Distribution of initial masses, M_ZAMS, of SN II progenitors experiencing binary interaction (red line) for increasing ranges of final core masses, M_He, preSN (on the right part). The contribution of each of the main binary scenarios is also shown in color below the distribution of binary-interacted progenitors. For reference we include the initial mass range of a single star corresponding to each M_He, preSN bin (black dashed line), which is shown in an arbitrary height. It becomes clear that the binary progenitors of SN II can originate from a wider range of lower on average M_ZAMS compared to single stars to form cores of similar mass, due to mass accretion or merging during their evolution. The results are for our standard assumptions although similar trends are found in all our model variations. The values on the y-axis show the number of SN II per bin in M_ZAMS per 10⁶ M_⊙ of stars formed.