Table 1.
Physical and dust properties of the Galactic post-AGB stars in this study.
Source | ID | [Fe/H] | Teff[K] | L/L⊙ |
![]() |
C/O | τ10 | Td[K] | Rin/R⊙ | Flag |
---|---|---|---|---|---|---|---|---|---|---|
IRAS Z02229+6208 | 1 | −0.45 ± 0.14 | 5952 | 13000 | 9973–1611 | − | 0.0082 | 300 | 1.84 × 105 | Q2 |
IRAS 04296+3429 | 2 | −0.62 ± 0.11 | 7272 | 6000 | 5971–20082 | − | 0.007 | 280 | 1.74 × 105 | Q2 |
IRAS 05113+1347 | 3 | −0.49 ± 0.15 | 5025 | 2100 | 1043–6731 | 2.42 ± 0.40 | 0.026 | 200 | 1.84 × 105 | Q2 |
IRAS 05341+0852 | 4 | −0.54 ± 0.11 | 6274 | 300 | 197–592 | 1.06 ± 0.30 | 0.028 | 320 | 2.60 × 104 | Q2 |
IRAS 06530-0213 | 5 | −0.32 ± 0.11 | 7809 | 6900 | 2736–8178 | 1.66 ± 0.36 | 0.0047 | 200 | 4.64 × 105 | Q2 |
IRAS 07134+1005 | 6 | −0.91 ± 0.20 | 7485 | 5500 | 4955–6098 | 1.24 ± 0.29 | 0.006 | 210 | 3.68 × 105 | Q1 |
IRAS 07430+1115 | 7 | −0.31 ± 0.15 | 5519 | 20 | 14–30 | 1.71 ± 0.30 | 0.020 | 230 | 1.39 × 104 | Q2 |
IRAS 08143-4406 | 8 | −0.43 ± 0.11 | 7013 | 5400 | 3927–5452 | 1.66 ± 0.39 | 0.002 | 150 | 6.81 × 105 | Q1 |
IRAS 08281-4850 | 9 | −0.26 ± 0.11 | 7462 | 7900 | 5567–16692 | 2.34 ± 0.24 | 0.007 | 280 | 1.94 × 105 | Q2 |
IRAS 12360-5740 | 10 | −0.40 ± 0.15 | 7273 | 6300 | 5178–7940 | 0.45 ± 0.20 | 0.0035 | 180 | 4.81 × 105 | Q1 |
IRAS 13245-5036 | 11 | −0.30 ± 0.10 | 9037 | 7100 | 7106–16800 | 1.11 ± 0.30 | 0.004 | 220 | 3.89 × 105 | Q2 |
IRAS 14325-6428 | 12 | −0.56 ± 0.10 | 7256 | 7035 | 3758–6988 | 2.27 ± 0.40 | 0.007 | 190 | 5.22 × 105 | Q2 |
IRAS 14429-4539 | 13 | −0.18 ± 0.11 | 9579 | 9000 | 1591–14624 | 1.29 ± 0.26 | 0.0085 | 360 | 1.20 × 105 | Q2 |
IRAS 19500+1709 | 14 | −0.59 ± 0.10 | 8239 | 7100 | 6194–8138 | 1.02 ± 0.17 | 0.0052 | 220 | 3.73 × 105 | Q1 |
IRAS 20000+3239 | 15 | −1.40 ± 0.20 | 5478 | 20200 | 9332–25218 | − | 0.010 | 220 | 5.32 × 105 | Q2 |
IRAS 22223+4327 | 16 | −0.30 ± 0.11 | 6008 | 2200 | 1956–2499 | 1.04 ± 0.22 | 0.006 | 150 | 4.93 × 105 | Q2 |
IRAS 22272+5435 | 17 | −0.77 ± 0.12 | 5325 | 6000 | 5234–6108 | 1.46 ± 0.26 | 0.0087 | 250 | 1.90 × 105 | Q1 |
IRAS 23304+6147 | 18 | −0.81 ± 0.20 | 6276 | 6400 | 6381–9386 | 2.8 ± 0.2 | 0.0085 | 200 | 4.22 × 105 | Q2 |
J052220.98 | LMC | −0.50 | 5750 | 4500 | – | 0.015 | 220 | – | 2.63 × 105 | |
J053250.69 | LMC | −1.10 | 6000 | 5200 | – | 0.006 | 250 | – | 2.06 × 105 | |
J004114.10 | SMC | −1.04 | 5750 | 5800 | – | 0.007 | 280 | – | 1.65 × 105 | |
J050632.10 | LMC | −0.40 | 7600 | 6000 | – | 0.003 | 240 | – | 2.74 × 105 | |
J003643.94 | SMC | −0.63 | 7500 | 6500 | – | 0.002 | 250 | – | 2.56 × 105 | |
J051848.84 | LMC | −1.00 | 6000 | 6700 | – | 0.008 | 240 | – | 2.62 × 105 | |
J004441.03 | SMC | −1.07 | 6000 | 8500 | – | 0.002 | 320 | – | 6.64 × 104 | |
J005803.08 | SMC | −1.03 | 6500 | 12 000 | – | 0.025 | 280 | – | 1.20 × 105 |
Notes. The columns are defined as follows (from left to right): Col. 1: Object name; 2: Source ID (from K22); (3)-(4): Metallicity and effective temperatures as listed in K22 (see their Table 1); (5): Luminosity derived in the present study (see Sect. 2); (6): Luminosity from K22 (see their Table 1), obtained considering the upper and lower limits of the distances retrieved from Bailer-Jones et al. (2021); (7): C/O from K22 (see their Table 3); (8)–(10): 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; (11): The quality flag (Q1 or Q2), based on the Gaia EDR3 RUWE parameter from K22. The last eight rows are the carbon stars in the sample of T22.
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