TY - JOUR
T1 - GOLDRUSH. IV. Luminosity Functions and Clustering Revealed with 1/44,000,000 Galaxies at z ∼2-7
T2 - Galaxy-AGN Transition, Star Formation Efficiency, and Implication for Evolution at z > 10
AU - Harikane, Yuichi
AU - Ono, Yoshiaki
AU - Ouchi, Masami
AU - Liu, Chengze
AU - Sawicki, Marcin
AU - Shibuya, Takatoshi
AU - Behroozi, Peter S.
AU - He, Wanqiu
AU - Shimasaku, Kazuhiro
AU - Arnouts, Stephane
AU - Coupon, Jean
AU - Fujimoto, Seiji
AU - Gwyn, Stephen
AU - Huang, Jiasheng
AU - Inoue, Akio K.
AU - Kashikawa, Nobunari
AU - Komiyama, Yutaka
AU - Matsuoka, Yoshiki
AU - Willott, Chris J.
N1 - Funding Information:
This paper is based on data collected at the Subaru Telescope and retrieved from the HSC data archive system, which is operated by Subaru Telescope and Astronomy Data Center (ADC) at NAOJ. Data analysis was in part carried out with the cooperation of Center for Computational Astrophysics (CfCA), NAOJ. This work was supported by the joint research program of the Institute for Cosmic Ray Research (ICRR), University of Tokyo.
Funding Information:
Part of the 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. (). 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’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). CADC is operated by the National Research Council of Canada with the support of the Canadian Space Agency.
Funding Information:
The Cosmic Dawn Center is funded by the Danish National Research Foundation under grant No. 140. This project has received funding from the European Union’s Horizon 2020 research and innovation program under the Marie Sklodowska-Curie grant agreement No. 847523 “INTERACTIONS.”
Funding Information:
The HSC collaboration includes the astronomical communities of Japan and Taiwan, and Princeton University. The HSC instrumentation and software were developed by the National Astronomical Observatory of Japan (NAOJ), the Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU), the University of Tokyo, the High Energy Accelerator Research Organization (KEK), the Academia Sinica Institute for Astronomy and Astrophysics in Taiwan (ASIAA), and Princeton University. Funding was contributed by the FIRST program from the Japanese Cabinet Office, MEXT, the Japan Society for the Promotion of Science (JSPS), Japan Science and Technology Agency (JST), the Toray Science Foundation, NAOJ, Kavli IPMU, KEK, ASIAA, and Princeton University.
Funding Information:
The Pan-STARRS1 Surveys (PS1) and the PS1 public science archive have been made possible through contributions by the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg, and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, the Queen’s University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation grant No. AST-1238877, the University of Maryland, Eotvos Lorand University (ELTE), the Los Alamos National Laboratory, and the Gordon and Betty Moore Foundation.
Funding Information:
We thank the anonymous referee for a careful reading and valuable comments that improved the clarity of the paper. We thank Masao Hayashi, Yoshiyuki Inoue, Kentaro Nagamine, Rui Marques Coelho Chaves, Shun Saito, Masayuki Tanaka, Yoshihiko Yamada for useful comments and discussions, and Thibaud Moutard and Yechi Zhang for providing their data of UV luminosity functions. This work is supported by the World Premier International Research Center Initiative (WPI Initiative), the Ministry of Education, Culture, Sports, Science and Technology, Japan, as well as KAKENHI Grant-in-Aid for Scientific Research (19J01222, 20H00180, 21H04467, and 21K13953) through the Japan Society for the Promotion of Science (JSPS).
Publisher Copyright:
© 2022. The Author(s). Published by the American Astronomical Society.
PY - 2022/3/1
Y1 - 2022/3/1
N2 - We present new measurements of rest-UV luminosity functions and angular correlation functions from 4,100,221 galaxies at z ∼2-7 identified in the Subaru/Hyper Suprime-Cam survey and CFHT Large Area U-band Survey. The obtained luminosity functions at z ∼4-7 cover a very wide UV luminosity range of ∼ 0.002-2000LUV∗ combined with previous studies, confirming that the dropout luminosity function is a superposition of the active galactic nucleus (AGN) luminosity function dominant at M UV ≲ -24 mag and the galaxy luminosity function dominant at M UV ≳ -22 mag, consistent with galaxy fractions based on 1037 spectroscopically identified sources. Galaxy luminosity functions estimated from the spectroscopic galaxy fractions show the bright-end excess beyond the Schechter function at ≳2σ levels, possibly made by inefficient mass quenching, low dust obscuration, and/or hidden AGN activity. By analyzing the correlation functions at z ∼2-6 with HOD models, we find a weak redshift evolution (within 0.3 dex) of the ratio of the star formation rate (SFR) to the dark matter accretion rate, SFR/Ṁh, indicating the almost constant star formation efficiency at z ∼2-6, as suggested by our earlier work at z ∼4-7. Meanwhile, the ratio gradually increases with decreasing redshift at z < 5 within 0.3 dex, which quantitatively reproduces the cosmic SFR density evolution, suggesting that the redshift evolution is primarily driven by the increase of the halo number density due to the structure formation, and the decrease of the accretion rate due to the cosmic expansion. Extrapolating this calculation to higher redshifts assuming the constant efficiency suggests a rapid decrease of the SFR density at z > 10 with ∝ 10-0.5(1+z), which will be directly tested with the James Webb Space Telescope.
AB - We present new measurements of rest-UV luminosity functions and angular correlation functions from 4,100,221 galaxies at z ∼2-7 identified in the Subaru/Hyper Suprime-Cam survey and CFHT Large Area U-band Survey. The obtained luminosity functions at z ∼4-7 cover a very wide UV luminosity range of ∼ 0.002-2000LUV∗ combined with previous studies, confirming that the dropout luminosity function is a superposition of the active galactic nucleus (AGN) luminosity function dominant at M UV ≲ -24 mag and the galaxy luminosity function dominant at M UV ≳ -22 mag, consistent with galaxy fractions based on 1037 spectroscopically identified sources. Galaxy luminosity functions estimated from the spectroscopic galaxy fractions show the bright-end excess beyond the Schechter function at ≳2σ levels, possibly made by inefficient mass quenching, low dust obscuration, and/or hidden AGN activity. By analyzing the correlation functions at z ∼2-6 with HOD models, we find a weak redshift evolution (within 0.3 dex) of the ratio of the star formation rate (SFR) to the dark matter accretion rate, SFR/Ṁh, indicating the almost constant star formation efficiency at z ∼2-6, as suggested by our earlier work at z ∼4-7. Meanwhile, the ratio gradually increases with decreasing redshift at z < 5 within 0.3 dex, which quantitatively reproduces the cosmic SFR density evolution, suggesting that the redshift evolution is primarily driven by the increase of the halo number density due to the structure formation, and the decrease of the accretion rate due to the cosmic expansion. Extrapolating this calculation to higher redshifts assuming the constant efficiency suggests a rapid decrease of the SFR density at z > 10 with ∝ 10-0.5(1+z), which will be directly tested with the James Webb Space Telescope.
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U2 - 10.3847/1538-4365/ac3dfc
DO - 10.3847/1538-4365/ac3dfc
M3 - Article
AN - SCOPUS:85126718955
SN - 0067-0049
VL - 259
JO - Astrophysical Journal, Supplement Series
JF - Astrophysical Journal, Supplement Series
IS - 1
M1 - 20
ER -