In this talk I will present our results on environmental secular evolution processes that affect satellite galaxies as they enter their hosts.
Our approaches consist of global statistical analysis of satellites, and the modelling of detailed observations. For the latter approach we study distant gas rich dwarf satellites like Leo T and Phoenix, which are entering the Milky Way. Both satellites present non-equilibrium offsets between their gaseous and stellar distributions, with Leo T also showing an offset between its younger and older stellar populations. Using hydrodynamical simulations that include the Milky Way coronal wind, we find that cored dark matter density models can better reproduce the estimated timescales of the offsets in Leo T.
From the global approach we present our latest analysis of the Milky Way and the Andromeda satellite galaxies, finding a transition radius at R*~0.4-0.6Rvir that delimits an inner satellite population with stellar densities that correlate with the tidal field of their hosts, and an outer less processed population. Furthermore, we find that this transition radius is also present in satellites of the Fornax and Virgo galaxy clusters, as well as in their cosmological galaxy simulation counterparts.
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