Table 4
Typical abundance uncertainties in clusters and sensitivity.
| [X/H] | σ[X/H]clus | Δ T eff | Δ log g | Δ v micro | σ line |
| (±80 K) | (±0.02) | (±0.1 km s-1) | |||
|
|
|||||
| Mg | 0.07 | ±0.05 | ±0.01 | ∓0.01 | 0.04 |
| Ca | 0.09 | ±0.06 | ±0.03 | ∓0.01 | 0.03 |
| Si | 0.10 | ±0.03 | ±0.01 | ∓0.03 | 0.04 |
| Ti | 0.11 | ∓0.07 | ±0.01 | ∓0.02 | ... |
| S | 0.07 | ∓0.04 | ±0.01 | ∓0.01 | ... |
| Al | 0.15 | ±0.10 | ±0.02 | ±0.01 | ... |
| Ni | 0.11 | ±0.05 | ±0.00 | ∓0.01 | 0.03 |
| Mn | 0.09 | ±0.08 | ±0.00 | ∓0.02 | ... |
| K | 0.08 | ±0.10 | ±0.01 | ±0.01 | ... |
| Cr | 0.10 | ±0.11 | ±0.01 | ∓0.02 | ... |
| Na | 0.09 | ±0.07 | ±0.02 | ∓0.01 | ... |
| Co | 0.09 | ±0.05 | ±0.00 | ∓0.01 | ... |
| V | 0.10 | ±0.10 | ±0.00 | ∓0.01 | ... |
| Fe | 0.08 | ±0.07 | ±0.02 | ∓0.04 | 0.02 |
| C | ... | ±0.03 | ±0.03 | ∓0.03 | 0.04 |
| N | ... | ±0.06 | ±0.01 | ∓0.01 | 0.02 |
| O | ... | ±0.10 | ±0.03 | ∓0.04 | 0.04 |
Notes. The typical star-to-star dispersion in [X/H] within the eight validation clusters is displayed for every element in Col. 2. Typical sensitivity of the abundance to uncertainties in the stellar parameters are computed by measuring the difference in [X/H] abundance due to changes of ±80 K (Col. 3), ±0.02 dex (Col. 4), and 0.10 km s-1 (Col. 5), in Teff, log g and vmicro, respectively. This was done using three stars near the middle of the parameter space (i.e. Teff~ 4700 K, log g~ 2.5, [Fe/H] ~−0.2). The standard error, σline, of the mean abundance is displayed in Col. 6 for elements where there are more than two lines.
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