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In galaxy clusters, efficiently accreting active galactic nuclei (AGN) arepreferentially located in the infall regions of the cluster projectedphase-space, and are rarely found in the cluster core. This has been attributedto both an increase in triggering opportunities for infalling galaxies, and areduction of those mechanisms in the hot, virialised, cluster core. Exploitingthe depth and completeness ($98\,$per cent at $r<19.8\,$mag) of the Galaxy AndMass Assembly survey (GAMA), we probe down the group halo mass function toassess whether AGN are found in the same regions in groups as they are inclusters. We select 451 optical AGN from 7498 galaxies with$\log_{10}(M_*/\text{M}_\odot) > 9.9$ in 695 groups with $11.53\leq\log_{10}(M_{200}/\text{M}_\odot) \leq 14.56$ at $z<0.15$. By analysing theprojected phase-space positions of these galaxies we demonstrate that whensplit both radially, and into physically derived infalling and corepopulations, AGN position within group projected phase-space is dependent onhalo mass. For groups with $\log_{10}(M_{200}/\text{M}_\odot)>13.5$, AGN arepreferentially found in the infalling galaxy population with $3.6\sigma$confidence. At lower halo masses we observe no difference in AGN fractionbetween core and infalling galaxies. These observations support a model where areduced number of low-speed interactions, ram pressure stripping andintra-group/cluster medium temperature, the dominance of which increase withhalo mass, work to inhibit AGN in the cores of groups and clusters with$\log_{10}(M_{200}/\text{M}_\odot)>13.5$, but do not significantly affectnuclear activity in cores of less massive structures.

Galaxy And Mass Assembly (GAMA): The effect of galaxy group environment on active galactic nuclei