al. (1981).

NLTE Analyses
-------------

The NLTE abundances of S were computed for the two [S [i]{} ]{}lines following the same procedures as described in Takada-Hidai & Takeda (1996). The grids of NLTE corrections were constructed for the parameter ranges of [$T_{\rm eff}$ ]{}$=4500$ – $6500$ K, [log $g$ ]{}$ = 1.0$ – $5.0$, and \[Fe/H\]$ = 0.0$ – $-3.0$, assuming a constant microturbulence of 2.0 [${\rm km \: s^{-1}}$]{}  and changing enhancement of S abundances. The grids for [S [i]{} ]{}8693.9 and [S [i]{} ]{}8694.6 lines are presented in Tables A1 and A2 in the Appendix, respectively. The NLTE corrections for the S abundance defined as $\Delta({\rm S}) \equiv$ log S$_{\rm NLTE}$ $-$ log S$_{\rm LTE}$ were evaluated on these grids for two [S [i]{} ]{}lines of the HIRES sample and the samples of [Fran[ç]{}ois ]{}(1987, 1988) and Clegg et al. (1981) using their measured [$W_{\lambda}$ ]{}. As for the OAO sample, since the [S [i]{} ]{}lines are blended, we computed the [$W_{\lambda}$ ]{}of each [S [i]{} ]{}line corresponding to the derived log S$_{\rm LTE}$ and used them to estimate $\Delta({\rm S})$. The average values of each $\Delta({\rm S})$ are given in the seventh column of Tables 6 and 7 for the HIRES sample and the giant star HD 111721 and for the sample of dwarfs, respectively.

The NLTE abundances of Fe were calculated for \[Fe [i]{}/H\]$_{\rm LTE}$ in all our samples using the polynomial relation derived by Israelian et al. (2001), which is based on the NLTE work of Thévenin & Idiart (1999). The results are shown as \[Fe [i]{}/H\]$_{\rm NLTE}$ in Tables 6 and 7.

The values of \[S/Fe [i]{}\]$_{\rm NLTE}$ were computed based on the above-obtained \[S/H\]$_{\rm LTE}$, $\Delta({\rm S})$, and \[Fe [i]{}/H\]$_{\rm NLTE}$, and are summarized in Tables 6 and 7 for each sample.

Since Fe abundances inferred from [Fe [ii]{} ]{}lines are separately dealt with in the HIRES sample, the results of \[S/Fe [ii]{}\]$_{\rm NLTE}$ are also entered in Table 6. Here we applied the values 