Table 3.
Derived and observed properties of the galaxy sample.
| Name | Redshift (1) | Stellar mass | SFRIR | SFRradio | AGN (2) | L1.4 GHz | LIR (3) | qTIR (4) |
|---|---|---|---|---|---|---|---|---|
| – | – | [M⊙] | [M⊙ yr−1] | [M⊙ yr−1] | [%] | [1024 W Hz−1] | [1039 W] | – |
| CVLA1002 | 3.503 ± 0.001(s) | 11.62 ± 0.44 | 2496 ± 1266 | 5307 ± 1790 | 41 ± 22 | 8.34 ± 1.60 | 3.15 ± 0.01 | 2.00 ± 0.08 |
| ALESS14 | 3.380 ± 0.25(p) | 11.07 ± 0.85 | 1123 ± 142 | 4213 ± 757 | 20 ± 1 | 7.63 ± 1.37 | 2.19 ± 0.20 | 1.88 ± 0.09 |
| CVLA1000 | 3.430 ± 0.32(p) | 12.13 ± 1.30 | 711 ± 40 | 4057 ± 792 | 10 ± 2 | 7.35 ± 1.44 | 2.15 ± 0.25 | 1.89 ± 0.10 |
| CVLA958 | 3.175 ± 0.001(s) | 11.19 ± 0.44 | 1225 ± 546 | 3382±641 | 20 ± 4 | 6.13 ± 1.16 | 0.58 ± 0.02 | 1.40 ± 0.11 |
| CVLA100 | 3.290 ± 0.39(p) | 10.36 ± 0.52 | 528 ± 96 | 3391 ± 781 | 60 ± 3 | 6.14 ± 1.41 | 1.98 ± 0.32 | 1.93 ± 0.10 |
| CVLA028 | 3.270 ± 0.24(p) | 11.13 ± 0.30 | 1565 ± 753 | 2167 ± 602 | 3 ± 7 | 3.92 ± 1.09 | 2.52 ± 0.22 | 2.23 ± 0.13 |
| ALESS09 | 3.694 ± 0.001(s) | 11.27 ± 0.81 | 978 ± 113 | 2140 ± 597 | 10 ± 1 | 3.88 ± 1.08 | 2.20 ± 0.01 | 2.18 ± 0.12 |
| ECDFS544 | 3.199 ± 0.001(s) | 11.42 ± 0.80 | 1083 ± 470 | 1520 ± 507 | 20 ± 3 | 2.75 ± 0.92 | 2.01 ± 0.01 | 2.29 ± 0.15 |
Notes. The SFR values derived from the IR emission are a product of the SED fitting described in the text, while the radio-derived SFRs are derived by assuming that the radio emission is solely due to star formation without contribution by an AGN. The second row of the table corresponds to the units of each parameter. (1)(s): spectroscopic redshift; (p): photometric redshift (accepting the solution with the lowest χ2 or the best available in the literature), (2)the AGN percentage (Bayesian values) is estimated by our CIGALE fitting and corresponds to the same wavelength range in which the dust luminosity of each source was estimated, (3)this infrared luminosity corresponds to the wavelength range 42–122 μm (rest frame), (4)according to Eq. (5) by Enia et al. (2022): qTIR = log(LIR/3.75 × 1012)−log L1.4 GHz
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