Table 3
Surrounding cloud dust temperatures and statistical deuterium fractionations observed towards protostellar hot cores.
| Source | Tdust | D/H (CH2 DOH) | D/H (CH3 OD) | [CH2DOH]/ | D/H (CH2DCN) | D/H (HDO) | Ref. |
|---|---|---|---|---|---|---|---|
| (K) | (%) | (%) | [CH3OD] | (%) | (%) | ||
| IRAS 16293-B | 16.6 ± 1.1 | 2.4 ± 0.5 | 1.8 ± 0.4 | 3.9 ± 1.1 | 1.2 ± 0.3 | 0.046 ± 0.013 | [1, 2, 3] |
| IRAS 2A | 13.1 ± 0.7 | 1.9 ± 0.5 | 1.6 − 7.1 | 0.8 − 3.6 | 1.2 ± 0.4 | 0.085 ± 0.040 | [4, 5] |
| IRAS 4A | 13.1 ± 0.7 | 1.2 ± 0.4 | 0.7 − 3.1 | 1.2 − 5.3 | 0.90 ± 0.37 | 0.17 ± 0.08 | [4, 6] |
| HH212 | 15.3 ± 0.7 | 1.0 ± 0.3 | 0.4 − 2.0 | 1.5 − 7.2 | – | – | [7, 4] |
| NGC 7129 FIRS1 | 19.3 ± 0.2 | 0.21 ± 0.04 | – | – | – | – | [8] |
| Sgr B2 | 24 ± 1 | 0.04 | 0.07 | 1.7 | 0.13 | – | [9] |
| Orion KL | 24.3 ± 0.4 | 0.037 ± 0.007 | 0.15 ± 0.05 | 0.73 ± 0.27 | – | 0.13 ± 0.06 | [10, 11] |
| NGC 6334 IMM1I | 23.9 ± 0.8 | 0.020 ± 0.007 | 0.48 ± 0.12 | 0.13 ± 0.03 | – | – | [12] |
Notes. For the CH3 OD column densities in IRAS 2A, IRAS 4A, and HH212, two estimates are given using the partition functions estimated by Parise (2004) and Jørgensen et al. (2018). The highest CH3 OD column densities (and the lowest [CH2 DOH]/[CH3OD] ratios) are those with the partition function estimated by Jørgensen et al. (2018).
References.[1] Jørgensen et al. (2018); [2] Calcutt et al. (2018); [3] Persson et al. (2013); [4] this work; [5] Coutens et al. (2014); [6] average between HDO/H2O ratios of 5 × 10−3 (Taquet et al. 2013a) and 5.4 × 10−4 (Persson et al. 2014, M. Persson, priv. comm.); [7] Bianchi et al. (2017); [8] Fuente et al. (2014); [9] Belloche et al. (2016); [10] Peng et al. (2012); [11] Neill et al. (2013); [12] Bøgelund et al. (2018).
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