Table 5.
Dust and gas properties of the OFGs.
| ID | log(Mdust) | Tdust | log(Mgas) | fgas | τdep |
|---|---|---|---|---|---|
| log(M⊙) | (K) | log(M⊙) | (Myr) | ||
| (1) | (2) | (3) | (4) | (5) | (6) |
| OFG1 | 8.49 |
(...) | 10.64 |
0.42 |
115 ± 20 |
| OFG2 | 8.80 |
37.0 |
10.96 |
0.61 |
249 ± 67 |
| OFG4 | 8.04 |
(...) | 10.39 |
0.38 |
46 ± 12 |
| OFG5 | 8.09 |
(...) | 10.49 |
0.67 |
114 ± 31 |
| OFG7 | 8.37 |
(...) | 10.75 |
0.72 |
52 ± 7 |
| OFG11 | 8.28 |
(...) | 10.57 |
0.59 |
97 ± 27 |
| OFG18 | 7.96 |
(...) | 10.71 |
0.95 |
180 ± 77 |
| OFG19 | 8.02 |
(...) | 10.39 |
0.55 |
90 ± 23 |
| OFG20 | 8.40 |
68.5 |
10.59 |
0.34 |
43 ± 6 |
| OFG25 | 8.66 |
(...) | 11.11 |
0.93 |
105 ± 9 |
| OFG27 | 9.01 |
51.4 |
11.07 |
0.48 |
66 ± 8 |
Notes. (1) Source ID; (2) Dust mass obtained from CIGALE for the galaxies with a Herschel counterpart or from the IR template library (Schreiber et al. 2018c) for the galaxies without a Herschel counterpart but with an ALMA counterpart (see Sect. 4.2). Since the dust emissivity used in Schreiber et al. (2018c) is different from the one of Draine et al. (2014; used in CIGALE), resulting in a systematic twice lower Mdust, here we have corrected the Mdust derived from the IR template library by multiplying by two. (3) Dust temperature obtained from a single temperature MBB model for the galaxies with a Herschel counterpart (see Sect. 4.5); (4) Gas mass obtained from the metallicity-dependent gas-to-dust mass ratio technique (see Sect. 4.4); (5) Gas fraction: fgas = Mgas/(M⋆ + Mgas); (6) Gas depletion time: τdep = Mgas/(SFRIR + SFRUV), which is the inverse of the star formation efficiency (SFE = 1/τdep).
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