$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{0629cosm_H3p.ps}\end{figure}$ Figure 1: Calculated column density (cm^-2) of H₃⁺ as a function of ${\zeta }$ for diffuse-phase models in which $n_{\rm H}$ = 100 cm^-3 and $\chi$ = 2. The horizontal value is that observed for ${\zeta }$ Persei.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{0629cosm_Hp.ps}\end{figure}$ Figure 2: Calculated column density (cm^-2) of H⁺ as a function of ${\zeta }$ for diffuse-phase models in which $n_{\rm H}$ = 100 cm^-3 and $\chi$ = 2.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{0629cosm_C.ps}\end{figure}$ Figure 3: Calculated column density (cm^-2) of N(C) as a function of ${\zeta }$ for diffuse-phase models in which $n_{\rm H}$ = 100 cm^-3 and $\chi$ = 2. The horizontal values are the observed limits for ${\zeta }$ Persei.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{0629cosm_OH.ps}\end{figure}$ Figure 4: Calculated column density (cm^-2) of OH as a function of ${\zeta }$ for diffuse-phase models in which $n_{\rm H}$ = 100 cm^-3, and $\chi$ = 2. The horizontal value is that observed for ${\zeta }$ Persei.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{0629cosm_HD.ps}\end{figure}$ Figure 5: Calculated column density (cm^-2) of HD as a function of ${\zeta }$ for models in which $n_{\rm H}$ = 100 cm^-3 and $\chi$ = 2. The horizontal values are the lower and upper limits to the observed values for ${\zeta }$ Persei.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{0629cosm_H3p.ps}\end{figure}$	Figure 1: Calculated column density (cm^-2) of H₃⁺ as a function of ${\zeta }$ for diffuse-phase models in which $n_{\rm H}$ = 100 cm^-3 and $\chi$ = 2. The horizontal value is that observed for ${\zeta }$ Persei.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{0629cosm_Hp.ps}\end{figure}$	Figure 2: Calculated column density (cm^-2) of H⁺ as a function of ${\zeta }$ for diffuse-phase models in which $n_{\rm H}$ = 100 cm^-3 and $\chi$ = 2.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{0629cosm_C.ps}\end{figure}$	Figure 3: Calculated column density (cm^-2) of N(C) as a function of ${\zeta }$ for diffuse-phase models in which $n_{\rm H}$ = 100 cm^-3 and $\chi$ = 2. The horizontal values are the observed limits for ${\zeta }$ Persei.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{0629cosm_OH.ps}\end{figure}$	Figure 4: Calculated column density (cm^-2) of OH as a function of ${\zeta }$ for diffuse-phase models in which $n_{\rm H}$ = 100 cm^-3, and $\chi$ = 2. The horizontal value is that observed for ${\zeta }$ Persei.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{0629cosm_HD.ps}\end{figure}$	Figure 5: Calculated column density (cm^-2) of HD as a function of ${\zeta }$ for models in which $n_{\rm H}$ = 100 cm^-3 and $\chi$ = 2. The horizontal values are the lower and upper limits to the observed values for ${\zeta }$ Persei.
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