Oxygen yields for He-star as well as for single-star H-rich explosion models. Top: comparison of the O yield for the ejecta arising from the He-star progenitor models (which implicitly assume an evolution in a binary system; the same set of models as in Fig. 2 is shown) and for those arising from the single-star models of Sukhbold et al. (2016, shown as filled red stars), which all reach core collapse with a residual H-rich envelope. The O yield for a given ZAMS mass is much lower for the He-star progenitors of SNe Ibc than for the red-supergiant progenitors of SNe II. Bottom: same as top, but now shown versus the pre-SN mass for He-star models and the final He-core mass for the single-star models.