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COSMOS-Web: Intrinsically Luminous z ≳ 10 Galaxy Candidates Test Early Stellar Mass Assembly

Caitlin M. CaseyCosmic Dawn Center (DAWN), DenmarkHollis B. AkinsThe University of Texas at Austin, 2515 Speedway Boulevard, Stop C1400, Austin, TX 78712, USA; [email protected]Marko ShuntovCosmic Dawn Center (DAWN), DenmarkO. IlbertAix Marseille Université, CNRS, CNES, LAM, Marseille, FranceLouise PaquereauInstitut d’Astrophysique de Paris, UMR 7095, CNRS and Sorbonne Université, 98 bis boulevard Arago, F-75014 Paris, FranceMaximilien FrancoThe University of Texas at Austin, 2515 Speedway Boulevard, Stop C1400, Austin, TX 78712, USA; [email protected]Christopher C. HaywardCenter for Computational Astrophysics, Flatiron Institute, 162 Fifth Avenue, New York, NY 10010, USASteven L. FinkelsteinThe University of Texas at Austin, 2515 Speedway Boulevard, Stop C1400, Austin, TX 78712, USA; [email protected]Michael Boylan-KolchinThe University of Texas at Austin, 2515 Speedway Boulevard, Stop C1400, Austin, TX 78712, USA; [email protected]B. E. RobertsonDepartment of Astronomy and Astrophysics, University of California, Santa Cruz, 1156 High Street, Santa Cruz, CA 95064, USAN. AllenCosmic Dawn Center (DAWN), DenmarkMalte BrinchCosmic Dawn Center (DAWN), DenmarkOlivia R. CooperThe University of Texas at Austin, 2515 Speedway Boulevard, Stop C1400, Austin, TX 78712, USA; [email protected]Rachel J. BruchKavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo, Kashiwa, Chiba 277-8583, JapanNicole E. DrakosDepartment of Astronomy and Astrophysics, University of California, Santa Cruz, 1156 High Street, Santa Cruz, CA 95064, USAAndreas L. FaisstCaltech/IPAC, MS 314-6, 1200 E. California Boulevard, Pasadena, CA 91125, USASeiji FujimotoThe University of Texas at Austin, 2515 Speedway Boulevard, Stop C1400, Austin, TX 78712, USA; [email protected]Steven GillmanCosmic Dawn Center (DAWN), DenmarkSantosh HarishLaboratory for Multiwavelength Astrophysics, School of Physics and Astronomy, Rochester Institute of Technology, 84 Lomb Memorial Drive, Rochester, NY 14623, USAMichaela HirschmannINAF, Astronomical Observatory of Trieste, Via Tiepolo 11, 34131 Trieste, ItalyShuowen JinCosmic Dawn Center (DAWN), DenmarkJ. S. KartaltepeLaboratory for Multiwavelength Astrophysics, School of Physics and Astronomy, Rochester Institute of Technology, 84 Lomb Memorial Drive, Rochester, NY 14623, USAA. M. KoekemoerSpace Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USAVasily KokorevKapteyn Astronomical Institute, University of Groningen, PO Box 800, 9700 AV Groningen, The NetherlandsDaizhong LiuMax-Planck-Institut für Extraterrestrische Physik (MPE), Giessenbachstr. 1, D-85748 Garching, GermanyArianna S. LongThe University of Texas at Austin, 2515 Speedway Boulevard, Stop C1400, Austin, TX 78712, USA; [email protected]G. MagdisCosmic Dawn Center (DAWN), DenmarkClaudia MarastonInstitute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Burnaby Road, Portsmouth PO1 3FX, UKCrystal L. MartinDepartment of Physics, University of California Santa Barbara, Santa Barbara, CA 93109, USAH. J. McCrackenInstitut d’Astrophysique de Paris, UMR 7095, CNRS and Sorbonne Université, 98 bis boulevard Arago, F-75014 Paris, FranceJed McKinneyThe University of Texas at Austin, 2515 Speedway Boulevard, Stop C1400, Austin, TX 78712, USA; [email protected]B. MobasherDepartment of Physics and Astronomy, University of California Riverside, 900 University Avenue, Riverside, CA 92521, USAJason RhodesJet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91001, USAR. Michael RichDepartment of Physics and Astronomy, University of California Los Angeles, PAB 430 Portola Plaza, Los Angeles, CA 90095, USAD. B. SandersInstitute for Astronomy, University of Hawai’i at Manoa, 2680 Woodlawn Drive, Honolulu, HI 96822, USAJ. D. SilvermanDepartment of Astronomy, School of Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo, Tokyo 113-0033, JapanSune ToftCosmic Dawn Center (DAWN), DenmarkAswin P. VijayanCosmic Dawn Center (DAWN), DenmarkJ. R. WeaverDepartment of Astronomy, University of Massachusetts, Amherst, MA 01003, USAStephen M. WilkinsAstronomy Centre, University of Sussex, Falmer, Brighton BN1 9QH, UKLilan YangKavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo, Kashiwa, Chiba 277-8583, JapanJorge A. ZavalaNational Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan

2024en

ABI

Аннотация

Abstract We report the discovery of 15 exceptionally luminous 10 ≲ z ≲ 14 candidate galaxies discovered in the first 0.28 deg 2 of JWST/NIRCam imaging from the COSMOS-Web survey. These sources span rest-frame UV magnitudes of −20.5 > M UV > −22, and thus constitute the most intrinsically luminous z ≳ 10 candidates identified by JWST to date. Selected via NIRCam imaging, deep ground-based observations corroborate their detection and help significantly constrain their photometric redshifts. We analyze their spectral energy distributions using multiple open-source codes and evaluate the probability of low-redshift solutions; we conclude that 12/15 (80%) are likely genuine z ≳ 10 sources and 3/15 (20%) likely low-redshift contaminants. Three of our z ∼ 12 candidates push the limits of early stellar mass assembly: they have estimated stellar masses ∼ 5 × 10 9 M ⊙ , implying an effective stellar baryon fraction of ϵ ⋆ ∼ 0.2−0.5, where ϵ ⋆ ≡ M ⋆ /( f b M halo ). The assembly of such stellar reservoirs is made possible due to rapid, burst-driven star formation on timescales < 100 Myr where the star formation rate may far outpace the growth of the underlying dark matter halos. This is supported by the similar volume densities inferred for M ⋆ ∼ 10 10 M ⊙ galaxies relative to M ⋆ ∼ 10 9 M ⊙ —both about 10 −6 Mpc −3 —implying they live in halos of comparable mass. At such high redshifts, the duty cycle for starbursts would be of order unity, which could cause the observed change in the shape of the UV luminosity function from a double power law to a Schechter function at z ≈ 8. Spectroscopic redshift confirmation and ensuing constraints of their masses will be critical to understand how, and if, such early massive galaxies push the limits of galaxy formation in the Lambda cold dark matter paradigm.

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DOI: 10.3847/1538-4357/ad2075

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