The WiggleZ Dark Energy Survey: mapping the distance-redshift relation with baryon acoustic oscillations

By C. Blake, E. Kazin, F. Beutler, T. Davis, David Parkinson, S. Brough, M. Colless, C. Contreras, W. Couch, Scott M. Croom and 19 more. 2011

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We present measurements of the baryon acoustic peak at redshifts z = 0.44, 0.6 and 0.73 in the galaxy correlation function of the final dataset of the WiggleZ Dark Energy Survey. We combine our correlation function with lower-redshift measurements from the 6-degree Field Galaxy Survey and Sloan Digital Sky Survey, producing a stacked survey correlation function in which the statistical significance of the detection of the baryon acoustic peak is 4.9-σ relative to a zero-baryon model with no peak. We fit cosmological models to this combined baryon acoustic oscillation (BAO) dataset comprising six distance-redshift data points, and compare the results to similar fits to the latest compilation of supernovae (SNe) and Cosmic Microwave Background (CMB) data. The BAO and SNe datasets produce consistent measurements of the equation-ofstate w of dark energy, when separately combined with the CMB, providing a powerful check for systematic errors in either of these distance probes. Combining all datasets we determine w = 1.03 ± 0.08 for a flat Universe, consistent with a cosmological constant model. Assuming dark energy is a cosmological constant and varying the spatial curvature, we find k = 0.004± 0.006.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/6c9642845f8dfaf802b7767814abf22badb4c223

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Citations in the corpus

The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: baryon acoustic oscillations in the correlation function of LOWZ and CMASS galaxies in Data Release 12 (2015, methodology): “As discussed in the previous section, our BOSS galaxy BAO measurements are consistent with those from the WiggleZ survey (Blake et al. 2011; Kazin et al. 2014) at z = 0.44, 0.60, and 0.73 and with earlier SDSS-II LRG analyses (Percival et al. 2010; Padmanabhan et al. 2012; Mehta et al. 2012; Xu et…”
H0LiCOW - V. New COSMOGRAIL time delays of HE 0435-1223: H0 to 3.8 per cent precision from strong lensing in a flat ΛCDM model (2016, methodology): “…et al. 2015b, hereafter “CMBL”), with Baryon Acoustic Oscillations surveys at various redshifts (Percival et al. 2010; Beutler et al. 2011; Blake et al. 2011; Anderson et al. 2012; Padmanabhan et al. 2012, hereafter BAO) and with the data of the Joint Lightcurve Analysis of Supernovae…”
The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: cosmological implications of the full shape of the clustering wedges in the data release 10 and 11 galaxy samples (2013, methodology): “…and correlation functions measured from N-body simulations (e.g. Sánchez et al. 2008; Montesano, Sánchez & Phleps 2010) and has been applied to the analysis of numerous galaxy samples (Sánchez et al. 2009, 2012, 2013; Beutler et al. 2011; Blake et al. 2011; Montesano, Sánchez & Phleps 2012).”
The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: cosmological analysis of the DR12 galaxy sample (2016, methodology): “The right panel of Figure 15 compares our measurements of fσ8 results those from other surveys: 2dfGRS (Percival et al. 2004b), 6dFGS (Beutler et al. 2012), GAMA (Blake et al. 2013), WiggleZ (Blake et al. 2012), VVDS (Guzzo et al. 2008), and VIPERS (de la Torre et al. 2013), as well as the measureme”
The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: tomographic BAO analysis of DR12 combined sample in Fourier space (2016, methodology): “The Planck 2015 data are combined to complement. polarization fluctuations of the CMB photons, the SN Ia sample of JLA (Betoule et al. 2014), the galaxy power spectra from the WiggleZ survey (Blake et al. 2011) and the tomographic measurement of the weak lensing shear angular power spectra provided ”
Simultaneous constraints on the growth of structure and cosmic expansion from the multipole power spectra of the SDSS DR7 LRG sample (2013, methodology): “We show some examples of similar works (Blake et al. 2011b; Reid et al. 2012a; Samushia et al. 2012; Xu et al. 2013) in Fig.”
KiDS-450 + 2dFLenS: Cosmological parameter constraints from weak gravitational lensing tomography and overlapping redshift-space galaxy clustering (2017, background): “…deviations from GR with the Canada-France-Hawaii Telescope Lensing Survey (CFHTLenS; Heymans et al. 2012; Hildebrandt et al. 2012; Erben et al. 2013; Miller et al. 2013), WiggleZ Dark Energy Survey (Blake et al. 2011, 2012), and the 6-degree-Field Galaxy Survey (6dFGS; Beutler et al. 2011, 2012).”
The clustering of galaxies in the SDSS‐III Baryon Oscillation Spectroscopic Survey: cosmological implications of the large‐scale two‐point correlation function (2012, methodology): “…et al. 1999; Spergel et al. 2003; Riess et al. 2004; Tegmark et al. 2004; Sánchez et al. 2006; Spergel et al. 2007; Riess et al. 2009; Komatsu et al. 2009; Sánchez et al. 2009; Komatsu 2010; Percival et al. 2010; Reid et al. 2010a; Riess et al. 2011; Blake et al. 2011; Montesano et al. 2012).”
Observational probes of cosmic acceleration (2012, methodology): “Combining the WiggleZ, SDSS+2dFGRS (Percival et al., 2010), and 6dFGS BAO measurements with WMAP7 and the Union-2 SN compilation, Blake et al. (2011d) infer Ωm = 0.289±0.015, H0 = 68.7± 1.9 km s−1 Mpc−1, ΩK = −0.004± 0.006, and w = −1.03± 0.08 (where w is assumed to be constant with redshift).”
Improved WiggleZ Dark Energy Survey Distance Measurements to z = 1 with Reconstruction of the Baryonic Acoustic Feature (2014, positive): “8 are the WiggleZ d z ≡ r s / D V results from the Blake et al. (2011) analysis: (0.0916 ± 0.0071,0.0726 ± 0.0034,0.0592 ± 0.0032)for z eff = 0.44,0.6,0.73, respectively.”
Cosmology and astrophysics from relaxed galaxy clusters - II. Cosmological constraints (2014, background): “…et al. 2007, 2010; Spergel et al. 2007; Kowalski et al. 2008; Mantz et al. 2008, 2010b; Dunkley et al. 2009; Vikhlinin et al. 2009; Rozo et al. 2010; Blake et al. 2011; Komatsu et al. 2011; Hinshaw et al. 2013; Suzuki et al. 2012; Anderson et al. 2014; Benson et al. 2013; Hasselfield et al.…”