@article {604550,
	title = {The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: towards a computationally efficient analysis without informative priors},
	journal = {Monthly Notices of the Royal Astronomical Society},
	volume = {468},
	year = {2017},
	month = {July 1, 2017},
	pages = {4116-4133},
	abstract = {We develop a new computationally efficient methodology calleddouble-probe analysis with the aim of minimizing informative priors(those coming from extra probes) in the estimation of cosmologicalparameters. Using our new methodology, we extract the dark energymodel-independent cosmological constraints from the joint data sets ofthe Baryon Oscillation Spectroscopic Survey (BOSS) galaxy sample andPlanck cosmic microwave background (CMB) measurements. We measure themean values and covariance matrix of {R, la,Ωbh2, ns, log(As),Ωk, H(z), DA(z),f(z)σ8(z)}, which give an efficient summary of thePlanck data and two-point statistics from the BOSS galaxy sample. TheCMB shift parameters are R=√{Ω _m H_0^2} r(z_*) andla = πr(z*)/rs(z*), wherez* is the redshift at the last scattering surface, andr(z*) and rs(z*) denote our comovingdistance to the z* and sound horizon at z*,respectively; Ωb is the baryon fraction at z = 0. Thisapproximate methodology guarantees that we will not need to putinformative priors on the cosmological parameters that galaxy clusteringis unable to constrain, I.e. Ωbh2 andns. The main advantage is that the computational timerequired for extracting these parameters is decreased by a factor of 60with respect to exact full-likelihood analyses. The results obtainedshow no tension with the flat Λ cold dark matter (ΛCDM)cosmological paradigm. By comparing with the full-likelihood exactanalysis with fixed dark energy models, on one hand we demonstrate thatthe double-probe method provides robust cosmological parameterconstraints that can be conveniently used to study dark energy models,and on the other hand we provide a reliable set of measurements assumingdark energy models to be used, for example, in distance estimations. Weextend our study to measure the sum of the neutrino mass using differentmethodologies, including double-probe analysis (introduced in thisstudy), full-likelihood analysis and single-probe analysis. Fromfull-likelihood analysis, we obtain Σmν < 0.12(68 per cent), assuming ΛCDM and Σmν ,
	keywords = {cosmological parameters;  distance scale;  large-scale structure of Universe;  cosmology: observations},
	isbn = {0035-8711},
	url = {http://adsabs.harvard.edu/abs/2017MNRAS.468.4116P},
	author = {Pellejero-Ibanez, Marcos and Chuang, Chia-Hsun and Rubi{\~n}o-Mart{\'\i}n, J. A. and Antonio J. Cuesta and Wang, Yuting and Zhao, Gongbo and Ashley J. Ross and Rodr{\'\i}guez-Torres, Sergio and Prada, Francisco and Slosar, An{\v z}e and Vazquez, Jose A. and Alam, Shadab and Beutler, Florian and Daniel J. Eisenstein and Gil-Mar{\'\i}n, H{\'e}ctor and Niklas Grieb, Jan and Ho, Shirley and Francisco-Shu Kitaura and Will J. Percival and Rossi, Graziano and Salazar-Albornoz, Salvador and Samushia, Lado and S{\'a}nchez, Ariel G. and Satpathy, Siddharth and Seo, Hee-Jong and Tinker, Jeremy L. and Tojeiro, Rita and Vargas-Maga{\~n}a, Mariana and Brownstein, Joel R. and Robert C. Nichol and Olmstead, Matthew D.}
}
