Table 4
Dust temperature, FIR luminosities, and FIR-based SFRs for the Herschel/SPIRE sources within the Planck beam.
| ID | T dust | L FIR | SFR | |
| [ K ] | [ 1012L⊙ ] | [ M⊙ yr-1 ] | ||
|
|
||||
| A (z = 1.7) | 25.9 ± 2.9 | 2.8 ± 0.4 | 482 ± 69 | |
| B (z = 1.7) | 26.3 ± 3.0 | 2.7 ± 0.4 | 465 ± 69 | |
| C (z = 1.7) | 32.0 ± 7.8 | 2.2 ± 0.8 | 379 ± 138 | |
| D (z = 1.7) | 31.7 ± 7.0 | 2.7 ± 0.8 | 465 ± 138 | |
| E (z = 1.7) | 26.4 ± 5.5 | 2.1 ± 0.5 | 362 ± 86 | |
|
|
||||
| A (z = 2.0) | 29.5 ± 3.5 | 4.3 ± 0.6 | 740 ± 103 | |
| B (z = 2.0) | 29.5 ± 3.4 | 4.1 ± 0.5 | 706 ± 86 | |
| C (z = 2.0) | 36.3 ± 9.0 | 3.3 ± 1.5 | 568 ± 258 | |
| D (z = 2.0) | 35.9 ± 8.2 | 4.0 ± 1.3 | 689 ± 223 | |
| E (z = 2.0) | 30.1 ± 6.7 | 3.1 ± 0.7 | 534 ± 121 | |
Notes. We provide two estimates for each of these quantities assuming that all the FIR signals arise from sources either at z = 1.7 (top part of the table) or at z = 2.0 (bottom), which serve as lower and upper limits (respectively) to the expected FIR estimations.
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