$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3734fig1.eps} \end{figure}$ Figure 1: Central surface brightness versus $b_j-K_{\rm s}$ colour for matched XSC objects. Open (filled) circles are cluster (background) early types, squares intermediate types and triangles late types.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{3734fig2} \end{figure}$ Figure 2: Optical - IR colour, $b_j-K_{\rm s}$ , versus redshift for matched PSC objects with galaxy spectra. Different optical image morphologies are indicated. The model tracks are from Poggianti (1997).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{3734fig3}\end{figure}$ Figure 3: A b_j (Drinkwater et al. 2001a) vs. $K_{\rm s}$ plot of our XSC sample, PSC sample and 6dfGRS completeness limits. XSC magnitudes were slightly underestimated in the 2MASS 2nd data release (see C2001) accounting for some of the gap between the XSC and PSC galaxies.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3734fig1.eps} \end{figure}$	Figure 1: Central surface brightness versus $b_j-K_{\rm s}$ colour for matched XSC objects. Open (filled) circles are cluster (background) early types, squares intermediate types and triangles late types.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=9cm,clip]{3734fig2} \end{figure}$	Figure 2: Optical - IR colour, $b_j-K_{\rm s}$ , versus redshift for matched PSC objects with galaxy spectra. Different optical image morphologies are indicated. The model tracks are from Poggianti (1997).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=9cm,clip]{3734fig3}\end{figure}$	Figure 3: A b_j (Drinkwater et al. 2001a) vs. $K_{\rm s}$ plot of our XSC sample, PSC sample and 6dfGRS completeness limits. XSC magnitudes were slightly underestimated in the 2MASS 2nd data release (see C2001) accounting for some of the gap between the XSC and PSC galaxies.
Open with DEXTER