Quasar Luminosity Function at z=7

被引：30

作者：

Matsuoka, Yoshiki ^{[1
]}

Onoue, Masafusa ^{[2
]}

Iwasawa, Kazushi ^{[3
,4
]}

Strauss, Michael A. ^{[5
]}

Kashikawa, Nobunari ^{[6
]}

Izumi, Takuma ^{[7
]}

Nagao, Tohru ^{[1
]}

Imanishi, Masatoshi ^{[7
,8
]}

Akiyama, Masayuki ^{[9
]}

Silverman, John D. ^{[10
]}

Asami, Naoko ^{[11
]}

Bosch, James ^{[5
]}

Furusawa, Hisanori ^{[7
]}

Goto, Tomotsugu ^{[12
,13
]}

Gunn, James E. ^{[5
]}

Harikane, Yuichi ^{[14
]}

Ikeda, Hiroyuki ^{[15
]}

Inayoshi, Kohei ^{[2
]}

Ishimoto, Rikako ^{[6
]}

Kawaguchi, Toshihiro ^{[16
]}

Kikuta, Satoshi ^{[17
]}

Kohno, Kotaro ^{[18
,19
]}

Komiyama, Yutaka ^{[7
,8
]}

Lee, Chien-Hsiu ^{[20
]}

Lupton, Robert H. ^{[5
]}

Minezaki, Takeo ^{[18
]}

Miyazaki, Satoshi ^{[7
,8
]}

Murayama, Hitoshi ^{[10
,21
,22
]}

Nishizawa, Atsushi J. ^{[23
]}

Oguri, Masamune ^{[24
,25
]}

Ono, Yoshiaki ^{[14
]}

Oogi, Taira ^{[1
]}

Ouchi, Masami ^{[7
,10
,14
]}

Price, Paul A. ^{[5
]}

Sameshima, Hiroaki ^{[18
]}

Sugiyama, Naoshi ^{[10
,26
]}

Tait, Philip J. ^{[27
]}

Takada, Masahiro ^{[10
]}

Takahashi, Ayumi ^{[28
]}

Takata, Tadafumi ^{[7
,8
]}

Tanaka, Masayuki ^{[7
,8
]}

Toba, Yoshiki ^{[1
,7
,29
]}

Wang, Shiang-Yu ^{[29
]}

Yamashita, Takuji ^{[7
]}

机构：

[1] Ehime Univ, Res Ctr Space & Cosm Evolut, Matsuyama, Ehime 7908577, Japan

[2] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China

[3] Univ Barcelona, IEEC UB, ICREA, Marti & Franques 1, E-08028 Barcelona, Spain

[4] Univ Barcelona, IEEC UB, Inst Ciencies Cosmos, Marti & Franques 1, E-08028 Barcelona, Spain

[5] Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA

[6] Univ Tokyo, Sch Sci, Dept Astron, Tokyo 1130033, Japan

[7] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan

[8] Grad Univ Adv Studies SOKENDAI, Dept Astron Sci, Mitaka, Tokyo 1818588, Japan

[9] Tohoku Univ, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan

[10] Univ Tokyo, WPI, Kavli Inst Phys & Math Universe, Kashiwa, Chiba 2778583, Japan

[11] Seisa Univ, Hakone, Kanagawa 2500631, Japan

[12] Natl Tsing Hua Univ, Inst Astron, Hsinchu 30013, Taiwan

[13] Natl Tsing Hua Univ, Dept Phys, Hsinchu 30013, Taiwan

[14] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan

[15] Wakayama Coll, Natl Inst Technol, Gobo, Wakayama 6440023, Japan

[16] Onomichi City Univ, Dept Econ Management & Informat Sci, Onomichi, Hiroshima 7228506, Japan

[17] Univ Tsukuba, Ctr Computat Sci, Tsukuba, Ibaraki 3058577, Japan

[18] Univ Tokyo, Inst Astron, Mitaka, Tokyo 1810015, Japan

[19] Univ Tokyo, Res Ctr Early Universe, Tokyo 1130033, Japan

[20] WM Keck Observ, Kamuela, HI 96743 USA

[21] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA

[22] Ernest Orlando Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA

[23] Nagoya Univ, Inst Adv Res, Furo Cho,Chikusa Ku, Nagoya, Aichi 4648602, Japan

[24] Chiba Univ, Ctr Frontier Sci, 1-33 Yayoi Cho,Inage Ku, Chiba 2638522, Japan

[25] Chiba Univ, Grad Sch Sci, Dept Phys, 1-33 Yayoi Cho,Inage Ku, Chiba 2638522, Japan

[26] Nagoya Univ, Grad Sch Sci, Furo Cho,Chikusa Ku, Nagoya, Aichi 4648602, Japan

[27] Subaru Telescope, Hilo, HI 96720 USA

[28] Ehime Univ, Grad Sch Sci & Engn, Matsuyama, Ehime 7908577, Japan

[29] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2023年 / 949卷 / 02期

基金：

日本学术振兴会; 美国国家科学基金会; 美国国家航空航天局; 日本科学技术振兴机构; 中国国家自然科学基金;

关键词：

HIGH-Z EXPLORATION; DIGITAL SKY SURVEY; HIGH-REDSHIFT QUASARS; X-RAY LUMINOSITY; INTERGALACTIC MEDIUM; Z-GREATER-THAN-5.7; QUASARS; COSMIC EVOLUTION; II; DISCOVERY; GALAXIES; AGN;

D O I：

10.3847/2041-8213/acd69f

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present the quasar luminosity function (LF) at z = 7, measured with 35 spectroscopically confirmed quasars at 6.55 < z < 7.15. The sample of 22 quasars from the Subaru High -z Exploration of Low-Luminosity Quasars (SHELLQs) project, combined with 13 brighter quasars in the literature, covers an unprecedentedly wide range of rest-frame ultraviolet magnitudes over -28 < M-1450 < -23. We found that the binned LF flattens significantly toward the faint end populated by the SHELLQs quasars. A maximum likelihood fit to a double power-law model has a break magnitude M-1450 * = -25.60(-0.30)(+ 0.40), a characteristic density Phi* = -1.35(-0.30)(+0.47) Gpc(-3) mag(-1), and a bright end slope beta = -3.34(-0.57)(+0.49), when the faint-end slope is fixed to alpha = -1.2 as observed at z <= 6. The overall LF shape remains remarkably similar from z = 4 to 7, while the amplitude decreases substantially toward higher redshifts, with a clear indication of an accelerating decline at z >= 6. The estimated ionizing photon density, 10(48.2 +/- 0.1) s(-1) Mpc-3, is less than 1% of the critical rate to keep the intergalactic medium ionized at z = 7, and thus indicates that quasars are not a major contributor to cosmic reionization.

引用

页数：8

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