All Figures

$\begin{figure} \par\includegraphics[width=18cm,clip]{3775fig1.ps} \end{figure}$ Figure 1: Negative image of the cluster NGC 6218 of 180 sec duration in the Bessell V band. North is up and East to the left. The field spans $3\hbox {$.\mkern -4mu^\prime $ }4$ on a side.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{3775fig2.ps} \end{figure}$ Figure 2: Colour-magnitude diagram of an area of $3\hbox {$.\mkern -4mu^\prime $ }4 \times 3\hbox {$.\mkern -4mu^\prime $ }4$ around the centre of NGC 6218.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{3775fig3.ps} \end{figure}$ Figure 3: Main sequence ridge line of NGC 6218 (solid curve) compared with the theoretical isochrones of Baraffe et al. (1997; dashed line) for an age of 10 Gyr and metallicity $[\rm M/H]=-1.0$ . The best fit of the isochrones to the observed MS requires a distance modulus (m-M)_V=14.23 and a colour excess E(B-V)=0.18, consistent with the most recent estimates of Hargis & Sandquist (2004).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3775fig4.ps} \end{figure}$ Figure 4: Individual CMDs of the four regions in which we have divided our NGC 6218 field.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3775fig5.ps} \end{figure}$ Figure 5: The squares are the LF of the four regions in NGC 6218, after correction for photometric incompleteness, as given in Table 4. The model LFs that best fit the data are shown as solid lines. The index of their corresponding power-law MF is, from bottom to top, $\alpha =1.4, 1.3, 0.6$ and 0.1. A positive index means that the number of stars decreases with mass. The MS stellar mass corresponding to the faintest data point of each LF is indicated, in units of ${M}_\odot$ .
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3775fig6.ps} \end{figure}$ Figure 6: Same LFs as those of Fig. 5, but here the solid lines show the LFs predicted by our multi-mass Michie-King model at various radii inside the cluster, starting from the same PGMF with index $\alpha = 0.1$ . The expected radial variation of the LF is fully consistent with the observations.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{3775fig7.ps} \end{figure}$ Figure 7: The surface brightness profile of NGC 6218 (crosses, from Trager et al. 1995) is well reproduced by our dynamical model (solid line). The observations are normalised to the central value of the best fitting profile (dashed line) as given by Trager et al. (1995).
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In the text

$\begin{figure} \par\includegraphics[width=18cm,clip]{3775fig1.ps} \end{figure}$	Figure 1: Negative image of the cluster NGC 6218 of 180 sec duration in the Bessell V band. North is up and East to the left. The field spans $3\hbox {$.\mkern -4mu^\prime $ }4$ on a side.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{3775fig2.ps} \end{figure}$	Figure 2: Colour-magnitude diagram of an area of $3\hbox {$.\mkern -4mu^\prime $ }4 \times 3\hbox {$.\mkern -4mu^\prime $ }4$ around the centre of NGC 6218.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{3775fig3.ps} \end{figure}$	Figure 3: Main sequence ridge line of NGC 6218 (solid curve) compared with the theoretical isochrones of Baraffe et al. (1997; dashed line) for an age of 10 Gyr and metallicity $[\rm M/H]=-1.0$ . The best fit of the isochrones to the observed MS requires a distance modulus (m-M)_V=14.23 and a colour excess E(B-V)=0.18, consistent with the most recent estimates of Hargis & Sandquist (2004).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3775fig4.ps} \end{figure}$	Figure 4: Individual CMDs of the four regions in which we have divided our NGC 6218 field.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{3775fig6.ps} \end{figure}$	Figure 6: Same LFs as those of Fig. 5, but here the solid lines show the LFs predicted by our multi-mass Michie-King model at various radii inside the cluster, starting from the same PGMF with index $\alpha = 0.1$ . The expected radial variation of the LF is fully consistent with the observations.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{3775fig7.ps} \end{figure}$	Figure 7: The surface brightness profile of NGC 6218 (crosses, from Trager et al. 1995) is well reproduced by our dynamical model (solid line). The observations are normalised to the central value of the best fitting profile (dashed line) as given by Trager et al. (1995).
Open with DEXTER