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Weak-lensing analysis of SPT-selected galaxy clusters using Dark Energy Survey Science Verification data

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Weak-lensing analysis of SPT-selected galaxy clusters using Dark Energy Survey Science Verification data. / DES Collaboration; SPT Collaborations; Avila, S.; D'Andrea, C. B.

In: Monthly Notices of the Royal Astronomical Society, Vol. 485, No. 1, 01.05.2019, p. 69-87.

Research output: Contribution to journalArticle

Harvard

DES Collaboration, SPT Collaborations, Avila, S & D'Andrea, CB 2019, 'Weak-lensing analysis of SPT-selected galaxy clusters using Dark Energy Survey Science Verification data', Monthly Notices of the Royal Astronomical Society, vol. 485, no. 1, pp. 69-87. https://doi.org/10.1093/mnras/stz234

APA

DES Collaboration, SPT Collaborations, Avila, S., & D'Andrea, C. B. (2019). Weak-lensing analysis of SPT-selected galaxy clusters using Dark Energy Survey Science Verification data. Monthly Notices of the Royal Astronomical Society, 485(1), 69-87. https://doi.org/10.1093/mnras/stz234

Vancouver

DES Collaboration, SPT Collaborations, Avila S, D'Andrea CB. Weak-lensing analysis of SPT-selected galaxy clusters using Dark Energy Survey Science Verification data. Monthly Notices of the Royal Astronomical Society. 2019 May 1;485(1):69-87. https://doi.org/10.1093/mnras/stz234

Author

DES Collaboration ; SPT Collaborations ; Avila, S. ; D'Andrea, C. B. / Weak-lensing analysis of SPT-selected galaxy clusters using Dark Energy Survey Science Verification data. In: Monthly Notices of the Royal Astronomical Society. 2019 ; Vol. 485, No. 1. pp. 69-87.

Bibtex

@article{cafa00e5ca014dbdb2ff5d4efcfeb2bd,
title = "Weak-lensing analysis of SPT-selected galaxy clusters using Dark Energy Survey Science Verification data",
abstract = "We present weak-lensing (WL) mass constraints for a sample of massive galaxy clusters detected by the South Pole Telescope (SPT) via the Sunyaev-Zel'dovich effect (SZE). We use griz imaging data obtained from the Science Verification (SV) phase of the Dark Energy Survey (DES) to fit the WL shear signal of 33 clusters in the redshift range 0.25 ≤ z ≤ 0.8 with NFW profiles and to constrain a four-parameter SPT mass-observable relation. To account for biases in WL masses, we introduce a WL mass to true mass scaling relation described by a mean bias and an intrinsic, lognormal scatter. We allow for correlated scatter within the WL and SZE mass-observable relations and use simulations to constrain priors on nuisance parameters related to bias and scatter from WL. We constrain the normalization of the ζ-M500 relation, ASZ =12.0-6.7+2.6 when using a prior on the mass slope BSZ from the latest SPT cluster cosmology analysis. Without this prior, we recover ASZ=10.8-5.2+2.3 and BSZ=1.30-0.44+0.22. Results in both cases imply lower cluster masses than measured in previous work with and without WL, although the uncertainties are large. The WL derived value of BSZ is ≈ 20 per cent lower than the value preferred by the most recent SPT cluster cosmology analysis. The method demonstrated in this work is designed to constrain cluster masses and cosmological parameters simultaneously and will form the basis for subsequent studies that employ the full SPT cluster sample together with the DES data.",
keywords = "cosmology: observations, galaxies: clusters: general, gravitational lensing: weak",
author = "{DES Collaboration} and {SPT Collaborations} and C. Stern and Dietrich, {J. P.} and S. Bocquet and D. Applegate and Mohr, {J. J.} and Bridle, {S. L.} and {Carrasco Kind}, M. and D. Gruen and M. Jarvis and T. Kacprzak and A. Saro and E. Sheldon and Troxel, {M. A.} and J. Zuntz and Benson, {B. A.} and R. Capasso and I. Chiu and S. Desai and D. Rapetti and Reichardt, {C. L.} and B. Saliwanchik and T. Schrabback and N. Gupta and Abbott, {T. M. C.} and Abdalla, {F. B.} and S. Avila and E. Bertin and D. Brooks and Burke, {D. L.} and {Carnero Rosell}, A. and J. Carretero and Castander, {F. J.} and D'Andrea, {C. B.} and {Da Costa}, {L. N.} and C. Davis and {De Vicente}, J. and Diehl, {H. T.} and P. Doel and J. Estrada and Evrard, {A. E.} and B. Flaugher and P. Fosalba and J. Frieman and J. Garc{\'i}a-Bellido and E. Gaztanaga and Gruendl, {R. A.} and J. Gschwend and G. Gutierrez and D. Hollowood and T. Jeltema",
year = "2019",
month = "5",
day = "1",
doi = "10.1093/mnras/stz234",
language = "English",
volume = "485",
pages = "69--87",
journal = "MNRAS",
issn = "0035-8711",
publisher = "Oxford University Press",
number = "1",

}

RIS

TY - JOUR

T1 - Weak-lensing analysis of SPT-selected galaxy clusters using Dark Energy Survey Science Verification data

AU - DES Collaboration

AU - SPT Collaborations

AU - Stern, C.

AU - Dietrich, J. P.

AU - Bocquet, S.

AU - Applegate, D.

AU - Mohr, J. J.

AU - Bridle, S. L.

AU - Carrasco Kind, M.

AU - Gruen, D.

AU - Jarvis, M.

AU - Kacprzak, T.

AU - Saro, A.

AU - Sheldon, E.

AU - Troxel, M. A.

AU - Zuntz, J.

AU - Benson, B. A.

AU - Capasso, R.

AU - Chiu, I.

AU - Desai, S.

AU - Rapetti, D.

AU - Reichardt, C. L.

AU - Saliwanchik, B.

AU - Schrabback, T.

AU - Gupta, N.

AU - Abbott, T. M. C.

AU - Abdalla, F. B.

AU - Avila, S.

AU - Bertin, E.

AU - Brooks, D.

AU - Burke, D. L.

AU - Carnero Rosell, A.

AU - Carretero, J.

AU - Castander, F. J.

AU - D'Andrea, C. B.

AU - Da Costa, L. N.

AU - Davis, C.

AU - De Vicente, J.

AU - Diehl, H. T.

AU - Doel, P.

AU - Estrada, J.

AU - Evrard, A. E.

AU - Flaugher, B.

AU - Fosalba, P.

AU - Frieman, J.

AU - García-Bellido, J.

AU - Gaztanaga, E.

AU - Gruendl, R. A.

AU - Gschwend, J.

AU - Gutierrez, G.

AU - Hollowood, D.

AU - Jeltema, T.

PY - 2019/5/1

Y1 - 2019/5/1

N2 - We present weak-lensing (WL) mass constraints for a sample of massive galaxy clusters detected by the South Pole Telescope (SPT) via the Sunyaev-Zel'dovich effect (SZE). We use griz imaging data obtained from the Science Verification (SV) phase of the Dark Energy Survey (DES) to fit the WL shear signal of 33 clusters in the redshift range 0.25 ≤ z ≤ 0.8 with NFW profiles and to constrain a four-parameter SPT mass-observable relation. To account for biases in WL masses, we introduce a WL mass to true mass scaling relation described by a mean bias and an intrinsic, lognormal scatter. We allow for correlated scatter within the WL and SZE mass-observable relations and use simulations to constrain priors on nuisance parameters related to bias and scatter from WL. We constrain the normalization of the ζ-M500 relation, ASZ =12.0-6.7+2.6 when using a prior on the mass slope BSZ from the latest SPT cluster cosmology analysis. Without this prior, we recover ASZ=10.8-5.2+2.3 and BSZ=1.30-0.44+0.22. Results in both cases imply lower cluster masses than measured in previous work with and without WL, although the uncertainties are large. The WL derived value of BSZ is ≈ 20 per cent lower than the value preferred by the most recent SPT cluster cosmology analysis. The method demonstrated in this work is designed to constrain cluster masses and cosmological parameters simultaneously and will form the basis for subsequent studies that employ the full SPT cluster sample together with the DES data.

AB - We present weak-lensing (WL) mass constraints for a sample of massive galaxy clusters detected by the South Pole Telescope (SPT) via the Sunyaev-Zel'dovich effect (SZE). We use griz imaging data obtained from the Science Verification (SV) phase of the Dark Energy Survey (DES) to fit the WL shear signal of 33 clusters in the redshift range 0.25 ≤ z ≤ 0.8 with NFW profiles and to constrain a four-parameter SPT mass-observable relation. To account for biases in WL masses, we introduce a WL mass to true mass scaling relation described by a mean bias and an intrinsic, lognormal scatter. We allow for correlated scatter within the WL and SZE mass-observable relations and use simulations to constrain priors on nuisance parameters related to bias and scatter from WL. We constrain the normalization of the ζ-M500 relation, ASZ =12.0-6.7+2.6 when using a prior on the mass slope BSZ from the latest SPT cluster cosmology analysis. Without this prior, we recover ASZ=10.8-5.2+2.3 and BSZ=1.30-0.44+0.22. Results in both cases imply lower cluster masses than measured in previous work with and without WL, although the uncertainties are large. The WL derived value of BSZ is ≈ 20 per cent lower than the value preferred by the most recent SPT cluster cosmology analysis. The method demonstrated in this work is designed to constrain cluster masses and cosmological parameters simultaneously and will form the basis for subsequent studies that employ the full SPT cluster sample together with the DES data.

KW - cosmology: observations

KW - galaxies: clusters: general

KW - gravitational lensing: weak

UR - http://www.scopus.com/inward/record.url?scp=85067185599&partnerID=8YFLogxK

U2 - 10.1093/mnras/stz234

DO - 10.1093/mnras/stz234

M3 - Article

AN - SCOPUS:85067185599

VL - 485

SP - 69

EP - 87

JO - MNRAS

JF - MNRAS

SN - 0035-8711

IS - 1

ER -

ID: 15846496