  We explore how the fraction of quenched galaxies changes in groups of
galaxies with respect to the distance to the center of the group, redshift, and
stellar mass to determine the dominant process of environmental quenching in
$0.2 < z < 0.8$ groups. We use new UV data from the UVCANDELS project in
addition to existing multiband photometry to derive new galaxy physical
properties of the group galaxies from the zCOSMOS 20k Group Catalog. Limiting
our analysis to a complete sample of log$(M_*/M_{\odot})>10.56$ group galaxies
we find that the probability of being quenched increases slowly with decreasing
redshift, diverging from the stagnant field galaxy population. A corresponding
analysis on how the probability of being quenched increases with time within
groups suggests that the dominant environmental quenching process is
characterized by slow ($\sim$Gyr) timescales. We find a quenching time of
approximately $4.91^{+0.91}_{-1.47} $Gyrs, consistent with the slow processes
of strangulation (Larson et al. 1980) and delayed-then-rapid quenching (Wetzel
et al. 2013 arXiv:1206.3571v2 [astro-ph.CO]), although more data are needed to
confirm this result.
