All Figures

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{4351fig1.eps} \end{figure}$ Figure 1: The GC metallicity distribution of the GC05 (panel a)) and reduced samples (panel b)). The adopted threshold between metal-rich and metal-poor GCs is indicated. The reddening distribution of the reduced sample GCs is in panel c), the corresponding metal-poor ones are in panel d), and the metal-rich ones in panel e). The insets in panels c)- e) show the high-reddening range. Note that the two GCs with $\mbox{$E(B-V)$ }\approx4.8\ and\ 5.5$ (inset of panel c)) have no metallicity determinations.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{4351fig2.eps} \end{figure}$ Figure 2: Spatial projections of the heliocentric positions of the metal-rich GCs of the GC05 ( left panels) and reduced ( right panels) samples. The reduced sample produces more concentrated distributions. The outlier metal-rich GCs NGC 6356 and Palomar 11 are identified in panels b), d) and f).
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{4351fig3.eps} \end{figure}$ Figure 3: Same as Fig. 2 for the metal-poor GCs.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4351fig4.eps} \end{figure}$ Figure 4: One-dimensional distribution functions of the reduced sample ( top panels), metal-poor ( middle panels), and metal-rich GCs ( bottom panels). The profiles were fitted with the exponential-decay function $\rm\phi(\xi)\propto e^{-\left\vert\frac{\xi-\xi_o}{\xi_h}\right\vert}$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4351fig5.eps} \end{figure}$ Figure 5: Radial density profiles of the GCs in the reduced sample as a function of Galactocentric distance. Panel a) - metal-poor GCs; panel b) - metal-rich; panel c) - all GCs. Dashed line: single power-law fit for large Galactocentric distances. Solid line: fit of $\rho (R)=\rho _{\rm o}/(1+R/R_{\rm C})^{\alpha }$ . Insets: fit of Sérsic's law $\rho(R)=a~{\rm e}^{-b\left[\left(R/R_{\rm C}\right)^{(1/n)}-1\right]}$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{4351fig6.eps} \end{figure}$ Figure 6: Radial density profiles of the metal-rich GCs in the reduced sample measured with spherically symmetric volume densities on oblateness-corrected ( top panel) and oblate ( bottom panel) spatial geometries.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{4351fig2.eps} \end{figure}$	Figure 2: Spatial projections of the heliocentric positions of the metal-rich GCs of the GC05 ( left panels) and reduced ( right panels) samples. The reduced sample produces more concentrated distributions. The outlier metal-rich GCs NGC 6356 and Palomar 11 are identified in panels b), d) and f).
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{4351fig3.eps} \end{figure}$	Figure 3: Same as Fig. 2 for the metal-poor GCs.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4351fig4.eps} \end{figure}$	Figure 4: One-dimensional distribution functions of the reduced sample ( top panels), metal-poor ( middle panels), and metal-rich GCs ( bottom panels). The profiles were fitted with the exponential-decay function $\rm\phi(\xi)\propto e^{-\left\vert\frac{\xi-\xi_o}{\xi_h}\right\vert}$ .
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{4351fig6.eps} \end{figure}$	Figure 6: Radial density profiles of the metal-rich GCs in the reduced sample measured with spherically symmetric volume densities on oblateness-corrected ( top panel) and oblate ( bottom panel) spatial geometries.
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