Same as Figure 6 divided into subsamples. (left) Group I: Subgroup with at least one gas-poor neighbors, or neighbor(s) with no H I. (Panel (a), (b), and (d) in Figure 5). (right) Group II: Subsample with only gas-rich neighbors (Panel (c) in Figure 5). Group I systems are showing tighter correlation of Bolometric luminosity (L_bol), Eddington ratio (λ_Edd) as a function of the relative extent of H I gas including low-density gas (D_HI, ext) to stellar disk (D₂₅). Hence, Group I systems are more likely to have exchanged gas with their surroundings, compared to the Group II shown in the right panel, where these systems are likely in an earlier phase of group interaction.