All Figures

$\begin{figure} \par\includegraphics[width=11cm,clip]{ms3788f1.eps} \end{figure}$ Figure 1: Digitized Sky Survey images of the galaxies IC 10, Leo A and Sextans A. The size of the IC 10 frame is $30\hbox {$^\prime $ }\times 30\hbox {$^\prime $ }$ , of Leo A and Sextans A $14\hbox {$^\prime $ }\times 12\hbox {$^\prime $ }$ . North is at the top, East to the left. Candidate PNe are marked with a cross and their id. number as in Table 1.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{ms3788f2.ps} \end{figure}$ Figure 2: The number of PNe in galaxies in or near the Local Group, versus the V-band luminosity in solar units. The dotted line shows the expected numbers based on a total number of PNe in the MW of 23 000. The dashed line is fitted to the known population in the LMC. Filled squares indicate LG gaseous galaxies, triangles indicate spheroidal galaxies and open circles show the NGC 3109 group.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{ms3788f3.ps} \end{figure}$ Figure 3: The ratio between the observed and expected number of PNe ( $\log~N_{\rm PN}$ - ( $\log~(L_V)-6.92$ ), see text) as a function of the metallicity of the galaxy (upper panel) or the ratio between carbon and M stars (lower panel). Squares are gas-rich local group galaxies, encircled squares are the three main LG spirals (M33, the Milky Way and M 31). Triangles are gas-poor spheroidal types and circles the galaxies probably not bound to the LG. In the lower panel only dwarf galaxies are shown.
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In the text

$\begin{figure} \par\includegraphics[width=10cm,clip]{ms3788f4.eps} \end{figure}$ Figure 4: The expected number of PNe vs. the absolute magnitude (M_*) of the brightest PN, before (panel on the left) and after (panel on the right) metallicity correction following Dopita et al. (1992) prescription. For M 31, LMC and SMC we report the magnitude of the cutoff of their PNLFs with errors from Ciardullo et al. (2002). For M 33 the magnitude of the cutoff is from Durrell et al. (2003). The horizontal line show the magnitude of the PNLF cutoff M_*=-4.53 as expected for a galaxy with a large population size. Dashed lines mark 1-mag around M_*=-4.53.
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In the text

$\begin{figure} \par\includegraphics[width=11cm,clip]{ms3788f1.eps} \end{figure}$	Figure 1: Digitized Sky Survey images of the galaxies IC 10, Leo A and Sextans A. The size of the IC 10 frame is $30\hbox {$^\prime $ }\times 30\hbox {$^\prime $ }$ , of Leo A and Sextans A $14\hbox {$^\prime $ }\times 12\hbox {$^\prime $ }$ . North is at the top, East to the left. Candidate PNe are marked with a cross and their id. number as in Table 1.
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$\begin{figure} \par\includegraphics[width=12cm,clip]{ms3788f2.ps} \end{figure}$	Figure 2: The number of PNe in galaxies in or near the Local Group, versus the V-band luminosity in solar units. The dotted line shows the expected numbers based on a total number of PNe in the MW of 23 000. The dashed line is fitted to the known population in the LMC. Filled squares indicate LG gaseous galaxies, triangles indicate spheroidal galaxies and open circles show the NGC 3109 group.
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