Special Location: NS2 2201
During the last decade observations of galaxies across cosmic times coupled with cosmological simulations have provided an increasingly clear description of galaxy evolution.
In particular we have a fairly detailed phenomenological picture of how galaxies transition from star forming to passive (or quenched) as a function of their internal properties (e.g. stellar mass) and the external environment (e.g. local density). In the Local Universe, the recent deployment of large FoV integral field spectrographs opened up exciting new possibilities to perform detailed investigations of objects undergoing environmental quenching. I will present the most recent results we obtained from VLT/MUSE spectroscopy of galaxies affected by gas stripping in local massive clusters of galaxies.
These detailed studies of small samples of galaxies are complemented by statistical studies of the full galaxy population. By exploiting the highly complete coverage of grism and spectroscopic redshifts from the 3D-HST survey, I derived the local environment for a deep and complete sample of galaxies in the five CANDELS/3D-HST deep fields at 0.5 < z < 2.5. By combining observational data and models I will present our latest results on the environmental quenching of satellite galaxies up to z ~ 2.5. I will discuss the quenching timescales due to environmental effects as a function of redshift, stellar mass and parent halo mass and what we can learn about the quenching mechanisms and gas content of the satellites at the epoch of infall.