Table C.1.
IR luminosities and star formation rates.
| ID | LIR, V20 | SFRV20 | LIR, 20K | SFR20K | LIR, 30K | SFR30K |
|---|---|---|---|---|---|---|
| (1010L⊙) | (M⊙ yr−1) | (1010L⊙) | (M⊙ yr−1) | (1010L⊙) | (M⊙ yr−1) | |
| J1448 | 78.4 ± 17.6 | 116.7 ± 26.3 | < 6.5 | < 9.7 | < 4.1 | < 6.1 |
| J2258 | 95.1 ± 35.0 | 141.6 ± 52.2 | < 8.8 | < 13.2 | < 5.6 | < 8.3 |
| ID83492 | 12.5 ± 4.8 | 18.6 ± 7.1 | < 10.8 | < 16.0 | < 6.4 | < 9.5 |
| J1109 | < 2.0 | < 2.9 | < 3.7 | < 5.5 | < 2.1 | < 3.1 |
| J1302 | < 3.9 | < 5.9 | < 4.8 | < 7.2 | < 2.7 | < 4.1 |
| J0912 | < 3.7 | < 5.5 | < 8.3 | < 12.3 | < 4.8 | < 7.1 |
| J2202 | < 23.9 | < 35.6 | < 2.5 | < 3.7 | < 1.4 | < 2.1 |
| ID97148 | < 0.8 | < 1.2 | < 11.8 | < 17.6 | < 7.1 | < 10.5 |
| Mean mergers | 60.9 ± 12.8 | 90.7 ± 19.0 | < 3.1 | < 4.6 | < 1.8 | < 2.7 |
| Stack isolated | < 2.6 | < 3.9 | < 1.5 | < 2.3 | < 0.9 | < 1.3 |
Notes. IR luminosity and SFR have been obtained (i) converting the CO(5-4) luminosity into LIR using the Valentino et al. (2020) relation (LIR, V20, SFRV20); (ii) considering the observed continuum upper limits and the average SED template for quiescent galaxies from Magdis et al. (2021). We considered both a template dust temperature of 20 K (LIR, 20K, SFR20K) and 30 K (LIR, 30K, SFR30K).
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