Formation and Evolution of
Galaxy Clusters Across Cosmic Time

The evolution of gas kinematics of massive galaxies is relatively well established up to higher redshifts, however, little is known about the kinematics of lower mass galaxies in high density environments. We use optical integral field spectroscopy from MUSE, as well as photometric observations from HST and HAWK-I, to study the morpho-kinematics of 18 low mass MACS0416 cluster galaxies at a redshift of ~0.4. By measuring fluxes of strong emission lines from the MUSE data, we have recovered the spatially-resolved star formation rates, gas-phase metallicities, and gas kinematics. We have used Galfit on the photometric observations to study the structure and morphology of the cluster members. We are modeling the gaseous velocity fields of the cluster members using a 3D approach. By doing so, we want to study scaling relations such as the Tully-Fisher (TFR) and Mass-Size relation for galaxies in different environments. We are planning to perform the same analysis for a matched sample of field galaxies.
We are searching for signs of cluster-specific processes such as ram pressure stripping using as tracers either enhanced gas-phase metallicities or disturbed gaseous velocity fields.
Our preliminary results reveal a sample of dispersion-dominated, compact dwarfs with maximum velocities vmax < 100 km/s, which depart from the TFR. This might indicate that their disks did not settle yet, or that they are affected by environmental processes. However, some of the cluster dwarfs are rotation-dominated disks and lie on the TFR.