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Recently, Suzaku has produced temperature and entropy profiles, along withprofiles of gas density, gas fraction, and mass, for multiple galaxy clustersout to ~r_200 (~= virial radius). In this paper, we compare these novel X-rayobservations with results from N-body + hydrodynamic adaptive mesh refinementcosmological simulations using the Enzo code. There is excellent agreement inthe temperature, density, and entropy profiles between a sample of 27 mostlysubstructure-free massive clusters in the simulated volume and the observedclusters. This supports our previous contention that clusters have "universal"outer temperature profiles. Furthermore, it appears that the simplest adiabaticgas physics used in these Enzo simulations is adequate to model the outerregions of these clusters without other mechanisms (e.g., non-gravitationalheating, cooling, magnetic fields, or cosmic rays). However, the outskirts ofthese clusters are not in hydrostatic equilibrium. There is significant bulkflow and turbulence in the outer intracluster medium created by accretion fromfilaments. Thus, the gas is not fully supported by thermal pressure. Theimplications for mass estimation from X-ray data are discussed.

Galaxy Clusters at the Edge: Temperature, Entropy, and Gas Dynamics at the Virial Radius