All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0853fig1.eps} \end{figure}$ Figure 1: SHASSA field #214. PG 1034+001 is marked by a circle. East is left and North is up. The field size is about 13 $^\circ$ $\times$ 13 $^\circ$ with a pixel size of 0 $.\mkern -4mu^\prime$ 8. Note the elliptic emission structure lying from SSE to NW, most prominent on the NE side. The diameter is about 6 $^\circ$ $\times$ 9 $^\circ$ . A second emission structure further outside can be seen to the NE.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0853fig2.eps} \end{figure}$ Figure 2: Position of PG 1034+001 and related objects in the $\log \mbox{$T_{\rm eff}$ }{-} \mbox{$\log g$ }$ plane compared with evolutionary tracks (labeled with the respective stellar masses in $M_\odot$ ) of born-again post-AGB stars (Blöcker 1995). The ellipse shows the error range in the spectral analysis of Werner et al. (1995).
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In the text

$\begin{figure} \par\includegraphics[width=8.7cm,clip]{0853fig3.eps} \end{figure}$ Figure 3: Galactic orbit of PG 1034+001. $\rho$ ist the distance from the Galactic Center, z is the distance perpendicular to the disk.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0853fig2.eps} \end{figure}$	Figure 2: Position of PG 1034+001 and related objects in the $\log \mbox{$T_{\rm eff}$ }{-} \mbox{$\log g$ }$ plane compared with evolutionary tracks (labeled with the respective stellar masses in $M_\odot$ ) of born-again post-AGB stars (Blöcker 1995). The ellipse shows the error range in the spectral analysis of Werner et al. (1995).
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$\begin{figure} \par\includegraphics[width=8.7cm,clip]{0853fig3.eps} \end{figure}$	Figure 3: Galactic orbit of PG 1034+001. $\rho$ ist the distance from the Galactic Center, z is the distance perpendicular to the disk.
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