An Inversion Method for Measuring Beta in Large Redshift Surveys

Abstract

A precision method for determining the value of Beta= Omega_m^{0.6}/b, where b is the galaxy bias parameter, is presented. In contrast to other existing techniques that focus on estimating this quantity by measuring distortions in the redshift space galaxy-galaxy correlation function or power spectrum, this method removes the distortions by reconstructing the real space density field and determining the value of Beta that results in a symmetric signal. To remove the distortions, the method modifies the amplitudes of a Fourier plane-wave expansion of the survey data parameterized by Beta. This technique is not dependent on the small-angle/plane-parallel approximation and can make full use of large redshift survey data. It has been tested using simulations with four different cosmologies and returns the value of Beta to +/- 0.031, over a factor of two improvement over existing techniques.

16 pages including 6 figures Submitted to The Astrophysical Journal

References in corpus (3)

• A measurement of the cosmological mass density from clustering in the 2dF Galaxy Redshift Survey
• The power spectrum of galaxies in the 2dF 100k redshift survey
• The Pairwise Velocity Distribution Function of Galaxies in the LCRS, 2dF, and SDSS Redshift Surveys

Cited by in corpus (2)

• Efficient simulations of large scale structure in modified gravity cosmologies with comoving Lagrangian acceleration
• The VIMOS Public Extragalactic Redshift Survey (VIPERS): Reconstruction of the redshift-space galaxy density field