The evolution of galaxy scaling relations in clusters at 0.5<z<1.5
  We present new gas kinematic observations with the OSIRIS instrument at the
GTC for galaxies in the Cl1604 cluster system at z=0.9. These observations
together with a collection of other cluster samples at different epochs
analyzed by our group are used to study the evolution of the Tully-Fisher,
velocity-size and stellar mass-angular momentum relations in dense environments
over cosmic time. We use 2D and 3D spectroscopy to analyze the kinematics of
our cluster galaxies and extract their maximum rotation velocities (Vmax). Our
methods are consistently applied to all our cluster samples which make them
ideal for an evolutionary comparison. Up to redshift one, our cluster samples
show evolutionary trends compatible with previous observational results in the
field and in accordance with semianalytical models and hydrodynamical
simulations concerning the Tully-Fisher and velocity-size relations. However,
we find a factor 3 drop in disk sizes and an average B-band luminosity
enhancement of 2 mag by z=1.5. We discuss the role that different
cluster-specific interactions may play in producing this observational result.
In addition, we find that our intermediate-to-high redshift cluster galaxies
follow parallel sequences with respect to the local specific angular
momentum-stellar mass relation, although displaying lower angular momentum
values in comparison with field samples at similar redshifts. This can be
understood by the stronger interacting nature of dense environments with
respect to the field.
