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-generation stochastic searches.
Statistical properties of astrophysical gravitational-wave backgrounds
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abstract
We investigate how a stochastic gravitational wave background, produced from a discrete set of astrophysical sources, differs from an idealised model consisting of an isotropic, unpolarised, and Gaussian background. We focus, in particular, on the different signatures produced from these two cases, as observed in a cross-correlation search. We show that averaged over many realisations of an astrophysical background, the cross-correlation measurement of an astrophysical background is identical to that of an idealised background. However, any one realisation of an astrophysical background can produce a different signature. Using a model consisting of an ensemble of binary neutron star coalescences, we quantify the typical difference between the signal from individual realisations of the astrophysical background and the idealised case. For advanced detectors, we find that, using a cross-correlation analysis, astrophysical backgrounds from many discrete sources are probably indistinguishable from an idealised background.
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All You Need is not $\Omega_\mathrm{gw}$: Beyond the Mean of the Cross-Correlation Estimator when Searching for an Astrophysical Gravitational-Wave Background
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-generation stochastic searches.