...${\textit{z} \sim 0.2}$[*]
Based on observations collected at European Southern Observatory (ESO 65.O-0251, 69.D-0653). 
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...[*]
Appendices A and B are only available in electronic form at http://www.edpsciences.org 
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...[*]
Table 2 is only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/425/797 
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...$\Omega_\Lambda=0.7$)[*]
We adopt this cosmology throughout the paper. With these parameters the age of the universe is ${\sim}13.5~\rm Gyr$, and the redshift $\rm0.2$corresponds to a lookback time of ${\sim} 2.5~\rm Gyr$. 
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...$\rm Dec=-06^\circ08'55'' $)[*]
The coordinates refer to $\rm J2000$ and define the peak of the X-ray emission (EAB95). 
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... packages[*]
IRAF is distributed by the National Optical Astronomy Observatories, which are operated by the Association of Universities for Research in Astronomy, Inc., under cooperative agreement with the National Science Foundation. 
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... magnitudes[*]
In the following, total magnitudes will be indicated by a pedex $\rm T$. 
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... estimates[*]
We adopted an upper limit of $100\%$ for the uncertainty on the flux. 
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... Sect. 4)[*]
The catalogue is available in electronic form at the CDS. 
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... early-type[*]
Sersic index greater than 2. 
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... photometry[*]
For E(B-V)=0.415, at $z \sim 0.2$, and practically for any galaxy spectral model, we have AB=1.630, AV=1.281, AR=1.049, AI=0.788 and AK=0.152. 
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... galaxies[*]
The only two bins for which galaxy counts deviate by more than $1\sigma $ from the model are at $K_{\rm T} > 17$. We note that limiting the fit range to $K_{\rm T} < 17$does not affect our results, giving $K^*_{0.9}= 15.34 \pm 0.2$. 
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... galaxies[*]
This estimate was obtained by using a Pure Luminosity Evolution model (see e.g. Pozzetti et al. 1996). 
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... objects[*]
We note that in the analysis of the optical-NIR colour gradients we consider only the $N \sim 60$ galaxies brighter than $K_{\rm T} = 16.5$. Proceding as described in La Barbera et al. (2003c), we estimated that at this limiting magnitude, in the redshift range adopted to select cluster members, only ${\sim} 1\%$ of the galaxies are expected to be field contaminants, proving the reliability of the cluster members selection for the surface photometry analysis. 
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... attempt[*]
Disk galaxies are included in the analysis of Sects. 6.1 and 6.2. However, the results are unchanged by excluding these galaxies from the samples. 
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... uncertainties[*]
To this aim, we took into account the correlation of the uncertainties on ${\log R_{\rm e}}$  and ${\rm\langle \mu \rangle_e}$. 
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... slope[*]
We note that Eq. (6) was derived assuming that Eq. (1) still holds once that aperture colours are replaced by the total galaxy colours, $R_{\rm T}-K_{\rm T}$. We verified, in fact, that the values of $\Gamma$ and $\Delta$ do not change significantly by using Kron magnitudes to estimate the galaxy colours. 
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... parameters[*]
The waveband dependence of the Photometric Plane will be investigated in a forthcoming paper, by using a larger sample of galaxies. 
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... IMCOMBINE[*]
The images taken under non-photometric conditions were suitably scaled to the others. 
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Copyright ESO 2004