All Figures

$\begin{figure} \par\includegraphics[width=13.4cm,clip]{0355fig1.eps} \end{figure}$ Figure 1: Normalised spectra of our sample of white dwarfs in the region of the Balmer series. When more than one sequence of exposures was available for a white dwarf, the average spectrum is presented. The positions of the Balmer lines are indicated. The spectra are displaced vertically by 0.7 units (or multiples thereof) for a better visualisation.
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In the text

$\begin{figure} \par\includegraphics[width=13.9cm,clip]{0355fig2.eps} \end{figure}$ Figure 2: Circular polarisation spectra (V/I) of our sample of white dwarfs in the region of the Balmer series. The average (V/I)-spectrum is plotted for multiple observations. For all spectra a horizontal line is drawn to indicate the zero level. Dashed vertical lines represent the positions where the Balmer lines are located. Spectra are displaced with relative shifts for a better visualisation.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0355fig3.eps} \end{figure}$ Figure 3: Circular polarisation spectra (V/I) of WD 0446-789 (average of observations from 30/11/03 and 28/01/03, thin solid line) in the region of H $\beta$ ( top), H $\gamma$ ( middle) and close to the Balmer jump ( bottom panel). The solid horizontal line indicates the zero level. The horizonal dashed lines indicate the position of the $1\sigma$ level of the average (V/I) spectrum. The light shading (cyan in the electronic version) represents the variation between (V/I) spectra predicted by the low-field approximation (Eq. (2)) using magnetic field values of $4283\pm 640$ G (thick solid line, red in the electronic version).
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{0355fig4.eps} \end{figure}$ Figure 4: As in Fig. 3 but for WD 2359-434 (average of observations from 04/11/03 and 29/11/03), where the best fit is at $\langle B_z\rangle=-3138\pm422$ G.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0355fig5.eps} \end{figure}$ Figure 5: As in Fig. 3 but for the 09/01/03 observation of the white dwarf WD 1105-048 where the best fit is at $\langle B_z\rangle=-3959\pm710$ G.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{0355fig6.eps} \end{figure}$ Figure 6: Artificial polarisation spectrum with the same noise level as WD 0446-789 plotted in Fig. 3. For this particular example, out of the 1000 simulations, the fitting procedure results in $\langle B_z\rangle=4449\pm449$ G.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{0355fig7.ps} \end{figure}$ Figure 7: Model atmosphere fit (solid line) of the 30/11/02 observation of WD 0446-789 (solid histogram). The dashed model profile for H $\delta$ indicates that this line was not used during the fitting procedure.
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In the text

$\begin{figure} \par\includegraphics[width=13.4cm,clip]{0355fig1.eps} \end{figure}$	Figure 1: Normalised spectra of our sample of white dwarfs in the region of the Balmer series. When more than one sequence of exposures was available for a white dwarf, the average spectrum is presented. The positions of the Balmer lines are indicated. The spectra are displaced vertically by 0.7 units (or multiples thereof) for a better visualisation.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{0355fig4.eps} \end{figure}$	Figure 4: As in Fig. 3 but for WD 2359-434 (average of observations from 04/11/03 and 29/11/03), where the best fit is at $\langle B_z\rangle=-3138\pm422$ G.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0355fig5.eps} \end{figure}$	Figure 5: As in Fig. 3 but for the 09/01/03 observation of the white dwarf WD 1105-048 where the best fit is at $\langle B_z\rangle=-3959\pm710$ G.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{0355fig6.eps} \end{figure}$	Figure 6: Artificial polarisation spectrum with the same noise level as WD 0446-789 plotted in Fig. 3. For this particular example, out of the 1000 simulations, the fitting procedure results in $\langle B_z\rangle=4449\pm449$ G.
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$\begin{figure} \par\includegraphics[width=7.4cm,clip]{0355fig7.ps} \end{figure}$	Figure 7: Model atmosphere fit (solid line) of the 30/11/02 observation of WD 0446-789 (solid histogram). The dashed model profile for H $\delta$ indicates that this line was not used during the fitting procedure.
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