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We analyse the demographics of black holes (BHs) in the large-volumecosmological hydrodynamical simulation Horizon-AGN. This simulationstatistically models how much gas is accreted onto BHs, traces the energydeposited into their environment and, consequently, the back-reaction of theambient medium on BH growth. The synthetic BHs reproduce a variety ofobservational constraints such as the redshift evolution of the BH mass densityand the mass function. Strong self-regulation via AGN feedback, weak supernovafeedback, and unresolved internal processes result in a tight BH-galaxy masscorrelation. Starting at z~2, tidal stripping creates a small population of BHsover-massive with respect to the halo. The fraction of galaxies hosting acentral BH or an AGN increases with stellar mass. The AGN fraction agreesbetter with multi-wavelength studies, than single-wavelength ones, unlessobscuration is taken into account. The most massive halos present BHmultiplicity, with additional BHs gained by ongoing or past mergers. In somecases, both a central and an off-centre AGN shine concurrently, producing adual AGN. This dual AGN population dwindles with decreasing redshift, as foundin observations. Specific accretion rate and Eddington ratio distributions arein good agreement with observational estimates. The BH population is dominatedin turn by fast, slow, and very slow accretors, with transitions occurring atz=3 and z=2 respectively.

The cosmic evolution of massive black holes in the Horizon-AGN simulation