Evolutionary sequences appropriate for hot hydrogen-deficient white dwarfs, and described in Althaus, Panei, Miller Bertolami et al. 2009, ApJ, 704, 1605, are provided. 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, Serenelli, Panei et al. 2005, A&A, 435, 631; Althaus, Corsico, Bischoff-Kim et al. 2010, ApJ, 717, 897, and references therein. Evolutionary sequences are computed selfconsistently from progenitor stars evolved from the ZAMS through the core hydrogen- and helium-burning evolutionary phases to the thermally pulsing AGB and, ultimately, to the born again episode that is responsible for the hydrogen deficiency. These calculations provide a homogeneous set of evolutionary tracks appropriate for mass and age determinations for both PG 1159 stars and DO-DB white dwarfs. White dwarf sequences are computed in a consistent way with the evolution of chemical abundance distribution caused by element diffusion along the whole cooling phase. Calculations are extended down to an effective temperature of 7000 K. The full treatment of the entire evolutionary history of white dwarfs provides consistent white dwarf initial configurations. In addition, our calculations also yield self-consistent interior chemical profiles (click here to download the chemical profiles of our hydrogen-deficient white dwarf models).

Also, colors and magnitudes for these sequences are provided for effective temperatures less than 50,000K. They are based on non-gray local thermodynamic equilibrium (LTE) model atmospheres (Rohrmann et al. 2002 ). The calculations were done for a pure helium composition and for the HST ACS filters (Vega-mag system) and UBVRI photometry.

The initial models for our white dwarf sequences correspond to realistic hydrogen-deficient PG 1159 stellar configurations derived from the full evolutionary calculations of their progenitor stars for solar metallicity (Miller Bertolami & Althaus 2006 ). Each cooling sequence file lists from left to right:

The table below lists the H-deficient white dwarf sequences considered. Additional sequences are provided upon request to Leandro Althaus at althaus@fcaglp.unlp.edu.ar

Note: For the 1M_sun model, two different sequences were computed with two different mass loss rates during the AGB evolution. In this way, we obtain a different number of thermal pulses and, in the end, two different remnant masses of 0.530 and 0. 542 M_sun, respectively.

Our evolutionary sequences in the plane surface gravity-effective temperature together with observational data of DO white dwarfs are shown in the figure below