All Figures

$\begin{figure} \par\includegraphics[angle=90,width=7.5cm,clip]{3907_f1.ps} \end{figure}$ Figure 1: Spectral coverage versus date of quiet Sun observation contained in the selected files.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=7.6cm,clip]{3907_f2.ps}\vspace*{6mm} \includegraphics[angle=90,width=7.6cm,clip]{3907_f3.ps} \end{figure}$ Figure 2: Intensity histogram for ( top) N IV line at 765 Å and ( bottom) H I line at 918 Å. The total number indicates the number of intensities in the $5\hbox {$^{\prime \prime }$ }$ bands. The full line indicates the best fit with a lognormal distribution.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8cm,clip]{3907_f4.ps} \end{figure}$ Figure 3: Quiet area intensities for N IV (765.15 Å). Squares: quiet solar activity ( $f_{10.7} \le 100$ ). Triangles: medium activity ( $100 < f_{10.7} \le 150$ ). Crosses: high activity ( f_10.7 > 150). The line shows the theoretical center-to-limb variation, while small symbols show the intensities transposed to the center of the solar disk.
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In the text

$\begin{figure} \par\includegraphics[width=5.8cm,clip]{3907_f5.ps} \end{figure}$ Figure 4: Slit position for the SUMER observations on 1997 January 23, using an EIT image at 171 Å (north is up). No significant changes of the appearance of the solar disk appearance were observed for the different files at this date. Note that the south edge of the Sun is at the bottom of the figure. The dark areas correspond to coronal holes.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=7.7cm,clip]{3907_f6.ps} \end{figure}$ Figure 5: Quiet area intensities for H I (918.13 Å). Squares: quiet solar activity ( $f_{10.7} \le 100$ ). Triangles: medium activity ( $100 < f_{10.7} \le 150$ ). Crosses: high activity ( f_10.7 > 150).
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In the text

$\begin{figure} \par\includegraphics[height=8.2cm,width=4.6cm,angle=90,clip]{3907... ...includegraphics[height=8.6cm,width=4.6cm,angle=90,clip]{3907_f8.ps} \end{figure}$ Figure 6: Fit of the continuum background. The full line is the mean SUMER spectrum at 1 Å resolution. The dotted line represents the fitted continuum. In the region between 793 and 892 Å, there is a lack of data corresponding to our selection criteria.
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In the text

$\begin{figure} \par\includegraphics[height=6.5cm,width=5.6cm,angle=90,clip]{3907_f9.ps} \end{figure}$ Figure 7: Mean quiet Sun differential emission measure from SUMER.
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In the text

$\begin{figure} \par\hfill{} \mbox{\includegraphics[ width=0.2\textheight, heigh... ...0.49\textwidth, angle=90, origin=lB]{3907_f15.ps} }\hfill{} \par \end{figure}$ Figure 8: Comparison of the synthetic reference spectrum with the SUMER data. Left panels show the spectrum in three different wavelength ranges; right panels show the ratio of the synthetic spectrum (labeled "this work'') to the composite SUMER spectrum.
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In the text

$\begin{figure} \par\includegraphics[height=8.5cm,width=5.53cm,angle=90,clip]{390... ...cludegraphics[height=8.5cm,width=5.53cm,angle=90,clip]{3907_f17.ps} \end{figure}$ Figure 9: Comparison of NRLEUV reference spectrum with this work. Left and right panels are defined as in Fig. 8.
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In the text

$\begin{figure} \par\includegraphics[height=8.6cm,width=5.8cm,angle=90,clip]{3907... ...ncludegraphics[height=8.4cm,width=5.8cm,angle=90,clip]{3907_f19.ps} \end{figure}$ Figure 10: Comparison of NRLEUV reference spectrum with the composite SUMER spectrum. Left and right panels are defined as in Fig. 8.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=7.5cm,clip]{3907_f1.ps} \end{figure}$	Figure 1: Spectral coverage versus date of quiet Sun observation contained in the selected files.
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$\begin{figure} \par\includegraphics[angle=90,width=7.6cm,clip]{3907_f2.ps}\vspace*{6mm} \includegraphics[angle=90,width=7.6cm,clip]{3907_f3.ps} \end{figure}$	Figure 2: Intensity histogram for ( top) N IV line at 765 Å and ( bottom) H I line at 918 Å. The total number indicates the number of intensities in the $5\hbox {$^{\prime \prime }$ }$ bands. The full line indicates the best fit with a lognormal distribution.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=90,width=8cm,clip]{3907_f4.ps} \end{figure}$	Figure 3: Quiet area intensities for N IV (765.15 Å). Squares: quiet solar activity ( $f_{10.7} \le 100$ ). Triangles: medium activity ( $100 < f_{10.7} \le 150$ ). Crosses: high activity ( f_10.7 > 150). The line shows the theoretical center-to-limb variation, while small symbols show the intensities transposed to the center of the solar disk.
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$\begin{figure} \par\includegraphics[width=5.8cm,clip]{3907_f5.ps} \end{figure}$	Figure 4: Slit position for the SUMER observations on 1997 January 23, using an EIT image at 171 Å (north is up). No significant changes of the appearance of the solar disk appearance were observed for the different files at this date. Note that the south edge of the Sun is at the bottom of the figure. The dark areas correspond to coronal holes.
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$\begin{figure} \par\includegraphics[angle=90,width=7.7cm,clip]{3907_f6.ps} \end{figure}$	Figure 5: Quiet area intensities for H I (918.13 Å). Squares: quiet solar activity ( $f_{10.7} \le 100$ ). Triangles: medium activity ( $100 < f_{10.7} \le 150$ ). Crosses: high activity ( f_10.7 > 150).
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$\begin{figure} \par\includegraphics[height=8.2cm,width=4.6cm,angle=90,clip]{3907... ...includegraphics[height=8.6cm,width=4.6cm,angle=90,clip]{3907_f8.ps} \end{figure}$	Figure 6: Fit of the continuum background. The full line is the mean SUMER spectrum at 1 Å resolution. The dotted line represents the fitted continuum. In the region between 793 and 892 Å, there is a lack of data corresponding to our selection criteria.
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$\begin{figure} \par\includegraphics[height=6.5cm,width=5.6cm,angle=90,clip]{3907_f9.ps} \end{figure}$	Figure 7: Mean quiet Sun differential emission measure from SUMER.
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$\begin{figure} \par\hfill{} \mbox{\includegraphics[ width=0.2\textheight, heigh... ...0.49\textwidth, angle=90, origin=lB]{3907_f15.ps} }\hfill{} \par \end{figure}$	Figure 8: Comparison of the synthetic reference spectrum with the SUMER data. Left panels show the spectrum in three different wavelength ranges; right panels show the ratio of the synthetic spectrum (labeled "this work'') to the composite SUMER spectrum.
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$\begin{figure} \par\includegraphics[height=8.5cm,width=5.53cm,angle=90,clip]{390... ...cludegraphics[height=8.5cm,width=5.53cm,angle=90,clip]{3907_f17.ps} \end{figure}$	Figure 9: Comparison of NRLEUV reference spectrum with this work. Left and right panels are defined as in Fig. 8.
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$\begin{figure} \par\includegraphics[height=8.6cm,width=5.8cm,angle=90,clip]{3907... ...ncludegraphics[height=8.4cm,width=5.8cm,angle=90,clip]{3907_f19.ps} \end{figure}$	Figure 10: Comparison of NRLEUV reference spectrum with the composite SUMER spectrum. Left and right panels are defined as in Fig. 8.
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