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Table 5.

Far-infrared properties of the CO detected sources.

ID PHz ID Herschel z SFRIR log(LIR) Tdust τdep zdep
ID (M yr−1) (L) (K) (Gyr)
G176 57 01 2.7534 3294 13.54 ± 0.08 34 ± 1 0.45 ± 0.09 2.28
G176 57 02 2.7536 1557 13.22 ± 0.17 35 ± 3 0.17 ± 0.09 2.56
G173 237 01 2.5572 1374 13.16 ± 0.14 30 ± 2 0.15 ± 0.06 2.40
G006 631 01 1.3615 250 12.42 ± 0.10 20 ± 1 0.73 ± 0.23 1.13
631 01 2.5422 1129 13.08 ± 0.10 30 ± 2 0.35 ± 0.11 2.21
G237 712 962 2.0577 457 12.68 ± 0.15 28 ± 2 0.54 ± 0.22 1.71
G237 712 9741 2.1590 217 12.36 ± 0.44 27 ± 5 0.37 ± 0.46 1.89
G191 832 01 2.5509 1523 13.21 ± 0.12 30 ± 2 0.43 ± 0.13 2.15
G191 832 07 2.6236 919 12.99 ± 0.22 32 ± 3 0.60 ± 0.33 2.07
832 07a 2.6225 < 918 < 12.99 ± 0.22 ... > 0.32 ± 0.20 < 2.30
832 07b 2.6247 < 920 < 12.99 ± 0.22 ... > 0.26 ± 0.18 < 2.36
G191 832 26 1.8899 256 12.43 ± 0.34 23 ± 4 1.38 ± 1.21 1.25
G059 124051 01 2.3568 1107 13.07 ± 0.16 30 ± 2 0.36 ± 0.14 2.06
G059 124051 03 2.3677 813 12.93 ± 0.19 27 ± 2 0.15 ± 0.08 2.23
G073 124052 03 1.5418 329 12.54 ± 0.23 26 ± 3 0.41 ± 0.26 1.37
G073 124052 15 1.4303 177 12.27 ± 0.25 20 ± 2 0.68 ± 0.45 1.19
15 2.6454 777 12.91 ± 0.25 30 ± 3 0.33 ± 0.22 2.31
G124 124053 01 2.1531 1238 13.12 ± 0.14 31 ± 2 0.29 ± 0.10 1.94
01a 2.1544 < 1240 < 13.12 ± 0.14 ... > 0.11 ± 0.02 < 2.07
01b 2.1523 < 1237 < 13.12 ± 0.14 ... > 0.16 ± 0.03 < 2.03
G124 124053 02 2.1614 932 12.99 ± 0.17 30 ± 3 0.49 ± 0.21 1.81
G124 124053 03 2.7189 1873 13.30 ± 0.03 38 ± 0 0.17 ± 0.05 2.53
G124 124053 15 2.0882 429 12.66 ± 0.29 27 ± 4 1.15 ± 0.85 1.44
G112 125018 06 2.3187 723 12.88 ± 0.25 30 ± 4 0.37 ± 0.26 2.02
G143 125026 02 2.5836 1259 13.12 ± 0.12 21 ± 1 0.34 ± 0.13 2.25
G131 125027 01 1.3235 577 12.78 ± 0.13 27 ± 2 0.46 ± 0.14 1.17
G131 125027 15 1.4367 203 12.33 ± 0.36 26 ± 5 0.68 ± 0.65 1.20
15 2.6549 876 12.97 ± 0.07 38 ± 0 0.34 ± 0.10 2.31
G052 125056 01 2.2726 1130 13.08 ± 0.14 30 ± 2 0.32 ± 0.12 2.02
G068 125107 02 1.7185 861 12.96 ± 0.09 28 ± 1 0.71 ± 0.16 1.39
G063 125132 02a 1.5962 < 686 < 12.86 ± 0.13 ... > 0.35 ± 0.09 < 1.44
02a 2.8942 < 2644 < 13.44 ± 0.03 ... > 0.19 ± 0.05 < 2.66
02b 2.2537 < 1578 < 13.22 ± 0.13 ... > 0.24 ± 0.06 < 2.06

Notes. The SFRIR is derived by fitting a modified black body spectrum (β = 1.8) to the SPIRE and SCUBA, when available, photometric data points, and assuming the Kennicutt (1998)LIR–SFR relation corrected for a Chabrier IMF. Whenever multiple sources are associated with the same Herschel source, LIR, the SFR, and zdep should be considered as upper limits, τdep as a lower limit, and Tdust is unconstrained as the far-IR emission is blended.

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