Table 1.
Observed line parameters for HC3S+ in the laboratory and in TMC-1.
| Ju − Jl | νobs(a) | νo − νc(b) |  (c) |
Δv(d) |  |
|---|---|---|---|---|---|
| (MHz) | (kHz) | (mK km s−1) | (km s−1) | (mK) | |
| 3–2 (e) | 16412.7583 | −1.8 | ... | ... | ... |
| 4–3 (e) | 21883.6632 | 2.4 | ... | ... | ... |
| 5–4 (e) | 27354.5443 | −0.8 | ... | ... | ... |
| 6–5 | 32825.4090 | 0.0 | 1.71 ± 0.40 | 0.61 ± 0.12 | 2.6 ± 0.4 |
| 7–6 | 38296.2400 | −7.5 | 1.74 ± 0.30 | 0.52 ± 0.09 | 3.1 ± 0.4 |
| 8–7 | 43767.0670 | 9.5 | 2.05 ± 0.30 | 0.40 ± 0.15 | 3.9 ± 0.4 |
| 9–8 | 49237.8310 | −3.4 | 3.20 ± 0.95 | 0.79 ± 0.15 | 3.6 ± 0.9 |
Notes.
Observed frequencies in the laboratory (below 30 GHz) and towards TMC-1 (above 30 GHz). For this source we adopted a vLSR of 5.83 km s−1 (Cernicharo et al. 2020a,b,c). The frequency uncertainty is 3 and 10 kHz for the laboratory and astronomical lines, respectively.
Observed minus calculated frequencies in kHz. The calculated frequencies are obtained from the merged fit to the astronomical and laboratory measurements (see Sect. 5).
Line width at half intensity derived by fitting a Gaussian function to the observed line profile (in km s−1).
Line observed in the laboratory (see Sect. 5).
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