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• W3120596863 abstract "ABSTRACT The [O iii] 88 $mu$m fine-structure emission line has been detected into the Epoch of Reionization (EoR) from star-forming galaxies at redshifts 6 &lt; z ≲ 9 with ALMA. These measurements provide valuable information regarding the properties of the interstellar medium (ISM) in the highest redshift galaxies discovered thus far. The [O iii] 88 $mu$m line observations leave, however, a degeneracy between the gas density and metallicity in these systems. Here, we quantify the prospects for breaking this degeneracy using future ALMA observations of the [O iii] 52 $mu$m line. Among the current set of 10 [O iii] 88 $mu$m emitters at 6 &lt; z ≲ 9, we forecast 52 $mu$m detections (at 6σ) in SXDF-NB1006-2, B14-6566, J0217-0208, and J1211-0118 within on-source observing times of 2–10 h, provided their gas densities are larger than about nH ≳ 102–103 cm−3. Other targets generally require much longer integration times for a 6σ detection. Either successful detections of the 52 $mu$m line or reliable upper limits will lead to significantly tighter constraints on ISM parameters. The forecasted improvements are as large as ∼3 dex in gas density and ∼1 dex in metallicity for some regions of parameter space. We suggest SXDF-NB1006-2 as a promising first target for 52 $mu$m line measurements. We discuss how such measurements will help in understanding the mass–metallicity relationship during the EoR." @default.
• W3120596863 created "2021-01-18" @default.
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• W3120596863 date "2021-04-01" @default.
• W3120596863 modified "2023-10-06" @default.
• W3120596863 title "The prospects for observing [O <scp>iii</scp>] 52 micron emission from galaxies during the Epoch of Reionization" @default.
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• W3120596863 doi "https://doi.org/10.1093/mnras/stab925" @default.
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