COSMOS2020: The Galaxy Stellar Mass Function: On the assembly and star formation cessation of galaxies at $0.2\lt z \leq 7.5$

Weaver, J. R.; Davidzon, I.; Toft, S.; Ilbert, O.; McCracken, H. J.; Gould, Katriona M. L.; Jespersen, Christian Kragh; Steinhardt, C.; Lagos, C. D. P.; Capak, P. L.; Casey, C. M.; Chartab, N.; Faisst, A. L.; Hayward, C. C.; Kartaltepe, Jeyhan S.; Kauffmann, O. B.; Koekemoer, Anton M.; Kokorev, V.; Laigle, C.; Liu, D.; Long, A.; Magdis, G. E.; McPartland, Conor; Milvang-Jensen, B.; Mobasher, B.; Moneti, A.; Y., Peng,; Sanders, D. B.; Shuntov, M.; Sneppen, A.; Valentino, F.; Zalesky, L.; G., Zamorani,

doi:10.48550/arxiv.2212.02512

Cited by 6 publications

(15 citation statements)

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“…Our number density estimates from the combined fields are of the order of ∼2.5 × 10 −5 Mpc −3 , consistent with some of the determinations with similar color or sSFR cuts (Schreiber et al 2018a;Merlin et al 2019). Our estimates are ∼2× larger than the most recent measurements in the largest contiguous survey among those considered, COSMOS (Weaver et al 2022a), also when adopting very consistent color selections (Gould et al 2023). Interestingly, earlier determinations in the same field retrieved significantly lower estimates (Muzzin et al 2013;Davidzon et al 2017;Cecchi et al 2019;Girelli et al 2019).…”

Section: A Compendium Of Number Densities Of Massive Quiescentsupporting

confidence: 87%

“…This seems to suggest that cosmic variance and early overdense environments are effective in producing substantial field-to-field variations also at z > 4 (Section 4.3). For reference, our number density estimates in the same massive bin (M å 10 10.6 M e ) are consistent with those in the COSMOS field by Weaver et al (2022a), but 1.8× larger than what was retrieved in the same field but using a color selection similar to ours (Gould et al 2023; see the discussion therein on the agreement with the latest COSMOS2020 number densities). When integrating down to lower mass limits (10 9.5 M e , but not homogenized among different works at this stage, given the impact of different depths at z > 4), we retrieve similar n to that in COSMOS ((1.0 ± 0.3) × 10 −5 Mpc −3 for M å > 10 9.9 M e ; Weaver et al 2022a) and 1.6-2× larger than in large-field HST surveys such as CANDELS (∼7.9 × 10 −6 Mpc −3 for the "complete" sample at M å > 5 × 10 9 M e ; Merlin et al 2019).…”

Section: High-redshift Candidatessupporting

confidence: 86%

“…The difference with previous works is similar in each bin, when available. This is consistent with the expected shape of the stellar mass function of red QGs, roughly peaking and flattening or turning over at ∼10 10.6 M e at these redshifts (Weaver et al 2022a) and revealing a steady buildup of lowermass QGs (Santini et al 2022). Promising low-mass QGs have already been confirmed with JWST/NIRISS at z ∼ 2.5 in the GLASS field (Marchesini et al 2023).…”

Section: A Look At Lower Massessupporting

confidence: 85%

“…Excellent depictions of how many QGs each individual survey or simulation find as a function of redshift are available in the literature (e.g., Straatman et al 2014;Cecchi et al 2019;Girelli et al 2019;Merlin et al 2019;Shahidi et al 2020;Casey et al 2022;Gould et al 2023;Long et al 2022;Weaver et al 2022a). However, drawing direct comparisons among different works and evaluating the impact of various selections is complicated by the introduction of systematic assumptions.…”

Section: A Compendium Of Number Densities Of Massive Quiescentmentioning

confidence: 99%

“…of each 0.5 dex bin to the total cosmic variance by the relative number densities inWeaver et al (2022a). The total cosmic variance is then computed as…”

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confidence: 99%

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

Valentino

Brammer

Gould

et al. 2023

ApJ

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We present the results of a systematic search for candidate quiescent galaxies in the distant universe in 11 JWST fields with publicly available observations collected during the first 3 months of operations and covering an effective sky area of ∼145 arcmin2. We homogeneously reduce the new JWST data and combine them with existing observations from the Hubble Space Telescope. We select a robust sample of ∼80 candidate quiescent and quenching galaxies at 3 < z < 5 using two methods: (1) based on their rest-frame UVJ colors, and (2) a novel quantitative approach based on Gaussian mixture modeling of the near-UV − U, U − V, and V − J rest-frame color space, which is more sensitive to recently quenched objects. We measure comoving number densities of massive (M ⋆ ≥ 1010.6 M ⊙) quiescent galaxies consistent with previous estimates relying on ground-based observations, after homogenizing the results in the literature with our mass and redshift intervals. However, we find significant field-to-field variations of the number densities up to a factor of 2–3, highlighting the effect of cosmic variance and suggesting the presence of overdensities of red quiescent galaxies at z > 3, as could be expected for highly clustered massive systems. Importantly, JWST enables the robust identification of quenching/quiescent galaxy candidates at lower masses and higher redshifts than before, challenging standard formation scenarios. All data products, including the literature compilation, are made publicly available.

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Section: A Compendium Of Number Densities Of Massive Quiescentsupporting

confidence: 87%

Section: High-redshift Candidatessupporting

confidence: 86%

Section: A Look At Lower Massessupporting

confidence: 85%

Section: A Compendium Of Number Densities Of Massive Quiescentmentioning

confidence: 99%

“…of each 0.5 dex bin to the total cosmic variance by the relative number densities inWeaver et al (2022a). The total cosmic variance is then computed as…”

mentioning

confidence: 99%

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

Valentino

Brammer

Gould

et al. 2023

ApJ

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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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Low-surface-brightness Galaxies are Missing in the Observed Stellar Mass Function

Kim

Lee

Gibson

et al. 2023

ApJ

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We investigate the impact of the surface-brightness (SB) limit on the galaxy stellar mass functions (GSMFs) using galaxy catalogs generated from the Horizon Run 5 (HR5) simulation. We compare the stellar-to-halo-mass relation, GSMF, and size–stellar mass relation of the HR5 galaxies with observational data and other cosmological simulations. The mean SB of simulated galaxies are computed using their effective radii, luminosities, and colors. To examine the cosmic SB dimming effect, we compute k-corrections from the spectral energy distributions of individual simulated galaxy at each redshift, apply the k-corrections to the galaxies, and conduct mock surveys based on the various SB limits. We find that the GSMFs are significantly affected by the SB limits at the low-mass end. This approach can ease the discrepancy between the GSMFs obtained from simulations and observations at 0.6 ≲ z ≤ 2. We also find that a redshift survey with an SB selection limit of μ r e = 25 mag arcsec−2 will miss 20% of galaxies with M ⋆ g = 10 9 M ⊙ at z = 0.625. The missing fraction of low-surface-brightness galaxies increases to 35%, 55%, and 80% at z = 0.9, 1.1, and 1.9, respectively, at the same SB limit.

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COSMOS2020: The Galaxy Stellar Mass Function: On the assembly and star formation cessation of galaxies at $0.2\lt z \leq 7.5$

Cited by 6 publications

References 0 publications

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

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

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

Low-surface-brightness Galaxies are Missing in the Observed Stellar Mass Function

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