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The role of active galactic nuclei (AGNs) during galaxy interactions and howthey influence the star formation in the system are still under debate. We usea sample of 1156 galaxies in galaxy pairs or mergers (hereafter `pairs') fromthe MaNGA survey. This pair sample is selected by the velocity offset,projected separation, and morphology, and is further classified into four casesalong the merger sequence based on morphological signatures. We then identify atotal of 61 (5.5%) AGNs in pairs based on the emission-line diagnostics. Noevolution of the AGN fraction is found, either along the merger sequence orcompared to isolated galaxies (5.0%). We observe a higher fraction of passivegalaxies in galaxy pairs, especially in the pre-merging cases, and associatethe higher fraction to their environmental dependence. The isolated AGN and AGNin pairs show similar distributions in their global stellar mass, starformation rate (SFR), and central [OIII] surface brightness. AGNs in pairs showradial profiles of increasing specific SFR and declining Dn4000 from center tooutskirts, and no significant difference from the isolated AGNs. This isclearly different from star-forming galaxies (SFGs) in our pair sample, whichshow enhanced central star formation, as reported before. AGNs in pairs havelower Balmer decrements at outer regions, possibly indicating less dustattenuation. Our findings suggest that AGNs likely follow an inside-outquenching and the merger impact on the star formation in AGNs is less prominentthan in SFGs.

An IFU View of the Active Galactic Nuclei in MaNGA Galaxy Pairs