Table 2
Elemental abundances for individual lines in the solar spectrum.
| Line | FEROS | MIKE 1 | MIKE 2 | MIKE 3 | MIKE 4 | ⟨MIKE⟩ | σ⟨MIKE⟩ | Solar abundance |
| R = 48 000 | R = 65 000 | R = 65 000 | R = 65 000 | R = 42 000 | from Asplund et al. (2009) | |||
|
|
||||||||
| Sr 4607 | 2.92 | 2.76 | 2.62 | 2.78 | 2.61 | 2.69 | 0.09 | 2.87 ± 0.07 |
|
|
||||||||
| Zr 4208 | 2.39 | 2.42 | 2.44 | 2.42 | 2.35 | 2.44 | 0.06 | 2.58 ± 0.04 |
| Zr 4687 | 2.43 | 2.55 | 2.48 | 2.52 | 2.43 | 2.50 | 0.05 | |
| Zr 4739 | 2.39 | 2.57 | 2.47 | 2.57 | 2.46 | 2.52 | 0.06 | |
| Zr 5112 | 2.57 | 2.54 | 2.48 | 2.51 | 2.45 | 2.50 | 0.04 | |
|
|
||||||||
| La 4662 | 1.31 | 1.21 | 1.29 | 1.36 | 1.38 | 1.31 | 0.08 | 1.10 ± 0.04 |
| La 4748 | 1.22 | 1.28 | 1.38 | 1.22 | 1.19 | 1.27 | 0.08 | |
| La 5122 | 1.10 | 1.11 | 1.18 | 1.14 | 1.21 | 1.16 | 0.05 | |
| La 6390 | 1.10 | 1.23 | 1.23 | 1.12 | 1.15 | 1.18 | 0.06 | |
|
|
||||||||
| Ce 4523 | 1.55 | 1.65 | 1.70 | 1.70 | 1.62 | 1.67 | 0.07 | 1.58 ± 0.04 |
| Ce 4572 | 1.72 | 1.70 | 1.68 | 1.80 | 1.65 | 1.71 | 0.07 | |
| Ce 4628 | 1.70 | 1.66 | 1.72 | 1.72 | 1.60 | 1.68 | 0.06 | |
| Ce 5187 | 1.48 | 1.45 | 1.45 | 1.36 | 1.38 | 1.41 | 0.05 | |
|
|
||||||||
| Nd 4177 | 1.33 | 1.45 | 1.49 | 1.45 | 1.41 | 1.45 | 0.03 | 1.42 ± 0.04 |
| Nd 4358 | 1.62 | 1.76 | 1.64 | 1.66 | 1.62 | 1.67 | 0.06 | |
| Nd 4446 | 1.30 | 1.38 | 1.43 | 1.38 | 1.36 | 1.39 | 0.03 | |
| Nd 5130 | 1.44 | 1.61 | 1.61 | 1.57 | 1.49 | 1.57 | 0.06 | |
| Nd 5319 | 1.28 | 1.25 | 1.25 | 1.31 | 1.33 | 1.29 | 0.04 | |
|
|
||||||||
| Sm 4467 | 0.83 | 0.85 | 0.93 | 0.92 | 0.84 | 0.89 | 0.05 | 0.96 ± 0.04 |
| Sm 4523 | 0.84 | 0.93 | 1.00 | 1.00 | 0.99 | 0.98 | 0.04 | |
| Sm 4577 | 0.91 | 1.04 | 1.00 | 0.93 | 0.95 | 0.98 | 0.05 | |
| Sm 4669 | 1.25 | 1.25 | 1.22 | 1.33 | 1.40 | 1.30 | 0.08 | |
|
|
||||||||
| Eu 4129 | 0.34 | 0.34 | 0.48 | 0.41 | 0.33 | 0.39 | 0.07 | 0.52 ± 0.04 |
Notes. Columns 2−6 list the single abundances for the different instruments and resolutions. Columns 7 and 8 show the median abundance values for MIKE spectra for the different observation runs and the one σ dispersion, respectively. The mean abundances are used as solar abundance for MIKE spectra observed in the run with R = 55 000 (see Table 1 in Bensby et al. 2014) since no solar spectra is available in this setting. Col. 9 lists the solar abundances values from Asplund et al. (2009).
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