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...

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Vydáno v:The Astrophysical journal Ročník 964; číslo 2; s. 120 - 141
Hlavní autoři: Pan, Hsi-An, Lin, Lihwai, Ellison, Sara L., Thorp, Mallory D., Sánchez, Sebastián F., Bluck, Asa F. L., Belfiore, Francesco, Piotrowska, Joanna M., Scudder, Jillian M., Baker, William M.
Médium: Journal Article
Jazyk:angličtina
Vydáno: Philadelphia The American Astronomical Society 01.04.2024
IOP Publishing
Témata:
Galactic evolution
Galaxies
Galaxy evolution
Interstellar medium
Molecular gases
Quenching
Star & galaxy formation
Star formation
Star formation rate
Stars
Stars & galaxies
ISSN:0004-637X, 1538-4357
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Abstract 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.
AbstractList 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 (ΣsSFR) is suppressed compared with main-sequence galaxies out to a galactocentric radius of 1.5 Re(∼7 kpc for our sample). By combining radial profiles of gas fraction (fgas) and star formation efficiency (SFE), we can discern the underlying mechanism that determines ΣsSFR at different galactocentric radii. Analysis of relative contributions of fgas and SFE to ΣsSFR 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 fgas 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 Re) is primarily attributable to a decrease in SFE. Conversely, in the disk regions (R > 0.5 Re), both fgas 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.
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.
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.
Author Thorp, Mallory D.
Baker, William M.
Bluck, Asa F. L.
Belfiore, Francesco
Scudder, Jillian M.
Piotrowska, Joanna M.
Lin, Lihwai
Sánchez, Sebastián F.
Pan, Hsi-An
Ellison, Sara L.
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  organization: Tamkang University Department of Physics, No. 151, Yingzhuan Road, Tamsui District, New Taipei City 251301, Taiwan
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  givenname: Lihwai
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  givenname: Sara L.
  orcidid: 0000-0002-1768-1899
  surname: Ellison
  fullname: Ellison, Sara L.
  organization: University of Victoria Department of Physics and Astronomy, Finnerty Road, Victoria, British Columbia V8P 1A1, Canada
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  givenname: Mallory D.
  surname: Thorp
  fullname: Thorp, Mallory D.
  organization: Universität Bonn Argelander-Institut für Astronomie, Auf dem Hügel 71, 53121 Bonn, Germany
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  givenname: Sebastián F.
  orcidid: 0000-0001-6444-9307
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  organization: Universidad Nacional Autónoma de México Instituto de Astronomía, A.P. 70-264, C.P. 04510, México, D.F., México
– sequence: 6
  givenname: Asa F. L.
  orcidid: 0000-0001-6395-4504
  surname: Bluck
  fullname: Bluck, Asa F. L.
  organization: Florida International University Department of Physics, 11200 SW 8th Street, Miami, FL 33199, USA
– sequence: 7
  givenname: Francesco
  orcidid: 0000-0002-2545-5752
  surname: Belfiore
  fullname: Belfiore, Francesco
  organization: INAF- Osservatorio Astrofisico di Arcetri , Largo E. Fermi 5, I-50125, Florence, Italy
– sequence: 8
  givenname: Joanna M.
  surname: Piotrowska
  fullname: Piotrowska, Joanna M.
  organization: California Institute of Technology Cahill Center for Astrophysics, 1216 East California Boulevard, Pasadena, CA 91125, USA
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  givenname: Jillian M.
  orcidid: 0000-0002-8798-3972
  surname: Scudder
  fullname: Scudder, Jillian M.
  organization: Oberlin College Department of Physics & Astronomy, Oberlin, OH, 44074, USA
– sequence: 10
  givenname: William M.
  orcidid: 0000-0003-0215-1104
  surname: Baker
  fullname: Baker, William M.
  organization: University of Cambridge Cavendish Laboratory–Astrophysics Group, 19 JJ Thomson Avenue, Cambridge, CB3 0HE, UK
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SubjectTerms Galactic evolution
Galaxies
Galaxy evolution
Interstellar medium
Molecular gases
Quenching
Star & galaxy formation
Star formation
Star formation rate
Stars
Stars & galaxies
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Title The ALMaQUEST Survey. XIII. Understanding Radial Trends in Star Formation Quenching via the Relative Roles of Gas Availability and Star Formation Efficiency
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