In this paper we study the distribution of dark matter in small galaxy groups , in a \Lambda CDM cosmology , identified using a physical criterion .
We quantify the amount of intra-group dark matter and characterize its distribution .
We find that compact associations of galaxies , as well as those intermediate and loose groups , have a rather flat profiles with a logarithmic slope of \gamma \approx - 0.2 .
Hence , the intra-group dark matter does not follow the same cuspy tendency that haloes of galaxies have .
In intermediate and loose galaxy associations the intragroup matter tends to be \mathrel { \hbox to 0.0 pt { \lower 3.0 pt \hbox { $ \mathchar 536 $ } \hss } \raise 2.0 pt% \hbox { $ \mathchar 316 $ } } 50 % that of the total mass of the group , and in compact associations is \mathrel { \hbox to 0.0 pt { \lower 3.0 pt \hbox { $ \mathchar 536 $ } \hss } \raise 2.0 pt% \hbox { $ \mathchar 316 $ } } 20 % within their group radius .
So , in general , common dark matter haloes of small galaxy groups are not cuspy nor massive .