Reproducing the entropy structure in galaxy groups

We carry out a comparison between observations and hydrodynamic simulations of entropy profiles of groups and clusters of galaxies. We use the Tree+SPH GADGET code to simulate four halos of sizes in the $M_{500}=1.0{-}16\times10^{13}~h^{-1}\,M_{\odot}$ range, corresponding to poor groups up to Virgo-like clusters. We concentrate on the effect of introducing radiative cooling, star formation, and a variety of non-gravitational heating schemes on the entropy structure and the stellar fraction. We show that all the simulations result in a correct entropy profile for the Virgo-like cluster. With the heating energy budget of ~0.7 keV/particle injected at $z_{\rm h}=3$, we are also able to reproduce the entropy profiles of groups. We obtain the flat entropy cores as a combined effect of preheating and cooling, while we achieve the high entropy at outskirts by preheating. The resulting baryon fraction locked into stars is in the 25–30% range, compared to 35–40% in the case of no preheating. Heating at higher redshift, $z_{\rm h}=9$, strongly delays the star-formation, but fails to produce a sufficiently high specific entropy