Table B.1.
Selected methanol transitions.
Transition | ν [GHz] | A/E | Eup/k [K] | L1641N | CARMA-7 | IRAS 16293 | NGC 2024 | Serpens FIRS | Serpens SMM4 | potential blending lines |
---|---|---|---|---|---|---|---|---|---|---|
7−1→60 | 181.295971 | E | 70.55 | ✓ | ✓ | ✓ | ✓ | ✓ | ✓ | 13CC2N, CH3OH with Eup = 1025.4 K |
41→31 | 193.506559 | E | 44.26 | ✓ | ✓ | ✓ | ✓ | ✓ | ✓ | |
41→31 | 195.146790 | A− | 37.95 | ✓ | ✓ | ✓ | ✓ | ✓ | ✓ | CH3OCHO |
91→90 | 322.239462 | A−+ | 119.88 | ✓ | ✓ | ✓ | ✓ | ✓ | ✓ | – |
101→100 | 326.630583 | A−+ | 143.27 | – | – | ✓ | – | ✓ | ✓ | – |
10−1→90 | 326.961232 | E | 133.15 | ✓ | ✓ | ✓ | ✓ | ✓ | ✓ | S17O, H2CCHCN |
71→61 | 335.582017 | A+ | 78.97 | ✓ | ✓ | ✓ | ✓ | ✓ | ✓ | – |
70→60 | 338.124488 | E | 78.08 | ✓ | ✓ | ✓ | ✓ | ✓ | ✓ | – |
7−1→6−1 | 338.344588 | E | 70.55 | ✓ | ✓ | ✓ | ✓ | ✓ | ✓ | – |
70→60 | 338.408698 | A+ | 64.98 | ✓ | ✓ | ✓ | ✓ | ✓ | ✓ | CH3OH with Eup = 243.8 K |
7−3→6−3 | 338.559963 | E | 127.71 | ✓ | ✓ | ✓ | – | ✓ | ✓ | – |
73→63 | 338.583216 | E | 112.71 | ✓ | – | ✓ | ✓ | ✓ | – | 33SO, CH3SH |
71→61 | 338.614936 | E | 86.05 | ✓ | ✓ | ✓ | ✓ | ✓ | ✓ | CH3OCHO |
72→62 | 338.639802 | A+ | 102.72 | ✓ | – | ✓ | ✓ | ✓ | ✓ | C2H5C–13–N |
71→61 | 341.415615 | A− | 80.09 | ✓ | ✓ | ✓ | ✓ | ✓ | ✓ | cis–DCOOH, n–C3H7CN |
Notes. Selected methanol lines used to perform our rotation diagrams (Fig. A.1). Possible contamination with other molecules is mentioned in the rightmost column. ✓ indicates well-distinguished/confidently-detected lines while the dash symbol (–) indicates a poor signal or non-detection. Certain methanol species that are highly improbable to blend with others are also identified: The 7−1→60 − E line falls within the range of frequencies of the 192→183 − E methanol line in all sources while the 70→60 − A+ methanol transition falls within the frequency range of the 76→66 − E methanol transition for the case of IRAS 16293 and CARMA 7, given the higher FWHM of the CH3OH lines in these sources compared to the rest of the sample. Line frequencies and upper-level energies were taken from the CDMS database (Müller et al. 2005).
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