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：128

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：

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

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) <i , indicating the almost constant star formation efficiency at z similar to 2-6, as suggested by our earlier work at z similar to 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 proportional to 10(-0.5(1+z)), which will be directly tested with the James Webb Space Telescope.

引用

页数：37

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 &gt; 10

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