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The next generation of ground-based gravitational-wave detectors will lookmuch deeper into the Universe and have unprecedented sensitivities andlow-frequency capabilities. Especially alluring is the possibility of detectingan early-Universe cosmological stochastic background that could provideimportant insights into the beginnings of our Universe and fundamental physicsat extremely high energies. However, even if next-generation detectors aresensitive to cosmological stochastic backgrounds, they will be masked by moredominant astrophysical backgrounds, namely the residual background from theimperfect subtraction of resolvable compact binary coalescences (CBCs) as wellas the CBC background from individually unresolvable CBCs. Using our latestknowledge of masses, rates, and delay time distributions, we present adata-driven estimate of the unresolvable CBC background that will be seen bynext-generation detectors. Accounting for statistical and systematic errors,this estimate quantifies an important piece in the CBC noise budget fornext-generation detectors and can help inform detector design and subtractionalgorithms. We compare our results with predictions for backgrounds fromseveral cosmological sources in the literature, finding that the unresolvablebackground will likely be a significant impediment for many models. Thismotivates the need for simultaneous inference methods or other statisticaltechniques to detect early-Universe cosmological backgrounds.

The unresolved stochastic background from compact binary mergers detectable by next-generation ground-based gravitational-wave observatories