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Dipole Anisotropy in Gravitational Wave Source Distribution
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Our local motion with respect to the cosmic frame of rest is believed to be dominantly responsible for the observed dipole anisotropy in the Cosmic Microwave Background Radiation (CMBR). We study the effect of this motion on the sky distribution of gravitational wave (GW) sources. We determine the resulting dipole anisotropy in GW source number counts, mass weighted number counts, which we refer to as mass intensity, and mean mass per source. The mass M dependence of the number density n(M) distribution of BBH is taken directly from the data. We also test the anisotropy in the observable mean mass per source along the direction of the CMB dipole. The current data sample is relatively small and consistent with isotropy. The number of sources required for this test is likely to become available in the near future.
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Measuring the cosmic dipole with golden dark sirens in the era of next-generation ground-based gravitational wave detectors
Golden dark sirens from next-generation gravitational-wave networks could constrain the cosmic dipole amplitude to about 10^-3 jointly with H0 and to about 10^-4 if H0 is fixed.
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