The ALMaQUEST Survey. XIII. Understanding Radial Trends in Star Formation Quenching via the Relative Roles of Gas Availability and Star Formation Efficiency
Star formation quenching is one of the key processes that shape the evolution of galaxies. In this study, we investigate the changes in molecular gas and star formation properties as galaxies transit from the star-forming main sequence to the passive regime. Our analysis reveals that as galaxies mov...
| Main Authors: | , , , , , , , , , |
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| Format: | Article |
| Language: | English |
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IOP Publishing
2024-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/ad28c1 |
| _version_ | 1797248771256483840 |
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| author | Hsi-An Pan Lihwai Lin Sara L. Ellison Mallory D. Thorp Sebastián F. Sánchez Asa F. L. Bluck Francesco Belfiore Joanna M. Piotrowska Jillian M. Scudder William M. Baker |
| author_facet | Hsi-An Pan Lihwai Lin Sara L. Ellison Mallory D. Thorp Sebastián F. Sánchez Asa F. L. Bluck Francesco Belfiore Joanna M. Piotrowska Jillian M. Scudder William M. Baker |
| author_sort | Hsi-An Pan |
| collection | DOAJ |
| description | Star formation quenching is one of the key processes that shape the evolution of galaxies. In this study, we investigate the changes in molecular gas and star formation properties as galaxies transit from the star-forming main sequence to the passive regime. Our analysis reveals that as galaxies move away from the main sequence toward the green valley the radial profile of specific star formation rate surface density (Σ _sSFR ) is suppressed compared with main-sequence galaxies out to a galactocentric radius of 1.5 R _e (∼7 kpc for our sample). By combining radial profiles of gas fraction ( f _gas ) and star formation efficiency (SFE), we can discern the underlying mechanism that determines Σ _sSFR at different galactocentric radii. Analysis of relative contributions of f _gas and SFE to Σ _sSFR uncovers a diverse range of quenching modes. Star formation in approximately half of our quenching galaxies is primarily driven by a single mode (i.e., either f _gas or SFE), or a combination of both. A collective analysis of all galaxies reveals that the reduction in star formation within the central regions ( R < 0.5 R _e ) is primarily attributable to a decrease in SFE. Conversely, in the disk regions ( R > 0.5 R _e ), both f _gas and SFE contribute to the suppression of star formation. Our findings suggest that multiple quenching mechanisms may be at play in our sample galaxies, and even within a single galaxy. We also compare our observational outcomes with those from galaxy simulations and discuss the implications of our data. |
| first_indexed | 2024-04-24T20:19:53Z |
| format | Article |
| id | doaj.art-beb4ec73ab4b45ce9d0e1bec9d01a993 |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-04-24T20:19:53Z |
| publishDate | 2024-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-beb4ec73ab4b45ce9d0e1bec9d01a9932024-03-22T10:01:34ZengIOP PublishingThe Astrophysical Journal1538-43572024-01-01964212010.3847/1538-4357/ad28c1The ALMaQUEST Survey. XIII. Understanding Radial Trends in Star Formation Quenching via the Relative Roles of Gas Availability and Star Formation EfficiencyHsi-An Pan0https://orcid.org/0000-0002-1370-6964Lihwai Lin1https://orcid.org/0000-0001-7218-7407Sara L. Ellison2https://orcid.org/0000-0002-1768-1899Mallory D. Thorp3Sebastián F. Sánchez4https://orcid.org/0000-0001-6444-9307Asa F. L. Bluck5https://orcid.org/0000-0001-6395-4504Francesco Belfiore6https://orcid.org/0000-0002-2545-5752Joanna M. Piotrowska7Jillian M. Scudder8https://orcid.org/0000-0002-8798-3972William M. Baker9https://orcid.org/0000-0003-0215-1104Department of Physics, Tamkang University , No. 151, Yingzhuan Road, Tamsui District, New Taipei City 251301, TaiwanInstitute of Astronomy and Astrophysics , Academia Sinica, Taipei 10617, TaiwanDepartment of Physics and Astronomy, University of Victoria , Finnerty Road, Victoria, British Columbia V8P 1A1, CanadaDepartment of Physics and Astronomy, University of Victoria , Finnerty Road, Victoria, British Columbia V8P 1A1, Canada; Argelander-Institut für Astronomie, Universität Bonn , Auf dem Hügel 71, 53121 Bonn, GermanyInstituto de Astronomía, Universidad Nacional Autónoma de México , A.P. 70-264, C.P. 04510, México, D.F., MéxicoDepartment of Physics, Florida International University , 11200 SW 8th Street, Miami, FL 33199, USAINAF- Osservatorio Astrofisico di Arcetri , Largo E. Fermi 5, I-50125, Florence, ItalyCahill Center for Astrophysics, California Institute of Technology , 1216 East California Boulevard, Pasadena, CA 91125, USADepartment of Physics & Astronomy, Oberlin College , Oberlin, OH, 44074, USAKavli Institute for Cosmology, University of Cambridge , Madingley Road, Cambridge, CB3 0HA, UK; Cavendish Laboratory–Astrophysics Group, University of Cambridge , 19 JJ Thomson Avenue, Cambridge, CB3 0HE, UKStar formation quenching is one of the key processes that shape the evolution of galaxies. In this study, we investigate the changes in molecular gas and star formation properties as galaxies transit from the star-forming main sequence to the passive regime. Our analysis reveals that as galaxies move away from the main sequence toward the green valley the radial profile of specific star formation rate surface density (Σ _sSFR ) is suppressed compared with main-sequence galaxies out to a galactocentric radius of 1.5 R _e (∼7 kpc for our sample). By combining radial profiles of gas fraction ( f _gas ) and star formation efficiency (SFE), we can discern the underlying mechanism that determines Σ _sSFR at different galactocentric radii. Analysis of relative contributions of f _gas and SFE to Σ _sSFR uncovers a diverse range of quenching modes. Star formation in approximately half of our quenching galaxies is primarily driven by a single mode (i.e., either f _gas or SFE), or a combination of both. A collective analysis of all galaxies reveals that the reduction in star formation within the central regions ( R < 0.5 R _e ) is primarily attributable to a decrease in SFE. Conversely, in the disk regions ( R > 0.5 R _e ), both f _gas and SFE contribute to the suppression of star formation. Our findings suggest that multiple quenching mechanisms may be at play in our sample galaxies, and even within a single galaxy. We also compare our observational outcomes with those from galaxy simulations and discuss the implications of our data.https://doi.org/10.3847/1538-4357/ad28c1Galaxy evolutionInterstellar mediumStar formation |
| spellingShingle | Hsi-An Pan Lihwai Lin Sara L. Ellison Mallory D. Thorp Sebastián F. Sánchez Asa F. L. Bluck Francesco Belfiore Joanna M. Piotrowska Jillian M. Scudder William M. Baker The ALMaQUEST Survey. XIII. Understanding Radial Trends in Star Formation Quenching via the Relative Roles of Gas Availability and Star Formation Efficiency The Astrophysical Journal Galaxy evolution Interstellar medium Star formation |
| title | The ALMaQUEST Survey. XIII. Understanding Radial Trends in Star Formation Quenching via the Relative Roles of Gas Availability and Star Formation Efficiency |
| title_full | The ALMaQUEST Survey. XIII. Understanding Radial Trends in Star Formation Quenching via the Relative Roles of Gas Availability and Star Formation Efficiency |
| title_fullStr | The ALMaQUEST Survey. XIII. Understanding Radial Trends in Star Formation Quenching via the Relative Roles of Gas Availability and Star Formation Efficiency |
| title_full_unstemmed | The ALMaQUEST Survey. XIII. Understanding Radial Trends in Star Formation Quenching via the Relative Roles of Gas Availability and Star Formation Efficiency |
| title_short | The ALMaQUEST Survey. XIII. Understanding Radial Trends in Star Formation Quenching via the Relative Roles of Gas Availability and Star Formation Efficiency |
| title_sort | almaquest survey xiii understanding radial trends in star formation quenching via the relative roles of gas availability and star formation efficiency |
| topic | Galaxy evolution Interstellar medium Star formation |
| url | https://doi.org/10.3847/1538-4357/ad28c1 |
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