All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=15.8cm,clip]{H4204F1.ps} \end{figure}$ Figure 1: Upper panel: observed FUSE spectrum of NGC 7469 with 0.05 Å binning. Lower panel: the FUSE spectrum corrected for foreground interstellar absorption. Identified broad emission lines are marked.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{H4204F2.ps} \end{figure}$ Figure 2: FUSE spectrum of NGC 7469 (with 0.05 Å bins) in the Ly $\beta$ /O VI region is shown as the thin black line. The overlayed color lines show the best fit (model A) as described in the text. The thin green line represents the fitted continuum and emission components. The thin red line shows the fitted intrinsic absorption components. The thin blue line shows the foreground Galactic absorption lines. The light blue lines illustrate the continuum and narrow O VI line profiles for the two extreme cases we considered, models D and E, which have no narrow line emission, or 2:1 narrow-line emission that is not absorbed, respectively. The intrinsic absorbing gas is readily visible as two separate complexes outlined in red. Corresponding absorption in Ly $\beta$ is weak at best.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.5cm,clip]{H4204F3.ps} \end{figure}$ Figure 3: The normalized line profiles in the upper panels show intrinsic O VI $\lambda 1032$ (the solid blue line) and O VI $\lambda 1038$ (the solid red line) absorbing components 1 and 2. These data are binned at 0.05 Å, and foreground Galactic absorption features have been divided out. The normalized profiles in the lower panels show the corresponding location in velocity space of expected Ly $\beta$ absorption, which is not definitively detected. Representative error bars at the velocity centroid of each component are shown.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{H4204F4.ps} \end{figure}$ Figure 4: Spectral energy distributions used for photoionization models of absorbing gas in NGC 7469. SED1, based on Kriss et al. (2000), is the solid line. SED2, based on the spectrum in this paper, is the dashed line. The curves are normalized so that SED2 matches the extinction-corrected flux at 1000 Å in the FUSE spectrum. The points with error bars showing the UV and X-ray fluxes as observed with XMM-Newton are consistent with SED2.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=15.8cm,clip]{H4204F1.ps} \end{figure}$	Figure 1: Upper panel: observed FUSE spectrum of NGC 7469 with 0.05 Å binning. Lower panel: the FUSE spectrum corrected for foreground interstellar absorption. Identified broad emission lines are marked.
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