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We make projections for measuring the black hole birth rate from the diffusesupernova neutrino background (DSNB) by future neutrino experiments, andconstrain the black hole merger fraction $\epsilon$, when combined withinformation on the black hole merger rate from gravitational wave experimentssuch as LIGO. The DSNB originates from neutrinos emitted by all the supernovaein the Universe, and is expected to be made up of two components: neutrinosfrom neutron-star-forming supernovae, and a sub-dominant component at higherenergies from black-hole-forming "unnovae". We perform a Markov Chain MonteCarlo analysis of simulated data of the DSNB in an experiment similar toHyper-Kamiokande, focusing on this second component. Since all knowledge of theneutrino emission from unnovae comes from simulations of collapsing stars, wechoose two sets of priors: one where the unnovae are well-understood and onewhere their neutrino emission is poorly known. By combining the black holebirth rate from the DSNB with projected measurements of the black hole mergerrate from LIGO, we show that the fraction of black holes which lead to binarymergers observed today $\epsilon$ could be constrained to be within the range$2 \cdot 10^{-4} \leq \epsilon \leq 3 \cdot 10^{-2}$ at $3 \sigma$ confidence,after ten years of running an experiment like Hyper-Kamiokande.

A "nu" look at gravitational waves: The black hole birth rate from neutrinos combined with the merger rate from LIGO