Distribution of initial masses, M_ZAMS, of SN progenitors with M_ZAMS <  M_min, WR ≈ 27 M_⊙. For a population of single stars (dashed black line) we expect the distribution to follow the IMF, with all progenitors between M_min, ccSN ≈ 7.6 M_⊙ and M_min, WR leading to Type II SNe. The shape of the distribution changes for progenitors that experienced binary interaction (solid black line). The progenitors of SN II arising from a population of binary interacting systems (red region) originate from lower on average M_ZAMS, even below M_min, ccSN. In addition, many stars with M_ZAMS <  M_min, WR lead to stripped-envelope SNe due to binary interaction (blue region, stacked on top of the red region), avoiding a hydrogen-rich event. The results are for our standard assumptions and show the number of SNe per bin in M_ZAMS per solar mass of star formation.