Статья

The 2dF Galaxy Redshift Survey: power-spectrum analysis of the final data set and cosmological implications

Shaun ColeDepartment of Physics, University of Durham, Science Laboratories, South Road, Durham DH1 3LEWill J. PercivalInstitute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh EH9 3HJJ. A. PeacockInstitute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh EH9 3HJP. NorbergInstitut fr Astronomie, Departement Physik, ETH Zurich, HPF G3.1, Zurich CH-8093, SwitzerlandC. M. BaughDepartment of Physics, University of Durham, Science Laboratories, South Road, Durham DH1 3LECarlos S. FrenkDepartment of Physics, University of Durham, Science Laboratories, South Road, Durham DH1 3LEI. K. BaldryDepartment of Physics & Astronomy, Johns Hopkins University, 3400 North Charles Street Baltimore, MD 21218-2686, USAJoss Bland‐HawthornAnglo-Australian Observatory, PO Box 296, Epping, NSW 2121, AustraliaTerry BridgesDepartment of Physics, Queen's University, Kingston, ON K7L 3N6, CanadaRussell CannonAnglo-Australian Observatory, PO Box 296, Epping, NSW 2121, AustraliaMatthew CollessAnglo-Australian Observatory, PO Box 296, Epping, NSW 2121, AustraliaC. A. CollinsAstrophysics Research Institute, Liverpool John Moores University, Twelve Quays House, Egerton Wharf, Birkenhead L14 1LDW. J. CouchSchool of Physics, University of New South Wales, Sydney, NSW 2052, AustraliaN. J. G. CrossDepartment of Physics & Astronomy, Johns Hopkins University, 3400 North Charles Street Baltimore, MD 21218-2686, USAGavin DaltonDepartment of Physics, Keble Road, Oxford OX1 3RHV. R. EkeDepartment of Physics, University of Durham, Science Laboratories, South Road, Durham DH1 3LERoberto De ProprisH.H. Wills Physics Laboratory, University of Bristol, Royal Fort, Tyndall Avenue, Bristol BS8 1TLSimon P. DriverResearch School of Astronomy & Astrophysics, The Australian National University, Weston Creek, ACT 2611, AustraliaG. EfstathiouInstitute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HARichard S. EllisDepartment of Astronomy, California Institute of Technology, Pasadena, CA 91125, USAKarl GlazebrookDepartment of Physics & Astronomy, Johns Hopkins University, 3400 North Charles Street Baltimore, MD 21218-2686, USACarole JacksonAustralia Telescope National Facility, PO Box 76, Epping NSW 1710, AustraliaAdrian JenkinsDepartment of Physics, University of Durham, Science Laboratories, South Road, Durham DH1 3LEO. LahavDepartment of Physics and Astronomy, University College London, Gower Street, London WC1E 6BTIan LewisDepartment of Physics, Keble Road, Oxford OX1 3RHS. L. LumsdenDepartment of Physics & Astronomy, E C Stoner Building, Leeds LS2 9JTS. MaddoxSchool of Physics and Astronomy, University of Nottingham, University Park, Nottingham NG7 2RDDarren S. MadgwickInstitute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HAB. A. PetersonResearch School of Astronomy & Astrophysics, The Australian National University, Weston Creek, ACT 2611, AustraliaWilliam J. SutherlandInstitute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HAKeith TaylorDepartment of Astronomy, California Institute of Technology, Pasadena, CA 91125, USAThe 2dFGRS Team

2005en

ABI

Аннотация

We present a power-spectrum analysis of the final 2dF Galaxy Redshift Survey (2dFGRS), employing a direct Fourier method. The sample used comprises 221 414 galaxies with measured redshifts. We investigate in detail the modelling of the sample selection, improving on previous treatments in a number of respects. A new angular mask is derived, based on revisions to the photometric calibration. The redshift selection function is determined by dividing the survey according to rest-frame colour, and deducing a self-consistent treatment of k-corrections and evolution for each population. The covariance matrix for the power-spectrum estimates is determined using two different approaches to the construction of mock surveys, which are used to demonstrate that the input cosmological model can be correctly recovered. We discuss in detail the possible differences between the galaxy and mass power spectra, and treat these using simulations, analytic models and a hybrid empirical approach. Based on these investigations, we are confident that the 2dFGRS power spectrum can be used to infer the matter content of the universe. On large scales, our estimated power spectrum shows evidence for the 'baryon oscillations' that are predicted in cold dark matter (CDM) models. Fitting to a CDM model, assuming a primordial n s = 1 spectrum, h = 0.72 and negligible neutrino mass, the preferred parameters are m h = 0.168 0.016 and a baryon fraction b / m = 0.185 0.046 (1 errors). The value of m h is 1 lower than the 0.20 0.03 in our 2001 analysis of the partially

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Идентификаторы

DOI: 10.1111/j.1365-2966.2005.09318.x

Цитирования и источники

Цитирований: 7Использованных источников: 0

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