{"arxiv_id":"astro-ph/0209478","incoming":{"papers":23,"sentences":25,"groups":[{"kind":"comparison","label":"Compares with it","papers":1,"sentences":1,"quotes":[{"arxiv_id":"1006.2760","title":"Simulations and Observations of the Microwave Universe","url":"/paper/1006.2760","section":"Low frequency point sources","sentence":"< g r a p h i c s > [Comparison of the 30 GHz differential source counts]Comparison of the 30 GHz differential source counts from [ref] rescaled by a factor of 0.7 (black dotted line) with the $1 σ$ ranges from measurements by (right-to-left) WMAP Ka band [ref] , DASI [ref] , VSA [ref] , CBI [ref] and GBT [ref]","intent_p":0.89,"contests_p":null}]},{"kind":"background","label":"Cites it as background","papers":13,"sentences":13,"quotes":[{"arxiv_id":"2105.03648","title":"Primordial black holes in interferometry","url":"/paper/2105.03648","section":"Conclusions","sentence":"Interferometric observations on the CMB have been considered and carried out over the last decades [ref] .","intent_p":0.97,"contests_p":null},{"arxiv_id":"2307.13083","title":"The Cosmic Microwave Background and $H_0$","url":"/paper/2307.13083","section":"Introduction","sentence":"The first detection of CMB polarization was announced by the Degree Angular Scale Interferometer [ref] in 2002, followed by the Wilkinson Microwave Anisotropy Probe [ref] .","intent_p":0.84,"contests_p":null},{"arxiv_id":"1608.07452","title":"Tensor Minkowski Functionals: first application to the CMB","url":"/paper/1608.07452","section":"Introduction","sentence":"This polarization was first detected by DASI [ref] .","intent_p":0.8,"contests_p":null},{"arxiv_id":"1907.12085","title":"Polarization of the Cosmic Infrared Background Fluctuations","url":"/paper/1907.12085","section":"Introduction","sentence":"In 2001, the Degree Angular Scale Interferometer (DASI) experiment for the first time detected an electriclike component ($E$-mode) of the predicted polarization signal [ref] and opened up a window for the CMB polarization science.","intent_p":0.93,"contests_p":null},{"arxiv_id":"1510.09217","title":"BICEP2 / Keck Array VI: Improved Constraints On Cosmology and Foregrounds When Adding 95 GHz Data From Keck Array","url":"/paper/1510.09217","section":"Introduction","sentence":"This naturally produces a polarization pattern with direction parallel/perpendicular to the gradient of its intensity—this is curl-free, or $E$-mode polarization, and was first detected in Ref. [ref] .","intent_p":0.9,"contests_p":null}]}],"unlabelled_sentences":11},"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/0209478"}}