Table 3.
Source parameters assumed for cyanoketene in each of the sets of observations.
| Source | Telescope | θs(a) | Tbg | ΔV | Tb (†) | Tex | Refs. |
|---|---|---|---|---|---|---|---|
| (″) | (K) | (km s−1) | (mK) | (K) | |||
| NGC 6334I | ALMA | – | 28.2 | 3.2 | 10.0 (b) | 135 | 1 |
| Sgr B2(N) | GBT | 20 | 19.2 | 25.0 | 3.7 | 5 | 2, 14, 15 |
| Sgr B2(N) | IRAM | 2.2 | 5.2 | 5.0 | 10.9 | 120 | 3 |
| Barnard 1 | IRAM | – | 2.7 | 0.8 | 2.5 | 10 | 4, 5 |
| IRAS 4A | IRAM | – | 2.7 | 5.0 | 2.3 | 21 | 4, 6 |
| L1157B1 | IRAM | – | 2.7 | 8.0 | 1.4 | 60 | 7 |
| L1157mm | IRAM | – | 2.7 | 3.0 | 2.8 | 60 | 7 |
| L1448R2 | IRAM | – | 2.7 | 8.0 | 2.4 | 60 | 8 |
| L1527 | IRAM | – | 2.7 | 0.5 | 1.9 | 12 | 8, 9 |
| L1544 | IRAM | – | 2.7 | 0.5 | 2.3 | 10 | 10, 11 |
| SVS13A | IRAM | 0.3 | 2.7 | 3.0 | 7.5 | 80 | 4, 6 |
| TMC1 | IRAM | – | 2.7 | 0.3 | 6.5 | 7 | 12, 13 |
Notes.
Taken either as the 1σ rms noise level at the location of the target line, or for line confusion limited spectra, the reported rms noise of the observations.
References. [1] McGuire et al. (2018a); [2] Neill et al. (2012); [3] Belloche et al. (2013); [4] Melosso et al. (2018); [5] Cernicharo et al. (2018); [6] Higuchi et al. (2018); [7] McGuire et al. (2015); [8] Jørgensen et al. (2002); [9] Araki et al. (2017); [10] Hily-Blant et al. (2018); [11] Crapsi et al. (2005); [12] McGuire et al. (2018b); [13] Gratier et al. (2016); [14] Remijan et al. (2008); [15] McGuire et al. (2016).
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