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 ξ± and the full configuration-dependent three-point shear correlation functions across all autoand cross-redshift bins. We compress the three-point functions into the mass aperture statistic 〈M3ap〉 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 Ωm-S8 plane when we add the 〈M3ap〉 data to ξ±. We present our findings for all relevant cosmological and systematic uncertainty parameters and discuss the complementarity of thirdorder and second-order statistics.
| Original language | English |
|---|---|
| Pages (from-to) | 1235141-12351426 |
| Number of pages | 11116286 |
| Journal | Physical Review D |
| Volume | 112 |
| Issue number | 12 |
| DOIs | |
| State | Published - Dec 4 2025 |
Funding
We thank Ryuichi Takahashi, Gary Bernstein and Masahiro Takada for useful discussions. We also thank Kazuyuki Akitsu for providing references to studies on galaxy clustering. B. J. and R. C. H. G. are partially sup ported by the U.S. Department of Energy Grant No. DE SC0007901 and S.S. is supported by the JSPS Overseas Research Fellowships. Part of this work was supported by the NASA ROSES Grant No. 22-ROMAN11-0011 via a JPL subaward. Funding for the DES projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciències de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the asso ciated Excellence Cluster Universe, the University of Michigan, NSF NOIRLab, the University of Nottingham, the Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at NSF Cerro Tololo Inter-American Observatory at NSF NOIRLab (NOIRLab Prop. ID 2012B-0001; PI: J. Frieman), which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data manage ment system is supported by the National Science Foundation under Grants No. AST-1138766 and No. AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under Grants No. PID2021-123012, No. PID2021-128989, No. PID2022-141079, No. SEV-2016-0588, No. CEX2020-001058-M and No. CEX2020-001007-S, some of which include ERDF funds from the European Union. I. F. A.E. is partially funded by the CERCA program of the Generalitat de Catalunya. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq Grant No. 465376/2014-2). This document was prepared by the DES Collaboration using the resources of the Fermi National Accelerator Laboratory (Fermilab), a U.S. Department of Energy, Office of Science, Office of High Energy Physics HEP User Facility. Fermilab is managed by Fermi Forward Discovery Group, LLC, acting under Contract No. 89243024CSC000002. R. C.H.G. and S.S. developed the pipeline, performed the analysis, and wrote the manuscript. B.J. served as project advisor and contributed to the manuscript. M. J. developed novel TREECORR functionalities. D.A. gen erated the CosmoGridV1 mocks used in this work. M.G. contributed with the two-point analysis setup. D. G., Z. G., and A.H. contributed by testing the simulations. A. H., G. A.M. and S.P. served as collaboration internal reviewers, and J. L. M. as collaboration final reader. is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under Grants No. AST-1138766 and No. AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under Grants No. PID2021-123012, No. PID2021-128989, No. PID2022-141079, No. SEV-2016-0588, No. CEX2020-001058-M and No. CEX2020-001007-S, some of which include ERDF funds from the European Union. I. F. A. E. is partially funded by the CERCA program of the Generalitat de Catalunya. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq Grant No. 465376/2014-2). This document was prepared by the DES Collaboration using the resources of the Fermi National Accelerator Laboratory (Fermilab), a U.S. Department of Energy, Office of Science, Office of High Energy Physics HEP User Facility. Fermilab is managed by Fermi Forward Discovery Group, LLC, acting under Contract No. 89243024CSC000002. We thank Ryuichi Takahashi, Gary Bernstein and Masahiro Takada for useful discussions. We also thank Kazuyuki Akitsu for providing references to studies on galaxy clustering. B. J. and R. C. H. G. are partially supported by the U.S. Department of Energy Grant No. DESC0007901 and S. S. is supported by the JSPS Overseas Research Fellowships. Part of this work was supported by the NASA ROSES Grant No. 22-ROMAN11-0011 via a JPL subaward. Funding for the DES projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciències de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, NSF NOIRLab, the University of Nottingham, the Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at NSF Cerro Tololo Inter-American Observatory at NSF NOIRLab (NOIRLab Prop. ID 2012B-0001; PI: J. Frieman), which