Methods for cluster cosmology and application to the SDSS in preparation for DES Year 1 release

DES Collaboration

doi:10.1093/mnras/stz1949

Methods for cluster cosmology and application to the SDSS in preparation for DES Year 1 release

DES Collaboration

Physics and Astronomy

Osservatorio Astronomico di Trieste
University of Trieste
University of Arizona
University of California at Riverside
Fermi National Accelerator Laboratory
University of Michigan, Ann Arbor
Stanford University
SLAC National Accelerator Laboratory
University of California at Santa Cruz
University of Sussex
Carnegie Mellon University
Max Planck Institute for Extraterrestrial Physics
Ludwig Maximilian University of Munich
Excellence Cluster Universe
National Optical Astronomy Observatory
University College London
Rhodes University
University of Portsmouth
Large Synoptic Survey Telescope
Institute for High Energy Physics
Institute of Space Studies of Catalonia
CSIC
CIEMAT
Jet Propulsion Laboratory, California Institute of Technology
The University of Chicago
Universidad Autónoma de Madrid
University of Cambridge
University of Illinois at Urbana-Champaign

Research output: Contribution to journal › Article › peer-review

126 Scopus citations

Abstract

We implement the first blind analysis of cluster abundance data to derive cosmological constraints from the abundance and weak lensing signal of redMaPPer clusters in the Sloan Digital Sky Survey (SDSS). We simultaneously fit for cosmological parameters and the richness-mass relation of the clusters. For a flat Δ cold dark matter cosmological model with massive neutrinos, we find S₈ ≡ σ₈(Ω_m/0.3)^0.5 = 0.79^+0.05_−0.04. This value is both consistent and competitive with that derived from cluster catalogues selected in different wavelengths. Our result is also consistent with the combined probes analyses by the Dark Energy Survey (DES), the Kilo-Degree Survey (KiDS), and with the cosmic microwave background (CMB) anisotropies as measured by Planck. We demonstrate that the cosmological posteriors are robust against variation of the richness-mass relation model and to systematics associated with the calibration of the selection function. In combination with baryon acoustic oscillation data and big bang nucleosynthesis data (Cooke et al.), we constrain the Hubble rate to be h = 0.66 ± 0.02, independent of the CMB. Future work aimed at improving our understanding of the scatter of the richness-mass relation has the potential to significantly improve the precision of our cosmological posteriors. The methods described in this work were developed for use in the forthcoming analysis of cluster abundances in the DES. Our SDSS analysis constitutes the first part of a staged-unblinding analysis of the full DES data set.

Original language	English
Pages (from-to)	4779-4800
Number of pages	22
Journal	Monthly Notices of the Royal Astronomical Society
Volume	488
Issue number	4
DOIs	https://doi.org/10.1093/mnras/stz1949
State	Published - Oct 1 2019

Keywords

Cosmological parameters
Galaxies: clusters: general
Large-scale structure of Universe

Access to Document

10.1093/mnras/stz1949

Cite this

@article{48a871ad9637449986556127e97b91c8,

title = "Methods for cluster cosmology and application to the SDSS in preparation for DES Year 1 release",

abstract = "We implement the first blind analysis of cluster abundance data to derive cosmological constraints from the abundance and weak lensing signal of redMaPPer clusters in the Sloan Digital Sky Survey (SDSS). We simultaneously fit for cosmological parameters and the richness-mass relation of the clusters. For a flat Δ cold dark matter cosmological model with massive neutrinos, we find S8 ≡ σ8(Ωm/0.3)0.5 = 0.79+0.05−0.04. This value is both consistent and competitive with that derived from cluster catalogues selected in different wavelengths. Our result is also consistent with the combined probes analyses by the Dark Energy Survey (DES), the Kilo-Degree Survey (KiDS), and with the cosmic microwave background (CMB) anisotropies as measured by Planck. We demonstrate that the cosmological posteriors are robust against variation of the richness-mass relation model and to systematics associated with the calibration of the selection function. In combination with baryon acoustic oscillation data and big bang nucleosynthesis data (Cooke et al.), we constrain the Hubble rate to be h = 0.66 ± 0.02, independent of the CMB. Future work aimed at improving our understanding of the scatter of the richness-mass relation has the potential to significantly improve the precision of our cosmological posteriors. The methods described in this work were developed for use in the forthcoming analysis of cluster abundances in the DES. Our SDSS analysis constitutes the first part of a staged-unblinding analysis of the full DES data set.",

keywords = "Cosmological parameters, Galaxies: clusters: general, Large-scale structure of Universe",

author = "\{DES Collaboration\} and M. Costanzi and E. Rozo and M. Simet and Y. Zhang and Evrard, \{A. E.\} and A. Mantz and Rykoff, \{E. S.\} and T. Jeltema and D. Gruen and S. Allen and T. McClintock and Romer, \{A. K.\} and \{von der Linden\}, A. and A. Farahi and J. DeRose and Varga, \{T. N.\} and J. Weller and P. Giles and Hollowood, \{D. L.\} and S. Bhargava and A. Bermeo-Hernandez and X. Chen and Abbott, \{T. M.C.\} and Abdalla, \{F. B.\} and S. Avila and K. Bechtol and D. Brooks and E. Buckley-Geer and Burke, \{D. L.\} and \{Carnero Rosell\}, A. and \{Carrasco Kind\}, M. and J. Carretero and M. Crocce and Cunha, \{C. E.\} and \{da Costa\}, \{L. N.\} and C. Davis and \{de Vicente\}, J. and Diehl, \{H. T.\} and Dietrich, \{J. P.\} and P. Doel and Eifler, \{T. F.\} and J. Estrada 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 Gruendl, \{R. A.\}",

note = "Publisher Copyright: {\textcopyright} 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society",

year = "2019",

month = oct,

day = "1",

doi = "10.1093/mnras/stz1949",

language = "English",

volume = "488",

pages = "4779--4800",

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

issn = "0035-8711",

number = "4",

}

TY - JOUR

T1 - Methods for cluster cosmology and application to the SDSS in preparation for DES Year 1 release

AU - DES Collaboration

AU - Costanzi, M.

AU - Rozo, E.

AU - Simet, M.

AU - Zhang, Y.

AU - Evrard, A. E.

AU - Mantz, A.

AU - Rykoff, E. S.

AU - Jeltema, T.

AU - Gruen, D.

AU - Allen, S.

AU - McClintock, T.

AU - Romer, A. K.

AU - von der Linden, A.

AU - Farahi, A.

AU - DeRose, J.

AU - Varga, T. N.

AU - Weller, J.

AU - Giles, P.

AU - Hollowood, D. L.

AU - Bhargava, S.

AU - Bermeo-Hernandez, A.

AU - Chen, X.

AU - Abbott, T. M.C.

AU - Abdalla, F. B.

AU - Avila, S.

AU - Bechtol, K.

AU - Brooks, D.

AU - Buckley-Geer, E.

AU - Burke, D. L.

AU - Carnero Rosell, A.

AU - Carrasco Kind, M.

AU - Carretero, J.

AU - Crocce, M.

AU - Cunha, C. E.

AU - da Costa, L. N.

AU - Davis, C.

AU - de Vicente, J.

AU - Diehl, H. T.

AU - Dietrich, J. P.

AU - Doel, P.

AU - Eifler, T. F.

AU - Estrada, J.

AU - Flaugher, B.

AU - Fosalba, P.

AU - Frieman, J.

AU - García-Bellido, J.

AU - Gaztanaga, E.

AU - Gerdes, D. W.

AU - Giannantonio, T.

AU - Gruendl, R. A.

PY - 2019/10/1

Y1 - 2019/10/1

N2 - We implement the first blind analysis of cluster abundance data to derive cosmological constraints from the abundance and weak lensing signal of redMaPPer clusters in the Sloan Digital Sky Survey (SDSS). We simultaneously fit for cosmological parameters and the richness-mass relation of the clusters. For a flat Δ cold dark matter cosmological model with massive neutrinos, we find S8 ≡ σ8(Ωm/0.3)0.5 = 0.79+0.05−0.04. This value is both consistent and competitive with that derived from cluster catalogues selected in different wavelengths. Our result is also consistent with the combined probes analyses by the Dark Energy Survey (DES), the Kilo-Degree Survey (KiDS), and with the cosmic microwave background (CMB) anisotropies as measured by Planck. We demonstrate that the cosmological posteriors are robust against variation of the richness-mass relation model and to systematics associated with the calibration of the selection function. In combination with baryon acoustic oscillation data and big bang nucleosynthesis data (Cooke et al.), we constrain the Hubble rate to be h = 0.66 ± 0.02, independent of the CMB. Future work aimed at improving our understanding of the scatter of the richness-mass relation has the potential to significantly improve the precision of our cosmological posteriors. The methods described in this work were developed for use in the forthcoming analysis of cluster abundances in the DES. Our SDSS analysis constitutes the first part of a staged-unblinding analysis of the full DES data set.

AB - We implement the first blind analysis of cluster abundance data to derive cosmological constraints from the abundance and weak lensing signal of redMaPPer clusters in the Sloan Digital Sky Survey (SDSS). We simultaneously fit for cosmological parameters and the richness-mass relation of the clusters. For a flat Δ cold dark matter cosmological model with massive neutrinos, we find S8 ≡ σ8(Ωm/0.3)0.5 = 0.79+0.05−0.04. This value is both consistent and competitive with that derived from cluster catalogues selected in different wavelengths. Our result is also consistent with the combined probes analyses by the Dark Energy Survey (DES), the Kilo-Degree Survey (KiDS), and with the cosmic microwave background (CMB) anisotropies as measured by Planck. We demonstrate that the cosmological posteriors are robust against variation of the richness-mass relation model and to systematics associated with the calibration of the selection function. In combination with baryon acoustic oscillation data and big bang nucleosynthesis data (Cooke et al.), we constrain the Hubble rate to be h = 0.66 ± 0.02, independent of the CMB. Future work aimed at improving our understanding of the scatter of the richness-mass relation has the potential to significantly improve the precision of our cosmological posteriors. The methods described in this work were developed for use in the forthcoming analysis of cluster abundances in the DES. Our SDSS analysis constitutes the first part of a staged-unblinding analysis of the full DES data set.

KW - Cosmological parameters

KW - Galaxies: clusters: general

KW - Large-scale structure of Universe

UR - https://www.scopus.com/pages/publications/85079669905

U2 - 10.1093/mnras/stz1949

DO - 10.1093/mnras/stz1949

M3 - Article

AN - SCOPUS:85079669905

SN - 0035-8711

VL - 488

SP - 4779

EP - 4800

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 4

ER -

Methods for cluster cosmology and application to the SDSS in preparation for DES Year 1 release

Abstract

Keywords

Access to Document

Other files and links

Fingerprint

Cite this