least squares minimization for these white dwarfs. We present our results of best fits for the photospheric parameters, using contour plots, with the uncertainties provided by our calculations. Our results are an independent measurement of Teff and log g for these white dwarf stars.