Radial and isoradial thermal structure of the intra-cluster medium from hydrodynamical N-body simulations of galaxy clusters

Clusters of galaxies form by gravitational collapse and accretion of subgroups under the influence of gravity. Analyses of the gas thermal structure within clusters obtained from X-ray observations reveals us the underlying dark matter structure and dynamics, provided that the baryonic physics is well understood. We use hydrodynamical N-body simulations of galaxy clusters evolving in cosmological context, in order to investigate the influence on gas cooling, heating conduction and star formation on the thermal structure of the intra-cluster medium (ICM), as observed from mock X-ray spectral-mapping analyses. In complement to radial analyses of gas temperature profiles, we analyse the isoradial thermal structure of the ICM through wavelet analyses in elliptical coordinates. We show from tests performed on mock XMM-Newton observations, that this scheme is particularly discriminant to constrain the gas physics assumed in numerical simulations from cluster sample analyses.