Статья

The WiggleZ Dark Energy Survey: testing the cosmological model with baryon acoustic oscillations at z= 0.6

Chris BlakeCentre for Astrophysics & Supercomputing, Swinburne University of Technology, PO Box 218, Hawthorn, VIC 3122, AustraliaTamara DavisDark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, DK-2100 Copenhagen Ø, DenmarkGregory B. PooleCentre for Astrophysics & Supercomputing, Swinburne University of Technology, PO Box 218, Hawthorn, VIC 3122, AustraliaDavid ParkinsonSchool of Mathematics and Physics, University of Queensland, Brisbane, QLD 4072, AustraliaSarah BroughAustralian Astronomical Observatory, PO Box 296, Epping, NSW 1710, AustraliaMatthew CollessAustralian Astronomical Observatory, PO Box 296, Epping, NSW 1710, AustraliaCarlos ContrerasCentre for Astrophysics & Supercomputing, Swinburne University of Technology, PO Box 218, Hawthorn, VIC 3122, AustraliaWarrick CouchCentre for Astrophysics & Supercomputing, Swinburne University of Technology, PO Box 218, Hawthorn, VIC 3122, AustraliaScott CroomSydney Institute for Astronomy, School of Physics, University of Sydney, NSW 2006, AustraliaMichael J. DrinkwaterSchool of Mathematics and Physics, University of Queensland, Brisbane, QLD 4072, AustraliaKarl ForsterCalifornia Institute of Technology, MC 278-17, 1200 East California Boulevard, Pasadena, CA 91125, USADavid GilbankAstrophysics and Gravitation Group, Department of Physics and Astronomy, University of Waterloo, Waterloo, ON N2L 3G1, CanadaMike GladdersDepartment of Astronomy and Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637, USAKarl GlazebrookCentre for Astrophysics & Supercomputing, Swinburne University of Technology, PO Box 218, Hawthorn, VIC 3122, AustraliaBen JelliffeSydney Institute for Astronomy, School of Physics, University of Sydney, NSW 2006, AustraliaRussell J. JurekAustralia Telescope National Facility, CSIRO, Epping, NSW 1710, AustraliaI-hui LiCentre for Astrophysics & Supercomputing, Swinburne University of Technology, PO Box 218, Hawthorn, VIC 3122, AustraliaBarry MadoreObservatories of the Carnegie Institute of Washington, 813 Santa Barbara St., Pasadena, CA 91101, USAD. Christopher MartinCalifornia Institute of Technology, MC 278-17, 1200 East California Boulevard, Pasadena, CA 91125, USAKevin PimbbletSchool of Physics, Monash University, Clayton, VIC 3800, AustraliaMichael PracyCentre for Astrophysics & Supercomputing, Swinburne University of Technology, PO Box 218, Hawthorn, VIC 3122, AustraliaRob SharpAustralian Astronomical Observatory, PO Box 296, Epping, NSW 1710, AustraliaEmily WisnioskiCentre for Astrophysics & Supercomputing, Swinburne University of Technology, PO Box 218, Hawthorn, VIC 3122, AustraliaDavid WoodsDepartment of Physics & Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, BC V6T 1Z1, CanadaTed K. WyderCalifornia Institute of Technology, MC 278-17, 1200 East California Boulevard, Pasadena, CA 91125, USAH. K. C. YeeDepartment of Astronomy and Astrophysics, University of Toronto, 50 St. George Street, Toronto, ON M5S 3H4, Canada

2011en

ABI

Аннотация

We measure the imprint of baryon acoustic oscillations (BAOs) in the galaxy clustering pattern at the highest redshift achieved to date, z= 0.6, using the distribution of N= 132 509 emission-line galaxies in the WiggleZ Dark Energy Survey. We quantify BAOs using three statistics: the galaxy correlation function, power spectrum and the band-filtered estimator introduced by Xu et al. The results are mutually consistent, corresponding to a 4.0 per cent measurement of the cosmic distance–redshift relation at z= 0.6 [in terms of the acoustic parameter ‘A(z)’ introduced by Eisenstein et al., we find A(z= 0.6) = 0.452 ± 0.018]. Both BAOs and power spectrum shape information contribute towards these constraints. The statistical significance of the detection of the acoustic peak in the correlation function, relative to a wiggle-free model, is 3.2σ. The ratios of our distance measurements to those obtained using BAOs in the distribution of luminous red galaxies at redshifts z= 0.2 and 0.35 are consistent with a flat Λ cold dark matter model that also provides a good fit to the pattern of observed fluctuations in the cosmic microwave background radiation. The addition of the current WiggleZ data results in a ≈30 per cent improvement in the measurement accuracy of a constant equation of state, w, using BAO data alone. Based solely on geometric BAO distance ratios, accelerating expansion (w < −1/3) is required with a probability of 99.8 per cent, providing a consistency check of conclusions based on supernovae observations. Further improvements in cosmological constraints will result when the WiggleZ survey data set is complete.

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Идентификаторы

DOI: 10.1111/j.1365-2966.2011.19077.x

Цитирования и источники

Цитирований: 2Использованных источников: 0

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