Table 2: Transitions and log gf of Mult. 6: LW = Lambert & Warner (1968); W = Wiese et al. (1969); Fr = François (1987); BQZ = Biemont et al. (1993); C = Chen et al. (2002, 2003).
Transition $\lambda$ LW W Fr BQZ C

(nm)

4p-4d ⁵P₃-⁵D $^\circ$ ₃ 869.3931 -0.56 -0.51 -0.74 -0.85 -0.52

⁵P₃-⁵D $^\circ$ ₄ 869.4626 0.03 0.08 -0.21 -0.26 0.05

**Table 2:** Transitions and log gf of Mult. 6: LW = Lambert & Warner (1968); W = Wiese et al. (1969); Fr = François (1987); BQZ = Biemont et al. (1993); C = Chen et al. (2002, 2003).
	Transition	$\lambda$	LW	W	Fr	BQZ	C
		(nm)
4p-4d	⁵P₃-⁵D $^\circ$ ₃	869.3931	-0.56	-0.51	-0.74	-0.85	-0.52
	⁵P₃-⁵D $^\circ$ ₄	869.4626	0.03	0.08	-0.21	-0.26	0.05

Source LaTeX | All tables | In the text

	1 Introduction
	2 Observational data
	3 Atmospheric parameters
	4 The S I spectrum
	5 Analysis
	6 Errors and sensitivity of abundances to stellar parameters
	7 Sulphur abundances
	8 Results
	9 Discussion
	10 Conclusions
	References
	Online Material
	Appendix A: Remarks on individual stars