Table 1
Binary post-AGB stars observed in this paper.
| Source | Mneb [M⊙] |
 |
Vlsr [kms−1] |
d [pc] |
|---|---|---|---|---|
| AC Herculis | 8.3 × 10−4 | ≳ 95 | −9.7 | 1100 |
| Red Rectangle | 1.4 × 10−2 | 90 | 0 | 710 |
| 89 Herculis | 1.4 × 10−2 | 50 | −8.0 | 1000 |
| HD52961 | 1.3 × 10−2 | ~50 | −7 | 2800 |
| IRAS 19157-0257 | 1.4 × 10−2 | ~50 | 46 | 2900 |
| IRAS 18123+0511 | 4.7 × 10−2 | ~30 | 99 | 3500 |
| IRAS 19125+0343 | 1.1 × 10−2 | 30 | 82.0 | 1500 |
| AI Canis Minoris | 1.9 × 10−2 | 25 | 29 | 1500 |
| IRAS 20056+1834 | 1.0 × 10−1 | 25 | −9 | 3000 |
| R Scuti | 3.2 × 10−2 | 25 | 56.1 | 1000 |
Notes. Sources are ordered based on their outflow/disk mass ratio. Nebular masses (Mneb) and velocities (VLSR) are derived from our single-dish and interferometric observations (Bujarrabal et al. 2013a, 2016; Gallardo Cava et al. 2021), except for HD 52961 (Gallardo Cava et al. in prep). Distances (d) are adopted from Bujarrabal et al. (2013a) except for HD 52961 (Oomen et al. 2019).
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