$\begin{figure} \par\includegraphics[width=4cm,clip]{0425f2a.eps}\hspace*{4mm} \i... ...f2b.eps}\hspace*{4mm} \includegraphics[width=4cm,clip]{0425f2c.eps} \end{figure}$ Figure 2: The variability due to the continuum image of a source a) is different relative to the image of the source at two spectral lines at frequencies, say, b) $\nu _{\rm abs1}$ and c) $\nu _{\rm abs2}$ . Since the observed variability properties depend sensitively on fine-scale source structure, the intensity scintillations caused by scattering in the ISM of our Galaxy are different in all three cases.
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In the text

$\begin{figure} \par\includegraphics[width=9.4cm,clip]{0425f3.eps} \end{figure}$ Figure 3: The amplitude of refractive moduluation exhibited by a point source of flux density $S_{\rm src}$ for $\beta =11/3$ and for a number of scattering measures and distances to the scattering medium, as given by Eq. (38).
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In the text

$\begin{figure} \par\includegraphics[width=14.3cm,clip]{0425f1.eps} \end{figure}$	Figure 1: The geometry of the absorbing system.
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$\begin{figure} \par\includegraphics[width=9.4cm,clip]{0425f3.eps} \end{figure}$	Figure 3: The amplitude of refractive moduluation exhibited by a point source of flux density $S_{\rm src}$ for $\beta =11/3$ and for a number of scattering measures and distances to the scattering medium, as given by Eq. (38).
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