Tables containing cooling tracks and absolute magnitudes on SDSS, GAIA DR2 and GAIA EDR3 passbands, for pure H and He atmosphere ultra-massive white dwarfs. Calculations have been done with the stellar LPCODE developed at University of La Plata, Argentina. Details about LPCODE can be found at Althaus et al. 2005, A&A 435, 631. The oxygen-neon and carbon-oxygen tracks are presented in Camisassa et al. (2019), and Camisassa et al. (2022), respectively. These models include the energy released latent heat and phase separation upon crystallization. Carbon-oxygen models also include the energy released by 22Ne sedimentation. The 22Ne initial abundances are set to be equal to the initial metallicity of the star. The initial chemical profiles are the result of the progenitor evolution (Siess 2010 for Oxygen-Neon cores and Althaus et al. 2021 for Carbon-Oxygen cores).
Two sets of tables are presented: one with H-rich envelopes and one with H-deficient envelopes, using the model atmospheres of Koester D. (2010) Mem. Soc. Astron. Italiana, 81, 921, and Koester D. & Kepler S. O. (2019), A&A, 628, A102. In each set, there are 4 folders, whose name corresponds to the initial metallicity (or 22Ne abundance) of the tracks. In each of these folders there are 4 cooling tracks, and the name of each file states the white dwarf mass, except for the "solar metallicity" folder (0.02), that has 8 tracks, because it also includes Oxygen-Neon tracks. White dwarf masses are: 1.10, 1.16, 1.23 and 1.29 Msun. The columns listed are, from left to right, effective temperature (in K), logarithm of the luminosity (in solar units), cooling time (in 10^9 years), logarithm of the surface gravity (in CGS), stellar radius (in solar units), magnitudes in the following passbands: Gaia DR3 (G3, Bp3 and Rp3), Sloan Digital Sky Survey (u, g, r, i and z), PANSTARRS (g,r,i,z and y), Bessell (U, V, B, R and I), 2MASS (J,H and K) and Galex (FUV and NUV).
Tables containing cooling tracks and absolute magnitudes on GAIA DR3, SDSS and PanSTARRS passbands, for pure H atmosphere ultra-massive white dwarfs with oxygen-neon cores and stellar masses of 1.29, 1.31, 1.33, 1.35, and 1.369Msun and pure H atmosphere ultra-massive white dwarfs with carbon-oxygen cores and stellar masses of 1.29, 1.31, 1.33, 1.35, 1.37 and 1.382Msun. There are 20 files and the name of each file states the white dwarf mass. R means that such tracks were calculated considering the effects of general relativity on the structure and evolution of the white dwarfs. N corresponds to the same stellar masses but for the Newtonian gravity. The columns listed are, from left to right, effective temperature (in K), logarithm of the luminosity (in solar units), cooling time (in 10^9 years), logarithm of the surface gravity (in CGS), stellar radius (in solar units), magnitudes in the Gaia DR3 passbands ( G3, BP 3, and RP 3), magnitudes in the Sloan Digital Sky Survey (u, g, r, i and z), and PanSTARRS (g,r,i,z,y) passbands. Details are found in: https://arxiv.org/pdf/2208.14144.pdf and https://arxiv.org/pdf/2306.05251