Measuring DA and H at z = 0.35 from the SDSS DR7 LRGs using baryon acoustic oscillations

By Xiaoying Xu, A. Cuesta, Nikhil Padmanabhan, Daniel J. Eisenstein, Cameron McBride. 2012

204 citations recorded by the source corpus.

We present measurements of the angular diameter distance DA(z) and the Hubble parameter H(z) at z = 0.35 using the anisotropy of the baryon acoustic oscillation (BAO) signal measured in the galaxy clustering distribution of the Sloan Digital Sky Survey (SDSS) Data Release 7 (DR7) Luminous Red Galaxies (LRG) sample. Our work is the first to apply density-field reconstruction to an anisotropic analysis of the acoustic peak. Reconstruction partially removes the effects of non-linear evolution and redshift-space distortions in order to sharpen the acoustic signal. We present the theoretical framework behind the anisotropic BAO signal and give a detailed account of the fitting model we use to extract this signal from the data. Our method focuses only on the acoustic peak anisotropy, rather than the more model-dependent anisotropic information from the broadband power. We test the robustness of our analysis methods on 160 LasDamas DR7 mock catalogues and find that our models are unbiased at the � 0.2% level in measuring the BAO anisotropy. After reconstruction we measure DA(z = 0.35) = 1050 ± 38 Mpc and H(z = 0.35) = 84.4 ± 7.0 km/s/Mpc assuming a sound horizon of rs = 152.76 Mpc. Note that these measurements are correlated with a correlation coefficient of 0.57. This represents a factor of 1.4improvement in the error on DA relative to the pre-reconstruction case; a factor of 1.2 improvement is seen for H.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/e66df22b2d3b352325d765be266318ec78bad6c2

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Citations in the corpus

The clustering of the SDSS main galaxy sample – II. Mock galaxy catalogues and a measurement of the growth of structure from redshift space distortions at z = 0.15 (2014, methodology): “Following Xu et al. (2013), we introduce two scale parameters, α and . α denotes the stretching of all scales and hence encapsulates the isotropic shift whilst parameterizes the AP effect.”
The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: observational systematics and baryon acoustic oscillations in the correlation function (2016, methodology): “The methodology we use to measure α||, α⊥ is based on that used in Xu et al. (2013); Anderson et al. (2014b); Ross et al. (2015), but we employ improved modeling of the postreconstruction quadrupole based on the results of Seo et al. (2015), which are similar to White (2015) and Cohn et al. (2016).”
The DESI Experiment Part I: Science,Targeting, and Survey Design (2016, methodology): “In the upper plot, the filled blue circle is the H0 measurement of [106], the solid black square shows the SDSS BAO measurement of [107], the red square shows the BOSS galaxy BAO measurement of [6], the red circle shows the BOSS Ly-α forest BAO measurement of [47], and the red x shows the BOSS Ly-α ”
The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: single-probe measurements from CMASS anisotropic galaxy clustering (2013, methodology): “…(see, e.g. Eisenstein et al. 2005; Okumura et al. 2008; Cabre & Gaztanaga 2009; Martinez et al. 2009; Sanchez et al. 2009; Kazin et al. 2010; Samushia, Percival & Raccanelli 2011; Chuang, Wang & Hemantha 2012; Padmanabhan et al. 2012; Xu et al. 2013; Hemantha, Wang & Chuang 2014; Oka et al. 2014).”
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).”
The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: cosmological analysis of the DR12 galaxy sample (2016, methodology): “This methodology follows that of Xu et al. (2013); Anderson et al. (2014a) and Anderson et al. (2014b).”
Baryon acoustic oscillations from the complete SDSS-III Ly$\alpha$-quasar cross-correlation function at $z=2.4$ (2017, background): “02 22 5v 3 [ as Beutler et al. 2011; Blake et al. 2011; Padmanabhan et al. 2012; Mehta et al. 2012; Chuang & Wang 2012; Xu et al. 2013; Ross et al. 2015) map distances and expansion rates for z < 0.8.”
The Completed SDSS-IV Extended Baryon Oscillation Spectroscopic Survey: Baryon Acoustic Oscillations with Lyα Forests (2020, unknown): “…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 al. 2017; Bautista et al. 2018), galaxy clusters (Hong et al. 2016), and quasars (Ata et al. 2018).”
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, methodology): “We follow the same methodology as in Ross et al. (2017), which was itself based on Xu et al. (2013) and Anderson et al. (2014).”
Baryon acoustic oscillations from the cross-correlation of Lyα absorption and quasars in eBOSS DR14 (2019, methodology): “Other measurements using galaxies cover the range 0.1 < z < 0.8 (Percival et al. 2007, 2010; Beutler et al. 2011; Blake et al. 2011; Padmanabhan et al. 2012; Mehta et al. 2012; Chuang & Wang 2012; Xu et al. 2013; Ross et al. 2015; Bautista et al. 2018).”
Simultaneous constraints on the growth of structure and cosmic expansion from the multipole power spectra of the SDSS DR7 LRG sample (2013, methodology): “Instead, the broadband shape of these moments that can significantly be altered by the AP effect might give most of the information (Padmanabhan & White 2008), leading to the difference from the result in Xu et al. (2013).”