The bias of the log power spectrum for discrete surveys

Andrew Repp, I. Szapudi

Research output: Contribution to journalArticle

2 Citations (Scopus)


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 PA* (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 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.

Original languageEnglish
Pages (from-to)L6-L10
JournalMonthly Notices of the Royal Astronomical Society: Letters
Issue number1
Publication statusPublished - Jan 1 2018


  • Cosmological parameters
  • Cosmology: miscellaneous
  • Cosmology: theory

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

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