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We analyze the basic properties of Brightest Cluster Galaxies (BCGs) producedby state of the art cosmological zoom-in hydrodynamical simulations. Thesesimulations have been run with different sub-grid physics included. Here wefocus on the results obtained with and without the inclusion of theprescriptions for supermassive black hole (SMBH) growth and of the ensuingActive Galactic Nuclei (AGN) feedback. The latter process goes in the rightdirection of decreasing significantly the overall formation of stars. However,BCGs end up still containing too much stellar mass, a problem that increaseswith halo mass, and having an unsatisfactory structure. This is in the sensethat their effective radii are too large, and that their density profilesfeature a flattening on scales much larger than observed. We also find that ourmodel of thermal AGN feedback has very little effect on the stellar velocitydispersions, which turn out to be very large. Taken together, these problems,which to some extent can be recognized also in other numerical studiestypically dealing with smaller halo masses, indicate that on one hand presentday sub-resolution models of AGN feedback are not effective enough indiminishing the global formation of stars in the most massive galaxies, but onthe other hand they are relatively too effective in their centers. It is likelythat a form of feedback generating large scale gas outflows from BCGsprecursors, and a more widespread effect over the galaxy volume, can alleviatethese difficulties.

Brightest cluster galaxies in cosmological simulations: achievements and limitations of AGN feedback models