It is often assumed that the hot intergalactic medium (IGM) dominating the baryon content of the largest objects in the Universe, such as clusters of galaxies, is ideal gas. However, the hot IGM is a plasma permeated by weak, tangled magnetic fields and as such its microphysics remains untreatable in a purely theoretical way. The lack of knowledge of the microphysical properties of the hot IGM, which determine its thermal conductivity and viscosity, is a missing key ingredient in galaxy formation models. This limits our understanding of how the energy from supernovae, accreting black holes, and merger shocks couples with the hot diffuse gas. The student will analyse X-ray, radio and SZ data of dynamically active clusters in order to gain a deeper understanding into the physical processes controlling the growth and evolution of these systems."