All Figures

$\begin{figure} \par\includegraphics[width=17.2cm,clip]{5685fig1.eps}\end{figure}$ Figure 1: I-, H- and K-band contour plots of IRAS 04158+2805. The contour lines are on the levels $I_{{\rm max}}\cdot 2^{-n}$ with $n=1,\dots ,9$ or 10 for the K-band image respectively.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{5685fig2.eps} \end{figure}$ Figure 2: X-ray spectrum of IRAS04158+2805 observed with Chandra.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{5685fig3.eps}\end{figure}$ Figure 3: Modeled SED (dashed line) compared to observed fluxes: IRS spectrum (solid line); Strom & Strom (1994, squares); Kenyon et al. (1990) and Kenyon & Hartmann (1995, circles); Luhman & Rieke (1998) and Luhman (2000, crosses); Motte & André (2001, diamonds); this paper, see Sect. 3.2 (triangle). The error bars of the photometric fluxes are smaller than their symbols and therefore not drawn.
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In the text

$\begin{figure} \par\includegraphics[width=17.4cm,clip]{5685fig4.eps}\end{figure}$ Figure 4: Polarisation maps of the observed ( left panel) and modelled ( middle panel) nebula. The vector length for 100% polarisation is indicated by the bar in the lower right corner. Right panel: comparison of the polarisation level as a function of position in the observed (solid) and modelled (dashed) nebula. These curves are estimated along the ridges (black curves) and symmetry axis (gray) of the nebula.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{5685fig5.eps}\end{figure}$ Figure 5: Definition of geometrical observables w, a, b, c and $\delta$ . The contour lines are shown for the levels $I_{{\rm max}}\cdot 2^{-n}$ $n=1\dots 10$ . The two ridges and the symmetry axis are drawn as dashed lines. Their intersection points with the contour lines of the flux level $I=I_{{\rm max}}\cdot 2^{-8}$ are shown as boxes and $I=1\cdot \sigma _{\rm noise}$ as circles, respectively. The counter nebula peak is shown as a star.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{5685fig6.eps}\end{figure}$ Figure 6: Examples of projections of f² (Eq. (4)) to different model parameter planes. The contour is plotted in a logarithmic scale. White areas correspond to minimal values of f². The colour range is identical in all four plots. The black cross shows the location of the best model, after the SED fitting.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{5685fig7.eps}\end{figure}$ Figure 7: Comparison between observations ( left) and best fitting model ( mid, see Table 2) in I-band ( top), H-band ( middle) and K-band ( bottom). For demonstration purposes, the right column shows the images of the best fitting model but with doubled dust disc mass ( $3\times 10^{-4}~M_\odot$ ).
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{5685fig8.eps}\end{figure}$ Figure 8: Difference of observed and modelled polarisation percentage ( top) and polarisation direction ( bottom) along the ridges (black) and the symmetry line (grey).
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In the text

$\begin{figure} \par\includegraphics[width=17.2cm,clip]{5685fig1.eps}\end{figure}$	Figure 1: I-, H- and K-band contour plots of IRAS 04158+2805. The contour lines are on the levels $I_{{\rm max}}\cdot 2^{-n}$ with $n=1,\dots ,9$ or 10 for the K-band image respectively.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{5685fig2.eps} \end{figure}$	Figure 2: X-ray spectrum of IRAS04158+2805 observed with Chandra.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{5685fig6.eps}\end{figure}$	Figure 6: Examples of projections of f² (Eq. (4)) to different model parameter planes. The contour is plotted in a logarithmic scale. White areas correspond to minimal values of f². The colour range is identical in all four plots. The black cross shows the location of the best model, after the SED fitting.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{5685fig7.eps}\end{figure}$	Figure 7: Comparison between observations ( left) and best fitting model ( mid, see Table 2) in I-band ( top), H-band ( middle) and K-band ( bottom). For demonstration purposes, the right column shows the images of the best fitting model but with doubled dust disc mass ( $3\times 10^{-4}~M_\odot$ ).
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{5685fig8.eps}\end{figure}$	Figure 8: Difference of observed and modelled polarisation percentage ( top) and polarisation direction ( bottom) along the ridges (black) and the symmetry line (grey).
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