Evolution of the Thermodynamic Properties of Clusters of Galaxies out to
  Redshift of 1.8
  The thermodynamic properties of the hot plasma in galaxy clusters retains
information on the processes leading to the formation and evolution of the gas
in their deep, dark matter potential wells. These processes are dictated not
only by gravity but also by gas physics, e.g. AGN feedback and turbulence. In
this work, we study the thermodynamic properties, e.g. density, temperature,
pressure, and entropy, of the most massive and the most distant ($z > 1.2$)
SPT-selected clusters, and compare them with those of the nearby clusters
($z<0.1$) to constrain their evolution as a function of time and radius. We
find that thermodynamic properties in the outskirts of high redshift clusters
are remarkably similar to the low redshift clusters, and their evolution
follows the prediction of the self-similar model. Their intrinsic scatter is
larger, indicating that the physical properties that lead to the formation and
virialization of cluster outskirts show evolving variance. On the other hand,
thermodynamic properties in the cluster cores deviates significantly from
self-similarity indicating that the processes that regulate the core are
already in place in these very high redshift clusters. This result is supported
by the unevolving physical scatter of all thermodynamic quantities in cluster
cores.
