http://arxiv.org/abs/2305.09372
The superposition of many astrophysical gravitational waves (GW) signals below typical detection thresholds baths detectors in a stochastic gravitational wave background (SGWB). In this work we present a Fourier space approach to compute the frequency-domain distribution of stochastic gravitational wave backgrounds produced by discrete sources. The expressions for the moment generating function and the distribution of observed (discrete) Fourier modes are provided. The results are then applied to the SGWB originating from the mergers of compact stellar remnants (black holes and neutron stars) in the Universe, which are found to exhibit a $-4$ power-law tail. This tail is verified in the signal-to-noise ratio distribution of GWTC events. Furthermore, the extent to which the subtraction of bright (loud) mergers gaussianizes the resulting confusion noise of unresolved sources is illustrated. The power-law asymptotic tail for the SGWB, and an exponentially decaying tail in the case of the confusion background, are also derived analytically. Our results generalize to any background of gravitational waves emanating from discrete sources.
Y. Ginat, R. Reischke, I. Rapoport, et. al.
Wed, 17 May 23
58/67
Comments: Comments welcome