$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0753fg1a.eps}\par\vspace*{2mm} \includegraphics[width=8.8cm,clip]{0753fg1b.eps} \end{figure}$ Figure 1: The comparison of equivalent widths with other works: a) with Zhao & Magain (1990) for BD +02 $^{\circ }$ 3375, b) with Stephens & Boesgaard (2002) for BD +42 $^{\circ }$ 2667.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0753fig2.eps} \end{figure}$ Figure 2: $T_{\rm eff}$ comparisons between this work and various literature studies. Circles: Nissen et al. (1997); triangles: Alonso et al. (1996); diamonds: Fulbright (2000); crosses: Takeda (2003).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0753fig3.eps} \end{figure}$ Figure 3: Toomre diagram: (U²+W²)^1/2 versus rotational velocity (V). We divide sample stars to two groups: definitively regrograde orbit stars with $V_{\rm tot} > 300$ km s^-1 (filled circles) and remaining stars with $V_{\rm tot}< 300$ km s^-1 (asterisks).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0753fg5a.eps}\par\vspace*{2mm} \includegraphics[width=8.8cm,clip]{0753fg5b.eps} \end{figure}$ Figure 5: a): The [O/Fe] ratio vs. [Fe/H] of our sample stars. b): Comparison with other studies. The open circles present the data from Beosgaard et al. (1999) using OH lines. The open triangles present O I triplets result from Mishenina et al. (2000), and the crosses present the forbidden line [O I] 6300 Å result from Nissen et al. (2002). The diamonds present reanalysed [O/Fe] ratio by Takeda (2003) for common stars. Our results are presented by filled triangles. The common stars are connected with solid lines.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0753fg1a.eps}\par\vspace*{2mm} \includegraphics[width=8.8cm,clip]{0753fg1b.eps} \end{figure}$	Figure 1: The comparison of equivalent widths with other works: a) with Zhao & Magain (1990) for BD +02 $^{\circ }$ 3375, b) with Stephens & Boesgaard (2002) for BD +42 $^{\circ }$ 2667.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0753fig2.eps} \end{figure}$	Figure 2: $T_{\rm eff}$ comparisons between this work and various literature studies. Circles: Nissen et al. (1997); triangles: Alonso et al. (1996); diamonds: Fulbright (2000); crosses: Takeda (2003).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0753fig3.eps} \end{figure}$	Figure 3: Toomre diagram: (U²+W²)^1/2 versus rotational velocity (V). We divide sample stars to two groups: definitively regrograde orbit stars with $V_{\rm tot} > 300$ km s^-1 (filled circles) and remaining stars with $V_{\rm tot}< 300$ km s^-1 (asterisks).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0753fg4a.eps}\par\vspace*{2mm} \includegraphics[width=8.8cm,clip]{0753fg4b.eps} \end{figure}$	Figure 4: The spectra of O I triplet for three sample stars, and spectra comparison with Zhang & Zhao (2003) for HD 108177.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0753fig6.eps} \end{figure}$	Figure 6: Abundance patterns for $\alpha$ -elements (Mg, Si, Ca and Ti).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0753fig7.eps} \end{figure}$	Figure 7: NLTE abundances of Sodium: filled symbols: this study, open triangles: Baumüller et al. (1998).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0753fig8.eps} \end{figure}$	Figure 8: Scandium abundance versus metallicity.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0753fig9.eps} \end{figure}$	Figure 9: Iron peak elements ratios as a function of metallicity.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0753fg10.eps} \end{figure}$	Figure 10: [Ba/Fe] vs. [Fe/H].
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