All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{1328fig1} \end{figure}$ Figure 1: (U-B) colour distribution derived from final sample of GCs used in this study.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1328fig2} \end{figure}$ Figure 2: Top panel: metallicity distribution derived from (U-B) colours of 69 GCs which have (U-B) photometric errors less than 0.1 mag. All photometry is corrected for Galactic extinction. Bottom panel: comparison between the derived metallicity distribution (shown in top panel) and that derived by Harris et al. (2003) using the metallicity sensitive (C-T₁) index.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{1328fig3} \end{figure}$ Figure 3: Best KS probabilities for various values of f₁ and for four final gas fractions $g_{\rm frac}$ . The shaded region shows a set of degenerate models that have high KS probabilities and therefore cannot be discounted completely. The KS probability for a single starburst scenario is shown by the solid line at 2 percent.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{1328fig4} \end{figure}$ Figure 4: Three GC formation histories corresponding to the best KS probabilities shown in the shaded region in Fig. 3.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{1328fig5} \end{figure}$ Figure 5: Age-metallicity grid showing the fraction of stellar mass predicted by the favoured model as a function of age and metallicity. The key indicates stellar fractions corresponding to the levels of shading in the plot.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{1328fig6} \end{figure}$ Figure 6: Comparison between observed MDF and that predicted by the favoured model (which gives the highest KS probabillity).
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{1328fig7} \end{figure}$ Figure 7: KS values for perturbed double starburst scenarios as a fraction of the KS values in the unperturbed case. The size of the perturbation applied to the system is 5 percent.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1328fig1} \end{figure}$	Figure 1: (U-B) colour distribution derived from final sample of GCs used in this study.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{1328fig2} \end{figure}$	Figure 2: Top panel: metallicity distribution derived from (U-B) colours of 69 GCs which have (U-B) photometric errors less than 0.1 mag. All photometry is corrected for Galactic extinction. Bottom panel: comparison between the derived metallicity distribution (shown in top panel) and that derived by Harris et al. (2003) using the metallicity sensitive (C-T₁) index.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{1328fig3} \end{figure}$	Figure 3: Best KS probabilities for various values of f₁ and for four final gas fractions $g_{\rm frac}$ . The shaded region shows a set of degenerate models that have high KS probabilities and therefore cannot be discounted completely. The KS probability for a single starburst scenario is shown by the solid line at 2 percent.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{1328fig4} \end{figure}$	Figure 4: Three GC formation histories corresponding to the best KS probabilities shown in the shaded region in Fig. 3.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{1328fig5} \end{figure}$	Figure 5: Age-metallicity grid showing the fraction of stellar mass predicted by the favoured model as a function of age and metallicity. The key indicates stellar fractions corresponding to the levels of shading in the plot.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{1328fig6} \end{figure}$	Figure 6: Comparison between observed MDF and that predicted by the favoured model (which gives the highest KS probabillity).
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{1328fig7} \end{figure}$	Figure 7: KS values for perturbed double starburst scenarios as a fraction of the KS values in the unperturbed case. The size of the perturbation applied to the system is 5 percent.
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