Persistence of the Color-Density Relation and Efficient Environmental
  Quenching to $z\sim1.4$
  Using ~5000 spectroscopically-confirmed galaxies drawn from the Observations
of Redshift Evolution in Large Scale Environments (ORELSE) survey we
investigate the relationship between color and galaxy density for galaxy
populations of various stellar masses in the redshift range $0.55 \le z \le
1.4$. The fraction of galaxies with colors consistent with no ongoing star
formation ($f_q$) is broadly observed to increase with increasing stellar mass,
increasing galaxy density, and decreasing redshift, with clear differences
observed in $f_q$ between field and group/cluster galaxies at the highest
redshifts studied. We use a semi-empirical model to generate mock group/cluster
galaxies unaffected by environmental processes and compare them to observed
populations to constrain the environmental quenching efficiency
($\Psi_{convert}$). High-density environments from $0.55 \le z \le 1.4$ appear
capable of efficiently quenching galaxies with
$\log(M_{\ast}/M_{\odot})>10.45$. Lower stellar mass galaxies also appear
efficiently quenched at the lowest redshifts, but this efficiency drops
precipitously with increasing redshift. Quenching efficiencies, combined with
simulated group/cluster accretion histories and results from a companion ORELSE
study, are used to constrain the average time from group/cluster accretion to
quiescence and the time between accretion and the inception of quenching. These
timescales were constrained to be <$t_{convert}$>=$2.4\pm0.3$ and
<$t_{delay}$>=$1.3\pm0.4$ Gyr, respectively, for galaxies with
$\log(M_{\ast}/M_{\odot})>10.45$ and <$t_{convert}$>=$3.3\pm0.3$ and
<$t_{delay}$>=$2.2\pm0.4$ Gyr for lower stellar mass galaxies. These quenching
efficiencies and associated timescales are used to rule out certain
environmental mechanisms as being those primarily responsible for transforming
the star-formation properties of galaxies over this 4 Gyr window in cosmic
time.
