$\begin{figure} \par\includegraphics[angle=90,width=7cm,clip]{1098f2.eps} \end{figure}$ Figure 2: Model of the star surrounded by a thin molecular layer. $\theta$ is the angle between the radius vector and the line of sight at the layer surface.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.7cm,clip]{1098f4a.eps}\hspace*{4mm} \includegraphics[angle=-90,width=7.7cm,clip]{1098f4b.eps} \end{figure}$ Figure 4: Fit and synthetic spectrum based on the November 2001 narrow band and November 2000 L band data of R Leo. Photometric data are from Whitelock et al. (2000a). An average layer optical depth of 1 has been used to compute the synthetic spectrum.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.5cm,clip]{1098f5a.eps}\hsp... ...ce*{3mm} \includegraphics[angle=-90,width=7.5cm,clip]{1098f5d.eps} \end{figure}$ Figure 5: Fit and synthetic spectrum based on the October 2000 narrow band and November 2000 L band data of Mira ( top). Fit and synthetic spectrum based on the November 2001 narrow band data of Mira ( bottom). Photometric data are from Whitelock et al. (2000a). Average layer optical depths of 0.10 and 0.40 have been used to compute the synthetic spectra for the 2000 and 2001 data, respectively.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.8cm,clip]{1098f6a.eps}\hspace*{3mm} \includegraphics[angle=-90,width=7.8cm,clip]{1098f6b.eps} \end{figure}$ Figure 6: Fit and synthetic spectrum based on the May 2002 narrow band data of T Cep. Photometric data are from Smith et al. (2002). An average layer optical depth of 0.20 has been used to compute the synthetic spectrum.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.7cm,clip]{1098f7a.eps}\hsp... ...ce*{4mm} \includegraphics[angle=-90,width=7.7cm,clip]{1098f7d.eps} \end{figure}$ Figure 7: Fit and synthetic spectrum based on the October 2000 narrow band and November 2000 L' band data of U Ori ( top). Fit and synthetic spectrum based on the November 2001 narrow band data of U Ori ( bottom). Photometric data are from Whitelock et al. (2000a). Average layer optical depths of 0.85 and 0.95 have been used to compute the synthetic spectra for the 2000 and 2001 data, respectively.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{1098f8a.eps}\hspac... ...pace*{3mm} \includegraphics[angle=-90,width=8cm,clip]{1098f8d.eps} \end{figure}$ Figure 8: Fit and synthetic spectrum based on the November 2001 ( top) and May 2002 ( bottom) narrow band data of $\chi$ Cyg. Photometric data are from Whitelock et al. (2000a). An average layer optical depth of 0.20 has been used to compute the synthetic spectra for the 2001 and 2002 data.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.8cm,clip]{1098f9.eps} \end{figure}$ Figure 9: Fit of the FLUOR and PTI K' band R Tri data. The discrepant datum at 172 arcsec^-1 is the outlier mentioned in the text.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.7cm,clip]{1098f11.eps} \end{figure}$ Figure 11: Linear radii deduced from the present interferometric measurements vs. pulsation periods. Continuous and dotted lines are expectations for respectively fundamental mode and first overtone pulsators from Wood (1989). Comparison of this figure with a similar figure in Feast (1996) dramatically illustrates the impact of the revised interpretation of Mira brightness distributions.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.5cm,clip]{1098f1.eps} \end{figure}$	Figure 1: Transmission of narrow band filters.
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$\begin{figure} \par\includegraphics[angle=90,width=7cm,clip]{1098f2.eps} \end{figure}$	Figure 2: Model of the star surrounded by a thin molecular layer. $\theta$ is the angle between the radius vector and the line of sight at the layer surface.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.3cm,clip]{1098f3.eps} \end{figure}$	Figure 3: Fit of the 1997 K band (triangles) and 2000 L band (circles) data of R Leo.
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$\begin{figure} \par\includegraphics[angle=-90,width=7.7cm,clip]{1098f4a.eps}\hspace*{4mm} \includegraphics[angle=-90,width=7.7cm,clip]{1098f4b.eps} \end{figure}$	Figure 4: Fit and synthetic spectrum based on the November 2001 narrow band and November 2000 L band data of R Leo. Photometric data are from Whitelock et al. (2000a). An average layer optical depth of 1 has been used to compute the synthetic spectrum.
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$\begin{figure} \par\includegraphics[angle=-90,width=7.8cm,clip]{1098f6a.eps}\hspace*{3mm} \includegraphics[angle=-90,width=7.8cm,clip]{1098f6b.eps} \end{figure}$	Figure 6: Fit and synthetic spectrum based on the May 2002 narrow band data of T Cep. Photometric data are from Smith et al. (2002). An average layer optical depth of 0.20 has been used to compute the synthetic spectrum.
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$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{1098f8a.eps}\hspac... ...pace*{3mm} \includegraphics[angle=-90,width=8cm,clip]{1098f8d.eps} \end{figure}$	Figure 8: Fit and synthetic spectrum based on the November 2001 ( top) and May 2002 ( bottom) narrow band data of $\chi$ Cyg. Photometric data are from Whitelock et al. (2000a). An average layer optical depth of 0.20 has been used to compute the synthetic spectra for the 2001 and 2002 data.
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$\begin{figure} \par\includegraphics[angle=-90,width=7.8cm,clip]{1098f9.eps} \end{figure}$	Figure 9: Fit of the FLUOR and PTI K' band R Tri data. The discrepant datum at 172 arcsec^-1 is the outlier mentioned in the text.
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$\begin{figure} \par\includegraphics[angle=-90,width=7.7cm,clip]{1098f10.eps} \end{figure}$	Figure 10: Extrapolation of the FLUOR model at $11.149~\mu$ m with $\tau =0.32$ .
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$\begin{figure} \par\includegraphics[angle=-90,width=7.7cm,clip]{1098f11.eps} \end{figure}$	Figure 11: Linear radii deduced from the present interferometric measurements vs. pulsation periods. Continuous and dotted lines are expectations for respectively fundamental mode and first overtone pulsators from Wood (1989). Comparison of this figure with a similar figure in Feast (1996) dramatically illustrates the impact of the revised interpretation of Mira brightness distributions.
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