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Flux limited X-ray surveys of galaxy clusters show that clusters come in tworoughly equally proportioned varieties: "cool core" clusters (CCs) andnon-"cool core" clusters (NCCs). In previous work, we have demonstrated usingcosmological $N$-body + Eulerian hydrodynamic simulations that NCCs are oftenconsistent with early major mergers events that destroy embryonic CCs. In thispaper we extend those results and conduct a series of simulationsusingdifferent methods of gas cooling, and of energy and metal feedback fromsupernovae, where we attempt to produce a population of clusters with realisticcentral cooling times, entropies, and temperatures. We find that the use ofmetallicity-dependent gas cooling is essential to prevent early overcooling,andthat adjusting the amount of energy and metal feedback can have a significantimpact on observable X-ray quantities of the gas. We are able to produceclusters with more realistic central observable quantities than have previouslybeen attained. However, there are still significant discrepancies between thesimulated clusters and observations, which indicates that a different approachto simulating galaxies in clusters is needed. We conclude by looking towards apromising subgrid method of modeling galaxy feedback in clusters which may helpto ameliorate the discrepancies between simulations and observations.

astrophysical journal/the astrophysical journal

On The Road To More Realistic Galaxy Cluster Simulations: The Effects of  Radiative Cooling and Thermal Feedback Prescriptions on the Observational  Properties of Simulated Galaxy Clusters