http://arxiv.org/abs/1910.08353
We investigate the correlation between the distribution of galaxies and the predicted gravitational-wave background of astrophysical origin. We show that the large angular scale anisotropies of this background are dominated by nearby non-linear structure, which depends on the notoriously hard to model galaxy power spectrum at small scales. In contrast, we report that the cross-correlation of this signal with galaxy catalogues depends only on linear scales and can be used to constrain the average contribution to the gravitational-wave background as a function of time. Using mock data based on a simplified model, we explore the effects of galaxy bias and the matter abundance on these constraints. Our results suggest that the gravitational-wave background when combined with near-future galaxy surveys, is a powerful probe for both gravitational-wave merger physics and cosmology.
G. Cañas-Herrera, O. Contigiani and V. Vardanyan
Mon, 21 Oct 19
11/54
Comments: 9 pages, 5 figures
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