Table 1
Summary of iron abundances derived from Fe i & Fe ii using different input parameters.
| Analysis run | [Fe i/H] | σ | [Fe ii/H] | σ | δFe | σ |
| (dex) | (dex) | (dex) | (dex) | (dex) | (dex) | |
|
|
||||||
| AGB L16 | −1.80 | 0.05 | −1.58 | 0.02 | −0.22 | 0.05 |
|
|
||||||
| RGB (C13 Teff) | −1.48 | 0.06 | −1.47 | 0.06 | −0.01 | 0.08 |
| AGB (C13 Teff) | −1.63 | 0.04 | −1.48 | 0.04 | −0.15 | 0.05 |
|
|
||||||
| RGB (L16 gfs) | −1.43 | 0.05 | −1.52 | 0.05 | + 0.09 | 0.07 |
| AGB (L16 gfs) | −1.52 | 0.06 | −1.53 | 0.04 | + 0.01 | 0.08 |
|
|
||||||
| RGB (Final) | −1.43 | 0.05 | −1.47 | 0.06 | + 0.04 | 0.07 |
| AGB (Final) | −1.52 | 0.06 | −1.48 | 0.04 | −0.04 | 0.07 |
Notes. Abundances are scaled based on a solar Fe abundance of log ϵ = 7.50 dex. Also shown is the difference δFe = Fe i−Fe ii. The first line shows the L16 AGB results. The second set of results were obtained using the C13 temperatures (Sect. 3). The 3rd set of results were obtained using our new IRFM Teff scale but adopting the L16log gf values. Our final results, using the IRFM temperatures and our log gf values, are in the last two rows. The typical number of Fe i lines analysed was 20–40, and 2–3 for Fe ii. The σ values are the 1σ star-to-star scatter only.
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