All Figures

$\begin{figure} \par\includegraphics[width=18cm,clip]{3660fg01.eps}\end{figure}$ Figure 1: Images of representative galaxies of all 4 morphological types, at two apparent magnitudes. Note that the grey scale contrasts are not identical in the 8 frames. As we explained in the text, for the fainter galaxies we sometimes used the brightness profile as additional evidence for the morphological classification.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3660fg02.eps}\end{figure}$ Figure 2: The cumulative rate of agreement between the results of different classifiers, to within n broad Hubble types. Clearly, the performance of the different classifications is very similar.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3660fg03.eps}\end{figure}$ Figure 3: The dependence of the fraction of ELG on the normalised projected cluster-centric distance R/r₂₀₀, for all galaxies in the 67 clusters with at least 20 member galaxies and with z<0.1(filled circles). Also shown are the fractions for the individual galaxy classes.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3660fg04.eps}\end{figure}$ Figure 4: For each of the 66 combinations of $P_{\rm E^*}$ and $P_{\rm S^*}$ , as determined by de Theije & Katgert from a PCA/ANN analysis of the ENACS spectra, we show the "mean'' morphological type (see text).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3660fg05.eps}\end{figure}$ Figure 5: The normalized cumulative $P_{\rm S^*}$ -distributions of the 4 morphological galaxy classes and of the emission-line galaxies.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3660fg06.eps}\end{figure}$ Figure 6: The mean spectra for ellipticals (E), S0 galaxies, early spirals (Se) and late spirals (Sl), without emission lines (non-ELG). The mean spectrum was determined by averaging individual spectra in which the mean flux was normalised to one (arbitrary units). The individual galaxy spectra were not spectro-photometrically calibrated, but have been corrected for the spectral response of spectrograph and detector.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{3660fg07.eps}\end{figure}$ Figure 7: The difference (in magnitudes) between the spectra of the faint (M_R>-20) and bright ( $M_R \le -20$ ) non-ELG galaxies, for different morphologies. The difference spectra have zero mean flux, but were shifted so that they could be shown in one figure.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,height=5.5cm,clip]{3660fg08.eps}\end{figure}$ Figure 8: The mean colors $\langle$ "v-g'' $\rangle$ (top) and $\langle$ "b-v'' $\rangle$ (bottom) of the various morphological classes. Note that the colors are instrumental, because the spectra were not spectro-photometrically calibrated. For each of the 4 galaxy classes we show the colors for bright ( $M_R \le -20$ ) galaxies (filled symbols) and faint (M_R>-20) galaxies (open symbols) separately.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{3660fg09.eps}\end{figure}$ Figure 9: The strengths of the absorption lines. Filled and open symbols refer to the bright and faint subsets of the 4 galaxy classes. The upper 3 panels show the strengths of the 3 metal line(-complexe)s, and the lower panel the strength of the H $\delta$ line. For the definition of the line-strength $\Delta m$ , see the text; absorption-line strength increases upwards.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{3660fg10.eps}\end{figure}$ Figure 10: The relation between color and metallicity. Because the $\langle$ "v-g'' $\rangle$ and $\langle$ "b-v'' $\rangle$ colors are very strongly correlated, we only show the correlation with $\langle$ "v-g'' $\rangle$ color. The metallicity was derived by combining the three measured line-strengths as described in the text. Note that the combined metallicity is given on the CaII-scale.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{3660fg11.eps}\end{figure}$ Figure 11: The ratio (in magnitudes) between the mean non-ELG and ELG spectra for different morphological classes. The residual spectra all have identical (i.e. zero) mean flux, but they were offset to be shown in one figure.
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In the text

$\begin{figure} \par\includegraphics[width=18cm,clip]{3660fg01.eps}\end{figure}$	Figure 1: Images of representative galaxies of all 4 morphological types, at two apparent magnitudes. Note that the grey scale contrasts are not identical in the 8 frames. As we explained in the text, for the fainter galaxies we sometimes used the brightness profile as additional evidence for the morphological classification.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3660fg02.eps}\end{figure}$	Figure 2: The cumulative rate of agreement between the results of different classifiers, to within n broad Hubble types. Clearly, the performance of the different classifications is very similar.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3660fg03.eps}\end{figure}$	Figure 3: The dependence of the fraction of ELG on the normalised projected cluster-centric distance R/r₂₀₀, for all galaxies in the 67 clusters with at least 20 member galaxies and with z<0.1(filled circles). Also shown are the fractions for the individual galaxy classes.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3660fg04.eps}\end{figure}$	Figure 4: For each of the 66 combinations of $P_{\rm E^}$ and $P_{\rm S^}$ , as determined by de Theije & Katgert from a PCA/ANN analysis of the ENACS spectra, we show the "mean'' morphological type (see text).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3660fg05.eps}\end{figure}$	Figure 5: The normalized cumulative $P_{\rm S^*}$ -distributions of the 4 morphological galaxy classes and of the emission-line galaxies.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{3660fg07.eps}\end{figure}$	Figure 7: The difference (in magnitudes) between the spectra of the faint (M_R>-20) and bright ( $M_R \le -20$ ) non-ELG galaxies, for different morphologies. The difference spectra have zero mean flux, but were shifted so that they could be shown in one figure.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{3660fg09.eps}\end{figure}$	Figure 9: The strengths of the absorption lines. Filled and open symbols refer to the bright and faint subsets of the 4 galaxy classes. The upper 3 panels show the strengths of the 3 metal line(-complexe)s, and the lower panel the strength of the H $\delta$ line. For the definition of the line-strength $\Delta m$ , see the text; absorption-line strength increases upwards.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{3660fg10.eps}\end{figure}$	Figure 10: The relation between color and metallicity. Because the $\langle$ "v-g'' $\rangle$ and $\langle$ "b-v'' $\rangle$ colors are very strongly correlated, we only show the correlation with $\langle$ "v-g'' $\rangle$ color. The metallicity was derived by combining the three measured line-strengths as described in the text. Note that the combined metallicity is given on the CaII-scale.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{3660fg11.eps}\end{figure}$	Figure 11: The ratio (in magnitudes) between the mean non-ELG and ELG spectra for different morphological classes. The residual spectra all have identical (i.e. zero) mean flux, but they were offset to be shown in one figure.
Open with DEXTER