Table 2
Origin of emission at different velocity offsets.
| Envelope | Mstar | Disk only | Envelope onlya |
|---|---|---|---|
| velocity | (M⊙) | (km s−1) | (km s−1) |
| UCMb | 0.19 | v ≤−1.74;v ≥ 1.79 | 0.98 ≤ v ≤ 1.30 |
| UCMb | 0.45 | v ≤-2.54;v ≥ 2.59 | 1.47 ≤ v ≤ 1.79 |
| Free fall | 0.19 | v ≤−1.74;v ≥ 1.79 | v = 0.98 |
| Free fall | 0.45 | v ≤−2.54;v ≥ 2.59 | 1.47 ≤ v ≤ 1.63 |
| Modified | |||
| free fallc | 0.45 | v ≤−1.10;v ≥ 1.14 | 0.50 ≤ v ≤ 0.98 |
Notes.The fiducialmodel is highlighted in boldface. A disk radius of 125 au is adopted for all models, except in the modified free fall case where a radius of 74 au is used (A17). For a 125 au disk, the disk-only channels would then be v ≤ −0.94;v ≥ 0.98 km s−1 and the envelope-only channels would be 0.50 ≤ v ≤ 0.66 km s−1. (a) Only for 13CO for which the redshifted emission becomes optically thick in the envelope. (b) Infalling rotating envelope (Ulrich 1976; Cassen & Moosman 1981). (c)Free fall velocity modified by a factor 0.3 and a disk radius of 74 au (Ohashi et al. 2014, A17).
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