Open AccessLarge‐scale bias in the Universe — II. Redshift‐space bispectrum
Author(s) -
Verde L.,
Heavens A. F.,
Matarrese S.,
Moscardini L.
Publication year - 1998
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1046/j.1365-8711.1998.t01-1-01937.x
Subject(s) - physics , bispectrum , redshift , universe , astrophysics , astronomy , scale (ratio) , redshift space distortions , cosmology , space (punctuation) , redshift survey , galaxy , spectral density , statistics , quantum mechanics , mathematics , philosophy , linguistics
The determination of the density parameter Ω 0 from the large‐scale distribution of galaxies is one of the major goals of modern cosmology. However, if galaxies are biased tracers of the underlying mass distribution, linear perturbation theory leads to a degeneracy between Ω 0 and the linear bias parameter b , and the density parameter cannot be estimated. In Matarrese, Verde &38; Heavens we developed a method based on second‐order perturbation theory to use the bispectrum to lift this degeneracy by measuring the bias parameter in an Ω 0 ‐independent way. The formalism was developed assuming that one has perfect information on the positions of galaxies in three dimensions. In galaxy redshift surveys, the three‐dimensional information is imperfect, because of the contaminating effects of peculiar velocities, and the resulting clustering pattern in redshift space is distorted. In this paper we combine second‐order perturbation theory with a model for collapsed, virialized structures, to extend the method to redshift space, and demonstrate that the method should be successful in determining with reasonable accuracy the bias parameter from state‐of‐the‐art surveys such as the Anglo‐Australian 2 degree Field Survey and the Sloan Digital Sky Survey.