Table A.1
Measured HDO/H2O and D/H ratios for comets and protostars.
| Object | HDO/H2O (× 10−4) | Tracers | Reference |
|---|---|---|---|
| Oort cloud comets | |||
| 1/P Halley | 4.2 ± 0.6 | H2DO+, H3O+ | 1 |
| C/1996 B2 Hyatuake | 5.8 ± 2.0 | HDO, H2O | 2 |
| C/1995 O1 Hale-Bopp | 6.6 ± 1.6 | HDO, H2O | 3 |
| C/2007 B3 Lulin | <11.2 | HDO, H2O | 4 |
| 8P/Tuttle | 8.2 ± 3.0 | HDO, H2O | 5 |
| C/2009 P1 Garradd | 4.12 ± 0.44 | HDO, H O, H2O |
6 |
| C/2002 T7 LINEAR | 5.0 ± 1.4 | OD, OH, 18OH | 7 |
| 153P Ikeya-Zhang | <5.6 ± 0.6 | HDO, H O |
8 |
| C/2012 F6 Lemmon | 6.5 ± 1.6 | HDO, H O, H2O |
9 |
| C/2014 Q2 Lovejoy | 1.4 ± 0.4 | HDO, H O, H2O |
9 |
| Jupiter family comets | |||
| 45P Honda-Mrkos-Pajdusakov (HMP) | <4.0 | HDO, H O, H2O |
10 |
| 103P Hartley 2 | 3.2 ± 0.5 | HDO, H O, H2O |
11 |
| 67/P Churyumov-Gerasimenko | 10.6 ± 1.4 | HDO, HD18O, H2O, H O |
12 |
| 46P/Wirtanen | 3.2 ± 1.3 | HDO, H O |
13 |
| Clustered protostars | |||
| NGC 1333 IRAS 4A-NW | 5.4 ± 1.5 | HDO, H O |
14 (a) |
| NGC 1333 IRAS 2A | 7.4 ± 2.1 | HDO, H O |
14 |
| NGC 1333 IRAS 4B | 5.9 ± 2.6 | HDO, H O |
14 |
| IRAS 16293–2422 | 9.2 ± 2.6 | HDO, H O |
14 |
| Isolated protostars | |||
| BHR71–IRS1 | 18 ± 4 | HDO, H O |
15 |
| B335 | 17 ± 3 | HDO, H O |
15 |
| L483 | 22 ± 4 | HDO, H O |
15 |
Notes. Protostars only include interferometric observations of hot corino emission toward low-mass Class 0 protostars. Conversions between HDO/H2O and D/H assumes the statistical ratio HDO/H2O = 2 × D/H. (a) Note that the value for IRAS 4A–NW has been adjusted from the value derived in Persson et al. (2014) since a mistake in the data analysis was discovered, which enhanced the HDO abundance by a factor of ~ 2.
References. (1) Brown et al. (2012); (2) Bockelée-Morvan et al. (1998); (3) Meier et al. (1998); (4) Gibb et al. (2012); (5) Villanueva et al. (2009); (6) Bockelée-Morvan et al. (2012); (7) Hutsemékers et al. (2008); (8) Biver et al. (2006); (9) Biver et al. (2016); (10) Lis et al. (2013); (11) Hartogh et al. (2011); (12) Altwegg et al. (2015); (13) Lis et al. (2019); (14) Persson et al. (2014); (15) this paper.
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