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We study how star formation (SF) is quenched in low-redshift disk galaxieswith integral-field spectroscopy. We select 131 face-on spiral galaxies withstellar mass greater than $\rm 3\times10^{10}M_\odot$, and with spatiallyresolved spectrum from MaNGA DR13. We subdivide the sample into four groupsbased on the offset of their global specific star formation rate (SFR) from thestar-forming main sequence and stack the radial profiles of stellar mass andSFR. By comparing the stacked profiles of quiescent and star-forming diskgalaxies, we find that the decrease of the global SFR is caused by thesuppression of SF at all radii, but with a more significant drop from thecenter to the outer regions following an inside-out pattern. As the globalspecific SFR decreases, the central stellar mass, the fraction of disk galaxieshosting stellar bars, and active galactic nuclei (AGNs; including both LINERsand Seyferts) all increase, indicating dynamical processes and AGN feedback arepossible contributors to the inside-out quenching of SF in the local universe.However, if we include only Seyferts, or AGNs with ${\rm EW(H\alpha)>3\AA}$,the increasing trend of AGN fraction with decreasing global sSFR disappears.Therefore, if AGN feedback is contributing to quenching, we suspect that itoperates in the low-luminosity AGN mode, as indicated by the increasing largebulge mass of the more passive disk galaxies.

SDSS-IV MaNGA: The Roles of AGNs and Dynamical Processes in Star Formation Quenching in Nearby Disk Galaxies