Dark Energy Survey Year 1 results: Weak lensing mass calibration of redMaPPer galaxy clusters

DES Collaboration

doi:10.1093/mnras/sty2711

Dark Energy Survey Year 1 results: Weak lensing mass calibration of redMaPPer galaxy clusters

DES Collaboration

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Abstract

We constrain the mass-richness scaling relation of redMaPPer galaxy clusters identified in the Dark Energy Survey Year 1 data using weak gravitational lensing.We split clusters into 4 × 3 bins of richness λ and redshift z for λ ≥ 20 and 0.2 ≤ z ≤ 0.65 and measure the mean masses of these bins using their stacked weak lensing signal. By modelling the scaling relation as 〈M_200m|λ, z〉=M₀(λ/40)^F((1+z)/1.35)^G,we constrain the normalization of the scaling relation at the 5.0 per cent level, finding M₀ = [3.081 ± 0.075(stat) ± 0.133(sys)] · 10¹⁴M_⊙ at λ = 40 and z = 0.35. The recovered richness scaling index is F = 1.356 ± 0.051 (stat) ± 0.008 (sys) and the redshift scaling index G = -0.30 ± 0.30 (stat) ± 0.06 (sys). These are the tightest measurements of the normalization and richness scaling index made to date from a weak lensing experiment. We use a semi-analytic covariance matrix to characterize the statistical errors in the recovered weak lensing profiles. Our analysis accounts for the following sources of systematic error: shear and photometric redshift errors, cluster miscentring, cluster member dilution of the source sample, systematic uncertainties in the modelling of the halo-mass correlation function, halo triaxiality, and projection effects.We discuss prospects for reducing our systematic error budget, which dominates the uncertainty on M₀. Our result is in excellent agreement with, but has significantly smaller uncertainties than, previous measurements in the literature, and augurs well for the power of the DES cluster survey as a tool for precision cosmology and upcoming galaxy surveys such as LSST, Euclid, and WFIRST.

Original language	English
Pages (from-to)	1352-1378
Number of pages	27
Journal	Monthly Notices of the Royal Astronomical Society
Volume	482
Issue number	1
DOIs	https://doi.org/10.1093/mnras/sty2711
State	Published - Jan 1 2019

Funding

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 (CAAS-TRO), through project number CE110001020, and the Brazilian In-stituto Nacional de Ciência e Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2). This paper has gone through internal review by the DES collaboration. TM and ER are supported by DOE grant DE-SC0015975. TNV and SS are supported by the SFB-Transregio 33 ‘The Dark Universe’ by the Deutsche Forschungsgemeinschaft (DFG) and the DFG cluster of excellence ‘Origin and Structure of the Universe’. ER ac- knowledges additional support by the Sloan Foundation, grant FG-2016-6443. Support for DG was provided by NASA through Einstein Postdoctoral Fellowship grant number PF5-160138 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. TJ, DH, and SE are supported by DOE grant DE-SC0010107. KR and SB acknowledge support from the UK Science and Technology Facilities Council via Research Training Grants ST/P000252/1 and ST/N504452/1, respectively. CV is supported by the Mexican National Council for Science and Technology via grant number 411117. AvdL is supported by DoE grant DE-SC0018053. This paper has gone through internal review by the DES collaboration. TMand ER are supported by DOE grant DE-SC0015975.TNV and SS are supported by the SFB-Transregio 33 'TheDarkUniverse' by the Deutsche Forschungsgemeinschaft (DFG) and the DFG cluster of excellence 'Origin and Structure of the Universe'. ER acknowledges additional support by the Sloan Foundation, grant FG-2016-6443. Support for DG was provided by NASA through Einstein Postdoctoral Fellowship grant number PF5-160138 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. TJ, DH, and SE are supported by DOE grant DE-SC0010107. KR and SB acknowledge support from the UK Science and Technology Facilities Council via Research Training Grants ST/P000252/1 and ST/N504452/1, respectively. CV is supported by the Mexican National Council for Science and Technology via grant number 411117. AvdL is supported by DoE grant DE-SC0018053. Part of our computations have been carried out on the computing facilities of the Computational Center for Particle and Astrophysics (C2PAP).Aportion of this researchwas carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, theMinistry of Science and Education of Spain, the Science and Technology FacilitiesCouncil of theUnitedKingdom, theHigher Education Funding Council for England, theNationalCenter 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 and 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 Dark Energy Survey. 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) includingERCgrant 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, and the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2). 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. This work used simulations and computations performed using computational resources at SLAC and at NERSC. 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 and 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 Desen-volvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovac¸ão, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. 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
Australian Research Council Centre of Excellence for All-sky Astrophysics
CAAS-TRO	CE110001020
Collaborating Institutions in the Dark Energy Survey
Conselho Nacional de Desen-volvimento Científico e Tecnológico
European Union’s Seventh Framework Program
FP7/2007
Fermi Research Alliance, LLC	DE-AC02-07CH11359
INCT
Kavli Institute of Cosmological Physics at the University of Chicago
Mexican National Council for Science and Technology	411117, DE-SC0018053
Ministry of Science and Education of Spain
Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University
National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign
U.S. National Science Foundation
National Science Foundation	AST-1138766, AST-1536171
U.S. Department of Energy	DE-SC0010107, DE-SC0015975
National Aeronautics and Space Administration	PF5-160138, NAS8-03060
Alfred P. Sloan Foundation	FG-2016-6443
Office of Science
High Energy Physics
University of Chicago
University of Illinois
Seventh Framework Programme	681431, 240672, 306478, 291329
Higher Education Funding Council for England
Center for Cosmology and Astroparticle Physics, Ohio State University
Instituto Nacional de Ciência e Tecnologia Midas
Engineering Research Centers
Science and Technology Facilities Council	ST/P000252/1, ST/N504452/1
University College London
European Commission
European Research Council
University of Edinburgh
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
Conselho Nacional de Desenvolvimento Científico e Tecnológico	465376/2014-2
Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro
Financiadora de Estudos e Projetos
Ministério da Ciência e Tecnologia
European Regional Development Fund
National Science Foundation

Keywords

Cosmology: observations
Galaxies: clusters: general
Gravitational lensing: weak

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10.1093/mnras/sty2711

Cite this

@article{15fa106efb7f455e812ffd8239bcff08,

title = "Dark Energy Survey Year 1 results: Weak lensing mass calibration of redMaPPer galaxy clusters",

abstract = "We constrain the mass-richness scaling relation of redMaPPer galaxy clusters identified in the Dark Energy Survey Year 1 data using weak gravitational lensing.We split clusters into 4 × 3 bins of richness λ and redshift z for λ ≥ 20 and 0.2 ≤ z ≤ 0.65 and measure the mean masses of these bins using their stacked weak lensing signal. By modelling the scaling relation as 〈M200m|λ, z〉=M0(λ/40)F((1+z)/1.35)G,we constrain the normalization of the scaling relation at the 5.0 per cent level, finding M0 = [3.081 ± 0.075(stat) ± 0.133(sys)] · 1014M⊙ at λ = 40 and z = 0.35. The recovered richness scaling index is F = 1.356 ± 0.051 (stat) ± 0.008 (sys) and the redshift scaling index G = -0.30 ± 0.30 (stat) ± 0.06 (sys). These are the tightest measurements of the normalization and richness scaling index made to date from a weak lensing experiment. We use a semi-analytic covariance matrix to characterize the statistical errors in the recovered weak lensing profiles. Our analysis accounts for the following sources of systematic error: shear and photometric redshift errors, cluster miscentring, cluster member dilution of the source sample, systematic uncertainties in the modelling of the halo-mass correlation function, halo triaxiality, and projection effects.We discuss prospects for reducing our systematic error budget, which dominates the uncertainty on M0. Our result is in excellent agreement with, but has significantly smaller uncertainties than, previous measurements in the literature, and augurs well for the power of the DES cluster survey as a tool for precision cosmology and upcoming galaxy surveys such as LSST, Euclid, and WFIRST.",

keywords = "Cosmology: observations, Galaxies: clusters: general, Gravitational lensing: weak",

author = "{DES Collaboration} and T. McClintock and Varga, {T. N.} and D. Gruen and E. Rozo and Rykoff, {E. S.} and T. Shin and P. Melchior and J. DeRose and S. Seitz and Dietrich, {J. P.} and E. Sheldon and Y. Zhang and {von der Linden}, A. and T. Jeltema and Mantz, {A. B.} and Romer, {A. K.} and S. Allen and Becker, {M. R.} and A. Bermeo and S. Bhargava and M. Costanzi and S. Everett and A. Farahi and N. Hamaus and Hartley, {W. G.} and Hollowood, {D. L.} and B. Hoyle and H. Israel and P. Li and N. MacCrann and G. Morris and A. Palmese and Plazas, {A. A.} and G. Pollina and Rau, {M. M.} and M. Simet and M. Soares-Santos and Troxel, {M. A.} and {Vergara Cervantes}, C. and Wechsler, {R. H.} and J. Zuntz and Abbott, {T. M.C.} and Abdalla, {F. B.} and S. Allam and J. Annis and S. Avila and Bridle, {S. L.} and D. Brooks and Burke, {D. L.} and E. Suchyta",

note = "Publisher Copyright: {\textcopyright} 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society.",

year = "2019",

month = jan,

day = "1",

doi = "10.1093/mnras/sty2711",

language = "English",

volume = "482",

pages = "1352--1378",

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

issn = "0035-8711",

publisher = "Oxford University Press",

number = "1",

}

TY - JOUR

T1 - Dark Energy Survey Year 1 results

T2 - Weak lensing mass calibration of redMaPPer galaxy clusters

AU - DES Collaboration

AU - McClintock, T.

AU - Varga, T. N.

AU - Gruen, D.

AU - Rozo, E.

AU - Rykoff, E. S.

AU - Shin, T.

AU - Melchior, P.

AU - DeRose, J.

AU - Seitz, S.

AU - Dietrich, J. P.

AU - Sheldon, E.

AU - Zhang, Y.

AU - von der Linden, A.

AU - Jeltema, T.

AU - Mantz, A. B.

AU - Romer, A. K.

AU - Allen, S.

AU - Becker, M. R.

AU - Bermeo, A.

AU - Bhargava, S.

AU - Costanzi, M.

AU - Everett, S.

AU - Farahi, A.

AU - Hamaus, N.

AU - Hartley, W. G.

AU - Hollowood, D. L.

AU - Hoyle, B.

AU - Israel, H.

AU - Li, P.

AU - MacCrann, N.

AU - Morris, G.

AU - Palmese, A.

AU - Plazas, A. A.

AU - Pollina, G.

AU - Rau, M. M.

AU - Simet, M.

AU - Soares-Santos, M.

AU - Troxel, M. A.

AU - Vergara Cervantes, C.

AU - Wechsler, R. H.

AU - Zuntz, J.

AU - Abbott, T. M.C.

AU - Abdalla, F. B.

AU - Allam, S.

AU - Annis, J.

AU - Avila, S.

AU - Bridle, S. L.

AU - Brooks, D.

AU - Burke, D. L.

AU - Suchyta, E.

PY - 2019/1/1

Y1 - 2019/1/1

N2 - We constrain the mass-richness scaling relation of redMaPPer galaxy clusters identified in the Dark Energy Survey Year 1 data using weak gravitational lensing.We split clusters into 4 × 3 bins of richness λ and redshift z for λ ≥ 20 and 0.2 ≤ z ≤ 0.65 and measure the mean masses of these bins using their stacked weak lensing signal. By modelling the scaling relation as 〈M200m|λ, z〉=M0(λ/40)F((1+z)/1.35)G,we constrain the normalization of the scaling relation at the 5.0 per cent level, finding M0 = [3.081 ± 0.075(stat) ± 0.133(sys)] · 1014M⊙ at λ = 40 and z = 0.35. The recovered richness scaling index is F = 1.356 ± 0.051 (stat) ± 0.008 (sys) and the redshift scaling index G = -0.30 ± 0.30 (stat) ± 0.06 (sys). These are the tightest measurements of the normalization and richness scaling index made to date from a weak lensing experiment. We use a semi-analytic covariance matrix to characterize the statistical errors in the recovered weak lensing profiles. Our analysis accounts for the following sources of systematic error: shear and photometric redshift errors, cluster miscentring, cluster member dilution of the source sample, systematic uncertainties in the modelling of the halo-mass correlation function, halo triaxiality, and projection effects.We discuss prospects for reducing our systematic error budget, which dominates the uncertainty on M0. Our result is in excellent agreement with, but has significantly smaller uncertainties than, previous measurements in the literature, and augurs well for the power of the DES cluster survey as a tool for precision cosmology and upcoming galaxy surveys such as LSST, Euclid, and WFIRST.

AB - We constrain the mass-richness scaling relation of redMaPPer galaxy clusters identified in the Dark Energy Survey Year 1 data using weak gravitational lensing.We split clusters into 4 × 3 bins of richness λ and redshift z for λ ≥ 20 and 0.2 ≤ z ≤ 0.65 and measure the mean masses of these bins using their stacked weak lensing signal. By modelling the scaling relation as 〈M200m|λ, z〉=M0(λ/40)F((1+z)/1.35)G,we constrain the normalization of the scaling relation at the 5.0 per cent level, finding M0 = [3.081 ± 0.075(stat) ± 0.133(sys)] · 1014M⊙ at λ = 40 and z = 0.35. The recovered richness scaling index is F = 1.356 ± 0.051 (stat) ± 0.008 (sys) and the redshift scaling index G = -0.30 ± 0.30 (stat) ± 0.06 (sys). These are the tightest measurements of the normalization and richness scaling index made to date from a weak lensing experiment. We use a semi-analytic covariance matrix to characterize the statistical errors in the recovered weak lensing profiles. Our analysis accounts for the following sources of systematic error: shear and photometric redshift errors, cluster miscentring, cluster member dilution of the source sample, systematic uncertainties in the modelling of the halo-mass correlation function, halo triaxiality, and projection effects.We discuss prospects for reducing our systematic error budget, which dominates the uncertainty on M0. Our result is in excellent agreement with, but has significantly smaller uncertainties than, previous measurements in the literature, and augurs well for the power of the DES cluster survey as a tool for precision cosmology and upcoming galaxy surveys such as LSST, Euclid, and WFIRST.

KW - Cosmology: observations

KW - Galaxies: clusters: general

KW - Gravitational lensing: weak

UR - http://www.scopus.com/inward/record.url?scp=85057185904&partnerID=8YFLogxK

U2 - 10.1093/mnras/sty2711

DO - 10.1093/mnras/sty2711

M3 - Article

AN - SCOPUS:85057185904

SN - 0035-8711

VL - 482

SP - 1352

EP - 1378

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 1

ER -

Dark Energy Survey Year 1 results: Weak lensing mass calibration of redMaPPer galaxy clusters

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