The WiggleZ Dark Energy Survey: the growth rate of cosmic structure since redshift z=0.9

By C. Blake, S. Brough, M. Colless, C. Contreras, W. Couch, Scott M. Croom, T. Davis, Michael Drinkwater, K. Forster, D. Gilbank and 15 more. 2011

445 citations recorded by the source corpus.

We present precise measurements of the growth rate of cosmic structure for the redshift range 0.1 < z < 0.9, using redshift-space distortions in the galaxy power spectrum of the WiggleZ Dark Energy Survey. Our results, which have a precision of around 10 per cent in four independent redshift bins, are well fitted by a flat Λ cold dark matter (ΛCDM) cosmological model with matter density parameter Ω_m = 0.27. Our analysis hence indicates that this model provides a self-consistent description of the growth of cosmic structure through large-scale perturbations and the homogeneous cosmic expansion mapped by supernovae and baryon acoustic oscillations. We achieve robust results by systematically comparing our data with several different models of the quasi-linear growth of structure including empirical models, fitting formulae calibrated to N-body simulations, and perturbation theory techniques. We extract the first measurements of the power spectrum of the velocity divergence field, P_(θθ) (k), as a function of redshift (under the assumption that P_(gθ) (k) = − √P_(gg)(k)P_(θθ) (k), where g is the galaxy overdensity field), and demonstrate that the WiggleZ galaxy–mass cross-correlation is consistent with a deterministic (rather than stochastic) scale-independent bias model for WiggleZ galaxies for scales k < 0.3 h Mpc^(−1). Measurements of the cosmic growth rate from the WiggleZ Survey and other current and future observations offer a powerful test of the physical nature of dark energy that is complementary to distance–redshift measures such as supernovae and baryon acoustic oscillations.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/2cf03e0f655b5d1c86ef0afdd083b842d22c53c9

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Citations in the corpus

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): The growth of structure at $0.5 < z < 1.2$ from redshift-space distortions in the clustering of the PDR-2 final sample (2016, background): “These included in particular the 6dfGS (Beutler et al. 2012), WiggleZ (e.g. Blake et al. 2011; Contreras et al. 2013) and BOSS (e.g. Reid et al. 2014; Beutler et al. 2016; Satpathy et al. 2016; Sanchez et al. 2016; Grieb et al. 2016).”
The clustering of galaxies in the SDSS-III DR9 Baryon Oscillation Spectroscopic Survey: testing deviations from Λ and general relativity using anisotropic clustering of galaxies (2012, methodology): “The AP effect has been recently used to jointly measureDA, H and fσ8 in three redshift bins from WiggleZ survey (Blake et al. 2012) and using the SDSS-II LRG sample (Chuang & Wang 2012).”
The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: measurements of the growth of structure and expansion rate at z = 0.57 from anisotropic clustering (2012, methodology): “The WiggleZ survey has recently analysed the anisotropic clustering of bright emission line galaxies over a broad redshift range (Blake et al. 2011b,c).”
Testing ΛCDM at the lowest redshifts with SN Ia and galaxy velocities (2016, background): “067 [64], GAMA [65], WiggleZ [66], BOSS [67], and VIPERS [68].”
The WiggleZ Dark Energy Survey: joint measurements of the expansion and growth history at z < 1 (2012, methodology): “By equating radial and tangential physical scales, independently of any underlying standard ruler, the observable ∆z/∆θ ∼ (1+z)DA(z)H(z)/c may be determined (Outram et al. 2004, Marinoni & Buzzi 2010, Blake et al. 2011c).”
The clustering of the SDSS-IV extended Baryon Oscillation Spectroscopic Survey DR14 quasar sample: measurement of the growth rate of structure from the anisotropic correlation function between redshift 0.8 and 2.2 (2018, methodology): “…where the precision on fσ 8 has reached 10 per cent, there are measurements from 2dF (Percival et al. 2004), 6dFGRS (Beutler et al. 2012), WiggleZ (Blake et al. 2011), and recently by Sloan Digital Sky Survey III Baryon Oscillation Spectroscopic Survey (SDSS-III BOSS, Alam et al. 2017) and…”
Galaxy And Mass Assembly (GAMA): improved cosmic growth measurements using multiple tracers of large-scale structure (2013, methodology): “First, in a similar analysis of the WiggleZ Dark Energy Survey, Blake et al. (2011) established that these models (including the free damping parameter) were an acceptable approximation to a large suite of other approaches for modelling non-linearities in RSD, including perturbation theory technique”
First Evidence of Running Cosmic Vacuum: Challenging the Concordance Model (2016, methodology): “Thus, while in our previous work we only used 6 BAO data points based on the A(z) estimator (cf. Table 3 of Blake et al. (2011b)), here we are using a total of 11 BAO points (none of them based on A(z), see S2-S3).”
The WiggleZ Dark Energy Survey: the transition to large-scale cosmic homogeneity (2012, methodology): “We use the values obtained by Blake et al. (2011a) in each redshift slice from fits to the WiggleZ twodimensional power spectrum – these are listed in Table 3.”
The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: Testing gravity with redshift-space distortions using the power spectrum multipoles (2013, methodology): “…= Ngal∑ i wc(xi)wFKP(xi)eik·xiL (k̂ · x̂i), (10) R (k) = Nran∑ i wFKP(xi)eik·xiL (k̂ · x̂i), (11) the power spectrum estimate is given by (Yamamoto et al. 2006; Blake et al. 2011a) P (k) = (2 + 1) 2A [( D (k) − α′R (k) ) × (D0(k) − α′R0(k))∗ − S ] , (12) where the ∗ represents the complex…”
The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: Measuring growth rate and geometry with anisotropic clustering (2013, methodology): “Previous studies either fix the shape parameters to their CMB best-fit values (e.g. Samushia, Percival & Raccanelli 2012), let Ωmh2 vary and fix the rest (e.g. Blake et al. 2011b) , or marginalise over them by taking a prior centered around CMB best-fit values (e.g. Chuang et al. 2012).”
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.”
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”
The Subaru FMOS galaxy redshift survey (FastSound). IV. New constraint on gravity theory from redshift space distortions at z ∼ 1.4 (2015, methodology): “…et al. 2015), the SDSS luminous red galaxy (LRG) sample (Yamamoto et al. 2008; Cabré & Gaztañaga 2009; Samushia et al. 2012), the WiggleZ survey (Blake et al. 2011; Contreras et al. 2013), the SDSS-III Baryon Oscillation Spectroscopi Survey (BOSS) (Reid et al. 2012; Tojeiro et al. 2012),…”