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TDCOSMO XXV: Measuring $H_{0}$ to 6.5% precision with quasar strong lensing and maximally flexible mass-sheet dynamics

William Sheu ^1,*, Tommaso Treu¹, Martin Millon^2,3, Frédéric Dux^4,5, Devon Williams¹, Shawn Knabel¹, Simon Birrer⁶, Pritom Mozumdar¹, Giacomo Queirolo⁷ et al. (TDCOSMO collaboration)

Giacomo Queirolo⁷, Anowar J. Shajib^8,9,10, Michele Cappellari¹¹, Kenneth C. Wong¹², Ildar M. Asfandiyarov¹³, Otabek A. Burkhonov¹³, Frédéric Courbin^14,15,16, Shuhrat A. Ehgamberdiev^13,17, Sofía Rojas-Ruiz¹, Asadulla M. Shaymanov¹³, and Talat A. Akhunov^18,13 (TDCOSMO collaboration)

¹Department of Physics and Astronomy, University of California, Los Angeles, California 90095, USA
²Institute for Particle Physics and Astrophysics, ETH Zurich, Wolfgang-Pauli-Strasse 27, CH-8093 Zurich, Switzerland
³Département de Physique Théorique, Université de Genève, 24 quai Ernest-Ansermet, CH-1211 Genève 4, Switzerland
⁴European Southern Observatory, Alonso de Córdova 3107, Vitacura, Santiago, Chile
⁵Institute of Physics, Laboratory of Astrophysics, Ecole Polytechnique Fédérale de Lausanne (EPFL), Observatoire de Sauverny, 1290 Versoix, Switzerland
⁶Department of Physics and Astronomy, Stony Brook University, Stony Brook, New York 11794, USA
⁷Laboratoire Univers et Particules de Montpellier (LUPM), CNRS and Université de Montpellier (UMR 5299), Parvis Alexander Grothendieck, F-34095 Montpellier Cedex 05, France
⁸Department of Astronomy and Astrophysics, University of Chicago, Chicago, Illinois 60637, USA
⁹Kavli Institute for Cosmological Physics, University of Chicago, Chicago, Illinois 60637, USA
¹⁰Center for Astronomy, Space Science and Astrophysics, Independent University, Bangladesh, Dhaka 1229, Bangladesh
¹¹Sub-Department of Astrophysics, Department of Physics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford, England OX1 3RH, United Kingdom
¹²Research Center for the Early Universe, Graduate School of Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan
¹³Ulugh Beg Astronomical Institute, 33 Astronomicheskaya Street, Tashkent 100052, Uzbekistan
¹⁴ICC-UB Institut de Ciències del Cosmos, Universitat de Barcelona, Martí Franquès, 1, 08028 Barcelona, Spain
¹⁵Institut Catalá de Recerca i Estudis Avançats (ICREA), Pg. Lluís Companys 23, 08010 Barcelona, Spain
¹⁶Institut dEstudis Espacials de Catalunya (IEEC), Edifici RDIT, Campus UPC, Castelldefels, 08860 Barcelona, Spain
¹⁷Samarkand State University, 15, University Boulevard, 140104, Samarkand, Uzbekistan
¹⁸National University of Uzbekistan, Department of Astronomy and Astrophysics, 100174 Tashkent, Uzbekistan

^*Contact author: wsheu@astro.ucla.edu

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Phys. Rev. D 114, 063509 – Published 10 September, 2026

DOI: https://doi.org/10.1103/rlrr-pzck

Abstract

We present a blind time-delay cosmography measurement of the Hubble-Lemaître constant $H_{0}$ based on the quadruply imaged quasar SDSSJ1433 + 6007. Our analysis combines deep Hubble Space Telescope imaging, extended time-delay monitoring from the Wendelstein and Maidanak Observatories, and spatially resolved stellar kinematics from the Keck Cosmic Web Imager and Reionization Mapper. We build a robust lens model to reconstruct the mass distribution and high-signal-to-noise kinematic maps to break the mass-sheet degeneracy, explicitly accounting for the lens galaxy’s oblateness, rotation, and anisotropy. Furthermore, we constrain the external convergence ( $κ_{ext}$ ) by characterizing the line-of-sight environment using wide-field photometry from the Dark Energy Spectroscopic Instrument (DESI) Legacy Survey data release 10. We incorporate these constraints into our joint lensing and dynamical model, running multiple iterations to estimate random and systematic uncertainties. Accounting for maximal flexibility of the mass-sheet transformation, and assuming a flat $Λ$ cold dark matter cosmology and an $Ω_{m, 0}$ prior from DESI data release 2, we infer $H_{0} = {73.2}_{- 4.7}^{+ 4.8} km s^{- 1} {Mpc}^{- 1}$ (a 6.5% precision) and an internal mass-sheet parameter $λ_{int} = 1.1 2_{- 0.06}^{+ 0.05}$ . Notably, $λ_{int}$ is $2 σ$ away from unity for this system, highlighting the importance of treating it as a free parameter. Our $H_{0}$ measurement is consistent with the result from our 2025 milestone paper, and it will be included in our next hierarchical analysis to improve the overall precision. Moving forward, the comprehensive pipeline demonstrated herein establishes a robust framework that can be readily applied to future strongly lensed systems to further refine cosmological constraints.

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TDCOSMO XXV: Measuring $H_{0}$ to 6.5% precision with quasar strong lensing and maximally flexible mass-sheet dynamics

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TDCOSMO XXV: Measuring H0 to 6.5% precision with quasar strong lensing and maximally flexible mass-sheet dynamics

Abstract

Physics Subject Headings (PhySH)

Article Text

References (106)

TDCOSMO XXV: Measuring $H_{0}$ to 6.5% precision with quasar strong lensing and maximally flexible mass-sheet dynamics