The Dark Energy Survey Supernova Program: slow supernovae show cosmological time dilation out to <i>z</i> ~ 1.

ABSTRACT We present a precise measurement of cosmological time dilation using the light curves of 1504 Type Ia supernovae from the Dark Energy Survey spanning a redshift range $0.1\lesssim z\lesssim 1.2$. We find that the width of supernova light curves is proportional to $(1+z)$, as expected for time dilation due to the expansion of the Universe. Assuming Type Ia supernovae light curves are emitted with a consistent duration $\Delta t_{\rm em}$, and parametrizing the observed duration as $\Delta t_{\rm obs}=\Delta t_{\rm em}(1+z)^b$, we fit for the form of time dilation using two methods. First, we find that a power of $b \approx 1$ minimizes the flux scatter in stacked subsamples of light curves across different redshifts. Secondly, we fit each target supernova to a stacked light curve (stacking all supernovae with observed bandpasses matching that of the target light curve) and find $b=1.003\pm 0.005$ (stat) $\pm \, 0.010$ (sys). Thanks to the large number of supernovae and large redshift-range of the sample, this analysis gives the most precise measurement of cosmological time dilation to date, ruling out any non-time-dilating cosmological models at very high significance.

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Publication Details

Journal
Monthly Notices of the Royal Astronomical Society
Published
2024-08-21
DOI
https://doi.org/10.1093/mnras/stae2008
Citations
10
Primary Topic
Gamma-ray bursts and supernovae
Type
article
Field-Weighted Citation Impact
3.32

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article

The Dark Energy Survey Supernova Program: slow supernovae show cosmological time dilation out to z ~ 1.

A. Pieres, B. Sánchez, I. Ferrero, S. R. Hinton et al.
10 citations
Monthly Notices of the Royal Astronomical Society
Gamma-ray bursts and supernovae
3.32
article

The Dark Energy Survey Supernova Program: slow supernovae show cosmological time dilation out to z ~ 1.

A. Pieres, B. Sánchez, I. Ferrero, S. R. Hinton, J. Myles, A. Möller, L. Galbany, J. Carretero, J. García-Bellido, S. Bocquet, D. Scolnic, S. Allam, J. L. Marshall, L. N. da Costa, M. R. Smith, G. Giannini, R. Keßler, J. Frieman, Karl Glazebrook, Gregory Tarlé, E. Suchyta, A. Palmese, Brad E. Tucker, P. Wiseman, A. R. Walker, P Shah, D. J. James, T. M. C. Abbott, J. Asorey, D. Sanchez Cid, D. Carollo, Eusebio Sanchez, Dillon Brout, J. Mena-Fernández, Geraint F. Lewis, A. Carnero Rosell, J. De Vicente, ENRIQUE GAZTAÑAGA, K. Honscheid, K. Kuehn, David Bacon, M. Vincenzi, T. M. Davis, R. L. C. Ogando, M. Lima, R. Miquel, M. E. S. Pereira, Christopher E. Lidman, David H. Brooks, H. T. Diehl, S. Desai, F. Andrade-Oliveira, M. Aguena, S Lee, E. Buckley‐Geer, M. Sullivan, R. C. Nichol, Ryan M. T. White, A A Plazas Malagón, N. Weaverdyck, R A Gruendl, O. Lahav, M. Schubnell, D. L. Burke, A. K. Romer, M. Sako, S Everett, J Lee, B Flaugher
article en
10 citations

Abstract

ABSTRACT We present a precise measurement of cosmological time dilation using the light curves of 1504 Type Ia supernovae from the Dark Energy Survey spanning a redshift range $0.1\lesssim z\lesssim 1.2$. We find that the width of supernova light curves is proportional to $(1+z)$, as expected for time dilation due to the expansion of the Universe. Assuming Type Ia supernovae light curves are emitted with a consistent duration $\Delta t_{\rm em}$, and parametrizing the observed duration as $\Delta t_{\rm obs}=\Delta t_{\rm em}(1+z)^b$, we fit for the form of time dilation using two methods. First, we find that a power of $b \approx 1$ minimizes the flux scatter in stacked subsamples of light curves across different redshifts. Secondly, we fit each target supernova to a stacked light curve (stacking all supernovae with observed bandpasses matching that of the target light curve) and find $b=1.003\pm 0.005$ (stat) $\pm \, 0.010$ (sys). Thanks to the large number of supernovae and large redshift-range of the sample, this analysis gives the most precise measurement of cosmological time dilation to date, ruling out any non-time-dilating cosmological models at very high significance.

Monthly Notices of the Royal Astronomical SocietyVol. 533(3)
Australian National University (AU), Institució Catalana de Recerca i Estudis Avançats (ES), Universidad Complutense de Madrid (ES), Oak Ridge National Laboratory (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), 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), Applied Materials (United States) (US), 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 Chicago (US), Valongo Observatory (BR), Institut d'Estudis Espacials de Catalunya (ES), Kavli Institute for Particle Astrophysics and Cosmology (US), 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), Atmospheric and Space Technology Research Associates (United States) (US), Laboratório Interinstitucional de e-Astronomia (BR), Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (ES), University of Southampton (GB), 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), Universidade Estadual Paulista (Unesp) (BR), 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, University of Pennsylvania, Ohio State University, University of Chicago, University of Portsmouth, National Centre for Supercomputing Applications, Higher Education Funding Council for England, Centres de Recerca de Catalunya, Australian Government, University College London, European Commission, University of Sussex, Deutsche Forschungsgemeinschaft, Generalitat de Catalunya, 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, Center for Cosmology and Astroparticle Physics, Ohio State University, Science and Technology Facilities Council, Australian Research Council, European Regional Development Fund, High Energy Physics, Integrated Electronics Engineering Center, Binghamton University, Argonne National Laboratory, Fermilab, Lawrence Berkeley National Laboratory, H2020 European Research Council, SLAC National Accelerator Laboratory
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Gamma-ray bursts and supernovae
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