Academic Journal
3D-DASH: The Evolution of Size, Shape, and Intrinsic Scatter in Populations of Young and Old Quiescent Galaxies at 0.5 < z < 3
| العنوان: | 3D-DASH: The Evolution of Size, Shape, and Intrinsic Scatter in Populations of Young and Old Quiescent Galaxies at 0.5 < z < 3 |
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| المؤلفون: | Maike Clausen, Katherine E. Whitaker, Ivelina Momcheva, Sam E. Cutler, Katherine A. Suess, John R. Weaver, Tim Miller, Arjen van der Wel, Stijn Wuyts, David Wake, Pieter van Dokkum, Rachel S. Bezanson, Gabriel Brammer, Marijn Franx, Erica J. Nelson, Natasha M. Förster Schreiber |
| المصدر: | The Astrophysical Journal, Vol 971, Iss 1, p 99 (2024) |
| بيانات النشر: | IOP Publishing |
| سنة النشر: | 2024 |
| المجموعة: | Directory of Open Access Journals: DOAJ Articles |
| مصطلحات موضوعية: | Galaxy evolution, Galaxy formation, High-redshift galaxies, Galaxy structure, Astrophysics, QB460-466 |
| الوصف: | We present a study of the growth of the quiescent galaxy population between 0.5 < z < 3 by tracing the number density and structural evolution of a sample of 4518 old and 583 young quiescent galaxies with log( M _⋆ / M _⊙ ) > 10.4, selected from the COSMOS2020 catalog with complementary Hubble Space Telescope F160W imaging from the 3D-DASH survey. Among the quiescent population at z ∼ 2, roughly 50% are recently quenched galaxies; these young quiescent galaxies become increasingly rare toward lower redshift, supporting the idea that the peak epoch of massive galaxy quenching occurred at z > 2. Our data show that while the effective half-light radius of quiescent galaxies generally increases with time, young quiescent galaxies are significantly smaller than their older counterparts at the same redshift. In this work we investigate the connection between this size difference and other structural properties, including axis ratio, color gradients, stellar mass, and the intrinsic scatter in effective radius. We demonstrate that the size difference is driven by the most massive subpopulation (log( M _⋆ / M _⊙ ) > 11) and does not persist when restricting the sample to intermediate-mass galaxies (10.4 < log( M _⋆ / M _⊙ ) < 11). Interestingly, the intrinsic scatter in physical size shows a strong coevolution over the investigated time period and peaks around z ∼ 2 for both populations, only diverging at z < 1. Taken together, and assuming we are not missing a significant population of lower surface brightness galaxies, while the formation and quenching mechanisms that dominate at higher redshifts yield compact remnants, multiple evolutionary pathways may explain the diverse morphologies of galaxies that quench at z < 1. |
| نوع الوثيقة: | article in journal/newspaper |
| اللغة: | English |
| تدمد: | 1538-4357 |
| Relation: | https://doi.org/10.3847/1538-4357/ad528a; https://doaj.org/toc/1538-4357; https://doaj.org/article/5569e1c430884ba6947a6a4b3c476f54 |
| DOI: | 10.3847/1538-4357/ad528a |
| الاتاحة: | https://doi.org/10.3847/1538-4357/ad528a https://doaj.org/article/5569e1c430884ba6947a6a4b3c476f54 |
| رقم الانضمام: | edsbas.B40F2832 |
| قاعدة البيانات: | BASE |
Full Text Finder | تدمد: | 15384357 |
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| DOI: | 10.3847/1538-4357/ad528a |