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 } \leq - 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 \times 10 ^ { 14 } M _ { \odot } , placing it on the border between rich groups and poor clusters .
However , comparison to the L _ { X } – \sigma _ { \nu } 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 \sim 1 Gyr .
While the majority of dynamical indicators for the group suggest it is virialized , 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 .