The first quenched galaxies, when and how?
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| Main Authors: | , , , , , , , , , , , , , |
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| Format: | Preprint |
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2024
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| author | Xie, Lizhi De Lucia, Gabriella Fontanot, Fabio Hirschmann, Michaela Bahé, Yannick M Balogh, Michael L. Muzzin, Adam Vulcani, Benedetta Baxter, Devontae C. Forrest, Ben Wilson, Gillian Rudnick, Gregory H. Cooper, M. C. Rescigno, Umberto |
| author_facet | Xie, Lizhi De Lucia, Gabriella Fontanot, Fabio Hirschmann, Michaela Bahé, Yannick M Balogh, Michael L. Muzzin, Adam Vulcani, Benedetta Baxter, Devontae C. Forrest, Ben Wilson, Gillian Rudnick, Gregory H. Cooper, M. C. Rescigno, Umberto |
| contents | Many quiescent galaxies discovered in the early Universe by \textit{JWST} raise fundamental questions on when and how these galaxies became and stayed quenched. Making use of the latest version of the semi-analytic model GAEA that provides good agreement with the observed quenched fractions up to $z\sim 3$, we make predictions for the expected fractions of quiescent galaxies up to $z\sim 7$ and analyze the main quenching mechanism. We find that in a simulated box of $685~{\rm Mpc}$ on a side, the first quenched massive ($M_{\star} \sim 10^{11} {\rm M}_{\odot}$), Milky Way mass, and low mass ($M_{\star} \sim 10^{9.5} {\rm M}_{\odot}$ ) galaxies appear at $z\sim 4.5$, $z\sim 6.2$, and before $z = 7$. Most quenched galaxies identified at early redshifts remain quenched for more than 1 Gyr. Independently of galaxy stellar mass, the dominant quenching mechanism at high redshift is accretion disk feedback (quasar winds) from a central massive black hole, which is triggered by mergers in massive and MW-mass galaxies, and by disk instabilities in low-mass galaxies. Environmental stripping becomes increasingly more important at lower redshift. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2402_01314 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | The first quenched galaxies, when and how? Xie, Lizhi De Lucia, Gabriella Fontanot, Fabio Hirschmann, Michaela Bahé, Yannick M Balogh, Michael L. Muzzin, Adam Vulcani, Benedetta Baxter, Devontae C. Forrest, Ben Wilson, Gillian Rudnick, Gregory H. Cooper, M. C. Rescigno, Umberto Astrophysics of Galaxies Many quiescent galaxies discovered in the early Universe by \textit{JWST} raise fundamental questions on when and how these galaxies became and stayed quenched. Making use of the latest version of the semi-analytic model GAEA that provides good agreement with the observed quenched fractions up to $z\sim 3$, we make predictions for the expected fractions of quiescent galaxies up to $z\sim 7$ and analyze the main quenching mechanism. We find that in a simulated box of $685~{\rm Mpc}$ on a side, the first quenched massive ($M_{\star} \sim 10^{11} {\rm M}_{\odot}$), Milky Way mass, and low mass ($M_{\star} \sim 10^{9.5} {\rm M}_{\odot}$ ) galaxies appear at $z\sim 4.5$, $z\sim 6.2$, and before $z = 7$. Most quenched galaxies identified at early redshifts remain quenched for more than 1 Gyr. Independently of galaxy stellar mass, the dominant quenching mechanism at high redshift is accretion disk feedback (quasar winds) from a central massive black hole, which is triggered by mergers in massive and MW-mass galaxies, and by disk instabilities in low-mass galaxies. Environmental stripping becomes increasingly more important at lower redshift. |
| title | The first quenched galaxies, when and how? |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2402.01314 |