FOREVER22: the first bright galaxies with Population III stars at redshifts z ≃ 10-20 and comparisons with JWST data

被引：26

作者：

Yajima, Hidenobu ^{[1
]}

Abe, Makito ^{[1
]}

Fukushima, Hajime ^{[1
]}

Ono, Yoshiaki ^{[2
]}

Harikane, Yuichi ^{[2
]}

Ouchi, Masami ^{[2
,3
,4
]}

Hashimoto, Takuya ^{[5
]}

Khochfar, Sadegh ^{[6
]}

机构：

[1] Univ Tsukuba, Ctr Computat Sci, 1-1-1 Tennodai, Tsukuba, Ibaraki 3058577, Japan

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

[3] Univ Tokyo, Kavli IPMU WPI, 5-1-5 Kashiwanoha, Kashiwa, Chiba 2778583, Japan

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

[5] Univ Tsukuba, Fac Pure & Appl Sci, Tomonaga Ctr Hist Universe TCHoU, Tsukuba, Ibaraki 3058571, Japan

[6] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Scotland

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2023年 / 525卷 / 04期

关键词：

stars: Population III; galaxies: evolution; galaxies: formation; galaxies: high-redshift; BILLION YEARS PROJECT; REMARKABLY LUMINOUS GALAXY; IONIZING PHOTON ESCAPE; DARK-MATTER HALOES; LY-ALPHA; METAL ENRICHMENT; MILLENNIUMTNG PROJECT; CONTINUUM SLOPES; MASS FUNCTION; BLACK-HOLES;

D O I：

10.1093/mnras/stad2497

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We study the formation of the first galaxies in overdense regions modelled by the FORmation and EVolution of galaxies in Extremely overdense Regions motivated by SSA22 (FOREVER22) simulation project. Our simulations successfully reproduce the star formation rates and the M UV-M star relations of candidate galaxies at z similar to 10-14 observed by the JWST. We suggest that the observed galaxies are hosted by dark matter haloes with M-h greater than or similar to 10(10) M-circle dot and are in short-period starburst phases. On the other hand, even simulated massive galaxies in overdense regions cannot reproduce the intense star formation rates and the large stellar masses of observed candidates at z similar to 16. Also, we show that the contribution of Population III stars to the ultraviolet (UV) flux decreases as the stellar mass increases and it is a few per cent for galaxies with M-star similar to 10(7) M-circle dot. Therefore, a part of the observed flux by JWST could be the light from Population III stars. Our simulations suggest that the UV flux can be dominated by Population III stars and the UV slope shows beta less than or similar to -3 if future observations would reach galaxies with M-stars similar to 10(5) M-circle dot at z similar to 20 of which the mass fraction of Population III stars can be greater than 10 per cent.

引用

页码：4832 / 4839

页数：8

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