Context. The evolution of galaxies is influenced by many physical processes, which may vary depending on their environment.Aims. We combine Hubble Space Telescope (HST) and Multi-Unit Spectroscopic... Show moreContext. The evolution of galaxies is influenced by many physical processes, which may vary depending on their environment.Aims. We combine Hubble Space Telescope (HST) and Multi-Unit Spectroscopic Explorer (MUSE) data of galaxies at 0.25 less than or similar to z less than or similar to 1.5 to probe the impact of environment on the size-mass relation, the main sequence (MS) relation, and the Tully-Fisher relation (TFR).Methods. We perform a morpho-kinematics modelling of 593 [O II] emitters in various environments in the COSMOS area from the MUSE-gAlaxy Groups In Cosmos survey. The HST F814W images are modelled with a bulge-disk decomposition to estimate their bulge-disk ratio, effective radius, and disk inclination. We use the [O II] lambda lambda 3727, 3729 doublet to extract the galaxies' ionised gas kinematics maps from the MUSE cubes, and we model those maps for a sample of 146 [O II] emitters, including bulge and disk components constrained from morphology and a dark matter halo.Results. We find an offset of 0.03 dex (1 sigma - significant) on the size-mass relation zero point between the field and the large structure sub-samples, with a richness threshold of N = 10 to separate between small and large structures, and of 0.06 dex (2 sigma) with N = 20. Similarly, we find a 0.1 dex (2 sigma) difference on the MS relation with N = 10 and 0.15 dex (3 sigma) with N = 20. These results suggest that galaxies in massive structures are smaller by 14% and have star formation rates reduced by a factor of 1.3-1.5 with respect to field galaxies at z approximate to 0.7. Finally, we do not find any impact of the environment on the TFR, except when using N = 20 with an offset of 0.04 dex (1 sigma). We discard the effect of quenching for the largest structures, which would lead to an offset in the opposite direction. We find that, at z approximate to 0.7, if quenching impacts the mass budget of galaxies in structures, these galaxies would have been affected quite recently and for roughly 0.7-1.5 Gyr. This result holds when including the gas mass but vanishes once we include the asymmetric drift correction. Show less
We investigate the buildup of galaxies from various vantage points. The first two chapters focus on the stellar content of galaxies, especially the distribution of stellar masses at birth and... Show moreWe investigate the buildup of galaxies from various vantage points. The first two chapters focus on the stellar content of galaxies, especially the distribution of stellar masses at birth and potential variations therein in various galactic environments. We find that in some cases these inferred variations can be due to an underestimation of model and measurement errors. Furthermore, we infer the consequences of these proposed variations on the interpretation of galaxy properties and galaxy formation processes. Chapters 3 and 4 focus on the buildup of galaxies in time through mergers and in-situ star formation. We test and improve observational models that aim to trace galaxies though cosmic time, by applying them to cosmological hydrodynamical simulations, for which we have access to the full history and evolution of galaxies since the beginning of time. The fifth chapter focusses on the buildup of galaxy morphology. We follow the buildup of morphological components in a cosmological simulation, which leads us to conclude that galaxy formation is a three-phase process, consisting of an early, rather disorganised, phase, followed by a phase in which stars are formed primarily in an organised rotating disk, and ending in a late phase of merger-driven spheroid formation. Show less
