{"paper":{"title":"A Spatially Resolved [CII] Survey of 31 $z\\sim7$ Massive Galaxies Hosting Luminous Quasars","arxiv_id":"2404.15413","primary_cat":"astro-ph.GA","submitted_at":"2024-04-23T18:04:12+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-1.13.0 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":false,"role":"background","text":"The [CII] 158 $\\mu$m emission line and the underlying far-infrared (FIR) dust continuum are important tracers for studying star formation and kinematic properties of early galaxies.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.04,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.49,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.0,"background":1.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":1,"p":0.92,"id":"s1","own":true,"role":"contribution","text":"We present a survey of the [CII] emission lines and FIR continua of 31 luminous quasars at $z>6.5$ using the Atacama Large Millimeter Array (ALMA) and the NOrthern Extended Millimeter Array (NOEMA) at sub-arcsec resolution.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.98,"main_claim_p":0.05,"quantitative":true,"quantitative_p":0.97,"role_probabilities":{"gap":0.0,"method":0.08,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.92,"interpretation":0.0}},{"i":2,"p":0.84,"id":"s2","own":true,"role":"contribution","text":"This survey more than doubles the number of quasars with [CII] and FIR observations at these redshifts and enables statistical studies of quasar host galaxies deep into the epoch of reionization.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.77,"main_claim_p":0.1,"quantitative":true,"quantitative_p":0.96,"role_probabilities":{"gap":0.04,"method":0.0,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.84,"interpretation":0.12}},{"i":3,"p":1.0,"id":"s3","own":true,"role":"result","text":"We detect [CII] emission in 27 quasar hosts with a luminosity range of $L_{\\rm [CII]}=(0.3-5.5)\\times10^9~L_\\odot$ and detect the FIR continuum of 28 quasar hosts with a luminosity range of $L_{\\rm FIR}=(0.5-13.0)\\times10^{12}~L_\\odot$.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.98,"main_claim_p":0.11,"quantitative":true,"quantitative_p":0.99,"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":4,"p":1.0,"id":"s4","own":true,"role":"result","text":"Both $L_{\\rm [CII]}$ and $L_{\\rm FIR}$ are correlated ($\\rho\\simeq0.4$) with the quasar bolometric luminosity, albeit with substantial scatter.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.93,"main_claim_p":0.12,"quantitative":true,"quantitative_p":0.98,"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":"The quasar hosts detected by ALMA are clearly resolved with a median diameter of $\\sim$5 kpc.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.95,"main_claim_p":0.06,"quantitative":true,"quantitative_p":0.98,"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":1.0,"id":"s6","own":true,"role":"result","text":"About 40% of the quasar host galaxies show a velocity gradient in [CII] emission, while the rest show either dispersion-dominated or disturbed kinematics.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.95,"main_claim_p":0.06,"quantitative":true,"quantitative_p":0.99,"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":7,"p":1.0,"id":"s7","own":true,"role":"result","text":"Basic estimates of the dynamical masses of the rotation-dominated host galaxies yield $M_{\\rm dyn}=(0.1-7.5)\\times10^{11}~M_\\odot$.","hedge":{"p":0.92,"label":"asserted"},"own_p":0.94,"main_claim_p":0.07,"quantitative":true,"quantitative_p":0.98,"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":8,"p":0.54,"id":"s8","own":true,"role":"result","text":"Considering our findings alongside those of literature studies, we found that the ratio between $M_{\\rm BH}$ and $M_{\\rm dyn}$ is about ten times higher than that of local $M_{\\rm BH}-M_{\\rm dyn}$ relation on average but with substantial scatter (the ratio difference ranging from $\\sim$0.6 to 60) and large 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