$\begin{figure} \par\includegraphics[width=5.8cm,clip]{0454f1.eps}\end{figure}$ Figure 1: Comparison of solar EW measured in this study with those from the literature (Edvardsson et al. 1993 - filled circles, Reddy et al. 2002 - open circles).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0454f2.eps} \end{figure}$ Figure 2: Comparison of our adopted temperatures with those estimated by Alonso et al. (1996), Blackwell & Lynas-Gray (1998) and di Benedetto (1998). Crosses indicate stars with ${\rm [Fe/H]}$ <-0.5. The two outliers HD 101177 and HD 165341 are discussed in the text. HD 165341 was measured by Alonso et al., that is why there are 3 points for the same star.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0454f4.eps}\end{figure}$ Figure 4: Grotrian diagram for MgI. Displayed are the radiative transitions treated explicity in the non-LTE calculations.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0454f5.eps} \end{figure}$ Figure 5: Comparison of synthetic NLTE profiles (continuous line) of the MgI lines to the observed spectrum of HD 224930 (dots).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0454f7.ps} \end{figure}$ Figure 7: ${\rm [Mg/Fe]}$ vs. ${\rm [Fe/H]}$ for the whole sample. Black dots indicate thick disk stars, open dots thin disk stars, small dots represent the unclassified stars.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{0454f12.eps} \end{figure}$ Figure 12: The maximum distance to the plane of orbits, ${Z_{\rm max}}$ , versus ${\rm [Fe/H]}$ for Bensby et al.'s sample. The classification thin disk / thick disk is the same as ours (Pr_i>80%).
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In the text

$\begin{figure} \par\includegraphics[width=5.8cm,clip]{0454f1.eps}\end{figure}$	Figure 1: Comparison of solar EW measured in this study with those from the literature (Edvardsson et al. 1993 - filled circles, Reddy et al. 2002 - open circles).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0454f2.eps} \end{figure}$	Figure 2: Comparison of our adopted temperatures with those estimated by Alonso et al. (1996), Blackwell & Lynas-Gray (1998) and di Benedetto (1998). Crosses indicate stars with ${\rm [Fe/H]}$ <-0.5. The two outliers HD 101177 and HD 165341 are discussed in the text. HD 165341 was measured by Alonso et al., that is why there are 3 points for the same star.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0454f3a.eps}\vspace*{1mm} \includegraphics[width=8.8cm,clip]{0454f3b.eps}\end{figure}$	Figure 3: Abundances of Fe and Mg vs. ${T_{\rm eff}}$ .
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0454f4.eps}\end{figure}$	Figure 4: Grotrian diagram for MgI. Displayed are the radiative transitions treated explicity in the non-LTE calculations.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0454f5.eps} \end{figure}$	Figure 5: Comparison of synthetic NLTE profiles (continuous line) of the MgI lines to the observed spectrum of HD 224930 (dots).
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$\begin{figure} \par\includegraphics[width=8cm,clip]{0454f6.ps} \end{figure}$	Figure 6: Distribution of the 174 stars in the plane metallicity - W velocity.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{0454f7.ps} \end{figure}$	Figure 7: ${\rm [Mg/Fe]}$ vs. ${\rm [Fe/H]}$ for the whole sample. Black dots indicate thick disk stars, open dots thin disk stars, small dots represent the unclassified stars.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{0454f8.ps} \end{figure}$	Figure 8: Same as Fig. 7 for Si.
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{0454f9.eps} \end{figure}$	Figure 9: Same as Fig. 7 for Ni.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{0454f10.ps} \end{figure}$	Figure 10: Correlation between ${\rm [Mg/Fe]}$ and ${\rm [Si/Fe]}$ .
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$\begin{figure} \par\includegraphics[width=8cm,clip]{0454f11.ps} \end{figure}$	Figure 11: The maximum distance to the plane of orbits, ${Z_{\rm max}}$ , versus ${\rm [Fe/H]}$ .
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{0454f12.eps} \end{figure}$	Figure 12: The maximum distance to the plane of orbits, ${Z_{\rm max}}$ , versus ${\rm [Fe/H]}$ for Bensby et al.'s sample. The classification thin disk / thick disk is the same as ours (Pr_i>80%).
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{0454f13.eps} \end{figure}$	Figure 13: A possible vertical gradient in [ $\alpha$ /Fe] in the thick disk?
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