Cosmological parameter constraints from SDSS luminous red galaxies: a new treatment of large-scale clustering

By Ariel G. Sánchez, Martín Crocce, Anna Cabré, C. Baugh, E. G. Mpe, Garching, Heidelberg · Germany, Csicieec, Barcelona, Spain. and 3 more. 2009

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We apply a new model for the spherically averaged correlation function at large pair separations to the measurement of the clustering of luminous red galaxies (LRGs) made from the SDSS by Cabre & Gaztanaga (2009a). Our model takes into account the form of the BAO peak and the large scale shape of the correlation function. We perform a Monte Carlo Markov chain analysis for different combinations of datasets and for different parameter sets. When used in combination with a compilation of the latest CMB measurements, the LRG clustering and the latest supernovae results give constraints on cosmological parameters which are comparable and in remarkably good agreement, resolving the tension reported in some studies. The best fitting model in the context of a flat, �-CDM cosmology is specified by m = 0.261 ± 0.013, b = 0.044 ± 0.001, ns = 0.96 ± 0.01, H0 = 71.6 ± 1.2kms 1 Mpc 1 and σ8 = 0.80 ± 0.02. If we allow the time-independent dark energy equation of state parameter to vary, we find results consistent with a cosmological constant at the 5% level using all data sets: wDE = 0.97 ± 0.05. The large scale structure measurements by themselves can constrain the dark energy equation of state parameter to wDE = 1.05 +0.16 0.15, independently of CMB or supernovae data. We do not find convincing evidence for an evolving equation of state. We provide a set of "extended distance priors" that contain the most relevant information from the CMB power spectrum and the shape of the LRG correlation function which can be used to constrain dark energy models and spatial curvature. Our model should provide an accurate description of the clustering even in much larger, forthcoming surveys, such as those planned with NASA's JDEM or ESA's Euclid mission.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/01810145b4e21f0e5fd282f366bcdf6019bddd5d

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Citations in the corpus

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): “2007, 2010; Reid et al. 2009), and the correlation function method (see, e.g., Eisenstein et al. 2005; Okumura et al. 2008; Cabre & Gaztanaga 2008; Martinez et al. 2009; Sanchez et al. 2009; Kazin et al. 2010a; Chuang, Wang, & Hemantha 2012).”
Lightcone mock catalogues from semi-analytic models of galaxy formation – I. Construction and application to the BzK colour selection (2012, background): “…our view of the galaxy distribution and have played a key role in shaping the constraints on our cosmological model (e.g. Norberg et al. 2001, 2002; Zehavi et al. 2005; Cole et al. 2005; Sánchez et al. 2006; Tegmark et al. 2006; Sánchez et al. 2009; Zehavi et al. 2011; Sanchez et al. 2012).”
The clustering of galaxies in the sdss-iii baryon oscillation spectroscopic survey: Baryon acoustic oscillations in the data release 9 spectroscopic galaxy sample (2012, unknown): “…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 2011; Seo et al. 2012), and it is already…”
The WiggleZ Dark Energy Survey: mapping the distance-redshift relation with baryon acoustic oscillations (2011, methodology): “The model of Equation 8 has been shown to yield unbiased results in baryon acoustic peak fits by Sánchez et al. (2008, 2009).”
Improved WiggleZ Dark Energy Survey Distance Measurements to z = 1 with Reconstruction of the Baryonic Acoustic Feature (2014, unknown): “This model has been investigated and applied by S´anchez et al. (2008, 2009, 2013), who show that it gives an unbiased measurement of α , D A , H and the equation of state of dark energy w DE .”
The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: Cosmological implications of the configuration-space clustering wedges (2016, background): “…about the nature of dark energy, potential deviations from the predictions of general relativity (GR), the physics of inflation, neutrino masses, etc. (Percival et al. 2002, 2010; Tegmark et al. 2004; Sánchez et al. 2006, 2009, 2012; Blake et al. 2011; Parkinson et al. 2012).”
The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: cosmological implications of the full shape of the clustering wedges in the data release 10 and 11 galaxy samples (2013, methodology): “…and correlation functions measured from N-body simulations (e.g. Sánchez et al. 2008; Montesano, Sánchez & Phleps 2010) and has been applied to the analysis of numerous galaxy samples (Sánchez et al. 2009, 2012, 2013; Beutler et al. 2011; Blake et al. 2011; Montesano, Sánchez & Phleps 2012).”
The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: single-probe measurements from CMASS anisotropic galaxy clustering (2013, methodology): “…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; Chuang, Wang & Hemantha 2012; Padmanabhan et al. 2012; Xu et al. 2013;…”
The WIRCam Deep Survey I. Counts, colours, and mass-functions derived from near-infrared imaging in the CFHTLS deep fields (2011, background): “Bower et al. adopt the cosmological parameters of the Millennium Simulation (Springel et al. 2005), consistent with cosmic microwave background radiation and large scale galaxy clustering (e.g. Sánchez et al. 2009):Ω0 = 0.25, Λ0 = 0.75,Ωb = 0.045,σ8 = 0.9 andh = 0.73.”
Dark matter direct-detection experiments (2015, background): “this type of simulations reproduce very accurately the measurements made by galaxy surveys [9][10][11].”
Cosmological constraints from the clustering of the Sloan Digital Sky Survey DR7 luminous red galaxies (vol 404, pg 60, 2010) (2009, background): “Note that Sánchez et al. (2009) have also recently C© 2010 The Authors.”
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): “…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 et al. 2011; Padmanabhan et al. 2012; Xu et al. 2012).”
The WiggleZ Dark Energy Survey: testing the cosmological model with baryon acoustic oscillations at z= 0.6 (2011, methodology): “• Model 5: The quasi-linear matter correlation function was generated using Equation 10 of Sanchez et al. (2009), following Crocce & Scoccimarro (2008), which includes the additional contribution of a “mode-coupling” term.”
One simulation to fit them all - changing the background parameters of a cosmological N-body simulation (2009, background): “…new probes such as the imprint of Baryonic Acoustic Oscillations (BAO, e.g. Eisenstein et al. 2005; Cole et al. 2005; Gaztanaga et al. 2008; Sánchez et al. 2009), the form of redshift-space distortions (Guzzo et al. 2008; Percival & White 2008), the clustering amplitude of dark matter…”
Dark matter halo merger histories beyond cold dark matter – I. Methods and application to warm dark matter (2012, background): “…paradigm (Peebles 1982) works extremely well on large scales (Seljak et al. 2005; Percival et al. 2007; Ferramacho, Blanchard & Zolnierowski 2009; Sánchez et al. 2009; Komatsu et al. 2011), but there remains the possibility of deviations from the CDM expectations on small scales – arising…”
The MICE Grand Challenge lightcone simulation – II. Halo and galaxy catalogues (2013, result): “…by looking in detail at the scale dependence of halo and galaxy bias in configuration space, from small scales relevant for full-shape fitting (Sánchez et al. 2009, 2013, 2014) to large 16 Note that our best-fitting non-local coefficient γ 2 is in perfect agreement with the one derived from…”
Interpreting large-scale redshift-space distortion measurements (2011, background): “Next order non-linear effect results in a tilt of correlation function on large scales just before the BAO peak (For details see, Sanchez et al. 2009).”
Baryon Acoustic Oscillations in the Sloan Digital Sky Survey Data Release 7 Galaxy Sample (2009, methodology): “Gaztanaga, Cabre & Hui (2008) and Sanchez et al. (2009) have also analysed the SDSS DR6 (Adelman-McCarthy et al. 2008) sample, obtaining cosmological constraints from the radial and spherically averaged BAO signal.”