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

Kexin Guo; Yingjie Peng; Li Shao; Hai Fu; Barbara Catinella; Luca Cortese; Feng Yuan; Renbin Yan; Chengpeng Zhang; Jing Dou

doi:10.3847/1538-4357/aaee88

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

Kexin Guo, Yingjie Peng, Li Shao, Hai Fu, Barbara Catinella, Luca Cortese, Feng Yuan, Renbin Yan, Chengpeng Zhang, Jing Dou

Physics And Astronomy

Research output: Contribution to journal › Article › peer-review

18 Scopus citations

Abstract

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.

Original language	English
Article number	19
Journal	Astrophysical Journal
Volume	870
Issue number	1
DOIs	https://doi.org/10.3847/1538-4357/aaee88
State	Published - Jan 1 2019

Bibliographical note

Funding Information:
We thank the anonymous referee for their valuable comments and suggestions that helped to improve the manuscript. We thank the discussions with Prof. Jing Wang, Prof. Martin Bureau, Prof. Michele Cappellari, Prof. Chris Lintott, and Dr. Zhi-zheng Pan. The first author is grateful for the constant encouragement of Prof. Xian-zhong Zheng. Y.P. acknowledges support from the National Key Program for Science and Technology Research and Development under grant No. 2016YFA0400702, and the NSFC grant No. 11773001. H.F. acknowledges support from the National Science Foundation under grant AST-1614326. Parts of this research were conducted by the Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), through project number CE170100013. This research is also supported jointly by China National Postdoctoral Science Foundation, China Scholarship Council and The International Centre for Radio Astronomy Research.

Funding Information:
Funding for the Sloan Digital Sky Survey IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science, and the Participating Institutions. SDSS-IV acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. The SDSS website is www.sdss.org. SDSS-IV is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS Collaboration including the Brazilian Participation Group, the Carnegie Institution for Science, Carnegie Mellon University, the Chilean Participation Group, the French Participation Group, Harvard-Smithsonian Center for Astrophysics, Instituto de Astrofísica de Canarias, The Johns Hopkins University, Kavli Institute for the Physics and Mathematics of the Universe (IPMU)/University of Tokyo, Lawrence Berkeley National Laboratory, Leibniz Institut für Astrophysik Potsdam (AIP), Max-Planck-Institut für Astronomie (MPIA Heidelberg), Max-Planck-Institut für Astrophysik (MPA Garching), Max-Planck-Institut für Extraterrestrische Physik (MPE), National Astronomical Observatories of China, New Mexico State University, New York University, University of Notre Dame, Observatário Nacional/MCTI, The Ohio State University, Pennsylvania State University, Shanghai Astronomical Observatory, United Kingdom Participation Group, Universidad Nacional Autónoma de México, University of Arizona, University of Colorado Boulder, University of Oxford, University of Portsmouth, University of Utah, University of Virginia, University of Washington, University of Wisconsin, Vanderbilt University, and Yale University.

Publisher Copyright:
© 2018. The American Astronomical Society. All rights reserved..

Keywords

galaxies: active
galaxies: evolution
galaxies: star formation
galaxies: structure

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.3847/1538-4357/aaee88

Cite this

@article{014ad1bc8fb846c49a0ed0af3b1db930,

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

abstract = "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.",

keywords = "galaxies: active, galaxies: evolution, galaxies: star formation, galaxies: structure",

author = "Kexin Guo and Yingjie Peng and Li Shao and Hai Fu and Barbara Catinella and Luca Cortese and Feng Yuan and Renbin Yan and Chengpeng Zhang and Jing Dou",

note = "Funding Information: We thank the anonymous referee for their valuable comments and suggestions that helped to improve the manuscript. We thank the discussions with Prof. Jing Wang, Prof. Martin Bureau, Prof. Michele Cappellari, Prof. Chris Lintott, and Dr. Zhi-zheng Pan. The first author is grateful for the constant encouragement of Prof. Xian-zhong Zheng. Y.P. acknowledges support from the National Key Program for Science and Technology Research and Development under grant No. 2016YFA0400702, and the NSFC grant No. 11773001. H.F. acknowledges support from the National Science Foundation under grant AST-1614326. Parts of this research were conducted by the Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), through project number CE170100013. This research is also supported jointly by China National Postdoctoral Science Foundation, China Scholarship Council and The International Centre for Radio Astronomy Research. Funding Information: Funding for the Sloan Digital Sky Survey IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science, and the Participating Institutions. SDSS-IV acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. The SDSS website is www.sdss.org. SDSS-IV is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS Collaboration including the Brazilian Participation Group, the Carnegie Institution for Science, Carnegie Mellon University, the Chilean Participation Group, the French Participation Group, Harvard-Smithsonian Center for Astrophysics, Instituto de Astrof{\'i}sica de Canarias, The Johns Hopkins University, Kavli Institute for the Physics and Mathematics of the Universe (IPMU)/University of Tokyo, Lawrence Berkeley National Laboratory, Leibniz Institut f{\"u}r Astrophysik Potsdam (AIP), Max-Planck-Institut f{\"u}r Astronomie (MPIA Heidelberg), Max-Planck-Institut f{\"u}r Astrophysik (MPA Garching), Max-Planck-Institut f{\"u}r Extraterrestrische Physik (MPE), National Astronomical Observatories of China, New Mexico State University, New York University, University of Notre Dame, Observat{\'a}rio Nacional/MCTI, The Ohio State University, Pennsylvania State University, Shanghai Astronomical Observatory, United Kingdom Participation Group, Universidad Nacional Aut{\'o}noma de M{\'e}xico, University of Arizona, University of Colorado Boulder, University of Oxford, University of Portsmouth, University of Utah, University of Virginia, University of Washington, University of Wisconsin, Vanderbilt University, and Yale University. Publisher Copyright: {\textcopyright} 2018. The American Astronomical Society. All rights reserved..",

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doi = "10.3847/1538-4357/aaee88",

language = "English",

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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 - Funding Information: We thank the anonymous referee for their valuable comments and suggestions that helped to improve the manuscript. We thank the discussions with Prof. Jing Wang, Prof. Martin Bureau, Prof. Michele Cappellari, Prof. Chris Lintott, and Dr. Zhi-zheng Pan. The first author is grateful for the constant encouragement of Prof. Xian-zhong Zheng. Y.P. acknowledges support from the National Key Program for Science and Technology Research and Development under grant No. 2016YFA0400702, and the NSFC grant No. 11773001. H.F. acknowledges support from the National Science Foundation under grant AST-1614326. Parts of this research were conducted by the Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), through project number CE170100013. This research is also supported jointly by China National Postdoctoral Science Foundation, China Scholarship Council and The International Centre for Radio Astronomy Research. Funding Information: Funding for the Sloan Digital Sky Survey IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science, and the Participating Institutions. SDSS-IV acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. The SDSS website is www.sdss.org. SDSS-IV is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS Collaboration including the Brazilian Participation Group, the Carnegie Institution for Science, Carnegie Mellon University, the Chilean Participation Group, the French Participation Group, Harvard-Smithsonian Center for Astrophysics, Instituto de Astrofísica de Canarias, The Johns Hopkins University, Kavli Institute for the Physics and Mathematics of the Universe (IPMU)/University of Tokyo, Lawrence Berkeley National Laboratory, Leibniz Institut für Astrophysik Potsdam (AIP), Max-Planck-Institut für Astronomie (MPIA Heidelberg), Max-Planck-Institut für Astrophysik (MPA Garching), Max-Planck-Institut für Extraterrestrische Physik (MPE), National Astronomical Observatories of China, New Mexico State University, New York University, University of Notre Dame, Observatário Nacional/MCTI, The Ohio State University, Pennsylvania State University, Shanghai Astronomical Observatory, United Kingdom Participation Group, Universidad Nacional Autónoma de México, University of Arizona, University of Colorado Boulder, University of Oxford, University of Portsmouth, University of Utah, University of Virginia, University of Washington, University of Wisconsin, Vanderbilt University, and Yale University. 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

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

Abstract

Bibliographical note

Keywords

ASJC Scopus subject areas

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