All Figures

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{2471fig1.eps} \end{figure}$ Figure 1: Faber-Jackson relation between the central velocity dispersion and the absolute restframe B magnitude. Local early-type galaxies in the Virgo (small triangles) and Coma (small squares) clusters are from Dressler et al. (1987), the straight line indicates their principal components fit (Ziegler & Bender 1997). Both, ellipticals in distant clusters (large triangles) and in the field (large circles) follow a similar distribution, which is offset to larger luminosities.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{2471fig2.eps} \end{figure}$ Figure 2: The Fundamental Plane in B seen edge-on. The local relation is a principal components fit to elliptical and S0 galaxies in Coma. Ellipticals in distant clusters are indicated by large triangles, distant field ellipticals by large circles. A typical errorbar is displayed in the upper left corner.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{2471fig3.eps} \end{figure}$ Figure 3: Mg_b- $\sigma$ relation between the central velocity dispersion and the central Mg_b line strength. Local galaxies (small symbols) are drawn from the compilation of Thomas et al. (2005) with E and S0 galaxies from the field (cyan circles) and clusters (magenta triangles). Both, ellipticals in distant clusters (green large triangles) and in the field (blue large circles) follow a similar distribution that is offset from the local relation (solid line) towards lower Mg_b-strengths for given $\sigma$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{2471fig4.eps} \end{figure}$ Figure 4: The same samples (and symbols) as in Fig. 3, displaying H $\beta$ vs. Mg_b taken as indicative of age and metallicity [Z/H], respectively. Big open triangle and square denote the mean value of the distant and local cluster sample respectively. The lines connect model values from Thomas et al. (2003) enhanced in Mg so that $\rm [Mg/Fe]=0.3$ . Solid lines correspond to ages of 2, 5, 10, 15 Gyr top to bottom and dashed lines to $\rm [Z/H]=-0.33, 0, 0.33, 0.67$ left to right.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{2471fig5.eps} \end{figure}$ Figure 5: The same samples (and symbols) as in Fig. 3, displaying Fe 5335 vs. Mg_b to investigate the relative enrichment of Fe and Mg. The lines connect model values from Thomas et al. (2003) for a constant age of 10 Gyr. Solid lines correspond to $\rm [Mg/Fe]=0$ , 0.3, 0.5 top to bottom and dashed lines to [Z/H]=-0.33, 0, 0.33, 0.67 left to right.
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In the text

$\begin{figure} \par\includegraphics[width=11.6cm,clip]{2471fig6.eps} \end{figure}$ Figure 6: The samples (and symbols) as in Fig. 3 except that the local sample is now restricted to Category 1 (ages older than $\sim$ 5 Gyr) galaxies. The lines indicate the local relations between age, metallicity [Z/H], and [ $\alpha$ /Fe] with velocity dispersion as derived through Monte Carlo simulations by Thomas et al. (2005), separately for the cluster (solid line) and field sample (dotted line). For the distant galaxies, the respective look-back times have been added to the derived ages.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{2471fig7.eps} \end{figure}$ Figure 7: The Fundamental Plane as in Fig. 2 but restricted to those galaxies for which we could derive light-averaged model ages of their stellar population. The open symbols represent the data "corrected'' for the predicted brightening for each galaxy and nicely match the distribution of the local galaxies.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{2471fig2.eps} \end{figure}$	Figure 2: The Fundamental Plane in B seen edge-on. The local relation is a principal components fit to elliptical and S0 galaxies in Coma. Ellipticals in distant clusters are indicated by large triangles, distant field ellipticals by large circles. A typical errorbar is displayed in the upper left corner.
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$\begin{figure} \par\includegraphics[width=7.4cm,clip]{2471fig5.eps} \end{figure}$	Figure 5: The same samples (and symbols) as in Fig. 3, displaying Fe 5335 vs. Mg_b to investigate the relative enrichment of Fe and Mg. The lines connect model values from Thomas et al. (2003) for a constant age of 10 Gyr. Solid lines correspond to $\rm [Mg/Fe]=0$ , 0.3, 0.5 top to bottom and dashed lines to [Z/H]=-0.33, 0, 0.33, 0.67 left to right.
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$\begin{figure} \par\includegraphics[width=7.4cm,clip]{2471fig7.eps} \end{figure}$	Figure 7: The Fundamental Plane as in Fig. 2 but restricted to those galaxies for which we could derive light-averaged model ages of their stellar population. The open symbols represent the data "corrected'' for the predicted brightening for each galaxy and nicely match the distribution of the local galaxies.
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