All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{galleti_fig1.eps} \end{figure}$ Figure 1: Residuals of the astrometric solution for PSC (filled circles) and XSC (crosses) sources. The histograms show the RMS of RA ( top panel) and Dec ( right panel). A circle of radius $r=1 \hbox {$^{\prime \prime }$ }$ has been superposed to the plot as a reference. The standard deviation of the distributions of the residuals in each directions (histograms) are also reported within the corresponding boxes.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{galleti_fig2.eps} % \end{figure}$ Figure 2: Comparison between the 2MASS photometry and previous NIR-photometry from the Master Catalogue. Left panels: 2MASS sources identifyied in the XSC. Right panels: 2MASS sources identifyied in the PSC. The extended source are in left panel and the points source in righ panel.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{galleti_fig3.eps} \end{figure}$ Figure 3: Comparison between the photometry of the final sample (corrected PSC+XSC) and previous NIR-photometry. The dashed lines encloses the range of $\pm$ 0.2 mag.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{galleti_fig4.eps} \end{figure}$ Figure 4: V-K vs. various optical colors for the confirmed globular clusters (small points) and for the confirmed galaxies (filled circles).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{galleti_fig5.eps} \end{figure}$ Figure 5: V-K vs. optical colors for the not-yet-confirmed candidates globular cluster (small open circles) and for controversial objects that have been classified as clusters by some authors and as galaxies by others (filled squares).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{galleti_fig2.eps} % \end{figure}$	Figure 2: Comparison between the 2MASS photometry and previous NIR-photometry from the Master Catalogue. Left panels: 2MASS sources identifyied in the XSC. Right panels: 2MASS sources identifyied in the PSC. The extended source are in left panel and the points source in righ panel.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{galleti_fig3.eps} \end{figure}$	Figure 3: Comparison between the photometry of the final sample (corrected PSC+XSC) and previous NIR-photometry. The dashed lines encloses the range of $\pm$ 0.2 mag.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{galleti_fig4.eps} \end{figure}$	Figure 4: V-K vs. various optical colors for the confirmed globular clusters (small points) and for the confirmed galaxies (filled circles).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{galleti_fig5.eps} \end{figure}$	Figure 5: V-K vs. optical colors for the not-yet-confirmed candidates globular cluster (small open circles) and for controversial objects that have been classified as clusters by some authors and as galaxies by others (filled squares).
Open with DEXTER