Table 1.
Physical and dust properties of the Galactic post-AGB stars targeted in this study.
| Source | ID | [Fe/H] | Teff [K] | L/L⊙ |  |
τ10 | Td [K] | Rin/R⊙ | Flag |
|---|---|---|---|---|---|---|---|---|---|
| IRAS 01259+6823 | 19 | −0.6 ± 0.1 | 5510 | 650 | 220–646 | 0.2 | 300 | 6.30 × 103 | Q1 |
| IRAS 08187–1905 | 20 | −0.6 ± 0.1 | 5772 | 2600 | 2099–3286 | 0.23 | 130 | 1.55 × 105 | Q2 |
| SAO 239853 | 21 | −0.8 ± 0.1 | 7452 | 20 500 | 13 080–48 520 | 0.28 | 140 | 3.80 × 105 | Q2 |
| HD 107369 | 22 | −1.1 ± 0.1 | 7533 | 900 | 814–1010 | < 10−4 | 150 | – | Q1 |
| HD 112374 | 23 | −1.2 ± 0.1 | 6393 | 11 000 | 9961–11 882 | ≤10−3 | 150 | 6.45 × 104 | Q1 |
| HD 133656 | 24 | −0.7 ± 0.1 | 8238 | 5200 | 4861–5690 | 0.005 | 150 | 2.00 × 105 | Q1 |
| HR 6144 | 25 | −0.4 ± 0.1 | 6728 | 25 500 | 22 212–30 419 | < 10−4 | 120 | – | Q1 |
| HD 161796 | 26 | −0.3 ± 0.1 | 6139 | 8000 | 5209–6322 | 0.3 | 130 | 2.85 × 105 | Q1 |
| IRAS 18025–3906 | 27 | −0.5 ± 0.15 | 6154 | 17 000 | 975–12 963 | 0.7 | 150 | 3.60 × 105 | Q2 |
| HD 335675 | 28 | −0.9 ± 0.2 | 6082 | 16 000 | 7303–28 359 | 0.9 | 390 | 3.95 × 104 | Q2 |
| IRAS 19386+0155 | 29 | −1.1 ± 0.14 | 6303 | 9600 | 4345–22 765 | 0.7 | 1000 | 6.00 × 103 | Q2 |
| IRAS 19475+3119 | 30 | −0.24 ± 0.15 | 8216 | 6500 | 5955–7545 | 0.09 | 120 | 4.15 × 105 | Q1 |
| HR 7671 | 31 | −1.6 ± 0.1 | 6985 | 3600 | 3449–3734 | < 10−4 | 30 | – | Q1 |
| J052740.75–702842.0 | LMC | −0.50 | 8283 | 5200 | – | 0.024 | 470 | 1.22 × 104 | – |
| J045119.94–670604.8 | LMC | −0.40 | 8280 | 5000 | – | 0.006 | 270 | 2.97 × 104 | – |
| J052241.52–675750.2 | LMC | −0.50 | 8284 | 5000 | – | 0.017 | 400 | 2.26 × 104 | – |
| J050221.17–691317.2 | LMC | −0.60 | 5250 | 4500 | – | 0.022 | 180 | 5.45 × 104 | – |
| J051906.86–694153.9 | LMC | −1.30 | 5613 | 3800 | – | 0.015 | 180 | 5.13 × 104 | – |
Notes. The quantities listed in the various columns are the following: 1: object name; 2: source ID (as reported in Kamath et al. 2022); 3 and 4: metallicity and effective temperatures, derived spectroscopically by Kamath et al. (2022); 5: luminosity derived in the present study for the Galactic sources; 6: luminosity from Kamath et al. (2022, see their Table 1), obtained in consideration of the upper and lower limits of the distances retrieved from Bailer-Jones et al. (2021); 7–9: optical depth at 10 μm, dust temperature and distance separating the central star from the inner border of the dusty region, found via SED fitting; 8: the quality flag (Q1 or Q2), based on the Gaia EDR3 renormalized unit weight error parameter, taken from Kamath et al. (2022). To ease the comparison with the results from Paper I, we report (in the 5 bottom lines) the non s-process enriched LMC sources studied in Paper I; for these sources, the metallicity and the effective temperature are from Kamath et al. (2015), while the luminosity and the dust properties are from Paper I.
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