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

Research output: Contribution to journalArticlepeer-review

Abstract

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 [Oiii] 88µm emitters. In a comoving volume of 50h−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 [Oiii] 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 [Oiii] emitters with LOIII,88 > 108 L☉ have star formation rates higher than 3 M☉ yr−1, and the typical metallicity is ∼ 0.1 Z☉. The galaxies are hosted by dark matter halos with masses greater than 1011 M☉. We propose to use the [Oiii] 5007Å line, to be detected by James Webb Space Telescope (JWST), to study the properties of galaxies whose [Oiii] 88µm line emission have been already detected with ALMA.

Original languageEnglish
JournalUnknown Journal
Publication statusPublished - 2018 May 18

Keywords

  • Galaxies: evolution
  • Galaxies: high-redshift
  • Galaxies: ISM

ASJC Scopus subject areas

  • General

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