All Figures

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{0669fig1.ps} \end{figure}$ Figure 1: The Pleiades mass function. The open triangles are from the Prosser and Stauffer Open Cluster Database and the filled circles are the data points from Moraux et al. (2003). The open squares have been obtained by applying the empirical magnitude-mass relation given by Dobbie et al. (2002). The log-normal fit (Eq. (2)) found by Moraux et al. (2003) is shown as a solid line.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{0669fig2.ps} \end{figure}$ Figure 2: Comparison of the log-normal fit of the observed Pleiades MF (shown as a solid line) to the model MFs. The dashed (dotted) histogram represents the system mass function at an age of 100 Myr from model A (B) of KAH for all systems within $R\le 15$ pc of the model cluster center. They have been scaled to match the Pleiades data around $m\simeq 1~M_{\odot}$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{0669fig3.ps} \end{figure}$ Figure 3: The single object mass function for model A (dashed histogram) and model B (dotted histogram) at t=100 Myr and $R\le 15$ pc. The shaded region represents the field mass function from Chabrier (2003) with uncertainties. The dots correspond to the shape of the standard three-part power-law IMF. All models are scaled to agree between $0.5~M_{\odot}$ and $1~M_{\odot}$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0669fig4.ps} \end{figure}$ Figure 4: Ratio of the number of systems within $R\le 2$ pc to the total number of cluster systems ( $R\le 15$ pc) per mass bin at t=100 Myr. The solid line corresponds to model A and the dashed line to model B. The stellar data points are from the observational survey of Pinfield et al. (1998) and the sub-stellar one is from Moraux et al. (2003) (filled circles).
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0669fig5.ps} \end{figure}$ Figure 5: Fraction of individual objects remaining inside the cluster ( $R\le 15$ pc) at t=100 Myr compared to the initial number of objects at t=0. The solid line corresponds to model A and the dashed line to model B. The ratio of the individual object MFs is shown, not of the system MFs.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{0669fig1.ps} \end{figure}$	Figure 1: The Pleiades mass function. The open triangles are from the Prosser and Stauffer Open Cluster Database and the filled circles are the data points from Moraux et al. (2003). The open squares have been obtained by applying the empirical magnitude-mass relation given by Dobbie et al. (2002). The log-normal fit (Eq. (2)) found by Moraux et al. (2003) is shown as a solid line.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{0669fig2.ps} \end{figure}$	Figure 2: Comparison of the log-normal fit of the observed Pleiades MF (shown as a solid line) to the model MFs. The dashed (dotted) histogram represents the system mass function at an age of 100 Myr from model A (B) of KAH for all systems within $R\le 15$ pc of the model cluster center. They have been scaled to match the Pleiades data around $m\simeq 1~M_{\odot}$ .
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{0669fig3.ps} \end{figure}$	Figure 3: The single object mass function for model A (dashed histogram) and model B (dotted histogram) at t=100 Myr and $R\le 15$ pc. The shaded region represents the field mass function from Chabrier (2003) with uncertainties. The dots correspond to the shape of the standard three-part power-law IMF. All models are scaled to agree between $0.5~M_{\odot}$ and $1~M_{\odot}$ .
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0669fig4.ps} \end{figure}$	Figure 4: Ratio of the number of systems within $R\le 2$ pc to the total number of cluster systems ( $R\le 15$ pc) per mass bin at t=100 Myr. The solid line corresponds to model A and the dashed line to model B. The stellar data points are from the observational survey of Pinfield et al. (1998) and the sub-stellar one is from Moraux et al. (2003) (filled circles).
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0669fig5.ps} \end{figure}$	Figure 5: Fraction of individual objects remaining inside the cluster ( $R\le 15$ pc) at t=100 Myr compared to the initial number of objects at t=0. The solid line corresponds to model A and the dashed line to model B. The ratio of the individual object MFs is shown, not of the system MFs.
Open with DEXTER