  We use a combination of new AAOmega multi-object wide-field spectroscopic
observations and literature data to define 111 spectroscopically confirmed
members of the massive NGC 5044 group with M_B <= -13.5 mag, providing a
three-fold increase in group members over previous analyses of this group. We
find the group to have a dynamical mass of 9.2 x 10^13 solar masses, placing it
on the border between rich groups and poor clusters. However, comparison to the
L_x-sigma and L_x-mass relations shows it more closely follows cluster scaling
relations. Using a combination of crossing time, X-ray contours and
line-of-sight velocity profile we are able to preclude growth of the NGC 5044
group via major sub-group mergers within the last ~1 Gyr. While the majority of
dynamical indicators for the group suggest it is virialised, we find evidence
for a small, dynamically distinct sub-group at 1.4 Mpc from the group centre,
suggesting that the NGC 5044 group is the dominant structure in its local
environment, and is currently accreting smaller groups.
