$\begin{figure} \par\includegraphics[angle=-90,width=8cm]{6916fig2.eps} \end{figure}$ Figure 2: Galactocentric variation of the [OIII] electron temperatures for PN with progenitor ages of 4-5 Gyr. The empty circles show some nebulae having extremely hot central stars, not included in the linear regression analysis.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm]{6916fig3.eps} \end{figure}$ Figure 3: The inverse correlation between the [OIII] electron temperatures and the O/H abundances for PN in the 4-5 Gyr age bracket. The empty circles show some nebulae having extremely hot central stars.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm]{6916fig1.eps} \end{figure}$	Figure 1: Age distribution of the PN progenitor stars in the Basic Sample of Maciel et al. (2006).
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$\begin{figure} \par\includegraphics[angle=-90,width=8cm]{6916fig2.eps} \end{figure}$	Figure 2: Galactocentric variation of the [OIII] electron temperatures for PN with progenitor ages of 4-5 Gyr. The empty circles show some nebulae having extremely hot central stars, not included in the linear regression analysis.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=-90,width=8cm]{6916fig3.eps} \end{figure}$	Figure 3: The inverse correlation between the [OIII] electron temperatures and the O/H abundances for PN in the 4-5 Gyr age bracket. The empty circles show some nebulae having extremely hot central stars.
Open with DEXTER