All Figures

$\begin{figure} \par\includegraphics[width=17.2cm,clip]{fig01.eps}\end{figure}$ Figure 1: A portion of the FUSE spectrum of Sk -68 80 in the wavelength range between 1015 and 1040 Å. Interstellar atomic absorption lines are labeled above the spectrum. The unlabeled tic marks indicate interstellar H₂ absorption lines from the Lyman and Werner bands.
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In the text

$\begin{figure} \par\includegraphics[width=5cm,clip]{fig02.eps}\end{figure}$ Figure 2: Atomic absorption profiles from O I, Fe II, P II, and C I in the direction of Sk -68 80, plotted against LSR velocity. Galactic IVC and HVC absorption occurs near +50 km s^-1 and +120 km s^-1(dotted lines), respectively. Local disk gas is seen at velocities <40 km s^-1; absorption from LMC gas occurs at velocities >160 km s^-1. Blending lines are labeled within the plot.
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In the text

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{fig03.eps}\end{figure}$ Figure 3: Curves of growth (COG) for atomic and molecular absorption in the IVC towards Sk -68 80. Atomic absorption lines (identified in the upper left corner) fit on a curve of growth with b=5.9^+2.8_-1.3 km s^-1. Molecular hydrogen lines (identified in the lower right corner) fit on a COG with a much lower b value of 1.5^+0.8_-0.2 km s^-1. Typical error bars for the data points in the different regions of the COG are shown on the left hand side.
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In the text

$\begin{figure} \par\includegraphics[width=15.4cm,clip]{fig04.eps}\end{figure}$ Figure 4: Selection of normalized H₂ absorption profiles towards Sk -68 80. The dotted lines indicate H₂ absorption by intermediate-velocity halo gas near +50 km s^-1and possibly high-velocity halo gas near +120 km s^-1(5 cases). H₂ absorption from local Galactic gas occurs near 0 km s^-1. Blends of other lines and their components are also labeled.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{fig05.eps}\end{figure}$ Figure 5: Rotational excitation of the H₂ gas in the IVC towards Sk -68 80. The two lowest rotational states (J=0,1) can be fitted to an equivalent Boltzmann temperature of $T_{01}=51\pm 11$ K, while the higher rotational states (J=2-4) fit to a temperature of $T_{24}=532\pm 124$ K.
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In the text

$\begin{figure} \par\includegraphics[width=5cm,clip]{fig06.eps}\end{figure}$ Figure A.1: Atomic and H₂ absorption profiles in direction of Sk -68 82. The strong Fe II line (upper panel) suggests a very similar component strucutre as for Sk -68 80. In contrast to Sk -68 80 (see Fig. 2), C I absorption is present in the HVC component. Weak molecular hydrogen absorption is present at IVC and HVC velocities, but the individual H₂ line profiles have very irregular shapes due to small-scale structure in the continuum flux at wavelengths between 1000 and 1080 Å. A cumulative H₂ profile from a co-addition of 15 lines is presented in the lower-most panel.

In the text

$\begin{figure} \par\includegraphics[width=17.2cm,clip]{fig01.eps}\end{figure}$	Figure 1: A portion of the FUSE spectrum of Sk -68 80 in the wavelength range between 1015 and 1040 Å. Interstellar atomic absorption lines are labeled above the spectrum. The unlabeled tic marks indicate interstellar H₂ absorption lines from the Lyman and Werner bands.
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$\begin{figure} \par\includegraphics[width=5cm,clip]{fig02.eps}\end{figure}$	Figure 2: Atomic absorption profiles from O I, Fe II, P II, and C I in the direction of Sk -68 80, plotted against LSR velocity. Galactic IVC and HVC absorption occurs near +50 km s^-1 and +120 km s^-1(dotted lines), respectively. Local disk gas is seen at velocities <40 km s^-1; absorption from LMC gas occurs at velocities >160 km s^-1. Blending lines are labeled within the plot.
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$\begin{figure} \par\includegraphics[width=15.4cm,clip]{fig04.eps}\end{figure}$	Figure 4: Selection of normalized H₂ absorption profiles towards Sk -68 80. The dotted lines indicate H₂ absorption by intermediate-velocity halo gas near +50 km s^-1and possibly high-velocity halo gas near +120 km s^-1(5 cases). H₂ absorption from local Galactic gas occurs near 0 km s^-1. Blends of other lines and their components are also labeled.
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$\begin{figure} \par\includegraphics[width=7.2cm,clip]{fig05.eps}\end{figure}$	Figure 5: Rotational excitation of the H₂ gas in the IVC towards Sk -68 80. The two lowest rotational states (J=0,1) can be fitted to an equivalent Boltzmann temperature of $T_{01}=51\pm 11$ K, while the higher rotational states (J=2-4) fit to a temperature of $T_{24}=532\pm 124$ K.
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