Table 3
Abundance results of J004441.04 together with the calcuted errors due to line to line scatter and uncertainties of the chosen atmosphere model.
| Species | N | log ϵ ± σϵ | log ϵ⊙ ± σϵ⊙ | [X/Fe] ± σtot | σ[X/Fe] | σTeff | σlog g | σξt | |||
| +250 K | –250 K | +0.5 dex | +0.5 km s-1 | –0.5 km s-1 | |||||||
|
|
|||||||||||
| C I | 6 | 8.76 ± 0.10 | 8.43 ± 0.05 | 1.67 ± 0.36 | 0.14 | –0.23 | 0.24 | 0.11 | 0.02 | –0.02 | |
| O I | 3 | 8.49 ± 0.09 | 8.69 ± 0.05 | 1.14 ± 0.50 | 0.13 | –0.35 | 0.32 | 0.12 | 0.02 | –0.05 | |
| Na I | 2 | 5.85 ± 0.08 | 6.24 ± 0.04 | 0.95 ± 0.14 | 0.12 | –0.08 | 0.06 | –0.02 | 0.01 | –0.03 | |
| Mg I | 1 | 6.75 ± 0.20 | 7.60 ± 0.04 | 0.49 ± 0.26 | 0.22 | –0.11 | 0.05 | –0.05 | 0.02 | –0.04 | |
| Si I | 2 | 6.63 ± 0.01 | 7.51 ± 0.03 | 0.46 ± 0.16 | 0.09 | –0.11 | 0.07 | –0.05 | 0.02 | –0.04 | |
| S I | 2 | 6.07 ± 0.13 | 7.12 ± 0.03 | 0.29 ± 0.26 | 0.16 | –0.17 | 0.15 | 0.03 | 0.02 | –0.04 | |
| Ca I | 4 | 5.33 ± 0.03 | 6.34 ± 0.04 | 0.33 ± 0.06 | 0.09 | –0.03 | 0.03 | 0.01 | 0.00 | 0.00 | |
| Sc II | 3 | 2.18 ± 0.08 | 3.15 ± 0.04 | 0.35 ± 0.14 | 0.15 | 0.08 | –0.08 | 0.01 | –0.01 | 0.01 | |
| Ti II | 3 | 4.02 ± 0.21 | 4.95 ± 0.05 | 0.39 ± 0.16 | 0.25 | 0.06 | –0.05 | 0.01 | –0.02 | 0.01 | |
| Cr II | 3 | 4.26 ± 0.04 | 5.64 ± 0.04 | −0.06 ± 0.08 | 0.13 | –0.02 | 0.00 | –0.02 | 0.01 | –0.02 | |
| Mn I | 2 | 4.77 ± 0.11 | 5.43 ± 0.04 | 0.68 ± 0.14 | 0.14 | –0.07 | 0.01 | –0.05 | 0.01 | –0.04 | |
| Fe I | 17 | 6.16 ± 0.07 | 7.50 ± 0.04 | 0.00 ± 0.03 | 0.11 | 0.00 | 0.00 | 0.00 | 0.00 | 0.00 | |
| Fe II | 4 | 6.18 ± 0.11 | 7.50 ± 0.04 | 0.00 ± 0.08 | 0.17 | 0.00 | 0.00 | 0.00 | 0.00 | 0.00 | |
| Ni I | 4 | 5.09 ± 0.17 | 6.22 ± 0.04 | 0.21 ± 0.13 | 0.19 | –0.05 | 0.01 | –0.04 | 0.03 | –0.04 | |
| Zn I | 1 | 3.85 ± 0.20 | 4.56 ± 0.05 | 0.63 ± 0.23 | 0.22 | –0.06 | 0.00 | –0.04 | –0.01 | 0.00 | |
| Y II | 2 | 3.04 ± 0.03 | 2.21 ± 0.05 | 2.15 ± 0.42 | 0.13 | 0.26 | –0.08 | 0.20 | –0.13 | 0.19 | |
| Zr II | 2 | 3.23 ± 0.11 | 2.58 ± 0.04 | 1.97 ± 0.22 | 0.17 | 0.13 | –0.08 | 0.07 | –0.06 | 0.07 | |
| La II | 9 | 2.62 ± 0.13 | 1.10 ± 0.04 | 2.84 ± 0.32 | 0.18 | 0.23 | –0.14 | 0.09 | –0.08 | 0.10 | |
| Ce II | 8 | 2.79 ± 0.13 | 1.58 ± 0.04 | 2.53 ± 0.18 | 0.18 | 0.12 | –0.12 | –0.01 | –0.02 | 0.01 | |
| Pr II | 2 | 2.10 ± 0.01 | 0.72 ± 0.04 | 2.70 ± 0.32 | 0.12 | 0.23 | –0.18 | 0.02 | –0.06 | 0.06 | |
| Nd II | 7 | 2.84 ± 0.10 | 1.42 ± 0.04 | 2.74 ± 0.31 | 0.16 | 0.24 | –0.17 | 0.03 | –0.05 | 0.07 | |
| Sm II | 2 | 1.85 ± 0.04 | 0.96 ± 0.04 | 2.21 ± 0.30 | 0.13 | 0.22 | –0.16 | 0.05 | –0.05 | 0.07 | |
| Eu II | 1 | 1.13 ± 0.10 | 0.52 ± 0.04 | 1.93 ± 0.24 | 0.16 | 0.10 | –0.13 | –0.06 | –0.04 | 0.04 | |
| Gd II | 1 | 1.75 ± 0.10 | 1.07 ± 0.04 | 2.00 ± 0.20 | 0.16 | 0.05 | –0.10 | –0.04 | 0.00 | –0.02 | |
| Dy II | 1 | 2.05 ± 0.20 | 1.10 ± 0.04 | 2.27 ± 0.22 | 0.12 | 0.11 | –0.16 | –0.05 | –0.01 | –0.01 | |
| Er II | 1 | 1.90 ± 0.20 | 0.92 ± 0.05 | 2.30 ± 0.25 | 0.24 | 0.04 | –0.07 | –0.04 | 0.01 | –0.02 | |
| Yb II | 1 | 2.15 ± 0.20 | 0.84 ± 0.11 | 2.63 ± 0.63 | 0.26 | –0.02 | –0.01 | –0.04 | 0.57 | 0.00 | |
| Lu II | 1 | 1.30 ± 0.20 | 0.10 ± 0.09 | 2.52 ± 0.15 | 0.15 | 0.02 | –0.06 | –0.03 | –0.04 | 0.06 | |
| Hf II | 1 | 2.15 ± 0.20 | 0.85 ± 0.04 | 2.62 ± 0.13 | 0.12 | 0.03 | –0.08 | –0.03 | 0.00 | –0.01 | |
| W II | 1 | 2.25 ± 0.20 | 0.85 ± 0.12 | 2.72 ± 0.27 | 0.26 | 0.02 | –0.07 | –0.04 | –0.01 | –0.01 | |
Notes. N represents the number of lines used for the abundance determination of the species. Uncertainties in log ϵ and log ϵ⊙ due to line-to-line scatter are given by σϵ and σϵ⊙ respectively. σ[X/Fe] , σTeff, σlog g and σξt represent the sensitivity of [X/Fe] to uncertainties in the line-to-line scatter, effective temperature, surface gravity and microturbulent velocity respectively. σtot represents the total uncertainty of [X/Fe] due to the line-to-line scatter and model uncertainties. Solar abundances are retrieved from Asplund et al. (2009). Abundances of elements indicated with italicised text are determined via synthetic spectra fitting. For more information, see text.
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