The Dipole of the Astrophysical Gravitational-Wave Background

Abstract

One of the main pillars of the ΛCDM model is the Cosmological Principle, which states that our Universe is statistically isotropic and homogeneous on large scales. Here we test this hypothesis using the Astrophysical Gravitational Wave Background (AGWB) expected to be measured by the Einstein Telescope-Cosmic Explorer network; in particular we perform a numerical computation of the AGWB dipole, evaluating the intrinsic contribution due to clustering and the kinematic effect induced by the observer motion. We apply a component separation technique in the GW context to disentangle the kinematic dipole, the intrinsic dipole and the shot noise (SN), based on the observation of the AGWB at different frequencies. We show how this technique can also be implemented in matched-filtering to minimize the covariance which accounts for both instrumental noise and SN. Since GW detectors are essentially full-sky, we expect that this powerful tool can help in testing the isotropy of our Universe in the next future.

42 pages, 5 figures; matches the version published in JCAP

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Cited by in corpus (12)

• Science with the Einstein Telescope: a comparison of different designs
• Cosmology with the Laser Interferometer Space Antenna
• The Science of the Einstein Telescope
• Circular Polarization of the Astrophysical Gravitational Wave Background
• Measuring kinematic anisotropies with pulsar timing arrays
• Probing parity-odd bispectra with anisotropies of GW $V$ modes
• Boltzmann equations for astrophysical Stochastic Gravitational Wave Backgrounds scattering off of massive objects
• On the response of the Einstein Telescope to Doppler anisotropies
• Astrometry meets Pulsar Timing Arrays: Synergies for Gravitational Wave Detection
• Unraveling the CMB lack-of-correlation anomaly with the cosmological gravitational wave background
• Unbiased estimation of gravitational-wave anisotropies from noisy data
• Galaxy number-count dipole and superhorizon fluctuations