Ionized gas disks in elliptical and S0 galaxies at $z<1$
  We analyse the extended, ionized-gas emission of 24 early-type galaxies
(ETGs) at $0<z<1$ from the ESO Distant Cluster Survey (EDisCS). We discuss
different possible sources of ionization and favour star-formation as the main
cause of the observed emission. 10 galaxies have disturbed gas kinematics,
while 14 have rotating gas disks. In addition, 15 galaxies are in the field,
while 9 are in the infall regions of clusters. This implies that, if the gas
has an internal origin, this is likely stripped as the galaxies get closer to
the cluster centre. If the gas instead comes from an external source, then our
results suggest that this is more likely acquired outside the cluster
environment, where galaxy-galaxy interactions more commonly take place. We
analyse the Tully-Fisher relation of the ETGs with gas disks, and compare them
to EDisCS spirals. Taking a matched range of redshifts, $M_{B}<-20$, and
excluding galaxies with large velocity uncertainties, we find that, at fixed
rotational velocity, ETGs are 1.7 mag fainter in $M_{B}$ than spirals. At fixed
stellar mass, we also find that ETGs have systematically lower specific
star-formation rates than spirals. This study constitutes an important step
forward towards the understanding of the evolution of the complex ISM in ETGs
by significantly extending the look-back-time baseline explored so far.
