Investigating the growing population of massive quiescent galaxies at cosmic noon
We explore the buildup of quiescent galaxies using a sample of 28,469 massive ( ★ ≥ 1011M ) galaxies at redshifts 1.5 < < 3.0, drawn from a 17.5 deg2 area (0.33 Gpc3 comoving volume at these redshifts). This allows for a robust study of the quiescent fraction as a function of mass at...
| Autores principales: | , , , , , , , , , , , , |
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| Formato: | Articulo Preprint |
| Lenguaje: | Inglés |
| Publicado: |
2020
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| Materias: | |
| Acceso en línea: | http://sedici.unlp.edu.ar/handle/10915/125002 |
| Aporte de: |
| id |
I19-R120-10915-125002 |
|---|---|
| record_format |
dspace |
| institution |
Universidad Nacional de La Plata |
| institution_str |
I-19 |
| repository_str |
R-120 |
| collection |
SEDICI (UNLP) |
| language |
Inglés |
| topic |
Ciencias Astronómicas galaxies: evolution galaxies: distances and redshifts galaxies: general |
| spellingShingle |
Ciencias Astronómicas galaxies: evolution galaxies: distances and redshifts galaxies: general Sherman, Sydney Jogee, Shardha Florez, Jonathan Stevans, Matthew L. Kawinwanichakij, Lalitwadee Wold, Isak Finkelstein, Steven L. Papovich, Casey Ciardullo, Robin Gronwall, Caryl Cora, Sofía Alejandra Hough, Tomás Vega Martínez, Cristian Antonio Investigating the growing population of massive quiescent galaxies at cosmic noon |
| topic_facet |
Ciencias Astronómicas galaxies: evolution galaxies: distances and redshifts galaxies: general |
| description |
We explore the buildup of quiescent galaxies using a sample of 28,469 massive ( ★ ≥ 1011M ) galaxies at redshifts 1.5 < < 3.0, drawn from a 17.5 deg2 area (0.33 Gpc3 comoving volume at these redshifts). This allows for a robust study of the quiescent fraction as a function of mass at 1.5 < < 3.0 with a sample ∼40 times larger at log( ★/M )≥ 11.5 than previous studies. We derive the quiescent fraction using three methods: specific star-formation rate, distance from the main sequence, and UVJ color-color selection. All three methods give similar values at 1.5 < < 2.0, however the results differ by up to a factor of two at 2.0 < < 3.0. At redshifts 1.5 < < 3.0 the quiescent fraction increases as a function of stellar mass. By = 2, only 3.3 Gyr after the Big Bang, the universe has quenched ∼25% of ★ = 1011M galaxies and ∼45% of ★ = 1012M galaxies. We discuss physical mechanisms across a range of epochs and environments that could explain our results. We compare our results with predictions from hydrodynamical simulations SIMBA and IllustrisTNG and semi-analytic models (SAMs) SAG, SAGE, and Galacticus. The quiescent fraction from IllustrisTNG is higher than our empirical result by a factor of 2 − 5, while those from SIMBA and the three SAMs are lower by a factor of 1.5 − 10 at 1.5 < < 3.0. |
| format |
Articulo Preprint |
| author |
Sherman, Sydney Jogee, Shardha Florez, Jonathan Stevans, Matthew L. Kawinwanichakij, Lalitwadee Wold, Isak Finkelstein, Steven L. Papovich, Casey Ciardullo, Robin Gronwall, Caryl Cora, Sofía Alejandra Hough, Tomás Vega Martínez, Cristian Antonio |
| author_facet |
Sherman, Sydney Jogee, Shardha Florez, Jonathan Stevans, Matthew L. Kawinwanichakij, Lalitwadee Wold, Isak Finkelstein, Steven L. Papovich, Casey Ciardullo, Robin Gronwall, Caryl Cora, Sofía Alejandra Hough, Tomás Vega Martínez, Cristian Antonio |
| author_sort |
Sherman, Sydney |
| title |
Investigating the growing population of massive quiescent galaxies at cosmic noon |
| title_short |
Investigating the growing population of massive quiescent galaxies at cosmic noon |
| title_full |
Investigating the growing population of massive quiescent galaxies at cosmic noon |
| title_fullStr |
Investigating the growing population of massive quiescent galaxies at cosmic noon |
| title_full_unstemmed |
Investigating the growing population of massive quiescent galaxies at cosmic noon |
| title_sort |
investigating the growing population of massive quiescent galaxies at cosmic noon |
| publishDate |
2020 |
| url |
http://sedici.unlp.edu.ar/handle/10915/125002 |
| work_keys_str_mv |
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Repositorios |
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