$\begin{figure} \par\resizebox{8.6cm}{!}{\includegraphics{2002fig1.ps}} \end{figure}$ Figure 1: The regions in the colour-colour diagram within which objects were deemed to be M, L or T dwarfs.
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In the text

$\begin{figure} \par\resizebox{8.6cm}{!}{\includegraphics{2002fig2.ps}} \end{figure}$ Figure 2: The relative positional errors between SuperCOSMOS and 2MASS. The solid line represents the errors in Right Ascension while the dotted line shows those in Declination.
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In the text

$\begin{figure} \par\resizebox{11.6cm}{!}{\includegraphics{2002fig3.ps}}\end{figure}$ Figure 3: A two colour diagram for all the objects found in the survey. The star symbols represent new discoveries while the solid circles are previously known objects.
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In the text

$\begin{figure} \par\resizebox{14cm}{!}{\includegraphics[scale=0.9]{2002fig4.ps}}\end{figure}$ Figure 4: Histograms showing the magnitude (J) and colour (I-J) of both the newly discovered and previously discovered objects.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{2002fig5.ps}}\end{figure}$ Figure 5: The normalized spectrum of SIPS1259-4336 ( top) along with that of an A0 standard star. The potassium doublet at 1.25 microns can clearly be seen.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{2002fig6.ps}}\end{figure}$ Figure 6: The deviation from the proper motion in RA and Dec plotted against time. The line shown is the path of parallax motion predicted by the astrometric solution.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{2002fig7.ps}}\end{figure}$ Figure 7: The parallax ellipse traced out by SIPS1259-4336; the dotted lines represent one sigma upper and lower limits on the parallax.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{2002fig8.ps}}\end{figure}$ Figure 8: Comparison of the fitted parallax and proper motions for the reference stars with SIPS1259-4336.
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In the text

$\begin{figure} \par\resizebox{12.5cm}{!}{\includegraphics{2002fg10.ps}}\end{figure}$ Figure 10: The areal completeness of the survey. The scale shows the probability that an area is free from both crowding and bright stars. The solid lines marked represent the galactic latitude cut.
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In the text

$\begin{figure} \par\resizebox{8.6cm}{!}{\includegraphics{2002fig1.ps}} \end{figure}$	Figure 1: The regions in the colour-colour diagram within which objects were deemed to be M, L or T dwarfs.
Open with DEXTER

$\begin{figure} \par\resizebox{8.6cm}{!}{\includegraphics{2002fig2.ps}} \end{figure}$	Figure 2: The relative positional errors between SuperCOSMOS and 2MASS. The solid line represents the errors in Right Ascension while the dotted line shows those in Declination.
Open with DEXTER

$\begin{figure} \par\resizebox{11.6cm}{!}{\includegraphics{2002fig3.ps}}\end{figure}$	Figure 3: A two colour diagram for all the objects found in the survey. The star symbols represent new discoveries while the solid circles are previously known objects.
Open with DEXTER

$\begin{figure} \par\resizebox{14cm}{!}{\includegraphics[scale=0.9]{2002fig4.ps}}\end{figure}$	Figure 4: Histograms showing the magnitude (J) and colour (I-J) of both the newly discovered and previously discovered objects.
Open with DEXTER

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{2002fig5.ps}}\end{figure}$	Figure 5: The normalized spectrum of SIPS1259-4336 ( top) along with that of an A0 standard star. The potassium doublet at 1.25 microns can clearly be seen.
Open with DEXTER

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{2002fig6.ps}}\end{figure}$	Figure 6: The deviation from the proper motion in RA and Dec plotted against time. The line shown is the path of parallax motion predicted by the astrometric solution.
Open with DEXTER

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{2002fig7.ps}}\end{figure}$	Figure 7: The parallax ellipse traced out by SIPS1259-4336; the dotted lines represent one sigma upper and lower limits on the parallax.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{2002fig8.ps}}\end{figure}$	Figure 8: Comparison of the fitted parallax and proper motions for the reference stars with SIPS1259-4336.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{2002fig9.ps}} \end{figure}$	Figure 9: The probability of detection plotted against the number of 2MASS images per square arc minute.
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$\begin{figure} \par\resizebox{12.5cm}{!}{\includegraphics{2002fg10.ps}}\end{figure}$	Figure 10: The areal completeness of the survey. The scale shows the probability that an area is free from both crowding and bright stars. The solid lines marked represent the galactic latitude cut.
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$\begin{figure} \par\resizebox{14cm}{!}{\includegraphics[scale=0.9]{2002fg11.ps}}\end{figure}$	Figure 11: The number of Luyten objects that could possibly be detected (grey) and those that were (solid).
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