{"paper":{"title":"ARGOS IV: The Kinematics of the Milky Way Bulge","arxiv_id":"1303.6656","primary_cat":"astro-ph.GA","submitted_at":"2013-03-26T20:44:22+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. No sentence in this record was written by a language model.","schema":"pith.compiled-record/v0","status":"compiled","abstract":{"source":"arXiv listing abstract v1","sentences":[{"i":0,"p":1.0,"id":"s0","own":true,"role":"contribution","text":"We present the kinematic results from our ARGOS spectroscopic survey of the Galactic bulge of the Milky Way.","hedge":{"p":0.96,"label":"asserted"},"own_p":0.94,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.04,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":1.0,"interpretation":0.0}},{"i":1,"p":0.65,"id":"s1","own":false,"role":"background","text":"Our aim is to understand the formation of the Galactic bulge.","hedge":{"p":0.63,"label":"asserted"},"own_p":0.16,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.02,"role_probabilities":{"gap":0.11,"method":0.0,"result":0.0,"background":0.65,"limitation":0.0,"future_work":0.05,"contribution":0.19,"interpretation":0.0}},{"i":2,"p":0.62,"id":"s2","own":true,"role":"contribution","text":"We examine the kinematics of about 17,400 stars in the bulge located within 3.5 kpc of the Galactic centre, identified from the 28,000 star ARGOS survey.","hedge":{"p":0.96,"label":"asserted"},"own_p":0.91,"main_claim_p":0.03,"quantitative":true,"quantitative_p":0.99,"role_probabilities":{"gap":0.0,"method":0.38,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.62,"interpretation":0.0}},{"i":3,"p":0.45,"id":"s3","own":false,"role":"background","text":"We aim to determine if the formation of the bulge has been internally driven from disk instabilities as suggested by its boxy shape, or if mergers have played a significant role as expected from Lambda CDM simulations.","hedge":{"p":0.82,"label":"hedged_possibility"},"own_p":0.11,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.08,"role_probabilities":{"gap":0.43,"method":0.0,"result":0.0,"background":0.45,"limitation":0.0,"future_work":0.01,"contribution":0.1,"interpretation":0.01}},{"i":4,"p":1.0,"id":"s4","own":true,"role":"result","text":"From our velocity measurements across latitudes b = -5 deg, -7.5 deg and -10 deg we find the bulge to be a cylindrically rotating system that transitions smoothly out into the disk.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.98,"main_claim_p":0.38,"quantitative":true,"quantitative_p":0.8,"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":5,"p":1.0,"id":"s5","own":true,"role":"result","text":"Within the bulge, we find a kinematically distinct metal-poor population ([Fe/H] < -1.0) that is not rotating cylindrically.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.97,"main_claim_p":0.11,"quantitative":true,"quantitative_p":0.9,"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":6,"p":0.76,"id":"s6","own":true,"role":"interpretation","text":"The 5% of our stars with [Fe/H] < -1.0 are a slowly rotating spheroidal population, which we believe are stars of the metal weak thick disk and halo which presently lie in the inner Galaxy.","hedge":{"p":0.57,"label":"hedged_possibility"},"own_p":0.89,"main_claim_p":0.09,"quantitative":true,"quantitative_p":0.99,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.24,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.76}},{"i":7,"p":0.78,"id":"s7","own":true,"role":"interpretation","text":"The kinematics of the two bulge components that we identified in ARGOS paper III (mean [Fe/H] = -0.25 and [Fe/H] = +0.15, respectively) demonstrate that they are likely to share a common formation origin and are distinct from the more metal poor populations of the thick disk and halo which are colocated inside the bulge.","hedge":{"p":0.84,"label":"hedged_possibility"},"own_p":0.9,"main_claim_p":0.23,"quantitative":true,"quantitative_p":0.93,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.22,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.78}},{"i":8,"p":0.99,"id":"s8","own":true,"role":"interpretation","text":"We do not exclude an underlying merger generated bulge component but our results favour bulge formation from instabilities in the early thin 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