  Combining high-fidelity group characterisation from the Galaxy and Mass
Assembly (GAMA) survey and source-tailored $z<0.1$ photometry from the WISE
survey, we present a comprehensive study of the properties of ungrouped
galaxies, compared to 497 galaxy groups (4$\leq$ N$_{\rm FoF}$ $\leq$ 20) as a
function of stellar and halo mass. Ungrouped galaxies are largely unimodal in
WISE color, the result of being dominated by star-forming, late-type galaxies.
Grouped galaxies, however, show a clear bimodality in WISE color, which
correlates strongly with stellar mass and morphology. We find evidence for an
increasing early-type fraction, in stellar mass bins between
$10^{10}\lesssim$M$_{\rm stellar} \lesssim10^{11}$ M$_\odot$, with increasing
halo mass. Using ungrouped, late-type galaxies with star-forming colors
(W2$-$W3$>$3), we define a star-forming main-sequence (SFMS), which we use to
delineate systems that have moved below the sequence ("quenched" for the
purposes of this work). We find that with increasing halo mass, the relative
number of late-type systems on the SFMS decreases, with a corresponding
increase in early-type, quenched systems at high stellar mass (M$_{\rm
stellar}>{10}^{10.5}$ M$_\odot$), consistent with mass quenching. Group
galaxies with masses M$_{\rm stellar}<{10}^{10.5}$ M$_\odot$ show evidence of
quenching consistent with environmentally-driven processes. The stellar mass
distribution of late-type, quenched galaxies suggests they may be an
intermediate population as systems transition from being star-forming and
late-type to the "red sequence". Finally, we use the projected area of groups
on the sky to extract groups that are (relatively) compact for their halo mass.
Although these show a marginal increase in their proportion of high mass and
early-type galaxies compared to nominal groups, a clear increase in quenched
fraction is not evident.
