Papers › Constraining spatial curvature with large-scale structure
Constraining spatial curvature with large-scale structure
Julien Bel, Julien Larena, Roy Maartens, Christian Marinoni, Louis Perenon
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We analyse the clustering of matter on large scales in an extension of the concordance model that allows for spatial curvature. We develop a consistent approach to curvature and wide-angle effects on the galaxy 2-point correlation function in redshift space. In particular we derive the Alcock-Paczynski distortion of fσ₈, which differs significantly from empirical models in the literature. A key innovation is the use of the `Clustering Ratio', which probes clustering in a different way to redshift-space distortions, so that their combination delivers more powerful cosmological constraints. We use this combination to constrain cosmological parameters, without CMB information. In a curved Universe, we find that Ω_(m, 0)=0.26±0.04 (68\% CL). When the clustering probes are combined with low-redshift background probes -- BAO and SNIa -- we obtain a CMB-independent constraint on curvature: Ω_(K,0) = 0.0041 _(-0.0504)^(+0.0500). We find no Bayesian evidence that the flat concordance model can be rejected. In addition we show that the sound horizon at decoupling is r_d = 144.57 ±2.34 Mpc, in agreement with its measurement from CMB anisotropies. As a consequence, the late-time Universe is compatible with flat ΛCDM and a standard sound horizon, leading to a small value of H₀, {\em without} assuming any CMB information. Clustering Ratio measurements produce the only low-redshift clustering data set that is not in disagreement with the CMB, and combining the two data sets we obtain Ω_(K,0)= -0.023 ±0.010.
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