Table 1
Observational parameters related to the molecular lines presented in this work.
| Line | Frequency | Eu ∕k | θbeam | δv | σ | Mapping area | Telescope |
|---|---|---|---|---|---|---|---|
| (GHz) | (K) | (′′) | (km s−1) | (mK) | (′ × ′) | ||
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) |
| C18O J = 1−0 | 109.7821734(63) | 5.3 | 25 | 0.05 | 92 | 2.5 × 9 | IRAM-30 m |
| 13CO J = 1−0 | 110.2013543(1) | 5.3 | 25 | 0.14 | 92 | 2.5 × 9 | IRAM-30 m |
| C17O J = 1−0 | 112.358982(15) | 5.4 | 25 | 0.14 | 100 | 2.5 × 9 | IRAM-30 m |
| C18O J = 2−1 | 219.5603541(15) | 15.8 | 32 | 0.08 | 65 | 3 × 9 | APEX-12 m |
| 13CO J = 2−1 | 220.3986842(1) | 15.9 | 32 | 0.08 | 59 | 3 × 9 | APEX-12 m |
| C17O J = 2−1 | 224.714187(80) | 16.2 | 32 | 0.08 | 65 | 3 × 9 | APEX-12 m |
Notes. (1)Observed transition. (2) Rest frequency taken from the Cologne Database for Molecular Spectroscopy (CDMS7, Müller et al. 2005). Uncertainties in the last digits are given in parentheses. For the C17O lines, only the frequency of the strongest HFS component is listed. (3) Upper energy level of the observed transition. (4) HPBW. (5) Channel widths in units of velocity. (6) RMS noise level. (7) Size of the mapped area. (8) Telescope.
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