Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=82mm,clip]{0547fig1.eps} \end{figure}$ Figure 1: A VLT/FORS2 V-band image of NGC 5236, showing the locations of the two clusters, and inserts showing HST close-ups. Each insert measures $6\hbox {$^{\prime \prime }$ }\times 6\hbox {$^{\prime \prime }$ }$ .
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In the text

$\begin{figure} \par\includegraphics[width=73mm,clip]{0547fig2.eps} \end{figure}$ Figure 2: Illustration of the cross-correlation technique. The solid curve shows the cross-correlation function (CCF) for cluster N5236-502 vs. the template star HR 4226. The three dashed curves show the CCFs for template star HR 5645 broadened by 0 km s^-1, 4 km s^-1 and 8 km s^-1, vs. HR 4226. For clarity, all CCFs have been shifted to a mean of 0 and normalised to a peak value of 1.
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In the text

$\begin{figure} \par\includegraphics[width=75mm,clip]{0547fig3.eps} \end{figure}$ Figure 3: B-V, U-B two-colour diagram indicating the location of the two clusters and the S-sequence of Girardi et al. (1995). The logarithm of the age is indicated along the sequence. The photometry has been corrected for foreground reddening only.
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In the text

$\begin{figure} \par\includegraphics[width=75mm,clip]{0547fig4.eps} \end{figure}$ Figure 4: Comparison of Bruzual & Charlot model colours with observed colours for cluster N5236-502. The horizontal solid and dashed lines indicate the cluster colours corrected for foreground reddening only and assuming an additional A_B=1.0 mag, respectively. The hatched areas indicate the ages and adopted uncertainties. The model colours are shown for Z=0.008, Z=0.020 and Z=0.050.
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In the text

$\begin{figure} \par\includegraphics[width=75mm,clip]{0547fig5.eps} \end{figure}$ Figure 5: Same as Fig. 4, except that cluster N5236-805 is shown.
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In the text

$\begin{figure} \par\includegraphics[width=13.5cm,clip]{0547fig6.eps} \end{figure}$ Figure 6: Absolute M_V magnitudes per solar mass computed for various combinations of stellar mass functions and isochrones. The solid line is from SSP models by Bruzual & Charlot (2000), computed for a Salpeter MF from 0.1-100 $~\mbox{$M_{\odot}$ }$ . The long-dashed, dotted-dashed and triple-dotted-dashed lines are for Salpeter MFs with lower mass limits of $M_{\rm min}=0.01~\mbox{$M_{\odot}$ }, 0.1~\mbox{$M_{\odot}$ }$ and $1.0~\mbox{$M_{\odot}$ }$ , computed from Padua isochrones, while the short-dashed line is for a Kroupa MF with $M_{\rm min}=0.01~\mbox{$M_{\odot}$ }$ . The dotted line is again for the Kroupa MF, but using isochrones from the Geneva group. All models are for solar metallicity. Data for the two clusters are shown with error bars.
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In the text

$\begin{figure} \par\includegraphics[width=82mm,clip]{0547fig1.eps} \end{figure}$	Figure 1: A VLT/FORS2 V-band image of NGC 5236, showing the locations of the two clusters, and inserts showing HST close-ups. Each insert measures $6\hbox {$^{\prime \prime }$ }\times 6\hbox {$^{\prime \prime }$ }$ .
Open with DEXTER

$\begin{figure} \par\includegraphics[width=73mm,clip]{0547fig2.eps} \end{figure}$	Figure 2: Illustration of the cross-correlation technique. The solid curve shows the cross-correlation function (CCF) for cluster N5236-502 vs. the template star HR 4226. The three dashed curves show the CCFs for template star HR 5645 broadened by 0 km s^-1, 4 km s^-1 and 8 km s^-1, vs. HR 4226. For clarity, all CCFs have been shifted to a mean of 0 and normalised to a peak value of 1.
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$\begin{figure} \par\includegraphics[width=75mm,clip]{0547fig3.eps} \end{figure}$	Figure 3: B-V, U-B two-colour diagram indicating the location of the two clusters and the S-sequence of Girardi et al. (1995). The logarithm of the age is indicated along the sequence. The photometry has been corrected for foreground reddening only.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=75mm,clip]{0547fig4.eps} \end{figure}$	Figure 4: Comparison of Bruzual & Charlot model colours with observed colours for cluster N5236-502. The horizontal solid and dashed lines indicate the cluster colours corrected for foreground reddening only and assuming an additional A_B=1.0 mag, respectively. The hatched areas indicate the ages and adopted uncertainties. The model colours are shown for Z=0.008, Z=0.020 and Z=0.050.
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$\begin{figure} \par\includegraphics[width=75mm,clip]{0547fig5.eps} \end{figure}$	Figure 5: Same as Fig. 4, except that cluster N5236-805 is shown.
Open with DEXTER