German Title: Die Entwicklung der grossskaligen Struktur im Universum seit z=1

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Abstract

In this thesis, the evolution of galaxy clustering from a redshift of $zsim1$ to the present epoch is investigated. The data used for this analysis were $sim4000$ galaxies in four fields of the Calar Alto Deep Imaging Survey (CADIS). The galaxies have luminosities brighter than $Ileq23^{mag}$, and redshifts with an error of $sigma_z=0.017$. The amplitude of the three-dimensional correlation function is estimated by deprojecting two-dimensional correlation functions. The reliability of the deprojection methods of the angular and projected correlation function is tested on the Las Campanas Redshift Survey (LCRS). Both angular and projected correlation function are calculated for different redshift bins, as local measurement the LCRS data is used. To facilitate the direct comparison of the two surveys, the influence of the redshift errors on the projected correlation function have to be taken into account. For evolution of the clustering strength the ansatz $xi(r_{com},z)propto(1+z)^q$ is used. For the galaxies as a whole the evolution parameter turns out to be $qapprox-1.9$, according to the prediction of linear theory. A formal dependency on the cosmology is presumably due to the small number of fields observed. However, the measured clustering growth clearly depends on Hubble type. At $zsim1$ early type galaxies are already much stronger clustered, an increase with $qsimeq-1$ is sufficient to explain the present day amplitude of the correlation function.