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 ^ { \prime } \times 13 ^ { \prime } size , placed ( semi- ) randomly into patches which are assumed to be widely separated on the sky and therefore uncorrelated .
Using the aperture mass statistics \left \langle M _ { ap } ^ { 2 } \right \rangle , 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 .