$\begin{figure} \par\includegraphics[width=7cm,clip]{4113fig1.ps}\end{figure}$ Figure 1: Distribution of the GSC-II fields (boxes) in equatorial coordinates. Lines show the location of the NGP, the galactic plane and the strips at $b = \pm 30^\circ$ and $b = +60^\circ$ .
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{4113fig2.eps} \end{figure}$ Figure 2: Final proper motion errors as a function of magnitude for one of the field towards the NGP included in this study.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{4113fig3a.eps}\hspace*{4mm} \includegraphics[width=7.5cm,clip]{4113fig3b.eps} \end{figure}$ Figure 3: Left panel: RPM diagram for a GSC-II region located towards the NGP. Stellar isochrones and WD cooling tracks are plotted with different lines (see text). Right panel: RPM diagram for all the candidates selected in the 1150 square degrees surveyed for this study. Dots show the unobserved targets, while triangles and asterisks are the spectroscopically confirmed WDs and contaminating (sub)dwarfs, respectively. Crosses indicate stars unclassified due to the low signal to noise of their spectra.
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In the text

$\begin{figure} \par\includegraphics[width=16.8cm,clip]{4113fig4.eps} \end{figure}$ Figure 4: Optical spectra. All the spectra are normalized at 5500 Å, shifted vertically from each other by arbitrary units, and ordered by increasing right ascension. Asterisks indicate spectra not fully calibrated, shown for classification only.
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In the text

$\begin{figure} \par\includegraphics[width=16.5cm,clip]{4113fig5.eps} \end{figure}$ Figure 5: Optical spectra. All the spectra are normalized at 5500 Å, shifted vertically from each other by arbitrary units, and ordered by increasing right ascension. Asterisks indicate spectra not fully calibrated, shown for classification only.
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In the text

$\begin{figure} \par\includegraphics[width=16.5cm,clip]{4113fig6.eps} \end{figure}$ Figure 6: Optical spectra. All the spectra are normalized at 5500 Å, shifted vertically from each other by arbitrary units, and ordered by increasing right ascension. Asterisks indicate spectra not fully calibrated, shown for classification only.
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{4113fig7.ps} \end{figure}$ Figure 7: Optical spectra of the peculiar WDs. Left panel shows GSC2U J 131147.2+292348 which is the coolest DQ with extremely strong C₂ bands. Right panel shows WD 1328+307 (G 165-7) which is a heavily blanketed DZ.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{4113fig1.ps}\end{figure}$	Figure 1: Distribution of the GSC-II fields (boxes) in equatorial coordinates. Lines show the location of the NGP, the galactic plane and the strips at $b = \pm 30^\circ$ and $b = +60^\circ$ .
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7cm,clip]{4113fig2.eps} \end{figure}$	Figure 2: Final proper motion errors as a function of magnitude for one of the field towards the NGP included in this study.
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$\begin{figure} \par\includegraphics[width=16.8cm,clip]{4113fig4.eps} \end{figure}$	Figure 4: Optical spectra. All the spectra are normalized at 5500 Å, shifted vertically from each other by arbitrary units, and ordered by increasing right ascension. Asterisks indicate spectra not fully calibrated, shown for classification only.
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$\begin{figure} \par\includegraphics[width=16.5cm,clip]{4113fig5.eps} \end{figure}$	Figure 5: Optical spectra. All the spectra are normalized at 5500 Å, shifted vertically from each other by arbitrary units, and ordered by increasing right ascension. Asterisks indicate spectra not fully calibrated, shown for classification only.
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$\begin{figure} \par\includegraphics[width=16.5cm,clip]{4113fig6.eps} \end{figure}$	Figure 6: Optical spectra. All the spectra are normalized at 5500 Å, shifted vertically from each other by arbitrary units, and ordered by increasing right ascension. Asterisks indicate spectra not fully calibrated, shown for classification only.
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$\begin{figure} \par\includegraphics[width=17cm,clip]{4113fig7.ps} \end{figure}$	Figure 7: Optical spectra of the peculiar WDs. Left panel shows GSC2U J 131147.2+292348 which is the coolest DQ with extremely strong C₂ bands. Right panel shows WD 1328+307 (G 165-7) which is a heavily blanketed DZ.
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