Table 3
Overview of the D/H ratios of water in the warm region (≲100 au, T ≳ 100 K) toward Class 0 protostars.
| Object | HDO/H2O (× 10−4) | D2O/HDO (× 10−2) | fD2/fD1 | Reference |
|---|---|---|---|---|
| Clustered protostars | ||||
| NGC 1333 IRAS 2A | 7.4 ± 2.1 | ... | ... | 1 |
| – | 17 ± 8 | 1.2 ± 0.5 | 7 ± 4 | 2 |
| NGC 1333 IRAS 4A-NW | 5.4 ± 1.5 | ... | ... | 1,3 |
| NGC 1333 IRAS 4B | 5.9 ± 2.6 | ... | ... | 1 |
| IRAS 16293–2422 | 9.2 ± 2.6 | ... | ... | 1 |
| Isolated protostars | ||||
| BHR71–IRS1 | 18 ± 4 | ... | ... | 3 |
| B335 | 17 ± 3 | ... | ... | 3 |
| – | 63 ± 15 | 1.4 ± 0.1 | 2.2 ± 0.5 | 4 |
| L483 | 22 ± 4 | ... | ... | 3 |
| – | 40 ± 5 | 1.0 ± 0.2 | 2.5 ± 0.3 | 4 |
Notes. For L483 and B335, the reported values are derived from the synthetic spectrum model. The table only include interferometric observations of the inner warm region toward low-mass Class 0 protostars.
References. (1) Persson et al. (2014); (2) Coutens et al. (2014); (3) Jensen et al. (2019); (4) This work.
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