Cosmological parameters; Cosmology: observations; Distance scale; Gravitational lensing: strong; 'current; Cosmology observations; Expansion rate; Hubble constant; Lens model; Measurements of; Time-delays; Astronomy and Astrophysics; Space and Planetary Science; astro-ph.GA; astro-ph.CO
Abstract :
[en] Time-delay cosmography leverages strongly lensed quasars to measure the Universe's current expansion rate, H0, independently from other methods. The latest TDCOSMO milestone measurement primarily used quadruply lensed quasars for their mass profile constraints. However, doubly lensed quasars, being more abundant and offering precise time delays, could expand the sample by a factor of 5, significantly advancing towards a 1% precision measurement of H0. We present the first TDCOSMO analysis of a doubly imaged source, HE 1104-1805, including the measurement of the four necessary ingredients. First, by combining 17 years of data from the SMARTS, Euler, and WFI telescopes, we measured a time delay of 176.3+11:4 -10:3 days. Second, using MUSE data, we extracted stellar velocity dispersion measurements in three radial bins with 5% to 13% precision. Third, employing F160W HST imaging for lens modelling and marginalising over various modelling choices, we measured the Fermat potential difference between the images. Fourth, using wide-field imaging, we measured the convergence added by objects not included in the lens modelling. By combining these four ingredients, we measured the time delay distance and the angular diameter distance to the deflector, favouring a power-law mass model over a baryonic and dark matter composite model. The measurement was performed blindly to prevent experimenter bias and resulted in a Hubble constant of H0 = 64:2+5:8 -5:0 × λint km s-1Mpc-1, where λint is the internal mass sheet degeneracy parameter. This is in agreement with the TDCOSMO-2025 milestone and its precision for λint = 1 is comparable to that obtained with the best-observed quadruply lensed quasars (4-6%). This work is a stepping stone towards a precise measurement of H0 using a large sample of doubly lensed quasars, supplementing the current sample. The next TDCOSMO milestone paper will include this system in its hierarchical analysis, constraining λint and H0 jointly with multiple lenses.
Research Center/Unit :
STAR - Space sciences, Technologies and Astrophysics Research - ULiège
Disciplines :
Space science, astronomy & astrophysics
Author, co-author :
Paic, Eric ; Research Center for the Early Universe, Graduate School of Science, The University of Tokyo, Tokyo, Japan ; Institute of Physics, Laboratory of Astrophysics, Ecole Polytechnique Fédérale de Lausanne (EPFL), Versoix, Switzerland
Courbin, Frédéric ; Institut de Ciències del Cosmos (ICCUB), Universitat de Barcelona (IEEC-UB), Barcelona, Spain ; Institució Catalana de Recerca i Estudis Avançats (ICREA), Barcelona, Spain
Fassnacht, Christopher D. ; Department of Physics and Astronomy, Uc Davis, Davis, United States
Galan, Aymeric ; Technical University of Munich, Tum School of Natural Sciences, Physics Department, Garching, Germany ; Max-Planck-Institut für Astrophysik, Garching, Germany
Millon, Martin ; Institute for Particle Physics and Astrophysics, Eth Zurich, Zurich, Switzerland
Sluse, Dominique ; Université de Liège - ULiège > Département d'astrophysique, géophysique et océanographie (AGO)
Williams, Devon M. ; Department of Physics and Astronomy, University of California, Los Angeles, United States
Birrer, Simon ; Department of Physics and Astronomy, Stony Brook University, Stony Brook, United States
Buckley-Geer, Elizabeth J.; Fermi National Accelerator Laboratory, Batavia, United States ; Department of Astronomy & Astrophysics, University of Chicago, Chicago, United States
Cappellari, Michele ; Sub-Department of Astrophysics, Department of Physics, University of Oxford, Oxford, United Kingdom
Dux, Frédéric ; Institute of Physics, Laboratory of Astrophysics, Ecole Polytechnique Fédérale de Lausanne (EPFL), Versoix, Switzerland ; European Southern Observatory, Santiago, Chile
Huang, Xiang-Yu ; Department of Physics and Astronomy, Stony Brook University, Stony Brook, United States
Knabel, Shawn ; Department of Physics and Astronomy, University of California, Los Angeles, United States
Lemon, Cameron ; Oskar Klein Centre, Department of Physics, Stockholm University, Stockholm, Sweden
Shajib, Anowar J. ; Department of Astronomy & Astrophysics, University of Chicago, Chicago, United States ; Kavli Institute for Cosmological Physics, University of Chicago, Chicago, United States ; Center for Astronomy Space Science and Astrophysics, Independent University, Dhaka, Bangladesh
Suyu, Sherry H. ; Technical University of Munich, Tum School of Natural Sciences, Physics Department, Garching, Germany ; Max-Planck-Institut für Astrophysik, Garching, Germany
Treu, Tommaso; Department of Physics and Astronomy, University of California, Los Angeles, United States
Wong, Kenneth C. ; Research Center for the Early Universe, Graduate School of Science, The University of Tokyo, Tokyo, Japan
Christensen, Lise ; Cosmic Dawn Center (DAWN), Niels Bohr Institute, University of Copenhagen, Copenhagen N, Denmark
Motta, Veronica ; Instituto de Fìsica y Astronomía, Universidad de Valparaíso, Valparaíso, Chile
Sonnenfeld, Alessandro ; Department of Astronomy, School of Physics and Astronomy, Shanghai Jiao Tong University, Shanghai, China ; Shanghai Key Laboratory for Particle Physics and Cosmology, Shanghai Jiao Tong University, Shanghai, China ; Key Laboratory for Particle Physics Astrophysics and Cosmology, Ministry of Education, Shanghai Jiao Tong University, Shanghai, China
F.R.S.-FNRS - Fonds de la Recherche Scientifique SNSF - Swiss National Science Foundation FONDECYT - Chile Fondo Nacional de Desarrollo Científico y Tecnológico NASA - National Aeronautics and Space Administration European Union
Funding number :
4.4503.1.
Funding text :
E.P. is supported by JSPS KAKENHI Grant Number JP24H00221. F.C. is supported by the Swiss National Science Foundation (SNSF) and by the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (COSMICLENS: grant agreement No 787886). C.D.F. acknowledges support for this work from the National Science Foundation under Grant No. AST-2407278. A.G. acknowledges support by the SNSF (Swiss National Science Foundation) through a mobility grant P500PT_211034. M.M. acknowledges support by the SNSF (Swiss National Science Foundation) through mobility grant P500PT_203114 and return CH grant P5R5PT_225598. D.S. acknowledges the support of the Fonds de la Recherche Scientifique-FNRS, Belgium, under grant No. 4.4503.1. S.B. acknowledges support by the Department of Physics and Astronomy, Stony Brook University. C.L. acknowledges funding from the European Union's Horizon Europe research and innovation programme under the Marie Sklodovska-Curie grant agreement No. 101105725. A.J.S. received support from NASA through STScI grants HST-GO-16773 and JWST-GO-2974. S.H.S. thanks the Max Planck Society for support through the Max Planck Fellowship. This work is supported in part by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany's Excellence Strategy - EXC-2094 - 390783311. T.T. acknowledges support by NSF through grants NSFAST-1906976, NSF-AST-1836016 and NSF-AST-2407277, and from the Moore Foundation through grant 8548. K.C. W. acknowledges support by JSPS KAKENHI Grant Numbers JP24K07089, JP24H00221. V.M. acknowledges support from ANID FONDECYT Regular grant number 1231418, Centro de Astrof\u00EDsica de Valpara\u00EDso CIDI 21, and ANID, Millennium Science Initiative, AIM23-0001. This work used observations collected at the European Southern Observatory under ESO programmes 092.0515(B) and 0102.A-0600(A). This work used Python packages Numpy (Harris et al. 2020), Astropy (Astropy Collaboration 2022), and Scipy (Virtanen et al. 2020).E.P. is supported by JSPS KAKENHI Grant Number JP24H00221. F.C. is supported by the Swiss National Science Foundation (SNSF) and by the European Research Council (ERC) under the European Union\u2019s Horizon 2020 research and innovation programme (COSMICLENS: grant agreement No 787886). C.D.F. acknowledges support for this work from the National Science Foundation under Grant No. AST-2407278. A.G. acknowledges support by the SNSF (Swiss National Science Foundation) through a mobility grant P500PT_211034. M.M. acknowledges support by the SNSF (Swiss National Science Foundation) through mobility grant P500PT_203114 and return CH grant P5R5PT_225598. D.S. acknowledges the support of the Fonds de la Recherche Scientifique-FNRS, Belgium, under grant No. 4.4503.1. S.B. acknowledges support by the Department of Physics and Astronomy, Stony Brook University. C.L. acknowledges funding from the European Union\u2019s Horizon Europe research and innovation programme under the Marie Sklodovska-Curie grant agreement No. 101105725. A.J.S. received support from NASA through STScI grants HST-GO-16773 and JWST-GO-2974. S.H.S. thanks the Max Planck Society for support through the Max Planck Fellowship. This work is supported in part by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany\u2019s Excellence Strategy \u2013 EXC-2094 \u2013 390783311. T.T. acknowledges support by NSF through grants NSF-AST-1906976, NSF-AST-1836016 and NSF-AST-2407277, and from the Moore Foundation through grant 8548. K.C.W. acknowledges support by JSPS KAKENHI Grant Numbers JP24K07089, JP24H00221. V.M. acknowledges support from ANID FONDECYT Regular grant number 1231418, Centro de Astrof\u00EDsica de Valpara\u00EDso CIDI 21, and ANID, Millennium Science Initiative, AIM23-0001. This work used observations collected at the European Southern Observatory under ESO programmes 092.0515(B) and 0102.A-0600(A). This work used Python packages Numpy (), Astropy (), and Scipy ().
