The SAMI Galaxy Survey: stellar population and structural trends across the Fundamental Plane
| Autor: | Sarah Brough, Nicholas Scott, Arjen van der Wel, Sarah M. Sweet, Matt S. Owers, Julia J. Bryant, Jon Lawrence, Matthew Colless, Michael Goodwin, Rob Sharp, Scott M. Croom, Nuria P. F. Lorente, Brent Groves, Francesco D'Eugenio, Samuel N. Richards, Joss Bland-Hawthorn, Jesse van de Sande, Sree Oh, Roger L. Davies |
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| Rok vydání: | 2021 |
| Předmět: |
ABSORPTION-LINE SPECTRA
formation [galaxies] Stellar population DATA RELEASE FOS: Physical sciences Astrophysics Astrophysics::Cosmology and Extragalactic Astrophysics 01 natural sciences SPATIALLY-RESOLVED SPECTROSCOPY Virial theorem cD Luminosity 0103 physical sciences TO-LIGHT RATIO 010303 astronomy & astrophysics evolution [galaxies] Astrophysics::Galaxy Astrophysics STAR-FORMATION HISTORIES Physics 010308 nuclear & particles physics Plane (geometry) Astronomy and Astrophysics Virial mass Observable stellar content [galaxies] ATLAS(3D) PROJECT Astrophysics - Astrophysics of Galaxies Galaxy spiral [galaxies] Physics and Astronomy Space and Planetary Science Astrophysics of Galaxies (astro-ph.GA) MASS ASSEMBLY GAMA MULTI-GAUSSIAN EXPANSION DIGITAL SKY SURVEY QUIESCENT GALAXIES Fundamental plane (elliptical galaxies) elliptical and lenticular [galaxies] |
| Zdroj: | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY |
| ISSN: | 0035-8711 1365-2966 |
| DOI: | 10.48550/arxiv.2104.10167 |
| Popis: | 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 (MGE) photometric measurements, and treating luminosity as the dependent variable, the FP has coefficients a=1.294$\pm$0.039, b= 0.912$\pm$0.025, and zero-point c= 7.067$\pm$0.078. We leverage the high signal-to-noise of SAMI integral field spectroscopy, to determine how structural and stellar-population observables affect the scatter about the FP. The FP residuals correlate most strongly (8$\sigma$ significance) with luminosity-weighted simple-stellar-population (SSP) age. In contrast, the structural observables surface mass density, rotation-to-dispersion ratio, S\'ersic 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 $\Upsilon_\star$) 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 $\Upsilon_\star$. This correlation implies that part of the FP scatter is due to the broad age and $\Upsilon_\star$ distribution at any given surface mass density. Using virial mass and $\Upsilon_\star$ 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%) of the FP scatter, on their own they do not explain the observed tilt of the FP away from the virial plane. Comment: 36 pages, 23 figures |
| Databáze: | OpenAIRE |
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