Dark Energy Survey Year 1 Results: A Precise H<inf>0</inf> Estimate from DES Y1, BAO, and D/H Data

T. M.C. Abbott; F. B. Abdalla; J. Annis; K. Bechtol; J. Blazek; B. A. Benson; R. A. Bernstein; G. M. Bernstein; E. Bertin; D. Brooks; D. L. Burke; A. Carnero Rosell; M. Carrasco Kind; J. Carretero; F. J. Castander; C. L. Chang; T. M. Crawford; C. E. Cunha; C. B. D'Andrea; L. N. da Costa; C. Davis; J. DeRose; S. Desai; H. T. Diehl; J. P. Dietrich; P. Doel; A. Drlica-Wagner; A. E. Evrard; E. Fernandez; B. Flaugher; P. Fosalba; J. Frieman; J. García-Bellido; E. Gaztanaga; D. W. Gerdes; T. Giannantonio; D. Gruen; R. A. Gruendl; J. Gschwend; G. Gutierrez; W. G. Hartley; J. W. Henning; K. Honscheid; B. Hoyle; D. Huterer; B. Jain; D. J. James; M. Jarvis; T. Jeltema; M. D. Johnson; M. W.G. Johnson; E. Krause; K. Kuehn; S. Kuhlmann; N. Kuropatkin; O. Lahav; A. R. Liddle; M. Lima; H. Lin; N. MacCrann; M. A.G. Maia; A. Manzotti; M. March; J. L. Marshall; R. Miquel; J. J. Mohr; T. Natoli; P. Nugent; R. L.C. Ogando; Y. Park; A. A. Plazas; C. L. Reichardt; K. Reil; A. Roodman; A. J. Ross; E. Rozo; E. S. Rykoff; E. Sanchez; V. Scarpine; M. Schubnell; D. Scolnic; I. Sevilla-Noarbe; E. Sheldon; M. Smith; R. C. Smith; M. Soares-Santos; F. Sobreira; E. Suchyta; G. Tarle; D. Thomas; M. A. Troxel; A. R. Walker; R. H. Wechsler; J. Weller; W. Wester; W. L.K. Wu; J. Zuntz

doi:10.1093/MNRAS/STY1939

Dark Energy Survey Year 1 Results: A Precise H<inf>0</inf> Estimate from DES Y1, BAO, and D/H Data

T. M.C. Abbott, F. B. Abdalla, J. Annis, K. Bechtol, J. Blazek, B. A. Benson, R. A. Bernstein, G. M. Bernstein, E. Bertin, D. Brooks, D. L. Burke, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, F. J. Castander, C. L. Chang, T. M. Crawford, C. E. Cunha, C. B. D'Andrea, L. N. da CostaC. Davis, J. DeRose, S. Desai, H. T. Diehl, J. P. Dietrich, P. Doel, A. Drlica-Wagner, A. E. Evrard, E. Fernandez, B. Flaugher, P. Fosalba, J. Frieman, J. García-Bellido, E. Gaztanaga, D. W. Gerdes, T. Giannantonio, D. Gruen, R. A. Gruendl, J. Gschwend, G. Gutierrez, W. G. Hartley, J. W. Henning, K. Honscheid, B. Hoyle, D. Huterer, B. Jain, D. J. James, M. Jarvis, T. Jeltema, M. D. Johnson, M. W.G. Johnson, E. Krause, K. Kuehn, S. Kuhlmann, N. Kuropatkin, O. Lahav, A. R. Liddle, M. Lima, H. Lin, N. MacCrann, M. A.G. Maia, A. Manzotti, M. March, J. L. Marshall, R. Miquel, J. J. Mohr, T. Natoli, P. Nugent, R. L.C. Ogando, Y. Park, A. A. Plazas, C. L. Reichardt, K. Reil, A. Roodman, A. J. Ross, E. Rozo, E. S. Rykoff, E. Sanchez, V. Scarpine, M. Schubnell, D. Scolnic, I. Sevilla-Noarbe, E. Sheldon, M. Smith, R. C. Smith, M. Soares-Santos, F. Sobreira, E. Suchyta, G. Tarle, D. Thomas, M. A. Troxel, A. R. Walker, R. H. Wechsler, J. Weller, W. Wester, W. L.K. Wu, J. Zuntz

Department of Physics

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Abstract

© 2018 The Author(s). 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.

Original language	English
Pages (from-to)	3879-3888
Journal	Monthly Notices of the Royal Astronomical Society
Volume	480
Issue number	3
DOIs	https://doi.org/10.1093/MNRAS/STY1939
Publication status	Published - 1 Jan 2018

Keywords

Cosmological parameters
Cosmology: observations
Distance scale

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10.1093/MNRAS/STY1939

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Abbott, T. M. C., Abdalla, F. B., Annis, J., Bechtol, K., Blazek, J., Benson, B. A., Bernstein, R. A., Bernstein, G. M., Bertin, E., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Chang, C. L., Crawford, T. M., Cunha, C. E., D'Andrea, C. B., ... Zuntz, J. (2018). Dark Energy Survey Year 1 Results: A Precise H<inf>0</inf> Estimate from DES Y1, BAO, and D/H Data. Monthly Notices of the Royal Astronomical Society, 480(3), 3879-3888. https://doi.org/10.1093/MNRAS/STY1939

@article{5886a69d6a844cf78dc00c7b2e50d8fe,

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

abstract = "{\textcopyright} 2018 The Author(s). 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 = "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 Johnson, {M. D.} and Johnson, {M. W.G.} and E. Krause and K. Kuehn and S. Kuhlmann and N. Kuropatkin and O. Lahav and Liddle, {A. R.} and M. Lima and H. Lin and N. MacCrann and Maia, {M. A.G.} and A. Manzotti and M. March and Marshall, {J. L.} and R. Miquel and Mohr, {J. J.} and T. Natoli and P. Nugent and Ogando, {R. L.C.} and Y. Park and Plazas, {A. A.} and Reichardt, {C. L.} and K. Reil and A. Roodman and Ross, {A. J.} and E. Rozo and Rykoff, {E. S.} and E. Sanchez and V. Scarpine and M. Schubnell and D. Scolnic and I. Sevilla-Noarbe and E. Sheldon and M. Smith and Smith, {R. C.} and M. Soares-Santos and F. Sobreira and E. Suchyta and G. Tarle and D. Thomas and Troxel, {M. A.} and Walker, {A. R.} and Wechsler, {R. H.} and J. Weller and W. Wester and Wu, {W. L.K.} and J. Zuntz",

year = "2018",

month = jan,

day = "1",

doi = "10.1093/MNRAS/STY1939",

language = "English",

volume = "480",

pages = "3879--3888",

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

issn = "0035-8711",

number = "3",

}

Abbott, TMC, Abdalla, FB, Annis, J, Bechtol, K, Blazek, J, Benson, BA, Bernstein, RA, Bernstein, GM, Bertin, E, Brooks, D, Burke, DL, Carnero Rosell, A, Carrasco Kind, M, Carretero, J, Castander, FJ, Chang, CL, Crawford, TM, Cunha, CE, D'Andrea, CB, da Costa, LN, Davis, C, DeRose, J, Desai, S, Diehl, HT, Dietrich, JP, Doel, P, Drlica-Wagner, A, Evrard, AE, Fernandez, E, Flaugher, B, Fosalba, P, Frieman, J, García-Bellido, J, Gaztanaga, E, Gerdes, DW, Giannantonio, T, Gruen, D, Gruendl, RA, Gschwend, J, Gutierrez, G, Hartley, WG, Henning, JW, Honscheid, K, Hoyle, B, Huterer, D, Jain, B, James, DJ, Jarvis, M, Jeltema, T, Johnson, MD, Johnson, MWG, Krause, E, Kuehn, K, Kuhlmann, S, Kuropatkin, N, Lahav, O, Liddle, AR, Lima, M, Lin, H, MacCrann, N, Maia, MAG, Manzotti, A, March, M, Marshall, JL, Miquel, R, Mohr, JJ, Natoli, T, Nugent, P, Ogando, RLC, Park, Y, Plazas, AA, Reichardt, CL, Reil, K, Roodman, A, Ross, AJ, Rozo, E, Rykoff, ES, Sanchez, E, Scarpine, V, Schubnell, M, Scolnic, D, Sevilla-Noarbe, I, Sheldon, E, Smith, M, Smith, RC, Soares-Santos, M, Sobreira, F, Suchyta, E, Tarle, G, Thomas, D, Troxel, MA, Walker, AR, Wechsler, RH, Weller, J, Wester, W, Wu, WLK & Zuntz, J 2018, 'Dark Energy Survey Year 1 Results: A Precise H<inf>0</inf> Estimate from DES Y1, BAO, and D/H Data', Monthly Notices of the Royal Astronomical Society, vol. 480, no. 3, pp. 3879-3888. https://doi.org/10.1093/MNRAS/STY1939

TY - JOUR

T1 - Dark Energy Survey Year 1 Results: A Precise H0 Estimate from DES Y1, BAO, and D/H Data

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 - Johnson, M. D.

AU - Johnson, M. W.G.

AU - Krause, E.

AU - Kuehn, K.

AU - Kuhlmann, S.

AU - Kuropatkin, N.

AU - Lahav, O.

AU - Liddle, A. R.

AU - Lima, M.

AU - Lin, H.

AU - MacCrann, N.

AU - Maia, M. A.G.

AU - Manzotti, A.

AU - March, M.

AU - Marshall, J. L.

AU - Miquel, R.

AU - Mohr, J. J.

AU - Natoli, T.

AU - Nugent, P.

AU - Ogando, R. L.C.

AU - Park, Y.

AU - Plazas, A. A.

AU - Reichardt, C. L.

AU - Reil, K.

AU - Roodman, A.

AU - Ross, A. J.

AU - Rozo, E.

AU - Rykoff, E. S.

AU - Sanchez, E.

AU - Scarpine, V.

AU - Schubnell, M.

AU - Scolnic, D.

AU - Sevilla-Noarbe, I.

AU - Sheldon, E.

AU - Smith, M.

AU - Smith, R. C.

AU - Soares-Santos, M.

AU - Sobreira, F.

AU - Suchyta, E.

AU - Tarle, G.

AU - Thomas, D.

AU - Troxel, M. A.

AU - Walker, A. R.

AU - Wechsler, R. H.

AU - Weller, J.

AU - Wester, W.

AU - Wu, W. L.K.

AU - Zuntz, J.

PY - 2018/1/1

Y1 - 2018/1/1

N2 - © 2018 The Author(s). 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 - © 2018 The Author(s). 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

U2 - 10.1093/MNRAS/STY1939

DO - 10.1093/MNRAS/STY1939

M3 - Article

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 -

Dark Energy Survey Year 1 Results: A Precise H<inf>0</inf> Estimate from DES Y1, BAO, and D/H Data

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