Dark Energy Survey Year 1 Results: Cross-correlation between Dark Energy Survey Y1 galaxy weak lensing and South Pole Telescope+Planck CMB weak lensing
AffiliationUniv Arizona, Dept Phys
Univ Arizona, Steward Observ
MetadataShow full item record
PublisherAMER PHYSICAL SOC
CitationOmori, Y., Baxter, E. J., Chang, C., Kirk, D., Alarcon, A., Bernstein, G. M., ... & Crawford, T. M. (2019). Dark Energy Survey Year 1 Results: Cross-correlation between Dark Energy Survey Y1 galaxy weak lensing and South Pole Telescope+ P l a n c k CMB weak lensing. Physical Review D, 100(4), 043517.
JournalPHYSICAL REVIEW D
RightsCopyright © 2019 American Physical Society
Collection InformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at firstname.lastname@example.org.
AbstractWe cross-correlate galaxy weak lensing measurements from the Dark Energy Survey (DES) year-one data with a cosmic microwave background (CMB) weak lensing map derived from South Pole Telescope (SPT) and Planck data, with an effective overlapping area of 1289 deg(2). With the combined measurements from four source galaxy redshift bins, we obtain a detection significance of 5.8 sigma. We fit the amplitude of the correlation functions while fixing the cosmological parameters to a fiducial Lambda CDM model, finding A = 0.99 +/- 0.17. We additionally use the correlation function measurements to constrain shear calibration bias, obtaining constraints that are consistent with previous DES analyses. Finally, when performing a cosmological analysis under the Lambda CDM model, we obtain the marginalized constraints of Omega(m) = 0.261(-0.051)(+0.070) and S-8 = sigma(8)root Omega(m)/0.3 = 0.660(-0.100)(+0.085). These measurements are used in a companion work that presents cosmological constraints from the joint analysis of two-point functions among galaxies, galaxy shears, and CMB lensing using DES, SPT, and Planck data.
VersionFinal published version
SponsorsNatural Sciences and Engineering Research Council of Canada; Canadian Institute for Advanced Research; Canada Research Chairs program; Kavli Foundation; U.S. Department of Energy [DE-SC0007901, DE-AC02-06CH11357, De-AC02-07CH11359]; Kavli Institute for Cosmological Physics at the University of Chicago [NSF PHY-1125897]; Canada Foundation for Innovation (CFI); ministere de l'Economie, de la science et de l'innovation du Quebec (MESI); Fonds de recherche du Quebec-Nature et technologies (FRQ-NT); National Science Foundation [OCI-0725070, ACI-1238993, PLR-1248097, AST-1138766, AST-1536171]; state of Illinois; Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231]; NSF Physics Frontier Center Grant [PHY-0114422]; Gordon and Betty Moore Foundation ; Australian Research Council Future Fellowship [FT150100074]; U.S. National Science Foundation; Ministry of Science and Education of Spain; Science and Technology Facilities Council of the United Kingdom; Higher Education Funding Council for England; National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign; Kavli Institute of Cosmological Physics at the University of Chicago; Center for Cosmology and Astro-Particle Physics at The Ohio State University; Mitchell Institute for Fundamental Physics and Astronomy at Texas AM University; Financiadora de Estudos e Projetos; Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico; Ministerio da Ciencia, Tecnologia e Inovacao; Deutsche Forschungsgemeinschaft; Collaborating Institutions in the Dark Energy Survey; Argonne National Laboratory; University of California at Santa Cruz; University of Cambridge; Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid; University of Chicago; University College London; DES-Brazil Consortium; University of Edinburgh; Eidgenossische Technische Hochschule (ETH) Zurich; Fermi National Accelerator Laboratory; University of Illinois at Urbana-Champaign; Institut de Ciencies de l'Espai (IEEC/CSIC); Institut de Fisica d'Altes Energies; Lawrence Berkeley National Laboratory; Ludwig-Maximilians Universitat Munchen; associated Excellence Cluster Universe; University of Michigan; National Optical Astronomy Observatory; University of Nottingham; Ohio State University; University of Pennsylvania; University of Portsmouth; SLAC National Accelerator Laboratory; Stanford University; University of Sussex; Texas AM University; OzDES Membership Consortium; MINECO [AYA2015-71825, ESP2015-66861, FPA2015-68048, SEV-2016-0588, SEV-2016-0597, MDM-2015-0509]; ERDF funds from the European Union; CERCA program of the Generalitat de Catalunya; European Research Council under the European Union's Seventh Framework Program (FP7/2007-2013) including ERC Grant [240672, 291329, 306478]; Australian Research Council Centre of Excellence for Allsky Astrophysics (CAASTRO) [CE110001020]; U.S. Department of Energy, Office of Science, Office of High Energy Physics [De-AC02-07CH11359]