The clustering of galaxies in the sdss-iii baryon oscillation spectroscopic survey: Baryon acoustic oscillations in the data release 9 spectroscopic galaxy sample

By L. Anderson, E. Aubourg, S. Bailey, F. Beutler, V. Bhardwaj, M. Blanton, A. Bolton, J. Brinkmann, J. Brownstein, A. Burden and 55 more. 2012

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We present a one per cent measurement of the cosmic distance scale from the detections of the baryon acoustic oscillations in the clustering of galaxies from the Baryon Oscillation Spectroscopic Survey (BOSS), which is part of the Sloan Digital Sky Survey III (SDSS-III). Our results come from the Data Release 11 (DR11) sample, containing nearly one million galaxies and covering approximately $8\,500$ square degrees and the redshift range $0.2<z<0.7$. We also compare these results with those from the publicly released DR9 and DR10 samples. Assuming a concordance $\Lambda$CDM cosmological model, the DR11 sample covers a volume of 13\,Gpc${}^3$ and is the largest region of the Universe ever surveyed at this density. We measure the correlation function and power spectrum, including density-field reconstruction of the baryon acoustic oscillation (BAO) feature. The acoustic features are detected at a significance of over $7\,\sigma$ in both the correlation function and power spectrum. Fitting for the position of the acoustic features measures the distance relative to the sound horizon at the drag epoch, $r_d$, which has a value of $r_{d,{\rm fid}}=149.28\,$Mpc in our fiducial cosmology. We find $D_V=(1264\pm25\,{\rm Mpc})(r_d/r_{d,{\rm fid}})$ at $z=0.32$ and $D_V=(2056\pm20\,{\rm Mpc})(r_d/r_{d,{\rm fid}})$ at $z=0.57$. At 1.0 per cent, this latter measure is the most precise distance constraint ever obtained from a galaxy survey. Separating the clustering along and transverse to the line-of-sight yields measurements at $z=0.57$ of $D_A=(1421\pm20\,{\rm Mpc})(r_d/r_{d,{\rm fid}})$ and $H=(96.8\pm3.4\,{\rm km/s/Mpc})(r_{d,{\rm fid}}/r_d)$. Our measurements of the distance scale are in good agreement with previous BAO measurements and with the predictions from cosmic microwave background data for a spatially flat cold dark matter model with a cosmological constant.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/d50fcfd9311f407f346a80a144a1f2363813390e

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Citations in the corpus

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, neutral): “…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 (Betoule et al.…”
The clustering of galaxies in the SDSS‐III Baryon Oscillation Spectroscopic Survey: cosmological implications of the large‐scale two‐point correlation function (2012, methodology): “Two of our companion papers, Anderson et al. (2012) and Reid et al. (2012), study the cosmological implications of the galaxy clustering in the CMASS sample.”
The clustering of Galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: including covariance matrix errors (2013, methodology): “With the increasing precision enabled by modern cosmological observations (e.g. Anderson et al. 2012; Planck 2013), there is increasing interest in making their statistical analysis as rigorous as the measurements themselves.”
The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: Testing gravity with redshift-space distortions using the power spectrum multipoles (2013, background): “The BAO scale has now been detected at several different redshifts (Eisenstein et al. 2005; Beutler et al. 2011; Blake et al. 2011b; Anderson et al. 2012, 2013b; Padmanabhan et al. 2012; Slosar et al. 2013).”
The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: single-probe measurements and the strong power of f(z)σ8(z) on constraining dark energy (2013, methodology): “Anderson et al. (2012) measuredα = 1.016 ± 0.017 from the position of the BAO peak of the two-point correlation function (monopole), before applying the reconstruction method on the density field.”
Nonlocal gravity. Conceptual aspects and cosmological predictions (2017, methodology): “ Light-curve Analysis [128]. Baryon Acoustic Oscillations (BAO). We use the isotropic constraints provided by 6dFGS at z e = 0:106 [129], SDSS-MGS DR7 at z e = 0:15 [130] and BOSS LOWZ at z e = 0:32 [131], as well as the anisotropic constraints from CMASS at z e = 0:57 [131]. Initially we will compa”
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”
Lyman-alpha forests cool warm dark matter (2015, background): “n data up to ‘= 29 (‘lowP’), and the ‘30 polarization data (denoted ‘TE’ and ‘EE’), as well as measurements of the BAO scale by 6dFGS [53], the main galaxy sample of SDSS [54], the BOSS LOW-Z sample [55] and the CMASS DR11 sample [55] (‘BAO’ herein). Although these additional sets have contributed t”
The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: tomographic BAO analysis of DR12 combined sample in Fourier space (2016, background): “…have been detected by a number of large galaxy surveys including the Sloan Digital Sky Survey (SDSS; Eisenstein et al. 2005; Percival et al. 2010; Anderson et al. 2012, 2014; Alam et al. 2016; Beutler et al. 2016, 2017; Cuesta et al. 2016; Gil-Marı́n et al. 2016; Ross et al. 2017), the…”
Improved WiggleZ Dark Energy Survey Distance Measurements to z = 1 with Reconstruction of the Baryonic Acoustic Feature (2014, positive): “A further application of the technique was performed by the SDSS-III Baryon Oscillation Spectroscopic Survey (BOSS) using a massive galaxy sample at z = 0.57 (Anderson et al. 2012, 2014b).”
Mock galaxy catalogues using the quick particle mesh method (2013, background): “…configuration space two-point function) for the four mock catalogues for a sample of haloes with M > 1013 h−1 M , chosen to roughly match the number density of BOSS CMASS galaxies (White et al. 2011; Anderson et al. 2012; Dawson et al. 2013) though other mass ranges look qualitatively similar.”