Table 3.
Details of the final sample of sources detected in the ALMA GOODS-South continuum map, from the primary catalog in the main part of the table and from the supplementary catalog below the solid line (see Sects. 4.1 and 4.2).
| ID | z | S/N |
 |
fdeboost |
 |
log10 M⋆ | 0″60 | 0″29 | S6 GHz | LX/1042 | IDsub(mm) |
|---|---|---|---|---|---|---|---|---|---|---|---|
| mJy | mJy | M⊙ | μJy | erg s−1 | |||||||
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11) | (12) |
| AGS1 | 2.309 | 11.26 | 1.90 ± 0.20 | 1.03 | 1.99 ± 0.15 | 11.05 | 1 | 1 | 18.38 ± 0.71 | 1.93 | GS6, ASA1 |
| AGS2 | 2.918 | 10.47 | 1.99 ± 0.22 | 1.03 | 2.13 ± 0.15 | 10.90 | 1 | 1 | – | 51.31 | |
| AGS3 | 2.582 | 9.68 | 1.84 ± 0.21 | 1.03 | 2.19 ± 0.15 | 11.33 | 1 | 1 | 19.84 ± 0.93 | 34.54 | GS5, ASA2 |
| AGS4 | 4.32 | 9.66 | 1.72 ± 0.20 | 1.03 | 1.69 ± 0.18 | 11.45 | 1 | 1 | 8.64 ± 0.77 | 10.39 | |
| AGS5 | 3.46 | 8.95 | 1.56 ± 0.19 | 1.03 | 1.40 ± 0.18 | 11.13 | 1 | 1 | 14.32 ± 1.05 | 37.40 | |
| AGS6 | 3.00 | 7.63 | 1.27 ± 0.18 | 1.05 | 1.26 ± 0.16 | 10.93 | 1 | 1 | 9.02 ± 0.57 | 83.30 | UDF1, ASA3 |
| AGS7 | 3.29 | 7.26 | 1.15 ± 0.17 | 1.05 | 1.20 ± 0.13 | 11.43 | 1 | 1 | – | 24.00 | |
| AGS8 | 1.95 | 7.10 | 1.43 ± 0.22 | 1.05 | 1.98 ± 0.20 | 11.53 | 1 | 1 | – | 3.46 | LESS18 |
| AGS9 | 3.847 | 6.19 | 1.25 ± 0.21 | 1.05 | 1.39 ± 0.17 | 10.70 | 1 | 1 | 14.65 ± 1.12 | – | |
| AGS10 | 2.41 | 6.10 | 0.88 ± 0.15 | 1.06 | 1.04 ± 0.13 | 11.32 | 1 | 1 | – | 2.80 | |
| AGS11 | 4.82 | 5.71 | 1.34 ± 0.25 | 1.08 | 1.58 ± 0.22 | 10.55 | 1 | 1 | – | – | |
| AGS12 | 2.543 | 5.42 | 0.93 ± 0.18 | 1.10 | 1.13 ± 0.15 | 10.72 | 1 | 1 | 12.65 ± 0.55 | 4.53 | UDF3, C1, ASA8 |
| AGS13 | 2.225 | 5.41 | 0.78 ± 0.15 | 1.10 | 0.47 ± 0.14 | 11.40 | 1 | 0 | 22.52 ± 0.81 | 13.88 | ASA12 |
| AGS14* | – | 5.30 | 0.86 ± 0.17 | 1.10 | 1.17 ± 0.15 | – | 1 | 0 | – | – | |
| AGS15 | – | 5.22 | 0.80 ± 0.16 | 1.11 | 0.64 ± 0.15 | – | 1 | 1 | – | – | LESS34 |
| AGS16* | – | 5.05 | 0.82 ± 0.17 | 1.12 | 0.99 ± 0.17 | – | 1 | 0 | – | – | |
| AGS17 | – | 5.01 | 0.93 ± 0.19† | 1.14 | 1.37 ± 0.18 | – | 1 | 0 | – | – | LESS10 |
| AGS18 | 2.794 | 4.93 | 0.85 ± 0.18† | 1.15 | 0.79 ± 0.15 | 11.01 | 1 | 0 | 6.21 ± 0.57 | – | UDF2, ASA6 |
| AGS19* | – | 4.83 | 0.69 ± 0.15 | 1.16 | 0.72 ± 0.13 | – | 1 | 0 | – | – | |
| AGS20 | 2.73 | 4.81 | 1.11 ± 0.24 | 1.16 | 1.18 ± 0.23 | 10.76 | 1 | 1 | 12.79 ± 1.40 | 4.02 | |
| AGS21 | 3.76 | 5.83 | 0.64 ± 0.11 | 1.07 | 0.88 ± 0.19 | 10.63 | 0 | 1 | – | 19.68 | |
| AGS22 | – | 4.90 | 1.05 ± 0.22 | 1.15 | 1.26 ± 0.22 | – | 1 | 0 | – | – | |
| AGS23 | 2.36 | 4.68 | 0.98 ± 0.21 | 1.19 | 1.05 ± 0.20 | 11.26 | 1 | 0 | – | – |
Notes. Columns: (1) IDs of the sources as shown in Fig. 1. The sources are sorted by S/N. * indicates galaxies that are most likely spurious (not detected at any other wavelength); (2) redshifts from the ZFOURGE catalog. Spectroscopic redshifts are shown with three decimal places. As AGS6 is not listed in the ZFOURGE catalog, we used the redshift computed by Dunlop et al. (2017); (3) S/N of the detections in the 0″60 mosaic (except for AGS21). This S/N is computed using the flux from Blobcat and is corrected for peak bias; (4) peak fluxes measured using Blobcat in the 0″60-mosaic image before de-boosting correction; (5) deboosting factor; (6) fluxes measured by PSF-fitting with Galfit in the 0″60-mosaic image before de-boosting correction; (7) stellar masses from the ZFOURGE catalog; (8), (9) flags for detection by Blobcat in the 0″60-mosaic and 0″29-mosaic images, where at least one combination of σp and σf gives a purity factor (Eq. (1)) greater than 80%; (10) flux for detection greater than 3 σ by VLA (5 cm). Some of these sources are visible in the VLA image but not detected with a threshold >3σ. AGS8 and AGS16 are not in the field of the VLA survey; (11) absorption-corrected intrinsic 0.5–7.0 keV luminosities. The X-ray luminosities have been corrected to account for the redshift difference between the redshifts provided in the catalog of Luo et al. (2017) and those used in the present table, when necessary. For this correction we used Eq. (1) from Alexander et al. (2003), and assuming a photon index of Γ = 2; (12) corresponding IDs for detections of the sources in previous (sub)millimeter ancillary data. UDF is for Hubble Ultra Deep Field survey (Dunlop et al. 2017) at 1.3 mm, C indicates the ALMA Spectroscopic Survey in the Hubble Ultra Deep Field (ASPECS) at 1.2 mm (Aravena et al. 2016), LESS indicates data at 870 μm presented in Hodge et al. (2013), GS indicates data at 870 μm presented in Elbaz et al. (2018), ASA indicates the ALMA 26 arcmin2 Survey of GOODS-S at One-millimeter (ASAGAO). We also note the pointed observations of AGS1 presented in Barro et al. (2017), and those of AGS13 by Talia et al. (2018). For the two sources marked by a †, the hypothesis a of a point-like source is no longer valid. We therefore apply correction factors of 2.3 and 1.7 to the peak flux values of AGS17 and AGS18 respectively, to take into account the extended flux emission of these sources.
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