We present a new, state-of-the-art computation of the diffuse supernova neutrino background (DSNB), where we use neutrino spectra from multidimensional, multisecond core-collapse supernova simulations—including both neutron-star and black-hole forming collapses—and binary evolution effects from modern population synthesis codes. Large sets of numerical results are processed and connected in a consistent manner, using two key quantities, the mass of the star’s carbon-oxygen (CO) core at an advanced precollapse stage—which depends on binary evolution effects—and the compactness parameter, which is the main descriptor of the postcollapse neutrino emission. The method enables us to model the neutrino emission of a very diverse, binary-affected population of stars, which cannot unambiguously be mapped in detail by existing core-collapse simulations. We find that including black hole-forming collapses enhances the DSNB by up to $\sim 50\%$ at $E\gtrsim 30–40\mathrm{MeV}$. Binary evolution effects can change the total rate of collapses, and generate a subpopulation of high core mass stars that are stronger neutrino emitters. However, the net effect on the DSNB is moderate—up to $\sim 15\%$ increase in flux—due to the rarity of these super-massive cores and to the relatively modest dependence of the neutrino emission on the CO core mass. The methodology presented here is suitable for extensions and generalizations, and therefore it lays the foundation for modern treatments of the DSNB.

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• Cosmic rays & astroparticles
• Novae & supernovae
• Binary stars
• Neutrinos