http://arxiv.org/abs/1708.00954
A primary goal of galaxy surveys is to tighten constraints on cosmological parameters, and the power spectrum $P(k)$ is the standard means of doing so. However, at translinear scales $P(k)$ is blind to much of these surveys’ information — information which the log density power spectrum recovers. For discrete fields (such as the galaxy density), $A^$ denotes the statistic analogous to the log density: $A^$ is a “sufficient statistic” in that its power spectrum (and mean) capture virtually all of a discrete survey’s information. However, the power spectrum of $A^$ is biased with respect to the corresponding log spectrum for continuous fields, and to use $P_{A^}(k)$ to constrain the values of cosmological parameters, we require some means of predicting this bias. Here we present a prescription for doing so; for Euclid-like surveys (with cubical cells 16$h^{-1}$ Mpc across) our bias prescription’s error is less than 3 per cent. This prediction will facilitate optimal utilization of the information in future galaxy surveys.
A. Repp and I. Szapudi
Fri, 4 Aug 17
34/47
Comments: 5 pages, 3 figures; submitted to MNRAS
You must be logged in to post a comment.