{"paper":{"title":"TDCOSMO XXVIII. The Hubble constant from the quadruply lensed quasar J1537$-$3010 with precise time delays","arxiv_id":"2609.00179","primary_cat":"astro-ph.CO","submitted_at":"2026-08-31T18:03:35+00:00","version_compiled":"v1"},"notice":"Every quoted sentence is the authors' text from the arXiv listing abstract. Labels and probabilities are the outputs of classifier-1.13.0 on the question bank abstract-p1-20260923, exactly as returned. No sentence in this record was written by a language model.","schema":"pith.compiled-record/v0","status":"compiled","abstract":{"source":"arXiv listing abstract v1","sentences":[{"i":0,"p":0.95,"id":"s0","own":true,"role":"contribution","text":"We present the first measurement of the Hubble constant ($H_0$) from the quadruply-lensed quasar J1537$-$3010, which has optically-measured time delays at $\\sim2 \\%$ precision.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.95,"main_claim_p":0.24,"quantitative":true,"quantitative_p":0.97,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.05,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.95,"interpretation":0.0}},{"i":1,"p":0.99,"id":"s1","own":true,"role":"method","text":"We combine these delays with multi-band imaging data from the Hubble Space Telescope (HST) and model the system with two independent software and teams.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.94,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.15,"role_probabilities":{"gap":0.0,"method":0.99,"result":0.0,"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":"method","text":"We adopt a mass profile that is maximally degenerate with $H_0$ to fully incorporate the mass-sheet degeneracy in the error budget, with nuisance parameters constrained by spatially resolved stellar kinematics from the Multi Unit Spectroscopic Explorer (MUSE) and a line-of-sight (LoS) analysis using the Euclid Flagship simulation.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.87,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.17,"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":3,"p":0.99,"id":"s3","own":true,"role":"method","text":"The entire analysis is performed blindly to $H_0$, distances and mass density slope of the main deflector.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.94,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.05,"role_probabilities":{"gap":0.0,"method":0.99,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.01,"interpretation":0.0}},{"i":4,"p":1.0,"id":"s4","own":true,"role":"result","text":"After unblinding, we measure $H_0 = 75.5^{+9.3}_{-5.8}\\ {\\rm km\\,s^{-1}\\,Mpc^{-1}}$, corresponding to a $10\\%$ precision measurement from a single system.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.98,"main_claim_p":0.92,"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":0.47,"id":"s5","own":true,"role":"result","text":"This precision is driven by conservative lens modeling assumptions including differences between lens modeling methods and the limited stellar kinematics constraints, from which we infer a total mass-sheet parameter $\\lambda\\equiv(1-\\kappa_{\\rm ext})\\lambda_{\\rm int} = 0.89^{+0.11}_{-0.06}$ ($\\lambda_{\\rm int}=0.89^{+0.09}_{-0.07}$) that is consistent with current results for elliptical galaxies ($\\lambda \\approx 1$).","hedge":{"p":0.55,"label":"asserted"},"own_p":0.94,"main_claim_p":0.07,"quantitative":true,"quantitative_p":0.99,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.47,"background":0.0,"limitation":0.09,"future_work":0.0,"contribution":0.0,"interpretation":0.44}},{"i":6,"p":1.0,"id":"s6","own":true,"role":"future_work","text":"Our lensing constraints, stellar kinematic measurements and LoS characterization will be included in subsequent population-level measurements of $H_0$.","hedge":{"p":0.87,"label":"asserted"},"own_p":0.77,"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":1.0,"contribution":0.0,"interpretation":0.0}},{"i":7,"p":1.0,"id":"s7","own":false,"role":"future_work","text":"Moreover, our lens models combined with future near-infrared spectroscopy and imaging from the James Webb Space Telescope will further reduce the uncertainties on $H_0$ from J1537$-$3010 alone, bringing it closer to the few percents precision of the time delays.","hedge":{"p":0.78,"label":"hedged_possibility"},"own_p":0.36,"main_claim_p":0.03,"quantitative":true,"quantitative_p":0.89,"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":1.0,"text":"After unblinding, we measure $H_0 = 75.5^{+9.3}_{-5.8}\\ {\\rm 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