Within the framework of the hierarchical growth of large-scale structures in the universe, mass is assembled inhomogeneously along walls and filaments which forms a "cosmic web", galaxy clusters are formed at the intersections of such filaments. Galaxy protoclusters (galaxy clusters in formation) are expected to contribute significantly to the star-formation rate density in the distant...
Protoclusters of galaxies are non-virialized overdense structures in the distant universe which collapse into galaxy clusters with masses log(M/M$_*$) > 14 by redshift 0. They are the precursors of present-day massive galaxy clusters. The evolution of galaxies in these overdense structures depart from the one observed in the field. On the other hand, the assembly and gravitational collapse of...
Deep observations of galaxy clusters reveal a diffuse light component, the intracluster light (ICL), which contains a record of all the processes that the system has undergone and provides information about the mechanisms that have shaped the population within the cluster.
In this talk I will present the most comprehensive study to date of the ICL of the Perseus cluster, taking advantage of...
Weak lensing effect is a sensitive probe for galaxy cluster detection, that needs of a large enough number of background galaxies observed to be profitable.
Euclid will conduct a 14,500 square degree weak lensing survey, measuring the shapes of billions of galaxies and opening a unique window for detecting galaxy clusters in this way.
The task of coordinating the science within Euclid related...
