Galaxy Evolution in dense environments observed by the IFS MUSE, a kinematic approach

Galaxies form and evolve in different environments, shaped by the distribution of dark matter halos. The evolution of galaxies in low-density environments significantly differs from those in dense structures, where environmental drivers reduce the gas content quenching their star formation capacity earlier than their isolated counterparts. The goal of this work is to study the TFR for galaxies at intermediate z groups. This relation provides key information on the dynamical support, and on formation and evolutionary state of galaxies. The advent of powerful IFS instruments like MUSE, allows to perform spatially resolved studies at intermediate redshifts (z). This research is based on the exploitation of an unique sample of 12 dense galaxy groups selected in the COSMOS field, from the GTO MUSE gAlaxy Groups In Cosmos (MAGIC) Survey, at 0.3 < z < 0.8. The kinematics was extracted using the [OII] λλ3726,3729 A doublet. A bulge-disk decomposition and a 2D kinematic modeling were applied to recover the maximum rotation velocity at 2.2 disk scale lengths (R_2.2), the intrinsic velocity dispersion (σ) and the dynamical mass. I performed a rigorous sample selection in setting limits on the spatial resolution and on the signal-to-noise ratio (SNR). I compared my results with previous studies in different environments finding our method reduces the outliers in the TFR. I found the stellar and baryonic mass fractions increase with stellar mass. I also found a clear offset of the TFR zero-point between different environments implying that at fixed stellar mass, galaxies in dense environments rotate faster than in low-density environments. The evolution of the TFR in dense environments could be due to a combination of quenching of star formation and contraction of the baryonic content.