**Table 2:** Stars from the literature that show a large discrepancy between the two sulphur diagnostics.
Star	Spectral	V	$T_{{\rm eff}}$	$\log~g$	[Fe/H]	$\xi_{\rm micro}$	$\xi_{\rm macro}$	$\log~\varepsilon{\rm (S)}^{b}$
	type^a	[mag]	[K]	(cgs)		[km s^-1]	[km s^-1]	$\lambda\lambda~9212{-}38$	$\lambda\lambda~8694{-}95$
					$\pm$ 0.15	$\pm$ 0.5	$\pm$ 0.5	$\pm$ 0.15	${\pm}{\sim}$ 0.15
Giants
HD 2665	G5III	7.8	$4990\pm 70$	$2.50\pm 0.20$	-1.74¹/-2.00²	1.5	5.5	5.60¹	5.89²
HD 216143	G5	7.8	$4540\pm 100$	$1.78\pm0.15$	-2.15⁴	2.1	-	5.48⁴	5.72⁴
Dwarfs and subgiants
HD 19445	sdG5	8.0	$5810\pm 150$	$4.46\pm0.20$	-1.90¹/-1.88²	1.5	4.5	5.50¹	5.97²
HD 84937	sdF5	8.3	$6300\pm 100$	$3.97\pm0.15$	-2.06¹/-2.11³	1.1	5.0	5.27¹	5.70³
HD 140283	sdF3	7.2	$5830\pm 100$	$3.67\pm0.15$	-2.55⁴	1.9	-	5.18⁴	5.53⁴

¹ Ryde & Lambert (2004) using $T_{{\rm eff}}$ , log g and $\xi$ from (2) and (3).
² Israelian & Rebolo (2001).
³ Takada-Hidai et al. (2002).
⁴ Takada-Hidai et al. (2005).

^a From Simbad (http://simbad.u-strasbg.fr).
^b $\log \varepsilon {\rm (S)}\equiv\log n_{\rm S}/n_{\rm H} + 12$ ; $\log$ $\varepsilon$ (S) $_\odot$ = 7.20 (Chen et al. 2002).

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