$\begin{figure} \par\includegraphics[width=15cm,clip]{0006fig2.eps} \end{figure}$ Figure 2: The V vs. (B-V) CMDs of all the six regions studied here are shown. These CMDs are used to estimate the stellar density after correcting for data incompleteness.
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In the text

$\begin{figure} \par\includegraphics[width=15.8cm]{0006fig3.eps} \end{figure}$ Figure 3: The stellar densities on the CMDs for regions 1 and 2. Panels a) and c) correspond to the observed CMDs, b) and d) correspond to the synthetic CMDs for regions 1 and 2 respectively.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{0006fig5.eps} \end{figure}$ Figure 5: The SFRs and the fraction of clusters in various age groups are plotted here for six regions. This plot helps to find out correlation between the increases or decreases in the rates of star and cluster formation.
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In the text

$\begin{figure} \par\includegraphics[width=15.7cm]{0006fig6.eps} \end{figure}$ Figure 6: The stellar densities on the CMDs for regions 3 and 4. Panels a) and c) correspond to the observed CMDs, b) and d) correspond to the synthetic CMDs for regions 3 and 4 respectively.
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In the text

$\begin{figure} \par\includegraphics[width=15.7cm]{0006fig7.eps} \end{figure}$ Figure 7: The stellar densities on the CMDs for regions 5 and 6. Panels a) and c) correspond to the observed CMDs, b) and d) correspond to the synthetic CMDs for the regions 5 and 6 respectively.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0006fig1.eps} \end{figure}$	Figure 1: The locations of the regions studied. The Bar and 30 Dor are also shown.
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$\begin{figure} \par\includegraphics[width=15cm,clip]{0006fig2.eps} \end{figure}$	Figure 2: The V vs. (B-V) CMDs of all the six regions studied here are shown. These CMDs are used to estimate the stellar density after correcting for data incompleteness.
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$\begin{figure} \par\includegraphics[width=15.8cm]{0006fig3.eps} \end{figure}$	Figure 3: The stellar densities on the CMDs for regions 1 and 2. Panels a) and c) correspond to the observed CMDs, b) and d) correspond to the synthetic CMDs for regions 1 and 2 respectively.
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$\begin{figure} \par\includegraphics[width=15.7cm,clip]{0006fig4.eps} \end{figure}$	Figure 4: The estimates of SFRs in the six regions between 10 Myr to 12 Gyr are plotted as histograms.
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$\begin{figure} \par\includegraphics[width=15cm,clip]{0006fig5.eps} \end{figure}$	Figure 5: The SFRs and the fraction of clusters in various age groups are plotted here for six regions. This plot helps to find out correlation between the increases or decreases in the rates of star and cluster formation.
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$\begin{figure} \par\includegraphics[width=15.7cm]{0006fig6.eps} \end{figure}$	Figure 6: The stellar densities on the CMDs for regions 3 and 4. Panels a) and c) correspond to the observed CMDs, b) and d) correspond to the synthetic CMDs for regions 3 and 4 respectively.
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$\begin{figure} \par\includegraphics[width=15.7cm]{0006fig7.eps} \end{figure}$	Figure 7: The stellar densities on the CMDs for regions 5 and 6. Panels a) and c) correspond to the observed CMDs, b) and d) correspond to the synthetic CMDs for the regions 5 and 6 respectively.
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