╨╧рб▒с>■ %'■ $ ье┴Ё┐ьddddSxSxЎ lввв╢┬я·щ ┌╬The direct detections of Gravitational Waves (GWs) by the Advanced LIGO and Advanced Virgo interferometers have opened a new exciting era of astronomy. Aside the current detections associated with individual loud events, one expects a superposition of many coincident unresolved events leading to a stochastic GW background (SGWB) of an astrophysical or cosmological origin. This stochastic background is predicted to be detected once the LIGO and Virgo interferometers reach design sensitivity.а In this talk, I will discuss how the anisotropic distribution of sources and the inhomogeneous geometry of the intervening spacetime can induce anisotropies in the SGWB. After presenting a general formalism analogous to the one used to study cosmic microwave background temperature anisotropies I will consider a SGWB of cosmological origin (cosmic strings), or astrophysical origin (compact binary coalescences).аI will show that in both cases, while the SGWB monopole is sensitive to the particular model one uses, the anisotropic angular power spectrum is basically insensitive to the cosmic string model or the nature of binary black holes population. Finally, I will discuss the noise in the anisotropies of the astrophysical GW background sourced by the finite sampling of both the galaxy distribution and the compact binary coalescence event rate, concluding that the induced scale-invariant bias term in the angular power spectrum will dominate the true cosmological power spectrum in any reasonable observing time.а
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