Table A.1
HDO/H2O abundance ratios for different objects.
| Type | Object | Origin | HDO/H2O | Tracers | Ref. |
| [× 10-4] | (Proxy) | ||||
|
|
|||||
| Comet | 1/P Halley | (OCC) | 6.3 ± 0.7 | H3O+, H2DO+ | 1 |
| Comet | C/1996 B2 Hyakutake | (OCC) | 5.8 ± 2.0 | H O, HDO |
2 |
| Comet | C/1995 O1 Hale-Bopp | (OCC) | 6.6 ± 1.6 | HDO, OH | 3 |
| Comet | 8P/Tuttle | (OCC) | 8.2 ± 2.9 | HO, HDO |
4 |
| Comet | C/2007 N3 Lulin | (OCC) | < 11.2 | HO, HDO |
5 |
| Comet | C/2002 T7 LINEAR | (OCC) | 5 ± 1.4 a | OH, 18OH, OD | 6 |
| Comet | 153P Ikeya-Zhang | (OCC) | < 5.6 ± 0.6 | HO, H O, HDO |
7 |
| Comet | C/2009 P1 Garradd | (OCC) | 2.06 ± 0.22 | HO, H2O, HDO |
8 |
|
|
|||||
| OCC Meanc | 6.4 ± 1.0 | ||||
|
|
|||||
| Comet | 103P Hartley 2 | (JFC) | 3.2 ± 0.5 | HO, HDO |
9 |
| Comet | 45P Honda-Mrkos-Pajdusakov (HMP) | (JFC) | < 4.0 | HO, HO, HDO |
10 |
|
|
|||||
| Planet | Earth (SMOW) | 3.114 ± 0.002 | 11 | ||
|
|
|||||
| Protosolar | 0.42 ± 0.08 b | 3He, 4He | 12 | ||
| (L)ISMc | ≥ 0.40 ± 0.02 | H, D | 13 | ||
|
|
|||||
| Protostar | IRAS 16293-2422 | <50 AU | 9.2 ± 2.6 | HO, HDO |
14 |
| Protostar | 340 | H O, HO, HD18O, HDO |
15 | ||
| Protostar | 300 | HO, HDO |
16 | ||
| Protostar | NGC 1333-IRAS 2A | ≲300 AU | 7.4 ± 2.1 | HO, HDO |
17 |
| Protostar | ≥ 100 | HO, HDO |
18 | ||
| Protostar | 30−800 | HO, HDO |
19 | ||
| Protostar | NGC 1333-IRAS 4A-NW | ≲300 AU | 19.1 ± 5.4 | HO, HDO |
17 |
| Protostar | 50−300 | HO, HDO |
19 | ||
| Protostar | 4−30 | HO, HDO |
20 | ||
| Protostar | NGC 1333-IRAS 4B | ≲300 AU | 5.9 ± 1.7 | HO, HDO |
17 |
| Protostar | 1−37 | HO, HDO |
20 | ||
| Protostar | < 6.4 | HO, HDO |
21 | ||
Notes. OCC – Oort Cloud Comet, JFC - Jupiter Family Comet. Some values are 2 × the D/H ratio and that the ratio in protostars refers to the warm gas in the inner regions.
Reference. (1) Eberhardt et al. (1995); (2) Bockelée-Morvan et al. (1998); (3) Meier et al. (1998); (4) Villanueva et al. (2009); (5) Gibb et al. (2012); (6) Hutsemékers et al. (2008); (7) Biver et al. (2006); (8) Bockelée-Morvan et al. (2012); (9) Hartogh et al. (2011); (9) Lis et al. (2013); (11) de Laeter et al. (2003, and ref. therein); (12) Geiss & Gloeckler (1998); Lellouch et al. (2001); (13) Prodanović et al. (2010, and ref. therein); (14) Persson et al. (2013); (15) Coutens et al. (2012); (16) Parise et al. (2005); (17) This work; (18) Liu et al. (2011); (19) Taquet et al. (2013); (20) (Coutens et al. 2013); (21) Jørgensen & van Dishoeck (2010b).
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