Table 2.
Projected semi-major axis, mass functions, effective temperature of the post-AGB star, luminosity of the post-AGB star, infrared luminosity as a function of post-AGB luminosity, SED category (Kluska et al. 2022), depletion, number of observations used in this work, and the average signal to noise in Hα.
| # | Object | a1sini | f(m) | Teff | Lmodel | LGaia | LIR/L⋆ | SED | Depletion | Nobs | (S/N)avg | Ref. |
|---|---|---|---|---|---|---|---|---|---|---|---|---|
| (AU) | (M⊙) | (K) | (L⊙) | (L⊙) | (L⊙) | |||||||
| 1 | AC Her | 1.18 ± 0.08 | 0.15 ± 0.03 | 5800 | 3600 ± 600 |
 |
0.21 | 2 | Mild | 33 | ∼65 | 1,6 |
| 2 | HD 213985 | 0.73 ± 0.03 | 0.78 ± 0.08 | 8250 | 300 ± 40 |
 |
0.45 | 1 | Strong | 25 | ∼70 | 1,11 |
| 3 | HD 52961 | 1.51 ± 0.03 | 0.274 ± 0.019 | 6000 | 1300 ± 200 |
 |
0.16 | 1 | Strong | 42 | ∼100 | 1,10 |
| 4 | IRAS 06165+3158 | 0.374 ± 0.011 | 0.10 ± 0.01 | 4250 | 600 ± 140 |
 |
0.08 | 3 | No | 28 | ∼30 | 1,13 |
| 5 | IRAS 19125+0343 | 0.56 ± 0.02 | 0.086 ± 0.010 | 7750 | 15 600 ± 2000 |
 |
1.33 | 0 | Strong | 20 | ∼55 | 1,14 |
| 6 | RV Tau | 1.38 ± 0.08 | 0.24 ± 0.02 | 4810 | 4700 ± 1000 |
 |
0.39 | 1 | Mild | 31 | ∼40 | 2 |
| 7 | SAO 173329 | 0.132 ± 0.003 | 0.023 ± 0.001 | 7000 | 1500 ± 200 |
 |
0.33 | 1 | No | 23 | ∼35 | 1,15 |
| 8 | SU Gem | 0.81 ± 0.04 | 0.15 ± 0.02 | 5250 | 1200 ± 200 |
 |
7.92 | 0 | Mild | 23 | ∼35 | 3,13 |
| 9 | U Mon | 3.4 ± 0.3 | 0.79 ± 0.18 | 5000 | 3600 ± 700 |
 |
0.23 | 3 | No | 36 | ∼40 | 1,16 |
| 10 | 89 Her | 0.106 ± 0.007 | 0.0019 ± 0.0004 | 6600 | 4200 ± 600 |
 |
0.42 | 1 | Mild | 26 | ∼125 | 1,5 |
| 11 | BD+46 442 | 0.3074 ± 0.0014 | 0.195 ± 0.003 | 6250 | 1000 ± 160 |
 |
0.16 | 1 | No | 52 | ∼40 | 1,7 |
| 12 | EP Lyr | 1.30 ± 0.12 | 0.22 ± 0.06 | 6200 | 7100 ± 1100 |
 |
0.02 | 3 | Moderate | 30 | ∼45 | 1,8 |
| 13 | HD 46703 | 0.839 ± 0.015 | 0.220 ± 0.012 | 6250 | 8200 ± 1300 |
 |
0.02 | 4 | Mild | 34 | ∼60 | 1,9 |
| 14 | HP Lyr | 1.27 ± 0.06 | 0.083 ± 0.007 | 6300 | 7900 ± 1300 |
 |
0.91 | 1 | Strong | 40 | ∼55 | 1,12 |
| 15 | IRAS 19135+3937 | 0.209 ± 0.008 | 0.075 ± 0.008 | 6000 | 600 ± 100 |
 |
0.28 | 1 | No | 22 | ∼35 | 1,13 |
| 16 | TW Cam | 0.83 ± 0.04 | 0.17 ± 0.02 | 4800 | 3200 ± 700 |
 |
0.46 | 1 | No | 42 | ∼50 | 1,16 |
Notes. The formal error on the effective temperatures is 250 K. Below the line are the objects of Paper I and II. The orbital data were obtained from (1) Oomen et al. (2018), (2) Manick et al. (2019), and (3) this work. The strength of the depletion patterns were determined by (1) Oomen et al. (2018) and (4) Oomen et al. (2019). The effective temperatures were obtained from (5) Kipper (2011), (6) Giridhar et al. (1998), (7) Gorlova et al. (2012), (8) Gonzalez et al. (1997), (9) Hrivnak et al. (2008), (10) Waelkens et al. (1991), (11) De Ruyter et al. (2006), (12) Giridhar et al. (2005), (13) Rao & Giridhar (2014), (14) Maas et al. (2005), (15) Rao et al. (2012), (16) Giridhar et al. (2000). The luminosities were calculated from the stellar radii found in this work (Lmodel) and from the Gaia parallaxes (LGaia). The infrared luminosities and SED categories are from Kluska et al. (2022).
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