White dwarfs simulated with our evolutionary code, presented in Benvenuto & De Vito (2003), De Vito & Benvenuto (2012), and Benvenuto et al. (2014). These white dwarfs come from a grid detailed in the associated paper. These stars are in a binary system with a compact object, from the ZAMS until their end as a white dwarf. The data from these tables corresponds to the final cooling track. Each table is in ASCII format, with the following columns: white dwarf mass (in solar masses), accretor mass (in solar masses), orbital period of the system (in days), radius (in solar radii), luminosity (in solar luminosities), hydrogen mass (in solar masses) and surface gravity (in CGS).