New Tables: tracks and colors for H- and He- atmosphere white dwarfs

Tables containing cooling tracks and absolute magnitudes on various photometric systems for pure H and He atmosphere white dwarfs. Calculations have been done with the stellar evolutionary code LPCODE developed at University of La Plata, Argentina. Details about LPCODE can be found at: Althaus et al. 2005, A&A 435, 631; 2010, ApJ 719, 612; 2012, A&A 537, A33; Rohrmann et al. 2012, A&A 546, A119; Salaris et al. 2013, A&A, 555, A96; Miller Bertolami et al. 2016, A&A 588, A25. LPCODE considers outer boundary conditions provided by non-grey model atmospheres and a full treatment of energy sources, in particular the energy contribution ensuing from phase separation of core chemical species upon crystallisation, ²²Ne sedimentation and residual nuclear burning. Abundance changes resulting from mixing induced by mean molecular weight inversion, convective mixing, nuclear burning, element diffusion, and phase separation of core chemical constituents upon crystallisation are considered during the WD regime. White dwarf evolutionary sequences are computed selfconsistently from progenitor stars evolved from the ZAMS through the core hydrogen- and helium-burning evolutionary phases (and off-center carbon ignition in the case of ultra-massive white dwarf progenitors) to the thermally pulsing AGB and, ultimately, to the white dwarf stage.