Article Dans Une Revue Astronomy & Astrophysics - A&A Année : 2025

COSMOS-Web: Stellar mass assembly in relation to dark matter halos across 0.2 < z < 12 of cosmic history

1 Cosmic Dawn Center (DAWN)
2 NBI - Niels Bohr Institute [Copenhagen]
3 LAM - Laboratoire d'Astrophysique de Marseille
4 The University of Texas at Austin, 2515 Speedway Blvd Stop C1400, Austin, TX 78712, USA
5 Laboratory for Multiwavelength Astrophysics, School of Physics and Astronomy, Rochester Institute of Technology, 84 Lomb Memorial Drive, Rochester, NY 14623, USA
6 STSci - Space Telescope Science Institute
7 IAP - Institut d'Astrophysique de Paris
8 ObAS - Observatoire astronomique de Strasbourg
9 Department of Physics and Astronomy, University of Hawaii, Hilo, 200 W Kawili St, Hilo, HI 96720, USA
10 Caltech/IPAC, 1200 E. California Blvd. Pasadena, CA 91125, USA
11 Department of Computer Science [Aalto]
12 DTU Space - National Space Institute [Lyngby]
13 Center for Computational Astrophysics [New York]
14 Institute of Physics, GalSpec, Ecole Polytechnique Federale de Lausanne, Observatoire de Sauverny, Chemin Pegasi 51, 1290 Versoix, Switzerland
15 IAC - Instituto de Astrofisica de Canarias
16 Department of Astrophysical Sciences [Princeton]
17 GSFC - NASA Goddard Space Flight Center
18 Purple Mountain Observatory
19 Department of Physics [Durham University]
20 Department of Physics [Boston]
21 UNIGE - Université de Genève = University of Geneva
22 OAPD - INAF - Osservatorio Astronomico di Padova
23 JPL - Jet Propulsion Laboratory
24 Department of Physics and Astronomy [UCLA, Los Angeles]
25 Department of Astronomy and Astrophysics, University of California, Santa Cruz, 1156 High Street, Santa Cruz, CA 95064, USA
26 UHM - University of Hawai‘i [Mānoa]
27 SU - Sorbonne Université
28 ESO - European Southern Observatory
29 Department of Astronomy [Amherst]
30 Astronomy Centre, Department of Physics and Astronomy, University of Sussex, Falmer, Brighton BN1 9QH, UK
A M Koekemoer
H J Mccracken
L. Paquereau
Y. Dubois
G. Gozaliasl
D. Le Borgne
D. Liu
R. Massey
D. Sanders
M. Trebitsch
J R Weaver

Résumé

We study the stellar mass assembly of galaxies via the stellar mass function (SMF) and the coevolution with dark matter halos via abundance matching in the largest redshift range to date, 0.2 < z < 12. We used the 0.53 deg 2 imaged by JWST from the COSMOS-Web survey, in combination with ancillary imaging in over 30 photometric bands, to select highly complete samples (down to log M /M = 7.5-8.8) in 15 redshift bins. Our results show that the normalization of the SMF monotonically decreases from z = 0.2 to z = 12 with strong mass-dependent evolution. At z > 5, we find increased abundances of massive (log M /M > 10.5) systems compared to predictions from semi-analytical models and hydrodynamical simulations. These findings challenge traditional galaxy formation models by implying integrated star formation efficiencies (SFEs) of ≡ M f -1 b M -1 halo 0.5. We find a flattening of the SMF at the high-mass end that is better described by a double power law at z > 5.5, after correcting for the Eddington bias. At z 5.5, it transitions to a Schechter law, which coincides with the emergence of the first massive quiescent galaxies in the Universe, indicating that physical mechanisms that suppress galaxy growth start to take place at z ∼ 5.5 on a global scale. By integrating the SMF, we trace the cosmic stellar mass density and infer the star formation rate density, which at z > 7.5 agrees remarkably with recent JWST UV luminosity function-derived estimates. This agreement solidifies the emerging picture of rapid galaxy formation leading to increased abundances of bright and massive galaxies in the first ∼0.7 Gyr. However, at z 3.5, we find significant tension (∼0.3 dex) with the cosmic star formation (SF) history from instantaneous SF measures, the causes of which remain poorly understood. We infer the stellar-to-halo mass relation (SHMR) and the SFE from abundance matching out to z = 12, finding a non-monotonic evolution. The SFE has the characteristic strong dependence with mass in the range of 0.02-0.2, and mildly decreases at the low-mass end out to z ∼ 3.5. At z ∼ 3.5, there is an upturn and the SFE increases sharply from ∼0.1 to approach a high SFE of 0.8-1 by z ∼ 10 for log(M h /M ) ≈ 11.5, albeit with large uncertainties. Finally, we use the SHMR to track the SFE and stellar mass growth throughout the halo history and find that they do not grow at the same rate -from the earliest times up until z ∼ 3.5 the halo growth rate outpaces galaxy assembly, but at z > 3.5 halo growth stagnates and accumulated gas reservoirs keep the SF going and galaxies outpace halos.

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insu-04975760 , version 1 (04-03-2025)

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M. Shuntov, O. Ilbert, S. Toft, R C Arango-Toro, H B Akins, et al.. COSMOS-Web: Stellar mass assembly in relation to dark matter halos across 0.2 < z < 12 of cosmic history. Astronomy & Astrophysics - A&A, 2025, 695, pp.A20. ⟨10.1051/0004-6361/202452570⟩. ⟨insu-04975760⟩
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