TY - JOUR
T1 - SDSS-IV MaNGA
T2 - The Roles of AGNs and Dynamical Processes in Star Formation Quenching in Nearby Disk Galaxies
AU - Guo, Kexin
AU - Peng, Yingjie
AU - Shao, Li
AU - Fu, Hai
AU - Catinella, Barbara
AU - Cortese, Luca
AU - Yuan, Feng
AU - Yan, Renbin
AU - Zhang, Chengpeng
AU - Dou, Jing
N1 - Publisher Copyright:
© 2018. The American Astronomical Society. All rights reserved..
PY - 2019/1/1
Y1 - 2019/1/1
N2 - We study how star formation (SF) is quenched in low-redshift disk galaxies with integral-field spectroscopy. We select 131 face-on spiral galaxies with stellar mass greater than 3 × 1010 M o, and with spatially resolved spectrum from MaNGA DR13. We subdivide the sample into four groups based on the offset of their global specific star formation rate (SFR) from the star-forming main sequence and stack the radial profiles of stellar mass and SFR. By comparing the stacked profiles of quiescent and star-forming disk galaxies, we find that the decrease of the global SFR is caused by the suppression of SF at all radii, but with a more significant drop from the center to the outer regions following an inside-out pattern. As the global specific SFR decreases, the central stellar mass, the fraction of disk galaxies hosting stellar bars, and active galactic nuclei (AGNs; including both LINERs and Seyferts) all increase, indicating dynamical processes and AGN feedback are possible contributors to the inside-out quenching of SF in the local universe. However, if we include only Seyferts, or AGNs with EW(Hα) > 3 the increasing trend of AGN fraction with decreasing global sSFR disappears. Therefore, if AGN feedback is contributing to quenching, we suspect that it operates in the low-luminosity AGN mode, as indicated by the increasing large bulge mass of the more passive disk galaxies.
AB - We study how star formation (SF) is quenched in low-redshift disk galaxies with integral-field spectroscopy. We select 131 face-on spiral galaxies with stellar mass greater than 3 × 1010 M o, and with spatially resolved spectrum from MaNGA DR13. We subdivide the sample into four groups based on the offset of their global specific star formation rate (SFR) from the star-forming main sequence and stack the radial profiles of stellar mass and SFR. By comparing the stacked profiles of quiescent and star-forming disk galaxies, we find that the decrease of the global SFR is caused by the suppression of SF at all radii, but with a more significant drop from the center to the outer regions following an inside-out pattern. As the global specific SFR decreases, the central stellar mass, the fraction of disk galaxies hosting stellar bars, and active galactic nuclei (AGNs; including both LINERs and Seyferts) all increase, indicating dynamical processes and AGN feedback are possible contributors to the inside-out quenching of SF in the local universe. However, if we include only Seyferts, or AGNs with EW(Hα) > 3 the increasing trend of AGN fraction with decreasing global sSFR disappears. Therefore, if AGN feedback is contributing to quenching, we suspect that it operates in the low-luminosity AGN mode, as indicated by the increasing large bulge mass of the more passive disk galaxies.
KW - galaxies: active
KW - galaxies: evolution
KW - galaxies: star formation
KW - galaxies: structure
UR - http://www.scopus.com/inward/record.url?scp=85059853677&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85059853677&partnerID=8YFLogxK
U2 - 10.3847/1538-4357/aaee88
DO - 10.3847/1538-4357/aaee88
M3 - Article
AN - SCOPUS:85059853677
SN - 0004-637X
VL - 870
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - 19
ER -