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COSMIC B1 PLUS TEST BOOK

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You came to the right site, we have detail news about Polestar 1 Introduction In recent years, observations of weak lensing by large-scale structure, called cosmic shear, have become an important tool for studying the Universe.

Remarkable constraints on the matter content of the Universe, its expansion history, and the amplitude of the cosmic density fluctuations have been obtained, e. Future cosmic shear surveys are expected to provide essential information on the properties of the dark matter and the dark energy, and on possible deviations of gravity from General Relativity Huterer Cosmic shear surveys aim at inferring the statistical properties of the convergence and shear field from the observed image shapes of distant galaxies.

There are various statistical measures that probe the two-point statistics of the convergence and shear, e.

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Thus, accurate knowledge of the noise properties of the shear correlation estimators is needed for reliable estimates of the errors on the cosmological parameters inferred from cosmic shear surveys.

The number of independent measurements in a cosmic shear survey is usually too small to permit an good estimate of the full covariance of the measured statistics directly from the data. Therefore, one has to resort to covariance estimates obtained by other means.

Supposedly the most accurate, but also computationally by far the most expensive approach is the direct estimation of a cosmic shear covariances from N-body simulations of cosmic structure formation e.

This method requires many independent realisations of the survey field. However, creating sufficiently many realistic mock observations to calculate covariances for future all-sky lensing surveys in various cosmologies and parameter ranges will remain a very challenging computational task in the foreseeable future.

This normal approximation is relatively easy to apply, and requires no additional information besides the convergence correlation itself and the basic survey parameters. Simulations show, however, that the normal approximation tends to underestimate the covariance of two-point lensing statistics e.

A thorough assessment of the accuracy of the halo model approach to cosmic shear covariances e. Normal random fields are arguably the most simple statistical models for the three dimensional matter distribution and the resulting weak-lensing convergence and shear fields.

There are few other classes of random fields that allow one to calculate their higher-order correlations analytically.

Already Hubble noted that observed galaxy densities roughly follow a log-normal distribution. In this work, we derive expressions for the cosmic shear covariance under the assumption that the underlying convergence field follows log-normal statistics.

Furthermore, we derive a simplified version of this log-normal approximation by only retaining the most important terms beyond normal statistics. We use numerical simulations to show that the log-normal and the simplified log-normal approximations reproduce the shear covariances for cosmic shear surveys much more accurately than the normal approximation. Furthermore, we demonstrate that, in contrast to the normal approximation, the uncertainties in the cosmological parameters inferred from the log-normal and the simplified log-normal approximation are in good agreement with the errors resulting from the covariances we estimated from the numerical simulations.

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Cosmic shear covariance: the log-normal approximation

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