The structural and scaling properties of galaxy clusters observed by XMM

In the simplest, purely gravitational, models of structure formation, galaxy clusters constitute a homologous family. Clusters are self-similar in shape and predictable scaling laws relate each physical property to the cluster total mass and redshift. How the structural and scaling properties of the observed cluster population compare to these predictions gives us insight into the formation of clusters and the internal physics which governs their evolution. I will discuss recent XMM results on the temperature and mass profiles of hot nearby clusters with particular emphasis on the distribution at large scale. I will also present new observations of MKW9 and A1983, two cool nearby clusters, and first results of the XMM follow-up of distant (z>0.3) clusters detected serendipitously with ROSAT (SHARC sample).