Sulphur abundances in halo giants from the [S ı] line at 1082 nm and the S ı triplet around 1045 nm

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Table 6

Adopted stellar parameters for the observed stars.

Star	T_eff	log g	[Fe/H]	ξ_micro	Refs.	ξ_macro^b
	(K)	(cgs)		(km s^-1)		(km s^-1)

HD 13979	5075 ± 100	1.90 ± 0.5	−2.26 ± 0.09	1.30 ± 0.5	1	7.0
HD 21581	4900 ± 103	2.24 ± 0.2	−1.64 ± 0.09	1.45^a	2	4.8
HD 23798	4375 ± 82	1.12 ± 0.2	−2.03 ± 0.13	2.20^a	2	7.3
HD 26297	4350 ± 138	1.46 ± 0.2	−1.51 ± 0.11	1.65^a	2	5.4
HD 29574	4200 ± 119	0.78 ± 0.2	−1.70 ± 0.12	2.00^a	2	6.0
HD 36702	4366 ± 100	0.95 ± 0.2	−2.06 ± 0.11	1.65 ± 0.15	3	6.0
HD 44007	4975 ± 103	2.24 ± 0.2	−1.65 ± 0.23	2.20^a	2	4.5
HD 83212	4533 ± 100	1.45 ± 0.2	−1.40 ± 0.13	1.80 ± 0.15	3	6.0
HD 85773	4450 ± 100	1.10 ± 0.5	−2.36 ± 0.09	2.10 ± 0.5	1	6.5
HD 103545	4725 ± 100	1.70 ± 0.5	−2.14 ± 0.09	1.30 ± 0.5	1	5.5

References. (1) Burris et al. (2000); (2) Fulbright & Johnson (2003); (3) Gratton et al. (2000).

Notes.

The reference does not clearly state the uncertainty, so we assume a generic uncertainty of ± 0.5 km s^-1. The size of this uncertainty does not affect the derived sulphur abundance much, see Table 7, because the sulphur lines used in this work are weak and do not depend much on microturbulence.

The macroturbulence is not taken from the references, but determined by us to fit the synthetic spectra to the observed spectra in Fig. 5.

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