{"paper":{"title":"The rates and time-delay distribution of multiply imaged supernovae behind lensing clusters","arxiv_id":"1210.7681","primary_cat":"astro-ph.CO","submitted_at":"2012-10-29T14:42:51+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":false,"role":"background","text":"Time delays of gravitationally lensed sources can be used to constrain the mass model of a deflector and determine cosmological parameters.","hedge":{"p":0.63,"label":"asserted"},"own_p":0.04,"main_claim_p":0.04,"quantitative":false,"quantitative_p":0.03,"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":0.99,"id":"s1","own":true,"role":"contribution","text":"We here present an analysis of the time-delay distribution of multiply imaged sources behind 17 strong lensing galaxy clusters with well-calibrated mass models.","hedge":{"p":0.91,"label":"asserted"},"own_p":0.94,"main_claim_p":0.06,"quantitative":true,"quantitative_p":0.89,"role_probabilities":{"gap":0.0,"method":0.01,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.99,"interpretation":0.0}},{"i":2,"p":1.0,"id":"s2","own":true,"role":"result","text":"We find that for time delays less than 1000 days, at z=3.0, their logarithmic probability distribution functions are well represented by P (log \\Delta t)=5.3 x 10^-4 \\Delta t^\\beta M_250^-2\\beta, with \\beta=0.77, where M_250 is the projected cluster mass inside 250 kpc (in 10^14 M_sun), and \\beta is the power-law slope of the distribution.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.96,"main_claim_p":0.53,"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":3,"p":0.68,"id":"s3","own":true,"role":"interpretation","text":"The resultant probability distribution function enables us to estimate the time-delay distribution in a lensing cluster of known mass.","hedge":{"p":0.82,"label":"asserted"},"own_p":0.73,"main_claim_p":0.13,"quantitative":false,"quantitative_p":0.04,"role_probabilities":{"gap":0.0,"method":0.01,"result":0.25,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.05,"interpretation":0.68}},{"i":4,"p":1.0,"id":"s4","own":true,"role":"result","text":"For a cluster with M_250=2 x 10^14 M_sun, the fraction of time delays less than 1000 days is approximately 3%.","hedge":{"p":0.91,"label":"asserted"},"own_p":0.89,"main_claim_p":0.09,"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":5,"p":0.7,"id":"s5","own":true,"role":"interpretation","text":"Taking Abell 1689 as an example, its dark halo and brightest galaxies, with central velocity dispersions larger than 500 km/s, mainly produce large time delays, while galaxy-scale mass clumps are responsible for generating smaller time delays.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.79,"main_claim_p":0.08,"quantitative":true,"quantitative_p":0.95,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.3,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.7}},{"i":6,"p":0.86,"id":"s6","own":true,"role":"contribution","text":"We estimate the probability of observing multiple images of a supernova in the known images of Abell 1689.","hedge":{"p":0.89,"label":"asserted"},"own_p":0.92,"main_claim_p":0.04,"quantitative":false,"quantitative_p":0.05,"role_probabilities":{"gap":0.0,"method":0.11,"result":0.03,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.86,"interpretation":0.0}},{"i":7,"p":0.98,"id":"s7","own":true,"role":"method","text":"A two-component model of estimating the supernova rate is applied in this work.","hedge":{"p":0.98,"label":"asserted"},"own_p":0.82,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.05,"role_probabilities":{"gap":0.0,"method":0.98,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.02,"interpretation":0.0}},{"i":8,"p":1.0,"id":"s8","own":true,"role":"result","text":"For a magnitude threshold of m_AB=26.5, the yearly rate of Type Ia (core-collapse) supernovae with time delays less than 1000 days is 0.004 +- 0.002 (0.029 +- 0.001).","hedge":{"p":1.0,"label":"asserted"},"own_p":0.92,"main_claim_p":0.16,"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":9,"p":1.0,"id":"s9","own":true,"role":"result","text":"If the magnitude threshold is lowered to m_AB ~ 27.0, the rate of core-collapse supernovae suitable for time delay observation is 0.044 +- 0.015 per year.","hedge":{"p":0.97,"label":"asserted"},"own_p":0.89,"main_claim_p":0.12,"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}}]},"compiled":{"main_claim":{"p":0.95,"text":"We find that for time delays less than 1000 days, at z=3.0, their logarithmic probability distribution functions are well represented by P (log \\Delta t)=5.3 x 10^-4 \\Delta t^\\beta M_250^-2\\beta, 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