# The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: Towards a computationally efficient analysis without informative priors

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**The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey : Towards a computationally efficient analysis without informative priors.** / Pellejero-Ibanez, Marcos; Chia-Hsun Chuang, Chuang; Rubiño-Martín, J. A.; Cuesta, Antonio J.; Wang, Yuting; Zhao, Gongbo; Ross, Ashley J.; Rodríguez-Torres, Sergio; Prada, Francisco; Slosar, Anže; Vazquez, Jose A.; Alam, Shadab; Beutler, Florian; Eisenstein, Daniel J.; Gil-Marín, Héctor; Grieb, Jan Niklas; Ho, Shirley; Kitaura, Francisco Shu; Percival, Will J.; Rossi, Graziano; Salazar-Albornoz, Salvador; Samushia, Lado; Sánchez, Ariel G.; Satpathy, Siddharth; Hee-Jong Seo, Seo; Tinker, Jeremy L.; Tojeiro, Rita; Vargas-Magaña, Mariana; Brownstein, Joel R.; Nichol, Robert C.; Olmstead, Matthew D.

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*Monthly Notices of the Royal Astronomical Society*, vol 468, no. 4, pp. 4116-4133. DOI: 10.1093/mnras/stx751

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*Monthly Notices of the Royal Astronomical Society*,

*468*(4), 4116-4133. DOI: 10.1093/mnras/stx751

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TY - JOUR

T1 - The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey

T2 - Monthly Notices of the Royal Astronomical Society

AU - Pellejero-Ibanez,Marcos

AU - Chia-Hsun Chuang,Chuang

AU - Rubiño-Martín,J. A.

AU - Cuesta,Antonio J.

AU - Wang,Yuting

AU - Zhao,Gongbo

AU - Ross,Ashley J.

AU - Rodríguez-Torres,Sergio

AU - Prada,Francisco

AU - Slosar,Anže

AU - Vazquez,Jose A.

AU - Alam,Shadab

AU - Beutler,Florian

AU - Eisenstein,Daniel J.

AU - Gil-Marín,Héctor

AU - Grieb,Jan Niklas

AU - Ho,Shirley

AU - Kitaura,Francisco Shu

AU - Percival,Will J.

AU - Rossi,Graziano

AU - Salazar-Albornoz,Salvador

AU - Samushia,Lado

AU - Sánchez,Ariel G.

AU - Satpathy,Siddharth

AU - Hee-Jong Seo,Seo

AU - Tinker,Jeremy L.

AU - Tojeiro,Rita

AU - Vargas-Magaña,Mariana

AU - Brownstein,Joel R.

AU - Nichol,Robert C.

AU - Olmstead,Matthew D.

PY - 2017/7/11

Y1 - 2017/7/11

N2 - We develop a new computationally efficient methodology called double-probe analysis with the aim of minimizing informative priors (those coming from extra probes) in the estimation of cosmological parameters. Using our new methodology, we extract the dark energy model-independent cosmological constraints from the joint data sets of the Baryon Oscillation Spectroscopic Survey (BOSS) galaxy sample and Planck cosmic microwave background (CMB) measurements. We measure the mean 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 the Planck data and two-point statistics from the BOSS galaxy sample. The CMB shift parameters are R=ΩmH20√r(z∗) and la = πr(z*)/rs(z*), where z* is the redshift at the last scattering surface, and r(z*) and rs(z*) denote our comoving distance to the z* and sound horizon at z*, respectively; Ωb is the baryon fraction at z = 0. This approximate methodology guarantees that we will not need to put informative priors on the cosmological parameters that galaxy clustering is unable to constrain, i.e. Ωbh2 and ns. The main advantage is that the computational time required for extracting these parameters is decreased by a factor of 60 with respect to exact full-likelihood analyses. The results obtained show no tension with the flat Λ cold dark matter (ΛCDM) cosmological paradigm. By comparing with the full-likelihood exact analysis with fixed dark energy models, on one hand we demonstrate that the double-probe method provides robust cosmological parameter constraints that can be conveniently used to study dark energy models, and on the other hand we provide a reliable set of measurements assuming dark energy models to be used, for example, in distance estimations. We extend our study to measure the sum of the neutrino mass using different methodologies, including double-probe analysis (introduced in this study), full-likelihood analysis and single-probe analysis. From full-likelihood analysis, we obtain Σmν < 0.12 (68 per cent), assuming ΛCDM and Σmν < 0.20 (68 per cent) assuming owCDM. We also find that there is degeneracy between observational systematics and neutrino masses, which suggests that one should take great care when estimating these parameters in the case of not having control over the systematics of a given sample.

AB - We develop a new computationally efficient methodology called double-probe analysis with the aim of minimizing informative priors (those coming from extra probes) in the estimation of cosmological parameters. Using our new methodology, we extract the dark energy model-independent cosmological constraints from the joint data sets of the Baryon Oscillation Spectroscopic Survey (BOSS) galaxy sample and Planck cosmic microwave background (CMB) measurements. We measure the mean 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 the Planck data and two-point statistics from the BOSS galaxy sample. The CMB shift parameters are R=ΩmH20√r(z∗) and la = πr(z*)/rs(z*), where z* is the redshift at the last scattering surface, and r(z*) and rs(z*) denote our comoving distance to the z* and sound horizon at z*, respectively; Ωb is the baryon fraction at z = 0. This approximate methodology guarantees that we will not need to put informative priors on the cosmological parameters that galaxy clustering is unable to constrain, i.e. Ωbh2 and ns. The main advantage is that the computational time required for extracting these parameters is decreased by a factor of 60 with respect to exact full-likelihood analyses. The results obtained show no tension with the flat Λ cold dark matter (ΛCDM) cosmological paradigm. By comparing with the full-likelihood exact analysis with fixed dark energy models, on one hand we demonstrate that the double-probe method provides robust cosmological parameter constraints that can be conveniently used to study dark energy models, and on the other hand we provide a reliable set of measurements assuming dark energy models to be used, for example, in distance estimations. We extend our study to measure the sum of the neutrino mass using different methodologies, including double-probe analysis (introduced in this study), full-likelihood analysis and single-probe analysis. From full-likelihood analysis, we obtain Σmν < 0.12 (68 per cent), assuming ΛCDM and Σmν < 0.20 (68 per cent) assuming owCDM. We also find that there is degeneracy between observational systematics and neutrino masses, which suggests that one should take great care when estimating these parameters in the case of not having control over the systematics of a given sample.

KW - cosmological parameters

KW - distance scale

KW - large-scale structure of Universe

KW - observations: observations

U2 - 10.1093/mnras/stx751

DO - 10.1093/mnras/stx751

M3 - Article

VL - 468

SP - 4116

EP - 4133

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

IS - 4

ER -

ID: 7756665