Astronomy & Astrophysics

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$\begin{figure} \par\includegraphics[width=8.0cm,clip]{2916.f1.ps} \end{figure}$ Figure 1: [X/Fe] ratios for O, Na, Mg, and Al versus $T_{\rm eff}$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.0cm,clip]{2916.f2.ps} \end{figure}$ Figure 2: [X/Fe] ratios for Si, Ca, Sc, and Ti versus $T_{\rm eff}$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.0cm,clip]{2916.f3.ps} \end{figure}$ Figure 3: [X/Fe] ratios for V, Mn, Co, and Ni versus $T_{\rm eff}$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.0cm,clip]{2916.f4.ps} \end{figure}$ Figure 4: [X/Fe] ratios for Cu, Y, Zr, and Ba versus $T_{\rm eff}$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.0cm,clip]{2916.f5.ps} \end{figure}$ Figure 5: [X/Fe] ratios for La, Ce, Nd, and Eu versus $T_{\rm eff}$ .
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2916.f6.ps} \end{figure}$ Figure 6: Summary of abundance ratios. For each element, the box represents the interquartile range while the horizontal line is the median value. The vertical lines extending from the box indicate the total range of the abundance, excluding outliers. Outliers are stars that lie more than 3 times the interquartile range from the median and are plotted as crosses. (Star NGC 6752-7 has been omitted due to its deviating [Fe/H].)
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In the text

$\begin{figure} \par\includegraphics[width=8.0cm]{2916.f7.ps} \end{figure}$ Figure 7: [X/Fe] ratios for Si, Ca, and Ti versus [Fe/H]. The small dots represent individual field stars taken from various sources (see text), the open circles are the mean value for different globular clusters, and the closed circle is mean value from this study. The error bars on the globular clusters represent the standard deviation.
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In the text

$\begin{figure} \par\includegraphics[width=8.0cm,clip]{2916.f8.ps} \end{figure}$ Figure 8: Same as Fig. 7 but for Sc, V, and Ni.
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In the text

$\begin{figure} \par\includegraphics[width=8.0cm,clip]{2916.f9.ps} \end{figure}$ Figure 9: Same as Fig. 7 but for Y, Ba, and Eu.
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In the text

$\begin{figure} \par\includegraphics[width=8.0cm,clip]{2916.f10.ps} \end{figure}$ Figure 10: Abundance ratios [Fe/H], [Si/Fe], and [X/Fe] (for s-process elements Y, Zr, Ba, La, and Ce) versus [Al/Fe]. Crosses represent the bump stars and filled circles represent the tip stars. The error bar shows the $\pm$ 1- $\sigma$ predicted error from Table 6. The dotted line is the mean abundance and the solid line is the linear least squares fit to the data (slope and associated error are included). Star NGC 6752-7 has been omitted due to its deviating [Fe/H].
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In the text

$\begin{figure} \par\includegraphics[width=8.0cm,clip]{2916.f11.ps} \end{figure}$ Figure 11: Same as Fig. 10 except for abundance ratios [Y/Eu], [Zr/Eu], [Ba/Eu], and [Ce/Eu] versus [Al/Fe]. Here we use only the abundances from ZrII lines.
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In the text

$\begin{figure} \par\includegraphics[width=8.0cm,clip]{2916.f1.ps} \end{figure}$	Figure 1: [X/Fe] ratios for O, Na, Mg, and Al versus $T_{\rm eff}$ .
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$\begin{figure} \par\includegraphics[width=8.0cm,clip]{2916.f2.ps} \end{figure}$	Figure 2: [X/Fe] ratios for Si, Ca, Sc, and Ti versus $T_{\rm eff}$ .
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$\begin{figure} \par\includegraphics[width=8.0cm,clip]{2916.f3.ps} \end{figure}$	Figure 3: [X/Fe] ratios for V, Mn, Co, and Ni versus $T_{\rm eff}$ .
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$\begin{figure} \par\includegraphics[width=8.0cm,clip]{2916.f4.ps} \end{figure}$	Figure 4: [X/Fe] ratios for Cu, Y, Zr, and Ba versus $T_{\rm eff}$ .
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$\begin{figure} \par\includegraphics[width=8.0cm,clip]{2916.f5.ps} \end{figure}$	Figure 5: [X/Fe] ratios for La, Ce, Nd, and Eu versus $T_{\rm eff}$ .
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$\begin{figure} \par\includegraphics[width=8.0cm]{2916.f7.ps} \end{figure}$	Figure 7: [X/Fe] ratios for Si, Ca, and Ti versus [Fe/H]. The small dots represent individual field stars taken from various sources (see text), the open circles are the mean value for different globular clusters, and the closed circle is mean value from this study. The error bars on the globular clusters represent the standard deviation.
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$\begin{figure} \par\includegraphics[width=8.0cm,clip]{2916.f8.ps} \end{figure}$	Figure 8: Same as Fig. 7 but for Sc, V, and Ni.
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$\begin{figure} \par\includegraphics[width=8.0cm,clip]{2916.f9.ps} \end{figure}$	Figure 9: Same as Fig. 7 but for Y, Ba, and Eu.
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$\begin{figure} \par\includegraphics[width=8.0cm,clip]{2916.f11.ps} \end{figure}$	Figure 11: Same as Fig. 10 except for abundance ratios [Y/Eu], [Zr/Eu], [Ba/Eu], and [Ce/Eu] versus [Al/Fe]. Here we use only the abundances from ZrII lines.
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