Measuring the Baryon Acoustic Oscillation scale using the SDSS and 2dFGRS

By Will J. Percival, Shaun Cole, Daniel J. Eisenstein, Robert Nichol, J. Peacock, Adrian Pope, A. Szalay. 2007

287 citations recorded by the source corpus.

We introduce a method to constrain general cosmological models using Baryon Acoustic Oscillation (BAO) distance measurements from galaxy samples covering different redshift ranges, and apply this method to analyse samples drawn from the SDSS and 2dFGRS. BAO are detected in the clustering of the combined 2dFGRS and SDSS main galaxy samples, and measure the distance‐redshift relation at z = 0.2. BAO in the clustering of the SDSS luminous red galaxies measure the distance‐redshift relation at z = 0.35. The observed scale of the BAO calculated from these samples and from the combined sample are jointly analysed using estimates of the correlated errors, to constrain the form of the distance measure DV (z) � [(1+ z) 2 D 2 cz/H(z)] 1/3 . Here DA is the angular diameter distance, and H(z) is the Hubble parameter. This gives rs/DV (0.2) = 0.1980±0.0058 and rs/DV (0.35) = 0.1094±0.0033 (1σ errors), with correlation coefficient of 0.39, where rs is the comoving sound horizon scale at recombination. Matching the BAO to have the same measured scale at all redshifts then gives DV (0.35)/DV (0.2) = 1.812 ± 0.060. The recovered ratio is roughly consistent

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/921bee0efca0bf63f5cf62e42bb50421c1c7d9cc

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Citations in the corpus

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An Overview of CHIME, the Canadian Hydrogen Intensity Mapping Experiment (2022, methodology): “…of the BAO scale at redshifts up to z ∼ 0.8 have been made by observing the distribution of optically-detected galaxies, using either spectroscopic (Percival et al. 2007; Beutler et al. 2011; Blake et al. 2011; Padmanabhan et al. 2012; Anderson et al. 2012; Ross et al. 2015; Alam et al. 2017,…”
Measuring DA and H at z = 0.35 from the SDSS DR7 LRGs using baryon acoustic oscillations (2012, background): “…primarily been focused on the spherically averaged (monopole) statistics (Cole et al. 2005; Eisenstein et al. 2005; Hütsi 2006; Tegmark et al. 2006; Percival et al. 2007; Kazin et al. 2010a; Percival et al. 2010; Beutler et al. 2011; Blake et al. 2011a; Mehta et al. 2012; Padmanabhan et al. 2012;…”
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The growth of structure in interacting dark energy models (2009, unknown): “[1–3]).”
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Observational constraints on an interacting dark energy model (2009, methodology): “We have verified that in the non-interacting case these definitions and our numerical routines lead to the same zdec and rs(adec) as those given as a test case in Percival et al. (2007).”
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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): “…results delivered, using both the power spectrum (see, e.g., Tegmark et al. 2004; Hutsi 2005; Padmanabhan et al. 2007; Blake et al. 2007; Percival et al. 2007, 2010; Reid et al. 2010; Montesano et al. 2011), and the correlation function method (see, e.g., Eisenstein et al. 2005; Okumura…”