2019A&A...621A..41G

Context. The hot plasma in a galaxy cluster is expected to be heated to high temperatures through shocks and adiabatic compression. The thermodynamical properties of the gas encode information on the processes leading to the thermalization of the gas in the cluster's potential well and on non-gravitational processes such as gas cooling, AGN feedback, shocks, turbulence, bulk motions, cosmic rays and magnetic field.
Aims. In this work we present the radial profiles of the thermodynamic properties of the intracluster medium (ICM) out to the virial radius for a sample of 12 galaxy clusters selected from the Planck all-sky survey. We determine the universal profiles of gas density, temperature, pressure, and entropy over more than two decades in radius, from 0.01R₅₀₀ to 2R₅₀₀.
Methods. We exploited X-ray information from XMM-Newton and Sunyaev-Zel'dovich constraints from Planck to recover thermodynamic properties out to 2R₅₀₀. We provide average functional forms for the radial dependence of the main quantities and quantify the slope and intrinsic scatter of the population as a function of radius.
Results. We find that gas density and pressure profiles steepen steadily with radius, in excellent agreement with previous observational results. Entropy profiles beyond R₅₀₀ closely follow the predictions for the gravitational collapse of structures. The scatter in all thermodynamical quantities reaches a minimum in the range [0.2-0.8]R₅₀₀ and increases outward. Somewhat surprisingly, we find that pressure is substantially more scattered than temperature and density.
Conclusions. Our results indicate that once accreting substructures are properly excised, the properties of the ICM beyond the cooling region (R>0.3R₅₀₀) follow remarkably well the predictions of simple gravitational collapse and require few non-gravitational corrections.