2016/07/11 by Marcos Pellejero-Ibanez, Chia-Hsun Chuang, Pellejero-Ibanez, Marcos +59
Physics and Astronomy · #Cosmology and Nongalactic Astrophysics (astro-ph.CO) #FOS: Physical sciences #astro-ph.CO
paper · pdf · doi:10.48550/arxiv.1607.03152
19 pages, 17 figures
arxiv created 2016/07/11 · arxiv updated 2016/07/13
We develop a new methodology called double-probe analysis with the aim of minimizing informative priors in the estimation of cosmological parameters. We extract the dark-energy-model-independent cosmological constraints from the joint data sets of Baryon Oscillation Spectroscopic Survey (BOSS) galaxy sample and Planck cosmic microwave background (CMB) measurement. We measure the mean values and covariance matrix of \R, la, Ωb h2, ns, log(As), Ωk, H(z), DA(z), f(z)σ8(z)\, which give an efficient summary of Planck data and 2-point statistics from BOSS galaxy sample, where R=√(Ωm H02) r(z_*), and la=πr(z_*)/rs(z_*), z_* is the redshift at the last scattering surface, and r(z_*) and rs(z_*) denote our comoving distance to z_* and sound horizon at z_* respectively. The advantage of this method is that we do not need to put informative priors on the cosmological parameters that galaxy clustering is not able to constrain well, i.e. Ωb h2 and ns. Using our double-probe results, we obtain Ωm=0.304±0.009, H0=68.2±0.7, and σ8=0.806±0.014 assuming ΛCDM; and Ωk=0.002±0.003 and w=-1.00±0.07 assuming owCDM. The results show no tension with the flat ΛCDM cosmological paradigm. By comparing with the full-likelihood analyses with fixed dark energy models, we demonstrate that the double-probe method provides robust cosmological parameter constraints which can be conveniently used to study dark energy models. We extend our study to measure the sum of neutrino mass and obtain Σmν<0.10/0.22 (68%/95%) assuming ΛCDM and Σmν<0.26/0.52 (68%/95%) assuming wCDM. This paper is part of a set that analyses the final galaxy clustering dataset from BOSS.