Final total mass (M_final; black), helium core mass (M_He; maroon), and carbon-oxygen core mass (M_CO; blue) as a function of initial mass (M_initial) for our default grid (top) and our grid with winds boosted by a factor of 1.5 (bottom). We also depict the stellar models (white crosses) that we interpolate between. In the background, we shade the mass ranges for final stellar structures that could give rise to SNe IIb if they explode at collapse (with 0 <  M_env ≤ 0.5 M_⊙; light blue shading) and WR stars that may produce SNe Ib/c (with M_env = 0, blue shading). We also mark the models that lead to successful explosions, according to the FR12-rapid, FR12-delayed, S16-N20, S16−S19.8, P20E16+N20, and C20 SN engines (horizontal magenta, brown, gray, light green, light orange, and dark orange bands of arbitrary y value). In the inset plots we show the final envelope mass (M_env) for models with initial masses of 15−40 M_⊙.