All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{applot.ps} \end{figure}$ Figure 1: A plot showing the sky coverage of the Alpha Per study. The solid line represent the later POSSII fields while the dotted lines are the earlier POSSI fields. The dashed circles marks out a five degree radius from the cluster centre (marked by an $\times$ ).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{plplot.ps} \end{figure}$ Figure 2: A plot showing the sky coverage of the Pleiades study. The solid line represent the later POSSII fields while the dotted lines are the earlier POSSI fields. The dashed circles marks out a five degree radius from the cluster centre (marked by an $\times$ ).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{errplot.ps} \end{figure}$ Figure 3: A plot showing how the errors in the proper motion vary with magnitude. The larger errors for bright stars in the $\eta$ axis are an artifact of the the plate measuring process due to saturated images.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{APphot.ps} \end{figure}$ Figure 4: Comparing the photographic plate magnitudes with the measured photoelectric magnitudes for the Alpha Per data set. The line shown is a quartic fit to the data. The photoelectric data has been naturalised to the photographic passband system.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{PLphot.ps} \end{figure}$ Figure 5: Comparing the photographic plate magnitudes with the measured photoelectric magnitudes for the Pleiades data set. The line shown is a quartic fit to the data. Again the photoelectric data has been naturalised to the photographic passband system.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{aa0238f6.eps} \end{figure}$ Figure 6: A colour magnitude diagram for stars in the initial sample for Alpha Per. Only stars above the line shown were included in the proper motion survey. For symbols see text.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{aa0238f7.eps} \end{figure}$ Figure 7: A colour magnitude diagram for stars in the initial sample for the Pleiades. Only stars above the line shown were included in the proper motion survey. For symbols see text.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{prob.ps} \end{figure}$ Figure 8: Proper motion vector point diagrams and probability histograms for each magnitude interval in the Pleiades study. In each VPD the cluster is the group in the bottom right hand corner, separate from the field stars around the origin.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{APprob.ps} \end{figure}$ Figure 9: Proper motion vector point diagrams and probability histograms for each magnitude interval in the Alpha Per study. In each VPD the cluster is the group in the bottom right hand corner, separate from the field stars around the origin.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{comp1.ps} \end{figure}$ Figure 10: An estimate of the incompleteness of the study of Alpha Per. The line shown is a least squares fit.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{compPL.ps} \end{figure}$ Figure 11: An estimate of the incompleteness of the study of the Pleiades. The line shown is a least squares fit.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{cLF.ps} \end{figure}$ Figure 12: The Luminosity Function derived for Alpha Per.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{PLcLF.ps} \end{figure}$ Figure 13: The Luminosity Function derived for the Pleiades. The striking feature is the peak at R=16-17.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{mlplot.ps} \end{figure}$ Figure 14: The mass-luminosity relation used for Alpha Per. The line is a sixth degree polynomial fit.
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In the text

$\begin{figure} \par\includegraphics[width=6.9cm,clip]{APmlplot.ps} \end{figure}$ Figure 15: The mass-luminosity relation used for the Pleiades. The line is a sixth degree polynomial fit.
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In the text

$\begin{figure} \par\includegraphics[width=6.9cm,clip]{mfall.ps} \end{figure}$ Figure 16: The derived cluster Mass Function for the Pleiades. Note the increasingly shallow gradient towards lower masses. The line shown is a log normal fit to the data. The solid circles are data points from this survey while the crosses are from Hambly et al. (1999) and references therein.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{APmfall.ps} \end{figure}$ Figure 17: The derived cluster Mass Function for Alpha Per. The line show is a power law fit.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{mlerr.ps} \end{figure}$ Figure 18: A plot showing possible systematic errors in the mass luminosity relation used for the Pleiades.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{APcrosscat.ps} \end{figure}$ Figure 19: A histogram of the membership probabilities calculated in this study of Alpha Per for stars previously identified as candidate members.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{crosscat.ps} \end{figure}$ Figure 20: A histogram of the membership probabilities calculated in this study of the Pleiades for stars previously identified as candidate members.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{applot.ps} \end{figure}$	Figure 1: A plot showing the sky coverage of the Alpha Per study. The solid line represent the later POSSII fields while the dotted lines are the earlier POSSI fields. The dashed circles marks out a five degree radius from the cluster centre (marked by an $\times$ ).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{plplot.ps} \end{figure}$	Figure 2: A plot showing the sky coverage of the Pleiades study. The solid line represent the later POSSII fields while the dotted lines are the earlier POSSI fields. The dashed circles marks out a five degree radius from the cluster centre (marked by an $\times$ ).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{errplot.ps} \end{figure}$	Figure 3: A plot showing how the errors in the proper motion vary with magnitude. The larger errors for bright stars in the $\eta$ axis are an artifact of the the plate measuring process due to saturated images.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{APphot.ps} \end{figure}$	Figure 4: Comparing the photographic plate magnitudes with the measured photoelectric magnitudes for the Alpha Per data set. The line shown is a quartic fit to the data. The photoelectric data has been naturalised to the photographic passband system.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{PLphot.ps} \end{figure}$	Figure 5: Comparing the photographic plate magnitudes with the measured photoelectric magnitudes for the Pleiades data set. The line shown is a quartic fit to the data. Again the photoelectric data has been naturalised to the photographic passband system.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{aa0238f6.eps} \end{figure}$	Figure 6: A colour magnitude diagram for stars in the initial sample for Alpha Per. Only stars above the line shown were included in the proper motion survey. For symbols see text.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{aa0238f7.eps} \end{figure}$	Figure 7: A colour magnitude diagram for stars in the initial sample for the Pleiades. Only stars above the line shown were included in the proper motion survey. For symbols see text.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{prob.ps} \end{figure}$	Figure 8: Proper motion vector point diagrams and probability histograms for each magnitude interval in the Pleiades study. In each VPD the cluster is the group in the bottom right hand corner, separate from the field stars around the origin.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{APprob.ps} \end{figure}$	Figure 9: Proper motion vector point diagrams and probability histograms for each magnitude interval in the Alpha Per study. In each VPD the cluster is the group in the bottom right hand corner, separate from the field stars around the origin.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{comp1.ps} \end{figure}$	Figure 10: An estimate of the incompleteness of the study of Alpha Per. The line shown is a least squares fit.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{compPL.ps} \end{figure}$	Figure 11: An estimate of the incompleteness of the study of the Pleiades. The line shown is a least squares fit.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8cm,clip]{cLF.ps} \end{figure}$	Figure 12: The Luminosity Function derived for Alpha Per.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8cm,clip]{PLcLF.ps} \end{figure}$	Figure 13: The Luminosity Function derived for the Pleiades. The striking feature is the peak at R=16-17.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{mlplot.ps} \end{figure}$	Figure 14: The mass-luminosity relation used for Alpha Per. The line is a sixth degree polynomial fit.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=6.9cm,clip]{APmlplot.ps} \end{figure}$	Figure 15: The mass-luminosity relation used for the Pleiades. The line is a sixth degree polynomial fit.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=6.9cm,clip]{mfall.ps} \end{figure}$	Figure 16: The derived cluster Mass Function for the Pleiades. Note the increasingly shallow gradient towards lower masses. The line shown is a log normal fit to the data. The solid circles are data points from this survey while the crosses are from Hambly et al. (1999) and references therein.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{APmfall.ps} \end{figure}$	Figure 17: The derived cluster Mass Function for Alpha Per. The line show is a power law fit.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{mlerr.ps} \end{figure}$	Figure 18: A plot showing possible systematic errors in the mass luminosity relation used for the Pleiades.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{APcrosscat.ps} \end{figure}$	Figure 19: A histogram of the membership probabilities calculated in this study of Alpha Per for stars previously identified as candidate members.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{crosscat.ps} \end{figure}$	Figure 20: A histogram of the membership probabilities calculated in this study of the Pleiades for stars previously identified as candidate members.
Open with DEXTER