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Salazar-Albornoz, Salvador; Sanchez, Ariel G.; Grieb, Jan Niklas; Crocce, Martin; Scoccimarro, Roman; Alam, Shadab; Beutler, Florian; Brownstein, Joel R.; Chuang, Chia-Hsun; Kitaura, Francisco-Shu; Olmstead, Matthew D.; Percival, Will J.; Prada, Francisco; Rodriguez-Torres, Sergio; Samushia, Lado; Tinker, Jeremy; Thomas, Daniel; Tojeiro, Rita; Wang, Yuting; Zhao, Gong-bo (2017): The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: angular clustering tomography and its cosmological implications. In: Monthly Notices of the Royal Astronomical Society, Vol. 468, No. 3: pp. 2938-2956
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Abstract

We investigate the cosmological implications of studying galaxy clustering using a tomographic approach applied to the final Baryon Oscillation Spectroscopic Survey (BOSS) DR12 galaxy sample, including both auto-and cross-correlation functions between redshift shells. We model the signal of the full shape of the angular correlation function, omega(theta), in redshift bins using state-of-the-art modelling of non-linearities, bias and redshift-space distortions. We present results on the redshift evolution of the linear bias of BOSS galaxies, which cannot be obtained with traditional methods for galaxy-clustering analysis. We also obtain constraints on cosmological parameters, combining this tomographic analysis with measurements of the cosmic microwave background (CMB) and Type Ia supernova (SNIa). We explore a number of cosmological models, including the standard Lambda cold dark matter model and its most interesting extensions, such as deviations from omega(DE) =-1, non-minimal neutrino masses, spatial curvature and deviations from general relativity (GR) using the growth-index gamma parametrization. These results are, in general, comparable to the most precise present-day constraints on cosmological parameters, and show very good agreement with the standard model. In particular, combining CMB, omega(theta) and SNIa, we find a value of w(DE) consistent with -1 to a precision better than 5 per cent when it is assumed to be constant in time, and better than 6 per cent when we also allow for a spatially curved Universe.