GOLDRUSH. IV. Luminosity Functions and Clustering Revealed with ∼4,000,000 Galaxies at z ∼ 2-7: Galaxy-AGN Transition, Star Formation Efficiency, and Implication for Evolution at z > 10

被引：151

作者：

Harikane, Yuichi ^{[1
,2
]}

Ono, Yoshiaki ^{[1
]}

Ouchi, Masami ^{[1
,3
,4
,5
]}

Liu, Chengze ^{[6
,7
]}

Sawicki, Marcin ^{[8
,9
]}

Shibuya, Takatoshi ^{[10
]}

Behroozi, Peter S. ^{[11
,12
]}

He, Wanqiu ^{[3
]}

Shimasaku, Kazuhiro ^{[13
,14
]}

Arnouts, Stephane ^{[15
]}

Coupon, Jean ^{[16
]}

Fujimoto, Seiji ^{[17
,18
]}

Gwyn, Stephen ^{[19
]}

Huang, Jiasheng ^{[20
,21
]}

Inoue, Akio K. ^{[22
,23
]}

Kashikawa, Nobunari ^{[13
,14
]}

Komiyama, Yutaka ^{[3
,4
]}

Matsuoka, Yoshiki ^{[24
]}

Willott, Chris J. ^{[19
]}

机构：

[1] Univ Tokyo, Inst Cosm Ray Res, 5-1-5 Kashiwanoha, Kashiwa, Chiba 2778582, Japan

[2] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England

[3] Natl Astron Observ, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan

[4] Grad Univ Adv Studies SOKENDAI, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan

[5] Univ Tokyo, Kavli Inst Phys & Math Universe Kavli IPMU, WPI, 5-1-5 Kashiwanoha, Kashiwa, Chiba, Japan

[6] Shanghai Jiao Tong Univ, Dept Astron, Sch Phys & Astron, Shanghai 200240, Peoples R China

[7] Shanghai Jiao Tong Univ, Shanghai Key Lab Particle Phys & Cosmol, Shanghai 200240, Peoples R China

[8] St Marys Univ, Inst Computat Astrophys, 923 Robie St, Halifax, NS B3H 3C3, Canada

[9] St Marys Univ, Dept Astron & Phys, 923 Robie St, Halifax, NS B3H 3C3, Canada

[10] Kitami Inst Technol, 165 Koen Cho, Kitami, Hokkaido 0908507, Japan

[11] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA

[12] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA

[13] Univ Tokyo, Sch Sci, Dept Astron, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan

[14] Univ Tokyo, Res Ctr Early Universe, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan

[15] Aix Marseille Univ, Lab Astrophys Marseille, CNES, CNRS, Marseille, France

[16] Univ Geneva, Astron Dept, Chemin Ecogia 16, CH-1290 Versoix, Switzerland

[17] Cosm Dawn Ctr DAWN, Copenhagen, Denmark

[18] Univ Copenhagen, Niels Bohr Inst, DK-128 Copenhagen, Denmark

[19] NRC Herzberg Astron & Astrophys, 5071 West Saanich Rd, Victoria, BC V9E 2E7, Canada

[20] Natl Astron Observ China, CASSACA, Beijing, Peoples R China

[21] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA

[22] Waseda Univ, Fac Sci & Engn, Sch Adv Sci & Engn, Dept Phys,Shinjuku Ku, 3-4-1 Okubo, Tokyo 1698555, Japan

[23] Waseda Univ, Fac Sci & Engn, Waseda Res Inst Sci & Engn, Shinjuku Ku, 3-4-1 Okubo, Tokyo 1698555, Japan

[24] Ehime Univ, Res Ctr Space & Cosm Evolut, Bunkyo Cho, Matsuyama, Ehime 7908577, Japan

来源：

ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES | 2022年 / 259卷 / 01期

基金：

日本学术振兴会; 日本科学技术振兴机构; 美国国家科学基金会; 欧盟地平线“2020”; 美国国家航空航天局; 新加坡国家研究基金会;

关键词：

HIGH-Z EXPLORATION; LY-ALPHA EMITTERS; LYMAN-BREAK GALAXIES; HALO OCCUPATION DISTRIBUTION; DEEP SURVEY SXDS; FORMING GALAXIES; BRIGHT END; FAINT-END; SPECTROSCOPIC SURVEY; DATA RELEASE;

D O I：

10.3847/1538-4365/ac3dfc

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present new measurements of rest-UV luminosity functions and angular correlation functions from 4,100,221 galaxies at z similar to 2-7 identified in the Subaru/Hyper Suprime-Cam survey and CFHT Large Area U-band Survey. The obtained luminosity functions at z similar to 4-7 cover a very wide UV luminosity range of similar to 0.002-2000L(UV)(*) 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 less than or similar to -24 mag and the galaxy luminosity function dominant at M-UV greater than or similar to -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 greater than or similar to 2 sigma levels, possibly made by inefficient mass quenching, low dust obscuration, and/or hidden AGN activity. By analyzing the correlation functions at z similar to 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/<(M)over dot>(h) 10 with proportional to 10(-0.5(1+z)), which will be directly tested with the James Webb Space Telescope.

引用

页数：37

共 253 条

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