{"paper":{"title":"The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: weighing the neutrino mass using the galaxy power spectrum of the CMASS sample","arxiv_id":"1211.3741","primary_cat":"astro-ph.CO","submitted_at":"2012-11-15T21:00:00+00:00","version_compiled":"v4"},"notice":"Every quoted sentence is the authors' text from the arXiv listing abstract. Labels and probabilities are the outputs of classifier-1.13-20260917 on the question bank abstract-p1-20260923, exactly as returned. No sentence in this record was written by a language model.","schema":"pith.compiled-record/v0","status":"compiled","abstract":{"source":"arXiv listing abstract v4","sentences":[{"i":0,"p":0.87,"id":"s0","own":true,"role":"contribution","text":"We measure the sum of the neutrino particle masses using the three-dimensional galaxy power spectrum of the SDSS-III Baryon Oscillation Spectroscopic Survey (BOSS) Data Release 9 (DR9) CMASS galaxy sample.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.97,"main_claim_p":0.1,"quantitative":false,"quantitative_p":0.07,"role_probabilities":{"gap":0.0,"method":0.12,"result":0.01,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.87,"interpretation":0.0}},{"i":1,"p":1.0,"id":"s1","own":true,"role":"result","text":"Combined with the cosmic microwave background (CMB), supernova (SN) and additional baryonic acoustic oscillation (BAO) data, we find upper 95 percent confidence limits of the neutrino mass $\\Sigma m_{\\nu}<0.340$ eV within a flat $\\Lambda$CDM background, and $\\Sigma m_{\\nu}<0.821$ eV, assuming a more general background cosmological model.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.96,"main_claim_p":0.8,"quantitative":true,"quantitative_p":0.99,"role_probabilities":{"gap":0.0,"method":0.0,"result":1.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":2,"p":1.0,"id":"s2","own":true,"role":"result","text":"The number of neutrino species is measured to be $N_{\\rm eff}=4.308\\pm0.794$ and $N_{\\rm eff}=4.032^{+0.870}_{-0.894}$ for these two cases respectively.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.96,"main_claim_p":0.07,"quantitative":true,"quantitative_p":0.99,"role_probabilities":{"gap":0.0,"method":0.0,"result":1.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":3,"p":0.59,"id":"s3","own":true,"role":"contribution","text":"We study and quantify the effect of several factors on the neutrino measurements, including the galaxy power spectrum bias model, the effect of redshift-space distortion, the cutoff scale of the power spectrum, and the choice of additional data.","hedge":{"p":0.97,"label":"asserted"},"own_p":0.95,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.06,"role_probabilities":{"gap":0.0,"method":0.41,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.59,"interpretation":0.0}},{"i":4,"p":0.97,"id":"s4","own":true,"role":"contribution","text":"The impact of neutrinos with unknown masses on other cosmological parameter measurements is investigated.","hedge":{"p":0.68,"label":"asserted"},"own_p":0.91,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.03,"role_probabilities":{"gap":0.0,"method":0.03,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.97,"interpretation":0.0}},{"i":5,"p":1.0,"id":"s5","own":true,"role":"result","text":"The fractional matter density and the Hubble parameter are measured to be $\\Omega_M=0.2796\\pm0.0097$, $H_0=69.72^{+0.90}_{-0.91}$ km/s/Mpc (flat $\\Lambda$CDM) and $\\Omega_M=0.2798^{+0.0132}_{-0.0136}$, $H_0=73.78^{+3.16}_{-3.17}$ km/s/Mpc (more general background model).","hedge":{"p":1.0,"label":"asserted"},"own_p":0.96,"main_claim_p":0.06,"quantitative":true,"quantitative_p":0.99,"role_probabilities":{"gap":0.0,"method":0.0,"result":1.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":6,"p":1.0,"id":"s6","own":true,"role":"result","text":"Based on a Chevallier-Polarski-Linder (CPL) parametrisation of the equation-of-state $w$ of dark energy, we find that $w=-1$ is consistent with observations, even allowing for neutrinos.","hedge":{"p":0.89,"label":"hedged_possibility"},"own_p":0.97,"main_claim_p":0.07,"quantitative":true,"quantitative_p":0.93,"role_probabilities":{"gap":0.0,"method":0.0,"result":1.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":7,"p":0.99,"id":"s7","own":true,"role":"result","text":"Similarly, the curvature \\Omega_K and the running of the spectral index $\\alpha_s$ are both consistent with zero.","hedge":{"p":0.79,"label":"hedged_possibility"},"own_p":0.92,"main_claim_p":0.03,"quantitative":true,"quantitative_p":0.66,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.99,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.01}},{"i":8,"p":1.0,"id":"s8","own":true,"role":"result","text":"The tensor-to-scaler ratio is constrained down to $r<0.198$ (95 percent CL, flat $\\Lambda$ CDM) and $r<0.440$ (95 percent CL, more general background 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