Table 4
CH3NH2 column density ratios.
| CH3NH2 /CH2NH | CH3NH2/NH2CHO | CH3NH2/CH3CN | References | ||
|---|---|---|---|---|---|
| CH3CN reference | 13C | 15N | |||
| MM1 II | ≥5.2 | 38 | 1.28 | 1.94 | This work |
| MM2 I | ≥1.2 | 8.16 | 0.71 | 0.70 | This work |
| MM3 I | ≥3.0 | ≥60 | 0.54 | 0.31 | This work |
| Model F | 7.27 | 20.5 | 16.3 | 1 | |
| Model M | 1.5 | 24 | 17.1 | 1 | |
| Model S | 0.45 | 2.34 | 5.23 | 1 | |
| Sgr B2(M) | 31(a) | 3.21 | 0.25 | 2 | |
| Sgr B2(N) | 0.75 | 0.44 | 0.31 | 2 | |
| Sgr B2(N) | 7.14 | 2.08 | 35.7 | 3 | |
| Sgr B2(N) | 5.49 | – | – | 4 | |
| Orion KL Hot Core | ≤2.86 | ≤3.13 | – | 5 | |
| IRAS 16293–2422B | ≤0.88 | ≤0.053 | ≤0.013 | 6, 7 | |
| Comet 67P(b) | – | ≤0.33 | ≤2 | 8 | |
Notes. The uncertainty on the column density ratios derived towards NGC 6334 I is estimated to be 40% (see Sect. 2). (a) Extended CH2NH emission. (b)Listed as upper limits based on the discussion in Sect. 2.4 of Altwegg et al. (2017).
References.(1) Garrod (2013); (2) Belloche et al. (2013); (3) Neill et al. (2014); (4) Halfen et al. (2013); (5) Pagani et al. (2017), Laurent Pagani, priv. comm.; (6) Calcutt et al. (2018); (7) Ligterink et al. (2018); (8) Goesmann et al. (2015).
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