$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{0697fig2.ps}\end{figure}$ Figure 2: The normalized distributions of morphological types for Isolated (solid line) and Perturbed (dashed line) galaxies.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.7cm,clip]{0697fig3.ps}\end{figure}$ Figure 3: The luminosity-size relation for Isolated (empty circles) and Perturbed (filled circles) galaxies. The lines are the best fit to the two families.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.7cm,clip]{0697fig4.ps}\end{figure}$ Figure 4: The mass-luminosity relation for Isolated and Perturbed galaxies. Same symbols as in Fig. 3. The rotation velocity was corrected for inclination. Only galaxies not later than Scd, with inclinations between 40 and 70 degrees have been plotted. The lines are the fits to both families.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{0697fig5.ps}\end{figure}$ Figure 5: The Tully-Fisher relation for Isolated and Perturbed galaxies. Same symbols and galaxies as in Fig. 4. The line represents the fit to the T-F relation as given by Tully & Pierce (2002).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{0697fig1.ps}\end{figure}$	Figure 1: The distribution of the f-values for galaxies in the Coma Cluster.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{0697fig2.ps}\end{figure}$	Figure 2: The normalized distributions of morphological types for Isolated (solid line) and Perturbed (dashed line) galaxies.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.7cm,clip]{0697fig3.ps}\end{figure}$	Figure 3: The luminosity-size relation for Isolated (empty circles) and Perturbed (filled circles) galaxies. The lines are the best fit to the two families.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.7cm,clip]{0697fig4.ps}\end{figure}$	Figure 4: The mass-luminosity relation for Isolated and Perturbed galaxies. Same symbols as in Fig. 3. The rotation velocity was corrected for inclination. Only galaxies not later than Scd, with inclinations between 40 and 70 degrees have been plotted. The lines are the fits to both families.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{0697fig5.ps}\end{figure}$	Figure 5: The Tully-Fisher relation for Isolated and Perturbed galaxies. Same symbols and galaxies as in Fig. 4. The line represents the fit to the T-F relation as given by Tully & Pierce (2002).
Open with DEXTER