| Affiliation: | 1Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ;2Department of Physics, University of Durham, South Road, Durham DH1 3LE;3Anglo-Australian Observatory, P. O. Box 296, Epping, NSW 2121, Australia;4Research School of Astronomy &Astrophysics, The Australian National University, Weston Creek, ACT 2611, Australia;5Astrophysics Research Institute, Liverpool John Moores University, Twelve Quays House, Birkenhead, L14 1LD;6Department of Astrophysics, University of New South Wales, Sydney, NSW 2052, Australia;7Department of Physics, University of Oxford, Keble Road, Oxford OX1 3RH;8School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews, Fife, KY6 9SS;9Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA;10Department of Astronomy, Caltech, Pasadena, CA 91125, USA;11Department of Physics &Astronomy, Johns Hopkins University, Baltimore, MD 21218-2686, USA;12Department of Physics, University of Leeds, Woodhouse Lane, Leeds, LS2 9JT;13School of Physics &Astronomy, University of Nottingham, Nottingham NG7 2RD |
| Abstract: | The 2dF Galaxy Redshift Survey has now measured in excess of 160 000 galaxy redshifts. This paper presents the power spectrum of the galaxy distribution, calculated using a direct Fourier transform based technique. We argue that, within the k -space region , the shape of this spectrum should be close to that of the linear density perturbations convolved with the window function of the survey. This window function and its convolving effect on the power spectrum estimate are analysed in detail. By convolving model spectra, we are able to fit the power-spectrum data and provide a measure of the matter content of the Universe. Our results show that models containing baryon oscillations are mildly preferred over featureless power spectra. Analysis of the data yields 68 per cent confidence limits on the total matter density times the Hubble parameter , and the baryon fraction , assuming scale-invariant primordial fluctuations. |
