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

Atacama Large Millimeter/submillimeter Array (ALMA) has enabled us to detect [O III] 88 μm line even at z > 9. To study the properties of high-redshift [O III] emitters, we calculate [O III] 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 [O III] 88 μm luminosity, L_{O III,88}, scales with SFR with slightly larger L_{O III,88} than a local relation. Some [O III] emitters have extended disk-like structure. We propose to use the ratio between [O III] 88 μm line and [O III] 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 [O III] emitters.