Large-Scale Anisotropic Correlation Function of SDSS Luminous Red Galaxies

By T. Okumura, Takahiko Matsubara, Daniel J. Eisenstein, I. Kayo, C. Hikage, A. Szalay, D. Schneider. 2007

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We study the large-scale anisotropic two-point correlation function using 46,760 luminous red galaxies at redshifts 0.16-0.47 from the Sloan Digital Sky Survey. We measure the correlation function as a function of separations parallel and perpendicular to the line of sight in order to take account of anisotropy of the large-scale structure in redshift space. We find a slight signal of baryonic features in the anisotropic correlation function, i.e., a “baryon ridge” corresponding to a baryon acoustic peak in the spherically averaged correlation function, which has already been reported using the same sample. The baryon ridge has primarily a spherical structure with a known radius in comoving coordinates. It enables us to divide the redshift distortion effects into dynamical and geometrical components and provides further constraints on cosmological parameters, including the dark energy equation-of-state. With an assumption of a flat Λ cosmology, we find the best-fit values of Ωm = 0.218−0.037+0.047 and Ωb = 0.047 ± 0.016 (68% CL) when we use the overall shape of the anisotropic correlation function of 40 < s < 200 h−1 Mpc including a scale of baryon acoustic oscillations. When an additional assumption of Ωbh2 = 0.024 is adopted, we obtain ΩDE = 0.770−0.040+0.051 and w = − 0.93−0.35+0.45. These constraints are estimated only from our data of the anisotropic correlation function, and they agree quite well with values both from the cosmic microwave background (CMB) anisotropies and from other complementary statistics using the LRG sample. With the CMB prior from the 3 year WMAP results, we give stronger constraints on those parameters.

Subfields: Astronomy and Astrophysics

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Interpreting large-scale redshift-space distortion measurements (2011, background): “This excess has been observed previously in spectroscopic (Okumura et al. 2008; Sanchez et al. 2009; Cabré & Gaztañaga 2009; Kazin et al. 2010) and photometric (Thomas, Abdalla & Lahav 2011; Crocce et al. 2011; Ross et al. 2011) data sets.”
Modelling the anisotropic two-point galaxy correlation function on small scales and single-probe measurements of H(z), DA(z) and f(z)σ8(z) from the Sloan Digital Sky Survey DR7 luminous red galaxies (2012, methodology): “…et al. 2007; Percival et al. 2007, 2010; Reid et al. 2010; Montesano, Sanchez & Phleps 2012) and the correlation function method (see e.g. Eisenstein et al. 2005; Okumura et al. 2008; Cabre & Gaztanaga 2009; Martinez et al. 2009; Sanchez E-mail: chia-hsun.chuang@uam.es †MultiDark Fellow.”
The WiggleZ Dark Energy Survey: the growth rate of cosmic structure since redshift z=0.9 (2011, methodology): “The SDSS Luminous Red Galaxy (LRG) sample enabled these measurements to be extended to somewhat higher redshifts z ≈ 0.35 (Tegmark et al. 2006, Cabre & Gaztanaga 2009, Okumura et al. 2008).”
The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: cosmological analysis of the DR12 galaxy sample (2016, methodology): “Below z = 0.2, the sample is affected by the bright limit of r > 16, and the BAO scale has been measured for z < 0.2 galaxies in the SDSS-I/II main galaxy redshift survey (Strauss et al. 2002) by Ross et al. (2015).”
Measuring DA and H at z = 0.35 from the SDSS DR7 LRGs using baryon acoustic oscillations (2012, methodology): “In the case of the BAO, the anisotropy can be measured using the clustering signal along different directions (Okumura et al. 2008; Blake et al. 2011b; Gaztañaga, Cabré & Hui 2011; Chuang & Wang 2012a; Kazin, Sánchez & Blanton 2012) or by looking at higher order multipoles of the two-point…”
Confronting Lemaitre–Tolman–Bondi models with observational cosmology (2008, methodology): “The BAO has been measured at different scales using a variety of techniques, and the feature has been detected in the 3D two-point correlation function [27, 28], the 3D power spectrum [29], and the angular power spectrum [30].”
Cosmological parameter constraints from SDSS luminous red galaxies: a new treatment of large-scale clustering (2009, methodology): “The most powerful BAO measurements currently come from samples of luminous red galaxies (LRGs; Cole et al. 2005; Hütsi 2006; Padmanabhan et al. 2007; Percival et al. 2007a,b; Gaztañaga, Cabre & Hui 2008b; Okumura et al. 2008; Cabre & Gaztañaga 2009; Martinez et al. 2009).”
The Subaru FMOS galaxy redshift survey (FastSound). IV. New constraint on gravity theory from redshift space distortions at z ∼ 1.4 (2015, background): “RSD has been analyzed for various redshift surveys (e.g.,Davis& Peebles 1983; Fisher et al. 1994; Peacock et al. 2001; Zehavi et al. 2002; Hawkins et al. 2003; Percival et al. 2004; Tegmark et al. 2004; daÂngela et al. 2005; Tegmark et al. 2006; Ross et al. 2007; Okumura et al. 2008).”
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, background): “…distances from redshifts obtained in spectroscopic surveys reveal an anisotropic galaxy distribution (Cole, Fisher & Weinberg 1995; Peacock et al. 2001; Percival et al. 2004; da Angela et al. 2008; Guzzo et al. 2008; Okumura et al. 2008; Blake et al. 2011b; Samushia, Percival & Raccanelli 2012a).”
The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: single-probe measurements from CMASS anisotropic galaxy clustering (2013, methodology): “…et al. 2007, 2010; Reid et al. 2010; Montesano, Sanchez & Phleps 2012), and the correlation function method (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;…”
FIVE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE OBSERVATIONS: COSMOLOGICAL INTERPRETATION (2008, unknown): “This is a powerful probe of dark energy; however, the accuracy of the current data do not allow us to extract DA(z) and H(z) separately, as one can barely measure BAO in the spherically averaged correlation function (Okumura et al. 2008).”
The clustering of galaxies in the sdss-iii baryon oscillation spectroscopic survey: Baryon acoustic oscillations in the data release 9 spectroscopic galaxy sample (2012, background): “…2010; Miller, Nichol & Batuski 2001; Eisenstein et al. 2005; Cole et al. 2005; Hütsi 2006; Blake et al. 2007, 2011a; Padmanabhan et al. 2007, 2012a; Okumura et al. 2008; Gaztanaga, Cabre & Hui 2009; Sanchez et al. 2009; Kazin et al. 2010; Reid et al. 2010; Beutler et al. 2011; Cabré & Gaztañaga…”
The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: measuring DA and H at z = 0.57 from the baryon acoustic peak in the data release 9 spectroscopic galaxy sample (2013, methodology): “Such anisotropic analyses have been performed on SDSS-II data (Okumura et al. 2008; Gaztañaga et al. 2009; Chuang & Wang 2012; Xu et al. 2013).”
Observational probes of cosmic acceleration (2012, methodology): “Okumura et al. (2008) performed a correlation function analysis of the LRG sample from SDSS DR3, achieving a weak indication of the radial BAO.”
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): “…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 et al. 2008; Cabre & Gaztanaga 2009; Martinez et al. 2009; Sanchez et al. 2009; Kazin et al. 2010a; Chuang, Wang, & Hemantha 2012; Samushia…”
MEASURING BARYON ACOUSTIC OSCILLATIONS ALONG THE LINE OF SIGHT WITH PHOTOMETRIC REDSHIFTS: THE PAU SURVEY (2008, background): “These two components can be separated by considering the anisotropic correlation function (see Okumura et al. 2008; Padmanabhan & White 2008; Cabre & Gaztanaga 2008; and Figures 17 and 18 in Gaztanaga et al. 2008, which show how the anisotropic correlation function changes for PAU-like photo-z…”
Forecasting cosmological constraints from redshift surveys (2008, methodology): “…Digital Sky Survey (SDSS; York et al. 2000), redshiftspace distortions have also been measured in the correlation function (Zehavi et al. 2005; Okumura et al. 2008; Cabré & Gazta˜naga 2008), and using an Eigenmode decomposition to separate real and redshift-space effects (Tegmark et al.…”
Measurements of H(z) and DA(z) from the two-dimensional two-point correlation function of Sloan Digital Sky Survey luminous red galaxies (2011, methodology): “The same selection criteria were used in previous papers (Zehavi et al. 2005; Eisenstein et al. 2005; Okumura et al. 2008; Kazin et al. 2010a).”