Table 4
Methylamine upper limits using the CH3 antisymmetric stretch band at 2898 cm−1.
| Source | N(CH3NH2) | (% H2O) |
|---|---|---|
| 1017 cm−2 | ||
| CRBR2422.8-342 | ≤6.7 | 16 |
| L1489 IRS | ≤2.3 | 5.3 |
| HH46 | ≤8.4 | 10 |
| DG Tau | ≤1.7 | 7.4 |
| RNO91 | ≤2.5 | 5.9 |
| HH300 | ≤2.1 | 8.0 |
| Mon R2 IRS 3 | ≤0.8 | 5.3 |
| NGC 7538 IRS 1 | ≤0.8 | 3.1 |
| NGC 7538 IRS 9 | ≤1.7 | 2.6 |
| W33 A | ≤4.2 | 3.4 |
| Comet 67P(a),(b) | – | 0.16 |
| Model(c) | – | 0.65 |
Notes. The methylamine abundances detected in the comet 67P/Churyumov-Gerasimenko and the predicted abundance for gas-grain astrochemical models of prestellar cores are also presented for comparison.
References.(a)Le Roy et al. (2015); (b)Altwegg et al. (2016); (c)Ioppolo et al. (2021).
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