All Figures

$\begin{figure} \par\includegraphics[width=77mm,clip]{0533f1.ps}\end{figure}$ Figure 1: Histogram of FWHM values for objects fitted during the first round of profile fitting. The narrow sequence of unresolved objects with FWHM $\approx 0$ is clearly seen. The vertical dashed line indicates the criteria used to select cluster candidates.
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In the text

$\begin{figure} \includegraphics[width=5.5cm,clip]{aa0533f2.eps}\end{figure}$ Figure 2: Illustrations of comment codes a-i. Please see Table 2 for the full comments associated with each code. Each panel shows a $4\hbox {$^{\prime \prime }$ }\times 4\hbox {$^{\prime \prime }$ }$ section around the cluster candidate.
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In the text

$\begin{figure} \par\includegraphics[width=20mm,clip]{0533f3a.ps}\includegraphics... ...=20mm,clip]{0533f3c.ps}\includegraphics[width=20mm,clip]{0533f3d.ps}\end{figure}$ Figure 3: Examples of objects classified as Type 2 (uncertain).
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In the text

$\begin{figure} \includegraphics[width=8.5cm,clip]{aa0533f4.eps}\end{figure}$ Figure 4: Two examples of how the appearance of cluster candidates can change dramatically depending on bandpass.
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In the text

$\begin{figure} \par\includegraphics[width=74mm,clip]{0533f5.ps}\end{figure}$ Figure 5: Size distribution for cluster candidates identified in ground-based surveys.
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In the text

$\begin{figure} \par\includegraphics[width=80mm,clip]{0533f6.ps}\end{figure}$ Figure 6: Magnitude distributions for ground-selected cluster candidates with FWHM <0.5 pc ( top) and FWHM >0.5 pc ( bottom). Sizes are from EFF fits with fixed $\alpha =1.5$ .
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In the text

$\begin{figure} \includegraphics[width=8.5cm,clip]{aa0533f7.eps}\end{figure}$ Figure 7: Examples of objects identified as clusters from the ground, but which are unresolved according to the ISHAPE fits.
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In the text

$\begin{figure} \par\includegraphics[width=75mm,clip]{0533f8.ps}\end{figure}$ Figure 8: Specific U-band luminosity (T_L(U)) vs. area-normalised star formation rate ( $\Sigma _{\rm SFR}$ ) for original ground-based data and updated values (filled diamonds) based on contamination rates estimated from HST data (Table 8).
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In the text

$\begin{figure} \par\includegraphics[width=78mm,clip]{0533f9.ps}\end{figure}$ Figure 9: Mean FWHM ( top) and effective radii ( bottom) for stellar clusters versus parent galaxy distance modulus.
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In the text

$\begin{figure} \par\includegraphics[width=76mm,clip]{0533f10.ps}\end{figure}$ Figure 10: Mean FWHM ( top) and effective radii ( bottom) for stellar clusters versus parent galaxy $\Sigma _{\rm SFR}$ (derived from IRAS far-infrared luminosities, as described in Paper III).
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In the text

$\begin{figure} \par\includegraphics[width=75mm,clip]{0533f11.ps}\end{figure}$ Figure 11: Distributions of FWHM and effective radii for the combined cluster samples. In the lower panel, the hatched and outlined histograms are for clusters with $1<\alpha <5$ and $\alpha <5$ , respectively.
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In the text

$\begin{figure} \par\includegraphics[width=73mm,clip]{0533f12.ps}\end{figure}$ Figure 12: Distribution of envelope slopes in four age bins.
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In the text

$\begin{figure} \par\includegraphics[width=84mm,clip]{0533f13.ps}\end{figure}$ Figure 13: Envelope slopes in different mass bins for two different ages.
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In the text

$\begin{figure} \par\includegraphics[width=84mm,clip]{0533f14.ps}\end{figure}$ Figure 14: Cluster FWHM versus age ( top) and mass ( bottom). The dashed curve in the lower panel represents a relation corresponding to FWHM $\propto M^{1/3}$ (constant density). The solid line is a least-squares power-law fit to FWHM vs. mass.
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In the text

$\begin{figure} \par\includegraphics[width=84mm,clip]{0533f15.ps}\end{figure}$ Figure 15: Effective radius ( $R_{\rm eff}$ ) versus age ( top) and mass ( bottom panel). Clusters with $\alpha \leq 1$ and $\alpha >1$ are shown with diamonds and plus markers, respectively. The dashed curve in the lower panel represents a relation corresponding $\mbox{$R_{\rm eff}$ }\propto M^{1/3}$ (constant density). The solid line is a least-squares power-law fit to $\mbox{$R_{\rm eff}$ }$ vs. mass for clusters with $\alpha >1$ .
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In the text

$\begin{figure} \par\includegraphics[width=80mm,clip]{0533f16.ps}\end{figure}$ Figure 16: Histograms of the $R_{\rm eff}$ distributions in four mass ranges. Filled histograms are for clusters with $\alpha >1$ , while the outlined histograms include clusters with $\alpha \leq 1$ . The shaded areas indicate the range of sizes in each mass interval corresponding to an $\mbox{$R_{\rm eff}$ }\propto M^{1/3}$ relation.
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In the text

$\begin{figure} \par\includegraphics[width=77mm,clip]{0533f1.ps}\end{figure}$	Figure 1: Histogram of FWHM values for objects fitted during the first round of profile fitting. The narrow sequence of unresolved objects with FWHM $\approx 0$ is clearly seen. The vertical dashed line indicates the criteria used to select cluster candidates.
Open with DEXTER

$\begin{figure} \includegraphics[width=5.5cm,clip]{aa0533f2.eps}\end{figure}$	Figure 2: Illustrations of comment codes a-i. Please see Table 2 for the full comments associated with each code. Each panel shows a $4\hbox {$^{\prime \prime }$ }\times 4\hbox {$^{\prime \prime }$ }$ section around the cluster candidate.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=20mm,clip]{0533f3a.ps}\includegraphics... ...=20mm,clip]{0533f3c.ps}\includegraphics[width=20mm,clip]{0533f3d.ps}\end{figure}$	Figure 3: Examples of objects classified as Type 2 (uncertain).
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$\begin{figure} \includegraphics[width=8.5cm,clip]{aa0533f4.eps}\end{figure}$	Figure 4: Two examples of how the appearance of cluster candidates can change dramatically depending on bandpass.
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$\begin{figure} \par\includegraphics[width=74mm,clip]{0533f5.ps}\end{figure}$	Figure 5: Size distribution for cluster candidates identified in ground-based surveys.
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$\begin{figure} \par\includegraphics[width=80mm,clip]{0533f6.ps}\end{figure}$	Figure 6: Magnitude distributions for ground-selected cluster candidates with FWHM <0.5 pc ( top) and FWHM >0.5 pc ( bottom). Sizes are from EFF fits with fixed $\alpha =1.5$ .
Open with DEXTER

$\begin{figure} \includegraphics[width=8.5cm,clip]{aa0533f7.eps}\end{figure}$	Figure 7: Examples of objects identified as clusters from the ground, but which are unresolved according to the ISHAPE fits.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=75mm,clip]{0533f8.ps}\end{figure}$	Figure 8: Specific U-band luminosity (T_L(U)) vs. area-normalised star formation rate ( $\Sigma _{\rm SFR}$ ) for original ground-based data and updated values (filled diamonds) based on contamination rates estimated from HST data (Table 8).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=78mm,clip]{0533f9.ps}\end{figure}$	Figure 9: Mean FWHM ( top) and effective radii ( bottom) for stellar clusters versus parent galaxy distance modulus.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=76mm,clip]{0533f10.ps}\end{figure}$	Figure 10: Mean FWHM ( top) and effective radii ( bottom) for stellar clusters versus parent galaxy $\Sigma _{\rm SFR}$ (derived from IRAS far-infrared luminosities, as described in Paper III).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=75mm,clip]{0533f11.ps}\end{figure}$	Figure 11: Distributions of FWHM and effective radii for the combined cluster samples. In the lower panel, the hatched and outlined histograms are for clusters with $1<\alpha <5$ and $\alpha <5$ , respectively.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=73mm,clip]{0533f12.ps}\end{figure}$	Figure 12: Distribution of envelope slopes in four age bins.
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$\begin{figure} \par\includegraphics[width=84mm,clip]{0533f13.ps}\end{figure}$	Figure 13: Envelope slopes in different mass bins for two different ages.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=84mm,clip]{0533f14.ps}\end{figure}$	Figure 14: Cluster FWHM versus age ( top) and mass ( bottom). The dashed curve in the lower panel represents a relation corresponding to FWHM $\propto M^{1/3}$ (constant density). The solid line is a least-squares power-law fit to FWHM vs. mass.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=80mm,clip]{0533f16.ps}\end{figure}$	Figure 16: Histograms of the $R_{\rm eff}$ distributions in four mass ranges. Filled histograms are for clusters with $\alpha >1$ , while the outlined histograms include clusters with $\alpha \leq 1$ . The shaded areas indicate the range of sizes in each mass interval corresponding to an $\mbox{$R_{\rm eff}$ }\propto M^{1/3}$ relation.
Open with DEXTER