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

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arxiv 2209.01221 v1 pith:GIYJXAIO submitted 2022-09-02 gr-qc astro-ph.HEhep-ph

Bei Zhou , Luca Reali , Emanuele Berti , Mesut Çal{i}şkan , Cyril Creque-Sarbinowski , Marc Kamionkowski , B. S. Sathyaprakash This is my paper · ORCID
classification gr-qcastro-ph.HEhep-ph
keywords binarybbhsbnsscosmiccurrentdetectorsgravitational-wavenetworks
verification ladder T0 review T1 audit T2 compute T3 formal
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The stochastic gravitational-wave backgrounds (SGWBs) for current detectors are 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 and subtracted, but previous work indicated that the situation should significantly improve with next-generation (XG) observatories. We revisit these conclusions by taking into account waveform-modeling uncertainties, updated astrophysical models, and (crucially) the full set of parameters that must be estimated to remove the resolved sources. Compared to previous studies, we find that the residual 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 cosmic supernovae or contributions from early-Universe phenomena like cosmic strings, stiff post-inflation fluids, or axion inflation.

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  1. All You Need is not $\Omega_\mathrm{gw}$: Beyond the Mean of the Cross-Correlation Estimator when Searching for an Astrophysical Gravitational-Wave Background

    gr-qc 2026-08 conditional novelty 6.0 of 10

    For a two-detector Cosmic Explorer network, the cross-correlation estimator of the binary black hole background has skewness 0.31 and excess kurtosis 1.3 at 20 Hz, a non-Gaussianity that will matter for next-generatio...

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