  It is often stated that the removal of gas by ram pressure stripping of a
galaxy disk is not a common process in galaxy groups. In this study, with the
aid of an observational classification of galaxies and a simple physical model,
we show that this may not be true. We examined and identified 45 ram-pressure
stripped galaxy candidates from a sample of 1311 galaxy group members within
125 spectroscopically-selected galaxy groups. 13 of these galaxies are the most
secure candidates with multiple distinct features. These candidate ram pressure
stripped galaxies have similar properties to those found in clusters -- they
occur at a range of stellar masses, are largely blue and star-forming and have
phase-space distributions consistent with being first infallers into their
groups. The only stand-out feature of these candidates is they exist not in
clusters, but in groups, with a median halo mass of 10$^{13.5}$ M$_\odot$.
Although this may seem surprising, we employ an analytic model of the expected
ram pressure stripping force in groups and find that reasonable estimates of
the relevant infall speeds and intragroup medium content would result in ram
pressure stripped galaxies at these halo masses. Finally, given the
considerable uncertainty on the lifetime of the ram-pressure phase, this
physical mechanism could be the dominant quenching mechanism in galaxy groups,
if our ram pressure stripped candidates can be confirmed.
