  We investigate the role that dense environments have on the quenching of star
formation and the transformation of morphology for a sample of galaxies
selected from the Sloan Digital Sky Survey. We make a distinction between
galaxies falling into groups $(13 \leq \log{(M_{\text{halo}}/M_{\odot})} < 14)$
and clusters $(\log{(M_{\text{halo}}/M_{\odot})} \geq 14)$, and compare to a
large sample of field galaxies. Using galaxy position in projected phase space
as a proxy for time since infall, we study how galaxy specific star formation
rate (sSFR) and morphology, parameterized by the bulge-to-total light ratio
(B/T), change over time. After controlling for stellar mass, we find clear
trends of increasing quenched and elliptical fractions as functions of infall
time for galaxies falling into both groups and clusters. The trends are
strongest for low mass galaxies falling into clusters. By computing quenching
and morphological transformation timescales, we find evidence that star
formation quenching occurs faster than morphological transformation in both
environments. Comparing field galaxies to recently infalling galaxies, we
determine there is pre-processing of both star formation and morphology, with
pre-processing affecting star formation rates more strongly. Our analysis
favours quenching mechanisms that act quickly to suppress star formation, while
other mechanisms that act on longer timescales transform morphology through
bulge growth and disc fading.
