$\begin{figure} \par\includegraphics[bb=33 21 536 513, width=8cm,clip]{4828f02.eps} \end{figure}$ Figure 2: Infrared two colour diagram according to that of Epchtein et al. (1987) to discriminate O-rich from carbon stars. The colours for blackbodies of different temperatures [K] are indicated. The two outliers in box "o3'' are discussed in the text.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4828f04a.ps}\hspace*{3mm} ... ...s}\hspace*{3mm} \includegraphics[width=8.5cm,clip]{4828f04d.ps}\par \end{figure}$ Figure 4: Theoretical period distribution of AGB stars inside the observed instability strip for carbon stars for masses of 2.5, 2.6, 3.0 (all at Z= 0.016), and 3.0 (at Z= 0.010) $M_{\odot }$ ( left to right, top to bottom). Every histogram is normalised to unity.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4828f05a.ps}\hspace*{3mm} ... ...5e.ps}\hspace*{3mm} \includegraphics[width=8.5cm,clip]{4828f05f.ps} \end{figure}$ Figure 5: Theoretical period distribution of AGB stars inside the observed instability strip for oxygen-rich stars for masses of 2.5, 3.0, 3.5, 4.0, 4.5, and 5.0 $M_{\odot }$ ( left to right, top to bottom). Every histogram is normalised to unity.
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In the text

$\begin{figure} \par\includegraphics[bb=30 30 509 734,width=8.4cm,clip]{4828f01.eps} \end{figure}$	Figure 1: Examples of K-band photometry for 5 stars with corresponding fit solutions.
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$\begin{figure} \par\includegraphics[bb=33 21 536 513, width=8cm,clip]{4828f02.eps} \end{figure}$	Figure 2: Infrared two colour diagram according to that of Epchtein et al. (1987) to discriminate O-rich from carbon stars. The colours for blackbodies of different temperatures [K] are indicated. The two outliers in box "o3'' are discussed in the text.
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$\begin{figure} \par\includegraphics[bb=41 37 371 365, width=8cm,clip]{4828f03.eps} \end{figure}$	Figure 3: Bolometric magnitude and IRAS flux-ratio. The line indicates the relation given in Groenewegen et al. (2002).
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4828f04a.ps}\hspace{3mm} ... ...s}\hspace{3mm} \includegraphics[width=8.5cm,clip]{4828f04d.ps}\par \end{figure}$	Figure 4: Theoretical period distribution of AGB stars inside the observed instability strip for carbon stars for masses of 2.5, 2.6, 3.0 (all at Z= 0.016), and 3.0 (at Z= 0.010) $M_{\odot }$ ( left to right, top to bottom). Every histogram is normalised to unity.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4828f05a.ps}\hspace{3mm} ... ...5e.ps}\hspace{3mm} \includegraphics[width=8.5cm,clip]{4828f05f.ps} \end{figure}$	Figure 5: Theoretical period distribution of AGB stars inside the observed instability strip for oxygen-rich stars for masses of 2.5, 3.0, 3.5, 4.0, 4.5, and 5.0 $M_{\odot }$ ( left to right, top to bottom). Every histogram is normalised to unity.
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