Input data adopted in this work for solar metallicity massive stars with mass loss. Left: non rotating models from Limongi & Chieffi (2006); right: rotating models from Hirschi, Meynet & Maeder (2005). Top: mass of the (H-exhausted) He core M_HeC, of the star at explosion M_Exp and of the compact remnant M_Rem as a function of the initial stellar mass M_∗. Bottom: derived quantities are the mass of the wind M_Wind = M_∗ − M_Exp, the mass of the nuclearly processed layer M_Proc = M_HeC − M_Rem and of the unprocessed (²²Ne-normal) envelope M_Env = M_Wind-M_Proc and the mass of the SN ejecta M_Ej = M_Exp − M_Rem In all cases, curves are smoothly interpolated between model results.