Cosmic shear in harmonic space from the Dark Energy Survey Year 1 Data: compatibility with configuration space results

Creators: Camacho, H.; Andrade-Oliveira, F.; Troja, A.; Rosenfeld, R.; Faga, L.; Gomes, R.; Doux, C.; Fang, X.; Lima, M.; Miranda, V.; Eifler, T. F.; Friedrich, O.; Gatti, M.; Bernstein, G. M.; Blazek, J.; Bridle, S. L.; Choi, A.; Davis, C.; DeRose, J.; Gaztanaga, E.; Gruen, D.; Hartley, W. G.; Hoyle, B.; Jarvis, M.; MacCrann, N.; Prat, J.; Rau, M. M.; Samuroff, S.; Sánchez, C.; Sheldon, E.; Troxel, M. A.; Vielzeuf, P.; Zuntz, J.; Abbott, T. M. C.; Aguena, M.; Allam, S.; Annis, J.; Bacon, D.; Bertin, E.; Brooks, D.; Burke, D. L.; Carnero Rosell, A.; Carrasco Kind, M.; Carretero, J.; Castander, F. J.; Cawthon, R.; Costanzi, M.; da Costa, L. N.; Pereira, M. E. S.; De Vicente, J.; Desai, S.; Diehl, H. T.; Doel, P.; Everett, S.; Evrard, A. E.; Ferrero, I.; Flaugher, B.; Fosalba, P.; Friedel, D.; Frieman, J.; García-Bellido, J.; Gerdes, D. W.; Gruendl, R. A.; Gschwend, J.; Gutierrez, G.; Hinton, S. R.; Hollowood, D. L.; Honscheid, K.; Huterer, D.; James, D. J.; Kuehn, K.; Kuropatkin, N.; Lahav, O.; Maia, M. A. G.; Marshall, J. L.; Melchior, P.; Menanteau, F.; Miquel, R.; Morgan, R.; Paz-Chinchón, F.; Petravick, D.; Pieres, A.; Plazas Malagón, A. A.; Reil, K.; Rodriguez-Monroy, M.; Sanchez, E.; Scarpine, V.; Schubnell, M.; Serrano, S.; Sevilla-Noarbe, I.; Smith, M.; Soares-Santos, M.; Suchyta, E.; Tarle, G.; Thomas, D.; To, C.; Varga, T. N.; Weller, J.; Wilkinson, R. D.; DES Collaboration

Abstract

We perform a cosmic shear analysis in harmonic space using the first year of data collected by the Dark Energy Survey (DES-Y1). We measure the cosmic weak lensing shear power spectra using the metacalibration catalogue and perform a likelihood analysis within the framework of CosmoSIS. We set scale cuts based on baryonic effects contamination and model redshift and shear calibration uncertainties as well as intrinsic alignments. We adopt as fiducial covariance matrix an analytical computation accounting for the mask geometry in the Gaussian term, including non-Gaussian contributions. A suite of 1200 lognormal simulations is used to validate the harmonic space pipeline and the covariance matrix. We perform a series of stress tests to gauge the robustness of the harmonic space analysis. Finally, we use the DES-Y1 pipeline in configuration space to perform a similar likelihood analysis and compare both results, demonstrating their compatibility in estimating the cosmological parameters S₈, σ₈, and Ωₘ. We use the DES-Y1 metacalibration shape catalogue, with photometric redshifts estimates in the range of 0.2−1.3, divided in four tomographic bins finding σ₈(Ωₘ/0.3)^(0.5) = 0.766 ± 0.033 at 68 per cent CL. The methods implemented and validated in this paper will allow us to perform a consistent harmonic space analysis in the upcoming DES data.

Additional Information

This research was partially supported by the Laboratório Interinstitucional de e-Astronomia (LIneA), the Brazilian funding agencies CNPq and CAPES, the Instituto Nacional de Ciência e Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2), and the Sao Paulo State Research Agency (FAPESP) through grants 2019/04881-8 (HC) and 2017/05549-1 (AT). The authors acknowledge the use of computational resources from LIneA, the Center for Scientific Computing (NCC/GridUNESP) of the Sao Paulo State University (UNESP), and from the National Laboratory for Scientific Computing (LNCC/MCTI, Brazil), where the SDumont supercomputer (sdumont.lncc.br) was used. This research used resources of the National Energy Research Scientific Computing Center (NERSC), a U.S. Department of Energy Office of Science User Facility operated under Contract No. DE-AC02-05CH11231. This paper has gone through internal review by the DES collaboration. 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 DES. 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, the National Optical Astronomy Observatory, 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. This study is based in part on observations at Cerro Tololo Inter-American Observatory at NSF's 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 grants AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015-71825, ESP2015-66861, FPA2015-68048, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA programme of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics. This work made use of the software packages MATPLOTLIB (Hunter 2007) and NUMPY (Harris et al. 2020). DATA AVAILABILITY STATEMENT. The DES Y1 catalogue is available in the Dark Energy Survey Data Management (DESDM) system at the National Center for Supercomputing Applications (NCSA) at the University of Illinois. It can be accessed at https://des.ncsa.illinois.edu/releases/y1a1/key-catalogs. The pipeline used for the measurement is publicly available at https://github.com/hocamachoc/3x2hs_measurements. Synthetic data produced by the analysis presented here can be shared on request to the corresponding author.

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Resource type: Journal Article
Publisher: Royal Astronomical Society
Published in: Monthly Notices of the Royal Astronomical Society, 516(4), 5799-5815, ISSN: 0035-8711.