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Table 2.

Derived properties of the GOODS-ALMA sources.

ID z log10(M) log10(LIR) SFR RSB log10(Mdust) log10(Mgas) fgas Tdust S1.1 mm
(M) (L) (M yr−1) (M) (M) (K) (mJy)
AGS1 2.309 11.15 12.81 ± 0.02 1103 4.8 9.2 ± 0.1 11.3 ± 0.1 0.57 38.3 ± 0.9 1.90 ± 0.20
AGS2 ( † ) 2.918 10.68 12.98 ± 0.14 1642 14.0 8.8 ± 0.1 11.0 ± 0.1 0.67 44.8 ± 4.6 1.99 ± 0.22
AGS3 2.582 11.33 12.84 ± 0.02 1187 3.3 9.1 ± 0.1 11.2 ± 0.1 0.42 41.0 ± 0.9 1.84 ± 0.21
AGS4 3.556 11.09 12.93 ± 0.02 1435 3.8 8.9 ± 0.1 11.0 ± 0.1 0.44 47.0 ± 1.8 1.72 ± 0.20
AGS5 3.46 11.13 12.94 ± 0.02 1487 3.8 8.9 ± 0.1 11.0 ± 0.1 0.44 43.9 ± 1.8 1.56 ± 0.19
AGS6 2.698 10.93 12.57 ± 0.02 651 3.5 9.0 ± 0.1 11.1 ± 0.1 0.59 39.5 ± 0.8 1.27 ± 0.18
AGS7 ( † ) 3.29 11.43 12.48 ± 0.10 522 0.8 8.7 ± 0.1 10.7 ± 0.1 0.17 37.4 ± 2.4 1.15 ± 0.17
AGS8 1.95 11.53 12.70 ± 0.02 861 3.1 9.3 ± 0.1 11.3 ± 0.1 0.38 32.4 ± 2.1 1.43 ± 0.22
AGS9 3.847 10.97 12.69 ± 0.03 843 2.7 9.0 ± 0.1 11.1 ± 0.1 0.59 38.8 ± 2.2 1.25 ± 0.21
AGS10 2.41 11.25 12.66 ± 0.02 803 2.8 9.0 ± 0.1 11.0 ± 0.1 0.37 39.0 ± 1.9 0.88 ± 0.15
AGS11 ( † ) 3.472 10.24 12.94 ± 0.07 1492 28.7 8.5 ± 0.1 10.8 ± 0.1 0.80 50.1 ± 2.5 1.34 ± 0.25
AGS12 2.543 10.77 12.76 ± 0.02 998 8.1 8.7 ± 0.1 10.9 ± 0.1 0.56 50.6 ± 1.3 0.93 ± 0.18
AGS13 2.225 11.40 12.43 ± 0.02 476 1.6 8.8 ± 0.1 10.8 ± 0.1 0.21 39.7 ± 1.4 0.78 ± 0.15
AGS15 ( † ) 3.472 10.56 12.78 ± 0.08 1034 9.5 8.9 ± 0.1 11.1 ± 0.1 0.78 38.9 ± 2.4 1.21 ( ⋆ ) ± 0.11
AGS17 3.467 10.52 13.08 ± 0.02 2070 20.9 9.0 ± 0.1 11.2 ± 0.1 0.84 49.6 ± 1.7 2.30 ( ⋆ ) ± 0.44
AGS18 2.696 11.11 12.43 ± 0.03 471 1.8 8.9 ± 0.1 11.0 ± 0.1 0.46 38.1 ± 1.4 1.70 ( ⋆ ) ± 0.30
AGS20 ( † ) 2.73 10.76 12.59 ± 0.08 666 5.1 8.6 ± 0.1 10.8 ± 0.1 0.52 40.6 ± 2.4 1.11 ± 0.24
AGS21 ( † ) 3.689 10.63 12.39 ± 0.06 437 3.2 8.3 ± 0.1 10.5 ± 0.1 0.41 43.7 ± 2.0 0.64 ± 0.11
AGS23 2.36 11.26 12.17 ± 0.05 256 0.9 9.2 ± 0.1 11.2 ± 0.1 0.48 29.1 ± 0.6 0.98 ± 0.21
AGS24 ( † ) 3.472 11.32 12.31 ± 0.11 353 0.6 8.5 ± 0.1 10.6 ± 0.1 0.16 37.3 ± 2.5 0.88 ± 0.22
AGS25 ( † ) 4.64 10.39 12.68 ± 0.07 832 8.0 8.2 ± 0.1 10.5 ± 0.1 0.55 51.5 ± 2.6 0.81 ± 0.19
AGS26 1.619 10.91 12.51 ± 0.02 553 6.1 9.0 ± 0.1 11.1 ± 0.1 0.62 38.2 ± 2.5 0.97 ± 0.15
AGS27 ( † ) 4.73 10.93 12.83 ± 0.06 1180 3.2 8.5 ± 0.1 10.6 ± 0.1 0.33 48.0 ± 2.6 1.43 ± 0.28
AGS28 2.15 11.17 12.38 ± 0.02 413 2.0 9.2 ± 0.1 11.2 ± 0.1 0.54 33.3 ± 0.5 1.56 ± 0.21
AGS29 ( † ) 1.117 10.77 11.96 ± 0.10 161 3.6 8.7 ± 0.1 10.9 ± 0.1 0.55 31.5 ± 2.4 0.61 ± 0.18
AGS30 ( † ) 0.646 10.40 11.84 ± 0.14 119 8.5 8.5 ± 0.1 10.8 ± 0.1 0.71 32.0 ± 2.4 0.67 ± 0.17
AGS31 2.45 11.38 12.38 ± 0.02 415 1.2 8.8 ± 0.1 10.8 ± 0.1 0.21 38.8 ± 2.9 0.72 ± 0.19
AGS32 ( † ) 4.73 11.00 12.73 ± 0.06 941 2.2 8.5 ± 0.1 10.7 ± 0.1 0.31 44.9 ± 2.5 1.23 ± 0.16
AGS33 ( † ) 2.68 10.71 12.40 ± 0.05 432 3.8 9.0 ± 0.1 11.1 ± 0.1 0.73 ... 1.77 ± 0.27
AGS34 2.75 10.82 12.15 ± 0.04 244 1.6 8.7 ± 0.2 10.9 ± 0.2 0.54 ... 0.55 ± 0.15
AGS35 2.99 10.85 12.74 ± 0.02 955 5.4 8.3 ± 0.1 10.5 ± 0.1 0.29 60.3 ± 3.6 1.16 ± 0.21
AGS36 ( † ) 0.665 10.46 10.92 ± 0.03 14 0.9 9.4 ± 0.1 11.7 ± 0.1 0.94 ... 0.74 ± 0.21
AGS37 1.956 11.19 12.36 ± 0.02 390 2.1 9.0 ± 0.1 11.0 ± 0.1 0.41 38.0 ± 1.6 1.10 ± 0.16
AGS38 1.314 11.08 11.64 ± 0.02 79 0.9 9.0 ± 0.3 11.1 ± 0.3 0.50 ... 1.00 ± 0.16
AGS39 2.36 10.57 12.49 ± 0.02 537 7.4 8.8 ± 0.1 11.0 ± 0.1 0.73 40.6 ± 1.7 0.80 ± 0.23

Notes. Columns: (1) source name; (2) redshifts (spectroscopic redshifts are shown to three decimal places); (3) stellar mass; (4) LIR derived from SED fitting; (5) SFR = SFRIR + SFRUV; (6) RSB = SFR/SFRMS, where SFRMS is the average SFR of MS galaxies following Schreiber et al. (2015); (7) dust mass. For galaxies for which we used the dust spectral energy distribution library presented in Schreiber et al. (2018b) (labeled by a † in this table), the dust mass is multiplied by a factor of 2, to be consistent with the dust mass derived by the Draine et al. (2014) model (see Schreiber et al. 2018b for details); (8) gas mass derived from Eq. (4); (9) gas fraction defined by fgas = Mgas/(Mgas + M); (10) dust temperature derived from a MBB model assuming β = 1.5. ( † )Indicates galaxies without a Herschel counterpart and whose LIR is determined only by the ALMA contribution. For these galaxies, we show the mass of gas as an indication but we do not use it in the rest of this paper; (11) flux density at 1.1 mm. ( ⋆ )Indicates changes in the flux density since F18. A summary of the fluxes (peak and integrated) as well as the sizes measured in the Main and Supplementary catalogs are given in Table A.1.

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