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 Sloan Digital Sky Survey passbands (u, g, r, i and z) and magni- tudes in the Gaia DR2 and EDR3 passbands ( G2, G BP 2, G RP 2, G3, G BP 3, and G RP 3).



H-rich table



H-deficient table