Towards More Realistic Simulations of Galaxy Clusters: Shocks and Radio Relics

Numerical simulations of galaxy clusters have advanced over time to the point where a large number of physical processes can be accurately captured. However, in order to accurately constrain the role of each process in cluster evolution, we must carefully compare with observational data. While single object comparisons are very useful, large statistical studies are needed to simultaneously study many parameters that go into each no thermal physical process. We do so here by studying large, extended radio features in the vicinity of galaxy clusters that are known as radio relics. In particular, we examine the ability for merger and large-scale structure shocks to accelerate electrons that emit via synchrotron radiation at radio wavelengths. By tracing the shocks in AMR/N-body cosmological simulations and using models of both the magnetic field and particle acceleration efficiency, we produce synthetic radio maps of a large sample of galaxy clusters. We then present a radio luminosity function and radio luminosity-cluster mass scaling relationships.