EDP Sciences
Free Access
Volume 389, Number 3, July III 2002
Page(s) 729 - 741
Section Cosmology
DOI https://doi.org/10.1051/0004-6361:20020626
Published online 01 July 2002

A&A 389, 729-741 (2002)
DOI: 10.1051/0004-6361:20020626

B-modes in cosmic shear from source redshift clustering

P. Schneider1, 2, L. van Waerbeke3, 4 and Y. Mellier3, 5

1  Institut f. Astrophysik u. Extr. Forschung, Universität Bonn, Auf dem Hügel 71, 53121 Bonn, Germany
    e-mail: peter@astro.uni-bonn.de
2  Max-Planck-Institut f. Astrophysik, Postfach 1317, 85741 Garching, Germany
3  Institute d'Astrophysique de Paris, 98 bis, boulevard Arago, 75014 Paris, France
4  Canadian Institute for Theoretical Astrophysics, 60 St Georges Str., Toronto, M5S 3H8 Ontario, Canada
5  Observatoire de Paris, DEMIRM/LERMA, 61 avenue de l'Observatoire, 75014 Paris, France

(Received 19 December 2001 / Accepted 19 April 2002 )

Weak gravitational lensing by the large scale structure can be used to probe the dark matter distribution in the Universe directly and thus to probe cosmological models. The recent detection of cosmic shear by several groups has demonstrated the feasibility of this new mode of observational cosmology. In the currently most extensive analysis of cosmic shear, it was found that the shear field contains unexpected modes, so-called , which are thought to be unaccountable for by lensing. can in principle be generated by an intrinsic alignment of galaxies from which the shear is measured, or may signify some remaining systematics in the data reduction and analysis. In this paper we show that in fact are produced by lensing itself. The effect comes about through the clustering of source galaxies, which in particular implies an angular separation-dependent clustering in redshift. After presenting the theory of the decomposition of a general shear field into E- and , we calculate their respective power spectra and correlation functions for a clustered source distribution. Numerical and analytical estimates of the relative strength of these two modes show that the resulting is very small on angular scales larger than a few arcminutes, but its relative contribution rises quickly towards smaller angular scales, with comparable power in both modes at a few arcseconds. The relevance of this effect with regard to the current cosmic shear surveys is discussed; it can not account for the apparent detection of a contribution on large angular scales in the cosmic shear analysis of van Waerbeke et al. (2002).

Key words: cosmology -- gravitational lensing -- large-scale structure of the Universe

Offprint request: P. Schneider, peter@astro.uni-bonn.de

© ESO 2002

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