The bias of the log power spectrum for discrete surveys
Abstract
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 Euclidlike surveys (with cubical cells 16h^{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.
 Publication:

Monthly Notices of the Royal Astronomical Society
 Pub Date:
 March 2018
 DOI:
 10.1093/mnrasl/slx201
 arXiv:
 arXiv:1708.00954
 Bibcode:
 2018MNRAS.475L...6R
 Keywords:

 cosmological parameters;
 cosmology: miscellaneous;
 cosmology: theory;
 Astrophysics  Cosmology and Nongalactic Astrophysics
 EPrint:
 5 pages, 4 figures