Improved WiggleZ Dark Energy Survey Distance Measurements to z = 1 with Reconstruction of the Baryonic Acoustic Feature

By E. Kazin, J. Koda, C. Blake, Nikhil Padmanabhan. 2014

295 citations recorded by the source corpus.

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 $D_{\mathrm V}(r_{\mathrm s}^\mathrm{fid}/r_{\mathrm s})$ of 1716 $\pm$ 83 Mpc, 2221 $\pm$ 101 Mpc, 2516 $\pm$ 86 Mpc (68% CL) at effective redshifts z = 0.44, 0.6, 0.73, respectively, where $D_{\mathrm V}$ is the volume-average-distance, and $r_{\mathrm s}$ is the sound horizon at the end of the baryon drag epoch. These significantly improved 4.8, 4.5 and 3.4 percent accuracy measurements are equivalent to those expected from surveys with up to 2.5 times the volume of WiggleZ. These measurements are fully consistent with cosmologies allowed by the analyses of the Planck Collaboration and the Sloan Digital Sky Survey.We provide the $D_{\mathrm V}(r_{\mathrm s}^\mathrm{fid}/r_{\mathrm s})$ posterior probability distributions and their covariances. When combining these measurements with temperature fluctuations measurements of Planck, the polarization of WMAP9, and the 6dF Galaxy Survey baryonic acoustic feature, we do not detect deviations from a flat LCDM model. Assuming this model we constrain the current expansion rate to $H_0$ = 67.15 $\pm$ 0.98 kms$^{-1}$Mpc$^{-1}$. Allowing the equation of state of dark energy to vary we obtain $w_\mathrm{DE}$ = -1.080 $\pm$ 0.135. When assuming a curved LCDM model we obtain a curvature value of $\Omega_{\mathrm K}$ = -0.0043 $\pm$ 0.0047.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/73df50f49d5edd8ff39c29094ac6f6f580b2907b

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In Astronomy and Astrophysics

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): “In addition to the values from this paper, we include the acoustic-scale measurement from the 6dFGS (Beutler et al. 2011) and WiggleZ survey (Blake et al. 2011; Kazin et al. 2014).”
The clustering of the SDSS DR7 Main Galaxy Sample I: a 4 per cent distance measure at z=0.15 (2014, methodology): “The white squares represent measurements made using SDSS DR7 data (Percival et al. 2010 and Xu et al. 2012) and the grey squares are measurements made by Kazin et al. (2014) using WiggleZ data.”
The completed SDSS-IV extended Baryon Oscillation Spectroscopic Survey: BAO and RSD measurements from anisotropic clustering analysis of the quasar sample in configuration space between redshift 0.8 and 2.2 (2020, background): “This quasar sample bridges the gap between lower redshift SDSS galaxy measurements (Kazin et al. 2014; Alam et al. 2017) and those from the Lyα-forest (Bautista et al. 2017; du Mas des Bour- boux et al. 2017).”
The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: baryon acoustic oscillations in the Fourier space (2016, background): “The WiggleZ survey extended these early detections to higher redshifts (Blake et al. 2011; Kazin et al. 2014), while the 6dF Galaxy Survey (6dFGS) measured the BAO signal at z = 0.1 (Beutler et al. 2011).”
Elucidating ΛCDM: Impact of Baryon Acoustic Oscillation Measurements on the Hubble Constant Discrepancy (2017, background): “…more galaxies, notably the Baryon Oscillation Spectroscopic Survey (BOSS5), have led to both improved precision in the BAO scale measurements over a range of redshifts, and improved analysis methodologies (e.g., Percival et al. 2014; Anderson et al. 2014; Kazin et al. 2014; Reid et al. 2016).”
The clustering of the SDSS-IV extended Baryon Oscillation Spectroscopic Survey DR14 quasar sample: a tomographic measurement of cosmic structure growth and expansion rate based on optimal redshift weights (2018, methodology): “…with higher precision have been performing actively using large galaxy surveys (Percival et al. 2010; Beutler et al. 2011, 2012; Contreras et al. 2013; Kazin et al. 2014; Ross et al. 2015; The Dark Energy Survey Collaboration et al. 2017; Alam et al. 2017; Bautista et al. 2018; Ata et al. 2018).”
Planck2015 results (2015, unknown): “14 show a reanalysis of the WiggleZ redshift survey by Kazin et al. (2014) that applyies peculiar velocity reconstructions.”
KiDS-450: cosmological parameter constraints from tomographic weak gravitational lensing (2016, background): “It successfully predicts key aspects of the observed large-scale structure, from baryonic acoustic oscillations (e.g. Anderson et al. 2014; Kazin et al. 2014; Ross et al. 2015) on the largest scales down to Mpc-scale galaxy clustering and associated inflow velocities (e.g. Peacock et al. 2001).”