Dark Energy Survey Year 3 results: Cosmological constraints from galaxy clustering and galaxy-galaxy lensing using the MagLim lens sample

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Autor(es): dc.contributorOhio State University-
Autor(es): dc.contributorCSIC-
Autor(es): dc.contributorInstitut d'Estudis Espacials de Catalunya (IEEC)-
Autor(es): dc.contributorUniversity of Wisconsin-Madison-
Autor(es): dc.contributorBarcelona Institute of Science and Technology-
Autor(es): dc.contributorCentro de Investigaciones Energéticas Medioambientales y Tecnológicas (CIEMAT)-
Autor(es): dc.contributorInstituto de Astrofisica de Canarias-
Autor(es): dc.contributorLaboratório Interinstitucional de e-Astronomia-LIneA-
Autor(es): dc.contributorUniversidad de La Laguna-
Autor(es): dc.contributorUniversity of Oslo-
Autor(es): dc.contributorUniversity of Arizona-
Autor(es): dc.contributorUniversity of Chicago-
Autor(es): dc.contributorUniversity of Pennsylvania-
Autor(es): dc.contributorStanford University-
Autor(es): dc.contributorCarnegie Mellon University-
Autor(es): dc.contributorArgonne National Laboratory-
Autor(es): dc.contributorUniversity of Michigan-
Autor(es): dc.contributorUniversidade Estadual Paulista (UNESP)-
Autor(es): dc.contributorUniversity of Hawai'i-
Autor(es): dc.contributorNortheastern University-
Autor(es): dc.contributorObservatoire de Sauverny-
Autor(es): dc.contributorNational Center for Supercomputing Applications-
Autor(es): dc.contributorUniversity of Illinois at Urbana-Champaign-
Autor(es): dc.contributorFermi National Accelerator Laboratory-
Autor(es): dc.contributorUniversity of Manchester-
Autor(es): dc.contributorLawrence Berkeley National Laboratory-
Autor(es): dc.contributorCalifornia Institute of Technology-
Autor(es): dc.contributorSanta Cruz Institute for Particle Physics-
Autor(es): dc.contributorUniversity of Cambridge-
Autor(es): dc.contributorSLAC National Accelerator Laboratory-
Autor(es): dc.contributorUniversity of Oxford-
Autor(es): dc.contributorUniversity of Geneva-
Autor(es): dc.contributorDuke University-
Autor(es): dc.contributorUniversity College London-
Autor(es): dc.contributorUniversity of Sussex-
Autor(es): dc.contributorUniversity of Tokyo-
Autor(es): dc.contributorBrookhaven National Laboratory-
Autor(es): dc.contributorUniversity of Edinburgh-
Autor(es): dc.contributorNSF's National Optical-Infrared Astronomy Research Laboratory-
Autor(es): dc.contributorUniversidad Autonoma de Madrid-
Autor(es): dc.contributorUniversity of Portsmouth-
Autor(es): dc.contributorInstitut d'Astrophysique de Paris-
Autor(es): dc.contributorUniversity of Trieste-
Autor(es): dc.contributorINAF-Osservatorio Astronomico di Trieste-
Autor(es): dc.contributorInstitute for Fundamental Physics of the Universe-
Autor(es): dc.contributorObservatório Nacional-
Autor(es): dc.contributorUniversity of Queensland-
Autor(es): dc.contributorIIT Hyderabad-
Autor(es): dc.contributorLudwig-Maximilians-Universität-
Autor(es): dc.contributorMax Planck Institute for Extraterrestrial Physics-
Autor(es): dc.contributorHarvard and Smithsonian-
Autor(es): dc.contributorMacquarie University-
Autor(es): dc.contributorLowell Observatory-
Autor(es): dc.contributorAustralian National University-
Autor(es): dc.contributorUniversidade de São Paulo (USP)-
Autor(es): dc.contributorTexas A&M University-
Autor(es): dc.contributorHarvard University-
Autor(es): dc.contributorPrinceton University-
Autor(es): dc.contributorInstitució Catalana de Recerca i Estudis Avanćats-
Autor(es): dc.contributorUFRGS-
Autor(es): dc.contributorUniversity of Southampton-
Autor(es): dc.contributorOak Ridge National Laboratory-
Autor(es): dc.contributorLudwig-Maximilians Universität München-
Autor(es): dc.creatorPorredon, A.-
Autor(es): dc.creatorCrocce, M.-
Autor(es): dc.creatorElvin-Poole, J.-
Autor(es): dc.creatorCawthon, R.-
Autor(es): dc.creatorGiannini, G.-
Autor(es): dc.creatorDe Vicente, J.-
Autor(es): dc.creatorCarnero Rosell, A.-
Autor(es): dc.creatorFerrero, I.-
Autor(es): dc.creatorKrause, E.-
Autor(es): dc.creatorFang, X.-
Autor(es): dc.creatorPrat, J.-
Autor(es): dc.creatorRodriguez-Monroy, M.-
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Autor(es): dc.creatorCastander, F. J.-
Autor(es): dc.creatorChoi, A.-
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Autor(es): dc.creatorDodelson, S.-
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Autor(es): dc.creatorBecker, M. R.-
Autor(es): dc.creatorBernstein, G. M.-
Autor(es): dc.creatorBlazek, J.-
Autor(es): dc.creatorCamacho, H.-
Autor(es): dc.creatorCampos, A.-
Autor(es): dc.creatorCarrasco Kind, M.-
Autor(es): dc.creatorChintalapati, P.-
Autor(es): dc.creatorCordero, J.-
Autor(es): dc.creatorDerose, J.-
Autor(es): dc.creatorDi Valentino, E.-
Autor(es): dc.creatorDoux, C.-
Autor(es): dc.creatorEifler, T. F.-
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Autor(es): dc.creatorHarrison, I.-
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Autor(es): dc.creatorSanchez, E.-
Autor(es): dc.creatorSanchez, J.-
Autor(es): dc.creatorSanchez Cid, D.-
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Autor(es): dc.creatorDietrich, J. P.-
Autor(es): dc.creatorDoel, P.-
Autor(es): dc.creatorDrlica-Wagner, A.-
Autor(es): dc.creatorEckert, K.-
Autor(es): dc.creatorEvrard, A. E.-
Autor(es): dc.creatorFlaugher, B.-
Autor(es): dc.creatorFrieman, J.-
Autor(es): dc.creatorGarcía-Bellido, J.-
Autor(es): dc.creatorGerdes, D. W.-
Autor(es): dc.creatorGiannantonio, T.-
Autor(es): dc.creatorGruendl, R. A.-
Autor(es): dc.creatorGschwend, J.-
Autor(es): dc.creatorGutierrez, G.-
Autor(es): dc.creatorHinton, S. R.-
Autor(es): dc.creatorHollowood, D. L.-
Autor(es): dc.creatorHonscheid, K.-
Autor(es): dc.creatorHoyle, B.-
Autor(es): dc.creatorJames, D. J.-
Autor(es): dc.creatorKuehn, K.-
Autor(es): dc.creatorKuropatkin, N.-
Autor(es): dc.creatorLahav, O.-
Autor(es): dc.creatorLidman, C.-
Autor(es): dc.creatorLima, M.-
Autor(es): dc.creatorLin, H.-
Autor(es): dc.creatorMaia, M. A.G.-
Autor(es): dc.creatorMarshall, J. L.-
Autor(es): dc.creatorMartini, P.-
Autor(es): dc.creatorMelchior, P.-
Autor(es): dc.creatorMenanteau, F.-
Autor(es): dc.creatorMiquel, R.-
Autor(es): dc.creatorMohr, J. J.-
Autor(es): dc.creatorMorgan, R.-
Autor(es): dc.creatorOgando, R. L.C.-
Autor(es): dc.creatorPalmese, A.-
Autor(es): dc.creatorPaz-Chinchón, F.-
Autor(es): dc.creatorPetravick, D.-
Autor(es): dc.creatorPieres, A.-
Autor(es): dc.creatorPlazas Malagón, A. A.-
Autor(es): dc.creatorRomer, A. K.-
Autor(es): dc.creatorSantiago, B.-
Autor(es): dc.creatorScarpine, V.-
Autor(es): dc.creatorSchubnell, M.-
Autor(es): dc.creatorSerrano, S.-
Autor(es): dc.creatorSmith, M.-
Autor(es): dc.creatorSoares-Santos, M.-
Autor(es): dc.creatorSuchyta, E.-
Autor(es): dc.creatorTarle, G.-
Autor(es): dc.creatorThomas, D.-
Autor(es): dc.creatorTo, C.-
Autor(es): dc.creatorVarga, T. N.-
Autor(es): dc.creatorWeller, J.-
Data de aceite: dc.date.accessioned2025-08-21T18:37:18Z-
Data de disponibilização: dc.date.available2025-08-21T18:37:18Z-
Data de envio: dc.date.issued2023-07-29-
Data de envio: dc.date.issued2023-07-29-
Data de envio: dc.date.issued2022-11-14-
Fonte completa do material: dc.identifierhttp://dx.doi.org/10.1103/PhysRevD.106.103530-
Fonte completa do material: dc.identifierhttp://hdl.handle.net/11449/247993-
Fonte: dc.identifier.urihttp://educapes.capes.gov.br/handle/11449/247993-
Descrição: dc.descriptionThe cosmological information extracted from photometric surveys is most robust when multiple probes of the large scale structure of the Universe are used. Two of the most sensitive probes are the clustering of galaxies and the tangential shear of background galaxy shapes produced by those foreground galaxies, so-called galaxy-galaxy lensing. Combining the measurements of these two two-point functions leads to cosmological constraints that are independent of the way galaxies trace matter (the galaxy bias factor). The optimal choice of foreground, or lens, galaxies is governed by the joint, but conflicting requirements to obtain accurate redshift information and large statistics. We present cosmological results from the full 5000 deg2 of the Dark Energy Survey's first three years of observations (Y3) combining those two-point functions, using for the first time a magnitude-limited lens sample (MagLim) of 11 million galaxies, especially selected to optimize such combination, and 100 million background shapes. We consider two flat cosmological models, the Standard Model with dark energy and cold dark matter (ΛCDM) a variation with a free parameter for the dark energy equation of state (wCDM). Both models are marginalized over 25 astrophysical and systematic nuisance parameters. In ΛCDM we obtain for the matter density ωm=0.320-0.034+0.041 and for the clustering amplitude S8σ8(ωm/0.3)0.5=0.778-0.031+0.037, at 68% C.L. The latter is only 1σ smaller than the prediction in this model informed by measurements of the cosmic microwave background by the Planck satellite. In wCDM we find ωm=0.32-0.046+0.044, S8=0.777-0.051+0.049 and dark energy equation of state w=-1.031-0.379+0.218. We find that including smaller scales, while marginalizing over nonlinear galaxy bias, improves the constraining power in the ωm-S8 plane by 31% and in the ωm-w plane by 41% while yielding consistent cosmological parameters from those in the linear bias case. These results are combined with those from cosmic shear in a companion paper to present full DES-Y3 constraints from the three two-point functions (3×2pt).-
Descrição: dc.descriptionCenter for Cosmology and Astro-Particle Physics Ohio State University-
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Idioma: dc.languageen-
Relação: dc.relationPhysical Review D-
???dc.source???: dc.sourceScopus-
Título: dc.titleDark Energy Survey Year 3 results: Cosmological constraints from galaxy clustering and galaxy-galaxy lensing using the MagLim lens sample-
Tipo de arquivo: dc.typelivro digital-
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