Second Order Corrections to Large Scale Structure Weak Lensing: Background Source Clustering

Details Second Order Corrections to Large Scale Structure Weak Lensing: Background Source Clustering Second Order Corrections to Large Scale Structure Weak Lensing: Background Source Clustering

2002-02-25

arxiv.org/abs/astro-ph/0202465v1

Astronomy and Astrophysics

Astrophysics

7 pages, 4 figures, MNRAS submitted

Scientific paper

We discuss the second order contributions to lensing statistics resulting from the clustering of background sources from which galaxy shape measurements are made in weak lensing experiments. In addition to a previously discussed contribution to the lensing skewness, background source clustering also contributes to the two-point correlation function, such as the angular power spectrum of convergence or shear. At arcminute scales or above, the second order contribution to the angular power spectrum of convergence due to source clustering is below the level of a few percent. The background clustering of sources also results in a non-Gaussian contribution to the power spectrum covariance of weak lensing convergence through a four-point correlation function or a trispectrum in Fourier space. The increase in variance is, at most, a few percent relative to the Gaussian contribution while the band powers are also correlated at the few percent level. The non-Gaussian contributions due to background source clustering is at least an order of magnitude smaller than those resulting from non-Gaussian aspects of the large scale structure due to the non-linear evolution of gravitational perturbations. We suggest that the background source clustering is unlikely to affect the precision measurements of cosmology from upcoming weak lensing surveys.

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