Table 4
Overview of evidence of the presence of disks in the CALYPSO sample of Class 0 objects.
| Source | Cont. emission(a) | Ang. momentum(b) | Kinematics on small scales(c) | ||||||||
|---|---|---|---|---|---|---|---|---|---|---|---|
| Compact | Cont. | Const. |  |
Grad.(h) | Kepl. | Kepl. |  |
||||
| cont. | size(e) | j(f) | (10−4 | rot.(i) | radius(j) | (M⊙) | |||||
| source(d) | (au) | km s−1 pc) | (au) | ||||||||
| L1448-2A | ✗ | <50 | ✓ | 4.5 ± 0.2 | ✗ | ... | ... | ... | |||
| L1448-NB | ✗ | <300(l) | ✓ | 16.0 ± 0.4 | ✓ | ✗ | <175 | ... | |||
| L1448-C | ✓ | 46 ± 15 | ✓ | 6.0 ± 0.2 | ✓ | ✓ | 200 | 0.8−2.3 | |||
| NGC 1333-IRAS 2A | ✓ | <62 | ✓ | 3.8 ± 0.4 | ✓ | ✗ | ... | ... | |||
| SVS13B | ✓ | <75 | ✓ | 2.5 ± 0.2 | ✓ | ✓(m) | 150 | 0.05−0.12 | |||
| NGC 1333-IRAS 4A | ✗ | <94 | ✗ | ... | ✗ | ... | ... | ... | |||
| NGC 1333-IRAS 4B | ✓ | 156 ± 31 | ✓ | 2.5 ± 0.3 | ✓ | ✗ | ... | ... | |||
| IRAM 04191 | ✓ | <60 | ✗ | ... | ✗ | ... | ... | ... | |||
| L1521F | ✓ | <60 | ✗ | ... | ✗ | ... | ... | ... | |||
| L1527 | ✓ | 54 ± 10 | ✓ | 5.6 ± 0.1 | ✓ | ✓ | 90 | 0.2−0.4 | |||
| SerpM-S68N | ✗ | <53 | ✗ | ... | ✗ | ... | ... | ... | |||
| SerpM-SMM4 | ✓ | 305 ± 42 | ✗ | ... | ✗ | ... | ... | ... | |||
| SerpS-MM18 | ✓ | <61 | ✗ | ... | ✓ | ✗ | ... | ... | |||
| SerpS-MM22 | ✓ | 88 ± 14 | ✗ | ... | ✗ | ... | ... | ... | |||
| L1157 | ✓ | <70 | ✗ | ... | ✗ | ... | ... | ... | |||
| GF9-2 | ✓ | 26 ± 9 | ✓ | 3.9 ± 0.3 | ✗ | ... | ... | ... | |||
Notes. (a)Compact continuum emission (Maury et al. 2019). (b)Specific angular momentum profile (Gaudel et al. 2020). (c)Gas kinematics down to 50 au scales (this study). (d)Detection of a compact continuum component in addition to emission of the extended envelope. The ✗ and ✓ symbols indicate a non-detection and a detection, respectively. (e) Radius of the compact continuum component scaled to the assumed distance. (f)Constant specific angular momentum j at scales between 50 and 1200 au. (g)Mean value of the specific angular momentum at scales <100 au, for sources in which j is constant. (h)Velocity gradient perpendicular to the jet, within ± 45°. (i) Detection of Keplerian rotation. (j)Radius of the region in Keplerian rotation. (k)Mass of the central object. (l)Upper limit derived from a model centered on NB2. There is no clear evidence for a disk-like component centered on NB2 at ≲ 1′′ scales (Maury et al. 2019, Table C.3). (m)Tentative detection.
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