Lifetime function of stars until they reach the post-AGB phase as a function of their initial mass. Top: linear axes. Bottom: logarithmic axes. The logarithmic scale makes it easier to distinguish the individual lines and data points. The points are from the models by Miller Bertolami (2016), and the lines are the fit relations to those data points. 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.