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We present an analysis of the properties of the ICM in an extended set ofcosmological hydrodynamical simulations of galaxy clusters and groups performedwith the TreePM+SPH GADGET-3 code. Besides a set of non-radiative simulations,we carried out two sets of simulations including radiative cooling, starformation, metal enrichment and feedback from supernovae, one of which alsoaccounts for the effect of feedback from AGN resulting from gas accretion ontosuper-massive black holes. These simulations are analysed with the aim ofstudying the relative role played by SN and AGN feedback on the generalproperties of the diffuse hot baryons in galaxy clusters and groups: scalingrelations, temperature, entropy and pressure radial profiles, and ICM chemicalenrichment. We find that simulations including AGN feedback produce scalingrelations that are in good agreement with X-ray observations at all massscales. However, our simulations are not able to account for the observeddiversity between CC and NCC clusters: unlike for observations, we find thattemperature and entropy profiles of relaxed and unrelaxed clusters are quitesimilar and resemble more the observed behaviour of NCC clusters. As for thepattern of metal enrichment, we find that an enhanced level of iron abundanceis produced by AGN feedback with respect to the case of purely SN feedback. Asa result, while simulations including AGN produce values of iron abundance ingroups in agreement with observations, they over-enrich the ICM in massiveclusters. The efficiency of AGN feedback in displacing enriched gas from halosinto the inter-galactic medium at high redshift also creates a widespreadenrichment in the outskirts of clusters and produces profiles of iron abundancewhose slope is in better agreement with observations.

On the role of AGN feedback on the thermal and chemodynamical properties of the hot intra-cluster medium