Dark Energy Survey Year 1 Results: Cosmological Constraints from Cluster Abundances, Weak Lensing, and Galaxy Correlations

To, C. and Krause, E. and Rozo, E. and Wu, H. and Desai, Shantanu et. al. (2021) Dark Energy Survey Year 1 Results: Cosmological Constraints from Cluster Abundances, Weak Lensing, and Galaxy Correlations. Physical Review Letters, 126 (14). ISSN 0031-9007

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We present the first joint analysis of cluster abundances and auto or cross-correlations of three cosmic tracer fields: galaxy density, weak gravitational lensing shear, and cluster density split by optical richness. From a joint analysis (4×2pt+N) of cluster abundances, three cluster cross-correlations, and the auto correlations of the galaxy density measured from the first year data of the Dark Energy Survey, we obtain ωm=0.305-0.038+0.055 and σ8=0.783-0.054+0.064. This result is consistent with constraints from the DES-Y1 galaxy clustering and weak lensing two-point correlation functions for the flat νΛCDM model. Consequently, we combine cluster abundances and all two-point correlations from across all three cosmic tracer fields (6×2pt+N) and find improved constraints on cosmological parameters as well as on the cluster observable-mass scaling relation. This analysis is an important advance in both optical cluster cosmology and multiprobe analyses of upcoming wide imaging surveys.

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IITH Creators:
IITH CreatorsORCiD
Desai, Shantanuhttp://orcid.org/0000-0002-0466-3288
Item Type: Article
Uncontrolled Keywords: Dark energy,Surveys,Tracers, Cluster densities, Cosmological parameters, Cross correlations, Galaxy clustering, Multi-probe analysis,Two point correlation functions
Subjects: Physics
Physics > Classical mechanics
Physics > Astronomy Astrophysics
Divisions: Department of Physics
Depositing User: . LibTrainee 2021
Date Deposited: 29 May 2021 09:41
Last Modified: 29 May 2021 09:41
URI: http://raiith.iith.ac.in/id/eprint/7876
Publisher URL: http://doi.org/10.1103/PhysRevLett.126.141301
OA policy: https://v2.sherpa.ac.uk/id/publication/13640
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