Table 4.
Typical internal uncertainties (sulfur abundance scatters, in dex) for different stellar types and S/N bins.
| Cool giant | Cool dwarf | Hot dwarf | ||||
|---|---|---|---|---|---|---|
| S/N | ∼40 | ∼200 | ∼40 | ∼100 | ∼80 | ∼140 |
| SI 674.3 | – | – | 0.06 | 0.06 | 0.05 | 0.02 |
| SI 674.8 | – | – | 0.04 | 0.03 | 0.02 | 0.02 |
| SI 675.7 | 0.03 | 0.03 | 0.06 | 0.04 | 0.02 | 0.02 |
Notes. These numbers refer to a single line in one spectrum. Since the final reported abundances are obtained by averaging up to three SI lines and several repeat spectra (when available), the actual relative uncertainties from star to star are much smaller. Only the SI 675.7 nm line can be safely analysed in cool giants.
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