Biasing from galaxy trough and peak profiles with the DES Y3 redMaGiC galaxies and the weak lensing mass map

DES Collaboration: Q. Hang et al.

Detalhes bibliográficos
Autores: Hang, Q., Alarcon, Alex, Crocce, Martín, DES Collaboration
Formato: artículo
Estado:Versión publicada
Fecha de publicación:2026
País:España
Recursos:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/424789
Acesso em linha:http://hdl.handle.net/10261/424789
Access Level:acceso abierto
Palavra-chave:Gravitational lensing: weak
Large-scale structure of Universe
Cosmology: observations
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dc.title.none.fl_str_mv Biasing from galaxy trough and peak profiles with the DES Y3 redMaGiC galaxies and the weak lensing mass map
title Biasing from galaxy trough and peak profiles with the DES Y3 redMaGiC galaxies and the weak lensing mass map
spellingShingle Biasing from galaxy trough and peak profiles with the DES Y3 redMaGiC galaxies and the weak lensing mass map
Hang, Q.
Gravitational lensing: weak
Large-scale structure of Universe
Cosmology: observations
title_short Biasing from galaxy trough and peak profiles with the DES Y3 redMaGiC galaxies and the weak lensing mass map
title_full Biasing from galaxy trough and peak profiles with the DES Y3 redMaGiC galaxies and the weak lensing mass map
title_fullStr Biasing from galaxy trough and peak profiles with the DES Y3 redMaGiC galaxies and the weak lensing mass map
title_full_unstemmed Biasing from galaxy trough and peak profiles with the DES Y3 redMaGiC galaxies and the weak lensing mass map
title_sort Biasing from galaxy trough and peak profiles with the DES Y3 redMaGiC galaxies and the weak lensing mass map
dc.creator.none.fl_str_mv Hang, Q.
Alarcon, Alex
Crocce, Martín
DES Collaboration
author Hang, Q.
author_facet Hang, Q.
Alarcon, Alex
Crocce, Martín
DES Collaboration
author_role author
author2 Alarcon, Alex
Crocce, Martín
DES Collaboration
author2_role author
author
author
dc.contributor.none.fl_str_mv European Commission
Ministerio de Educación y Ciencia (España)
Ministerio de Ciencia e Innovación (España)
Agencia Estatal de Investigación (España)
Generalitat de Catalunya
Crocce, Martín [0000-0002-9745-6228]
Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
dc.subject.none.fl_str_mv Gravitational lensing: weak
Large-scale structure of Universe
Cosmology: observations
topic Gravitational lensing: weak
Large-scale structure of Universe
Cosmology: observations
description DES Collaboration: Q. Hang et al.
publishDate 2026
dc.date.none.fl_str_mv 2026
2026
2026
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https://doi.org/10.1093/mnras/stag006
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dc.publisher.none.fl_str_mv Oxford University Press
Royal Astronomical Society
publisher.none.fl_str_mv Oxford University Press
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spelling Biasing from galaxy trough and peak profiles with the DES Y3 redMaGiC galaxies and the weak lensing mass mapHang, Q.Alarcon, AlexCrocce, MartínDES CollaborationGravitational lensing: weakLarge-scale structure of UniverseCosmology: observationsDES Collaboration: Q. Hang et al.We measure the correspondence between the distribution of galaxies and matter around troughs and peaksin the projected galaxy density, by comparing redMaGiC galaxies (0.15 < z < 0.65) to weak lensing mass maps from the Dark Energy Survey (DES) Y3 data release. We obtain stacked profiles, as a function of angle θ, of the galaxy density contrast δg and the weak lensing convergence κ, in the vicinity of these identified troughs and peaks, referred to as ‘void’ and ‘cluster’ superstructures. The ratio of the profiles depend mildly on θ, indicating good consistency between the profile shapes. We model the amplitude of this ratio using a function F(η, θ ) that depends on cosmological parameters η, scaled by the galaxy bias. We construct templates of F(η, θ ) using a suite of N-body (Gower Street) simulations forward-modelled with DES Y3-like noise and systematics. We discuss and quantify the caveats of using a linear bias model to create galaxy maps from the simulation dark matter shells. We measure the galaxy bias in three lens tomographic bins (near to far): 2.32+0.86 −0.27, 2.18+0.86 −0.23, 1.86+0.82 −0.23 for voids, and 2.46+0.73 −0.27, 3.55+0.96 −0.55, 4.27+0.36 −1.14 for clusters, assuming the best-fitting Planck cosmology. Similar values with ∼ 0.1σ shifts are obtained assuming the mean DES Y3 cosmology. The biases from troughs and peaks are broadly consistent, although a larger bias is derived for peaks, which is also larger than those measured from the DES Y3 3 × 2-point analysis. This method shows an interesting avenue for measuring field-level bias that can be applied to future lensing surveys.QH and OL acknowledge STFC Consolidated Grant ST/R000476/1. OL also acknowledges visits to All Souls College and to the Physics Department, University of Oxford. NJ is supported by STFC Consolidated Grant ST/V000780/1 and ERC-selected UKRI Frontier Research Grant EP/Y03015X/1. The Gower Street simulations were generated under the DiRAC project p153 ‘Likelihood-free inference with the Dark Energy Survey’ (ACSP255/ACSC1) using DiRAC (STFC) HPC facilities. JW has been supported by the STFC UCL Centre for Doctoral Training in Data Intensive Science. AK has been supported by a Lendület excellence grant by the Hungarian Academy of Sciences (MTA), the European Union’s Horizon Europe research and innovation programme under the Marie Skłodowska-Curie grant agreement number 101130774, and the Hungarian Ministry of Innovation and Technology NRDI Office grant OTKA NN147550. The authors would like to thank Christopher Davis, Elisa Legnani, and Shivam Pandey for serving as the DES internal review committee, whose helpful comments and suggestions improved the quality of this manuscript. The authors would also like to thank the anonymous referee in the MNRAS review process for constructive and insightful comments. 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 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 Grant Numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants PID2021-123012, PID2021-128989 PID2022-141079, SEV-2016-0588, CEX2020-001058-M, and CEX2020-001007-S, some of which include ERDF funds from the European Union. IFAE 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 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.With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (CEX2020-001058-M)With funding from the Spanish government through the "Severo Ochoa Centre of Excelence" accreditation (CEX2020-001007-S)Peer reviewedOxford University PressRoyal Astronomical SocietyEuropean CommissionMinisterio de Educación y Ciencia (España)Ministerio de Ciencia e Innovación (España)Agencia Estatal de Investigación (España)Generalitat de CatalunyaCrocce, Martín [0000-0002-9745-6228]Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]202620262026info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Publisher's versioninfo:eu-repo/semantics/publishedVersionapplication/pdfhttp://hdl.handle.net/10261/424789reponame:DIGITAL.CSIC. 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