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Table 2.

Characteristics of the sources forming the Supplementary Catalog.

ID ALMA IDCLS IDZF IDS − CLS zCLS zZF zsp S/N Flux log10(M*) S3 GHz
(mJy) (M⊙) (μJy)
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11)
AGS24 ... ... ... ... ... 3.472sp 3.93 0.88 ± 0.22pf 11.32 12.43 ± 2.19
AGS25 ... 11353 ... ... 4.644 ... 4.36 0.81 ± 0.19pf 10.39 6.69 ± 1.78
AGS26 8409 11442 J033237.75−275000.8 1.711 1.592 1.619sp 4.31 0.97 ± 0.15 10.91 85.09 ± 2.55
AGS27 11287 14926 J033216.54−274825.7 4.931 4.729 ... 3.76 1.43 ± 0.28 10.93 5.95 ± 1.86
AGS28 10286 13388 J033253.87−274901.9 2.021 2.149 ... 4.10 1.56 ± 0.21 11.17 17.19 ± 1.85
AGS29 9242 12438 J033248.53−274934.8 1.346 1.071 1.117sp 3.56 0.61 ± 0.18pf 10.77 65.01 ± 2.38
AGS30 8557 11581 J033240.33−274957.3 0.646 0.672 0.65sp 4.00 0.67 ± 0.17pf 10.40 ...
AGS31 3584 6153 J033216.53−275247.0 2.686 2.445 ... 3.93 0.72 ± 0.19pf 11.38 ...
AGS32 16822 19964 J033226.78−274604.2 4.526 4.729 ... 3.92 1.23 ± 0.16 11.00 4.47 ± 1.38
AGS33 16558 19463 J033211.93−274615.5 2.571 2.676 ... 3.85 1.77 ± 0.27 10.71 21.20 ± 2.84
AGS34 14035 17374 J033222.32−274711.9 2.866 2.750 ... 3.72 0.55 ± 0.15pf 10.82 15.55 ± 1.98
AGS35 10497 14146 J033243.67−274851.0 2.986 9.476 ... 3.71 1.16 ± 0.21 10.85 31.49 ± 1.42
AGS36 20859 23463 J033236.70−274406.6 0.646 0.663 0.665sp 3.66 0.74 ± 0.21pf 10.46 11.71 ± 1.60
AGS37 7184 10241 J033217.22−275037.3 1.971 1.864 1.956sp 3.64 1.10 ± 0.16 11.19 22.61 ± 4.39
AGS38 14638 17465 J033242.37−274707.8 1.346 1.323 1.314sp 3.62 1.00 ± 0.16 11.08 9.92 ± 2.28
AGS39 6131 9248 J033222.00−275112.3 2.906 2.360 ... 3.62 0.80 ± 0.23pf 10.57 17.24 ± 2.29

Notes. Columns: (1) source ID; (2), (3), (4) IDs of the HST-WFC3 (from the CANDELS catalog), ZFOURGE and IRAC (SEDS catalog) counterparts of these detections; (5), (6) photometric redshifts from the CANDELS catalog (Guo et al. 2013), zCLS, and ZFOURGE catalog (Straatman et al. 2016), zZF (we note that AGS24 has a redshift of z ≃ 3.472 determined by Zhou et al. 2020, see Sect. 4.2.2); (7) spectroscopic redshift when available (see Sect. 5.1), flagged with an “sp” exponent to avoid confusion; (8) S/N of the detections in the 060 mosaic. This S/N is given for the peak flux; (9) flux and error on the flux as explained in Sect. 5.2. “pf” indicates that the flux used is the peak flux, as the size measured by uvmodelfit is below the size limit given by Eq. (2). If there is no indication, the flux used is the flux given by uvmodelfit; (10) stellar mass as described in Sect. 5.1; (11) 3 GHz flux density from VLA (PI W. Rujopakarn, priv. comm.).

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