Abstract
Large deviation statistics is implemented to predict the statistics of cosmic densities in cylinders applicable to photometric surveys. It yields few percent accurate analytical predictions for the one-point probability distribution function (PDF) of densities in concentric or compensated cylinders; and also captures the density-dependence of their angular clustering (cylinder bias). All predictions are found to be in excellent agreement with the cosmological simulation Horizon Run 4 in the quasi-linear regime where standard perturbation theory normally breaks down. These results are combined with a simple local bias model that relates dark matter and tracer densities in cylinders and validated on simulated halo catalogues. This formalism can be used to probe cosmology with existing and upcoming photometric surveys like DES, Euclid or WFIRST containing billions of galaxies.
Highlights
Understanding the nature of dark energy is the main challenge cosmology is facing today, as it accounts for ∼70 per cent of the energy budget of our Universe
This paper theoretically models the one- and two-point statistics of densities-in-concentric-cylinders that can be obtained from measured 2D maps of the large scale structure in redshift bins
The general formalism of large deviation statistics for cosmic densities has been presented in Bernardeau et al (2014b); Bernardeau & Reimberg (2016); Uhlemann et al (2016) for 3D spherical cells
Summary
Understanding the nature of dark energy is the main challenge cosmology is facing today, as it accounts for ∼70 per cent of the energy budget of our Universe. This paper theoretically models the one- and two-point statistics of densities-in-concentric-cylinders that can be obtained from measured 2D maps of the large scale structure in redshift bins It focuses on extending and combining Uhlemann et al (2016, 2017a) to projected densities extracted from photometric – quasicylindrical – galaxy surveys with tracer bias. In a highly symmetric configuration such as cylindrical symmetry, one can take advantage of the fact that a non-linear solution to the gravitational dynamics (so-called cylindrical collapse) is known exactly and can be used to accurately probe the non-linear regime This statistics allows us to study the density dependence of gravitational clustering in terms of the conditional one-point PDF of the density within underdense Appendix A contains further details on the treatment in the main text, in particular regarding the cylinder depth and leading order cumulants from perturbation theory, while Appendix B shortly addresses the accuracy of lognormal reconstructions
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