All Figures

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0142fig1.ps} \end{figure}$ Figure 1: Field of 10 $\times$ 10 arcmin² centered on NGC 2506, with the 4 stars observed with FEROS indicated by their numbers according to Marconi et al. (1997).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0142fig2.ps} \end{figure}$ Figure 2: Field of 10 $\times$ 10 arcmin² centered on NGC 6134, with the 6 stars observed with FEROS or UVES indicated by their numbers according to Lindoff (1972).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0142fig3.ps} \end{figure}$ Figure 3: Field of 10 $\times$ 10 arcmin² centered on IC 4651, with the 5 stars observed with FEROS indicated by their numbers according to Lindoff (1972), and Meibom (2000).
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{0142fig4.ps} \end{figure}$ Figure 4: CMDs for the three clusters, with the stars analyzed here indicated by larger symbols. a) NGC 2506: B and V taken from Marconi et al. (1997); only stars with membership probability greater than 0.7 (Chiu & van Altena 1981) are shown. b) NGC 6134: V, b-y taken from Bruntt et al. (1999). c) IC 4651: V, b-y taken from Anthony-Twarog & Twarog (2000).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0142fig5.ps} \end{figure}$ Figure 5: Spectroscopic gravities as a function of the derived photometric gravities. Different symbols are used for the 3 clusters. In the inset, only the clump stars and red giant stars are plotted, excluding the stars near the RGB-tip.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0142fig6.ps} \end{figure}$ Figure 6: Comparison between the observed spectrum of the field metal-rich giant star HR 3627 (open squares) and the synthetic spectrum computed by optimizing the Kurucz line lists (solid lines). Small regions around 2 Fe I and 2 Fe II lines are shown.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0142fig7.ps} \end{figure}$ Figure 7: Comparison between the observed UVES spectrum of star 421 in NGC 6134 (open squares) with synthetic spectra of two Fe I and two Fe II lines (solid lines). The spectral synthesis was computed by using the atmospheric parameters appropriate to the star and 3 Fe abundances: $\rm [Fe/H]=-0.2$ , 0.0 and +0.2 dex from top to bottom, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0142fig1.ps} \end{figure}$	Figure 1: Field of 10 $\times$ 10 arcmin² centered on NGC 2506, with the 4 stars observed with FEROS indicated by their numbers according to Marconi et al. (1997).
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0142fig2.ps} \end{figure}$	Figure 2: Field of 10 $\times$ 10 arcmin² centered on NGC 6134, with the 6 stars observed with FEROS or UVES indicated by their numbers according to Lindoff (1972).
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0142fig3.ps} \end{figure}$	Figure 3: Field of 10 $\times$ 10 arcmin² centered on IC 4651, with the 5 stars observed with FEROS indicated by their numbers according to Lindoff (1972), and Meibom (2000).
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$\begin{figure} \par\includegraphics[width=15cm,clip]{0142fig4.ps} \end{figure}$	Figure 4: CMDs for the three clusters, with the stars analyzed here indicated by larger symbols. a) NGC 2506: B and V taken from Marconi et al. (1997); only stars with membership probability greater than 0.7 (Chiu & van Altena 1981) are shown. b) NGC 6134: V, b-y taken from Bruntt et al. (1999). c) IC 4651: V, b-y taken from Anthony-Twarog & Twarog (2000).
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0142fig5.ps} \end{figure}$	Figure 5: Spectroscopic gravities as a function of the derived photometric gravities. Different symbols are used for the 3 clusters. In the inset, only the clump stars and red giant stars are plotted, excluding the stars near the RGB-tip.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0142fig6.ps} \end{figure}$	Figure 6: Comparison between the observed spectrum of the field metal-rich giant star HR 3627 (open squares) and the synthetic spectrum computed by optimizing the Kurucz line lists (solid lines). Small regions around 2 Fe I and 2 Fe II lines are shown.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0142fig7.ps} \end{figure}$	Figure 7: Comparison between the observed UVES spectrum of star 421 in NGC 6134 (open squares) with synthetic spectra of two Fe I and two Fe II lines (solid lines). The spectral synthesis was computed by using the atmospheric parameters appropriate to the star and 3 Fe abundances: $\rm [Fe/H]=-0.2$ , 0.0 and +0.2 dex from top to bottom, respectively.
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