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

By C. Blake, T. Davis, Gregory B. Poole, David Parkinson, S. Brough, M. Colless, C. Contreras, W. Couch, Scott M. Croom, Michael Drinkwater and 16 more. 2011

219 citations recorded by the source corpus.

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.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/c8d11ed703057e8a48eaf533062c0d585a228a71

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Citations in the corpus

Baryon acoustic oscillations in the Lyα forest of BOSS DR11 quasars (2014, methodology): “Other measurements of DV/rd were made at z ∼ 0.1 by the 6dFGRS (Beutler et al., 2011), at (0.4 < z < 0.8) by WiggleZ (Blake et al., 2011a), and, using galaxy clusters, at z ∼ 0.3 by Veropalumbo et al. (2013).”
The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey:a large sample of mock galaxy catalogues (2012, methodology): “Alternatively, the lognormal model has been used to generate large numbers of mock catalogues, from which covariance matrices are calculated (Cole et al. 2005; Percival et al. 2010; Blake et al. 2011).”
H0LiCOW – I. H0 Lenses in COSMOGRAIL's wellspring: program overview (2016, background): “…probe relative luminosity distances (e.g., Riess et al. 1998; Perlmutter et al. 1999; Conley et al. 2011; Suzuki et al. 2012; Betoule et al. 2014) and BAO (e.g., Eisenstein et al. 2005; Percival et al. 2010; Blake et al. 2011; Anderson et al. 2014) that yield absolute angular diameter distances.”
Validation of the Scientific Program for the Dark Energy Spectroscopic Instrument (2023, background): “Measurements from 2dFGRS (Colless et al. 2001) and the Sloan Digital Sky Survey (SDSS; York et al. 2000) marked the first use of BAO as a cosmological probe (Cole et al. 2005; Eisenstein et al. 2005), thus motivating the design of surveys dedicated to BAO and clustering measurements, such as WiggleZ”
TWO ACCURATE TIME-DELAY DISTANCES FROM STRONG LENSING: IMPLICATIONS FOR COSMOLOGY (2012, background): “We show in Figure 11 a comparison of the cosmological constraints of the two lenses, BAOs (e.g., Percival et al. 2010; Blake et al. 2011; Mehta et al. 2012), and supernovae (SN; e.g., Hicken et al. 2009; Suzuki et al. 2012), when each is combined with WMAP7 in the owCDM cosmology.”
Measurement of BAO correlations at $z=2.3$ with SDSS DR12 \lya-Forests (2017, background): “Results at other redshifts have been obtained by 6dFGRS at z ∼ 0.11 (Beutler et al. 2011), WiggleZ at 0.4 < z < 0.8 (Blake et al. 2011), SDSS-I at z ∼ 0.35 (Padmanabhan et al. 2012; Mehta et al. 2012; Chuang & Wang 2012; Xu et al. 2013) and SDSS-I at z ∼ 0.15 (Ross et al. 2015).”
Extragalactic science, cosmology, and Galactic archaeology with the Subaru Prime Focus Spectrograph (2012, methodology): “In particular, the CMBinferred BAO scale of 150 Mpc gives a powerful standard ruler for this geometrical test (Eisenstein et al. 2005; Percival et al. 2007; Blake et al. 2011; Hu & Haiman 2003; Seo & Eisenstein 2003).”
The clustering of the SDSS-IV extended Baryon Oscillation Spectroscopic Survey DR14 quasar sample: First measurement of baryon acoustic oscillations between redshift 0.8 and 2.2 (2017, background): “…Sloan Digital Sky Survey (SDSS) I and II (e.g. Eisenstein et al. 2005; Percival et al. 2010; Ross et al. 2015), the 2-degree Field Galaxy Redshift Survey (2dFGRS) (Percival et al. 2001; Cole et al. 2005), WiggleZ (Blake et al. 2011), and the 6-deg Field Galaxy Survey (6dFGS) (Beutler et al. 2011).”
The VIMOS Public Extragalactic Survey (VIPERS) - First Data Release of 57 204 spectroscopic measurements (2013, methodology): “Similarly, the WiggleZ survey targets emission-line galaxies selected from UV observations of the GALEX satellite (Drinkwater et al. 2010; Blake et al. 2011b,a).”
The VIMOS Public Extragalactic Redshift Survey (VIPERS) - an unprecedented view of galaxies and large-scale structure at 0.5 < z < 1.2 (2013, methodology): “…for future dark energy experiments, as testified by the exponential growth in the number of works on both measurements (e.g. Beutler et al. 2012; Blake et al. 2011a; Reid et al. 2012), and theoretical modelling (e.g. Song & Percival 2009; Percival & White 2009; White et al. 2009; Scoccimarro…”
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).”
A 2 per cent distance to $z$=0.35 by reconstructing baryon acoustic oscillations - I. Methods and application to the Sloan Digital Sky Survey (2012, background): “There have now been multiple detections of the BAO feature in galaxy surveys (Cole et al. 2005; Eisenstein et al. 2005; Blake et al. 2007, 2011a,b; Padmanabhan et al. 2007; Percival et al. 2007, 2010; Gaztañaga et al. 2009a; Gaztañaga, Cabré & Hui 2009b; Kazin et al. 2010; Reid et al. 2010;…”
Dark Energy Survey Year 1 results: measurement of the baryon acoustic oscillation scale in the distribution of galaxies to redshift 1 (2017, background): “We include measurements from Beutler et al. (2011, 6dFGS), Ross et al. (2015a, SDSS MGS), Alam et al. (2016, SDSS-III Baryon Oscillation Spectroscopic Survey (BOSS)), Kazin et al. (2014,WiggleZ), Ata et al. (2017, eBOSS quasars), and the combination of Bautista et al. (2017a) and du Mas des Bourboux”
The Completed SDSS-IV Extended Baryon Oscillation Spectroscopic Survey: Baryon Acoustic Oscillations with Lyα Forests (2020, methodology): “At redshifts z2 the BAO scale has been studied using discrete tracers such as galaxies (Percival et al. 2007, 2010; Beutler et al. 2011; Blake et al. 2011; Anderson et al. 2012, 2014a, 2014b; Chuang & Wang 2012; Mehta et al. 2012; Padmanabhan et al. 2012; Xu et al. 2013; Ross et al. 2015; Alam et…”
H i intensity mapping: a single dish approach (2012, methodology): “Originally applied to the Third Data Release (DR3) of the SDSS Luminous Red Galaxy (LRG) survey (Eisenstein et al. 2005), subsequent detections have been reported by a number of groups analysing data from 2dF (Cole et al. 2005), SDSS DR7 (Percival et al. 2010), WiggleZ (Blake et al. 2011), 6dF (Beut”