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

Published online by Cambridge University Press:  10 June 2020

Kana Moriwaki
Kana Moriwaki*
Affiliation:
Department of Physics, The University of Tokyo, 7-3-1 Hongo, Bunkyo, Tokyo113-0033, Japan email: kana.moriwaki@utap.phys.s.u-tokyo.ac.jp
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Abstract

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Atacama Large Millimeter/submillimeter Array (ALMA) has enabled us to detect [Oiii] 88 μm line even at z > 9. To study the properties of high-redshift [Oiii] emitters, we calculate [Oiii] luminosities of galaxies in a cosmological simulation by applying a physical model of Hii region and using the photoionization code cloudy. We find that the [Oiii] 88 μm luminosity, LOIII,88, scales with SFR with slightly larger LOIII,88 than a local relation. Some [Oiii] emitters have extended disk-like structure. We propose to use the ratio between [Oiii] 88 μm line and [Oiii] 5007 Å line, which can be detected with James Webb Space Telescope (JWST), to estimate the gas density and the metallicity in HII region of high-redshift [Oiii] emitters.

Keywords

galaxies: formationgalaxies: high-redshiftgalaxies: ISM
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S341: Challenges in Panchromatic Modelling with Next Generation Facilities , November 2019 , pp. 249 - 252
Copyright
© International Astronomical Union 2020

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