Constraints on Quenching of $z\lesssim2$ Massive Galaxies from the
  Evolution of the average Sizes of Star-Forming and Quenched Populations in
  COSMOS
  We use $>$9400 $\log(m/M_{\odot})>10$ quiescent and star-forming galaxies at
$z\lesssim2$ in COSMOS/UltraVISTA to study the average size evolution of these
systems, with focus on the rare, ultra-massive population at
$\log(m/M_{\odot})>11.4$. The large 2-square degree survey area delivers a
sample of $\sim400$ such ultra-massive systems. Accurate sizes are derived
using a calibration based on high-resolution images from the Hubble Space
Telescope. We find that, at these very high masses, the size evolution of
star-forming and quiescent galaxies is almost indistinguishable in terms of
normalization and power-law slope. We use this result to investigate possible
pathways of quenching massive $m>M^*$ galaxies at $z<2$. We consistently model
the size evolution of quiescent galaxies from the star-forming population by
assuming different simple models for the suppression of star-formation. These
models include an instantaneous and delayed quenching without altering the
structure of galaxies and a central starburst followed by compaction. We find
that instantaneous quenching reproduces well the observed mass-size relation of
massive galaxies at $z>1$. Our starburst$+$compaction model followed by
individual growth of the galaxies by minor mergers is preferred over other
models without structural change for $\log(m/M_{\odot})>11.0$ galaxies at
$z>0.5$. None of our models is able to meet the observations at $m>M^*$ and
$z<1$ with out significant contribution of post-quenching growth of individual
galaxies via mergers. We conclude that quenching is a fast process in galaxies
with $ m \ge 10^{11} M_\odot$, and that major mergers likely play a major role
in the final steps of their evolution.
