Table A.1
Fe i and Fe ii lines used in the analysis.
| Fe i , λ | [Fe/H] | Wλ( ⊙ ) | Wλ (Twin) | Fe ii , λ | [Fe/H] | Wλ( ⊙ ) | Wλ (Twin) |
| 5166.281 | 0.02 | 135.4 | 136.0 | 5197.577 | 0.02 | 82.9 | 84.0 |
| 5198.711 | 0.02 | 101.3 | 102.5 | 5234.625 | 0.03 | 85.9 | 87.4 |
| 5216.274 | 0.03 | 123.4* | 125.8* | 5264.812 | 0.04 | 47.3 | 50.0 |
| 5217.389 | 0.04 | 117.5 | 120.8 | 5284.109 | 0.01 | 63.4 | 63.9 |
| 5225.535 | 0.02 | 75.3* | 76.1* | 5325.553 | 0.00 | 42.1 | 42.1 |
| 5242.491 | 0.05 | 86.4 | 88.8 | 5414.073 | 0.04 | 30.2 | 31.7 |
| 5247.049 | 0.05 | 65.6 | 67.6 | 5425.257 | 0.02 | 45.5 | 46.4 |
| 5250.208 | 0.03 | 69.8 | 71.0 | 6247.557 | 0.03 | 53.6 | 55.0 |
| 5295.299 | 0.01 | 29.7* | 30.2* | 6456.383 | 0.03 | 61.4 | 62.8 |
| 5367.466 | 0.00 | 153.1 | 155.7 | ||||
| 5379.574 | 0.02 | 61.3 | 62.2 | ||||
| 5522.446 | 0.04 | 43.8* | 45.7* | ||||
| 5638.262 | –0.01 | 77.7 | 77.2 | ||||
| 5662.516 | 0.03 | 92.6 | 94.4 | ||||
| 5679.023 | 0.01 | 59.5 | 60.1 | ||||
| 5701.514 | 0.02 | 84.2 | 85.1 | ||||
| 6065.482 | 0.02 | 121.6 | 121.7 | ||||
| 6151.617 | 0.01 | 49.6 | 50.1 | ||||
| 6200.313 | 0.01 | 72.7 | 73.7 | ||||
| 6213.429 | 0.04 | 80.1 | 82.0 | ||||
| 6229.225 | 0.02 | 37.1 | 38.1 | ||||
| 6252.554 | 0.04 | 120.1 | 123.8 | ||||
| 6421.349 | 0.02 | 119.0 | 120.1 | ||||
| 6498.937 | 0.01 | 48.2 | 48.6 |
Notes. To minimize the influence of blends, the equivalent width, Wλ, is based on the best synthetic fit ignoring obvious blends in the observed data. Where strong blends were present in the outermost parts of the wings, and an integration over the full line was impossible, a tighter integration limit was chosen, consistently for the spectrum of M67-1194 and the Sun. For a few lines with strong blends in one wing, a symmetric line was assumed and Wλ integrated over the range: line core – (left or right) wing and doubled. These latter lines are marked in the table with an asterisk (*).
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