Dark Energy Survey Year 1 Results: A Precise H0 Estimate from DES Y1, BAO, and D/H Data

The Dark Energy Survey and the South Pole Telescope Collaborations

doi:10.1093/MNRAS/STY1939

Dark Energy Survey Year 1 Results: A Precise H₀ Estimate from DES Y1, BAO, and D/H Data

The Dark Energy Survey and the South Pole Telescope Collaborations

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Abstract

We combine Dark Energy Survey Year 1 clustering and weak lensing data with baryon acoustic oscillations and Big Bang nucleosynthesis experiments to constrain the Hubble constant. Assuming a flat ΛCDM model with minimal neutrino mass (Σm_υ = 0.06 eV), we find H₀ = 67.4 _-1.2 ^+1.1 km s^-1 Mpc^-1 (68 per cent CL). This result is completely independent of Hubble constant measurements based on the distance ladder, cosmic microwave background anisotropies (both temperature and polarization), and strong lensing constraints. There are now five data sets that: (a) have no shared observational systematics; and (b) each constrains the Hubble constant with fractional uncertainty at the few-per cent level. We compare these five independent estimates, and find that, as a set, the differences between them are significant at the 2.5σ level (χ²/dof = 24/11, probability to exceed = 1.1 per cent). Having set the threshold for consistency at 3σ, we combine all five data sets to arrive at H₀ = 69.3_-0.6 ^+0.4 km s^-1 Mpc^-1.

Original language	English
Pages (from-to)	3879-3888
Number of pages	10
Journal	Monthly Notices of the Royal Astronomical Society
Volume	480
Issue number	3
DOIs	https://doi.org/10.1093/MNRAS/STY1939
State	Published - 2018

Funding

are partially supported by MINECO under grants AYA2015-71825, ESP2015-66861, FPA2015-68048, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020. The South Pole Telescope program is supported by the National Science Foundation through grant PLR-1248097. Partial support is also provided by the NSF Physics Frontier Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation, and the Gordon and Betty Moore Foundation through Grant GBMF#947 to the University of Chicago. This paper has gone through internal review by the DES collaboration. ER is supported by DOE grant DE-SC0015975 and by the Sloan Foundation, grant FG-2016-6443. YP is supported by DOE grant DE-SC0015975. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology an d Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University,Financiadora de Estudos e Projetos, Fundac¸ão Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovac¸ão, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the DES. The DES data management system is supported by the National Science Foundation under Grant Numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions This paper has gone through internal review by the DES collaboration. ER is supported by DOE grant DE-SC0015975 and by the Sloan Foundation, grant FG-2016-6443. YP is supported by DOE grant DE-SC0015975. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology an d Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the DES. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciències de l'Espai (IEEC/CSIC), the Institut de Física d'Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universit ät München and the associated Excellence Cluster Universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, TexasA&MUniversity, and the OzDESMembership Consortium. Based in part on observations at Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under Grant Numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015-71825, ESP2015-66861, FPA2015-68048, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020. The South Pole Telescope program is supported by the National Science Foundation through grant PLR-1248097. Partial support is also provided by the NSF Physics Frontier Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation, and the Gordon and Betty Moore Foundation through Grant GBMF#947 to the University of Chicago. This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics. TheUnited StatesGovernment retains and the publisher, by accepting the article for publication, acknowledges that the United States Government retains a non-exclusive, paid-up, irrevocable, world-wide license to publish or reproduce the published form of this manuscript, or allow others to do so, for United States Government purposes. Based in part on observations at Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics. The United States Government retains and the publisher, by accepting the article for publication, acknowledges that the United States Government retains a non-exclusive, paid-up, irrevocable, world-wide license to publish or reproduce the published form of this manuscript, or allow others to do so, for United States Government purposes.

Funders	Funder number
Center for Cosmology an d Astro-Particle Physics at the Ohio State University
Fermi Research Alliance, LLC	DE-AC02-07CH11359
Ministério da Ciência
Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University
NSF Physics Frontier Center	PHY-0114422
National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign
Science and Technology Facilities Council of the United Kingdom
National Science Foundation	PLR-1248097, AST-1138766, AST-1536171
National Science Foundation
U.S. Department of Energy	DE-SC0015975
U.S. Department of Energy
Alfred P. Sloan Foundation	FG-2016-6443
Alfred P. Sloan Foundation
Gordon and Betty Moore Foundation	GBMF#947
Gordon and Betty Moore Foundation
Kavli Foundation
University of Illinois at Urbana-Champaign
Stanford University
Office of Science
High Energy Physics
University of Pennsylvania
Ohio State University
University of Chicago
Texas A and M University
University of Portsmouth
Seventh Framework Programme	240672, 306478, 291329
Seventh Framework Programme
Higher Education Funding Council for England
Science and Technology Facilities Council
University of Cambridge
University College London
European Commission
European Research Council
University of Nottingham
University of Sussex
Australian Research Council	CE110001020
Australian Research Council
Deutsche Forschungsgemeinschaft
Generalitat de Catalunya
Ministerio de Economía y Competitividad	SEV-2016-0588, SEV-2016-0597, ESP2015-66861, MDM-2015-0509, FPA2015-68048, AYA2015-71825
Ministerio de Economía y Competitividad
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
Ministry of Education and Science of Ukraine
European Regional Development Fund
National Science Foundation

Keywords

Cosmological parameters
Cosmology: observations
Distance scale

Access to Document

10.1093/MNRAS/STY1939

Cite this

@article{cf40aa7d0fb449f19539a8fe1cd9dbd3,

title = "Dark Energy Survey Year 1 Results: A Precise H0 Estimate from DES Y1, BAO, and D/H Data",

abstract = "We combine Dark Energy Survey Year 1 clustering and weak lensing data with baryon acoustic oscillations and Big Bang nucleosynthesis experiments to constrain the Hubble constant. Assuming a flat ΛCDM model with minimal neutrino mass (Σmυ = 0.06 eV), we find H0 = 67.4 -1.2 +1.1 km s-1 Mpc-1 (68 per cent CL). This result is completely independent of Hubble constant measurements based on the distance ladder, cosmic microwave background anisotropies (both temperature and polarization), and strong lensing constraints. There are now five data sets that: (a) have no shared observational systematics; and (b) each constrains the Hubble constant with fractional uncertainty at the few-per cent level. We compare these five independent estimates, and find that, as a set, the differences between them are significant at the 2.5σ level (χ2/dof = 24/11, probability to exceed = 1.1 per cent). Having set the threshold for consistency at 3σ, we combine all five data sets to arrive at H0 = 69.3-0.6 +0.4 km s-1 Mpc-1.",

keywords = "Cosmological parameters, Cosmology: observations, Distance scale",

author = "{The Dark Energy Survey and the South Pole Telescope Collaborations} and Abbott, {T. M.C.} and Abdalla, {F. B.} and J. Annis and K. Bechtol and J. Blazek and Benson, {B. A.} and Bernstein, {R. A.} and Bernstein, {G. M.} and E. Bertin and D. Brooks and Burke, {D. L.} and {Carnero Rosell}, A. and {Carrasco Kind}, M. and J. Carretero and Castander, {F. J.} and Chang, {C. L.} and Crawford, {T. M.} and Cunha, {C. E.} and D'Andrea, {C. B.} and {da Costa}, {L. N.} and C. Davis and J. DeRose and S. Desai and Diehl, {H. T.} and Dietrich, {J. P.} and P. Doel and A. Drlica-Wagner and Evrard, {A. E.} and E. Fernandez and B. Flaugher and P. Fosalba and J. Frieman and J. Garc{\'i}a-Bellido and E. Gaztanaga and Gerdes, {D. W.} and T. Giannantonio and D. Gruen and Gruendl, {R. A.} and J. Gschwend and G. Gutierrez and Hartley, {W. G.} and Henning, {J. W.} and K. Honscheid and B. Hoyle and D. Huterer and B. Jain and James, {D. J.} and M. Jarvis and T. Jeltema and E. Suchyta",

note = "Publisher Copyright: {\textcopyright} 2018 The Author(s).",

year = "2018",

doi = "10.1093/MNRAS/STY1939",

language = "English",

volume = "480",

pages = "3879--3888",

journal = "Monthly Notices of the Royal Astronomical Society",

issn = "0035-8711",

publisher = "Oxford University Press",

number = "3",

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TY - JOUR

T1 - Dark Energy Survey Year 1 Results

T2 - A Precise H0 Estimate from DES Y1, BAO, and D/H Data

AU - The Dark Energy Survey and the South Pole Telescope Collaborations

AU - Abbott, T. M.C.

AU - Abdalla, F. B.

AU - Annis, J.

AU - Bechtol, K.

AU - Blazek, J.

AU - Benson, B. A.

AU - Bernstein, R. A.

AU - Bernstein, G. M.

AU - Bertin, E.

AU - Brooks, D.

AU - Burke, D. L.

AU - Carnero Rosell, A.

AU - Carrasco Kind, M.

AU - Carretero, J.

AU - Castander, F. J.

AU - Chang, C. L.

AU - Crawford, T. M.

AU - Cunha, C. E.

AU - D'Andrea, C. B.

AU - da Costa, L. N.

AU - Davis, C.

AU - DeRose, J.

AU - Desai, S.

AU - Diehl, H. T.

AU - Dietrich, J. P.

AU - Doel, P.

AU - Drlica-Wagner, A.

AU - Evrard, A. E.

AU - Fernandez, E.

AU - Flaugher, B.

AU - Fosalba, P.

AU - Frieman, J.

AU - García-Bellido, J.

AU - Gaztanaga, E.

AU - Gerdes, D. W.

AU - Giannantonio, T.

AU - Gruen, D.

AU - Gruendl, R. A.

AU - Gschwend, J.

AU - Gutierrez, G.

AU - Hartley, W. G.

AU - Henning, J. W.

AU - Honscheid, K.

AU - Hoyle, B.

AU - Huterer, D.

AU - Jain, B.

AU - James, D. J.

AU - Jarvis, M.

AU - Jeltema, T.

AU - Suchyta, E.

PY - 2018

Y1 - 2018

N2 - We combine Dark Energy Survey Year 1 clustering and weak lensing data with baryon acoustic oscillations and Big Bang nucleosynthesis experiments to constrain the Hubble constant. Assuming a flat ΛCDM model with minimal neutrino mass (Σmυ = 0.06 eV), we find H0 = 67.4 -1.2 +1.1 km s-1 Mpc-1 (68 per cent CL). This result is completely independent of Hubble constant measurements based on the distance ladder, cosmic microwave background anisotropies (both temperature and polarization), and strong lensing constraints. There are now five data sets that: (a) have no shared observational systematics; and (b) each constrains the Hubble constant with fractional uncertainty at the few-per cent level. We compare these five independent estimates, and find that, as a set, the differences between them are significant at the 2.5σ level (χ2/dof = 24/11, probability to exceed = 1.1 per cent). Having set the threshold for consistency at 3σ, we combine all five data sets to arrive at H0 = 69.3-0.6 +0.4 km s-1 Mpc-1.

AB - We combine Dark Energy Survey Year 1 clustering and weak lensing data with baryon acoustic oscillations and Big Bang nucleosynthesis experiments to constrain the Hubble constant. Assuming a flat ΛCDM model with minimal neutrino mass (Σmυ = 0.06 eV), we find H0 = 67.4 -1.2 +1.1 km s-1 Mpc-1 (68 per cent CL). This result is completely independent of Hubble constant measurements based on the distance ladder, cosmic microwave background anisotropies (both temperature and polarization), and strong lensing constraints. There are now five data sets that: (a) have no shared observational systematics; and (b) each constrains the Hubble constant with fractional uncertainty at the few-per cent level. We compare these five independent estimates, and find that, as a set, the differences between them are significant at the 2.5σ level (χ2/dof = 24/11, probability to exceed = 1.1 per cent). Having set the threshold for consistency at 3σ, we combine all five data sets to arrive at H0 = 69.3-0.6 +0.4 km s-1 Mpc-1.

KW - Cosmological parameters

KW - Cosmology: observations

KW - Distance scale

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U2 - 10.1093/MNRAS/STY1939

DO - 10.1093/MNRAS/STY1939

M3 - Article

AN - SCOPUS:85055268179

SN - 0035-8711

VL - 480

SP - 3879

EP - 3888

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 3

ER -