Analysis of two-point statistics of cosmic shear: II. Optimizing the survey geometry

Details Analysis of two-point statistics of cosmic shear: II. Optimizing the survey geometry Analysis of two-point statistics of cosmic shear: II. Optimizing the survey geometry

2003-08-07

arxiv.org/abs/astro-ph/0308119v2

Astron.Astrophys.413:465-476,2004

Astronomy and Astrophysics

Astrophysics

13 pages, 11 figures, Appeared in A&A, 2004. Typos corrected and minor changes made to match the published version

Scientific paper

10.1051/0004-6361:20034172

We present simulations of a cosmic shear survey and show how the survey geometry influences the accuracy of determination of cosmological parameters. We numerically calculate the full covariance matrices Cov of two-point statistics of cosmic shear, based on the expressions derived in the first paper of this series. The individual terms are compared for two survey geometries with large and small cosmic variance. We use analyses based on maximum likelihood of Cov and the Fisher information matrix in order to derive expected constraints on cosmological parameters. As an illustrative example, we simulate various survey geometries consisting of 300 individual fields of 13'x13' size, placed (semi-)randomly into patches which are assumed to be widely separated on the sky and therefore uncorrelated. Using the aperture mass statistics, the optimum survey consists of 10 patches with 30 images in each patch. If \Omega_m, \sigma_8 and \Gamma are supposed to be extracted from the data, the minimum variance bounds on these three parameters are 0.17, 0.25 and 0.04 respectively. These variances raise slightly when the initial power spectrum index n_s is also to be determined from the data. The cosmological constant is only poorly constrained.

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