Abstract
We present a joint cosmic shear analysis of the Dark Energy Survey (DES Y3) and the Kilo-Degree Survey (KiDS-1000) in a collaborative effort between the two survey teams. We find consistent cosmological parameter constraints between DES Y3 and KiDS-1000 which, when combined in a joint-survey analysis, constrain the parameter (Formula Presented) with a mean value of (Formula Presented). The mean marginal is lower than the maximum a posteriori estimate, S8 = 0.801, owing to skewness in the marginal distribution and projection effects in the multi-dimensional parameter space. Our results are consistent with S8 constraints from observations of the cosmic microwave background by Planck, with agreement at the 1.7σ level. We use a Hybrid analysis pipeline, defined from a mock survey study quantifying the impact of the different analysis choices originally adopted by each survey team. We review intrinsic alignment models, baryon feedback mitigation strategies, priors, samplers and models of the non-linear matter power spectrum.
| Original language | English |
|---|---|
| Journal | Open Journal of Astrophysics |
| Volume | 6 |
| DOIs | |
| State | Published - 2023 |
| Externally published | Yes |
Funding
Dark Energy Survey: This project used public archival data from the Dark Energy Survey (DES). 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, Funda\u00E7\u00E3o Carlos Chagas Filho de Amparo \u00E0 Pesquisa do Estado do Rio de Janeiro, Conselho Na-cional de Desenvolvimento Cient\u00EDfico e Tecnol\u00F3gico and the Minist\u00E9rio da Ci\u00EAncia, Tecnologia e Inova\u00E7\u00E3o, 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 Energ\u00E9ticas, Medioambientales y Tecnol\u00F3gicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgen\u00F6ssische Technische Hochschule (ETH) Z\u00FCrich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ci\u00E8ncies de l\u2019Espai (IEEC/CSIC), the Institut de F\u00EDsica d\u2019Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universit\u00E4t M\u00FCnchen and the associated Excellence Cluster Universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, The Ohio State University, the OzDES Membership Consortium, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, and Texas A&M University. The DES results in this paper are based on observations at Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. Kilo-Degree Survey: The KiDS results in this paper are based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme IDs 177.A-3016, 177.A-3017, 177.A-3018 and 179.A-2004, and on data products produced by the KiDS consortium. The KiDS production team acknowledges support from: Deutsche Forschungsgemeinschaft, ERC, NOVA and NWO-M grants; Target; the University of Padova, and the University Federico II (Naples). Data processing for VIKING has been contributed by the VISTA Data Flow System at CASU, Cambridge and WFAU, Edinburgh. Authors: We thank the anonymous referee for their thorough review, positive comments and constructive remarks. We acknowledge support from: the European Research Council under grant numbers 647112 (MA, BG, CH, CL, TT) and 770935 (AD, HHi, CM, RR, JLvdB, AHW); the UK Science and Technology Facilities Council (STFC) under grant numbers ST/V000594/1 (CH, JP, AP, NR, JZ) and ST/V000780/1 (BJ); the Max Planck Society and the Alexander von Humboldt Foundation in the framework of the Max Planck-Humboldt Research Award endowed by the Federal Ministry of Education and Research (CH, BS, MY); the Netherlands Organisation for Scientific Research (NWO) under grant numbers 621.016.402 (JTAdJ) and 639.043.512 (HHo). AA acknowledges the support of a Kavli Fellowship. AC acknowledges support from the SPHEREx project under a contract from NASA/Goddard Space Flight Center to the California Institute of Technology. MB is supported by the Polish National Science Center through grants 2020/38/E/ST9/00395, 2018/30/E/ST9/00698, 2018/31/G/ST9/03388 and 2020/39/B/ST9/03494, and by the Polish Ministry of Science and Higher Education through grant DIR/WK/2018/12. RD acknowledges support from the NSF Graduate Research Fellowship Program under grant number DGE-2039656. BG acknowledges the support of the Royal Society through an Enhancement Award (RGF/EA/181006) and the Royal Society of Edinburgh through the Saltire Early Career Fellowship (ref. number 1914). HHi is supported by a Heisenberg grant of the Deutsche Forschungsgemeinschaft (Hi 1495/5-1). HHi and AHW acknowledge funding from the German Science Foundation DFG, via the Collaborative Research Center SFB1491 \u201CCosmic Interacting Matters - From Source to Signal\u201D. KK acknowledges support from the Royal Society and Imperial College. SL is supported by NOVA, the Netherlands Research School for Astronomy. XL is supported in part by the Department of Energy grant DE-SC0010118 and in part by a grant from the Simons Foundation (Simons Investigator in Astrophysics, Award ID 620789). NRN acknowledges financial support from the National Science Foundation of China, Research Fund for Excellent International Scholars (12150710511), and from the China Manned Space Project research grant CMS-CSST-2021-A01. SS and JB are supported in part by NSF grant AST-2206563. HYS acknowledges the support from CMS-CSST-2021-A01 and CMS-CSST-2021-A04, NSFC of China under grant 11973070, and Key Research Program of Frontier Sciences, CAS, Grant No. ZDBS-LY-7013 and Program of Shanghai Academic/Technology Research Leader. CS acknowledges support from the Agencia Nacional de Investigaci\u00F3n y Desarrollo (ANID) through FONDECYT grant no. 11191125 and BASAL project FB210003. TT acknowledges funding from the Swiss National Science Foundation under the Ambizione project PZ00P2_193352. AHW is supported by the Deutsches Zentrum f\u00FCr Luft-und Raumfahrt (DLR), made possible by the Bundesministerium f\u00FCr Wirtschaft und Klimaschutz. For the purpose of open access, the authors have applied a Creative Commons Attribution (CC BY) licence to any Author Accepted Manuscript version arising from this submission. Hyper Suprime-Cam Survey: The HSC collaboration includes the astronomical communities of Japan and Taiwan, and Princeton University. The HSC instrumentation and software were developed by the National Astronomical Observatory of Japan (NAOJ), the Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU), the University of Tokyo, the High Energy Accelerator Research Organization (KEK), the Academia Sinica Institute for Astronomy and Astrophysics in Taiwan (ASIAA), and Princeton University. Funding was contributed by the FIRST program from the Japanese Cabinet Office, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), the Japan Society for the Promotion of Science (JSPS), Japan Science and Technology Agency (JST), the Toray Science Foundation, NAOJ, Kavli IPMU, KEK, ASIAA, and Princeton University. The HSC results in this paper make use of software developed for Vera C. Rubin Observatory. We thank the Rubin Obsertevatory for making their code available as free software at http://pipelines.lsst.io/. The HSC results in this paper are based on data collected at the Subaru Telescope and retrieved from the HSC data archive system, which is operated by the Subaru Telescope and Astronomy Data Center (ADC) at NAOJ. Data analysis was in part carried out with the cooperation of Center for Computational Astrophysics (CfCA), NAOJ. We are honoured and grateful for the opportunity of observing the Universe from Maunakea, which has the cultural, historical and natural significance in Hawaii.
Keywords
- Cosmology
- Weak Gravitational Lensing