All Figures

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{fig1a.ps}\hspace*{-0.7mm} \includegraphics[width=8.4cm,clip]{fig1b.ps}\end{figure}$ Figure 1: $\rm 20\hbox {$^\prime $ }\times 20\hbox {$^\prime $ }$ XDSS R images of M 52 ( left panel) and NGC 3960 ( right panel).
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In the text

$\begin{figure} \par\includegraphics[width=4.5cm,clip]{fig2a.eps}\includegraphics[width=4.5cm,clip]{fig2b.eps}\end{figure}$ Figure 2: $\mbox{$J$ }\times\mbox{$(J-H)$ }$ CMDs of the central 10 $^\prime$ of M 52 ( left panel) and NGC 3960 ( right panel). Solid lines: fiducial lines used to derive the differential reddening (Sect. 3.1). Red stars belong mostly to the field (Sect. 3.2). Error bars are shown in the right panels of Fig. 4.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=\textwidth]{fig3a.eps}\hspace*{4cm} \includegraphics[width=\textwidth]{fig3b.eps} } \end{figure}$ Figure 3: Left panel: spatial grid used to derive the differential reddening in M 52. Only stars with colours consistent with the cluster's (Sect. 3.4) are plotted here. North is up and East left. Right panel: $\mbox{$J$ }\times\mbox{$(J-H)$ }$ CMDs extracted from the spatial grid ( left panel). The fiducial line of the central cell is shown in all panels as a continuous line. Spatial orientation follows that in the left panel. $\Delta X\rm_O$ and $\Delta Y\rm_O$ give the displacement along right ascension and declination of the center of each cell with respect to the central cell.
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In the text

$\begin{figure} \par\includegraphics[width=8.25cm,clip]{fig4.eps}\end{figure}$ Figure 4: Panel a): field stars ("x'') are superimposed on the differential-reddening corrected CMD of the central 5 $^\prime$ of M 52. Extraction areas match. Panel b): field-star decontaminated CMD. Solid line: 60 Myr Padova isochrone with $\mbox{$(m-M)_J$ }=11.3$ $\pm$ 0.1 and $\mbox{$E(J-H)$ }=0.18$ $\pm$ 0.01. Bottom panels: same as the top panels for NGC 3960. Solid line in panel d): 1.1 Gyr Padova isochrone with $\mbox{$(m-M)_J$ }=11.3$ $\pm$ 0.1 and $\mbox{$E(J-H)$ }=0.04$ $\pm$ 0.01. Colour-magnitude filters used to isolate MS/evolved stars are shown as dotted lines in panels b) and d).
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{fig5.eps}\end{figure}$ Figure 5: Filled circles: differential-reddening corrected + colour-magnitude filtered radial density profiles (RDPs) of M 52 ( left panel) and NGC 3960 ( right panel). Dashed lines: two-parameter King profile where the core size is indicated. Shaded regions: stellar background level. For comparison purposes the RDPs prior to the colour-magnitude filtering are shown as empty circles.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{fig6.eps}\end{figure}$ Figure 6: Overall ( top panels), halo ( middle) and core ( bottom) mass functions of M 52 ( left panels) and NGC 3960 ( right). Dashed lines: fits with $\phi (m)\propto m^{-(1+\chi )}$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{fig7.eps}\end{figure}$ Figure 7: Relations involving structural parameters of OCs. Open circles: clusters more massive than 1000 $M_\odot$ . Squares with a dot: m<1000 $M_\odot$ . Dotted lines: least-squares fits to nearby clusters. Square: M 52. Triangle: NGC 3960. Shaded areas: $1\sigma$ borders of least-squares fits. Arrows indicate lower-limit estimates of mass, density and evolutionary parameter. Observed and extrapolated values of mass, density and evolutionary parameter of M 52 are shown. In panels d) and e) we show both determinations of $d_{\rm GC}$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{fig8.eps}\end{figure}$ Figure 8: Relations involving evolutionary parameters of open clusters. Symbols as in Fig. 7. Panels f) and i): fit of the linear-decay function $\chi (t)=\chi _{\rm o}-t/t_{\rm f}$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{fig1a.ps}\hspace*{-0.7mm} \includegraphics[width=8.4cm,clip]{fig1b.ps}\end{figure}$	Figure 1: $\rm 20\hbox {$^\prime $ }\times 20\hbox {$^\prime $ }$ XDSS R images of M 52 ( left panel) and NGC 3960 ( right panel).
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$\begin{figure} \par\includegraphics[width=4.5cm,clip]{fig2a.eps}\includegraphics[width=4.5cm,clip]{fig2b.eps}\end{figure}$	Figure 2: $\mbox{$J$ }\times\mbox{$(J-H)$ }$ CMDs of the central 10 $^\prime$ of M 52 ( left panel) and NGC 3960 ( right panel). Solid lines: fiducial lines used to derive the differential reddening (Sect. 3.1). Red stars belong mostly to the field (Sect. 3.2). Error bars are shown in the right panels of Fig. 4.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{fig5.eps}\end{figure}$	Figure 5: Filled circles: differential-reddening corrected + colour-magnitude filtered radial density profiles (RDPs) of M 52 ( left panel) and NGC 3960 ( right panel). Dashed lines: two-parameter King profile where the core size is indicated. Shaded regions: stellar background level. For comparison purposes the RDPs prior to the colour-magnitude filtering are shown as empty circles.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{fig6.eps}\end{figure}$	Figure 6: Overall ( top panels), halo ( middle) and core ( bottom) mass functions of M 52 ( left panels) and NGC 3960 ( right). Dashed lines: fits with $\phi (m)\propto m^{-(1+\chi )}$ .
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{fig8.eps}\end{figure}$	Figure 8: Relations involving evolutionary parameters of open clusters. Symbols as in Fig. 7. Panels f) and i): fit of the linear-decay function $\chi (t)=\chi _{\rm o}-t/t_{\rm f}$ .
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