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We investigate the isotropic and anisotropic components of the StochasticGravitational Wave Background (SGWB) originated from unresolved merging compactbinaries in galaxies. We base our analysis on an empirical approach to galacticastrophysics that allows to follow the evolution of individual systems. We thencharacterize the energy density of the SGWB as a tracer of the total matterdensity, in order to compute the angular power spectrum of anisotropies withthe Cosmic Linear Anisotropy Solving System (CLASS) public code in fullgenerality. We obtain predictions for the isotropic energy density and for theangular power spectrum of the SGWB anisotropies, and study the prospect fortheir observations with advanced Laser Interferometer Gravitational-Wave andVirgo Observatories and with the Einstein Telescope. We identify thecontributions coming from different type of sources (binary black holes, binaryneutron stars and black hole-neutron star) and from different redshifts. Weexamine in detail the spectral shape of the energy density for all types ofsources, comparing the results for the two detectors. We find that the powerspectrum of the SGWB anisotropies behaves like a power law on large angularscales and drops at small scales: we explain this behaviour in terms of theredshift distribution of sources that contribute most to the signal, and of thesensitivities of the two detectors. Finally, we simulate a high resolution fullsky map of the SGWB starting from the power spectra obtained with CLASS andincluding Poisson statistics and clustering properties.

Intensity and anisotropies of the stochastic Gravitational Wave background from merging compact binaries in galaxies