Volume 520, September-October 2010
|Number of page(s)||16|
|Section||Cosmology (including clusters of galaxies)|
|Published online||13 October 2010|
COSEBIs: Extracting the full E-/B-mode information from cosmic shear correlation functions
Argelander-Institut für Astronomie,
Universität Bonn, Auf dem Hügel 71,
53121 Bonn, Germany e-mail: email@example.com
2 Center for Cosmology and Astro-Particle Physics, The Ohio State University, 191 W. Woodruff Ave., Columbus, OH 43210, USA e-mail: firstname.lastname@example.org
3 California Institute of Technology, Dept. of Astronomy, MC 105-24, Pasadena CA 91125, USA e-mail: email@example.com
Accepted: 29 June 2010
Context. Cosmic shear is considered one of the most powerful methods for studying the properties of dark energy in the Universe. As a standard method, the two-point correlation functions (ϑ) of the cosmic shear field are used as statistical measures for the shear field.
Aims. In order to separate the observed shear into E- and B-modes, the latter being most likely produced by remaining systematics in the data set and/or intrinsic alignment effects, several statistics have been defined before. Here we aim at a complete E-/B-mode decomposition of the cosmic shear information contained in the on a finite angular interval.
Methods. We construct two sets of such E-/B-mode measures, namely Complete Orthogonal Sets of E-/B-mode Integrals (COSEBIs), characterized by weight functions between the and the COSEBIs which are polynomials in ϑ or polynomials in ϑ, respectively. Considering the likelihood in cosmological parameter space, constructed from the COSEBIs, we study their information content.
Results. We show that the information grows with the number of COSEBI modes taken into account, and that an asymptotic limit is reached which defines the maximum available information in the E-mode component of the . We show that this limit is reached the earlier (i.e., for a smaller number of modes considered) the narrower the angular range is over which are measured, and it is reached much earlier for logarithmic weight functions. For example, for on the interval 1' ≤ ϑ ≤ 400', the asymptotic limit for the parameter pair (, ) is reached for ~25 modes in the linear case, but already for 5 modes in the logarithmic case. The COSEBIs form a natural discrete set of quantities, which we suggest as method of choice in future cosmic shear likelihood analyses.
Key words: large-scale structure of Universe / gravitational lensing: weak / cosmological parameters / methods: statistical
© ESO, 2010
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