Table 4
Centrifugal radius Rcent assuming angular momentum conservation.
| Source | ⟨j100 au ⟩(a) | M100 au (b) | Rcent (c) |  (d) |
 (e) |
|---|---|---|---|---|---|
| (10−4 km s−1 pc) | (M⊙) | (au) | (au) | (M⊙) | |
| L1448-2A | 4.5 ± 0.2 | 0.005–0.2 | 50−1810 | <50 | 0.2 |
| L1448-NB | 16.0 ± 0.4 | 0.042–0.2 | 500−2920 | <50 | 3.0 |
| L1448-C | 6.0 ± 0.2 | 0.025–0.2 | 70−690 | 41 ± 15 | 0.5 |
| IRAS2A | 3.8 ± 0.4 | 0.020–0.2 | 30−330 | ≲65 | 0.1 |
| SVS13-B | 2.5 ± 0.2 | 0.019–0.2 | 10−160 | ≲75 | 0.05 |
| IRAS4B | 2.5 ± 0.3 | 0.003–0.2 | 10−840 | 155 ± 30 | 0.02 |
| L1527 | 5.6 ± 0.1 | 0.001–0.2 | 70−1060 | 54 ± 10 | 0.3 |
| GF9-2 | 3.9 ± 0.3 | 0.002–0.2 | 40−3080 | 36 ± 9 | 0.2 |
Notes. (a) Weighted mean of specific angular momentum in the inner envelopes (50 au < r ≤ 1600 au). (b) Range of the object mass at 100 au, the minimum and maximum values are defined in Sect. 5.3. (c) Centrifugal radii estimated from ⟨j100 au⟩ and M100 au using Eq. (2), assuming conservation of angular momentum. (d) Candidate disk radius determined from the CALYPSO study of PdBI dust continuum emission at 1.3 and 3 mm (Maury et al. 2019), corrected by the assumed distance (see Table 1). (e) Total minimum mass that needs to be enclosed at r < 100 au to form a disk equal to 
if the angular momentum ⟨j100 au⟩ was conserved. This minimum mass considers the mass of the stellar embryo and the mass of the optically thick inner envelope enclosed within 100 au.
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