Galaxy populations in protoclusters at cosmic noon
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2024
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| author | Andrews, Moira Artale, M. Celeste Kumar, Ankit Lee, Kyoung-Soo Florek, Tess Anand, Kaustub Cerdosino, Candela Ciardullo, Robin Firestone, Nicole Gawiser, Eric Gronwall, Caryl Guaita, Lucia Hong, Sungryong Hwang, Ho Seong Lee, Jaehyun Lee, Seong-Kook Padilla, Nelson Park, Jaehong Popescu, Roxana Ramakrishnan, Vandana Song, Hyunmi Cádiz, F. Vivanco Vogelsberger, Mark |
| author_facet | Andrews, Moira Artale, M. Celeste Kumar, Ankit Lee, Kyoung-Soo Florek, Tess Anand, Kaustub Cerdosino, Candela Ciardullo, Robin Firestone, Nicole Gawiser, Eric Gronwall, Caryl Guaita, Lucia Hong, Sungryong Hwang, Ho Seong Lee, Jaehyun Lee, Seong-Kook Padilla, Nelson Park, Jaehong Popescu, Roxana Ramakrishnan, Vandana Song, Hyunmi Cádiz, F. Vivanco Vogelsberger, Mark |
| contents | We investigate the physical properties and redshift evolution of simulated galaxies residing in protoclusters at cosmic noon, to understand the influence of the environment on galaxy formation. This work is to build clear expectations for the ongoing ODIN survey, devoted to mapping large-scale structures at z=2.4, 3.1, and 4.5 using Ly$α$-emitting galaxies (LAEs) as tracers. From the IllustrisTNG simulations, we define subregions centered on the most massive clusters ranked by total stellar mass at z=0 and study the properties of galaxies within, including LAEs. To model the LAE population, we take a semi-analytical approach that assigns Ly$α$ luminosity and equivalent width based on the UV luminosities to galaxies in a probabilistic manner. We investigate stellar mass, star formation rate, major mergers, and specific star formation rate of the population of star-forming galaxies and LAEs in the field and protocluster environment and trace their evolution. We find that the overall shape of the UV luminosity function (LF) in simulated protocluster environments is characterized by a shallower faint-end slope and an excess on the bright end, signaling different formation histories for galaxies therein. The difference is milder for the Ly$α$ LF. While protocluster galaxies follow the same SFR-$M_{\odot}$ scaling relation as average field galaxies, a larger fraction appears to have experienced major mergers in the last 200 Myr and as a result shows enhanced star formation at a ~60% level, leading to a flatter distribution in both SFR and $M_{\odot}$ relative to galaxies in the average field. We find that protocluster galaxies, including LAEs, begin to quench much earlier (z~0.8-1.6) than field galaxies (z~0.5-0.9); our result is in agreement with recent observational results and highlights the importance of large-scale environment on the overall formation history of galaxies. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2410_08412 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Galaxy populations in protoclusters at cosmic noon Andrews, Moira Artale, M. Celeste Kumar, Ankit Lee, Kyoung-Soo Florek, Tess Anand, Kaustub Cerdosino, Candela Ciardullo, Robin Firestone, Nicole Gawiser, Eric Gronwall, Caryl Guaita, Lucia Hong, Sungryong Hwang, Ho Seong Lee, Jaehyun Lee, Seong-Kook Padilla, Nelson Park, Jaehong Popescu, Roxana Ramakrishnan, Vandana Song, Hyunmi Cádiz, F. Vivanco Vogelsberger, Mark Astrophysics of Galaxies Cosmology and Nongalactic Astrophysics We investigate the physical properties and redshift evolution of simulated galaxies residing in protoclusters at cosmic noon, to understand the influence of the environment on galaxy formation. This work is to build clear expectations for the ongoing ODIN survey, devoted to mapping large-scale structures at z=2.4, 3.1, and 4.5 using Ly$α$-emitting galaxies (LAEs) as tracers. From the IllustrisTNG simulations, we define subregions centered on the most massive clusters ranked by total stellar mass at z=0 and study the properties of galaxies within, including LAEs. To model the LAE population, we take a semi-analytical approach that assigns Ly$α$ luminosity and equivalent width based on the UV luminosities to galaxies in a probabilistic manner. We investigate stellar mass, star formation rate, major mergers, and specific star formation rate of the population of star-forming galaxies and LAEs in the field and protocluster environment and trace their evolution. We find that the overall shape of the UV luminosity function (LF) in simulated protocluster environments is characterized by a shallower faint-end slope and an excess on the bright end, signaling different formation histories for galaxies therein. The difference is milder for the Ly$α$ LF. While protocluster galaxies follow the same SFR-$M_{\odot}$ scaling relation as average field galaxies, a larger fraction appears to have experienced major mergers in the last 200 Myr and as a result shows enhanced star formation at a ~60% level, leading to a flatter distribution in both SFR and $M_{\odot}$ relative to galaxies in the average field. We find that protocluster galaxies, including LAEs, begin to quench much earlier (z~0.8-1.6) than field galaxies (z~0.5-0.9); our result is in agreement with recent observational results and highlights the importance of large-scale environment on the overall formation history of galaxies. |
| title | Galaxy populations in protoclusters at cosmic noon |
| topic | Astrophysics of Galaxies Cosmology and Nongalactic Astrophysics |
| url | https://arxiv.org/abs/2410.08412 |