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Recently, rapid observational and theoretical progress has established thatblack holes (BHs) play a decisive role in the formation and evolution ofindividual galaxies as well as galaxy groups and clusters. In particular, thereis compelling evidence that BHs vigorously interact with their surroundings inthe central regions of galaxy clusters, indicating that any realistic model ofcluster formation needs to account for these processes. This is also suggestedby the failure of previous generations of hydrodynamical simulations without BHphysics to simultaneously account for the paucity of strong cooling flows inclusters, the slope and amplitude of the observed cluster scaling relations,and the high-luminosity cut-off of central cluster galaxies. Here we usehigh-resolution cosmological simulations of a large cluster and group sample tostudy how BHs affect their host systems. We focus on two specific properties,the halo gas fraction and the X-ray luminosity-temperature scaling relation,both of which are notoriously difficult to reproduce in self-consistenthydrodynamical simulations. We show that BH feedback can solve both of theseissues, bringing them in excellent agreement with observations, withoutalluding to the `cooling only' solution that produces unphysically brightcentral galaxies. By comparing a large sample of simulated AGN-heated clusterswith observations, our new simulation technique should make it possible toreliably calibrate observational biases in cluster surveys, thereby enablingvarious high-precision cosmological studies of the dark matter and dark energycontent of the universe.

Simulations of AGN feedback in galaxy clusters and groups: impact on gas fractions and the Lx-T scaling relation