Table 4
Subsample of dynamically and spectroscopically determined stellar masses.
| Source | Dynamical M⋆ | Vsys | Spectroscopic M⋆ | Difference |
|---|---|---|---|---|
| (M⊙) | (km s−1) | (M⊙) | (σ) | |
| J15450887−3417333 | 0.3 ± 0.1 | 4.8 |
0.14 ± 0.03 | 1.5 |
| Sz 68 | 2.0 |
5.2 |
2.13 ± 0.34 | 0.2 |
| Sz 69 | 0.3 ± 0.1 | 5.5 |
0.19 ± 0.03 | 1.1 |
| Sz 71 | 0.5 |
3.6 |
0.42 ± 0.11 | 0.5 |
| Sz 73 | 0.8 |
4.3 |
0.82 ± 0.16 | 0.1 |
| Sz 83 | >0.3 | 4.7 |
0.75 ± 0.19 | ... |
| Sz 84 | 0.4 ± 0.1 | 5.2 |
0.18 ± 0.03 | 2.1 |
| J16000236−4222145 | 0.3 ± 0.1 | 4.1 ± 0.2 | 0.24 ± 0.03 | 0.6 |
| Sz 130 | 0.4 |
4.6 |
0.37 ± 0.10 | 0.1 |
| Sz 133 | 1.0 ± 0.2 | 5.3 |
0.63 ± 0.05 | 1.8 |
| Sz 90 | 0.3 |
5.5 |
0.79 ± 0.18 | 1.1 |
| Sz 98 | 0.9 |
3.2 |
0.74 ± 0.20 | 0.7 |
| Sz 100 | 0.4 ± 0.1 | 1.9 ± 0.2 | 0.18 ± 0.03 | 2.1 |
| Sz 108B | 0.3 |
2.5 |
0.19 ± 0.03 | 1.1 |
| Sz 114 | 0.3 ± 0.1 | 5.0 |
0.23 ± 0.03 | 0.7 |
| J16102955−3922144 | 0.2 ± 0.1 | 3.5 |
0.22 ± 0.03 | 0.2 |
Notes. In this subsample, the dynamical M⋆ is estimatedwith our method described in Sect. 3 but with fixed PA and i adopted from the continuum analysis by Ansdell et al. (2016) and Tazzari et al. (2017). The spectroscopic M⋆ is obtained from Alcalá et al. (2014, 2017), which is estimated with the stellar evolutionary model by Siess et al. (2000).
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