|Title||Testing the LCDM paradigm with the mass distribution and abundance of massive galaxy clusters out to z=1.4|
Multi-wavelength studies of galaxy clusters across cosmic time are an invaluable resource for understanding the formation of structure in its baryonic and dark matter components, as well as the underlying cosmological model. The dark matter mass distribution within galaxy clusters, over a wide range of radial scales and redshift baseline, provide a powerful test of the currently favoured LCDM cosmological scenario. I will illustrate how space and ground-based facilities enable nowadays accurate measurements of dark matter density profiles of massive clusters, using a combination of lensing, X-ray and dynamical methods, out to to z1, providing accurate (10%) measurements of cluster masses out to z=1.4. This can be used to challenge the standard LCDM model by setting stringent limits on the space density of the most massive distant clusters in the Universe. Prospects from on-going and future cluster surveys will also be discussed.