The evolution of the large scale structure of the universe since z=1

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.

Level thesis:degree_level

thesis.doctoral

Grantor dc:publisher

Universität Heidelberg

Year

2001

Author dc:creator

• Phleps, Stefanie

Contributors dc:contributor

• Meisenheimer, Klaus

Repository record source_url

http://www.ub.uni-heidelberg.de/archiv/1824

OAI identifier oai:identifier

oai:archiv.ub.uni-heidelberg.de:1824