Fueling and feedback mechanisms at the nodes of the cosmic web

The environment plays a key role in shaping how galaxies form and evolve. Galaxies in dense nodes of the cosmic web are thought to grow and quench earlier, and faster and become more massive than those in the field. To understand the physical drivers of this environmental effect, we must probe the most crowded regions of the Universe at the epoch when growth was at its peak and the transition to quiescence was triggered, around 10 billion years ago (z 2). This period saw the downturn of the cosmic star-formation and black-hole accretion histories, the quenching and morphological transformation of massive galaxies, and the virialisation of the first clusters. Several processes might be at play: stellar and AGN feedback, reduced gas accretion, disk instabilities, morphological quenching, interactions, and ram-pressure stripping. The ELT/SHARP instrument, with its sensitivity, spectral resolution, wavelength coverage, and multiplexing capabilities over a wide field, is ideally suited to study these mechanisms by targeting multiple members of dense structures simultaneously. Cluster and protocluster cores at z 2 span roughly 1 arcmin and host about ten massive (Mstar > 10 10.5 Msun) galaxies. VESPER can deliver spatially resolved gas and stellar kinematics, map recent and past star formation, identify companions, inflows, outflows, shocks, and AGN activity for the most massive core members. With 80 hr of VESPER time, we can obtain this type of data for about 60 galaxies selected from the densest regions of five clusters at 1.5 < z < 1.7 and five protoclusters at 2 < z < 2.5 spanning the evolutionary phases of maximal growth and rapid decline. Such a sample would permit to trace the evolution from protoclusters to virialised clusters and identify the environmental processes responsible for their rapid transformations.