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A crucial ingredient in population synthesis studies involving massive starsis the determination of whether they explode or implode in the end. While thefinal fate of a massive star is sensitive to its core structure at the onset ofcollapse, the existing binary population synthesis studies do not reachcore-collapse. Instead, they employ simple prescriptions to infer their finalfates without knowing the presupernova core structure. We explore a potentialsolution to this problem by treating the carbon-oxygen (CO) core independentlyfrom the rest of the star. Using the implicit hydrodynamics code KEPLER, wehave computed an extensive grid of 3496 CO-core models from a diverse range ofinitial conditions, each evolved from carbon ignition until core-collapse. Thefinal core structure, and thus the explodability, varies non-monotonically anddepends sensitively on both the mass and initial composition of the CO-core.Although bare CO-cores are not perfect substitutes for cores embedded inmassive stars, our models compare well both with MESA and full hydrogenic andhelium star calculations. Our results can be used to infer the presupernovacore structures from population synthesis estimates of CO-core properties, thusto determine the final outcomes based on the results of modern neutrino-drivenexplosion simulations. A sample application is presented for a population ofType-IIb supernova progenitors. All of our models are available athttps://doi.org/10.5281/zenodo.3785377.

Towards a Realistic Explosion Landscape for Binary Population Synthesis