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Table 4.

CO-derived properties.

ID PHz ID Herschel Line (a) Mgas(b)

ID (1010 K km s−1 pc2) (1010M)
G176 57 01 CO(3–2) 22.26 ± 1.48 42.81 ± 2.84 149.85 ± 9.95
G176 57 02 CO(3–2) 3.88 ± 1.28 7.46 ± 2.46 26.10 ± 8.61
G173 237 01 CO(3–2) 3.11 ± 0.67 5.97 ± 1.29 20.90 ± 4.51
G006 (c) 631 01 CO(2–1) 4.36 ± 0.87 5.19 ± 1.04 18.18 ± 3.64
CO(3–2) 5.94 ± 1.19 11.42 ± 2.28 39.98 ± 8.00
G237 712 962 CO(3–2) 3.68 ± 0.70 7.08 ± 1.35 24.80 ± 4.73
G237 712 9741 CO(4–3) 0.93 ± 0.30 2.28 ± 0.72 7.98 ± 2.53
G191 832 01 CO(3–2) 9.66 ± 1.16 18.58 ± 2.23 65.05 ± 7.81
G191 832 07 CO(3–2) 8.18 ± 1.36 15.73 ± 2.62 55.07 ± 9.18
07a CO(3–2) 4.42 ± 1.55 8.50 ± 2.97 29.75 ± 10.41
07b CO(3–2) 3.54 ± 1.55 6.81 ± 2.98 23.83 ± 10.43
G191 832 26 CO(2–1) 8.49 ± 1.73 10.10 ± 2.07 35.36 ± 7.23
G059 124051 01 CO(4–3) 4.66 ± 0.55 11.37 ± 1.35 39.80 ± 4.72
G059 124051 03 CO(4–3) 1.46 ± 0.31 3.57 ± 0.76 12.48 ± 2.67
G073 124052 03 CO(2–1) 3.24 ± 1.00 3.85 ± 1.19 13.49 ± 4.18
G073 (c) 124052 15 CO(2–1) 2.87 ± 0.82 3.42 ± 0.97 11.97 ± 3.40
CO(3–2) 3.81 ± 1.08 7.33 ± 2.08 25.66 ± 7.29
G124 124053 01 CO(3–2) 5.25 ± 0.79 10.09 ± 1.51 35.33 ± 5.30
01a CO(3–2) 2.05 ± 0.42 3.94 ± 0.81 13.79 ± 2.83
01b CO(3–2) 3.02 ± 0.60 5.80 ± 1.16 20.30 ± 4.06
G124 124053 02 CO(3–2) 6.84 ± 0.95 13.16 ± 1.83 46.06 ± 6.40
G124 124053 03 CO(5–4) 2.85 ± 0.78 8.90 ± 2.42 31.13 ± 8.48
G124 124053 15 CO(3–2) 7.31 ± 1.39 14.06 ± 2.68 49.22 ± 9.37
G112 125018 06 CO(3–2) 4.00 ± 1.34 7.69 ± 2.58 26.92 ± 9.04
G143 125026 02 CO(5–4) 3.96 ± 0.88 12.36 ± 2.75 43.28 ± 9.62
G131 125027 01 CO(2–1) 6.33 ± 0.66 7.53 ± 0.78 26.36 ± 2.74
G131 (c) 125027 15 CO(2–1) 3.29 ± 0.88 3.92 ± 1.05 13.72 ± 3.67
CO(3–2) 4.36 ± 1.17 8.39 ± 2.24 29.36 ± 7.85
G052 125056 01 CO(3–2) 5.36 ± 0.84 10.31 ± 1.61 36.09 ± 5.63
G068 125107 02 CO(2–1) 14.73 ± 1.78 17.54 ± 2.12 61.39 ± 7.41
G063 (c) 125132 02a CO(2–1) 5.83 ± 1.45 6.94 ± 1.73 24.30 ± 6.04
CO(3–2) 7.34 ± 1.82 14.12 ± 3.51 49.40 ± 12.28
02b CO(3–2) 5.68 ± 1.28 10.93 ± 2.46 38.25 ± 8.61

Notes.

(a)

The luminosity is obtained from the of the reported CO transition and assuming the SMG brightness temperature ratios from Bothwell et al. (2013). The uncertainty introduced by this choice of brightness temperature ratio is a factor of 1.8 on the derived , and gas mass.

(b)

Gas masses are derived from assuming αCO = 3.5 M pc−2 (K km s−1)−1 (Magdis et al. 2017).

(c)

The two estimates are derived from the same line, but assuming two different transitions and relative redshifts.

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