Table 3
Abundance results of IRAS 05113+1347, IRAS 05341+0852, IRAS 07430+1115, and IRAS 22272+5435.
IRAS 05113 | IRAS 05341 | IRAS 07430 | IRAS 22272 | ||||||||||||||||||
[Fe/H] =−0.49 | [Fe/H] =−0.54 | [Fe/H] =−0.31 | [Fe/H] =−0.77 | ||||||||||||||||||
Teff = 5500 K | Teff = 6750 K | Teff = 6000 K | Teff = 5750 K | ||||||||||||||||||
log g = 0.5 dex | log g = 1.25 dex | log g = 1.00 dex | log g = 0.5 dex | ||||||||||||||||||
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Ion | log ϵ⊙ | N | log ϵ | σ l2l | [X/Fe] | σ tot | N | log ϵ | σ l2l | [X/Fe] | σ tot | N | log ϵ | σ l2l | [X/Fe] | σ tot | N | log ϵ | σ l2l | [X/Fe] | σ tot |
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C I | 8.43 | 6 | 8.87 | 0.11 | 0.65 | 0.16 | 16 | 8.73 | 0.10 | 1.03 | 0.10 | 6 | 8.87 | 0.06 | 0.79 | 0.13 | 14 | 8.71 | 0.07 | 1.05 | 0.12 |
O I | 8.69 | 1 | 8.49 | 0.20 | 0.01 | 0.27 | 2 | 8.71 | 0.07 | 0.75 | 0.11 | 2 | 8.64 | 0.20 | 0.30 | 0.22 | 2 | 8.55 | 0.02 | 0.63 | 0.09 |
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Na I | 6.24 | 2 | 5.88 | 0.01 | 0.17 | 0.12 | 1 | 6.00 | 0.20 | 0.46 | 0.23 | 2 | 6.20 | 0.09 | 0.27 | 0.12 | 2 | 5.90 | 0.00 | 0.42 | 0.09 |
Mg I | 7.60 | 1 | 7.20 | 0.20 | 0.13 | 0.24 | 1 | 6.88 | 0.20 | –0.02 | 0.24 | 2 | 7.26 | 0.01 | –0.03 | 0.11 | 3 | 6.75 | 0.20 | –0.08 | 0.17 |
Al I | 6.45 | 2 | 6.37 | 0.13 | 0.24 | 0.15 | 1 | 6.07 | 0.20 | 0.39 | 0.23 | ||||||||||
Si I | 7.51 | 4 | 7.23 | 0.06 | –0.07 | 0.20 | 5 | 7.04 | 0.10 | 0.26 | 0.18 | 5 | 7.52 | 0.13 | 0.36 | 0.19 | 4 | 7.06 | 0.05 | 0.32 | 0.16 |
S I | 7.12 | 1 | 6.97 | 0.20 | 0.06 | 0.25 | 3 | 6.65 | 0.09 | 0.25 | 0.15 | 2 | 6.69 | 0.02 | –0.08 | 0.13 | 2 | 6.64 | 0.02 | 0.28 | 0.11 |
Ca I | 6.34 | 3 | 5.66 | 0.03 | –0.14 | 0.10 | 7 | 5.83 | 0.05 | 0.20 | 0.08 | 7 | 6.03 | 0.09 | –0.0 | 0.08 | 8 | 5.81 | 0.10 | 0.24 | 0.08 |
Ca II | 6.34 | 3 | 5.97 | 0.09 | 0.36 | 0.12 | 1 | 5.79 | 0.20 | 0.22 | 0.24 | ||||||||||
Sc II | 3.15 | 6 | 2.87 | 0.09 | –0.08 | 0.13 | 6 | 2.72 | 0.09 | 0.30 | 0.09 | 4 | 3.00 | 0.06 | 0.20 | 0.10 | 3 | 2.75 | 0.20 | 0.37 | 0.18 |
Ti I | 4.95 | 4 | 4.47 | 0.09 | 0.05 | 0.13 | 5 | 4.90 | 0.11 | 0.27 | 0.11 | 2 | 4.50 | 0.05 | 0.32 | 0.10 | |||||
Ti II | 4.95 | 3 | 4.41 | 0.05 | –0.34 | 0.12 | 2 | 4.50 | 0.20 | 0.28 | 0.19 | 9 | 4.86 | 0.09 | 0.26 | 0.09 | 2 | 4.47 | 0.03 | 0.29 | 0.11 |
V I | 3.93 | 3 | 3.71 | 0.11 | 0.32 | 0.15 | 1 | 4.00 | 0.20 | 0.38 | 0.24 | ||||||||||
V II | 3.93 | 2 | 3.99 | 0.03 | 0.41 | 0.13 | 2 | 3.21 | 0.03 | 0.05 | 0.11 | ||||||||||
Cr I | 5.64 | 4 | 5.02 | 0.03 | –0.09 | 0.10 | 2 | 4.99 | 0.06 | 0.05 | 0.12 | 2 | 5.20 | 0.02 | –0.13 | 0.09 | 4 | 4.91 | 0.06 | 0.03 | 0.08 |
Cr II | 5.64 | 10 | 5.03 | 0.06 | 0.12 | 0.07 | 6 | 5.16 | 0.07 | –0.13 | 0.08 | 9 | 4.94 | 0.06 | 0.06 | 0.07 | |||||
Mn I | 5.43 | 1 | 4.60 | 0.20 | –0.3 | 0.24 | 2 | 4.96 | 0.06 | –0.15 | 0.11 | 1 | 4.58 | 0.20 | –0.08 | 0.22 | |||||
Mn II | 5.43 | 1 | 5.40 | 0.20 | 0.70 | 0.22 | 1 | 4.60 | 0.20 | –0.06 | 0.22 | ||||||||||
Fe I | 7.50 | 21 | 6.96 | 0.11 | 0.00 | 0.08 | 47 | 6.80 | 0.10 | 0.00 | 0.06 | 43 | 7.19 | 0.08 | 0.00 | 0.05 | 35 | 6.73 | 0.07 | 0.00 | 0.05 |
Fe II | 7.50 | 10 | 7.29 | 0.13 | 0.00 | 0.11 | 20 | 6.77 | 0.07 | 0.00 | 0.05 | 17 | 7.15 | 0.08 | 0.00 | 0.06 | 24 | 6.73 | 0.08 | 0.00 | 0.05 |
Co I | 4.99 | 2 | 4.59 | 0.01 | 0.13 | 0.13 | |||||||||||||||
Ni I | 6.22 | 5 | 5.78 | 0.10 | 0.10 | 0.11 | 6 | 5.81 | 0.06 | 0.29 | 0.08 | 11 | 5.89 | 0.12 | –0.01 | 0.09 | 8 | 5.66 | 0.07 | 0.21 | 0.07 |
Cu I | 4.19 | 1 | 3.94 | 0.20 | 0.28 | 0.24 | 1 | 4.25 | 0.20 | 0.76 | 0.23 | 2 | 3.92 | 0.07 | 0.05 | 0.12 | 1 | 3.80 | 0.20 | 0.37 | 0.22 |
Zn I | 4.56 | 1 | 4.15 | 0.20 | –0.2 | 0.32 | 1 | 4.46 | 0.20 | 0.25 | 0.28 | 1 | 4.06 | 0.20 | 0.27 | 0.29 | |||||
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Y II | 2.21 | 2 | 3.30 | 0.20 | 1.29 | 0.22 | 4 | 3.47 | 0.10 | 1.98 | 0.12 | 1 | 3.25 | 0.20 | 1.39 | 0.24 | 4 | 3.14 | 0.08 | 1.69 | 0.12 |
Zr II | 2.58 | 3 | 3.73 | 0.11 | 1.36 | 0.15 | 2 | 3.61 | 0.06 | 1.76 | 0.10 | 2 | 3.45 | 0.12 | 1.22 | 0.15 | 3 | 3.35 | 0.08 | 1.54 | 0.11 |
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La II | 1.10 | 6 | 2.69 | 0.16 | 1.80 | 0.16 | 8 | 2.82 | 0.08 | 2.45 | 0.11 | 11 | 2.50 | 0.12 | 1.75 | 0.12 | 6 | 2.65 | 0.20 | 2.32 | 0.15 |
Ce II | 1.58 | 4 | 3.18 | 0.10 | 1.80 | 0.14 | 5 | 3.12 | 0.06 | 2.27 | 0.10 | 5 | 2.71 | 0.09 | 1.47 | 0.11 | 4 | 2.66 | 0.06 | 1.84 | 0.11 |
Pr II | 0.72 | 6 | 2.20 | 0.14 | 1.68 | 0.16 | 7 | 2.27 | 0.09 | 2.28 | 0.14 | 11 | 1.94 | 0.13 | 1.57 | 0.14 | 13 | 1.81 | 0.07 | 1.86 | 0.13 |
Nd II | 1.42 | 8 | 2.88 | 0.05 | 1.66 | 0.13 | 23 | 3.18 | 0.11 | 2.49 | 0.13 | 17 | 2.64 | 0.08 | 1.57 | 0.12 | 7 | 2.61 | 0.05 | 1.96 | 0.13 |
Sm II | 0.96 | 3 | 2.10 | 0.09 | 1.34 | 0.16 | 2 | 1.99 | 0.12 | 1.76 | 0.16 | 4 | 2.05 | 0.13 | 1.43 | 0.15 | 3 | 1.67 | 0.09 | 1.47 | 0.14 |
Eu II | 0.52 | 2 | 1.21 | 0.10 | 0.90 | 0.16 | 2 | 1.25 | 0.09 | 1.46 | 0.14 | 2 | 0.98 | 0.07 | 0.81 | 0.13 | 2 | 0.89 | 0.06 | 1.14 | 0.12 |
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Gd II | 1.07 | 3 | 2.29 | 0.09 | 1.43 | 0.16 | 2 | 2.17 | 0.08 | 1.82 | 0.12 | 3 | 2.00 | 0.07 | 1.28 | 0.13 | 13 | 1.99 | 0.12 | 1.69 | 0.16 |
Tb II | 0.30 | 1 | 1.70 | 0.20 | 1.75 | 0.27 | |||||||||||||||
Dy II | 1.10 | 2 | 2.34 | 0.01 | 1.44 | 0.14 | 2 | 2.25 | 0.20 | 1.88 | 0.20 | 2 | 2.18 | 0.00 | 1.43 | 0.13 | 8 | 2.13 | 0.09 | 1.80 | 0.11 |
Er II | 0.92 | 4 | 2.15 | 0.07 | 1.43 | 0.14 | 2 | 2.23 | 0.05 | 2.04 | 0.12 | 3 | 1.74 | 0.04 | 1.58 | 0.10 | |||||
Yb II | 0.84 | 1 | 2.50 | 0.20 | 2.39 | 0.24 | 1 | 2.00 | 0.20 | 1.93 | 0.24 | ||||||||||
Lu II | 0.10 | 2 | 1.34 | 0.20 | 1.45 | 0.23 | 2 | 1.74 | 0.01 | 2.36 | 0.12 | 1 | 0.85 | 0.20 | 1.10 | 0.25 | 2 | 1.25 | 0.20 | 1.92 | 0.21 |
Hf II | 0.85 | 2 | 2.19 | 0.09 | 1.55 | 0.16 | 1 | 2.15 | 0.20 | 2.02 | 0.23 | 2 | 1.85 | 0.20 | 1.77 | 0.19 | |||||
W II | 0.85 | 1 | 3.07 | 0.20 | 2.95 | 0.25 | 1 | 2.30 | 0.20 | 2.21 | 0.25 |
Notes. For each ion, the table lists the used number of lines (N) for the abundance determination, the determined abundance (log ϵ), the uncertainty on this abundance due to line-to-line scatter (σl2l), the element over iron ratio ([X/Fe]) and the total uncertainty on [X/Fe] (σtot) which includes line-to-line scatter and atmospheric parameter uncertainty (see text for details). The solar abundances (log ϵ⊙) in the second column are retrieved from Asplund et al. (2009). For all elemental abundances determined via only one spectral line or via spectrum synthesis, we adopt a line-to-line scatter of 0.20 dex.
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