$\begin{figure} \par {\includegraphics[height=17.6cm,width=16.8cm,clip]{2179fig3.eps} } \end{figure}$ Figure 3: Observed window in 12 emission lines. Line formation temperatures [MK] are given in the bracket. Contours represent coronal hole ( upper part) and quiet Sun ( lower part).
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In the text

$\begin{figure} \par {\includegraphics[height=17.6cm,width=17.3cm,clip]{2179fig4.eps} } \end{figure}$ Figure 4: Quiet Sun intensities are plotted against coronal hole intensities. Intensity units are [10^-3 W m^-2 sr^-1]. Solid line represents a straight line fit. Fit parameters are given in Table 1. Dotted line represents the line of equal intensity.
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In the text

$\begin{figure} \par\includegraphics[height=6.58cm,width=14cm,clip]{2179fig1.eps} \end{figure}$	Figure 1: Contribution functions plotted as a function of temperature (from CHIANTI version 4.02).
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$\begin{figure} \par {\includegraphics[angle=90,width=8.8cm,clip]{2179fig2.ps} } \end{figure}$	Figure 2: EIT 195 Å image and the raster position.
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$\begin{figure} \par {\includegraphics[height=17.6cm,width=16.8cm,clip]{2179fig3.eps} } \end{figure}$	Figure 3: Observed window in 12 emission lines. Line formation temperatures [MK] are given in the bracket. Contours represent coronal hole ( upper part) and quiet Sun ( lower part).
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$\begin{figure} \par {\includegraphics[height=17.6cm,width=17.3cm,clip]{2179fig4.eps} } \end{figure}$	Figure 4: Quiet Sun intensities are plotted against coronal hole intensities. Intensity units are [10^-3 W m^-2 sr^-1]. Solid line represents a straight line fit. Fit parameters are given in Table 1. Dotted line represents the line of equal intensity.
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