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The stochastic gravitational-wave backgrounds (SGWBs) for current detectorsare dominated by binary black-hole (BBH) and binary neutron-star (BNS)coalescences. The sensitivity of current networks of gravitational-wave (GW)detectors allows only a small fraction of BBHs and BNSs to be resolved andsubtracted, but previous work indicated that the situation should significantlyimprove with next-generation (XG) observatories. We revisit these conclusionsby taking into account waveform-modeling uncertainties, updated astrophysicalmodels, and (crucially) the full set of parameters that must be estimated toremove the resolved sources. Compared to previous studies, we find that theresidual background from BBHs and BNSs is large even with XG detector networks.New data analysis methods will thus be required to observe the SGWB from cosmicsupernovae or contributions from early-Universe phenomena like cosmic strings,stiff post-inflation fluids, or axion inflation.

Compact Binary Foreground Subtraction in Next-Generation Ground-Based Observatories