Improving Weak Lensing Mass Map Reconstructions using Gaussian and Sparsity Priors: Application to DES SV

Journal Article · Tue May 15 00:00:00 EDT 2018 · Monthly Notices of the Royal Astronomical Society

DOI:https://doi.org/10.1093/mnras/sty1252· OSTI ID:1437399

Jeffrey, N.  ^[1]; Abdalla, F. B. ^[2]; Lahav, O. ^[1]; Lanusse, F. ^[3]; Starck, J. -L ^[4]; Leonard, A. ^[1]; Kirk, D. ^[1]; Chang, C. ^[5]; Baxter, E. ^[6]; Kacprzak, T. ^[7]; Seitz, S. ^[8]; Vikram, V. ^[9]; Whiteway, L. ^[1]; Abbott, T. M. C. ^[10]; Allam, S. ^[11]; Avila, S. ^[12]; Bertin, E. ^[13]; Brooks, D. ^[1]; Rosell, A. Carnero ^[14]; Kind, M. Carrasco ^[15] ; Carretero, J. ^[16]; Castander, F. J. ^[17]; Crocce, M. ^[17]; Cunha, C. E. ^[18]; D’Andrea, C. B. ^[6]; da Costa, L. N. ^[14]; Davis, C. ^[18]; De Vicente, J. ^[19]; Desai, S. ^[20]; Doel, P. ^[1]; Eifler, T. F. ^[21]; Evrard, A. E. ^[22]; Flaugher, B. ^[11]; Fosalba, P. ^[17]; Frieman, J. ^[23]; García-Bellido, J. ^[24]; Gerdes, D. W. ^[22]; Gruen, D. ^[25]; Gruendl, R. A. ^[15]; Gschwend, J. ^[14]; Gutierrez, G. ^[11]; Hartley, W. G. ^[26]; Honscheid, K. ^[27]; Hoyle, B. ^[8]; James, D. J. ^[28]; Jarvis, M. ^[6]; Kuehn, K. ^[29]; Lima, M. ^[30]; Lin, H. ^[11]; March, M. ^[6]; Melchior, P. ^[31]; Menanteau, F. ^[15]; Miquel, R. ^[32]; Plazas, A. A. ^[33]; Reil, K. ^[34]; Roodman, A. ^[25]; Sanchez, E. ^[19]; Scarpine, V. ^[11]; Schubnell, M. ^[35]; Sevilla-Noarbe, I. ^[19]; Smith, M. ^[36]; Soares-Santos, M. ^[37]; Sobreira, F. ^[38]; Suchyta, E. ^[39]; Swanson, M. E. C. ^[40]; Tarle, G. ^[35]; Thomas, D. ^[41]; Walker, A. R. ^[10]

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1. Department of Physics & Astronomy, University College London, Gower Street, London, WC1E 6BT, UK
2. Department of Physics & Astronomy, University College London, Gower Street, London, WC1E 6BT, UK; Department of Physics and Electronics, Rhodes University, PO Box 94, Grahamstown, 6140, South Africa
3. McWilliams Center for Cosmology, Department of Physics, Carnegie Mellon University, Pittsburgh, PA 15213, USA
4. Laboratoire AIM, UMR CEA-CNRS-Paris 7, Irfu, SAp/SEDI, Service d’Astrophysique, CEA Saclay, 91191 Gif-sur-Yvette Cedex, France
5. Kavli Institute for Cosmological Physics, University of Chicago, Chicago, IL 60637, USA
6. Department of Physics and Astronomy, University of Pennsylvania, Philadelphia, PA 19104, USA
7. Department of Physics, ETH Zurich, Wolfgang-Pauli-Strasse 16, CH-8093 Zurich, Switzerland
8. Max Planck Institute for Extraterrestrial Physics, Giessenbachstrasse, 85748 Garching, Germany; Universitäts-Sternwarte, Fakultät für Physik, Ludwig-Maximilians Universität München, Scheinerstr. 1, 81679 München, Germany
9. Argonne National Laboratory, 9700 South Cass Avenue, Lemont, IL 60439, USA
10. Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, Casilla 603, La Serena, Chile
11. Fermi National Accelerator Laboratory, P. O. Box 500, Batavia, IL 60510, USA
12. Institute of Cosmology & Gravitation, University of Portsmouth, Portsmouth, PO1 3FX, UK; Instituto de Fisica Teorica UAM/CSIC, Universidad Autonoma de Madrid, 28049 Madrid, Spain
13. CNRS, UMR 7095, Institut d’Astrophysique de Paris, F-75014, Paris, France; Sorbonne Universités, UPMC Univ Paris 06, UMR 7095, Institut d’Astrophysique de Paris, F-75014, Paris, France
14. Laboratório Interinstitucional de e-Astronomia - LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ - 20921-400, Brazil; Observatório Nacional, Rua Gal. José Cristino 77, Rio de Janeiro, RJ - 20921-400, Brazil
15. Department of Astronomy, University of Illinois at Urbana-Champaign, 1002 W. Green Street, Urbana, IL 61801, USA; National Center for Supercomputing Applications, 1205 West Clark St., Urbana, IL 61801, USA
16. Institut de Física d’Altes Energies (IFAE), The Barcelona Institute of Science and Technology, Campus UAB, 08193 Bellaterra (Barcelona) Spain
17. Institut d’Estudis Espacials de Catalunya (IEEC), 08193 Barcelona, Spain; Institute of Space Sciences (ICE, CSIC), Campus UAB, Carrer de Can Magrans, s/n, 08193 Barcelona, Spain
18. Kavli Institute for Particle Astrophysics & Cosmology, P. O. Box 2450, Stanford University, Stanford, CA 94305, USA
19. Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), Madrid, Spain
20. Department of Physics, IIT Hyderabad, Kandi, Telangana 502285, India
21. Department of Astronomy/Steward Observatory, 933 North Cherry Avenue, Tucson, AZ 85721-0065, USA; Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Dr., Pasadena, CA 91109, USA
22. Department of Astronomy, University of Michigan, Ann Arbor, MI 48109, USA; Department of Physics, University of Michigan, Ann Arbor, MI 48109, USA
23. Fermi National Accelerator Laboratory, P. O. Box 500, Batavia, IL 60510, USA; Kavli Institute for Cosmological Physics, University of Chicago, Chicago, IL 60637, USA
24. Instituto de Fisica Teorica UAM/CSIC, Universidad Autonoma de Madrid, 28049 Madrid, Spain
25. Kavli Institute for Particle Astrophysics & Cosmology, P. O. Box 2450, Stanford University, Stanford, CA 94305, USA; SLAC National Accelerator Laboratory, Menlo Park, CA 94025, USA
26. Department of Physics & Astronomy, University College London, Gower Street, London, WC1E 6BT, UK; Department of Physics, ETH Zurich, Wolfgang-Pauli-Strasse 16, CH-8093 Zurich, Switzerland
27. Center for Cosmology and Astro-Particle Physics, The Ohio State University, Columbus, OH 43210, USA; Department of Physics, The Ohio State University, Columbus, OH 43210, USA
28. Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA
29. Australian Astronomical Observatory, North Ryde, NSW 2113, Australia
30. Departamento de Física Matemática, Instituto de Física, Universidade de São Paulo, CP 66318, São Paulo, SP, 05314-970, Brazil; Laboratório Interinstitucional de e-Astronomia - LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ - 20921-400, Brazil
31. Department of Astrophysical Sciences, Princeton University, Peyton Hall, Princeton, NJ 08544, USA
32. Institució Catalana de Recerca i Estudis Avançats, E-08010 Barcelona, Spain; Institut de Física d’Altes Energies (IFAE), The Barcelona Institute of Science and Technology, Campus UAB, 08193 Bellaterra (Barcelona) Spain
33. Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Dr., Pasadena, CA 91109, USA
34. SLAC National Accelerator Laboratory, Menlo Park, CA 94025, USA
35. Department of Physics, University of Michigan, Ann Arbor, MI 48109, USA
36. School of Physics and Astronomy, University of Southampton, Southampton, SO17 1BJ, UK
37. Fermi National Accelerator Laboratory, P. O. Box 500, Batavia, IL 60510, USA; Department of Physics, Brandeis University, Waltham, MA 02453, USA
38. Instituto de Física Gleb Wataghin, Universidade Estadual de Campinas, 13083-859, Campinas, SP, Brazil; Laboratório Interinstitucional de e-Astronomia - LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ - 20921-400, Brazil
39. Computer Science and Mathematics Division, Oak Ridge National Laboratory, Oak Ridge, TN 37831
40. National Center for Supercomputing Applications, 1205 West Clark St., Urbana, IL 61801, USA
41. Institute of Cosmology & Gravitation, University of Portsmouth, Portsmouth, PO1 3FX, UK

Mapping the underlying density field, including non-visible dark matter, using weak gravitational lensing measurements is now a standard tool in cosmology. Due to its importance to the science results of current and upcoming surveys, the quality of the convergence reconstruction methods should be well understood. We compare three methods: Kaiser–Squires (KS), Wiener filter, and Glimpse. Kaiser–Squires is a direct inversion, not accounting for survey masks or noise. The Wiener filter is well-motivated for Gaussian density fields in a Bayesian framework. Glimpse uses sparsity, aiming to reconstruct non-linearities in the density field. We compare these methods with several tests using public Dark Energy Survey (DES) Science Verification (SV) data and realistic DES simulations. The Wiener filter and Glimpse offer substantial improvements over smoothed Kaiser–Squires with a range of metrics. Both the Wiener filter and Glimpse convergence reconstructions show a 12 percent improvement in Pearson correlation with the underlying truth from simulations. To compare the mapping methods’ abilities to find mass peaks, we measure the difference between peak counts from simulated ΛCDM shear catalogues and catalogues with no mass fluctuations (a standard data vector when inferring cosmology from peak statistics); the maximum signal-to-noise of these peak statistics is increased by a factor of 3.5 for the Wiener filter and 9 for Glimpse. With simulations, we measure the reconstruction of the harmonic phases; the phase residuals’ concentration is improved 17 percent by Glimpse and 18 percent by the Wiener filter. The correlationbetween reconstructions from data and foreground redMaPPer clusters is increased 18 percent by the Wiener filter and 32 percent by Glimpse.

• Research Organization: SLAC National Accelerator Laboratory (SLAC), Menlo Park, CA (United States); Fermi National Accelerator Laboratory (FNAL), Batavia, IL (United States); Oak Ridge National Laboratory (ORNL), Oak Ridge, TN (United States)
• Sponsoring Organization: USDOE Office of Science (SC), High Energy Physics (HEP); USDOE Office of Science (SC), Advanced Scientific Computing Research (ASCR)
• Contributing Organization: DES Collaboration
• Grant/Contract Number: AC02-07CH11359; AC05-00OR22725
• OSTI ID: 1437399
• Alternate ID(s): OSTI ID: 1468024
• Report Number(s): FERMILAB-PUB-18-001-PPD; DES-2017-0309; arXiv:1801.08945; 1650958; TRN: US1900322
• Journal Information: Monthly Notices of the Royal Astronomical Society, Vol. 479, Issue 3; ISSN 0035-8711
• Publisher: Royal Astronomical Society
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTRONOMY AND ASTROPHYSICS