Table 3.
Characteristics of the spectral lines inverted in this study to obtain the atmospheric parameters of the solar atmosphere where these lines are formed (Borrero et al. 2013; Bloomfield et al. 2007).
| Element | Ion | λ (Å) | Exc. pot. (eV) | log(gf) | Term | α |
 ) |
|---|---|---|---|---|---|---|---|
| Fe | I | 15648.515 | 5.426 | −0.669 |
 |
0.229 | 975 |
| Fe | I | 15662.018 | 5.830 | −0.190 |
 |
0.240 | 1197 |
Notes. The first and second columns are the atomic element and the ionisation state of the atom in the inverted spectral lines. The third column corresponds to the air wavelength of the transition in angstroms, the next column is the excitation potential of the lower level, the fifth column is the oscillation strength, and the lower and upper levels are listed in the sixth column. The seventh and eighth columns are the Barklem velocity exponential and Barklem cross-section (in units of the Bohr radius squared), respectively. The last two values were calculated following the ABO theory (Barklem 1998; Anstee & O’Mara 1995) and can be obtained from the tabulated tables in Anstee & O’Mara (1995).
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