The SAMI Galaxy Survey: stellar population and structural trends across the Fundamental Plane

Author:

D’Eugenio Francesco12ORCID,Colless Matthew23ORCID,Scott Nicholas34ORCID,van der Wel Arjen1ORCID,Davies Roger L5ORCID,van de Sande Jesse34ORCID,Sweet Sarah M6ORCID,Oh Sree23ORCID,Groves Brent7ORCID,Sharp Rob2ORCID,Owers Matt S89ORCID,Bland-Hawthorn Joss34ORCID,Croom Scott M34ORCID,Brough Sarah310ORCID,Bryant Julia J3411ORCID,Goodwin Michael11,Lawrence Jon S11ORCID,Lorente Nuria P F11ORCID,Richards Samuel N12ORCID

Affiliation:

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

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

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

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

5. Sub-department of Astrophysics, Department of Physics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH, UK

6. School of Mathematics and Physics, University of Queensland, Brisbane, QLD 4072, Australia

7. International Centre for Radio Astronomy Research (ICRAR), University of Western Australia, Crawley, WA 6009, Australia

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

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

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

11. Australian Astronomical Optics, Macquarie University, Sydney, NSW 2109, Australia

12. SOFIA Science Center, USRA, NASA Ames Research Center, Building N232, M/S 232-12, P.O. Box 1, Moffett Field, CA 94035-0001, USA

Abstract

ABSTRACT We study the Fundamental Plane (FP) for a volume- and luminosity-limited sample of 560 early-type galaxies from the SAMI survey. Using r-band sizes and luminosities from new multi-Gaussian expansion photometric measurements, and treating luminosity as the dependent variable, the FP has coefficients a = 1.294 ± 0.039, b = 0.912 ± 0.025, and zero-point c = 7.067 ± 0.078. We leverage the high signal-to-noise ratio of SAMI integral field spectroscopy, to determine how structural and stellar population observables affect the scatter about the FP. The FP residuals correlate most strongly (8σ significance) with luminosity-weighted simple stellar population (SSP) age. In contrast, the structural observables surface mass density, rotation-to-dispersion ratio, Sérsic index, and projected shape all show little or no significant correlation. We connect the FP residuals to the empirical relation between age (or stellar mass-to-light ratio Υ⋆ ) and surface mass density, the best predictor of SSP age amongst parameters based on FP observables. We show that the FP residuals (anti)correlate with the residuals of the relation between surface density and Υ⋆ . This correlation implies that part of the FP scatter is due to the broad age and Υ⋆ distribution at any given surface mass density. Using virial mass and Υ⋆, we construct a simulated FP and compare it to the observed FP. We find that, while the empirical relations between observed stellar population relations and FP observables are responsible for most (75 per cent) of the FP scatter, on their own they do not explain the observed tilt of the FP away from the virial plane.

Funder

H2020

Australian Research Council

STFC

Alfred P. Sloan Foundation

National Science Foundation

U.S. Department of Energy

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

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