@article{06c61c9abb8a4a0189f04f1cb4f091a4,
title = "COSMOS2020: The galaxy stellar mass function: The assembly and star formation cessation of galaxies at 0.2< z ≤ 7.5",
abstract = "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 deg2 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.",
keywords = "Galaxies: evolution, Galaxies: high-redshift, Galaxies: luminosity function, Galaxies: statistics, Mass function",
author = "Weaver, {J. R.} and I. Davidzon and S. Toft and O. Ilbert and McCracken, {H. J.} and Gould, {K. M.L.} and Jespersen, {C. K.} and C. Steinhardt and Lagos, {C. D.P.} and Capak, {P. L.} and Casey, {C. M.} and N. Chartab and Faisst, {A. L.} and Hayward, {C. C.} and Kartaltepe, {J. S.} and Kauffmann, {O. B.} and Koekemoer, {A. M.} and V. Kokorev and C. Laigle and D. Liu and A. Long and Magdis, {G. E.} and McPartland, {C. J.R.} and B. Milvang-Jensen and B. Mobasher and A. Moneti and Y. Peng and Sanders, {D. B.} and M. Shuntov and A. Sneppen and F. Valentino and L. Zalesky and G. Zamorani",
note = "Funding Information: The authors thank Vadim Ruskov, Sidney Lower, Desika Narayanan, Stephen Wilkins, William Roper, Lukas Furtak, and Pratika Dayal for helpful discussions. We are also grateful for the many helpful and constructive comments from the anonymous referee. The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant No. 140. S.T. and J.W. acknowledge support from the European Research Council (ERC) Consolidator Grant funding scheme (project ConTExt, grant No. 648179). O.I. acknowledges the funding of the French Agence Nationale de la Recherche for the project iMAGE (grant ANR-22-CE31-0007). H.J.Mc.C. acknowledges support from the PNCG. I.D. has received funding from the European Union{\textquoteright}s Horizon 2020 research and innovation program under the Marie Sk{\l}odowska-Curie grant agreement No. 896225. This work used the CANDIDE computer system at the IAP supported by grants from the PNCG, CNES, and the DIM-ACAV and maintained by S. Rouberol. B.M.J. is supported in part by Independent Research Fund Denmark grant DFF – 7014-00017. G.E.M. acknowledges the Villum Fonden research grant 13160 “Gas to stars, stars to dust: tracing star formation across cosmic time”. D.R. acknowledges support from the National Science Foundation under grant numbers AST-1614213 and AST-1910107. Y.P. acknowledges National Science Foundation of China (NSFC) Grant No. 12125301, 12192220, 12192222, and the science research grants from the China Manned Space Project with No. CMS-CSST-2021-A07. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. This work is based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO program ID 179.A-2005 and on data products produced by CALET and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. This work is based in part on observations made with the NASA/ESA Hubble Space Telescope, obtained from the Data Archive at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. This research is also partly supported by the Centre National d{\textquoteright}Etudes Spatiales (CNES). These data were obtained and processed as part of the CFHT Large Area U-band Deep Survey (CLAUDS), which is a collaboration between astronomers from Canada, France, and China described in Sawicki et al. (2019). CLAUDS is based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the CFHT which is operated by the National Research Council (NRC) of Canada, the Institut National des Science de l{\textquoteright}Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. CLAUDS uses data obtained in part through the Telescope Access Program (TAP), which has been funded by the National Astronomical Observatories, Chinese Academy of Sciences, and the Special Fund for Astronomy from the Ministry of Finance of China. CLAUDS uses data products from TERAPIX and the Canadian Astronomy Data Centre (CADC) and was carried out using resources from Compute Canada and Canadian Advanced Network For Astrophysical Research (CANFAR). Publisher Copyright: {\textcopyright} 2023 EDP Sciences. All rights reserved.",
year = "2023",
month = sep,
day = "25",
doi = "10.1051/0004-6361/202245581",
language = "English",
volume = "677",
journal = "Astronomy and Astrophysics",
issn = "0004-6361",
publisher = "EDP SCIENCES S A",
}