{"paper":{"title":"Follow-up of SN 2025wny V: Lens Modelling and Cosmography of a Strongly Lensed Superluminous Supernova at $z = 2.015$ using Space Data","arxiv_id":"2608.28430","primary_cat":"astro-ph.CO","submitted_at":"2026-08-28T15:12:58+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":true,"role":"contribution","text":"We present a lensing and cosmographic analysis of the strongly lensed Type I superluminous supernova SN 2025wny at redshift $z=2.015$, multiply imaged by two foreground galaxies at $z=0.376$.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.86,"main_claim_p":0.08,"quantitative":true,"quantitative_p":0.95,"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":1.0,"id":"s1","own":true,"role":"method","text":"Using imaging obtained with the Hubble Space Telescope and the James Webb Space Telescope, we model the lens system with two elliptical power-law mass distributions and an external shear component.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.96,"main_claim_p":0.02,"quantitative":true,"quantitative_p":0.53,"role_probabilities":{"gap":0.0,"method":1.0,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":2,"p":0.98,"id":"s2","own":true,"role":"method","text":"In addition to the supernova image positions, the modelling incorporates the surface-brightness distribution of the lensed host galaxy.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.83,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.04,"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":3,"p":1.0,"id":"s3","own":true,"role":"result","text":"The inferred Einstein radii are $\\theta_{\\rm E,1}\\simeq 1.6$\" and $\\theta_{\\rm E,2}\\simeq 0.7$ - $0.8$\", with broadly consistent results across all filters.","hedge":{"p":0.97,"label":"asserted"},"own_p":0.94,"main_claim_p":0.04,"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":0.99,"id":"s4","own":true,"role":"result","text":"After accounting for microlensing by stars in the lens galaxies, the posterior distribution spans total magnifications of approximately $\\mu_{\\rm tot}\\sim 5$--$50$, with flux ratios of the multiple images consistent with observations.","hedge":{"p":0.83,"label":"asserted"},"own_p":0.94,"main_claim_p":0.05,"quantitative":true,"quantitative_p":0.99,"role_probabilities":{"gap":0.0,"method":0.01,"result":0.99,"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":"Combining the lens models with spectroscopically and photomerically measured time delays yields a filter-marginalized constraint of \\[ H_0 = 66.7^{+7.6}_{-6.3}\\; {\\rm km\\,s^{-1}\\,Mpc^{-1}}, \\] for a fiducial model with isothermal mass profiles.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.95,"main_claim_p":0.5,"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":6,"p":1.0,"id":"s6","own":true,"role":"result","text":"Allowing the density slopes of the lens galaxies to vary over a broad range results in \\[ H_0 = 70.8^{+8.2}_{-6.1}\\; {\\rm km\\,s^{-1}\\,Mpc^{-1}}.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.95,"main_claim_p":0.21,"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":false,"role":"limitation","text":"\\] These values are conditional on the adopted parameterization of the lens mass distribution, the assumed priors on the density slopes, and possible additional lensing contributions from the surrounding large-scale environment.","hedge":{"p":0.74,"label":"asserted"},"own_p":0.37,"main_claim_p":0.06,"quantitative":false,"quantitative_p":0.04,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.0,"background":0.0,"limitation":1.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":8,"p":0.93,"id":"s8","own":true,"role":"result","text":"We find that incorporating the currently available stellar kinematic measurements has only a modest effect on the inferred value of $H_0$.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.95,"main_claim_p":0.07,"quantitative":false,"quantitative_p":0.44,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.93,"background":0.0,"limitation":0.01,"future_work":0.0,"contribution":0.0,"interpretation":0.06}},{"i":9,"p":1.0,"id":"s9","own":false,"role":"future_work","text":"Future measurements of the lens-galaxy kinematics and a detailed characterization of the lens environment will further strengthen the utility of SN 2025wny as a cosmological probe.","hedge":{"p":0.72,"label":"hedged_possibility"},"own_p":0.15,"main_claim_p":0.05,"quantitative":false,"quantitative_p":0.06,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.0,"background":0.0,"limitation":0.0,"future_work":1.0,"contribution":0.0,"interpretation":0.0}}]},"compiled":{"main_claim":{"p":0.8,"text":"Combining the lens models with spectroscopically and photomerically measured time delays yields a filter-marginalized constraint of \\[ H_0 = 66.7^{+7.6}_{-6.3}\\; 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