Determining T_eff and log g of White Dwarfs with Infrared Excess

Understanding the physical properties of white dwarfs is crucial for unraveling their evolutionary histories and their roles in stellar populations. In this study, we analyze a dataset composed of 31 HETDEX DA white dwarfs with infrared excess, eight of which have SDSS observed spectra. Our goal is to determine the effective temperature (T_eff) and surface gravity (logg) of each spectrum through the fitting of atmospheric models produced by Detlev Koester to our observed data. Because of the infrared excess, we only use the absorption lines in the Balmer series to determine T_eff and logg. Employing a modified \chisq method , we fitted the Balmer line profiles of the models to the observed data to find the best solutions for T_eff and logg for each of the 31 HETDEX observed spectra. In order to select the best solution amongst the families of solutions, we have compared our determinations to the SDSS colors. In this talk, we present our results for the WDs with infrared excess observed by HETDEX and our initial attempts to model the additional source.