Formation and Evolution of
Galaxy Clusters Across Cosmic Time

Scientific consensus has emerged around the influence of baryonic processes in protocluster evolution. Still, many questions remain open about the exact way and the extent to which energetic processes, like star formation, stellar feedback and AGN feedback, influence the evolution of galaxies and galaxy (proto)clusters. We used a new set of cosmological hydrodynamical zoom simulations, called COMPASS, containing 72 galaxy clusters with final masses M200 > 1e14 Msun to explore the effects of such processes in the evolution of protoclusters of galaxies. We found that independent of the subgrid physics implemented, the integrated SFR at high redshifts of simulated protoclusters with masses M200 ~ 1.5 x 1e13 Msun (at z ~ 4.3) is approximately 4 times lower than the ones observed for protoclusters of similar total mass and integrated gas mass, such as SPT2349-56 (M200 ~ 2 x 1e13 Msun at z ~ 4.3). Moreover, observed protocluster galaxies at high redshift show strong starburst, that are not reproduced in simulations. Possible reasons for this discrepancy in the SFR are either a numerical artifact related to resolution or the existence of physical processes responsible for triggering bursty star formation in protocluster galaxies, not yet modeled in current simulations.