The power spectrum of galaxies in the 2dF 100k redshift survey

We compute the real-space power spectrum and the redshift-space distortions of galaxies in the 2dF 100k galaxy redshift survey using pseudo-Karhunen-Loève eigenmodes and the stochastic bias formalism. Our results agree well with those published by the 2dFGRS team, and have the added advantage of pro...

Full description

Saved in:
Bibliographic Details
Published in:Monthly notices of the Royal Astronomical Society 2002-10, Vol.335 (4), p.887-908
Main Authors: Tegmark, Max, Hamilton, Andrew J. S., Xu, Yongzhong
Format: Article
Language:English
Subjects:
galaxies: distances and redshifts
galaxies: statistics
large-scale structure of Universe
methods: data analysis
Citations: Items that this one cites
Items that cite this one
Online Access:Get full text
Tags: Add Tag
No Tags, Be the first to tag this record!
Description
Summary:We compute the real-space power spectrum and the redshift-space distortions of galaxies in the 2dF 100k galaxy redshift survey using pseudo-Karhunen-Loève eigenmodes and the stochastic bias formalism. Our results agree well with those published by the 2dFGRS team, and have the added advantage of producing easy-to-interpret uncorrelated minimum-variance measurements of the galaxy–galaxy, galaxy–velocity and velocity–velocity power spectra in 27 k-bands, with narrow and well-behaved window functions in the range 0.01 h Mpc−1 < k < 0.8 h Mpc−1. We find no significant detection of baryonic wiggles, although our results are consistent with a standard flat ΩΛ= 0.7‘concordance’ model and previous tantalizing hints of baryonic oscillations. We measure the galaxy-matter correlation coefficient r > 0.4 and the redshift-distortion parameter β= 0.49 ± 0.16 for r= 1 (β= 0.47 ± 0.16 without finger-of-god compression). Since this is an apparent-magnitude limited sample, luminosity-dependent bias may cause a slight red-tilt in the power spectrum. A battery of systematic error tests indicate that the survey is not only impressive in size, but also unusually clean, free of systematic errors at the level to which our tests are sensitive. Our measurements and window functions are available at together with the survey mask, radial selection function and uniform subsample of the survey that we have constructed.
ISSN:0035-8711
1365-2966
DOI:10.1046/j.1365-8711.2002.05622.x