Table A.2
Observational results at the 4′′ E EVS.
| Line | Telescope | S 1 | Δυ1 |
| [Jy] | [km s-1] | ||
|
|
|||
| 12CO(1–0) | SEST | 0.81 | |
| 12CO(2–1) | ALMA | 3.0 | 15.7 |
| 12CO(3–2) 2 | APEX | 3.4 | |
| 12CO(4–3) 3 | APEX | 3.0 | |
| 13CO(1–0) | SEST | 0.16 | |
| 13CO(2–1) | ALMA | 1.1 | 10.0 |
| C18O(2–1) | ALMA | 0.061 | 8.7 |
| 13CS(5–4) | ALMA | 0.047 | 7.3 |
| SO(55–44) | ALMA | 0.074 | 9.4 |
| SO(65–54) | ALMA | 0.093 | 8.9 |
| SiO(5–4) | ALMA | 0.50 | 7.8 |
| 29SiO(5–4) | ALMA | 0.19 | 6.8 |
| H2CO(303–202) | ALMA | 0.14 | 7.2 |
| H2CO(322–221) | ALMA | 0.042 | 7.6 |
| H2CO(321–220) | ALMA | 0.041 | 6.5 |
H CO(312 − 211) |
ALMA | 0.03 | 8.3 |
| CH3OH(42–31) | ALMA | 0.039 | 6.5 |
| CH3OH(8-1–70) | ALMA | 0.065 | 7.4 |
Notes. The ALMA data are integrated over an 1′′× 1′′ area centered on the spot.
The 1σ noise levels lie in the range 2−4 mJy, therefore the uncertainties in the line parameters are dominated by uncertainties in the cleaning process and the somewhat complicated brightness distributions. We estimate the uncertainties to be about 25% in the flux density and 1 km s-1 in the line width.
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