{"arxiv_id":"astro-ph/0011179","incoming":{"papers":12,"sentences":12,"groups":[{"kind":"data_used","label":"Uses its data or values","papers":5,"sentences":5,"quotes":[{"arxiv_id":"2404.01742","title":"Cosmological study of a symmetric teleparallel gravity model","url":"/paper/2404.01742","section":"sLog model","sentence":"Before moving ahead with the investigation of the background phenomenology, we want to consider the predictions of BBN and EDE constraints to give us an informative limit on the parameters of the sLog model: * BBN constraint: The BBN constraint on the helium abundance is $|ΔY_p| < 0.01$ [ref] and it can be related to the effective cosmological gravitational coupling, $G_c$.","intent_p":0.96,"contests_p":null},{"arxiv_id":"0907.3919","title":"On Possible Variation in the Cosmological Baryon Fraction","url":"/paper/0907.3919","section":"$^2H$","sentence":"These are the results tabulated in [ref] [from [ref] ] plus those of [ref] and [ref] .","intent_p":1.0,"contests_p":null},{"arxiv_id":"0912.5297","title":"New cosmological constraints on primordial black holes","url":"/paper/0912.5297","section":"Current status of observations of light elements","sentence":"The weighted mean of these measurements, $D/H = (2.82 ±0.26) ×10^-5$ [ref] , agrees well with the prediction of standard BBN with the baryon-to-photon ratio inferred by observations of the CMB anisotropy [ref] .","intent_p":0.82,"contests_p":null},{"arxiv_id":"1007.4173","title":"Nuclear Reaction Uncertainties, Massive Gravitino Decays and the Cosmological Lithium Problem","url":"/paper/1007.4173","section":"Principal Nuclear Reaction Rates","sentence":"D/H: We use the deuterium abundance as determined in several high-redshift quasar absorption systems, which have a weighted mean abundance [ref]","intent_p":1.0,"contests_p":null},{"arxiv_id":"2607.27141","title":"The art of simulating the early Universe. Part III: Scalar-Gauge-Fluid Dynamics","url":"/paper/2607.27141","section":"Scalar field-fluid dynamics","sentence":"Combining the energy density and the pressure defined in pressure_and_energy_density_def, again assuming LTE and integrating by parts, one finds the following thermodynamic relation, [equation] Based on the baryon-to-photon ratio measured at present time $η_B ≡n_B/n_γ≃6 ×10^-10$ [ref] , the chemical potential can usually be neglected at high $T$, since we expect $μ/T ∼η_B$ at $T ≫m_e ≃0.5$ MeV [ref] .","intent_p":0.87,"contests_p":null}]}],"unlabelled_sentences":7},"outgoing":{"papers":0,"sentences":0,"groups":[],"unlabelled_sentences":0},"claims":[],"thresholds":{"intent_p":0.8,"supports_p":0.95,"contests_p":0.7},"method":"Citing sentences come from each paper's LaTeX source; every \\cite marks the sentence and the works it cites. Pith's classifier typed each sentence. A label is shown at intent probability 0.8 or more (0.95 for support), a contest at 0.7 or more. Measured accuracy against two blind model families is at https://pith.science/accuracy. The quoted sentences are the citing authors' own.","held_up":null,"_links":{"html":"https://pith.science/paper/astro-ph/0011179"}}