All Figures

$\begin{figure} \par\includegraphics[height=21.8cm,width=8.5cm,clip]{2490Fig2.ps} \end{figure}$ Figure 2: The effect of $\alpha$ -enhancement, micro-turbulent velocity $\xi$ , new vs old ODFs, and inclusion of "predicted lines'' are illustrated by sample spectra. To increase readability all spectra have been broadened to a rotational velocity of 20 km s^-1. In each panel the bottom part highlights the difference between the plotted spectra (always in the sense solid - dotted lines).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2490Fig3.ps} \end{figure}$ Figure 3: The observed spectra (solid thick lines) of two eclipsing binaries compared with synthetic ones computed without (solid thin line) and with (dotted line) inclusion of so-called "predicted lines''. The synthetic spectra are computed for the atmospheric parameters ( $T_{\rm eff}$ , $\log g$ ) and co-rotational rotational velocity as derived from the accurate orbital solutions of Siviero et al. (2004, for V432 Aur) and Marrese et al. (2005, for V570 Per) and their chemical abundance analysis. The spectra of the two components are shifted at the appropriate radial velocity and combined following the light-ratio at the these wavelengths as derived in the orbital solution. The synthetic spectra computed without the "predicted lines'' offer a much better representation of the observed ones, and the effect of the inclusion of "predicted lines'' becomes worst with increasing metallicity.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=17.8cm,clip]{2490Fig4.ps} \end{figure}$ Figure 4: The use of our synthetic spectral library at resolving power $R_{\rm P}=8500$ to classify RAVE spectra. The left panels show the results of $\chi ^2$ fitting in gravity and temperature of spectra of HD stars from RAVE fields 1607m492 and 1716m425, with spectral types from the Michigan Project (Houk 1978) and calibration into $T_{\rm eff}$ and $\log g$ by Straizys & Kuriliene (1981). The dotted lines represent margins for $\pm$ 3% in $T_{\rm eff}$ and $\pm$ 0.25 dex in gravity. The error bars on each point represent the spread in the results of $\chi ^2$ fitting of three different spectra of the same object secured on different nights. On the right panels, examples of a match between observed and synthetic spectra are provided for two HD stars from the same RAVE fields. The results of the $\chi ^2$ fitting for the two spectra are given for $T_{\rm eff}$ , $\log g$ and metallicity.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{2490Fig5.ps} \end{figure}$ Figure 5: Comparison of synthetic colors along the Main Sequence truncated at M2V. The observed empirical Main Sequence of Fitzgerald (1970) serves as a comparison. The adopted band transmission profiles are those of Buser (1978).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2490Fig6.ps} \end{figure}$ Figure 6: The behaviour of photometric colors along the Main Sequence for individual spectral types. The same data of Fig. 5 are used. The adopted band transmission profiles for $R_{\rm C}$ and $I_{\rm C}$ are those of Bessell (1990).
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In the text

$\begin{figure} \par\includegraphics[height=21.8cm,width=8.5cm,clip]{2490Fig2.ps} \end{figure}$	Figure 2: The effect of $\alpha$ -enhancement, micro-turbulent velocity $\xi$ , new vs old ODFs, and inclusion of "predicted lines'' are illustrated by sample spectra. To increase readability all spectra have been broadened to a rotational velocity of 20 km s^-1. In each panel the bottom part highlights the difference between the plotted spectra (always in the sense solid - dotted lines).
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$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{2490Fig5.ps} \end{figure}$	Figure 5: Comparison of synthetic colors along the Main Sequence truncated at M2V. The observed empirical Main Sequence of Fitzgerald (1970) serves as a comparison. The adopted band transmission profiles are those of Buser (1978).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2490Fig6.ps} \end{figure}$	Figure 6: The behaviour of photometric colors along the Main Sequence for individual spectral types. The same data of Fig. 5 are used. The adopted band transmission profiles for $R_{\rm C}$ and $I_{\rm C}$ are those of Bessell (1990).
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