  We have examined the morphological make-up of X-ray bright groups. The
brighter galaxies in these groups exhibit clear morphology-density and
morphology-radius relations. The group morphology-density relation is offset
from the cluster relation in the sense that at a given surface density, X-ray
bright groups have a lower spiral fraction. After correcting for projection
effects the morphology-3D density relation is still shifted towards fewer
spirals for a given 3D density, in comparison with clusters. A simple model
which corrects the group data for the effects of projection and for the
expected higher merging rate in groups, brings the morphology-density relation
into good agreement with that of clusters, suggesting that the relation may be
driven by two-body interactions. The fraction of S0 galaxies in these X-ray
bright groups is at least as high as that observed in nearby clusters. Given
the low velocity dispersion of groups, this indicates that ram pressure
stripping is not the dominant mechanism for S0 formation.
