Volume 554, June 2013
|Number of page(s)||12|
|Section||Cosmology (including clusters of galaxies)|
|Published online||17 June 2013|
An optimized correlation function estimator for galaxy surveys
APC, Astroparticule et Cosmologie, Université Paris Diderot, CNRS/IN2P3,
CEA/Irfu, Observatoire de Paris,
Sorbonne Paris Cité, 10 rue Alice Domon et Lonie
Paris Cedex 13,
2 Laboratoire AIM, CEA/DSM-CNRS-Université Paris Diderot, IRFU, SEDI-SAP, Service d’Astrophysique, Centre de Saclay, 91191 Gif-Sur-Yvette Cedex, France
3 CEA centre de Saclay, irfu/SPP, 91191 Gif-sur-Yvette, France
4 CPPM, Aix-Marseille Université, CNRS/IN2P3, 13288 Marseille, Cedex 9, France
5 Institute of Cosmology and Gravitation, Portsmouth University, Dennis Sciama Building, PO1 3 FX Portsmouth, UK
6 Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA
7 Department of Astronomy and Astrophysics, The Pennsylvania State University, University Park, PA 16802, USA
8 Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA 16802, USA
9 Steward Observatory, University of Arizona 933, N. Cherry Avenue, Tucson, AZ, 85721, USA
Accepted: 28 March 2013
Measuring the two-point correlation function of the galaxies in the Universe gives access to the underlying dark matter distribution, which is related to cosmological parameters and to the physics of the primordial Universe. The estimation of the correlation function for current galaxy surveys makes use of the Landy-Szalay estimator, which is supposed to reach minimal variance. This is only true, however, for a vanishing correlation function. We study the Landy-Szalay estimator when these conditions are not fulfilled and propose a new estimator that provides the smallest variance for a given survey geometry. Our estimator is a linear combination of ratios between pair counts of data and/or random catalogues (DD, RR, and DR). The optimal combination for a given geometry is determined by using lognormal mock catalogues. The resulting estimator is biased in a model-dependent way, but we propose a simple iterative procedure for obtaining an unbiased model-independent estimator. Our method can be easily applied to any dataset and requires few extra mock catalogues compared to the standard Landy-Szalay analysis. Using various sets of simulated data (lognormal, second-order LPT, and N-body), we obtain a 20–25% gain on the error bars on the two-point correlation function for the SDSS geometry and ΛCDM correlation function. When applied to SDSS data (DR7 and DR9), we achieve a similar gain on the correlation functions, which translates into a 10–15% improvement over the estimation of the densities of matter Ωm and dark energy ΩΛ in an open ΛCDM model. The constraints derived from DR7 data with our estimator are similar to those obtained with the DR9 data and the Landy-Szalay estimator, which covers a volume twice as large and has a density that is three times higher.
Key words: surveys / large-scale structure of Universe / galaxies: statistics / distance scale / cosmology: observations / methods: data analysis
© ESO, 2013
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