Evolutionary sequences appropriate for PG 1159 stars, and described in Miller Bertolami & Althaus 2006, A&A, 454, 845, 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 (VLTP) and LTP episodes that are 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 white dwarf stars . Each evolutionary track file lists from left to right:

The stellar mass of our sequences are: 0.870, 0.741, 0.664, 0.609, 0.584, 0.565, 0.542, 0.530, 0.515, 0.512 Msun. All of these sequences experienced a VLTP episode, except the last one that experienced a LTP episode.

Some of our evolutionary tracks in the g-Teff plane together with observational data of PG 11159 stars are shown in the figure below: