An Atlas of Color-selected Quiescent Galaxies at z &gt; 3 in Public JWST Fields

Valentino, F.; Brammer, Gabriel; Gould, Katriona M. L.; Kokorev, Vasily; Fujimoto, Seiji; Jespersen, Christian Kragh; Vijayan, Aswin P.; Weaver, John R.; Ito, K.; Tanaka, Masayuki; Ilbert, O.; Magdis, G.; Whitaker, Katherine E.; Faisst, Andreas L.; Gallazzi, Anna; Gillman, Steven; Giménez-Arteaga, Clara; Gómez-Guijarro, Carlos; Kubo, Mariko; Heintz, K. E.; Hirschmann, Michaela; Oesch, Pascal; Onodera, Makoto; Rizzo, Francesca; Lee, Minju; Strait, Victoria; Toft, Sune

doi:10.3847/1538-4357/acbefa

Cited by 39 publications

(31 citation statements)

References 144 publications

(224 reference statements)

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“…COSMOS-Web will provide the ideal data set for identifying candidate quiescent galaxies and measuring (or placing constraints) on their number densities and relative abundances. Figure 12 highlights the expected number density of massive (M å > 10 10 M e ) quiescent (specific SFR, SFR/M å < 10 −11 yr −1 ) galaxies from the cosmological hydrodynamical simulations IllustrisTNG100 (Pillepich et al 2018), EAGLE (McAlpine et al 2016, and FLARES (Lovell et al 2022), as well as the DREaM semiempirical model (Drakos et al 2022) and predictions from the empirical model of Long et al (2022), in comparison to some of the currently identified quiescent galaxy candidates in the literature (Muzzin et al 2013;Straatman et al 2014;Schreiber et al 2018;Girelli et al 2019;Merlin et al 2019;Shahidi et al 2020;Carnall et al 2023a;Weaver et al 2022a;Gould et al 2023;Valentino et al 2023). Note that each study selects quiescent galaxies slightly differently, and the resulting samples span a range of stellar mass cuts, with the vast majority of candidates having M å > 10 10 M e .…”

Section: The First Quiescent Galaxiesmentioning

confidence: 99%

COSMOS-Web: An Overview of the JWST Cosmic Origins Survey

Casey,

Kartaltepe,

Drakos

et al. 2023

ApJ

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We present the survey design, implementation, and outlook for COSMOS-Web, a 255 hr treasury program conducted by the James Webb Space Telescope in its first cycle of observations. COSMOS-Web is a contiguous 0.54 deg2 NIRCam imaging survey in four filters (F115W, F150W, F277W, and F444W) that will reach 5σ point-source depths ranging ∼27.5–28.2 mag. In parallel, we will obtain 0.19 deg2 of MIRI imaging in one filter (F770W) reaching 5σ point-source depths of ∼25.3–26.0 mag. COSMOS-Web will build on the rich heritage of multiwavelength observations and data products available in the COSMOS field. The design of COSMOS-Web is motivated by three primary science goals: (1) to discover thousands of galaxies in the Epoch of Reionization (6 ≲ z ≲ 11) and map reionization’s spatial distribution, environments, and drivers on scales sufficiently large to mitigate cosmic variance, (2) to identify hundreds of rare quiescent galaxies at z > 4 and place constraints on the formation of the universe’s most-massive galaxies (M ⋆ > 1010 M ⊙), and (3) directly measure the evolution of the stellar-mass-to-halo-mass relation using weak gravitational lensing out to z ∼ 2.5 and measure its variance with galaxies’ star formation histories and morphologies. In addition, we anticipate COSMOS-Web’s legacy value to reach far beyond these scientific goals, touching many other areas of astrophysics, such as the identification of the first direct collapse black hole candidates, ultracool subdwarf stars in the Galactic halo, and possibly the identification of z > 10 pair-instability supernovae. In this paper we provide an overview of the survey’s key measurements, specifications, goals, and prospects for new discovery.

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Section: The First Quiescent Galaxiesmentioning

confidence: 99%

COSMOS-Web: An Overview of the JWST Cosmic Origins Survey

Casey,

Kartaltepe,

Drakos

et al. 2023

ApJ

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“…It is tempting to speculate whether these candidate members, if real, may have had their SFRs truncated below 10% of their peak star-forming episode, one definition of a quiescent galaxy (Nanayakkara et al 2022). Numerous NIRCam imaging studies have informed us that quiescent galaxies are more common than expected at z = 3-4, implying an early and relatively rapid buildup of stellar material in galaxies and/or an efficient conversion rate of gas to stars at early times (Nanayakkara et al 2022;Carnall et al 2023;Valentino et al 2023). A comprehensive investigation of the physical properties and star formation histories of these galaxies/candidates should uncover hints regarding their assembly and their connection to any larger galaxy overdensity.…”

Section: 2mentioning

confidence: 99%

The JWST PEARLS View of the El Gordo Galaxy Cluster and of the Structure It Magnifies

Frye

Pascale

Foo

et al. 2023

ApJ

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The massive galaxy cluster El Gordo (z = 0.87) imprints multitudes of gravitationally lensed arcs onto James Webb Space Telescope Near-Infrared Camera (NIRCam) images. Eight bands of NIRCam imaging were obtained in the “Prime Extragalactic Areas for Reionization and Lensing Science” (“PEARLS”) program. Point-spread function–matched photometry across Hubble Space Telescope and NIRCam filters supplies new photometric redshifts. A new light-traces-mass lens model based on 56 image multiplicities identifies the two mass peaks and yields a mass estimate within 500 kpc of (7.0 ± 0.30) × 1014 M ⊙. A search for substructure in the 140 cluster members with spectroscopic redshifts confirms the two main mass components. The southeastern mass peak that contains the brightest cluster galaxy is more tightly bound than the northwestern one. The virial mass within 1.7 Mpc is (5.1 ± 0.60)×1014 M ⊙, lower than the lensing mass. A significant transverse velocity component could mean the virial mass is underestimated. We contribute one new member to the previously known z = 4.32 galaxy group. Intrinsic (delensed) positions of the five secure group members span a physical extent of ∼60 kpc. 13 additional candidates selected by spectroscopic/photometric constraints are small and faint, with a mean intrinsic luminosity ∼2.2 mag fainter than L *. NIRCam imaging admits a fairly wide range of brightnesses and morphologies for the group members, suggesting a more diverse galaxy population in this galaxy overdensity.

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“…Number densities derived from photometric and spectroscopic observations span ∼2 dex, but they generally remain higher than those extracted from simulations (Ilbert et al 2013;Straatman et al 2014;Davidzon et al 2017;Merlin et al 2018;Schreiber et al 2018;Girelli et al 2019;Merlin et al 2019;Carnall et al 2020;Santini et al 2021;Shahidi et al 2020;Valentino et al 2020;Carnall et al 2022;Valentino et al 2023). The disagreement among observational works and with theoretical predictions is likely due to a mix of several factors, primarily different sample selections and quiescent criteria used together with analyses done using multiple diverse data sets.…”

Section: Number Densitiesmentioning

confidence: 98%

“…The next few years will undoubtedly see our knowledge of QGs at z > 3 grow vastly with the recent launch and successful commissioning of JWST (Rigby et al 2023), for which QGs at z > 3 have already been reported (Carnall et al 2022;Cheng et al 2023;Pérez-González et al 2023;Rodighiero et al 2023;Valentino et al 2023) and even confirmed Carnall et al 2023), as well as ongoing large, groundbased surveys such as the Cosmic Dawn Survey C. J. R. McPartland et al 2023, in preparation).…”

Section: Summary Andmentioning

confidence: 99%

COSMOS2020: Exploring the Dawn of Quenching for Massive Galaxies at 3 < z < 5 with a New Color-selection Method

Gould

Brammer

Valentino

et al. 2023

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We select and characterize a sample of massive (log(M */M ⊙) > 10.6) quiescent galaxies (QGs) at 3 < z < 5 in the latest Cosmological Evolution Survey catalog (COSMOS2020). QGs are selected using a new rest-frame color-selection method, based on their probability of belonging to the quiescent group defined by a Gaussian mixture model (GMM) trained on rest-frame colors (NUV − U, U − V, V − J) of similarly massive galaxies at 2 < z < 3. We calculate the quiescent probability threshold above which a galaxy is classified as quiescent using simulated galaxies from the shark semi-analytical model. We find that, at z ≥ 3 in shark, the GMM/NUVU − VJ method outperforms classical rest-frame UVJ selection and is a viable alternative. We select galaxies as quiescent based on their probability in COSMOS2020 at 3 < z < 5, and compare the selected sample to both UVJ- and NUVrJ-selected samples. We find that, although the new selection matches UVJ and NUVrJ in number, the overlap between color selections is only ∼50%–80%, implying that rest-frame color commonly used at lower-redshift selections cannot be equivalently used at z > 3. We compute median rest-frame spectral energy distributions for our sample and find the median QG at 3 < z < 5 has a strong Balmer/4000 Å break, and residual NUV flux indicating recent quenching. We find the number densities of the entire quiescent population (including post-starbursts) more than doubles from 3.5 ± 2.2 × 10−6 Mpc−3 at 4 < z < 5 to 1.4 ± 0.4 × 10−5 Mpc−3 at 3 < z < 4, confirming that the onset of massive galaxy quenching occurs as early as 3 < z < 5.

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An Atlas of Color-selected Quiescent Galaxies at z > 3 in Public JWST Fields

Cited by 39 publications

References 144 publications

COSMOS-Web: An Overview of the JWST Cosmic Origins Survey

COSMOS-Web: An Overview of the JWST Cosmic Origins Survey

The JWST PEARLS View of the El Gordo Galaxy Cluster and of the Structure It Magnifies

COSMOS2020: Exploring the Dawn of Quenching for Massive Galaxies at 3 < z < 5 with a New Color-selection Method

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