All Figures

$\begin{figure} \par\includegraphics[width=3cm,clip]{Hh121_f1a.eps}\hspace*{1.3cm} \includegraphics[width=3cm,clip]{Hh121_f1b.eps} \end{figure}$ Figure 1: Images of NGC 1566 and NGC 5247 in B-band with superposed fitted curves of spiral arms.
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In the text

$\begin{figure} \par\subfigure[]{\includegraphics[width=3.2cm,clip]{Hh121_f2a.eps... ... \subfigure[]{\includegraphics[width=3.1cm,clip]{Hh121_f2d.eps} } \end{figure}$ Figure 2: Panel a) shows $V_V=V_\alpha /V_{\alpha \rightarrow \infty }$ with different z₀ $(z_0 =2/\alpha )$ . V_V is the ratio for the amplitude of the gravitational potential perturbation of a disk with finite thickness to that of an infinitely thin disk. The curves from top down correspond to $z_{01}=0.20~\rm{kpc}$ $(\alpha_{01}=10.00~\rm{kpc}^{-1})$ , $z_{02}=0.50~\rm{kpc}$ $(\alpha_{02}=4.00~\rm{kpc}^{-1})$ , and $z_{03}=1.00~\rm{kpc}$ $(\alpha_{03}=2.00~\rm{kpc}^{-1})$ , respectively. Panels b)- d) are three panels for NGC 1566 to illustrate the changes of z₀ with r₀, $\Lambda$ , and m, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=3cm,clip]{Hh121_f1a.eps}\hspace*{1.3cm} \includegraphics[width=3cm,clip]{Hh121_f1b.eps} \end{figure}$	Figure 1: Images of NGC 1566 and NGC 5247 in B-band with superposed fitted curves of spiral arms.
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