The distribution and physical properties of high-redshift [OIII] emitters in a cosmological hydrodynamics simulation

Kana Moriwaki*, Naoki Yoshida, Ikkoh Shimizu, Yuichi Harikane, Yuichi Matsuda, Hiroshi Matsuo, Takuya Hashimoto, Akio K. Inoue, Yoichi Tamura, Tohru Nagao

*この研究の対応する著者

研究成果: Article査読

20 被引用数 (Scopus)

抄録

Recent observations with the Atacama Large Millimeter/submillimeter Array (ALMA) detected far-infrared emission lines such as the [OIII] 88μm line from galaxies at z ~ 7-9. We use a cosmological simulation of galaxy formation to study the physical properties of [O III] 88μm emitters. In a comoving volume of 50 h-1 Mpc on a side, we locate 34 galaxies with stellar masses greater than 108 M at z = 9, and more than 270 such galaxies at z = 7. We calculate the [O III] 88μm luminosities (LOIII,88) by combining a physical model of HII regions with emission line calculations using the photoionization code CLOUDY.We show that the resulting LOIII,88, for a given star formation rate, is slightly higher than predicted from the empirical relation for local galaxies, and is consistent with recent observations of galaxies at redshifts 7-9. Bright [O III] emitters with LOIII,88 > 108 L have star formation rates higher than 3M yr-1, and the typical metallicity is ~0.1Z. The galaxies are hosted by dark matter haloes with masses greater than 1011M. We propose to use the [OIII] 5007Å line, to be detected by James Webb Space Telescope, to study the properties of galaxies whose [OIII] 88 μm line emission has been already detected with ALMA.

本文言語English
ページ(範囲)L84-L88
ジャーナルMonthly Notices of the Royal Astronomical Society: Letters
481
1
DOI
出版ステータスPublished - 2018 11 21
外部発表はい

ASJC Scopus subject areas

  • 天文学と天体物理学
  • 宇宙惑星科学

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