Mathematics – Logic
Scientific paper
Jul 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005phdt........41s&link_type=abstract
PhD (Thesis), Rheinische Friedrich-Wilhelms Universitaet, Bonn, Germany
Mathematics
Logic
1
Weak Gravitational Lensing, Cosmic Shear, Galaxy Biasing, Cosmology
Scientific paper
The statistical relation between the galaxy and dark matter distribution is commonly summarised by the so-called galaxy bias parameters. The dependence of galaxy biasing on galaxy population, redshift and scale will add new pieces to the puzzle of galaxy formation and evolution. Weak gravitational lensing offers the opportunity to probe galaxy bias as a function of redshift and (even non-linear) scale. Chapter 1 of this thesis sets the framework for describing cosmic structure formation. In particular, it introduces statistical quantities that are commonly employed to quantify clustering and galaxy bias. The basics of weak gravitational lensing are described as well. In Chapter 2, a phenomenological model for the evolution of galaxy bias on large linear scales is derived. The important bottom line of this model is that the evolution of galaxy bias, and the relative bias between different galaxy populations, is sensitive to the details of the physical process that locally adds galaxies to, or removes galaxies from, a population of galaxies. The aperture statistics incorporating weak gravitational lensing, that can be used to measure the galaxy bias from contemporary wide-field galaxy surveys, are explained and discussed in Chapter 3. In Chapter 4, the aperture statistics are applied to the Garching-Bonn Deep Survey (GaBoDS). Using these data the dark matter-galaxy bias is measured for a range of scales and three typical redshifts. Chapter 5 applies the weak lensing analysis of galaxy biasing to the COMBO-17 survey to measure galaxy biasing for early-type and late-type galaxies, broadly selected by colour, belonging to four distinct narrow redshift bins. Leaving the topic of galaxy bias, Chapter 6 studies how constraints on the redshifts of source galaxies improve the confidence on cosmological parameters derived from second-order cosmic shear correlations. A new method is introduced, based on the recipe for Monte Carlo simulation in Chapter 3, to estimate the covariances of the statistical errors in measured cosmic shear correlations.
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