2013/12/03 by A. K. Inoue, Akio K. Inoue, Ikkoh Shimizu +9 · 1 citation
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics and Star Formation Studies #Emission spectrum #Galaxies: Formation, Evolution, Phenomena #Galaxy #Line (geometry) #Metallicity #Redshift #Spectral line #astro-ph.CO #astro-ph.GA
paper · pdf · doi:10.1088/2041-8205/780/2/l18
published as 2014, ApJ, 780, L18 · ApJL in press
arxiv created 2013/12/03 · openalex publication_date 2013/12/16 · arxiv updated 2014/06/19 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We investigate the potential use of nebular emission lines in the rest-frame far-infrared (FIR) for determining spectroscopic redshift of z > 8 galaxies with the Atacama Large Millimeter/submillimeter Array (ALMA). After making a line emissivity model as a function of metallicity, especially for the [O iii ] 88 μm line which is likely to be the strongest FIR line from H ii regions, we predict the line fluxes from high- z galaxies based on a cosmological hydrodynamics simulation of galaxy formation. Since the metallicity of galaxies reaches at ∼0.2 Z ☉ even at z > 8 in our simulation, we expect the [O iii ] 88 μm line as strong as 1.3 mJy for 27 AB objects, which is detectable at a high significance by <1 hr integration with ALMA. Therefore, the [O iii ] 88 μm line would be the best tool to confirm the spectroscopic redshifts beyond z = 8.