https://scholars.lib.ntu.edu.tw/handle/123456789/633940
標題: | The LEGA-C and SAMI Galaxy Surveys: Quiescent Stellar Populations and the Mass-Size Plane across 6 Gyr | 作者: | Tania M. Barone Francesco D'Eugenio Nicholas Scott Matthew Colless Sam P. Vaughan Arjen van der Wel Amelia Fraser-McKelvie Anna de Graaff Jesse van de Sande PO-FENG WU Rachel Bezanson Sarah Brough Eric Bell Scott M. Croom Luca Cortese Simon Driver Anna R. Gallazzi Adam Muzzin David Sobral Joss Bland-Hawthorn Julia J. Bryant Michael Goodwin Jon S. Lawrence Nuria P. F. Lorente Matt S. Owers |
關鍵字: | galaxies: abundances | galaxies: evolution | galaxies: fundamental parameters | galaxies: statistics | galaxies: stellar content | galaxies: structure; astro-ph.GA; astro-ph.GA | 公開日期: | 2-七月-2021 | 卷: | 512 | 期: | 3 | 來源出版物: | Monthly Notices of the Royal Astronomical Society | 摘要: | We investigate the change in mean stellar population age and metallicity ([Z/H]) scaling relations for quiescent galaxies from intermediate redshift ($0.60\leq z\leq0.76$) using the LEGA-C Survey, to low redshift ($0.014\leq z\leq0.10$) using the SAMI Galaxy Survey. We find that, similarly to their low-redshift counterparts, the stellar metallicity of quiescent galaxies at $0.60\leq z\leq 0.76$ closely correlates with $M_*/R_\mathrm{e}$ (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 required by metal-rich stellar and supernova ejecta to escape the system and avoid being recycled into later stellar generations. On the other hand, we find no correlation between stellar age and $M_*/R_\mathrm{e}^2$ (stellar mass surface density $\Sigma$) in the LEGA-C sample, despite this being a strong relation at low redshift. We consider this change in the age--$\Sigma$ relation in the context of the redshift evolution of the star-forming and quiescent populations in the mass--size plane, and find our results can be explained as a consequence of 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 $z\sim 0$ age--$\Sigma$ relation is therefore a result of building up the quiescent and star-forming populations with galaxies that formed at a range of redshifts and so a range of surface densities. |
描述: | 18 pages, 11 figures, accepted to MNRAS |
URI: | https://scholars.lib.ntu.edu.tw/handle/123456789/633940 | ISSN: | 00358711 | DOI: | 10.1093/mnras/stac705 |
顯示於: | 物理學系 |
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