The distribution and physical properties of high-redshift [O?iii] emitters in a cosmological hydrodynamics simulation
The distribution and physical properties of high-redshift [O?iii] emitters in a cosmological hydrodynamics simulation
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宇宙流体动力学模拟中高红移[O?iii]发射体的分布和物理性质
DOI：
10.1093/mnrasl/sly167
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发表时间：
2018
影响因子：
--
通讯作者：
Nagao Tohru
中科院分区：
文献类型：
--
作者：
Moriwaki Kana;Yoshida Naoki;Shimizu Ikkoh;Harikane Yuichi;Matsuda Yuichi;Matsuo Hiroshi;Hashimoto Takuya;Inoue Akio K;Tamura Yoichi;Nagao Tohru
Recent observations with the Atacama Large Millimeter/submillimeter Array (ALMA) detected far-infrared emission lines such as the [Oiii]line from galaxies atz∼ 7−9. We use a cosmological simulation of galaxy formation to study the physical properties of [Oiii]emitters. In a comoving volume of 50h−1Mpc on a side, we locate 34 galaxies with stellar masses greater thanatz= 9, and more than 270 such galaxies atz= 7. We calculate the [Oiii]luminosities ($L_{{\rm O\,{{\rm {\small{III}}}, 88}}}$) by combining a physical model of Hiiregions with emission line calculations using the photoionization codecloudy. We show that the resulting $L_{{\rm O\,{{\rm {\small{III}}}, 88}}}$, 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 $L_{{\rm O\,{{\rm {\small{III}}}, 88}}}\gt 10^8\, \rm L_{\odot }$ have star formation rates higher than, and the typical metallicity is. The galaxies are hosted by dark matter haloes with masses greater than. We propose to use the [Oiii] 5007 Å line, to be detected byJames Webb Space Telescope, to study the properties of galaxies whose [Oiii]line emission has been already detected with ALMA.
Recent observations with the Atacama Large Millimeter/submillimeter Array (ALMA) detected far-infrared emission lines such as the [Oiii]line from galaxies atz∼ 7−9. We use a cosmological simulation of galaxy formation to study the physical properties of [Oiii]emitters. In a comoving volume of 50h−1Mpc on a side, we locate 34 galaxies with stellar masses greater thanatz= 9, and more than 270 such galaxies atz= 7. We calculate the [Oiii]luminosities ($L_{{\rm O\,{{\rm {\small{III}}}, 88}}}$) by combining a physical model of Hiiregions with emission line calculations using the photoionization codecloudy. We show that the resulting $L_{{\rm O\,{{\rm {\small{III}}}, 88}}}$, 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 $L_{{\rm O\,{{\rm {\small{III}}}, 88}}}\gt 10^8\, \rm L_{\odot }$ have star formation rates higher than, and the typical metallicity is. The galaxies are hosted by dark matter haloes with masses greater than. We propose to use the [Oiii] 5007 Å line, to be detected byJames Webb Space Telescope, to study the properties of galaxies whose [Oiii]line emission has been already detected with ALMA.