Evolution of cluster disk galaxies to z=1.5

Total mass, angular momentum, and star formation processes are the main drivers of galaxy properties and distinct evolutionary pathways. Environment has an additional impact with specific gravitational and hydrodynamical interactions. To disentangle the different effects we collected over the recent years 2D- and 3D-spectroscopic data of emission-line disk galaxies that allows to measure and derive physical properties like star formation rates, chemical abundances, stellar populations, kinematics, and dynamical masses. Our cluster samples at z=1.5, 0.9, 0.5, and 0.2 encompass important cosmological epochs from the start of cluster assembly over the peak of merging activity to the local era. We combine our kinematic data with structural (stellar) parameters to construct scaling relations like the Tully-Fisher (Vmax-Luminosity), Velocity-Size, and Mass-Angular Momentum relations enabling the study of galaxy evolution in a quantitative way. In comparison to field galaxies at similar epochs observed with the same observing techniques and to cosmological simulations we derive differential evolution with respect to luminosity, mass, size, and angular momentum that can be explained by various interaction processes at the different epochs.