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We investigated the variation in the fraction of optical active galacticnuclei (AGN) hosts with stellar mass, as well as their local and globalenvironments. Our sample is composed of cluster members and field galaxies at$z \le 0.1$ and we consider only strong AGN. We find a strong variation in theAGN fraction ($F_{AGN}$) with stellar mass. The field population comprises ahigher AGN fraction compared to the global cluster population, especially forobjects with log $M_* > 10.6$. Hence, we restricted our analysis to moremassive objects. We detected a smooth variation in the $F_{AGN}$ with localstellar mass density for cluster objects, reaching a plateau in the fieldenvironment. As a function of clustercentric distance we verify that $F_{AGN}$is roughly constant for R $> $ R$_{200}$, but show a steep decline inwards. Wehave also verified the dependence of the AGN population on cluster velocitydispersion, finding a constant behavior for low mass systems ($\sigma_P\lesssim 650-700$ km s$^{-1}$). However, there is a strong decline in $F_{AGN}$for higher mass clusters ($>$ 700 km s$^{-1}$). When comparing the $F_{AGN}$ inclusters with or without substructure we only find different results forobjects at large radii (R $> $ R$_{200}$), in the sense that clusters withsubstructure present some excess in the AGN fraction. Finally, we have foundthat the phase-space distribution of AGN cluster members is significantlydifferent than other populations. Due to the environmental dependence of$F_{AGN}$ and their phase-space distribution we interpret AGN to be the resultof galaxy interactions, favored in environments where the relative velocitiesare low, typical of the field, low mass groups or cluster outskirts.

NoSOCS in SDSS. VI. The Environmental Dependence of AGN in Clusters and Field in the Local Universe