All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{MS3485f1.eps}\end{figure}$ Figure 1: 4-month summer 1991 IRIS power spectra (up: with no gap filling / down: with repetitive music method).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{MS3485f2.eps}\end{figure}$ Figure 2: IRIS frequency shifts in the frequency range from 1.8 mHz to the acoustic cut-off frequency. (1) from the Lorentzian profile fitting $-\blacksquare -$ : $\ell =0$ , $-\bullet -$ : $\ell =1$ and $-\blacktriangledown -$ : $\ell =2$ , (2) from the cross-correlation method -*-, and (3) from the cross-correlation method adapted for frequencies beyond 4.5 mHz $-\blacklozenge -$ .
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{MS3485f3.eps}\end{figure}$ Figure 3: Solar p-mode linewidths $\Gamma$ and solar activity cycle.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{MS3485f4.eps}\end{figure}$ Figure 4: p-mode frequency shifts (solid line: $\delta \nu _{2.6-3.7}$ / dashed line: $\delta \nu _{3.7-4.5}$ ) and International Sunspot Number $R_{\rm I}$ for comparison (black line).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{MS3485f5.eps}\end{figure}$ Figure 5: Linewidths $\Gamma$ averaged between 2.6 mHz $\leq \nu \leq$ 3.7 mHz compared to the International Sunspot Number $R_{\rm I}$ (black line), as solar activity proxy.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=8.8cm,clip]{MS3485f6.eps}\end{figure}$ Figure 6: Daily averaged IRIS power spectrum.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{MS3485f7.eps}\end{figure}$ Figure 7: Power spectrum of the continuum part in Fig. 6 over the frequency range from 5.8 to 7.5 mHz. The prominent peak corresponds to a periodicity of 70.8 $\mu$ Hz in this pseudo-mode range.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{MS3485f1.eps}\end{figure}$	Figure 1: 4-month summer 1991 IRIS power spectra (up: with no gap filling / down: with repetitive music method).
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$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{MS3485f2.eps}\end{figure}$	Figure 2: IRIS frequency shifts in the frequency range from 1.8 mHz to the acoustic cut-off frequency. (1) from the Lorentzian profile fitting $-\blacksquare -$ : $\ell =0$ , $-\bullet -$ : $\ell =1$ and $-\blacktriangledown -$ : $\ell =2$ , (2) from the cross-correlation method -*-, and (3) from the cross-correlation method adapted for frequencies beyond 4.5 mHz $-\blacklozenge -$ .
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$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{MS3485f3.eps}\end{figure}$	Figure 3: Solar p-mode linewidths $\Gamma$ and solar activity cycle.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{MS3485f4.eps}\end{figure}$	Figure 4: p-mode frequency shifts (solid line: $\delta \nu _{2.6-3.7}$ / dashed line: $\delta \nu _{3.7-4.5}$ ) and International Sunspot Number $R_{\rm I}$ for comparison (black line).
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$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{MS3485f5.eps}\end{figure}$	Figure 5: Linewidths $\Gamma$ averaged between 2.6 mHz $\leq \nu \leq$ 3.7 mHz compared to the International Sunspot Number $R_{\rm I}$ (black line), as solar activity proxy.
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$\begin{figure} \par\includegraphics[angle=0,width=8.8cm,clip]{MS3485f6.eps}\end{figure}$	Figure 6: Daily averaged IRIS power spectrum.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{MS3485f7.eps}\end{figure}$	Figure 7: Power spectrum of the continuum part in Fig. 6 over the frequency range from 5.8 to 7.5 mHz. The prominent peak corresponds to a periodicity of 70.8 $\mu$ Hz in this pseudo-mode range.
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