The LEGA-C and SAMI galaxy surveys: quiescent stellar populations and the mass–size plane across 6 Gyr

Author:

Barone Tania M1234ORCID,D’Eugenio Francesco56ORCID,Scott Nicholas24ORCID,Colless Matthew14ORCID,Vaughan Sam P234ORCID,van der Wel Arjen5ORCID,Fraser-McKelvie Amelia47ORCID,de Graaff Anna8ORCID,van de Sande Jesse24ORCID,Wu(吳柏鋒) Po-Feng9ORCID,Bezanson Rachel10ORCID,Brough Sarah411ORCID,Bell Eric12ORCID,Croom Scott M24ORCID,Cortese Luca47ORCID,Driver Simon7ORCID,Gallazzi Anna R13ORCID,Muzzin Adam14ORCID,Sobral David15ORCID,Bland-Hawthorn Joss24ORCID,Bryant Julia J2416ORCID,Goodwin Michael16,Lawrence Jon S17ORCID,Lorente Nuria P F17ORCID,Owers Matt S1819ORCID

Affiliation:

1. Research School of Astronomy and Astrophysics, The Australian National University, Canberra, ACT 2611, Australia

2. Sydney Institute for Astronomy, School of Physics, The University of Sydney, Sydney, NSW 2006, Australia

3. Centre for Astrophysics and Supercomputing, Swinburne University of Technology, P.O. Box 218, Hawthorn, VIC 3122, Australia

4. ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), Australia

5. Sterrenkundig Observatorium, Universiteit Gent, Krijgslaan 281 S9, B-9000 Gent, Belgium

6. Cavendish Laboratory and Kavli Institute for Cosmology, University of Cambridge, Madingley Rise, Cambridge CB3 0HA, UK

7. International Centre for Radio Astronomy Research, The University of Western Australia, 35 Stirling Hwy, 6009 Crawley, WA, Australia

8. Leiden Observatory, Leiden University, P.O.Box 9513, NL-2300 AA Leiden, The Netherlands

9. Academia Sinica Institute of Astronomy and Astrophysics, No. 1, Section 4, Roosevelt Road, Taipei 10617, Taiwan

10. Department of Physics and Astronomy and PITT PACC, University of Pittsburgh, Pittsburgh, PA 15260, USA

11. School of Physics, University of New South Wales, Sydney, NSW 2052, Australia

12. Department of Astronomy, University of Michigan, 1085 S. University Ave., Ann Arbor, MI, 48109, USA

13. INAF - Osservatorio Astrofisico di Arcetri, Largo Enrico Fermi 5, I-50125 Firenze, Italy

14. Department of Physics and Astronomy, York University, 4700 Keele St., Toronto, Ontario, M3J 1P3, Canada

15. Department of Physics, Lancaster University, Lancaster LA1 4YB, UK

16. Australian Astronomical Optics - USyd, University of Sydney, Sydney, NSW 2006, Australia

17. Australian Astronomical Optics - Maquarie, Macquarie University, Sydney, NSW 2109, Australia

18. Department of Physics and Astronomy, Macquarie University, Sydney, NSW 2109, Australia

19. Astronomy, Astrophysics and Astrophotonics Research Centre, Macquarie University, Sydney, NSW 2109, Australia

Abstract

ABSTRACT We investigate changes in stellar population age and metallicity ([Z/H]) scaling relations for quiescent galaxies from intermediate redshift (0.60 ≤  $z$ ≤ 0.76) using the LEGA-C Survey to low redshift (0.014 ≤  $z$ ≤ 0.10) using the SAMI Galaxy Survey. Specifically, we study how the spatially integrated global age and metallicity of individual quiescent galaxies vary in the mass–size plane, using the stellar mass M* and a dynamical mass proxy derived from the virial theorem MD ∝ σ2 Re. We find that, similarly to at low redshift, the metallicity of quiescent galaxies at 0.60 ≤  $z$ ≤ 0.76 closely correlates with M/Re (a proxy for the gravitational potential or escape velocity), in that galaxies with deeper potential wells are more metal-rich. This supports the hypothesis that the relation arises due to the gravitational potential regulating the retention of metals by determining the escape velocity for metal-rich stellar and supernova ejecta to escape the system and avoid being recycled into later stellar generations. Conversely, we find no correlation between age and surface density ($M/R_\mathrm{e}^2$) at 0.60 ≤  $z$ ≤ 0.76, despite this relation being strong at low redshift. We consider this change in the age–$M/R_\mathrm{e}^2$ relation in the context of the redshift evolution of the star-forming and quiescent mass–size relations, and find our results are consistent with galaxies forming more compactly at higher redshifts and remaining compact throughout their evolution. Furthermore, galaxies appear to quench at a characteristic surface density that decreases with decreasing redshift. The $z$ ∼  0 age–$M/R_\mathrm{e}^2$ relation is therefore a result of building up the quiescent and star-forming populations with galaxies that formed at a range of redshifts and therefore a range of surface densities.

Funder

European Research Council

Australian Government

Australian Research Council

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

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