All Figures

$\begin{figure} \par {\includegraphics[angle=90,width=7.3cm,clip]{0050fig1.ps} } \end{figure}$ Figure 1: Correspondence between the location and extent of the slit for each position in $\mu \equiv \cos \theta$ and the angle on the sky along the observations line from the center of the disk $\omega \equiv \Omega \sin \theta$ , where $\Omega$ is the solar angular radius which is assumed to be 959.5 arcsec. The positionsof the center of the slit are marked with asterisks. For position # 6, part of the slit was outside the solar disk; the center of the illuminated part of the slit is located at the tip of the arrow, and the right limit is marked with a vertical line at $\omega = \Omega$ .
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In the text

$\begin{figure} \par {\includegraphics[angle=90,width=7.3cm,clip]{0050fig2.ps} } \end{figure}$ Figure 2: Contour plot showing the reduced $\chi ^2$ , normalized to unity at its minimum, as a function of the relative resolving power and the amount of scattered light for the $\mu =1$ setup centered around the Ca I $\lambda 6162$ line.
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In the text

$\begin{figure} \par {\includegraphics[angle=90,width=7.6cm,clip]{0050fig3.ps} } \end{figure}$ Figure 3: Comparison of the spectra at the center of the disk in the region around Ca I $\lambda 6162.2$ from Brault & Neckel (1987; convolved with a Gaussian; solid line) and the Gregory Coudé Telescope (after removal of scattered light; filled circles).
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In the text

$\begin{figure} \par {\includegraphics[width=5.8cm,angle=90,clip]{0050fig4a.ps} } {\includegraphics[width=6cm,angle=90,clip]{0050fig4b.ps} } \end{figure}$ Figure 4: Center (filled circles) and limb (solid) spectra in the region around Ca I $\lambda 6162.2$ ( top panel) and around Co I $\lambda 5301.0$ ( bottom panel).
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In the text

$\begin{figure} \par {\includegraphics[angle=90,width=7.7cm,clip]{0050fig5.ps} } \end{figure}$ Figure 5: Response functions to the temperature at $\mu =0.32$ and 1.00 for the core of the lines of the O I infrared triplet (solid) and the Na I $\lambda 6160.8$ (dashed) lines.
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In the text

$\begin{figure} \par\mbox{\includegraphics[height=6.8cm,width=4.5cm,angle=90,clip... ...udegraphics[height=6.1cm,width=4.4cm,angle=90,clip]{0050fig6d.ps} } \end{figure}$ Figure 6: Center (at rest with the continuum normalized to 1) and limb (shifted to the red with the continuum normalized to 1 and subtracted 0.05) spectra for the O I infrared triplet lines. Observations (filled circles) and calculations are compared for three different models: LTE, NLTE/ $S_{\rm H}=0$ , and NLTE/ $S_{\rm H}=1$ . The bottom-right panel shows the variation of the quality of the fit as a function of the position of the disk: LTE (solid), NLTE/ $S_{\rm H}=0$ (dashed) and NLTE/ $S_{\rm H}=1$ (dot-dashed). The $\chi '^2$ values have been normalized to 1 at the minimum.
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In the text

$\begin{figure} \par\mbox{\includegraphics[height=6.7cm,width=4.5cm,angle=90,clip... ...udegraphics[height=6.1cm,width=4.4cm,angle=90,clip]{0050fig7d.ps} } \end{figure}$ Figure 7: Center (at rest with the continuum normalized to 1) and limb (shifted to the red with the continuum normalized to 1 and subtracted 0.05) spectra for Na I $\lambda 6160.8$ . Observations (filled circles) and calculations are compared for three different models: LTE, NLTE/ $S_{\rm H}=0$ , and NLTE/ $S_{\rm H}=1$ . The bottom-right panel shows the variation of the quality of the fit as a function of the position of the disk as in Fig. 6.
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In the text

$\begin{figure} \par\mbox{\includegraphics[height=6.8cm,width=4.5cm,angle=90,clip... ...udegraphics[height=6.1cm,width=4.4cm,angle=90,clip]{0050fig8d.ps} } \end{figure}$ Figure 8: Similar to Fig. 6 for the 3D time-dependent simulation of the solar surface.
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In the text

$\begin{figure} \par {\includegraphics[angle=90,width=7.3cm,clip]{0050fig2.ps} } \end{figure}$	Figure 2: Contour plot showing the reduced $\chi ^2$ , normalized to unity at its minimum, as a function of the relative resolving power and the amount of scattered light for the $\mu =1$ setup centered around the Ca I $\lambda 6162$ line.
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$\begin{figure} \par {\includegraphics[angle=90,width=7.6cm,clip]{0050fig3.ps} } \end{figure}$	Figure 3: Comparison of the spectra at the center of the disk in the region around Ca I $\lambda 6162.2$ from Brault & Neckel (1987; convolved with a Gaussian; solid line) and the Gregory Coudé Telescope (after removal of scattered light; filled circles).
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$\begin{figure} \par {\includegraphics[width=5.8cm,angle=90,clip]{0050fig4a.ps} } {\includegraphics[width=6cm,angle=90,clip]{0050fig4b.ps} } \end{figure}$	Figure 4: Center (filled circles) and limb (solid) spectra in the region around Ca I $\lambda 6162.2$ ( top panel) and around Co I $\lambda 5301.0$ ( bottom panel).
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$\begin{figure} \par {\includegraphics[angle=90,width=7.7cm,clip]{0050fig5.ps} } \end{figure}$	Figure 5: Response functions to the temperature at $\mu =0.32$ and 1.00 for the core of the lines of the O I infrared triplet (solid) and the Na I $\lambda 6160.8$ (dashed) lines.
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$\begin{figure} \par\mbox{\includegraphics[height=6.8cm,width=4.5cm,angle=90,clip... ...udegraphics[height=6.1cm,width=4.4cm,angle=90,clip]{0050fig8d.ps} } \end{figure}$	Figure 8: Similar to Fig. 6 for the 3D time-dependent simulation of the solar surface.
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