Dark Energy Survey Year 3: Blue shear
J. McCulloughSLAC National Accelerator LaboratoryA. AmonPrinceton UniversityElisa LegnaniBarcelona Institute of Science and TechnologyE. LegnaniBarcelona Institute of Science and TechnologyD GruenLudwig-Maximilians-UniversitätD. GruenExcellence Cluster ORIGINSA. RoodmanSLAC National Accelerator LaboratoryA RoodmanSLAC National Accelerator LaboratoryO. FriedrichLudwig-Maximilians-UniversitätO FriedrichLudwig-Maximilians-UniversitätN. MacCrannUniversity of CambridgeM. BeckerArgonne National LaboratoryM. R. BeckerArgonne National LaboratoryJ. MylesPrinceton UniversityScott DodelsonCarnegie Mellon UniversityS. DodelsonCarnegie Mellon UniversityS. SamuroffNortheastern UniversityS SamuroffNortheastern UniversityJ. BlazekNortheastern UniversityJ BlazekNortheastern UniversityJ PratKTH Royal Institute of Technology and Stockholm UniversityJ. PratUniversity of ChicagoK HonscheidLaboratório Interinstitucional de e-Astronomia - LIneAA. PieresLaboratório Interinstitucional de e-Astronomia - LIneAA PieresSLAC National Accelerator LaboratoryA. FertéArgonne National LaboratoryA. Drlica-WagnerFermi National Accelerator LaboratoryA. AlarconFermi National Accelerator LaboratoryA. ChoiNASA Goddard Space Flight CenterA Drlica-WagnerNASA Goddard Space Flight CenterA. Navarro-AlsinaUniversidade Estadual de CampinasA ChoiUniversidade Estadual de CampinasA Navarro-AlsinaCarnegie Mellon UniversityA. A. Plazas MalagónStanford UniversityA. CamposSLAC National Accelerator LaboratoryA. PorredonRuhr University BochumA. J. RossThe Ohio State UniversityArya FarahiLaboratório Interinstitucional de e-Astronomia - LIneAB. YinCarnegie Mellon UniversityA.J. RossCarnegie Mellon UniversityB. FlaugherFermi National Accelerator LaboratoryA. Carnero RosellFermi National Accelerator LaboratoryB YinFermi National Accelerator LaboratoryB FlaugherUniversity of PennsylvaniaB. YannyUniversity of ChicagoC. SánchezStanford UniversityC. DavisStanford UniversityC. ChangThe Ohio State UniversityChristopher DavisUniversité Grenoble AlpesC. ToUniversity College LondonD. BrooksUniversity College LondonC. DouxLPSC - Laboratoire de Physique Subatomique et de Cosmologie (53 avenue des Martyrs - 38026 Grenoble Cedex - France)D. Sanchez CidMedioambientales y Tecnológicas (CIEMAT)David J. BrooksMedioambientales y Tecnológicas (CIEMAT)D. J. JamesSanta Cruz Institute for Particle PhysicsD. L. HollowoodSanta Cruz Institute for Particle PhysicsD Sanchez CidUniversity of MichiganD. HutererUniversity of MichiganD.L HollowoodStanford UniversityDragan HutererInstitute of Space Sciences (ICEE. GaztanagaInstitut d’Estudis Espacials de Catalunya (IEEC)E. M. HuffCalifornia Institute of TechnologyE. S. RykoffCalifornia Institute of TechnologyE. GaztañagaOak Ridge National LaboratoryEric HuffBrookhaven National LaboratoryE. SuchytaMedioambientales y Tecnológicas (CIEMAT)E. SheldonETH ZurichE. SánchezUniversity of MichiganF. TarsitanoInstitut d’Estudis Espacials de Catalunya (IEEC)F. Andrade-OliveiraUniversity of PennsylvaniaG. GutierrezFermi National Accelerator LaboratoryF. J. CastanderFermi National Accelerator LaboratoryG. M. BernsteinInstitute of Science and TechnologyG. GianniniBarcelona Institute of Science and TechnologyG GutierrezUniversity of MichiganG. TarleUniversity of MichiganG GianniniFermi National Accelerator LaboratoryG. TarléUniversity of ArizonaH. HuangUniversity of ArizonaI. HarrisonCardiff UniversityH. T. DiehlCardiff UniversityHung-Jin HuangMedioambientales y Tecnológicas (CIEMAT)I HarrisonUniversité de ToulouseI. Sevilla-NoarbeInstitute of Theoretical AstrophysicsJ. Elvin-PooleUniversity of WaterlooI. TutusausUniversity Avenue WI. FerreroTexas A&M UniversityJ Elvin-PoolePerimeter Institute for Theoretical PhysicsJ. WellerMax Planck Institute for Extraterrestrial PhysicsJ. L. MarshallMax Planck Institute for Extraterrestrial PhysicsJ. MuirUniversity of EdinburghJ. ZuntzUniversity of EdinburghJ WellerInstitute of Science and TechnologyJ ZuntzLawrence Berkeley National LaboratoryJ. DeRoseLawrence Berkeley National LaboratoryJ. FriemanUniversity of ChicagoJ. CarreteroFermi National Accelerator LaboratoryJoseph DeRoseUniversity of ManchesterJ. CorderoUniversidad Autonoma de MadridJ. De VicenteLPSC GrenobleJ. García-BellidoUniversity of PennsylvaniaJ. Mena-FernándezUniversity of SussexK. EckertUniversity Avenue MadisonK. HernerFermi National Accelerator LaboratoryA. K. RomerFermi National Accelerator LaboratoryK. HonscheidThe Ohio State UniversityK. BechtolThe Ohio State UniversityK HernerLowell ObservatoryK. KuehnUniversity of ChicagoL. F. SeccoLaboratório Interinstitucional de e-Astronomia - LIneAL. N. da CostaFermi National Accelerator LaboratoryM. PaternoUniversity of MichiganM. Soares-SantosUniversity of PennsylvaniaM. RaveriUniversity of Genova and INFNM. GattiUniversity of Genova and INFNMarco RaveriDuke University DurhamM. YamamotoLancaster UniversityM. SmithNational Center for Supercomputing ApplicationsM. Carrasco KindDuke University DurhamM. A. TroxelUniversity of PennsylvaniaM. JarvisUniversity of PennsylvaniaM AguenaMike JarvisLawrence Berkeley National LaboratoryO. LahavUniversity College LondonM. E. C. SwansonUniversity College LondonN. WeaverdyckUniversity College LondonO LahavUniversity of SouthamptonP. DoelInstitute of Science and TechnologyR. MiquelInstitute of Science and TechnologyP. WisemanNational Center for Supercomputing ApplicationsR. CawthonWilliam Jewell CollegeR MiquelWilliam Jewell CollegeR. A. GruendlFermi National Accelerator LaboratoryR CawthonUniversity of QueenslandS. AllamUniversity of ManchesterS. R. HintonLudwig-Maximilians-UniversitätS. L. BridleIIT HyderabadS. DesaiIIT HyderabadS. PandeyUniversity of PennsylvaniaS. BocquetUniversity of PennsylvaniaS DesaiCalifornia Institute of TechnologyS. EverettCalifornia Institute of Technology
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Modeling the intrinsic alignment (IA) of galaxies poses a challenge to weak lensing analyses. The Dark Energy Survey is expected to be less impacted by IA when limited to blue, star-forming galaxies. The cosmological parameter constraints from this blue cosmic shear sample are stable to IA model choice, unlike passive galaxies in the full DES Y3 sample, the goodness-of-fit is improved and the $Ω_{m}$ and $S_8$ better agree with the cosmic microwave background. Mitigating IA with sample selection, instead of flexible model choices, can reduce uncertainty in $S_8$ by a factor of 1.5.
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