Table 2
Abundance corrections for the Fe spectral lines in the visible range, for the different magnetic flux cases.
| λ | Δlog ϵ(Fe)⊙ | Δlog ϵ(Fe)⊙ | Δlog ϵ(Fe)⊙ | W HD | ID |
| [nm] | [dex] | [dex] | [dex] | [pm] | |
| (50 G – HD) | (100 G – HD) | (200 G – HD) | |||
|
|
|||||
| 410.091 | +0.01 | +0.03 | +0.04 | 0.55 | 0L |
| 415.025 | +0.02 | +0.04 | +0.06 | 7.94 | 0L |
| 423.027 | +0.01 | +0.01 | +0.02 | 0.69 | 0L |
| 430.603 | +0.01 | +0.02 | +0.03 | 1.98 | 0L |
| 437.113 | +0.01 | +0.01 | +0.02 | 0.10 | 0L |
| 486.364 | +0.02 | +0.05 | +0.09 | 6.60 | 0L |
| 524.705 | +0.04 | +0.09 | +0.14 | 6.74 | A |
| 525.021 | +0.04 | +0.08 | +0.12 | 6.72 | A |
| 525.065 | +0.03 | +0.06 | +0.08 | 9.56 | LL |
| 543.452 | +0.04 | +0.07 | +0.10 | 24.72 | 0L |
| 557.609 | +0.02 | +0.05 | +0.07 | 10.91 | 0L |
| 579.119 | +0.01 | +0.02 | +0.03 | 0.37 | 0L |
| 585.923 | +0.01 | +0.02 | +0.03 | 0.18 | 0L |
| 594.036 | +0.01 | +0.02 | +0.03 | 0.25 | 0L |
| 601.392 | +0.01 | +0.02 | +0.03 | 0.28 | 0L |
| 608.271 | +0.02 | +0.05 | +0.08 | 3.84 | A |
| 611.332 | 0.00 | +0.01 | +0.03 | 0.92 | II |
| 616.946 | +0.01 | +0.03 | +0.05 | 0.16 | 0L |
| 617.334 | +0.03 | +0.07 | +0.11 | 6.98 | A |
| 624.065 | +0.03 | +0.06 | +0.10 | 4.76 | A |
| 630.150 | +0.02 | +0.04 | +0.05 | 11.75 | LL |
| 630.249 | +0.02 | +0.04 | +0.06 | 9.55 | LL |
| 633.084 | +0.01 | +0.02 | +0.04 | 1.37 | LL |
|
|
|||||
| ⟨ ⟩ | 0.019 | 0.040 | 0.061 | ||
| ±0.011 | ±0.023 | ±0.034 | |||
|
|
|||||
| ⟨ ⟩* | 0.032 | 0.070 | 0.110 | ||
| ±0.008 | ±0.014 | ±0.020 | |||
Notes. Columns in the top part list the rest wavelength of the absorption lines and their abundance corrections for the three magnetic flux cases, the equivalent width obtained from the spectral synthesis based on our HD series, and the identifiers associated with each spectral line, following the convention introduced in Table 1. In the bottom part, ⟨ ⟩ indicates the unweighted mean of the abundance corrections for the visible lines and corresponding rms for the different magnetic flux cases, and ⟨ ⟩
refers to the values obtained when averaging for just the 5 lines in common with Asplund et al. (2000b).
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