Simulating the effect of AGN feedback on the metal enrichment of galaxy clusters

We present a study of the effect of AGN feedback on metal enrichment and thermal properties of the intracluster medium (ICM) in hydrodynamical simulations. The cosmological simulations are performed for a set of clusters using a version of the TreePM-SPH Gadget code that follows chemo-dynamical evolution by accounting for metal enrichment by different stellar populations. Besides runs not including any efficient form of energy feedback, we carry out simulations including: (i) kinetic feedback in the form of galactic winds triggered by supernova explosions; (ii) AGN feedback from gas accretion onto super-massive black holes (BHs); (iii) AGN feedback in which a 'radio mode' is included. We find that AGN feedback is able to quench star formation in the brightest cluster galaxies at z<4 and provides correct temperature profiles in the central regions of galaxy groups. However, its effect is not sufficient to create cool cores in massive clusters. AGN feedback creates a widespread enrichment in the outskirts of clusters, thanks to its efficiency in displacing enriched gas from galactic halos to the inter-galactic medium at relatively high redshift. Iron abundance profiles are in better agreement with observations, with a more pristine enrichment of the ICM around and beyond the cluster virial regions. From the pattern of the relative abundances of Silicon and Iron, we conclude that a significant fraction of ICM enrichment in simulations is contributed by a diffuse population of intra-cluster stars. Our simulations also predict that profiles of Z_Si/Z_Fe abundance ratio do not increase at least out to 0.5 R_vir. Our results clearly show that different sources of energy feedback leave distinct imprints in the enrichment pattern of the ICM, that are more evident when looking at cluster external regions.