The Dark Energy Survey Supernova Program: an updated measurement of the Hubble constant using the inverse distance ladder

ABSTRACT We measure the current expansion rate of the Universe, Hubble’s constant $H_0$, by calibrating the absolute magnitudes of supernovae to distances measured by baryon acoustic oscillations (BAO). This ‘inverse distance ladder’ technique provides an alternative to calibrating supernovae using nearby absolute distance measurements, replacing the calibration with a high-redshift anchor. We use the recent release of 1829 supernovae from the Dark Energy Survey spanning $0.01\lt z\lt 1.13$ anchored to the recent baryon acoustic oscillation measurements from Dark Energy Spectroscopic Instrument (DESI) spanning $0.30 \lt z_{\mathrm{eff}}\lt 2.33$. To trace cosmology to $z=0$, we use the third-, fourth-, and fifth-order cosmographic models, which, by design, are agnostic about the energy content and expansion history of the universe. With the inclusion of the higher redshift DESI-BAO data, the third-order model is a poor fit to both data sets, with the fourth-order model being preferred by the Akaike Information Criterion. Using the fourth-order cosmographic model, we find $H_0=67.19^{+0.66}_{-0.64}\mathrm{~km} \mathrm{~s}^{-1} \mathrm{~Mpc}^{-1}$, in agreement with the value found by Planck without the need to assume Flat-$\Lambda$CDM. However, the best-fitting expansion history differs from that of Planck, providing continued motivation to investigate these tensions.

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Publication Details

Journal
Monthly Notices of the Royal Astronomical Society
Published
2025-01-23
DOI
https://doi.org/10.1093/mnras/staf122
Citations
16
Primary Topic
Cosmology and Gravitation Theories
Type
article
Field-Weighted Citation Impact
16.17

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article

The Dark Energy Survey Supernova Program: an updated measurement of the Hubble constant using the inverse distance ladder

R Camilleri, A. Pieres, N. Suntzeff, A. Roodman et al.
16 citations
Monthly Notices of the Royal Astronomical Society
Cosmology and Gravitation Theories
16.17
article

The Dark Energy Survey Supernova Program: an updated measurement of the Hubble constant using the inverse distance ladder

R Camilleri, A. Pieres, N. Suntzeff, A. Roodman, B. Sánchez, O. Lahav, S. Everett, I. Ferrero, S. R. Hinton, A. Möller, L. Galbany, J. Carretero, J. García-Bellido, S. Bocquet, D. Scolnic, L. N. da Costa, G. Giannini, P. Armstrong, Karl Glazebrook, F. J. Castander, S. Kent, A. A. Plazas, Gregory Tarlé, E. Suchyta, P. Wiseman, Christopher J. Conselice, D Huterer, P Shah, A. Palmese, T. M. C. Abbott, J. Asorey, D. Sanchez Cid, D. Carollo, Eusebio Sanchez, Dillon Brout, J. Mena-Fernández, M. Šako, Geraint F. Lewis, A. Carnero Rosell, ENRIQUE GAZTAÑAGA, David Bacon, D L Hollowood, M. Vincenzi, T. M. Davis, R. L. C. Ogando, K. Herner, J Myles, M. Lima, M. E. S. Pereira, Christopher E. Lidman, H. T. Diehl, F. Andrade-Oliveira, M. Aguena, S Lee, E. Buckley‐Geer, M. Sullivan, S. Samuroff, R. C. Nichol, S Desai, R A Gruendl, A R Walker, J Frieman, K Kuehn, R Miquel, D J James, B E Tucker, K Honscheid, S Allam, D. L. Burke, I Sevilla-Noarbe, N. Weaverdyck, J Lee, B. Flaugher, M Schubnell, J. L. Marshall, M.E.C. Swanson, K. Bechtol, A. K. Romer, S. Àvila, Donal Brooks, M Smith
article en
16 citations

Abstract

ABSTRACT We measure the current expansion rate of the Universe, Hubble’s constant $H_0$, by calibrating the absolute magnitudes of supernovae to distances measured by baryon acoustic oscillations (BAO). This ‘inverse distance ladder’ technique provides an alternative to calibrating supernovae using nearby absolute distance measurements, replacing the calibration with a high-redshift anchor. We use the recent release of 1829 supernovae from the Dark Energy Survey spanning $0.01\lt z\lt 1.13$ anchored to the recent baryon acoustic oscillation measurements from Dark Energy Spectroscopic Instrument (DESI) spanning $0.30 \lt z_{\mathrm{eff}}\lt 2.33$. To trace cosmology to $z=0$, we use the third-, fourth-, and fifth-order cosmographic models, which, by design, are agnostic about the energy content and expansion history of the universe. With the inclusion of the higher redshift DESI-BAO data, the third-order model is a poor fit to both data sets, with the fourth-order model being preferred by the Akaike Information Criterion. Using the fourth-order cosmographic model, we find $H_0=67.19^{+0.66}_{-0.64}\mathrm{~km} \mathrm{~s}^{-1} \mathrm{~Mpc}^{-1}$, in agreement with the value found by Planck without the need to assume Flat-$\Lambda$CDM. However, the best-fitting expansion history differs from that of Planck, providing continued motivation to investigate these tensions.

Monthly Notices of the Royal Astronomical SocietyVol. 537(2)
Australian National University (AU), Institució Catalana de Recerca i Estudis Avançats (ES), Universidad Complutense de Madrid (ES), Oak Ridge National Laboratory (US), Northeastern University (US), Centre National de la Recherche Scientifique (FR), The University of Sydney (AU), Fermi National Accelerator Laboratory (US), Institute of Space Sciences (ES), Jet Propulsion Laboratory (US), University of Wisconsin–Madison (US), University of Nottingham (GB), Lawrence Berkeley National Laboratory (US), University of Illinois Urbana-Champaign (US), Universität Hamburg (DE), University of Sussex (GB), The University of Queensland (AU), Duke University (US), Universidade de São Paulo (BR), University of Oslo (NO), Institute for High Energy Physics (ES), Princeton University (US), University of Michigan (US), Lowell Observatory (US), Trieste Astronomical Observatory (IT), Mitchell Institute (US), SLAC National Accelerator Laboratory (US), Australian Astronomical Observatory (AU), University of Surrey (GB), University of Manchester (GB), CEA Grenoble (FR), University of Chicago (US), Valongo Observatory (BR), Institut d'Estudis Espacials de Catalunya (ES), Kavli Institute for Particle Astrophysics and Cosmology (US), Institute of Space Sciences (ES), Center for Astrophysics Harvard & Smithsonian (US), National Observatory (BR), Instituto de Astrofísica de Canarias (ES), Institut National de Physique Nucléaire et de Physique des Particules (FR), National Center for Supercomputing Applications (US), Cerro Tololo Inter-American Observatory (CL), Laboratoire de Physique Subatomique et de Cosmologie (FR), NSF NOIRLab (US), Laboratório Interinstitucional de e-Astronomia (BR), Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (ES), University of Southampton (GB), Institute of Science and Technology, University College London (GB), The Ohio State University (US), Swinburne University of Technology (AU), University of Portsmouth (GB), Universidad Autónoma de Madrid (ES), Indian Institute of Technology Hyderabad (IN), Carnegie Mellon University (US), University of Pennsylvania (US), Ludwig-Maximilians-Universität München (DE), Université Grenoble Alpes (FR), Texas A&M University (US), University of California, Berkeley (US), Stanford University (US), Macquarie University (AU)
National Science Foundation, U.S. Department of Energy, National Aeronautics and Space Administration, Albert Ellis Institute, University of Pennsylvania, Ohio State University, University of Chicago, Texas A and M University, University of Portsmouth, National Centre for Supercomputing Applications, Higher Education Funding Council for England, Space Telescope Science Institute, Centres de Recerca de Catalunya, University College London, European Commission, University of Nottingham, University of Sussex, University of Edinburgh, Deutsche Forschungsgemeinschaft, Generalitat de Catalunya, Eidgenössische Technische Hochschule Zürich, Ministério da Ciência, Tecnologia e Inovação, Conselho Nacional de Desenvolvimento Científico e Tecnológico, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Financiadora de Estudos e Projetos, Ministerio de Ciencia e Innovación, Institut de Física d'Altes Energies, University of Illinois at Urbana-Champaign, Office of Science, Science and Technology Facilities Council, Australian Research Council, European Regional Development Fund, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, Agencia Estatal de Investigación, High Energy Physics, Integrated Electronics Engineering Center, Binghamton University, Argonne National Laboratory, Fermilab, Lawrence Berkeley National Laboratory, SLAC National Accelerator Laboratory
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