Initial orbital period P_i versus the initial mass ratio q_i for the computed binary evolution models (squares), with a color-coding denoting the remaining envelope mass of the primary star at the time of its core collapse. The envelope mass can be used to indicate the anticipated SN type if no CSM interaction would occur (see color bar). The black lines separate systems without mass transfer (above the thick full-drawn), Case C (above the dashed line), Case B+C systems (above the dotted line), and pure Case B systems. where the latter is not investigated in the area in which no binary models are computed. The background pattern of circles indicates a likely CE evolution, where for wide, open circles the energy criterion implies that a CE ejection would be possible, and small filled circles imply the opposite. Here, symbols in red color indicate that the donor star’s core may collapse before the end of the common envelope phase is reached. As in this case, the pre-SN envelope structure is not well constrained, we give the corresponding squares multiple background colors, indicating the range of possibilities. The star symbols represent the multi-D models of Lau et al. (2022). Black arrows point out rows and columns in the plot for which data is displayed in Table 1.