All Figures

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{HD4736fig1.eps} \end{figure}$ Figure 1: Comparison between the distances given by JP94 and the MS fitting distances we obtain for a subsample of 10 clusters (see text for details). The solid line represent the 1:1 relationship between the two sets of distances.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{HD4736fig2.eps} \end{figure}$ Figure 2: Best-fitting isochrone for the MS and turn-off region of the cluster NGC 2420. Reddening, distance modulus, age and metallicity employed in the fit are given.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{HD4736fig3.eps} \end{figure}$ Figure 3: Fit to the ages of the calibrating clusters (filled circles) given in Table 1.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{HD4736fig4.eps} \end{figure}$ Figure 4: Ages for the 71 old OCs plus 47 Tuc, as a function of the cluster [Fe/H]. Open squares denote the 11 calibrating clusters. Individual clusters discussed in the text are labelled.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{HD4736fig5.eps} \end{figure}$ Figure 5: Comparison between our derived ages and those given by JP94. The solid line denotes the 1:1 relationship.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{HD4736fig6.eps} \end{figure}$ Figure 6: Cumulative age distribution ( upper panel) and differential age distribution ( lower panel) for the 71 OCs in our sample. In the upper panel the age distribution from the Monte Carlo simulations discussed in the text (filled circles) is shown together with the actual cumulative distribution (open squares). The line with slope corresponding to a dissolution timescale of 2.5 Gyr is also displayed.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{HD4736fig7.eps} \end{figure}$ Figure 7: Comparison of the cumulative age distributions for clusters located in two different ranges of height above the Galactic plane, |z| ( upper panel), or galactocentric distance, $R_{\rm gc}$ ( lower panel; see text for details). The line with a slope corresponding to a dissolution timescale of 2.5 Gyr is displayed in both panels.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{HD4736fig8.eps} \end{figure}$ Figure 8: Relationship between [Fe/H] and galactocentric distance for the 38 clusters with metallicities on the G00 scale. The solid line displays the linear best-fit considering all 38 clusters; the dashed line shows the best-fit excluding Be 29.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{HD4736fig9.eps} \end{figure}$ Figure 9: Age distribution as a function of $\rm [Fe/H]_{corr}$ ([Fe/H] corrected to the solar circle, see text for details) for the 38 clusters with [Fe/H] on the G00 scale.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{HD4736fig10.eps} \end{figure}$ Figure 10: Age distribution as a function of [Fe/H] for the clusters analyzed in this study (filled circles) and the GCs studied by SW02 (open squares).
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{HD4736fig11.eps} \end{figure}$ Figure 11: Histogram of the ages of the GC sample studied by SW02, compared to the OC ages derived in this study (shaded histogram).
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{HD4736fig1.eps} \end{figure}$	Figure 1: Comparison between the distances given by JP94 and the MS fitting distances we obtain for a subsample of 10 clusters (see text for details). The solid line represent the 1:1 relationship between the two sets of distances.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{HD4736fig2.eps} \end{figure}$	Figure 2: Best-fitting isochrone for the MS and turn-off region of the cluster NGC 2420. Reddening, distance modulus, age and metallicity employed in the fit are given.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{HD4736fig3.eps} \end{figure}$	Figure 3: Fit to the ages of the calibrating clusters (filled circles) given in Table 1.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{HD4736fig4.eps} \end{figure}$	Figure 4: Ages for the 71 old OCs plus 47 Tuc, as a function of the cluster [Fe/H]. Open squares denote the 11 calibrating clusters. Individual clusters discussed in the text are labelled.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{HD4736fig5.eps} \end{figure}$	Figure 5: Comparison between our derived ages and those given by JP94. The solid line denotes the 1:1 relationship.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{HD4736fig7.eps} \end{figure}$	Figure 7: Comparison of the cumulative age distributions for clusters located in two different ranges of height above the Galactic plane, \|z\| ( upper panel), or galactocentric distance, $R_{\rm gc}$ ( lower panel; see text for details). The line with a slope corresponding to a dissolution timescale of 2.5 Gyr is displayed in both panels.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{HD4736fig8.eps} \end{figure}$	Figure 8: Relationship between [Fe/H] and galactocentric distance for the 38 clusters with metallicities on the G00 scale. The solid line displays the linear best-fit considering all 38 clusters; the dashed line shows the best-fit excluding Be 29.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{HD4736fig9.eps} \end{figure}$	Figure 9: Age distribution as a function of $\rm [Fe/H]_{corr}$ ([Fe/H] corrected to the solar circle, see text for details) for the 38 clusters with [Fe/H] on the G00 scale.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{HD4736fig10.eps} \end{figure}$	Figure 10: Age distribution as a function of [Fe/H] for the clusters analyzed in this study (filled circles) and the GCs studied by SW02 (open squares).
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{HD4736fig11.eps} \end{figure}$	Figure 11: Histogram of the ages of the GC sample studied by SW02, compared to the OC ages derived in this study (shaded histogram).
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