All Figures

$\begin{figure} \par\includegraphics[width=5cm,clip]{3448fig1.eps} \end{figure}$ Figure 1: P II $\lambda$ 1533 absorption line profile toward HD 93222. Three components are easily identified. When detected, Cl I, C I, and S I lines are used to constrain the velocity distribution (turbulent velocity and radial velocity). P II and O I lines have very similar optical depths since the $N \cdot f$ product is approximately the same (see text).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7cm,clip]{3448fig2.ps} \end{figure}$ Figure 2: The P II $\lambda$ 1125 line toward HD 93222 as observed with FUSE ( top) and of the $\lambda$ 1533 line as observed with STIS ( bottom). The two lines have approximately the same oscillator strength. Given the relatively low spectral resolution, the FUSE observation allow us to calculate the integrated column density along the sightline while the STIS observation gives the possibility to investigate column densities of each component.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=6cm,clip]{3448fig3.ps} \end{figure}$ Figure 3: The P II column density integrated over each sightline versus the total hydrogen column density defined as $\log [N({\rm H~{\sc i}}) + 2 \times N({\rm H}_2)]$ . The thick line shows the solar phosphorus abundance (Asplund et al. 2004) and the thin dashed line shows the regression fit.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=6cm,clip]{3448fig4.ps} \end{figure}$ Figure 4: P II total column density over each sightline is plotted versus the total O I column density. The thick line shows the solar ratio (Asplund et al. 2004) and the thin dashed line shows the regression fit.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=6cm,clip]{3448fig5.ps} \end{figure}$ Figure 5: P II column density of each individual component along the sightlines plotted against the corresponding O I column density. The thick line shows the solar ratio (Asplund et al. 2004) and the thin dashed line shows the regression fit.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=13cm,clip]{3448fig6.ps} \end{figure}$ Figure 6: Compiled measurements of P II and O I column densities found in the literature (see Table 6) overplotted on our results. Empty circles represent sightlines toward stars with distances less than 200 pc. Filled circles represent the values of this study (results plotted in Fig. 5 toward stars between $\approx$ 400 and $\approx$ 5000 pc), and diamonds represent values found in the literature toward stars with comparable distances. Finally, triangles show measures in the extragalactic ISM. The thick line represent the solar P/O proportion (Asplund et al. 2004).
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In the text

$\begin{figure} \par\includegraphics[width=5cm,clip]{3448fig1.eps} \end{figure}$	Figure 1: P II $\lambda$ 1533 absorption line profile toward HD 93222. Three components are easily identified. When detected, Cl I, C I, and S I lines are used to constrain the velocity distribution (turbulent velocity and radial velocity). P II and O I lines have very similar optical depths since the $N \cdot f$ product is approximately the same (see text).
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$\begin{figure} \par\includegraphics[angle=-90,width=6cm,clip]{3448fig3.ps} \end{figure}$	Figure 3: The P II column density integrated over each sightline versus the total hydrogen column density defined as $\log [N({\rm H~{\sc i}}) + 2 \times N({\rm H}_2)]$ . The thick line shows the solar phosphorus abundance (Asplund et al. 2004) and the thin dashed line shows the regression fit.
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$\begin{figure} \par\includegraphics[angle=-90,width=6cm,clip]{3448fig4.ps} \end{figure}$	Figure 4: P II total column density over each sightline is plotted versus the total O I column density. The thick line shows the solar ratio (Asplund et al. 2004) and the thin dashed line shows the regression fit.
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$\begin{figure} \par\includegraphics[angle=-90,width=6cm,clip]{3448fig5.ps} \end{figure}$	Figure 5: P II column density of each individual component along the sightlines plotted against the corresponding O I column density. The thick line shows the solar ratio (Asplund et al. 2004) and the thin dashed line shows the regression fit.
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