Table B.1
Comparison between heliocentric velocities derived from CO observations and those compiled by Oomen et al. (2018) for the CO-observed post-AGB disk sources.
| Source | VLSR [km s−1] | Vhel, CO [km s−1] | Vhel [km s−1] | Residual [km s−1] |
|---|---|---|---|---|
| Red Rectangle | 0.0 | 18.8 | 20.0 | –1.2 |
| IRAS 08544–4431 | 45.0 | 61.0 | 62.4 | –1.4 |
| ACHer | –10.0 | –29.69 | –28.8 | –0.9 |
| IRAS 19157–0247 | 49.0 | 33.1 | 31.7 | 1.4 |
| HD 213985 | –29.0 | –27.5 | –42.0 | 14.5 |
| DYOri | –16.0 | –1.6 | –0.1 | –1.5 |
| HD 52961 | –7.0 | 7.6 | 6.2 | 1.4 |
| UMon | 10.5 | 28.1 | 24.1 | 3.9 |
| HR 4049 | –45.0 | –33.4 | –31.9 | –1.5 |
| HD 95767 | –32.0 | –21.0 | –20.3 | –0.7 |
| HD 108015 | –2.0 | 4.3 | 4.0 | 0.3 |
| 89Her | −8.0 | –27.9 | –27.0 | –0.9 |
| IRAS 19125+0343 | 84.0 | 66.9 | 67.3 | –0.4 |
Notes. The heliocentric velocities derived from CO emission (Vhel,CO) are compared with those compiled by Oomen et al. (2018) (Vhel), and the residuals are defined as Vhel,CO - Vhel. The LSR velocities (VLSR) are included for reference. velocities are in km s−1 . The CO velocities can be found in this work and in Bujarrabal et al. (2013, 2016, 2017, 2018); Gallardo Cava et al. (2021).
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