The first 62 AGN observed with SDSS-IV MaNGA - IV: gas excitation and star-formation rate distributions

We present maps of the ionized gas flux distributions, excitation, star-formation rate SFR, surface mass density \(\Sigma_{H+}\), and obtain total values of SFR and ionized gas masses {\it M} for 62 Active Galactic Nuclei (AGN) observed with SDSS-IV MaNGA and compare them with those of a control sample of 112 non-active galaxies. The most luminous AGN -- with \(L(\rm{[OIII]}\lambda 5007) \ge 3.8\times 10^{40}\,\mbox{erg}\,\mbox{s}^{-1}\), and those hosted by earlier-type galaxies are dominated by Seyfert excitation within 0.2 effective radius \(R_e\) from the nucleus, surrounded by LINER excitation or transition regions, while the less luminous and hosted by later-type galaxies show equally frequent LINER and Seyfert excitation within \(0.2\,R_e\). The extent \(R\) of the region ionized by the AGN follows the relation \(R\propto\,L(\rm{[OIII]})^{0.5}\) -- as in the case of the Broad-Line Region. The SFR distribution over the region ionized by hot stars is similar for AGN and controls, while the integrated SFR -- in the range \(10^{-3}-10\)\,M\(_\odot\)\,yr\(^{-1}\) is also similar for the late-type sub-sample, but higher in the AGN for 75\% of the early-type sub-sample. We thus conclude that there is no signature of AGN quenching star formation in the body of the galaxy in our sample. We also find that 66\% of the AGN have higher ionized gas masses \(M\) than the controls -- in the range 10\(^5-3\times10^7\)\,M\(_\odot\) -- while 75\% of the AGN have higher \(\Sigma_{H+}\) within \(0.2\,R_e\) than the control galaxies.