Blake, Chris and Jurek, Russell J. and Brough, Sarah and Colless, Matthew and Couch, Warrick and Croom, Scott and Davis, Tamara and Drinkwater, Michael J. and Forbes, Duncan and Glazebrook, Karl and Madore, Barry and Martin, Chris and Pimbblet, Kevin and Poole, Gregory B. and Pracy, Michael and Sharp, Rob and Small, Todd and Woods, David (2009) The WiggleZ Dark Energy Survey: small-scale clustering of Lyman-break galaxies at z < 1. Monthly Notices of the Royal Astronomical Society, 395 (1). pp. 240-254. ISSN 0035-8711 http://resolver.caltech.edu/CaltechAUTHORS:20090805-113146524
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The WiggleZ Dark Energy Survey is a large-scale structure survey of intermediate-redshift ultraviolet-selected (UV-selected) emission-line galaxies scheduled to cover 1000 deg^2, spanning a broad redshift range 0.2 < z < 1.0 . The main scientific goal of the survey is the measurement of baryon acoustic oscillations (BAO) in the galaxy clustering pattern at a significantly higher redshift than previous studies. The BAO may be applied as a standard cosmological ruler to constrain dark energy models. Based on the first 20 per cent of the data set, we present initial results concerning the small-scale clustering of the WiggleZ targets, together with survey forecasts. The WiggleZ galaxy population possesses a clustering length r_0 = 4.40 ± 0.12 h^(−1) Mpc, which is significantly larger than z = 0 UV-selected samples, with a slope γ = 1.92 ± 0.08 . This clustering length is comparable to z = 3 Lyman-break galaxies with similar UV luminosities. The clustering strength of the sample increases with optical luminosity, UV luminosity and reddening rest-frame colour. The full survey, scheduled for completion in 2010, will map an effective volume V_eff ≈ 1 Gpc^3 (evaluated at a scale k = 0.15 h Mpc^(−1)) and will measure the angular diameter distance and Hubble expansion rates in three redshift bins with accuracies of ≈5 per cent. We will determine the value of a constant dark energy equation-of-state parameter, wcons, with a higher precision than existing supernovae observations using an entirely independent technique. The WiggleZ and supernova measurements lie in highly complementary directions in the plane of w_(cons) and the matter density Ω_m. The forecast using the full combination of WiggleZ, supernova and cosmic microwave background (CMB) data sets is a marginalized error Δw_(cons) = 0.07 , providing a robust and precise measurement of the properties of dark energy including cross-checking of systematic errors.
|Additional Information:||© 2009 RAS. Accepted 2008 December 22. Received 2008 December 20; in original form 2008 April 8. We acknowledge financial support from the Australian Research Council through Discovery Project grants funding the positions of SB, MP, GBP and TD.We also thank the University of Queensland for supporting the PhD scholarship of RJJ.We acknowledge the efforts ofNick Jones and David Barnes in creating the onlineWiggleZ data base, and Emily Wisnioski for incorporating Principal Component Analysis sky subtraction into the data reduction pipeline. We thank Karl Forster for his assistance in scheduling our GALEX observations and Sebastien Heinis, Ted Wyder and Mark Seibert for invaluable GALEX support and discussions. We acknowledge correlation function modelling performed by Carlos Contreras and Ben Jelliffe which revealed a mistake in the submitted version of this paper. GALEX is a NASA Small Explorer, launched in 2003 April. We gratefully acknowledgeNASA’s support for construction, operation and science analysis for the GALEX mission, developed in cooperation with the Centre National d’Etudes Spatiales of France and the Korean Ministry of Science and Technology. Finally, the WiggleZ survey would not be possible without the dedicated work of the staff of the Anglo-Australian Observatory in the development and support of the AAOmega spectrograph, and the running of the AAT.|
|Subject Keywords:||surveys; galaxies: starburst; cosmology: observations; large-scale structure of Universe|
|Usage Policy:||No commercial reproduction, distribution, display or performance rights in this work are provided.|
|Deposited By:||Jason Perez|
|Deposited On:||01 Sep 2009 22:04|
|Last Modified:||26 Dec 2012 11:08|
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