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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