A surprising abundance of massive quiescent galaxies at 3 &lt; z &lt; 5 in the first data from JWST CEERS

Carnall, A. C.; McLeod, D. J.; McLure, R. J.; Dunlop, J. S.; Begley, R.; Cullen, F.; Donnan, C. T.; Hamadouche, M. L.; Jewell, S. M.; Jones, E. W.; Pollock, C. L.; V., Wild,

doi:10.48550/arxiv.2208.00986

Cited by 3 publications

(7 citation statements)

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“…We find the number density of our sample, defined as the number of galaxies that fit our selection criteria at 𝑧 ∼ 4.2 divided by the effective volume of the TNG300 simulated box, to be 𝑛 = 1.32 × 10 −5 Mpc −3 . This closely resembles the observational number densities calculated by Carnall et al (2022) reflecting massive quiescent galaxies located by JWST at 3 < 𝑧 < 5, and by Schreiber et al (2018) in their study of massive quiescent galaxies at 3 < 𝑧 < 4 identified in the ZFOURGE and 3DHST catalogues (Skelton et al 2014;Straatman et al 2016). The authors of Schreiber et al (2018) report a number density of 2.0 ± 0.3 × 10 −5 𝑛/Mpc −3 for a spectroscopic sample of quiescent galaxies at 3 < 𝑧 < 4 , and the number density of quiescent galaxies in Carnall et al (2022)'s robust sub-sample at 3 < 𝑧 < 4 is found to be 6.3 +3.8 −2.5 × 10 −5 𝑛/Mpc −3 .…”

Section: Results and Discussion: The First Quiescent Central Galaxies...supporting

confidence: 85%

“…This closely resembles the observational number densities calculated by Carnall et al (2022) reflecting massive quiescent galaxies located by JWST at 3 < 𝑧 < 5, and by Schreiber et al (2018) in their study of massive quiescent galaxies at 3 < 𝑧 < 4 identified in the ZFOURGE and 3DHST catalogues (Skelton et al 2014;Straatman et al 2016). The authors of Schreiber et al (2018) report a number density of 2.0 ± 0.3 × 10 −5 𝑛/Mpc −3 for a spectroscopic sample of quiescent galaxies at 3 < 𝑧 < 4 , and the number density of quiescent galaxies in Carnall et al (2022)'s robust sub-sample at 3 < 𝑧 < 4 is found to be 6.3 +3.8 −2.5 × 10 −5 𝑛/Mpc −3 . Valentino et al (2020) show that the number densities of these quiescent galaxies at 3 < 𝑧 < 4 are consistent between simulations and observations.…”

Section: Results and Discussion: The First Quiescent Central Galaxies...supporting

confidence: 85%

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The first quiescent galaxies in TNG300

Hartley

Nelson

Suess

et al. 2023

Monthly Notices of the Royal Astronomical Society

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We identify the first quiescent galaxies in TNG300, the largest volume of the IllustrisTNG cosmological simulation suite, and explore their quenching processes and time evolution to z = 0. We find that the first quiescent galaxies with stellar masses M* > 3 × 1010M⊙ and specific star formation rates sSFR <10−11yr−1 emerge at z ∼ 4.2 in TNG300. Suppression of star formation in these galaxies begins with a thermal mode of AGN feedback at z ∼ 6, and a kinetic feedback mode acts in each galaxy by z ∼ 4.7 to complete the quenching process, which occurs on a time-scale of ∼0.35 Gyr. Surprisingly, we find that the majority of these galaxies are not the main progenitors of their z = 0 descendants; instead, four of the five galaxies fall into more massive galaxies in subsequent mergers at a range of redshifts 2.5 < z < 0.2. By z = 0, these descendants are the centres of galaxy clusters with average stellar masses of 8 × 1011M⊙. We make predictions for the first quenched galaxies to be located by the James Webb Space Telescope (JWST).

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Section: Results and Discussion: The First Quiescent Central Galaxies...supporting

confidence: 85%

Section: Results and Discussion: The First Quiescent Central Galaxies...supporting

confidence: 85%

The first quiescent galaxies in TNG300

Hartley

Nelson

Suess

et al. 2023

Monthly Notices of the Royal Astronomical Society

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“…Recently, Carnall et al (2022) reported that the hosts of both AEGIS 525 and AEGIS 532 are quiescent. That study used the time-dependent quiescent selection criteria sSFR < 0.2/t obs , where t obs is the age of the universe at the redshift of the galaxy.…”

Section: Star Formation Activitymentioning

confidence: 99%

“…At higher redshifts (z = 3-5), the discovery of a growing population of massive (M * > 10 11 M e ) galaxies that fully quenched 1-2 Gyr after the Big Bang further necessitates a rapid and efficient quenching mechanism (Schreiber et al 2018;Forrest et al 2020aForrest et al , 2020bCarnall et al 2022;Labbe et al 2022). However, the role that AGN play in this process is still uncertain, with some models finding that AGN feedback is not the leading mechanism shaping the bright end of the galaxy luminosity function at these redshifts (Yung et al 2019a(Yung et al , 2019b.…”

Section: Introductionmentioning

confidence: 99%

CEERS Key Paper. II. A First Look at the Resolved Host Properties of AGN at 3 < z < 5 with JWST

Kocevski

Schwarz

McGrath

et al. 2023

ApJL

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We report on the host properties of five X-ray-luminous active galactic nuclei (AGN) identified at 3 < z < 5 in the first epoch of imaging from the Cosmic Evolution Early Release Science Survey. Each galaxy has been imaged with the JWST Near-Infrared Camera, which provides rest-frame optical morphologies at these redshifts. We also derive stellar masses and star formation rates for each host by fitting its spectral energy distribution using a combination of galaxy and AGN templates. We find that three of the AGN hosts have spheroidal morphologies, one is a bulge-dominated disk, and one is dominated by pointlike emission. None are found to show strong morphological disturbances that might indicate a recent interaction or merger event. When compared to a sample of mass-matched inactive galaxies, we find that the AGN hosts have morphologies that are less disturbed and more bulge-dominated. Notably, all four of the resolved hosts have rest-frame optical colors consistent with a quenched or poststarburst stellar population. The presence of AGN in passively evolving galaxies at z > 3 is significant because a rapid feedback mechanism is required in most semianalytic models and cosmological simulations to explain the growing population of massive quiescent galaxies observed at these redshifts. Our findings show that AGN can continue to inject energy into these systems after their star formation is curtailed, potentially heating their halos and preventing renewed star formation. Additional observations will be needed to determine what role this feedback may play in helping to quench these systems and/or maintain their quiescent state.

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“…Even with this configuration, the best solution remains a galaxy around z = 5 and with A V ∼ 5. While passive sources at 3 < z < 5 are already emerging in JWST early observations (Carnall et al 2022b ), the existence of a massive source with log(M * /M ) ∼11.56, dusty and quenched at z = 5 in a small surv e y volume is v ery une xpected. The majority of quiescent galaxies that have spectroscopy and studied individually in detail at z ∼ 2-4 to date do not show evidence of abundant dust content (Valentino et al 2020 ).…”

Section: Top-right)mentioning

confidence: 99%

JWST unveils heavily obscured (active and passive) sources up to z ∼ 13

Rodighiero

Bisigello

Iani

et al. 2022

Monthly Notices of the Royal Astronomical Society: Letters

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A wealth of extragalactic populations completely missed at UV-optical wavelengths has been identified in the last decade, combining the deepest HST and Spitzer observations. These dark sources are thought to be dusty and star-forming systems at 3 < z < 5, and major contributors to the stellar mass build up. In this letter, we report an investigation of the deep JWST survey in the SMACS0723 cluster, analysing NIRCam and MIRI images. We search for sources in the F444W band that are undetected in the F200W catalogues. We characterize the properties of these sources via detailed Spectral Energy Distribution (SED) modelling, accounting for a wide set of parameters and star formation histories, after a careful determination of their photometry. Among a robust sample of 20 candidates, we identify a mixed population of very red sources. We highlight the identification of evolved systems, with stellar masses M* ∼ 109–11 M⊙ at 8 < z < 13 characterized by unexpectedly important dust content at those epochs (AV up to ∼5.8 mag), challenging current model predictions. We further identify an extremely red source (F200W-F440W ∼ 7 mag) that can be reproduced only by the spectrum of a passive, quenched galaxy of M* ∼ 1011.56 M⊙ at z ∼ 5, filled of dust (AV ∼ 5 mag).

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A surprising abundance of massive quiescent galaxies at 3 < z < 5 in the first data from JWST CEERS

Cited by 3 publications

References 0 publications

The first quiescent galaxies in TNG300

The first quiescent galaxies in TNG300

CEERS Key Paper. II. A First Look at the Resolved Host Properties of AGN at 3 < z < 5 with JWST

JWST unveils heavily obscured (active and passive) sources up to z ∼ 13

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