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$\begin{figure} \par\includegraphics[height=3.5cm,width=8.8cm,clip]{0238fig1.eps}\end{figure}$ Figure 1: Initial position of a giant planet with mass $M_{\rm G}$ relative to the reference frame centered at the primary star with mass $M_{\rm A}$ . The secondary star has mass $M_{\rm B}$ and the center of mass is denoted by CM. Note that the initial position of the giant planet is different for inner (S-type) and outer (P-type) planetary orbits. The choice of the initial velocities $V_{\rm B}$ and $V_{\rm G}$ is described in the main text.
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In the text

$\begin{figure} \par\includegraphics[height=6.7cm,width=7cm,clip]{0238fig2.eps}\end{figure}$ Figure 2: Stable planetary orbit obtained for the binary system 3 given in Table 1. The criterion for stable orbits is given in the main text.
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In the text

$\begin{figure} \par\includegraphics[height=6.7cm,width=7cm,clip]{0238fig3.eps}\end{figure}$ Figure 3: Marginally stable planetary orbit obtained for the binary system 3 given in Table 1. The criterion for marginally stable orbits is given in the main text.
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In the text

$\begin{figure} \par\includegraphics[height=6.7cm,width=7cm,clip]{0238fig4.eps}\end{figure}$ Figure 4: Unstable planetary orbit obtained for the binary system 3 given in Table 1. The criterion for unstable orbits is given in the main text.
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In the text

$\begin{figure} \par\includegraphics[height=6.5cm,width=7cm,clip]{0238fig5.eps}\end{figure}$ Figure 5: Range of mass ratios and separation ratios corresponding to stable, marginally stable and unstable inner (S-type) planetary orbits in binary systems. The simulations are based on 1000 orbits.
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In the text

$\begin{figure} \par\includegraphics[height=6.5cm,width=7cm,clip]{0238fig6.eps}\end{figure}$ Figure 6: Range of mass ratios and sparation ratios corresponding to stable, marginally stable and unstable outer (P-type) planetary orbits in binary systems. The simulations are based on 1000 orbits.
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In the text

$\begin{figure} \par\includegraphics[height=6.7cm,width=7cm,clip]{0238fig2.eps}\end{figure}$	Figure 2: Stable planetary orbit obtained for the binary system 3 given in Table 1. The criterion for stable orbits is given in the main text.
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$\begin{figure} \par\includegraphics[height=6.7cm,width=7cm,clip]{0238fig3.eps}\end{figure}$	Figure 3: Marginally stable planetary orbit obtained for the binary system 3 given in Table 1. The criterion for marginally stable orbits is given in the main text.
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$\begin{figure} \par\includegraphics[height=6.7cm,width=7cm,clip]{0238fig4.eps}\end{figure}$	Figure 4: Unstable planetary orbit obtained for the binary system 3 given in Table 1. The criterion for unstable orbits is given in the main text.
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$\begin{figure} \par\includegraphics[height=6.5cm,width=7cm,clip]{0238fig5.eps}\end{figure}$	Figure 5: Range of mass ratios and separation ratios corresponding to stable, marginally stable and unstable inner (S-type) planetary orbits in binary systems. The simulations are based on 1000 orbits.
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$\begin{figure} \par\includegraphics[height=6.5cm,width=7cm,clip]{0238fig6.eps}\end{figure}$	Figure 6: Range of mass ratios and sparation ratios corresponding to stable, marginally stable and unstable outer (P-type) planetary orbits in binary systems. The simulations are based on 1000 orbits.
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