All Figures

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{5901fig1CMJN.eps}\end{figure}$ Figure 1: The complete FUSE spectrum of PG 1159-035 compared to our final model spectrum (black graph). The detected photospheric lines are identified. Labels in brackets denote lines that are visible in the model but not unambiguously seen in the observation. Overplotted is the same model but now attenuated by ISM absorption lines (grey graph; in the online version of this paper the graph is red). The ISM lines are not labeled. Photospheric model parameters are given in Table 7. In all figures of this paper the observed spectra are shifted such that the photospheric lines are located at rest wavelengths.
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In the text

$\begin{figure} \par\includegraphics[width=18cm]{5901fig2CMJN.eps}\end{figure}$ Figure 2: Similar to Fig. 1. Here we show the complete HST spectrum of PG 1159-035. In addition to the photospheric lines we also label the interstellar components of the resonance doublets from C IV and Si IV.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{5901fig3CMJN.eps}\end{figure}$ Figure 3: The O V 1371.30 Å line compared with two models with different effective temperatures.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{5901fig4.eps}\end{figure}$ Figure 4: Depth dependence of temperature, electron density, and ionisation fractions of all considered chemical elements in the final atmospheric model (for its parameters see Table 7).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{5901fig5CMJN.eps}\end{figure}$ Figure 5: The N V resonance doublet compared with two models with different nitrogen abundance. The model with N = 0.001 (mass fraction) fits the observed profiles very well. Note the weak blueshifted ISM components which are included in the model.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{5901fig6CMJN.eps}\end{figure}$ Figure 6: The photospheric Si IV resonance doublet is barely detectable while the ISM component (included in the model) is relatively strong. The two model profiles suggest that the silicon abundance is about 0.5 solar.
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In the text

$\begin{figure} \par\includegraphics[width=6.6cm,clip]{5901fig7CMJN.eps}\end{figure}$ Figure 7: Examples for newly discovered lines from highly ionised silicon (Si V-VI) compared with models with solar and 0.5 solar Si abundance.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{5901fig8CMJN.eps}\end{figure}$ Figure 8: The non-detection of the P V resonance doublet and the two model spectra suggest that the P abundance is at most solar.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{5901fig9CMJN.eps}\end{figure}$ Figure 9: The relative weakness of the S VI resonance doublet suggests a strongly subsolar sulfur abundance.
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In the text

$\begin{figure} \par\includegraphics[width=6.6cm,clip]{5901fig10CMJN.eps}\end{figure}$ Figure 10: Computed Fe VII lines (with solar and 0.1 solar Fe abundance) compared with observations. There is no clear evidence for the presence of iron lines in PG 1159-035. This suggests that iron is depleted and we estimate an upper abundance limit of 0.3 solar.
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In the text

$\begin{figure} \par\includegraphics[width=18cm]{5901fig2CMJN.eps}\end{figure}$	Figure 2: Similar to Fig. 1. Here we show the complete HST spectrum of PG 1159-035. In addition to the photospheric lines we also label the interstellar components of the resonance doublets from C IV and Si IV.
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$\begin{figure} \par\includegraphics[width=7.9cm,clip]{5901fig3CMJN.eps}\end{figure}$	Figure 3: The O V 1371.30 Å line compared with two models with different effective temperatures.
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$\begin{figure} \par\includegraphics[width=12cm,clip]{5901fig4.eps}\end{figure}$	Figure 4: Depth dependence of temperature, electron density, and ionisation fractions of all considered chemical elements in the final atmospheric model (for its parameters see Table 7).
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{5901fig5CMJN.eps}\end{figure}$	Figure 5: The N V resonance doublet compared with two models with different nitrogen abundance. The model with N = 0.001 (mass fraction) fits the observed profiles very well. Note the weak blueshifted ISM components which are included in the model.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{5901fig6CMJN.eps}\end{figure}$	Figure 6: The photospheric Si IV resonance doublet is barely detectable while the ISM component (included in the model) is relatively strong. The two model profiles suggest that the silicon abundance is about 0.5 solar.
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$\begin{figure} \par\includegraphics[width=6.6cm,clip]{5901fig7CMJN.eps}\end{figure}$	Figure 7: Examples for newly discovered lines from highly ionised silicon (Si V-VI) compared with models with solar and 0.5 solar Si abundance.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{5901fig8CMJN.eps}\end{figure}$	Figure 8: The non-detection of the P V resonance doublet and the two model spectra suggest that the P abundance is at most solar.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{5901fig9CMJN.eps}\end{figure}$	Figure 9: The relative weakness of the S VI resonance doublet suggests a strongly subsolar sulfur abundance.
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$\begin{figure} \par\includegraphics[width=6.6cm,clip]{5901fig10CMJN.eps}\end{figure}$	Figure 10: Computed Fe VII lines (with solar and 0.1 solar Fe abundance) compared with observations. There is no clear evidence for the presence of iron lines in PG 1159-035. This suggests that iron is depleted and we estimate an upper abundance limit of 0.3 solar.
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