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The two dimensional structure of hot gas in galaxy clusters containsinformation about the hydrodynamical state of the cluster, which can be used tounderstand the origin of scatter in the thermodynamical properties of the gas,and to improve the use of clusters to probe cosmology. Using a set ofhydrodynamical simulations, we provide a comparison between various mapscurrently employed in the X-ray analysis of merging clusters and those clustermaps anticipated from forthcoming observations of the thermalSunyaev-Zel'dovich effect. We show the following: 1) an X-ray pseudo-pressure,defined as square root of the soft band X-ray image times the temperature mapis a good proxy for the SZ map; 2) we find that clumpiness is the main reasonfor deviation between X-ray pseudo-pressure and SZ maps; 3) the level ofclumpiness can be well characterized by X-ray pseudo-entropy maps. 4) Wedescribe the frequency of deviation in various maps of clusters as a functionof the amplitude of the deviation. This enables both a comparison toobservations and a comparison to effects of introduction of complex physicalprocesses into simulation.

Hydrodynamic simulations of correlation and scatter in galaxy cluster maps