Connection Between Stellar Mass Distributions Within Galaxies and
  Quenching Since z =2
  We study the history from $z\sim2$ to $z\sim0$ of the stellar mass assembly
of quiescent and star-forming galaxies in a spatially resolved fashion. For
this purpose we use multi-wavelength imaging data from the Hubble Space
Telescope (HST) over the GOODS fields and the Sloan Digital Sky Survey (SDSS)
for the local population. We present the radial stellar mass surface density
profiles of galaxies with $M_{\ast}>10^{10} M_{\odot}$, corrected for
mass-to-light ratio ($M_{\ast}/L$) variations, and derive the half-mass radius
($R_{m}$), central stellar mass surface density within 1 kpc ($\Sigma_{1}$) and
surface density at $R_{m}$ ($\Sigma_{m}$) for star-forming and quiescent
galaxies and study their evolution with redshift. At fixed stellar mass, the
half-mass sizes of quiescent galaxies increase from $z\sim2$ to $z\sim0$ by a
factor of $\sim3-5$, whereas the half-mass sizes of star-forming galaxies
increase only slightly, by a factor of $\sim2$. The central densities
$\Sigma_{1}$ of quiescent galaxies decline slightly (by a factor of
$\lesssim1.7$) from $z\sim2$ to $z\sim0$, while for star-forming galaxies
$\Sigma_{1}$ increases with time, at fixed mass. We show that the central
density $\Sigma_{1}$ has a tighter correlation with specific star-formation
rate (sSFR) than $\Sigma_{m}$ and for all masses and redshifts galaxies with
higher central density are more prone to be quenched. Reaching a high central
density ($\Sigma_{1} \gtrsim 10^{10} M_{\odot} \mathrm{kpc}^2$) seems to be a
prerequisite for the cessation of star formation, though a causal link between
high $\Sigma_{1}$ and quenching is difficult to prove and their correlation can
have a different origin.
