All Figures

$\begin{figure} \par\includegraphics[width=8.05cm,clip]{5816f1.ps}\end{figure}$ Figure 1: EMMI spectra of the three YMCs with PN candidates. Each panel shows the raw spectrum (thick lines) and the residuals when the best-fitting solar-metallicity model spectrum from González-Delgado et al. (2005) is subtracted (thin lines, blue in the on-line edition).
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In the text

$\begin{figure} \mbox{\parbox{2.8cm}{ N5236-254 \\ \includegraphics[width=2.8cm,... ...{ N3621-1106 \\ \includegraphics[width=2.8cm,clip]{5816f2c.ps} } } \end{figure}$ Figure 2: HST/WFPC2 F606W ( $\approx$ V-band) images of the three YMCs. Each panel is $4\hbox {$^{\prime \prime }$ }$ $\times$ $4\hbox {$^{\prime \prime }$ }$ and the scale is $0\hbox{$.\!\!^{\prime\prime}$ }10$ pixel^-1.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{5816f3a.ps}\vspace*{3mm} \... ...6f3b.ps}\vspace*{3mm} \includegraphics[width=7.5cm,clip]{5816f3c.ps}\end{figure}$ Figure 3: Gaussian emission line fits to the spectra after subtraction of best-fitting solar-metallicity SSP models. In each panel, the thick lines represent the observed spectra while the thin lines (red in the on-line edition) are the Gaussian fits. The regions around H $\beta$ +[O III] and H $\alpha$ +[N II] are shown on the same flux scale.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{5816f4.ps}\end{figure}$ Figure 4: $U\!-\!B$ vs. $B\!-\!V$ two-colour diagram for the three YMCs. Also shown is the S-sequence from Girardi et al. (1995). The numbers along the S-curve indicate the log(age) corresponding to the major tick marks.
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In the text

$\begin{figure} \par\includegraphics[width=6.85cm,clip]{5816f5.ps}\end{figure}$ Figure 5: H-R diagram for the PN candidates in NGC 5236, with $\log$ $T_{\rm eff}$ and $\log L_{\rm cs}/L_{\odot}$ estimated from the [O III] and H $\beta$ lines using the calibrations given by Dopita et al. (1992). Solar-metallicity post-AGB hydrogen-burning evolutionary tracks from Vassiliadis & Wood (1994) are shown for comparison, with the main sequence and core mass (in parentheses) at 10⁴ K indicated. Both objects are consistent with a core mass close to 0.60 $M_\odot$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.35cm,clip]{5816f6.ps}\end{figure}$ Figure 6: Absolute M_V magnitude versus log(age) for all clusters in the spectroscopic sample. The clusters containing PN candidates are indicated with filled circles. Ages in this figure are estimated from broad-band colours.
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{5816f7.ps}\end{figure}$ Figure 7: Stellar lifetime as a function of initial mass, according to Salasnich et al. (2000) model tracks. The curve is a power-law fit to the points.
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In the text

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{5816f8.ps}\end{figure}$ Figure 8: Predicted number of planetary nebulae per 10⁶ $M_\odot$ versus age for a single-aged stellar population, assuming a PN lifetime of 10⁴ years, a Salpeter-like IMF, and the stellar mass-lifetime relation from Fig. 7.
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In the text

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{5816f9.ps}\end{figure}$ Figure 9: Predicted number of planetary nebulae per 10⁶ $L_{\odot ,V}$ versus age for a single-aged stellar population, using the same assumptions as in Fig. 8 and mass-to-light ratios from Bruzual & Charlot SSP models.
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In the text

$\begin{figure} \par\includegraphics[width=8.05cm,clip]{5816f1.ps}\end{figure}$	Figure 1: EMMI spectra of the three YMCs with PN candidates. Each panel shows the raw spectrum (thick lines) and the residuals when the best-fitting solar-metallicity model spectrum from González-Delgado et al. (2005) is subtracted (thin lines, blue in the on-line edition).
Open with DEXTER

$\begin{figure} \mbox{\parbox{2.8cm}{ N5236-254 \\ \includegraphics[width=2.8cm,... ...{ N3621-1106 \\ \includegraphics[width=2.8cm,clip]{5816f2c.ps} } } \end{figure}$	Figure 2: HST/WFPC2 F606W ( $\approx$ V-band) images of the three YMCs. Each panel is $4\hbox {$^{\prime \prime }$ }$ $\times$ $4\hbox {$^{\prime \prime }$ }$ and the scale is $0\hbox{$.\!\!^{\prime\prime}$ }10$ pixel^-1.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{5816f3a.ps}\vspace{3mm} \... ...6f3b.ps}\vspace{3mm} \includegraphics[width=7.5cm,clip]{5816f3c.ps}\end{figure}$	Figure 3: Gaussian emission line fits to the spectra after subtraction of best-fitting solar-metallicity SSP models. In each panel, the thick lines represent the observed spectra while the thin lines (red in the on-line edition) are the Gaussian fits. The regions around H $\beta$ +[O III] and H $\alpha$ +[N II] are shown on the same flux scale.
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$\begin{figure} \par\includegraphics[width=7.4cm,clip]{5816f4.ps}\end{figure}$	Figure 4: $U\!-\!B$ vs. $B\!-\!V$ two-colour diagram for the three YMCs. Also shown is the S-sequence from Girardi et al. (1995). The numbers along the S-curve indicate the log(age) corresponding to the major tick marks.
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$\begin{figure} \par\includegraphics[width=7.35cm,clip]{5816f6.ps}\end{figure}$	Figure 6: Absolute M_V magnitude versus log(age) for all clusters in the spectroscopic sample. The clusters containing PN candidates are indicated with filled circles. Ages in this figure are estimated from broad-band colours.
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$\begin{figure} \par\includegraphics[width=7.3cm,clip]{5816f7.ps}\end{figure}$	Figure 7: Stellar lifetime as a function of initial mass, according to Salasnich et al. (2000) model tracks. The curve is a power-law fit to the points.
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$\begin{figure} \par\includegraphics[width=7.1cm,clip]{5816f8.ps}\end{figure}$	Figure 8: Predicted number of planetary nebulae per 10⁶ $M_\odot$ versus age for a single-aged stellar population, assuming a PN lifetime of 10⁴ years, a Salpeter-like IMF, and the stellar mass-lifetime relation from Fig. 7.
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$\begin{figure} \par\includegraphics[width=7.1cm,clip]{5816f9.ps}\end{figure}$	Figure 9: Predicted number of planetary nebulae per 10⁶ $L_{\odot ,V}$ versus age for a single-aged stellar population, using the same assumptions as in Fig. 8 and mass-to-light ratios from Bruzual & Charlot SSP models.
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