Table 2
Detected CO lines, their radial velocities with a typical error of 2 km s-1 as determined in Sect. 5.3, and the stellar radial velocities derived from photospheric absorption lines in Cols. 1–3.
| Name | v CO | v ⋆ | 12CO | 12CO | 12CO | 12CO | 12CO | 13CO | 12CO |
| km s-1 | km s-1 | vu = 1 | vu = 2 | vu = 3 | vu = 4 | vu = 5 | vu = 1 | v = (2–0) | |
|
|
|||||||||
| Emission | |||||||||
| HD 100546 | 14 | 18a | R08–P37 | R17–P28 | R25–P21 | R32–P17 | R39–P09 | R18–P23 | no |
| HD 97048 | 16 | 21a | R08–P36 | R17–P07 | R26–R05 | R27–P17 | R33–P09 | R15–R04 | no |
| HD 179218 | 17 | 15.4 ±2.3b | R06–P36 | R14–P28 | R23–P21 | R27–P20 | – | R21–P21 | no |
| HD 101412 | 16 | 16.9 ±0.2b | R09–P37 | R17–P32 | R26–P26 | R35–P20 | – | R23–P29 | yes |
| HD 141569 | –11 | −12 ±7c | R09–P13† | R14–P01† | ‡ | ‡ | ‡ | R09–R00† | no |
| HD 190073 | –1 | 0.21 ±1.03 | R08–P38 | R13–P32 | – | – | – | R23–P23 | no |
| HD 98922 | 3 | 0.2 ±2.2c | R07–P38 | R13–P28 | – | – | – | R16–P27 | ⋆ |
| HD 95881 | 18 | 36a, ■ | R06–P37 | – | – | – | – | R16–P25 | no |
| R CrA | –13◇ | 0d | P04–P37 | – | – | – | – | – | no |
| HD 135344B | 2 | 1.6 ±1.3b | R08–P38 | – | – | – | – | – | no |
| HD 150193 | –6 | −4.9 ±3.9c | R06–P36 | – | – | – | – | – | no |
| HD 104237 | 14 | 13a | R08–P10† | – | – | – | – | – | ⋆ |
| HD 142666 | – | −7.0 ±2.7c | – | – | – | – | – | – | ⋆ |
| Absorption | |||||||||
| HD 97048 | 16 | 21a | R04–P04 | – | – | – | – | R02–P01 | no |
| R CrA | –3 | 0d | R08–P15 | – | – | – | – | R08–P04 | R08–P08 |
Notes. Emission lines are listed in the upper panel, and absorption lines in the lower.
Even though we do not detect these CO transitions in our spectra, they have been detected by Brittain et al. (2007) in this source.
Not all spectra have S/N sufficient to identify the ro-vibrational transitions, accordingly this may be a subset of all transitions.
The CO emission lines from R CrA most likely originate from an outflow as discussed in Sect. 5.5.
Reference. References for the stellar radial velocity are: and
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