Jesús Falcón-Barroso

Abstract The hierarchical model of galaxy evolution suggests that mergers have a substantial impact on the intricate processes that drive stellar assembly within a galaxy. However, accurately measuring the contribution of accretion to a galaxy’s total stellar mass and its balance with in situ star formation poses a persistent challenge, as it is neither directly observable nor easily inferred from observational properties.

Abstract In the standard cosmological model, the assembly of galaxies is primarily driven by the growth of their host dark matter halos. At the centre of these halos, however, baryonic processes take over, leading to the plethora of observed galaxy properties. The coupling between baryonic and dark matter physics is central to our understanding of galaxies, and yet, it remains a challenge for theoretical models and observations.

Abstract Galaxies in the Universe are distributed in a web-like structure characterized by different large-scale environments: dense clusters, elongated filaments, sheetlike walls and under-dense regions, called voids1,2,3,4,5. The low density in voids is expected to affect the properties of their galaxies.