dynamical substructure, and ICM properties. The different quantifications of the environment will allow us to disentangle the effects of local and large-scale density, cluster and group merging, dynamical state and mass of the host system on the properties of galaxies in different ranges of mass.

Recent studies investigated the effects of the local and large-scale environment on galaxy evolution, mainly considering groups of galaxies. Some of these works defined the environment through the luminosity-density only [e.g. @LTH12], or associate galaxy groups to a large-scale environment identified by a smoothed luminosity field [e.g. @LLY13], or are limited to massive galaxies [e.g. @CSC13]. Therefore, although there is a general agreement that the group environment is important for the evolution of the group members, a study of global and internal properties of galaxy population in groups and, in general, in different structures dynamically bound in a supercluster is still lacking. For instance, @RMB12 found that both local (distance from the centre) and global (mass) group environments play a role in quenching star formation, while @Ziparo14 show that global group-scale mechanisms linked to the presence of a hot gas halo are dominant in quenching SF in group galaxies rather than purely density related processes.

