To better understand the processes involved in the formation and evolution of elliptical galaxies, 2D models were created in the course of this thesis, which offer the possibilities to constrain the probabilities of various scenarios. The galaxies are members of the clusters MACS J1206.2-0847 and MACS J0416.1-2403 at an average redshift of z ∼ 0.4. Utilizing the, by the models determined structural parameters Sérsic index n and effective radius r e, as well as the total integrated magnitude,

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... ial surface brightness profiles were derived for each of the observed galaxies in each of the twelve bands along with radial profiles for the four colors g475 − I814, r625 − Y105, I814 − H160 and Y105 − H160. Thereupon the logarithmic slopes of these color profiles were determined, as well as the influence on them from the ages and metallicities of the underlying stellar populations. It became apparent that the sizes of the stellar structures on average decrease with increasing wavelength, while n remains constant. Already this observation indicates on average negative color gradients, which are indeed also found. As a consequence one can conclude that the stars are redder in the centers of the galaxies than in the exterior regions. Whether this is the result of radial variations in age and/or metallicity should be answered with the help of models of stellar populations. To that end for the mentioned colors a variety of values were simulated at the redshifts of the galaxy clusters, being based on differing formation redshifts and metallicities. A comparison of the simulated against the measured values yields that both a radial difference in ages and especially a metallicity gradient are the reasons for the observed color gradients. The magnitudes of these gradients favour a scenario, which predicts with progression in time a passive evolution combined with minor dry mergers with mass-poor systems, which are relaxing mainly into a more extended structure than the initial one for very distant (z ∼ 2), compact, but mass-rich [...]