{"paper":{"title":"A Counter-rotating Bulge in the Sb Galaxy NGC 7331","arxiv_id":"astro-ph/9602142","primary_cat":"astro-ph","submitted_at":"1996-02-27T20:14:19+00:00","version_compiled":"v2"},"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 v2","sentences":[{"i":0,"p":0.98,"id":"s0","own":true,"role":"result","text":"We have found that the bulge of the large, nearby Sb galaxy NGC 7331 rotates retrograde to its disk.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.97,"main_claim_p":0.89,"quantitative":false,"quantitative_p":0.39,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.98,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.02,"interpretation":0.0}},{"i":1,"p":0.74,"id":"s1","own":true,"role":"result","text":"Analysis of spectra in the region of the near-IR Ca II triplet along the major axis shows that, in the radial range between 5'' and ~20'', the line of sight velocity distribution of the absorption lines has two distinct peaks, and can be decomposed into a fast-rotating component with v/sigma > 3, and a slower rotating, retrograde component with v/sigma between 1 -- 1.5.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.95,"main_claim_p":0.12,"quantitative":true,"quantitative_p":0.99,"role_probabilities":{"gap":0.0,"method":0.25,"result":0.74,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.01,"interpretation":0.0}},{"i":2,"p":1.0,"id":"s2","own":true,"role":"result","text":"The radial surface brightness profile of the counter-rotating component follows that of the bulge, obtained from a 2-dimensional bulge-disk decomposition of a near-infrared K-band image, while the fast rotating component follows the disk.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.91,"main_claim_p":0.08,"quantitative":false,"quantitative_p":0.18,"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":0.99,"id":"s3","own":true,"role":"result","text":"At the radius where the disk starts to dominate the isophotes change from being considerably boxy to very disky.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.84,"main_claim_p":0.04,"quantitative":true,"quantitative_p":0.7,"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":4,"p":0.39,"id":"s4","own":true,"role":"contribution","text":"Although a number of spiral galaxies have been found that contain cold, couter-rotating disks, this is the first galaxy known to have a boxy, probably triaxial, fairly warm, counter-rotating component, which is dominating in the central regions.","hedge":{"p":0.83,"label":"asserted"},"own_p":0.73,"main_claim_p":0.43,"quantitative":true,"quantitative_p":0.65,"role_probabilities":{"gap":0.21,"method":0.0,"result":0.32,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.39,"interpretation":0.08}},{"i":5,"p":0.97,"id":"s5","own":false,"role":"interpretation","text":"If it is a bar seen end-on, this bar has to be thicker than the disk.","hedge":{"p":0.72,"label":"hedged_possibility"},"own_p":0.34,"main_claim_p":0.04,"quantitative":true,"quantitative_p":0.91,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.02,"background":0.0,"limitation":0.01,"future_work":0.0,"contribution":0.0,"interpretation":0.97}},{"i":6,"p":0.96,"id":"s6","own":true,"role":"result","text":"We find that NGC 7331, even though it is a fairly early-type spiral, does not have a conventional, co-rotating bulge.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.95,"main_claim_p":0.56,"quantitative":false,"quantitative_p":0.2,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.96,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.04}},{"i":7,"p":1.0,"id":"s7","own":false,"role":"interpretation","text":"The fact that the inner component is retrograde makes us believe that it was formed from infalling material, in either stellar or gaseous form (e.g. Balcells & Quinn 1990).","hedge":{"p":0.91,"label":"hedged_possibility"},"own_p":0.43,"main_claim_p":0.12,"quantitative":false,"quantitative_p":0.1,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":1.0}},{"i":8,"p":1.0,"id":"s8","own":false,"role":"interpretation","text":"Another possibility however is that the structure has been there since the formation of the galaxy.","hedge":{"p":0.93,"label":"hedged_possibility"},"own_p":0.14,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.03,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":1.0}},{"i":9,"p":0.97,"id":"s9","own":false,"role":"interpretation","text":"In this case it will be a challenge to explain the large change in orientation of the angular momentum when going outward 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