Table 1.
Lines used to derived stellar abundances.
| Species | Line | Line mask [Å] |
Segment mask [Å] |
log gf | ||
|---|---|---|---|---|---|---|
| centre [Å] | Start | End | Start | End | ||
| Mg I | 4702.9909 | 4702.00 | 4704.00 | 4680 | 4720 | −0.44 |
| Ti II | 4563.7574 | 4562.75 | 4564.75 | 4540 | 4580 | −0.69 |
| Ti II | 4571.9713 | 4570.97 | 4572.97 | 4550 | 4590 | −0.31 |
| Fe II | 4583.8292 | 4582.70 | 4584.70 | 4560 | 4600 | −1.86 |
| Ba II | 4554.0290 | 4553.00 | 4555.00 | 4535 | 4575 | 0.17 |
Notes. Only Mg4702, Ti4563 and Fe4583 were used for fitting the trend models. All wavelengths are given in Å. The line mask describes the wavelength interval used in the fitting of abundances, and the segment mask describes the entire wavelength region modelled around a line, as described in Sect. 4.4.1.
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