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

DES Collaboration, T. McClintock, T. N. Varga, D. Gruen, Eduardo Rozo, E. S. Rykoff, T. Shin, P. Melchior, J. DeRose, S. Seitz, J. P. Dietrich, E. Sheldon, Y. Zhang, A. von der Linden, T. Jeltema, A. B. Mantz, A. K. Romer, S. Allen, M. R. Becker, A. Bermeo & 31 others S. Bhargava, M. Costanzi, S. Everett, A. Farahi, N. Hamaus, W. G. Hartley, D. L. Hollowood, B. Hoyle, H. Israel, P. Li, N. MacCrann, G. Morris, A. Palmese, A. A. Plazas, G. Pollina, M. M. Rau, M. Simet, M. Soares-Santos, M. A. Troxel, C. Vergara Cervantes, R. H. Wechsler, J. Zuntz, T. M.C. Abbott, F. B. Abdalla, S. Allam, J. Annis, S. Avila, S. L. Bridle, D. Brooks, D. L. Burke, A. Carnero Rosell

Research output: Contribution to journalArticle

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.

LanguageEnglish (US)
Pages1352-1378
Number of pages27
JournalMonthly Notices of the Royal Astronomical Society
Volume482
Issue number1
DOIs
StatePublished - Jan 1 2019

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dark energy
galaxies
calibration
scaling
energy
cosmology
systematic errors
modeling
halos
dilution
triaxial stresses
matrix
budgets
index
experiment
projection
shear
normalisation
profiles

Keywords

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

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Dark Energy Survey Year 1 results : Weak lensing mass calibration of redMaPPer galaxy clusters. / DES Collaboration.

In: Monthly Notices of the Royal Astronomical Society, Vol. 482, No. 1, 01.01.2019, p. 1352-1378.

Research output: Contribution to journalArticle

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T1 - Dark Energy Survey Year 1 results

T2 - Monthly Notices of the Royal Astronomical Society

AU - DES Collaboration

AU - McClintock, T.

AU - Varga, T. N.

AU - Gruen, D.

AU - Rozo, Eduardo

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 - Carnero Rosell, A.

PY - 2019/1/1

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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

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