Abstract
We study the distribution of intragroup dark matter in small groups of dark matter galaxy size halos in a ΛCDM cosmology. These groups are identified using a physical criterion and may be an appropriate representation of small galaxy groups. We quantify the amount of intra-group dark matter and characterize its distribution. We find that compact associations of halos, as well as intermediate and loose groups, have rather flat intragroup dark matter profiles, with logarithmic slopes of γ ≈ 0 and ≈ -0.2, respectively. Hence, the intra-group dark matter of these halo systems does not follow the same cuspy tendency of galactic halos. In intermediate and loose associations of galaxy-size halos, the intragroup matter tends to be ≲ 50% of the total mass of the group, while in compact associations it is ≲ 20% of the mass within their group radius.
