Table 1.
Properties of the optically dark galaxies.
| ID | RA | Dec | zphot | zspec | assumed z | log M⋆ | log LIR | SFR | RSB | F1.1 mm | F2 mm | log LCO | H | F3 GHz | F6 GHz | L1.4 GHz |
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| [deg] | [deg] | log [M⊙] | log [L⊙] | [M⊙ yr−1] | [mJy] | [mJy] | log [L⊙] | [mag] | [μJy] | [μJy] | [W Hz−1] | |||||
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11) | (12) | (13) | (14) | (15) | (16) | (17) |
| AGS4 | 53.148839 | −27.821192 | – | 3.556 | 3.556 | 11.09 |
12.93 ± 0.02 | 1435 |
3.8 |
1.72 ± 0.20 | 0.29 ± 0.02 | 4.95 ± 0.93 | 25.23 | 17.28 ± 1.66 | 8.64 ± 0.77 | 2.73 × 1024 |
| AGS11 | 53.108818 | −27.869055 | – | – | 3.472 | 10.24 |
12.94 ± 0.07 | 1492 |
28.7 |
1.34 ± 0.25 | 0.30 ± 0.02 | – | – | 4.48 ± 1.06 | – | 6.72 × 1023 |
| AGS15 | 53.074847 | −27.875880 | 3.96 |
– | 3.472 | 10.56 |
12.78 ± 0.08 | 1034 |
9.5 |
1.21 ± 0.11 | 0.32 ± 0.02 | – | 27.11 | 5.38 ± 1.06 | – | 8.08 × 1023 |
| AGS17 | 53.079374 | −27.870770 | – | 3.467 | 3.467 | 10.52 |
13.08 ± 0.02 | 2070 |
20.9 |
2.30 ± 0.44 | 0.35 ± 0.02 | 5.22 ± 1.01 | – | 39.00 ± 3.94 | 1.16 ± 0.32 | 5.86 × 1024 |
| AGS24 | 53.087178 | −27.840217 | 3.58 |
– | 3.472 | 11.32 |
12.31 ± 0.11 | 353 |
0.6 |
0.88 ± 0.22 | 0.19 ± 0.02 | – | – | 12.43 ± 2.19 | 1.41 ± 0.32 | 1.87 × 1024 |
| AGS25 | 53.183710 | −27.836515 | 4.64 | – | 4.64 | 10.39 | 12.68 ± 0.07 | 832 |
8.0 |
0.82 ± 0.19 | – | – | – | 3.92 ± 1.06 | 1.07 ± 0.32 | 5.90 × 1023 |
Columns: (1) source names; (2) (3) coordinates in the ALMA image (J2000): see F18 and F20a; (4) photometric redshifts: see Sect. 2.4.1; (5) spectroscopic redshifts: the spectroscopic redshifts of AGS4 and AGS17 are derived from the CO(6-5) line measured in our ALMA spectroscopic scan follow-up, see Sect. 3; (6) assumed redshifts: We assign the redshift of AGS11, AGS15 and AGS24 to be the same as the central position of the redshift peak that presents an overdensity centered on AGS24, zpeak = 3.472, as discussed in Sects. 5.2 and 5.3, which is consistent with their photometric redshifts. For each galaxy, all the properties are measured assuming the redshift listed here; (7) stellar masses: see Sect. 2.4.2; (8) infrared luminosities: see Sect. 2.4.3; (9) SFRs: see Sect. 2.4.4; (10) starburstness: as in F20a, RSB = SFR/SFRMS, where SFRMS is the average SFR of MS galaxies as defined in Schreiber et al. (2018a); (11) flux densities at 1.1 mm: Peak fluxes measured using Blobcat as in F18 and the fluxes of AGS15 and AGS17 are updated in F20a; (12) peak fluxes at 2 mm from the ALMA band4 follow-up; (13) CO luminosities: the CO(6-5) line detected in our ALMA spectroscopic scan follow-up; (14) H-band AB magnitudes: After de-blending, AGS4 and AGS15 turn out to have H-band magnitudes higher than the detection limit; (15) flux densities at 3 GHz: the flux densities of AGS4, 17 and 24 are the peak flux derived using PyBDSF1 (Rujopakarn et al., in prep.), flux densities of AGS11, 15 and 25 are the peak flux densities in the 3 GHz image; (15) flux densities at 6 GHz: the flux density of AGS4 is the peak flux derived using PyBDSF1, flux densities of AGS17, 24 and 25 are the peak flux densities in the 6 GHz image, AGS11 and AGS15 do not have peak flux density higher than 3σ; (17) luminosity at 1.4 GHz: derived from the flux density at 3 GHz using Eq. (1).
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