All Figures

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{7344fig1.eps}\end{figure}$ Figure 1: The VLT/UVES spectrum of HD 84937 in the spectral region 9210-9240 Å overlaid with the B2III spectrum of HR 5488. Below is the spectrum of HD 84937 (shifted $\sim$ 0.5 units in relative flux) after removal of the telluric lines using the IRAF task telluric to divide with a scaled version of the spectrum of HR 5488.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{7344fig2.eps}\end{figure}$ Figure 2: The VLT/UVES spectrum of HD 84937 in the spectral region 8685-8705 Å overlaid with the B2III spectrum of HR 5488. Below is the spectrum of HD 84937 (shifted down 0.04 units in relative flux) after division with the spectrum of HR 5488.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{7344fig3.eps}\end{figure}$ Figure 3: Observed H $\beta$ profiles in the spectra of CD $-24\hbox {$^\circ $ }17504$ ( $T_{\rm eff}$ = 6340 K, upper jagged line) and LP 815-43 ( $T_{\rm eff}$ = 6480 K, lower jagged line) compared to synthetic profiles (thin lines) computed for model atmospheres with log g = 4.3, $\mbox{\rm [Fe/H]}= -2.8$ and $T_{\rm eff}$ = 6000, 6300, 6600 K, respectively. An index, $\beta$ (UVES), measuring the strength of the H $\beta$ line is defined from the total flux in the C bands relative to the total flux in the L bands (see Appendix B).
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{7344fig4.eps}\end{figure}$ Figure 4: The difference of effective temperatures derived from ( $V\!-\!K)_0$ and H $\beta$ using three different calibrations of ( $V\!-\!K)_0$ . The comparison includes only 38 stars; LP 651-4 falls outside the range in ( $V\!-\!K)_0$ where the calibrations are valid, and CD $-71\hbox {$^\circ $ }1234$ is missing Strömgren photometry; hence, its interstellar reddening excess, $E\mbox{($V\!-\!K)$ }$ , could not be derived. Three stars known to be single-lined spectroscopic binaries are marked.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{7344fig5.eps}\end{figure}$ Figure 5: The difference in S abundances derived from the $\lambda 9212.9$ and $\lambda 9237.5$ S I lines as a function of $T_{\rm eff}$ and [Fe/H]. The rms deviation between the two sets of abundances is $\pm$ 0.06 dex.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{7344fig6.eps}\end{figure}$ Figure 6: UVES observations (dots) of the $\lambda \lambda 9212.9, 9237.5$ S I lines in the spectrum of HD 181743. The four synthetic profiles marked by a, b, c and d refer to log $\epsilon ({\rm S})$ = 5.33, 5.63, 5.93 and 6.23 corresponding to [S/Fe] = 0.0, 0.3, 0.6 and 0.9, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{7344fig7.eps}\end{figure}$ Figure 7: UVES spectra (jagged line) of the region around the $\lambda 8694.6$ S I line. For each star, the three synthetic profiles marked by a, b and c correspond to [S/Fe] = 0.3, 0.6 and 0.9.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{7344fig8.eps}\end{figure}$ Figure 8: Comparison of S abundances derived from the S I 9212.9, 9237.5 Å pair and the $\lambda 8694.6$ line. Filled circles refer to LTE. Open circles include non-LTE corrections according to Takeda et al. (2005) with the hydrogen collisional parameter $S_{\rm H} = 1$ , and crosses refer to $S_{\rm H} = 0.1$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{7344fig9.eps}\end{figure}$ Figure 9: The CRIRES spectrum of G 29-23 around the 1.046 ${\mu }$ m S I triplet (dots) compared with synthetic profiles for three sulphur abundances, log $\epsilon ({\rm S})$ = 5.51, 5.81 and 6.11 corresponding to [S/Fe] = 0.0, 0.3 and 0.6, respectively. As seen, the [S/Fe] = 0.3 case provides an excellent fit to the observations.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{7344f10.eps}\end{figure}$ Figure 10: The $\lambda 4810.5$ Zn I line in UVES spectra of three stars. The spectra of G 04-37 and CD $-24\hbox {$^\circ $ }17504$ have been offset in relative flux by 0.04 and 0.08, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{7344f11.eps}\end{figure}$ Figure 11: [S/Fe] vs. [Fe/H] for our sample of halo stars supplemented with disk stars (shown as crosses) from Chen et al. (2002). Filled circles with error bars show data based on S abundances derived from the $\lambda \lambda 9212.9, 9237.5$ S I lines, and open circles show data based on the weak $\lambda 8694.6$ S I line. In the upper panel LTE has been assumed in deriving the S abundances, whereas the lower panel includes non-LTE corrections from Takeda et al. (2005) with the hydrogen collisional parameter $S_{\rm H} = 1$ . In both cases, the iron abundances are the LTE values derived from Fe II lines.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{7344f12.eps}\end{figure}$ Figure 12: [Zn/Fe] vs. [Fe/H] for our sample of halo stars. The upper panel refers to LTE Zn abundances. The lower panel includes non-LTE corrections from Takeda et al. (2005) corresponding to a hydrogen collisional parameter $S_{\rm H} = 1$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{7344f13.eps}\end{figure}$ Figure 13: [S/Zn] vs. [Zn/H] for Galactic stars and damped Lyman-alpha systems. Typical 1- $\sigma$ error bars are shown.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{7344fB1.eps}\end{figure}$ Figure B.1: The relation between $\beta$ (UVES) and $T_{\rm eff}$ as calculated for a set of model atmospheres. The full drawn line corresponds to log g = 4.3, [Fe/H] = -2.0, the dotted line to log g = 3.9, [Fe/H] = -2.0, and the dashed line to log g = 4.3, [Fe/H] = -3.2.

In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{7344fB2.eps}\end{figure}$ Figure B.2: The photometric index of the H $\beta$ line vs. the index measured from the profile of H $\beta$ in UVES spectra. 1- $\sigma$ error bars: $\sigma (\beta$ (UVES) $)=\pm 0.015$ and $\sigma (\beta$ (phot) $)=\pm 0.006$ are shown in the lower right corner. Stars having $\mbox{\rm [Fe/H]}< -2.0$ are plotted with filled circles, and stars having $-2.0 < \mbox{\rm [Fe/H]}< -1.0$ with open circles.

In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{7344fB3.eps}\end{figure}$ Figure B.3: The HP2 index of the H $\delta$ line (from Ryan et al. 1999) vs. $\beta$ (UVES).

In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{7344fig1.eps}\end{figure}$	Figure 1: The VLT/UVES spectrum of HD 84937 in the spectral region 9210-9240 Å overlaid with the B2III spectrum of HR 5488. Below is the spectrum of HD 84937 (shifted $\sim$ 0.5 units in relative flux) after removal of the telluric lines using the IRAF task `telluric` to divide with a scaled version of the spectrum of HR 5488.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{7344fig2.eps}\end{figure}$	Figure 2: The VLT/UVES spectrum of HD 84937 in the spectral region 8685-8705 Å overlaid with the B2III spectrum of HR 5488. Below is the spectrum of HD 84937 (shifted down 0.04 units in relative flux) after division with the spectrum of HR 5488.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{7344fig5.eps}\end{figure}$	Figure 5: The difference in S abundances derived from the $\lambda 9212.9$ and $\lambda 9237.5$ S I lines as a function of $T_{\rm eff}$ and [Fe/H]. The rms deviation between the two sets of abundances is $\pm$ 0.06 dex.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{7344fig6.eps}\end{figure}$	Figure 6: UVES observations (dots) of the $\lambda \lambda 9212.9, 9237.5$ S I lines in the spectrum of HD 181743. The four synthetic profiles marked by a, b, c and d refer to log $\epsilon ({\rm S})$ = 5.33, 5.63, 5.93 and 6.23 corresponding to [S/Fe] = 0.0, 0.3, 0.6 and 0.9, respectively.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{7344fig7.eps}\end{figure}$	Figure 7: UVES spectra (jagged line) of the region around the $\lambda 8694.6$ S I line. For each star, the three synthetic profiles marked by a, b and c correspond to [S/Fe] = 0.3, 0.6 and 0.9.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{7344fig8.eps}\end{figure}$	Figure 8: Comparison of S abundances derived from the S I 9212.9, 9237.5 Å pair and the $\lambda 8694.6$ line. Filled circles refer to LTE. Open circles include non-LTE corrections according to Takeda et al. (2005) with the hydrogen collisional parameter $S_{\rm H} = 1$ , and crosses refer to $S_{\rm H} = 0.1$ .
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{7344fig9.eps}\end{figure}$	Figure 9: The CRIRES spectrum of G 29-23 around the 1.046 ${\mu }$ m S I triplet (dots) compared with synthetic profiles for three sulphur abundances, log $\epsilon ({\rm S})$ = 5.51, 5.81 and 6.11 corresponding to [S/Fe] = 0.0, 0.3 and 0.6, respectively. As seen, the [S/Fe] = 0.3 case provides an excellent fit to the observations.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{7344f10.eps}\end{figure}$	Figure 10: The $\lambda 4810.5$ Zn I line in UVES spectra of three stars. The spectra of G 04-37 and CD $-24\hbox {$^\circ $ }17504$ have been offset in relative flux by 0.04 and 0.08, respectively.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{7344f12.eps}\end{figure}$	Figure 12: [Zn/Fe] vs. [Fe/H] for our sample of halo stars. The upper panel refers to LTE Zn abundances. The lower panel includes non-LTE corrections from Takeda et al. (2005) corresponding to a hydrogen collisional parameter $S_{\rm H} = 1$ .
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{7344f13.eps}\end{figure}$	Figure 13: [S/Zn] vs. [Zn/H] for Galactic stars and damped Lyman-alpha systems. Typical 1- $\sigma$ error bars are shown.
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