Table 1.
Detected lines in our IRAM observations.
| ν | Backend | Δv |
 |
rms | |
|---|---|---|---|---|---|
| (GHz) | (km s−1) | (K) | (mK) | ||
| 12CO | 115.271 | FTS | 0.52 | 25.3 | 50–100 |
| 13CO | 110.201 | FTS | 0.54 | 10.8 | 50–100 |
| VESPA | 0.054 | 11.9 | 150–300 | ||
| C18O | 109.782 | FTS | 0.54 | 2.6 | 50–100 |
| VESPA | 0.054 | 4.1 | 150–300 | ||
| N2H+ | 93.1763 | FTS | 0.64 | 1.8 | 50–100 |
Notes. The beam FWHM ranges from 21″ at 115 GHz to 26″ at 93 GHz. The columns are (1) the name of the species. All the transitions are J = 1 − 0. (2) Frequency of the transition from the CDMS database (Endres et al. 2016), except for N2H+, which is taken from Pagani et al. (2009). For transitions with multiple components, ν is given for the component with the highest frequency. (3) Spectrometer used to record the data. FTS and VESPA were used at resolutions of 200 kHz and 20 kHz, respectively. (4) Velocity resolution. All spectra were resampled with channels of 0.6 km s−1 (FTS) or 0.06 km s−1 (VESPA). (5) Maximum main-beam temperature of the transition in the map. (6) Approximate rms range computed from a 10 km s−1 range, at least 20 km s−1 off the line, where no astronomical signal is found.
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