Table 4
Dynamical masses of the sample.
| Source | ⟨ ΔVCO ⟩ | r half | i | Mdyn,vir | Mdyn,rot |
| ( km s-1) | (kpc) | (deg) | (1010 M⊙) | (1010 M⊙) | |
|
|
|||||
| G09v1.97 | 348 ± 164 | 0.9 ± 0.1 | 47 ± 5 | 2.9 ± 2.7 | 2.5 ± 2.4 |
| G09v1.40 | 263 ± 70 | 0.4 ± 0.1 | 48 ± 11 | 0.8 ± 0.5 | 0.7 ± 0.5 |
| SDP17b | 286 ± 44 | 3.1 ± 0.9 | 39 ± 11 | 7.0 ± 3.0 | 8.3 ± 5.4 |
| SDP81 | 560 ± 139 | 3.3 ± 0.7 | 50 ± 7 | 29.1 ± 15.6 | 23.3 ± 13.6 |
| G12v2.43 | 237 ± 68 | 3 ± 1 | 55 | 4.7 ± 3.2 a | 3.3 ± 2.2a |
| G12v2.30 | 713 ± 153 | 1.6 ± 0.1 | 77 ± 2 | 22.8 ± 9.9 | 11.1 ± 4.9 |
| NCv1.143 | 265 ± 55 | 0.8 ± 0.2 | 51 ± 10 | 1.6 ± 0.8 | 1.2 ± 0.7 |
| NAv1.195 | 266 ± 19 | 1.6 ± 0.2 | 35 ± 9 | 3.1 ± 0.6 | 4.4 ± 2.2 |
| NAv1.177 | 252 ± 35 | 3 ± 1 | 55 | 5.4 ± 2.3 a | 3.7 ± 1.6a |
| NBv1.78 | 597 ± 121 | 0.6 ± 0.2 | 51 ± 7 | 5.5 ± 3.3 | 4.3 ± 2.7 |
| NAv1.144 | 208 ± 35 | 0.9 ± 0.3 | 55 ± 8 | 1.1 ± 0.5 | 0.7 ± 0.4 |
| NAv1.56 | 650 ± 28 b | 1.5 ± 0.4 | 52 ± 5 | 17.8 ± 5.0 | 13.2 ± 4.1 |
| G15v2.235 | 480 ± 111 | 1.7 ± 0.3 | 59 ± 8 | 11.2 ± 5.6 | 7.1 ± 3.8 |
|
|
|||||
| G12v2.890 | 344 ± 92 | 3 ± 1 | 55 | 10.0 ± 6.3 a | 6.9 ± 4.4a |
| G12v2.257 | 395 ± 206 | 3 ± 1 | 55 | 13.2 ± 14.4 a | 9.2 ± 10.0 a |
|
|
|||||
| G15v2.779c | 830 ± 86 | 3.8 ± 0.4 | 43 ± 7 | 73.5 ± 17.0 | 72.8 ± 22.6 |
Notes. ⟨ ΔVCO ⟩ is the average value of the CO linewidths, the errors are from standard deviations. We recall the values of half-light radius rhalf in this table. i is the inclination angle derived from the major and minor axis ratio from lensing models in Bu13. Mdyn,vir and Mdyn,rot are the dynamical masses enclosed in rhalf.
Due to lacking rhalf and b/a ratio of the rotating disk from lensing models, we use a typical value of rhalf = 3 ± 1 kpc (by assigning a 30% uncertainty) and i = 55° (see text) for the estimation of these dynamical masses.
Because of the limited data quantity for this source, we take the CO(4–3) data of NAv1.56 from the NOEMA observation (Oteo et al., in prep.), which offers better accuracy.
The physical properties of G15v2.779 are taken from or computed according to Cox et al. (2011) and O13.
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