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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)

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
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.


Radial velocity determined based on CaII lines.


No observations available.

Reference. References for the stellar radial velocity are: and

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