Статья

COSMOS2020: The galaxy stellar mass function

J. R. WeaverDimen-sions (ASTRO 3D), Stromlo, AustraliaI. DavidzonNiels Bohr Institute, University of Copenhagen, Jagtvej 128, 2200 Copenhagen N, DenmarkSune ToftNiels Bohr Institute, University of Copenhagen, Jagtvej 128, 2200 Copenhagen N, DenmarkO. IlbertAix Marseille Univ., CNRS, CNES, LAM, 13000 Marseille, FranceH. J. McCrackenSorbonne Université, CNRS, UMR 7095, Institut d'Astrophysique de Paris, 98 bis bd Arago, 75014 Paris, FranceKatriona M. L. GouldCosmic Dawn Center (DAWN) , Copenhagen N, DenmarkC. K. JespersenDepartment of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USACharles L. SteinhardtCosmic Dawn Center (DAWN) , Copenhagen N, DenmarkClaudia del P. LagosInternational Centre for Radio Astronomy Research (ICRAR), M468, University of Western Australia, 35 Stirling Hwy, Crawley, WA 6009, AustraliaP. CapakC. M. CaseyDepartment of Astronomy, The University of Texas at Austin, 2515 Speedway Blvd Stop C1400, Austin, TX 78712, USAN. ChartabThe Observatories of the Carnegie Institution for Science, 813 Santa Barbara St., Pasadena, CA 91101, USAAndreas L. FaisstCaltech/IPAC, MS314-6, 1200 E. California Blvd, Pasadena, CA 91125, USAChristopher C. HaywardCenter for Computational Astrophysics, Flatiron Institute, 162 Fifth Avenue, New York, NY 10010, USAJ. S. KartaltepeLaboratory for Multiwavelength Astrophysics, School of Physics and Astronomy, Rochester Institute of Technology, 84 Lomb Memo-rial Drive, Rochester, NY 14623, USAO. B. KauffmannAix Marseille Univ., CNRS, CNES, LAM, 13000 Marseille, FranceA. M. KoekemoerSpace Telescope Science Institute, 3700 San Martin Dr., Baltimore, MD 21218, USAVasily KokorevNiels Bohr Institute, University of Copenhagen, Jagtvej 128, 2200 Copenhagen N, DenmarkC. LaigleSorbonne Université, CNRS, UMR 7095, Institut d'Astrophysique de Paris, 98 bis bd Arago, 75014 Paris, FranceDaizhong LiuMax-Planck-Institut für Extraterrestrische Physik (MPE), Giessen-bachstr. 1, 85748 Garching, GermanyA. LongDepartment of Astronomy, The University of Texas at Austin, 2515 Speedway Blvd Stop C1400, Austin, TX 78712, USAG. MagdisCosmic Dawn Center (DAWN) , Copenhagen N, DenmarkConor McPartlandCosmic Dawn Center (DAWN) , Copenhagen N, DenmarkB. Milvang-JensenCosmic Dawn Center (DAWN) , Copenhagen N, DenmarkB. MobasherPhysics and Astronomy Department, University of California, 900 University Avenue, Riverside, CA 92521, USAA. MonetiSorbonne Université, CNRS, UMR 7095, Institut d'Astrophysique de Paris, 98 bis bd Arago, 75014 Paris, FranceYingjie PengKavli Institute for Astronomy and Astrophysics, Peking University, 5 Yiheyuan Road, Beijing 100871, PR ChinaD. B. SandersInstitute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822, USAMarko ShuntovSorbonne Université, CNRS, UMR 7095, Institut d'Astrophysique de Paris, 98 bis bd Arago, 75014 Paris, FranceAlbert SneppenNiels Bohr Institute, University of Copenhagen, Jagtvej 128, 2200 Copenhagen N, DenmarkFrancesco ValentinoNiels Bohr Institute, University of Copenhagen, Jagtvej 128, 2200 Copenhagen N, DenmarkL. ZaleskyInstitute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822, USAG. ZamoraniIstituto Nazionale di Astrofisica -Osservatorio di Astrofisica e Scienza dello Spazio, Via Gobetti 93/3, 40129 Bologna, Italy

2023en

ABI

Аннотация

Context. How galaxies form, assemble, and cease their star formation is a central question within the modern landscape of galaxy evolution studies. These processes are indelibly imprinted on the galaxy stellar mass function (SMF), and its measurement and understanding is key to uncovering a unified theory of galaxy evolution. Aims. We present constraints on the shape and evolution of the galaxy SMF, the quiescent galaxy fraction, and the cosmic stellar mass density across 90% of the history of the Universe from z = 7.5 → 0.2 as a means to study the physical processes that underpin galaxy evolution. Methods. The COSMOS survey is an ideal laboratory for studying representative galaxy samples. Now equipped with deeper and more homogeneous near-infrared coverage exploited by the COSMOS2020 catalog, we leverage the large 1.27 deg 2 effective area to improve sample statistics and understand spatial variations (cosmic variance) – particularly for rare, massive galaxies – and push to higher redshifts with greater confidence and mass completeness than previous studies. We divide the total stellar mass function into star-forming and quiescent subsamples through NUVrJ color-color selection. The measurements are then fit with single- and double-component Schechter functions to infer the intrinsic galaxy stellar mass function, the evolution of its key parameters, and the cosmic stellar mass density out to z = 7.5. Finally, we compare our measurements to predictions from state-of-the-art cosmological simulations and theoretical dark matter halo mass functions. Results. We find a smooth, monotonic evolution in the galaxy stellar mass function since z = 7.5, in general agreement with previous studies. The number density of star-forming systems have undergone remarkably consistent growth spanning four decades in stellar mass from z = 7.5 → 2 whereupon high-mass systems become predominantly quiescent (“downsizing”). Meanwhile, the assembly and growth of low-mass quiescent systems only occurred recently, and rapidly. An excess of massive systems at z ≈ 2.5 − 5.5 with strikingly red colors, with some being newly identified, increase the observed number densities to the point where the SMF cannot be reconciled with a Schechter function. Conclusions. Systematics including cosmic variance and/or active galactic nuclei contamination are unlikely to fully explain this excess, and so we speculate that they may be dust-obscured populations similar to those found in far infrared surveys. Furthermore, we find a sustained agreement from z ≈ 3 − 6 between the stellar and dark matter halo mass functions for the most massive systems, suggesting that star formation in massive halos may be more efficient at early times.

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Идентификаторы

DOI: 10.1051/0004-6361/202245581

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Цитирований: 1Использованных источников: 0

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