All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{9988fig1.eps} \end{figure}$ Figure 1: Close up on the southern side of NGC 1600 using the final SOI/SOAR images. North is upwards and East is to the left of the images. Left panel: I band; right panel: B band.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{9988fig2.ps} \end{figure}$ Figure 2: Panel a): total source counts as a function of calibrated B magnitudes in different elliptical annuli centred on NGC 1600. The solid line shows the source counts in the field region, away from NGC 1600 and from the other galaxies in its group. The semi-major axis range (in pixels) of the different annuli is given in the lower-right. Panels b), c): the symbols are the field-subtracted counts in the same annuli as in panel a). The middle lines are Gaussian fits to the counts, using Eqs. (1) and (2). The lines immediately above and below of each fit are Gaussian functions with a 1 $\sigma$ variation in normalization relative to the fitted one. The final fit, shown by a long dashed line in panel c), was carried out for the range $500 \leq R({\rm pix}) \leq 800$ .
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{9988fig3.ps} \end{figure}$ Figure 3: Panel a): total source counts as a function of calibrated I magnitudes in different elliptical annuli centred on NGC 1600. The solid line shows the source counts in the field region, away from NGC 1600 and from the other galaxies in its group. The semi-major axis range (in pixels) of the different annuli is given in the lower-right. Panels b), c): the symbols are field-subtracted counts in the same annuli as in panel a). The middle lines are Gaussian fits to the counts, using Eqs. (1) and (2). The lines immediately above and below each fit are Gaussian functions with a 1 $\sigma$ variation in normalization relative to the fitted one.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{9988fig4.ps} \end{figure}$ Figure 4: The points correspond to the star cluster density profile measured using source counts in the I (solid circles) and B bands (open circles). The star and the cross in the inner region are linear extrapolations in the figure of the measured densities in I and B, respectively. The curves show the surface brightness profiles in I (dashed line) and B (dotted line), in arbitrary units.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{9988fig5.ps} \end{figure}$ Figure 5: Panel a): total source counts as a function of calibrated (B-I) colours in different elliptical annuli centred on NGC 1600. The solid line shows the source counts in the field region, away from any of the galaxies in NGC 1600 group. Panels b), c): field subtracted counts in the same annuli as in panel a), as indicated.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{9988fig6.ps} \end{figure}$ Figure 6: On-sky distribution of optical and X-ray sources in NGC 1600's group. The small dots are star cluster candidates selected in this work. Only sources with magnitudes and colours in the ranges where an excess is seen relative to the field are are plotted. The large circles are the discrete X-ray sources from Sivakoff et al. (2004). The crosses indicate matched optical/X-ray sources.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{9988fig1.eps} \end{figure}$	Figure 1: Close up on the southern side of NGC 1600 using the final SOI/SOAR images. North is upwards and East is to the left of the images. Left panel: I band; right panel: B band.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{9988fig4.ps} \end{figure}$	Figure 4: The points correspond to the star cluster density profile measured using source counts in the I (solid circles) and B bands (open circles). The star and the cross in the inner region are linear extrapolations in the figure of the measured densities in I and B, respectively. The curves show the surface brightness profiles in I (dashed line) and B (dotted line), in arbitrary units.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{9988fig5.ps} \end{figure}$	Figure 5: Panel a): total source counts as a function of calibrated (B-I) colours in different elliptical annuli centred on NGC 1600. The solid line shows the source counts in the field region, away from any of the galaxies in NGC 1600 group. Panels b), c): field subtracted counts in the same annuli as in panel a), as indicated.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{9988fig6.ps} \end{figure}$	Figure 6: On-sky distribution of optical and X-ray sources in NGC 1600's group. The small dots are star cluster candidates selected in this work. Only sources with magnitudes and colours in the ranges where an excess is seen relative to the field are are plotted. The large circles are the discrete X-ray sources from Sivakoff et al. (2004). The crosses indicate matched optical/X-ray sources.
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