Table 1
HC3N transitions in the G+0.693 spectral survey (Sect. 2).
| Transition (Jup – Jlow) | Frequency (GHz) | log I (nm2 MHz) | Eup (K) | Telescope | HPBW (″) | rms (mK) |
|---|---|---|---|---|---|---|
| Low-J | ||||||
| 5–4 | 45.4903 | –3.164 | 4.4 | Yebes 40m | 39 | 0.9 |
| 8–7 | 72.7838 | –2.564 | 12.2 | IRAM 30m | 34 | 3.5 |
| 9–8 | 81.8815 | –2.416 | 15.7 | IRAM 30m | 30 | 3.5 |
| 10–9 | 90.9790 | –2.285 | 19.6 | IRAM 30m | 27 | 1.1 |
| 11–10 | 100.0764 | –2.167 | 24.0 | IRAM 30m | 24 | 3.3 |
| 12–11 | 109.1736 | –2.061 | 28.8 | IRAM 30m | 22 | 2.0 |
| 14–13 | 127.3677 | –1.877 | 39.7 | IRAM 30m | 19 | 9.3 |
| 15–14 | 136.4644 | –1.796 | 45.8 | IRAM 30m | 18 | 3.6 |
| 16–15 | 145.5610 | –1.722 | 52.4 | IRAM 30m | 17 | 4.8 |
| 17–16 | 154.6573 | –1.653 | 59.4 | IRAM 30m | 16 | 2.3 |
| 18–17 | 163.7533 | –1.590 | 66.8 | IRAM 30m | 15 | 1.4 |
| 19–18 | 172.8493 | –1.531 | 74.7 | IRAM 30m | 14 | 1.6 |
| High-J | ||||||
| 22–21 | 200.1354 | –1.379 | 100.8 | IRAM 30m | 12 | 7.3 |
| 23–22 | 209.2302 | –1.335 | 110.5 | IRAM 30m | 12 | 7.3 |
| (a) | 218.3247 | –1.295 | 120.5 | IRAM 30m | 11 | 7.3 |
| 24–23 | APEX(b) | 27 | 1.0 | |||
| 25–24 | 227.4189 | –1.257 | 131.0 | IRAM 30m | 10 | 7.5 |
| 26–25 | 236.5128 | –1.222 | 141.9 | IRAM 30m | 10 | 7.5 |
| APEX | 25 | 2.1 | ||||
| Not used in the analysis | ||||||
| 2–1(c) | 18.1962 | –4.351 | 0.4 | GBT | 42 | 2.3 |
| 4–3 (c) | 36.3923 | –3.452 | 2.6 | Yebes 40m | 48 | 0.9 |
| 28–27(d) | 254.6995 | –1.160 | 165.0 | IRAM 30m | 10 | 10.6 |
| 29–28(e) | 263.7923 | –1.132 | 177.2 | APEX | 22 | 1.3 |
| 30–29( f) | 272.8847 | –1.106 | 189.8 | IRAM 30m | 9 | 10.6 |
Notes. Columns 1 and 2 list the rotational transitions and the related frequencies, respectively. Log I is the base 10 logarithm of the integrated intensity at 300 K and Eup is the energy of the upper level (Cols. 3 and 4). Columns 5, 6, and 7 indicate the telescope used, the relative halfpower beam width at the frequency of the transition, and the rms achieved, respectively. (a)This transition has also been mapped with SMA+APEX data, as explained in Sect. 2.2. (b)From single-pointing observations described in Sect. 2.1. (c)It includes more extended gas (see Appendix A). (d) Contaminated by CH2NH. (e) Contaminated by HNCO. ( f) Transition intensity within the spectrum noise level.
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