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Fig. 5.


Upper panels: surface number density of galaxies as a function of the cluster-centric radius (left panels), and distance from Fornax-A (right panels). Middle panels: corresponding cumulative number fractions as function of radii. The black solid lines correspond to the giant galaxies with Mr < −18.5 mag, the green dashed and red dotted lines correspond to dE(N)s and dE(nN)s, respectively, and the blue dash-dotted lines correspond to the late-type dwarfs. For a reference, the purple opaque lines show the cumulative profile for a uniform radial surface-density distribution without any cluster-centric concentration. Bottom panels: deprojected volume densities of the galaxies obtained from the radial surface density profiles using the onion peeling technique described in Appendix B. The shaded areas correspond to the uncertainties in the deprojected profiles, estimated with the Monte Carlo method. The vertical gray dotted lines in the left panels correspond to the virial radius of the cluster.

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