Lifetime function of stars until they reach the post-AGB phase as a function of their initial mass. The lines are the fit relations to the models of Miller Bertolami (2016) with original metallicities of Z = 0.0001, 0.001, 0.01, and 0.02, as in Fig. 1. Here, the extrapolation of these fits to Z = 0.05 is also shown. The points are the results of newly run models following the procedure of Miller Bertolami (2016) for Z = 0.05, and the lines are the fit relations to those data points. The linear helium abundance is at Y = 0.345 and the cutoff helium abundance at Y = 0.285. The thick lines are at the same metallicities as the ones from the original models (Z = 0.0001, 0.001, 0.01, and 0.02) and the thin lines are at Z = 0.00001, 0.0003, 0.003, and 0.014, where the last three values are the logarithmic midpoints of the original metallicities.