Volume 386, Number 3, May II 2002
|Page(s)||784 - 795|
|Published online||15 May 2002|
Cosmological information from quasar-galaxy correlations induced by weak lensing
Max-Planck-Institut für Astrophysik, PO Box 1317, 85741 Garching, Germany
2 Institut d'Astrophysique de Paris, 98bis Bld. Arago, 75014 Paris, France
Corresponding author: B. Ménard, email@example.com
Accepted: 14 February 2002
The magnification bias of large-scale structures, combined with galaxy biasing, leads to a cross-correlation of distant quasars with foreground galaxies on angular scales of the order of arcminutes and larger. The amplitude and angular shape of the cross-correlation function wQG contain information on cosmological parameters and the galaxy bias factor. While the existence of this cross-correlation has firmly been established, existing data did not allow an accurate measurement of wQG yet, but wide area surveys like the Sloan Digital Sky Survey now provide an ideal database for measuring it. However, wQG depends on several cosmological parameters and the galaxy bias factor. We study in detail the sensitivity of wQG to these parameters and develop a strategy for using the data. We show that the parameter space can be reduced to the bias factor , and , and compute the accuracy with which these parameters can be deduced from SDSS data. Under reasonable assumptions, it should be possible to reach relative accuracies of the order of – for , , and . This method is complementary to other weak-lensing analyses based on cosmic shear.
Key words: cosmology / large-scale structure of Universe / gravitational lensing
© ESO, 2002
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.