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We investigate the coupled formation and evolution of galaxies and theirembedded supermassive black holes using state-of-the-art hydrodynamicsimulations of cosmological structure formation. For the first time, weself-consistently follow the dark matter dynamics, radiative gas cooling, starformation, as well as black hole growth and associated feedback processes,starting directly from initial conditions appropriate for the LambdaCDMcosmology. Our modeling of the black hole physics is based on an approach wehave developed in simulations of isolated galaxy mergers. Here we examine: (i)the predicted global history of black hole mass assembly (ii) the evolution ofthe local black hole-host mass correlations and (iii) the conditions that allowrapid growth of the first quasars, and the properties of their hosts anddescendants today. We find a total black hole mass density in good agreementwith observational estimates. The black hole accretion rate density peaks atlower redshift and evolves more strongly at high redshift than the starformation rate density, but the ratio of black hole to stellar mass densitiesshows only a moderate evolution at low redshifts. We find strong correlationsbetween black hole masses and properties of the stellar systems, agreeing wellwith the measured local M_BH-sigma and M_BH -M_* relationships, but alsosuggesting (dependent on the mass range) a weak evolution with redshift in thenormalization and the slope. Our simulations also produce massive black holesat high redshift, due to extended periods of exponential growth in regions thatcollapse early and exhibit strong gas inflows. These first supermassive BHsystems however are not necessarily the most massive ones today, since they areoften overtaken in growth by quasars that form later. (abridged)

Direct cosmological simulations of the growth of black holes and galaxies