Astronomy & Astrophysics

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{2390fig1.eps} \end{figure}$ Figure 1: Comparaison of [Mg/H] computed under NLTE approximation by M04 and LTE [Mg/H] computed by the other authors. No systematic trend can be observed. The mean difference is null, the dispersion 0.13 dex for 126 stars in common.
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In the text

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{2390fig2.eps} \end{figure}$ Figure 2: Comparaison of [Na/H] computed under NLTE approximation by G03 and LTE [Na/H] computed by the other authors. No systematic trend can be observed. The mean difference is null, the dispersion 0.07 dex for 130 stars in common.
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In the text

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{2390fig3.eps} \end{figure}$ Figure 3: Differences between [O/H] on the LTE 6300 Å scale derived by authors having stars in common.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{2390fig5.eps}\end{figure}$ Figure 5: $\sigma _W$ vs. [Fe/H] of the whole sample in several bins of metallicity. Error bars correspond to the standard error for $\sigma _W (\sigma _W/\sqrt {2N})$ and standard deviation for [Fe/H].
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{2390fig6.eps}\end{figure}$ Figure 6: Eccentricity of the orbits vs. [Fe/H] of the whole sample in several bins of metallicity. Error bars correspond to the standarddeviations.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{2390fig7.eps}\end{figure}$ Figure 7: Age vs. [Fe/H] in several bins of metallicity for stars having well defined ages. Error bars correspond to the standard deviations.
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{2390fig8.eps}\end{figure}$ Figure 8: The sample of 639 stars plotted in the (U, V) plane. Thick disk stars are represented by red dots, thin disk stars by open green squares and Hercules stars by open blue circles. The small dots correspond to stars which could not be classified into the 3 subgroups.
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In the text

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{2390fig10a.eps}\includegra... ...p]{2390fig10g.eps}\includegraphics[width=7.1cm,clip]{2390fig10h.eps}\end{figure}$ Figure 10: Averaged [X/Fe] vs. [Fe/H] per bin of metallicity in the thin disk (green squares) in the thick disk (red filled circles) and in the Hercules stream (blue open circles). Errors bars correspond to the standard deviations around the mean value in each bin.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{2390fig11.eps}\end{figure}$ Figure 11: Age vs. [Fe/H] for stars having well-defined ages. As in Figs. 8 and 9, the different symbols indicate thin disk, thick disk and Hercules stars.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{2390fig12.eps}\end{figure}$ Figure 12: Age vs. [Fe/H] for stars having well-defined ages. As in Figs. 8 and 9, the different symbols indicate thin disk, thick disk and Hercules stars.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm]{2390fig13.eps}\end{figure}$ Figure 13: Zmax, the maximal distance to the plane reached by the orbit, in several bins of metallicity for thick disk stars.
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In the text

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{2390fig1.eps} \end{figure}$	Figure 1: Comparaison of [Mg/H] computed under NLTE approximation by M04 and LTE [Mg/H] computed by the other authors. No systematic trend can be observed. The mean difference is null, the dispersion 0.13 dex for 126 stars in common.
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$\begin{figure} \par\includegraphics[width=6.8cm,clip]{2390fig2.eps} \end{figure}$	Figure 2: Comparaison of [Na/H] computed under NLTE approximation by G03 and LTE [Na/H] computed by the other authors. No systematic trend can be observed. The mean difference is null, the dispersion 0.07 dex for 130 stars in common.
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$\begin{figure} \par\includegraphics[width=6.8cm,clip]{2390fig3.eps} \end{figure}$	Figure 3: Differences between [O/H] on the LTE 6300 Å scale derived by authors having stars in common.
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$\begin{figure} \par\includegraphics[width=6.8cm,clip]{2390fig4a.eps}\includegrap... ...lip]{2390fig4g.eps}\includegraphics[width=6.8cm,clip]{2390fig4h.eps}\end{figure}$	Figure 4: [X/Fe] vs. [Fe/H].
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$\begin{figure} \par\includegraphics[width=7.2cm,clip]{2390fig5.eps}\end{figure}$	Figure 5: $\sigma _W$ vs. [Fe/H] of the whole sample in several bins of metallicity. Error bars correspond to the standard error for $\sigma _W (\sigma _W/\sqrt {2N})$ and standard deviation for [Fe/H].
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$\begin{figure} \par\includegraphics[width=7.2cm,clip]{2390fig6.eps}\end{figure}$	Figure 6: Eccentricity of the orbits vs. [Fe/H] of the whole sample in several bins of metallicity. Error bars correspond to the standarddeviations.
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$\begin{figure} \par\includegraphics[width=7.2cm,clip]{2390fig7.eps}\end{figure}$	Figure 7: Age vs. [Fe/H] in several bins of metallicity for stars having well defined ages. Error bars correspond to the standard deviations.
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$\begin{figure} \par\includegraphics[width=7.3cm,clip]{2390fig8.eps}\end{figure}$	Figure 8: The sample of 639 stars plotted in the (U, V) plane. Thick disk stars are represented by red dots, thin disk stars by open green squares and Hercules stars by open blue circles. The small dots correspond to stars which could not be classified into the 3 subgroups.
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$\begin{figure} \par\includegraphics[width=7.3cm,clip]{2390fig9.eps}\end{figure}$	Figure 9: As for Fig. 8, but in the Toomre diagram: $UW=\sqrt {U^2+W^2}$ ${\rm ~km~s}^{-1}$ .
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$\begin{figure} \par\includegraphics[width=7.1cm,clip]{2390fig10a.eps}\includegra... ...p]{2390fig10g.eps}\includegraphics[width=7.1cm,clip]{2390fig10h.eps}\end{figure}$	Figure 10: Averaged [X/Fe] vs. [Fe/H] per bin of metallicity in the thin disk (green squares) in the thick disk (red filled circles) and in the Hercules stream (blue open circles). Errors bars correspond to the standard deviations around the mean value in each bin.
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$\begin{figure} \par\includegraphics[width=7.2cm,clip]{2390fig11.eps}\end{figure}$	Figure 11: Age vs. [Fe/H] for stars having well-defined ages. As in Figs. 8 and 9, the different symbols indicate thin disk, thick disk and Hercules stars.
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$\begin{figure} \par\includegraphics[width=7.2cm,clip]{2390fig12.eps}\end{figure}$	Figure 12: Age vs. [Fe/H] for stars having well-defined ages. As in Figs. 8 and 9, the different symbols indicate thin disk, thick disk and Hercules stars.
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$\begin{figure} \par\includegraphics[width=7.5cm]{2390fig13.eps}\end{figure}$	Figure 13: Zmax, the maximal distance to the plane reached by the orbit, in several bins of metallicity for thick disk stars.
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