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

Casey, Caitlin M.; Kartaltepe, Jeyhan S.; Drakos, Nicole E.; Franco, Maximilien; Ilbert, O.; Rose, C. A.; Cox, Isabella G.; Nightingale, J. W.; Robertson, Brant; Silverman, John D.; Koekemoer, Anton M.; Massey, Richard; McCracken, H. J.; Rhodes, Jason; Akins, Hollis B.; Amvrosiadis, Aristeidis; Arango-Toro, Rafael C.; Bagley, Micaela B.; Capak, P.; Champagne, Jaclyn B.; Chartab, Nima; Ortiz, Óscar A. Chávez; Cooke, Kevin C.; Cooper, Olivia R.; Darvish, Behnam; Ding, Xuheng; Faisst, Andreas L.; Finkelstein, Steven L.; Fujimoto, Seiji; Gentile, Fabrizio; Gillman, Steven; Gould, Katriona M. L.; Gozaliasl, G.; Harish, S.P.; Hayward, Christopher C.; He, Qiuhan; Hemmati, Shoubaneh; Hirschmann, Michaela; Jin, S.; Khostovan, Ali Ahmad; Kokorev, Vasily; Lambrides, Erini; Laigle, C.; Leung, Gene C. K.; Liu, Daizhong; Liaudat, Tobias; Long, Arianna S.; Magdis, G.; Mahler, Guillaume; Mainieri, V.; Manning, Sinclaire M.; Maraston, Claudia; Martin, Crystal L.; McCleary, Jacqueline; McKinney, Jed; McPartland, Conor; Mobasher, Bahram; Pattnaik, Rohan; Renzini, A.; Rich, R. Michael; Sanders, David B.; Sattari, Zahra; Scognamiglio, D.; Scoville, N. Z.; Sheth, Kartik; Shuntov, Marko; Sparre, Martin; Suzuki, Tomoko L.; Talia, M.; Toft, Sune; Trakhtenbrot, Benny; Urry, C. Megan; Valentino, Francesco; Vanderhoof, Brittany N.; Vardoulaki, E.; Weaver, John R.; Whitaker, Katherine E.; Wilkins, Stephen M.; Liu, Yang; Zavala, Jorge A.

doi:10.48550/arxiv.2211.07865

Cited by 14 publications

(14 citation statements)

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“…The HST-dark galaxy A is unambiguously detected and resolved with JWST though, an important question that remains is whether JWST can detect (see a similar discussion for HST in Dey et al 1999) similarly dusty objects that are unlensed at higher redshift, especially the JWST prospects on dusty galaxies in the Epoch of Reionization (z > 6). To answer this, we compare the best-fit SED model of galaxy A at different redshifts with the depths of major JWST surveys, including UNCOVER (PIs: I. Labbe, R. Bezanson et al 2022), CEERS (PI: S. Finkelstein; Bagley et al 2022) and COSMOS-Web (PIs: J. Kartaltepe, C. Casey et al 2022). At higher redshift, galaxies are less massive and more compact given the mass-size relation (e.g., see van der Wel et al 2014).…”

Section: Detectability At Higher Zmentioning

confidence: 99%

JWST Insight into a Lensed HST-dark Galaxy and Its Quiescent Companion at z = 2.58

Kokorev

Jin

Magdis

et al. 2023

ApJL

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Using the novel James Webb Space Telescope (JWST)/NIRCam observations in the A2744 field, we present a first spatially resolved overview of a Hubble Space Telescope (HST)-dark galaxy, spectroscopically confirmed at z = 2.58 with magnification μ ≈ 1.9. While being largely invisible at ∼1 μm with NIRCam, except for sparse clumpy substructures, the object is well detected and resolved in the long-wavelength bands with a spiral shape clearly visible in F277W. By combining ancillary Atacama Large Millimeter/submillimeter Array (ALMA) and Herschel data, we infer that this object is an edge-on dusty spiral with an intrinsic stellar mass log (M */M ⊙) ∼ 11.3 and a dust-obscured star formation rate ∼300 M ⊙ yr−1. A massive quiescent galaxy (log (M */M ⊙) ∼ 10.8) with tidal features lies 2.″0 away (r ∼ 9 kpc), at a consistent redshift as inferred by JWST photometry, indicating a potential major merger. The dusty spiral lies on the main sequence of star formation, and shows high dust attenuation in the optical (3 < A V < 4.5). In the far-infrared, its integrated dust spectral energy distribution is optically thick up to λ 0 ∼ 500 μm, further supporting the extremely dusty nature. Spatially resolved analysis of the HST-dark galaxy reveals a largely uniform A V ∼ 4 area spanning ∼57 kpc2, which spatially matches to the ALMA 1 mm continuum emission. Accounting for the surface brightness dimming and the depths of current JWST surveys, unlensed analogs of the HST-dark galaxy at z > 4 would be only detectable in F356W and F444W in an UNCOVER-like survey, and become totally JWST-dark at z ∼ 6. This suggests that detecting highly attenuated galaxies in the Epoch of Reionization might be a challenging task for JWST.

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Section: Detectability At Higher Zmentioning

confidence: 99%

JWST Insight into a Lensed HST-dark Galaxy and Its Quiescent Companion at z = 2.58

Kokorev

Jin

Magdis

et al. 2023

ApJL

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“…mAB > 29), its relatively narrow field of view is not expected to significantly increase survey area compared to past Hubble surveys. Wide-field JWST programs, such as Cycle 1 GO/Treasury program COSMOS-Web (Kartaltepe et al 2021;Casey et al 2022, ∼ 0.60 deg 2 ), will still be able to cover areas that are comparable to a handful of WFI pointings and are therefore an important pathfinder to inform future Roman deep-field survey strategies. Thanks to the excellent launch delivered by ESA and Arianespace that resulted in significant conservation of JWST 's on-board fuel, its expected mission lifespan has been prolonged to upwards of 15 to 20 years.…”

mentioning

confidence: 99%

Semi-analytic forecasts for Roman – the beginning of a new era of deep-wide galaxy surveys

Yung

Somerville

Finkelstein

et al. 2022

Monthly Notices of the Royal Astronomical Society

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The Nancy Grace Roman Space Telescope, NASA’s next flagship observatory, will redefine deep-field galaxy survey with a field of view two orders of magnitude larger than Hubble and an angular resolution of matching quality. These future deep-wide galaxy surveys necessitate new simulations to forecast their scientific output and to optimise survey strategies. In this work, we present five realizations of 2-deg2 lightcones, containing a total of ≳ 25 million simulated galaxies with −16 ≳ MUV ≳ −25 spanning z ∼ 0 to 10. This dataset enables a new set of experiments with the impacts of survey size on the derived galaxy formation and cosmological constraints. The intrinsic and observable galaxy properties are predicted using a well-established, physics-based semi-analytic modelling approach. We provide forecasts for number density, cosmic SFR, field-to-field variance, and angular two-point correlation functions, and demonstrate how the future wide-field surveys will be able to improve these measurements relative to current generation surveys. We also present a comparison between these lightcones and others that have been constructed with empirical models. The mock lightcones are designed to facilitate the exploration of multi-instrument synergies and connecting with current generation instruments and legacy surveys. In addition to Roman, we also provide photometry for a number of other instruments on upcoming facilities, including Euclid and Rubin, as well as the instruments that are part of many legacy surveys. Full object catalogues and data tables for the results presented in this work are made available through a web-based, interactive portal.

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“…The relative difference in flux between the low-z dusty galaxy SED and the high −z LBG solution for both galaxies is 0.2-0.25 mag in MIRI/F560W and 0.35 in MIRI/F770W. The expected apparent magnitudes in all MIRI bands are 23-24 mag, well above the 5σ sensitivity thresholds of Cycle 1 JWST deep fields with MIRI coverage such as COSMOS-Web and CEERs (Casey et al 2022;Finkelstein et al 2022b).…”

Section: Resultsmentioning

confidence: 84%

“…We first normalize the stack to a continuum flux on the order of ∼10 nJy over λ obs = 2-3.5 μm and assume it to be undetected in F115W and F150W. This represents a plausible scenario given the relative filter depths of JWST Cycle 1 extragalactic deep fields (Bagley et al 2022;Casey et al 2022;Finkelstein et al 2022b) and is similar to CEERS-93316 (Donnan et al 2023) and CEERS2_2159 (Finkelstein et al 2022b), a z = 16.4 LBG candidate selected from CEERS (Bagley et al 2022;Finkelstein et al 2022a). CEERS-93316 has a tentative 2.6σ SCUBA-2 detection (Zavala et al 2023) and environmental evidence (Naidu et al 2022b), both indicating a possible lower-redshift solution at z ∼ 4.8.…”

Section: Resultsmentioning

confidence: 99%

“…Strong emission lines mask the red slope of the dusty template between F277W and F356W, and the SED is further confused with the Lyman break falling halfway between F200W. Such scenarios are possible given the relative filter depths of JWST Cycle 1 NIRCam extragalactic surveys in CEERS (blue; Bagley et al 2022;Finkelstein et al 2022b) and COSMOS-Web (pink; Casey et al 2022) for example. operators, computer support, and office staff employees, especially during the challenging times presented by the COVID-19 pandemic.…”

Section: Discussionmentioning

confidence: 99%

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Broad Emission Lines in Optical Spectra of Hot, Dust-obscured Galaxies Can Contribute Significantly to JWST/NIRCam Photometry

McKinney

Finnerty

Casey

et al. 2023

ApJL

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Selecting the first galaxies at z > 7 − 10 from JWST surveys is complicated by z < 6 contaminants with degenerate photometry. For example, strong optical nebular emission lines at z < 6 may mimic JWST/NIRCam photometry of z > 7–10 Lyman-break galaxies (LBGs). Dust-obscured 3 < z < 6 galaxies in particular are potentially important contaminants, and their faint rest-optical spectra have been historically difficult to observe. A lack of optical emission line and continuum measures for 3 < z < 6 dusty galaxies now makes it difficult to test their expected JWST/NIRCam photometry for degenerate solutions with NIRCam dropouts. Toward this end, we quantify the contribution by strong emission lines to NIRCam photometry in a physically motivated manner by stacking 21 Keck II/NIRES spectra of hot, dust-obscured, massive ( log M * / M ⊙ ≳ 10 – 11 ) and infrared (IR) luminous galaxies at z ∼ 1–4. We derive an average spectrum and measure strong narrow (broad) [O iii]5007 and Hα features with equivalent widths of 130 ± 20 Å (150 ± 50 Å) and 220 ± 30 Å (540 ± 80 Å), respectively. These features can increase broadband NIRCam fluxes by factors of 1.2 − 1.7 (0.2–0.6 mag). Due to significant dust attenuation (A V ∼ 6), we find Hα+[N ii] to be significantly brighter than [O iii]+Hβ and therefore find that emission-line dominated contaminants of high −z galaxy searches can only reproduce moderately blue perceived UV continua of S λ ∝ λ β with β > − 1.5 and z > 4. While there are some redshifts (z ∼ 3.75) where our stack is more degenerate with the photometry of z > 10 LBGs at λ rest ∼ 0.3–0.8 μm , redder filter coverage beyond λ obs > 3.5 μm and far-IR/submillimeter follow-up may be useful for breaking the degeneracy and making a crucial separation between two fairly unconstrained populations, dust-obscured galaxies at z ∼ 3–6 and LBGs at z > 10.

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

Cited by 14 publications

References 0 publications

JWST Insight into a Lensed HST-dark Galaxy and Its Quiescent Companion at z = 2.58

JWST Insight into a Lensed HST-dark Galaxy and Its Quiescent Companion at z = 2.58

Semi-analytic forecasts for Roman – the beginning of a new era of deep-wide galaxy surveys

Broad Emission Lines in Optical Spectra of Hot, Dust-obscured Galaxies Can Contribute Significantly to JWST/NIRCam Photometry

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