Cosmology with second- and third-order shear statistics for the Dark Energy Survey: Methods and simulated analysis

We present a new pipeline designed for the robust inference of cosmological parameters using both second- and third-order shear statistics. We build a theoretical model for rapid evaluation of three-point correlations using our fastnc code and integrate it into the cosmosis framework. We measure the two-point functions ${\ensuremath{\xi}}_{\ifmmode\pm\else\textpm\fi{}}$ and the full configuration-dependent three-point shear correlation functions across all auto- and cross-redshift bins. We compress the three-point functions into the mass aperture statistic $⟨{\mathcal{M}}_{\mathrm{ap}}^{3}⟩$ for a set of 796 simulated shear maps designed to model the Dark Energy Survey Year 3 data. We estimate from it the full covariance matrix and model the effects of intrinsic alignments, shear calibration biases and photometric redshift uncertainties. We apply scale cuts to minimize the contamination from the baryonic signal as modeled through hydrodynamical simulations. We find a significant improvement of 83% on the figure of merit in the ${\mathrm{\ensuremath{\Omega}}}_{\mathrm{m}}\text{\ensuremath{-}}{S}_{8}$ plane when we add the $⟨{\mathcal{M}}_{\mathrm{ap}}^{3}⟩$ data to ${\ensuremath{\xi}}_{\ifmmode\pm\else\textpm\fi{}}$. We present our findings for all relevant cosmological and systematic uncertainty parameters and discuss the complementarity of third-order and second-order statistics.

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Publication Details

Journal
Physical review. D/Physical review. D.
Published
2025-11-11
DOI
https://doi.org/10.1103/3f1p-spfp
Citations
3
Primary Topic
Cosmology and Gravitation Theories
Type
article
Field-Weighted Citation Impact
3.46
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article

Cosmology with second- and third-order shear statistics for the Dark Energy Survey: Methods and simulated analysis

S. R. Hinton, S. Allam, D. Gruen, J. L. Marshall et al.
3 citations
Physical review. D/Physical review. D.
Cosmology and Gravitation Theories
3.46
article

Cosmology with second- and third-order shear statistics for the Dark Energy Survey: Methods and simulated analysis

S. R. Hinton, S. Allam, D. Gruen, J. L. Marshall, J. Muir, A. A. Plazas, Gregory Tarlé, Ashadul Halder, O. Alves, J. Carretero, S. Pandey, D. Sanchez Cid, D.J James, Eusebio Sanchez, J. Weller, Zengtai Gong, N Jeffrey, J. Mena-Fernández, A. Carnero Rosell, ENRIQUE GAZTAÑAGA, S. Bocquet, C. To, R. A. Gruendl, J. García-Bellido, Dhayaa Anbajagane, Mike Jarvis, R. L. C. Ogando, K. Herner, Gabriela A. Marques, M. E. S. Pereira, F. Andrade-Oliveira, Dragan Huterer A, A. Pieres, C. Doux, J Blazek, Rafael C. H. Gomes, N. Weaverdyck, D. Brooks, G. Gutierrez, S Samuroff, M. Soares-Santos, L. N. da Costa, M. E. C. Swanson, B. Flaugher, K Honscheid, B. X. Santiago, P. Doel, D. Bacon, I Sevilla-Noarbe, S Everett, J Frieman, J García-Bellido, V. Vikram, M. Gatti, S. Sugiyama, Bhuvnesh Jain, M Smith, D. Gebauer, R. Miquel
article en
3 citations

Abstract

We present a new pipeline designed for the robust inference of cosmological parameters using both second- and third-order shear statistics. We build a theoretical model for rapid evaluation of three-point correlations using our fastnc code and integrate it into the cosmosis framework. We measure the two-point functions ${\ensuremath{\xi}}_{\ifmmode\pm\else\textpm\fi{}}$ and the full configuration-dependent three-point shear correlation functions across all auto- and cross-redshift bins. We compress the three-point functions into the mass aperture statistic $⟨{\mathcal{M}}_{\mathrm{ap}}^{3}⟩$ for a set of 796 simulated shear maps designed to model the Dark Energy Survey Year 3 data. We estimate from it the full covariance matrix and model the effects of intrinsic alignments, shear calibration biases and photometric redshift uncertainties. We apply scale cuts to minimize the contamination from the baryonic signal as modeled through hydrodynamical simulations. We find a significant improvement of 83% on the figure of merit in the ${\mathrm{\ensuremath{\Omega}}}_{\mathrm{m}}\text{\ensuremath{-}}{S}_{8}$ plane when we add the $⟨{\mathcal{M}}_{\mathrm{ap}}^{3}⟩$ data to ${\ensuremath{\xi}}_{\ifmmode\pm\else\textpm\fi{}}$. We present our findings for all relevant cosmological and systematic uncertainty parameters and discuss the complementarity of third-order and second-order statistics.

Physical review. D/Physical review. D.Vol. 112(12)
University of Calicut (IN), Institució Catalana de Recerca i Estudis Avançats (ES), California Institute of Technology (US), Universitat Autònoma de Barcelona (ES), Oak Ridge National Laboratory (US), Northeastern University (US), Fermi National Accelerator Laboratory (US), Institute of Space Sciences (ES), Harvard University (US), Lawrence Berkeley National Laboratory (US), University of Illinois Urbana-Champaign (US), Universidad de La Laguna (ES), Universität Hamburg (DE), The University of Queensland (AU), Urbana University (US), Perimeter Institute (CA), University of California, Santa Cruz (US), Institute for High Energy Physics (ES), University of Zurich (CH), University of Cambridge (GB), University of Michigan (US), Mitchell Institute (US), The Ohio State University at Lima (US), SLAC National Accelerator Laboratory (US), University of California System (US), LMU Klinikum (DE), CEA Grenoble (FR), Central University of Kerala (IN), California University of Pennsylvania (US), University of Chicago (US), Valongo Observatory (BR), Max Planck Institute for Extraterrestrial Physics (DE), Institut d'Estudis Espacials de Catalunya (ES), Kavli Institute for Particle Astrophysics and Cosmology (US), Menlo School (US), Institute of Particle Physics (CA), Institut Català de Ciències del Clima (ES), Jesus University (KR), Instituto de Física La Plata (AR), Michigan United (US), Astrobiology Center (JP), California Consortium of Addiction Programs and Professionals (US), Unidades Centrales Científico-Técnicas (ES), Institute of Astronomy (RU), Center for Astrophysics Harvard & Smithsonian (US), National Observatory (BR), Institut für Urheber- und Medienrecht (DE), Instituto de Astrofísica de Canarias (ES), Barcelona Institute of Science and Technology (ES), National Center for Supercomputing Applications (US), Hamburg Institut (Germany) (DE), Laboratoire de Physique Subatomique et de Cosmologie (FR), Science Oxford (GB), Laboratório Interinstitucional de e-Astronomia (BR), Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (ES), State Library of Ohio (US), Institute of Science and Technology, Institut des langues et cultures d'Europe, Amérique, Afrique, Asie et Australie (FR), University College London (GB), The Ohio State University (US), University of Portsmouth (GB), University of Cincinnati (US), Universidad Autónoma de Madrid (ES), Lancaster University (GB), Columbia University (US), University of Pennsylvania (US), Ludwig-Maximilians-Universität München (DE), Universidad del Noreste (MX), Université Grenoble Alpes (FR), Texas A&M University (US), Netherlands Institute for Radio Astronomy (NL), University of California, Berkeley (US), Stanford University (US)
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Cosmology and Gravitation Theories
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