@article{oai:nagoya.repo.nii.ac.jp:00028347,
 author = {Tamura, Yoichi and Mawatari, Ken and Hashimoto, Takuya and Inoue, Akio K. and Zackrisson, Erik and Christensen, Lise and Binggeli, Christian and Matsuda, Yuichi and Matsuo, Hiroshi and Takeuchi, Tsutomu T. and Asano, Ryosuke S. and Sunaga, Kaho and Shimizu, Ikkoh and Okamoto, Takashi and Yoshida, Naoki and Lee, Minju M. and Shibuya, Takatoshi and Taniguchi, Yoshiaki and Umehata, Hideki and Hatsukade, Bunyo and Kohno, Kotaro and Ota, Kazuaki},
 issue = {1},
 journal = {The Astrophysical Journal},
 month = {Mar},
 note = {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 LIR=(1.7±0.3)×10^11L⊙ if assuming a dust temperature of T dust = 50 K and an emissivity index of β = 1.5, yielding a large dust mass of 4×10^6M⊙. The ultraviolet-to-far-IR spectral energy distribution modeling where the [O iii] emissivity model is incorporated suggests the presence of a young (τ age ≈ 4 Myr), star-forming (SFR ≈ 60M⊙ yr^−1), moderately metal-polluted (Z ≈ 0.2Z ⊙) stellar component with a mass of M star = 3 × 10^8 M ⊙. An analytic dust mass evolution model with a single episode of star formation does not reproduce the metallicity and dust mass in τ age ≈ 4 Myr, suggesting a pre-existing evolved stellar component with M star ~ 3 × 10^9 M☉ and τage ~ 0.3 Gyr as the origin of the dust mass.},
 title = {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},
 volume = {874},
 year = {2019}
}