The evolution of the mass-size relation for early type galaxies from z~1
  to the present: dependence on environment, mass-range and detailed morphology
  [abridged] We study the dependence of the galaxy size evolution on
morphology, stellar mass and large scale environment for a sample of 298 group
and 384 field quiescent early-type galaxies from the COSMOS survey, selected
from z~1 to the present, and with masses $log(M/M_\odot)>10.5$.
  The galaxy size growth depends on galaxy mass and early-type galaxy
morphology, e.g., elliptical galaxies evolve differently than lenticular
galaxies. At the low mass end -$10.5<Log(M/M_\odot)<11$, ellipticals do not
show strong size growth from $z\sim1$ to the present (10% to 30% depending on
the morphological classification). On the other end, massive ellipticals
-log(M/M_\odot)>11.2$- approximately doubled their size. Interestingly,
lenticular galaxies display different behavior: they appear more compact on
average and they do show a size growth of \sim60% since z=1 independent of
stellar mass. We compare our results with state-of-the art semi-analytic
models.
  While major and minor mergers can account for most of the galaxy size growth,
we find that with present data and the theoretical uncertainties in the
modeling we cannot state clear evidence favoring either merger or mass loss via
quasar and/or stellar winds as the primary mechanism driving the evolution.
  The galaxy mass--size relation and the size growth do not depend on
environment in the halo mass range explored in this work (field to group mass
$log(M_h/M_\odot)<14$), i.e., group and field galaxies follow the same trends,
which is at variance with predictions from current hierarchical models that
show a clear dependence of size growth on halo mass for massive ellipticals
-$log(M_*/M_\odot)>11.2$.
