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The next generation ground-based gravitational wave interferometers willpossibly observe mergers of binary black holes (BBHs) and binary neutron stars(BNSs) to redshift $z\gtrsim{}10$ and $z\gtrsim{}2$, respectively. Here, wecharacterize the properties of merging BBHs, BNSs and neutron star-black holebinaries across cosmic time, by means of population-synthesis simulationscombined with the Illustris cosmological simulation. We find that the mass ofmerging compact objects does not depend (or depends very mildly) on the mergerredshift. Even the mass distribution of black holes depends only mildly onredshift, because BBHs originating from metal-poor progenitors($Z\leq{}4\times{}10^{-3}$) dominate the entire population of merging BBHsacross cosmic time. For a common-envelope efficiency $\alpha{}\ge{}3$, the maindifference between the mass distribution of BBHs merging in the last Gyr andthat of BBHs merging more than 11 Gyr ago is that there is an excess of heavymerging black holes ($20-35$ M$_\odot$) in the last Gyr. This excess isexplained by the longer delay time of massive BBHs.

The properties of merging black holes and neutron stars across cosmic time