{"paper":{"title":"Parallax Beyond a Kiloparsec from Spatially Scanning the Wide Field Camera 3 on the Hubble Space Telescope","arxiv_id":"1401.0484","primary_cat":"astro-ph.IM","submitted_at":"2014-01-02T17:46:00+00:00","version_compiled":"v1"},"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. 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5 kpc, a factor of ten farther than achieved thus far with HST.","hedge":{"p":0.54,"label":"hedged_possibility"},"own_p":0.35,"main_claim_p":0.3,"quantitative":true,"quantitative_p":0.99,"role_probabilities":{"gap":0.02,"method":0.08,"result":0.25,"background":0.01,"limitation":0.0,"future_work":0.0,"contribution":0.47,"interpretation":0.17}},{"i":2,"p":0.64,"id":"s2","own":false,"role":"background","text":"Long-period classical Cepheid variable stars in the Milky Way, nearly all of which reside beyond 1 kpc, are especially compelling targets for parallax measurements from scanning, as they may be used to anchor a determination of the Hubble constant to ~1%.","hedge":{"p":0.98,"label":"hedged_possibility"},"own_p":0.12,"main_claim_p":0.15,"quantitative":true,"quantitative_p":0.98,"role_probabilities":{"gap":0.04,"method":0.0,"result":0.0,"background":0.64,"limitation":0.0,"future_work":0.0,"contribution":0.03,"interpretation":0.29}},{"i":3,"p":0.61,"id":"s3","own":true,"role":"result","text":"We illustrate the method by measuring to high precision the parallax of a classical Cepheid, SY Aurigae, at a distance of more than 2 kpc, using 5 epochs of spatial-scan data obtained at intervals of 6 months.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.98,"main_claim_p":0.21,"quantitative":true,"quantitative_p":0.99,"role_probabilities":{"gap":0.0,"method":0.01,"result":0.61,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.38,"interpretation":0.0}},{"i":4,"p":0.73,"id":"s4","own":false,"role":"contribution","text":"Rapid spatial scans also enable photometric measurements of bright Milky Way Cepheids---which would otherwise saturate even in the shortest possible pointed observations---on the same flux scale as extragalactic Cepheids, which is a necessity for reducing a leading source of systematic error in the Hubble constant.","hedge":{"p":0.91,"label":"asserted"},"own_p":0.48,"main_claim_p":0.09,"quantitative":false,"quantitative_p":0.41,"role_probabilities":{"gap":0.03,"method":0.16,"result":0.01,"background":0.01,"limitation":0.0,"future_work":0.0,"contribution":0.73,"interpretation":0.06}},{"i":5,"p":0.52,"id":"s5","own":true,"role":"contribution","text":"We demonstrate this capability with photometric measurements of SY Aur on the same system used for Cepheids in Type Ia supernova host 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