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The occurrence of dual active galactic nuclei (AGN) on scales of a few tensof kpc can be used to study merger-induced accretion on massive black holes(MBHs) and to derive clues on MBH mergers, using dual AGN as a parentpopulation of precursors. We investigate the properties of dual AGN in thecosmological simulation Horizon-AGN. We create catalogs of dual AGN selectedwith distance and luminosity criteria, plus sub-catalogs where further masscuts are applied. We divide the sample into dual AGN hosted in differentgalaxies, on the way to a merger, and into those hosted in one galaxy, afterthe galaxy merger has happened. We find that the relation between MBH andgalaxy mass is similar to that of general AGN population and we compare theproperties of dual AGN also with a control sample, discussing differences andsimilarities in masses and Eddington ratios. The typical mass ratio of galaxymergers associated to dual AGN is 0.2, with mass loss in the smaller galaxydecreasing the mass ratio as the merger progresses. Between 30 and 80 per centof dual AGN with separations between 4 and 30~kpc can be matched to an ensuingMBH merger. The dual AGN fraction increases with redshift and with separationthreshold, although above 50~kpc the increase of multiple AGN limits that ofduals. Multiple AGN are generally associated with massive halos, and mass lossof satellites shapes the galaxy-halo relation.

Dual AGN in the Horizon-AGN simulation and their link to galaxy and massive black hole mergers, with an excursus on multiple AGN