Detection of the Far-infrared [O iii] and Dust Emission in a Galaxy at Redshift 8.312: Early Metal Enrichment in the Heart of the Reionization Era
By Y. Tamura, Kentarou Mawatari, T. Hashimoto, A. Inoue, E. Zackrisson, L. Christensen, C. Binggeli, Y. Matsuda, H. Matsuo, T. Takeuchi and 12 more. Astrophysical Journal, 2018
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We present the Atacama Large Millimeter/submillimeter Array detection of the [O iii] 88 μm line and rest-frame 90 μm dust continuum emission in a Y-dropout Lyman break galaxy (LBG), MACS0416_Y1 lying behind the Frontier Field cluster MACS J0416.1−2403. This [O iii] detection confirms the LBG with a spectroscopic redshift of z = 8.3118 ± 0.0003, making this object one of the farthest galaxies ever identified spectroscopically. The observed 850 μm flux density of 137 ± 26 μJy corresponds to a de-lensed total infrared (IR) luminosity of if assuming a dust temperature of Tdust = 50 K and an emissivity index of β = 1.5, yielding a large dust mass of . The ultraviolet-to-far-IR spectral energy distribution modeling where the [O iii] emissivity model is incorporated suggests the presence of a young (τage ≈ 4 Myr), star-forming ( yr−1), moderately metal-polluted (Z ≈ 0.2Z⊙) stellar component with a mass of Mstar = 3 × 108 M⊙. An analytic dust mass evolution model with a single episode of star formation does not reproduce the metallicity and dust mass in τage ≈ 4 Myr, suggesting a pre-existing evolved stellar component with Mstar ∼ 3 × 109 M☉ and τage ∼ 0.3 Gyr as the origin of the dust mass.
Subfields: Astronomy and Astrophysics
View Paper: https://www.semanticscholar.org/paper/02491a016f25f9e5fcbf8bbd85929e2c0e7008b4
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In Astronomy and Astrophysics
Citations in the corpus
- Inferences on the timeline of reionization at z ∼ 8 from the KMOS Lens-Amplified Spectroscopic Survey (2019, methodology): “∗∗∗ This object was spectroscopically confirmed by Tamura et al. (2018) at z = 8.31.”
- The GLASS-JWST Early Release Science Program. I. Survey Design and Release Plans (2022, background): “…Labbé et al. 2013; Smit et al. 2014; RobertsBorsani et al. 2016; Castellano et al. 2017; De Barros et al. 2019), or even mature stellar populations governed by strong Balmer breaks (Hashimoto et al. 2018; Tamura et al. 2019; Roberts-Borsani et al. 2020; Strait et al. 2020; Laporte et al. 2021).”