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As the sensitivity of current and future gravitational-wave detectorsimproves, it will become possible to measure the evolution of the binary blackhole merger rate with redshift. Here, we combine detailed fits tostate-of-the-art dynamical models of binary black hole formation in dense starclusters with a cosmological model of cluster formation across cosmic time. Wefind a typical merger rate of 14 $\rm{Gpc}^{-3} \rm{yr}^{-1}$ in the localuniverse, with a reasonable range of 4-18 $\rm{Gpc}^{-3} \rm{yr}^{-1}$,depending on the rate of cluster disruption and the cluster initial massfunction. This rate increases by a factor of 6 to redshift $z=2.7$ beforedeclining at higher redshifts. We compare the merger rate from binariesproduced in clusters to similar estimates from isolated binaries and triples ingalactic fields, and discuss various ways that these different formationchannels could add up to the current merger rate observed by LIGO/Virgo.

Redshift Evolution of the Black Hole Merger Rate from Globular Clusters