{"arxiv_id":"1104.5403","incoming":{"papers":1,"sentences":3,"groups":[{"kind":"method_or_tool","label":"Uses its method or tool","papers":1,"sentences":1,"quotes":[{"arxiv_id":"1203.2307","title":"The 21 cm Signature of Shock Heated and Diffuse Cosmic String Wakes","url":"/paper/1203.2307","section":"Diffuse Cosmic String Wakes","sentence":"To derive this noise temperature per pixel in [ref] we began with the thermal noise per visibility as given by Morales [ref] to arrive at the thermal noise per pixel for the brightness temperature.","intent_p":0.9,"contests_p":null}]}],"unlabelled_sentences":2},"outgoing":{"papers":12,"sentences":20,"groups":[{"kind":"method_or_tool","label":"Uses the method or tool of","papers":2,"sentences":3,"quotes":[{"arxiv_id":"0709.1144","title":"Cosmic Microwave Background Statistics for a Direction-Dependent Primordial Power Spectrum","url":"/paper/0709.1144","section":"Forecasting the anisotropies","sentence":"We follow Pullen-Kamionkowski [ref] and expand the anisotropic $P_b(q⃗)$ in terms of spherical harmonics P_b(q⃗) = 𝒫(q) [1+∑_L,M g_L,M (q) Y_L,M(q̂)] To estimate the constraints possible on the $g_L,M$'s, we calculate the Fisher matrix.","intent_p":0.97,"contests_p":null},{"arxiv_id":"astro-ph/9712195","title":"Interferometric Observation of Cosmic Microwave Background Anisotropies","url":"/paper/astro-ph/9712195","section":"The angular power spectrum in the flat sky distant observer approximation","sentence":"We follow [ref] for the definition of the $a$'s, and applying it to our case, for large $l$ we define a 2-D vector $l⃗=(lcosϕ_l,lsinϕ_l)$, such that a(l⃗,χ) = ( ∑^l_m=-l [(i l)^-m√(4π2l+1(l+m)!(l-m)!) e^imϕ_l a_lm ] ) ∼ ∫d^2ϵ e^(-i l⃗ ·ϵ⃗) δ_21(χ,x̂)","intent_p":0.85,"contests_p":null}]},{"kind":"data_used","label":"Uses data or values from","papers":2,"sentences":2,"quotes":[{"arxiv_id":"astro-ph/0401206","title":"The CMBR fluctuations from HI perturbations prior to reionization","url":"/paper/astro-ph/0401206","section":"The 21 cm brightness temperature and its power spectrum","sentence":"[ref] gives the proportionality constant $g(z)$ for redshift $z$ between 10 and 1000.","intent_p":0.98,"contests_p":null},{"arxiv_id":"0901.0555","title":"ARCADE 2 Measurement of the Extra-Galactic Sky Temperature at 3-90 GHz","url":"/paper/0901.0555","section":"Forecasting the anisotropies","sentence":"The system temperature is given by ARCADE 2 [ref] as T_sys = 1.26 K ((1+z) 1 GHz/ν_21)^2.6","intent_p":0.99,"contests_p":null}]},{"kind":"background","label":"Cites as background","papers":3,"sentences":4,"quotes":[{"arxiv_id":"astro-ph/0608032","title":"Cosmology at Low Frequencies: The 21 cm Transition and the High-Redshift Universe","url":"/paper/astro-ph/0608032","section":"The 21 cm brightness temperature and its power spectrum","sentence":"This difference in intensity is expressed through the brightness temperature [ref] :","intent_p":0.85,"contests_p":null},{"arxiv_id":"0709.1144","title":"Cosmic Microwave Background Statistics for a Direction-Dependent Primordial Power Spectrum","url":"/paper/0709.1144","section":"Introduction","sentence":"Put another way, “the density of matter may differ from one point in the Universe to another, but the distribution of matter is described as a realization of a random field with a variance that is everywhere the same and the same in every direction” [ref] .","intent_p":0.84,"contests_p":null},{"arxiv_id":"astro-ph/0701357","title":"Imprints of a Primordial Preferred Direction on the Microwave Background","url":"/paper/astro-ph/0701357","section":"Introduction","sentence":"Ackerman, Carroll and Wise [ref] have considered the possibility that rotational invariance was broken in a scale invariant way during inflation, by an effect that has since disappeared.","intent_p":0.82,"contests_p":null}]}],"unlabelled_sentences":11},"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/1104.5403"}}