Lifetime τ (until the white dwarf phase or core collapse) as a function of initial mass for single stars adopted in this work (black line) is compared with predictions that we obtained using the MESA stellar evolutionary code (Paxton et al. 2011) with and without overshooting (dark and lightblue dots) and with Geneva models of Schaller et al. (1992, black dots). Single stars with masses less than M_min,cc end their lives as white dwarfs instead of ccSNe (hashed region). ccSNe are expected between τ_min,cc and τ_max,cc (yellow shaded region), which refer to the lifetimes of the most and least massive star to undergo core collapse. The bottom panel shows the relative difference in lifetimes with respect to the lifetimes used in our work (Sect. 2.2).