Статья

The WiggleZ Dark Energy Survey: improved distance measurements to z = 1 with reconstruction of the baryonic acoustic feature

Eyal Kazin1Centre for Astrophysics & Supercomputing, Swinburne University of Technology, PO Box 218, Hawthorn VIC 3122, AustraliaJun Koda1Centre for Astrophysics & Supercomputing, Swinburne University of Technology, PO Box 218, Hawthorn VIC 3122, AustraliaChris Blake1Centre for Astrophysics and Supercomputing, Swinburne University of Technology, PO Box 218, Hawthorn, VIC 3122, AustraliaNikhil Padmanabhan3Department of Physics, Yale University, 260 Whitney Ave, New Haven, CT 06520, USASarah Brough4Australian Astronomical Observatory, PO Box 915, North Ryde, NSW 1670, AustraliaMatthew Colless4Australian Astronomical Observatory, PO Box 915, North Ryde, NSW 1670, AustraliaC. Contreras1Centre for Astrophysics and Supercomputing, Swinburne University of Technology, PO Box 218, Hawthorn, VIC 3122, AustraliaW. J. Couch1Centre for Astrophysics and Supercomputing, Swinburne University of Technology, PO Box 218, Hawthorn, VIC 3122, AustraliaS. M. Croom6Sydney Institute for Astronomy, School of Physics, University of Sydney, NSW 2006, AustraliaDarren Croton1Centre for Astrophysics and Supercomputing, Swinburne University of Technology, PO Box 218, Hawthorn, VIC 3122, AustraliaT. M. Davis7School of Mathematics and Physics, University of Queensland, Brisbane, QLD 4072, AustraliaM. J. Drinkwater7School of Mathematics and Physics, University of Queensland, Brisbane, QLD 4072, AustraliaKarl Förster8California Institute of Technology, MC 278-17, 1200 East California Boulevard, Pasadena, CA 91125, USAD. G. Gilbank9South African Astronomical Observatory, PO Box 9, Observatory 7935, South AfricaM. D. Gladders10Department of Astronomy and Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637, USAKarl Glazebrook1Centre for Astrophysics and Supercomputing, Swinburne University of Technology, PO Box 218, Hawthorn, VIC 3122, AustraliaBen Jelliffe6Sydney Institute for Astronomy, School of Physics, University of Sydney, NSW 2006, AustraliaRussell J. Jurek11Australia Telescope National Facility, CSIRO, Epping, NSW 1710, AustraliaI-hui Li12Department of Astronomy and Astrophysics, University of Toronto, 50 St George Street, Toronto, ON M5S 3H4, CanadaBarry F. Madore13Observatories of the Carnegie Institute of Washington, 813 Santa Barbara St, Pasadena, CA 91101, USAD. Christopher Martin8California Institute of Technology, MC 278-17, 1200 East California Boulevard, Pasadena, CA 91125, USAKevin A. Pimbblet14School of Physics, Monash University, Clayton, VIC 3800, AustraliaGregory B. Poole1Centre for Astrophysics and Supercomputing, Swinburne University of Technology, PO Box 218, Hawthorn, VIC 3122, AustraliaMichael Pracy6Sydney Institute for Astronomy, School of Physics, University of Sydney, NSW 2006, AustraliaR. Sharp17Research School of Astronomy and Astrophysics, Australian National University, Weston Creek, ACT 2600, AustraliaEmily WisnioskiInfrared and Submillimeter Astronomy, MPI for Extraterrestrial Physics, Max Planck SocietyDavid Woods19Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, BC V6T 1Z1 CanadaTed K. Wyder8California Institute of Technology, MC 278-17, 1200 East California Boulevard, Pasadena, CA 91125, USAH. K. C. Yee12Department of Astronomy and Astrophysics, University of Toronto, 50 St George Street, Toronto, ON M5S 3H4, Canada

2014en

ABI

Аннотация

We present significant improvements in cosmic distance measurements from the WiggleZ Dark Energy Survey, achieved by applying the reconstruction of the baryonic acoustic feature technique. We show using both data and simulations that the reconstruction technique can often be effective despite patchiness of the survey, significant edge effects and shot-noise. We investigate three redshift bins in the redshift range 0.2 < z < 1, and in all three find improvement after reconstruction in the detection of the baryonic acoustic feature and its usage as a standard ruler. We measure model-independent distance measures DV(rfid s/rs) of 1716 ± 83, 2221 ± 101, 2516 ± 86 Mpc (68 per cent CL) at effective redshifts z = 0.44, 0.6, 0.73, respectively, where DV is the volume-averaged distance, and rs is the sound horizon at the end of the baryon drag epoch. These significantly improved 4.8, 4.5 and 3.4 per cent accuracy measurements are equivalent to those expected from surveys with up to 2.5 times the volume of WiggleZ without reconstruction applied. These measurements are fully consistent with cosmologies allowed by the analyses of the Planck Collaboration and the Sloan Digital Sky Survey. We provide the DV(rfid s/rs) posterior probability distributions and their covariances. When combining these measurements with temperature fluctuations measurements of Planck, the polarization of Wilkinson Microwave Anisotropy Probe 9, and the 6dF Galaxy Survey baryonic acoustic feature, we do not detect deviations from a flat Λ cold dark matter (ΛCDM) model. Assuming this model, we constrain the current expansion rate to H0 = 67.15 ± 0.98 km s-1Mpc-1. Allowing the equation of state of dark energy to vary, we obtain wDE =-1.080 ± 0.135. When assuming a curved ΛCDM model we obtain a curvature value of ΩK =-0.0043 ± 0.0047.

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Идентификаторы

DOI: 10.1093/mnras/stu778

Цитирования и источники

Цитирований: 3Использованных источников: 0

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