All Figures

$\begin{figure} \par\includegraphics[width=13.2cm,clip]{7904fig1.ps}\end{figure}$ Figure 1: Left panel: CMD for NGC 2324 (photometry from Kyeong et al. 2001); we also show the best-fit isochrone (from the Padova set by Bertelli et al. 1994) corresponding to the values given in the box and adopted in the paper. Right panel: CMD for NGC 2477 (photometry from EIS, aligned to the Kassis et al. 1997, one). In both panels the (red) filled circles indicate stars for which we derived abundances, and the (blue) triangles discarded stars (see text).
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In the text

$\begin{figure} \par\includegraphics[width=12.5cm,clip]{7904fig2.ps}\end{figure}$ Figure 2: Example of spectra for NGC 2324 ( upper panel) and NGC 2477 ( lower panel), shifted to RV = 0 km s^-1. Notice the wide lines for the giant star 10360 in NGC 2324, indicative of a fast rotation; objects 6530 and 7109 in NGC 2477 are MS stars. A few lines used in our abundance analysis are indicated.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{7904fig3.ps}\end{figure}$ Figure 3: Comparison for the three NGC 3960 stars in common with B06; small, filled symbols indicate the individual stars (square: c6, triangle: c5, circle: c8), while the starred (red) symbols indicate the average for each element.
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In the text

$\begin{figure} \par\includegraphics[width=12.5cm,clip]{7904fig4.ps}\par\includegraphics[width=12.5cm,clip]{fig4.ps}\end{figure}$ Figure 4: Comparison of the abundances of Na, Ni and $\alpha$ elements for the five clusters in the present paper (red filled circles) and i) thin-disk field stars (grey open squares, Soubiran & Girard 2005); ii) NGC 6253 (blue filled circle, S07); iii) NGC 6819, Cr 261 and NGC 6791 (green filled squares, Bragaglia et al. 2001; Carretta et al. 2005, 2007); iv) the outer Galactic disk clusters Be 31, Be 29, Be 20, NGC 2141, plus M 67 (orange filled triangles, Yong et al. 2005); the outer Galactic disk clusters Be 22, Be 66 and Saurer 1 (purple inverse triangles, Villanova et al. 2005; Carraro et al. 2004). The comparison of Ba abundances for the same OCs is made with Allende Prieto et al. (2004, grey crosses).
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{7904fig5.ps}\end{figure}$ Figure 5: $\alpha$ -elements versus $R_{\rm GC}$ (panel a)) and age (panel b)), metallicity versus age (panel c)) and $R_{\rm GC}$ (panel d)) for the open clusters considered; symbols are as in the preceding figure.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{7904figa1.ps}\end{figure}$ Figure A.1: Interstellar Na I D1 and D2 lines for the three MS stars in NGC 3960: multiple components are visible, and the dominant ones are found at RVs of about -3, 26 and 40 km s^-1.

In the text

$\begin{figure} \par\includegraphics[width=12.5cm,clip]{7904fig2.ps}\end{figure}$	Figure 2: Example of spectra for NGC 2324 ( upper panel) and NGC 2477 ( lower panel), shifted to RV = 0 km s^-1. Notice the wide lines for the giant star 10360 in NGC 2324, indicative of a fast rotation; objects 6530 and 7109 in NGC 2477 are MS stars. A few lines used in our abundance analysis are indicated.
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$\begin{figure} \par\includegraphics[width=7.6cm,clip]{7904fig3.ps}\end{figure}$	Figure 3: Comparison for the three NGC 3960 stars in common with B06; small, filled symbols indicate the individual stars (square: c6, triangle: c5, circle: c8), while the starred (red) symbols indicate the average for each element.
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$\begin{figure} \par\includegraphics[width=6.5cm,clip]{7904fig5.ps}\end{figure}$	Figure 5: $\alpha$ -elements versus $R_{\rm GC}$ (panel a)) and age (panel b)), metallicity versus age (panel c)) and $R_{\rm GC}$ (panel d)) for the open clusters considered; symbols are as in the preceding figure.
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