Table 2.
Physical properties of our sample of galaxies.
| Source | z[CII] | log(M*) | log(SFR[CII]) | log(MH2, TOT) | 12 + log(O/H) |
|---|---|---|---|---|---|
| [M⊙] | [M⊙ yr−1] | [M⊙] | |||
| (1) | (2) | (3) | (4) | (5) | (6) |
| Haro2 | 0.0049 |
 |
 |
 |
8.23 ± 0.03 |
| Haro3 | 0.0032 |
 |
 |
 |
8.28 ± 0.01 |
| Haro11 | 0.0207 |
 |
 |
 |
8.36 ± 0.01 |
| He2-10 | 0.0029 |
 |
 |
 |
8.43 ± 0.01 |
| HS0052+2536 | 0.0462 |
 |
 |
 |
8.07 ± 0.20 |
| HS1222+3741 | 0.0405 |
 |
 |
 |
7.79 ± 0.01 |
| HS1304+3529 | 0.0162 |
 |
 |
 |
7.93 ± 0.10 |
| HS1330+3651 | 0.0165 |
 |
 |
 |
7.98 ± 0.10 |
| HS1442+4250 | 0.0022 |
 |
 |
 |
7.60 ± 0.01 |
| HS2352+2733 | 0.0273 |
 |
 |
 |
8.40 ± 0.20 |
| IZw18 | 0.0025 |
 |
 |
 |
7.14 ± 0.01 |
| IIZw40 | 0.0026 |
 |
 |
 |
8.23 ± 0.01 |
| Mrk153 | 0.0080 |
 |
 |
 |
7.86 ± 0.04 |
| Mrk209 | 0.0010 |
 |
 |
 |
7.74 ± 0.01 |
| Mrk930 | 0.0183 |
 |
 |
 |
8.03 ± 0.01 |
| Mrk1089 | 0.0134 |
 |
 |
 |
8.10 ± 0.08 |
| Mrk1450 | 0.0032 |
 |
 |
 |
7.84 ± 0.01 |
| SBS0335–052 | 0.0136 |
 |
 |
 |
7.25 ± 0.01 |
| SBS1159+545 | 0.0121 |
 |
 |
 |
7.44 ± 0.01 |
| SBS1211+540 | 0.0030 |
 |
 |
 |
7.58 ± 0.01 |
| SBS1249+493 | 0.0248 |
 |
 |
 |
7.68 ± 0.02 |
| SBS1415+437 | 0.0021 |
 |
 |
 |
7.55 ± 0.01 |
| SBS1533+574 | 0.0114 |
 |
 |
 |
8.05 ± 0.01 |
| UGC4483 | 0.0006 |
 |
 |
 |
7.46 ± 0.02 |
| UM133 | 0.0053 |
 |
 |
 |
7.82 ± 0.01 |
| UM311 | 0.0057 |
 |
 |
 |
8.36 ± 0.01 |
| UM448 | 0.0184 |
 |
 |
 |
8.32 ± 0.01 |
| UM461 | 0.0034 |
 |
 |
 |
7.73 ± 0.01 |
| VIIZw403 | −0.0002 |
 |
 |
 |
7.66 ± 0.01 |
Notes. Column key: (1) source name; (2) redshift based on [CII] emission line; (3) stellar mass from CIGALE; (4) SFR from [CII] emission; (5) mass of total molecular gas estimated from [CII] luminosity; (6) metallicity values in 12 + log(O/H) from Madden et al. (2013). SFRs and MH2, TOT were obtained from the [CII] luminosity of the narrow components following the relations found by De Looze et al. (2014) and Madden et al. (2020) for the DGS galaxies, respectively. The typical z[CII] uncertainties based on the spectral resolution are 0.0001.
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