All Figures

$\begin{figure} \par\includegraphics[width=18cm,height=8.1cm,clip]{0157fi01.ps} \end{figure}$ Figure 1: K-band image ( left panel) and luminosity-weighted map ( right panel) for the field of galaxies A 2163B. The image is centered at $\rm RA= 16h ~ 15m ~ 48s$ and $\rm Dec=-06^\circ 02'10''$ , and was smoothed for the plot by a Gaussian convolution. The scale and the orientation of the image are shown in the lower left corner of the left panel. In the same panel, the crosses indicates the positions of the radio sources in the field. In the right plot, the circles enclose the regions that were used to calculate the LF in the higher density environment (see Sect. 3.2).
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In the text

$\begin{figure} \par\includegraphics[width=12cm,height=12cm,clip]{0157fi02.ps} \end{figure}$ Figure 2: Optical-NIR CM diagrams for galaxies in the field of A 2163B. For each panel, the slope and zeropoint of the CM relations are shown in the lower left corner, while the error bars from the left to the right denote the averaged uncertainties on colours and magnitudes at $K_{\rm T}=15$ and $K_{\rm T}=18$ , respectively.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=8.5cm,height=8.5cm,clip]{0157fi03.ps} \end{figure}$ Figure 3: K-band LF of A 2163B. The two curves indicate the best-fit Schecter functions obtained by fitting both $\alpha$ and K^* (solid line) and by fitting only K^* with $\alpha$ fixed to -0.9 (dashed line). In the last case, the three brightest cluster galaxies were excluded from the fit: the first bin was not considered while the galaxy counts for the second bin are marked by the empty circle. Contours in the smaller panel denote $1\sigma$ , $2\sigma$ and $3\sigma$ probability levels, respectively.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=8.5cm,height=8.5cm,clip]{0157fi04.ps} \end{figure}$ Figure 4: K-band LF of A 2163B in the low- and high- density environments. The points and the error bars corresponding to the high density region have been shifted by $\rm +0.1~mag$ for sake of semplicity. The curves show the best fitting Schechter functions.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=8.4cm,height=8.4cm,clip]{0157fi05.ps}\vspace*{-2mm} \end{figure}$ Figure 5: Distribution of photometric redshifts. The solid line and thedashed region indicate the estimate of the cluster redshift, $z_{\rm c}$ , and the relative uncertainty ( $1\sigma$ standard interval). Dashed lines enclosethe range of z $\rm_p$ , $\Delta z$ , used to select cluster members.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=13.7cm,height=11.7cm,clip]{0157fi06.ps} \end{figure}$ Figure 6: 2D fits of galaxies in the K-band image. For each plot, from left to right, the galaxy image, the 2D model and the residual map are shown. The size of the horizontal white bar is 5''.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=10cm,height=10cm,clip]{0157fi07.ps} \end{figure}$ Figure 7: Comparison of structural parameter in the optical. For each panels, differences are computed between R and I bands. The correlation between effective parameters is shown inside the lower right panel.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=10cm,height=10cm,clip]{0157fi08.ps} \end{figure}$ Figure 8: Same of Fig. 7 for the R- and K-band parameters.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=12.2cm,height=6.2cm,clip]{0157fi09.ps} \end{figure}$ Figure 9: Distributions of V-R and V-K colour gradients. The mean values are marked by a solid line.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=13.3cm,height=6.8cm,clip]{0157fi10.ps} \end{figure}$ Figure 10: Kormendy relations in R and K bands. Dashed lines mark the completeness magnitudes and the surface brightness cut ( right panel) of each sample. The typical uncertainties on the effective parameters are indicated by the ellipses in the lower left corner of each panel. The ellipses mark the contours that enclose a probability of $68\%$ for a 2D normal deviate.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=13cm,height=6.5cm,clip]{0157fi11.ps} \end{figure}$ Figure 11: Ratios of optical to NIR effective radii and colour gradients are plotted versus the logarithm of the K-band effective radius. The dashed lines mark the mean values of $\log R_{\rm e}^R / R_{\rm e}^K$ and grad(V-K) in the left and right panels, respectively. Data were binned in order to have the same number of points in each bin. The solid lines mark the best-fits to the data, while the dot-dashed lines indicate the $1\sigma$ confidence intervals.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=11cm,height=11cm,clip]{0157fi12.ps} \end{figure}$ Figure 12: Distribution of galaxies in the space of structural parameters. Upper-left: ${\log R_{\rm e}}$ - ${\log n}$ relation. The ellipses is in the upper plots are the $68\%$ probability contours. The solid and dot-dashed lines are the best-fit and the $1\sigma$ confidence lines, respectively. The region affected by the magnitude selection is filled by a dashed pattern. Upper-right: edge-on projection of the PHP with the best-fit relation marked by a solid line. Lower-left: "long'' edge-on projection of the PHP. Lower-right: face-on view of the PHP. The shaded region is delimited on the right by the line that results from the intersection of the plane $K_{\rm T}=\rm const.$ with a plane parallel to the PHP but with zeropoint $\rm c+2 \cdot \sigma _c$ .
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In the text

$\begin{figure} \par\includegraphics[width=12cm,height=12cm,clip]{0157fi02.ps} \end{figure}$	Figure 2: Optical-NIR CM diagrams for galaxies in the field of A 2163B. For each panel, the slope and zeropoint of the CM relations are shown in the lower left corner, while the error bars from the left to the right denote the averaged uncertainties on colours and magnitudes at $K_{\rm T}=15$ and $K_{\rm T}=18$ , respectively.
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$\begin{figure} \par\includegraphics[angle=0,width=8.5cm,height=8.5cm,clip]{0157fi04.ps} \end{figure}$	Figure 4: K-band LF of A 2163B in the low- and high- density environments. The points and the error bars corresponding to the high density region have been shifted by $\rm +0.1~mag$ for sake of semplicity. The curves show the best fitting Schechter functions.
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$\begin{figure} \par\includegraphics[angle=0,width=8.4cm,height=8.4cm,clip]{0157fi05.ps}\vspace*{-2mm} \end{figure}$	Figure 5: Distribution of photometric redshifts. The solid line and thedashed region indicate the estimate of the cluster redshift, $z_{\rm c}$ , and the relative uncertainty ( $1\sigma$ standard interval). Dashed lines enclosethe range of z $\rm_p$ , $\Delta z$ , used to select cluster members.
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$\begin{figure} \par\includegraphics[angle=0,width=13.7cm,height=11.7cm,clip]{0157fi06.ps} \end{figure}$	Figure 6: 2D fits of galaxies in the K-band image. For each plot, from left to right, the galaxy image, the 2D model and the residual map are shown. The size of the horizontal white bar is 5''.
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$\begin{figure} \par\includegraphics[angle=0,width=10cm,height=10cm,clip]{0157fi07.ps} \end{figure}$	Figure 7: Comparison of structural parameter in the optical. For each panels, differences are computed between R and I bands. The correlation between effective parameters is shown inside the lower right panel.
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$\begin{figure} \par\includegraphics[angle=0,width=10cm,height=10cm,clip]{0157fi08.ps} \end{figure}$	Figure 8: Same of Fig. 7 for the R- and K-band parameters.
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$\begin{figure} \par\includegraphics[angle=0,width=12.2cm,height=6.2cm,clip]{0157fi09.ps} \end{figure}$	Figure 9: Distributions of V-R and V-K colour gradients. The mean values are marked by a solid line.
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$\begin{figure} \par\includegraphics[angle=0,width=13.3cm,height=6.8cm,clip]{0157fi10.ps} \end{figure}$	Figure 10: Kormendy relations in R and K bands. Dashed lines mark the completeness magnitudes and the surface brightness cut ( right panel) of each sample. The typical uncertainties on the effective parameters are indicated by the ellipses in the lower left corner of each panel. The ellipses mark the contours that enclose a probability of $68\%$ for a 2D normal deviate.
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