Luminosity of pre-SN models at the end of core-carbon burning, as a function of initial mass (left) and CO core mass (right). The colors represent different values of convective core overshooting and the black circles indicate models that are expected to collapse into BHs. The gray-shaded region is the range of luminosity in which no SN IIP progenitors have been observed so far 5.1 ≤ log(L/L_⊙)≤5.5 (Davies & Beasor 2020). The blue line in the right panel shows our fit function to the luminosity and CO core masses of our models (see text).