Phenotypic redshifts with self-organizing maps: A novel method to characterize redshift distributions of source galaxies for weak lensing
Romain BuchsInstitute of Science, Technology, and Policy, ETH Zurich, Universitätstrasse 41, CH-8092 Zurich, SwitzerlandC. DavisDescartes Labs, Inc., 100 N Guadelupe St, Santa Fe, NM 87501, USAD. GruenDepartment of Physics, Stanford University, 382 Via Pueblo Mall, Stanford, CA 94305, USAJoseph DeRoseDepartment of Physics, Stanford University, 382 Via Pueblo Mall, Stanford, CA 94305, USAA. AlarconInstitut d’Estudis Espacials de Catalunya (IEEC), E-08034 Barcelona, SpainG. M. BernsteinDepartment of Physics and Astronomy, University of Pennsylvania, Philadelphia, PA 19104, USAC. SánchezDepartment of Physics and Astronomy, University of Pennsylvania, Philadelphia, PA 19104, USAJ. MylesDepartment of Physics, Stanford University, 382 Via Pueblo Mall, Stanford, CA 94305, USAA. RoodmanKavli Institute for Particle Astrophysics and Cosmology, P. O. Box 2450, Stanford University, Stanford, CA 94305, USAS. W. AllenDepartment of Physics, Stanford University, 382 Via Pueblo Mall, Stanford, CA 94305, USAA. AmonKavli Institute for Particle Astrophysics and Cosmology, P. O. Box 2450, Stanford University, Stanford, CA 94305, USAA. ChoiCenter for Cosmology and Astro-Particle Physics, The Ohio State University, Columbus, OH 43210, USADaniel MastersInfrared Processing and Analysis Center, Pasadena, CA 91125, USAR. MiquelInstitució Catalana de Recerca i Estudis Avançats, E-08010 Barcelona, SpainM. A. TroxelDepartment of Physics, Duke University Durham, NC 27708, USAR.H. WechslerDepartment of Physics, Stanford University, 382 Via Pueblo Mall, Stanford, CA 94305, USAT. M. C. AbbottCerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, Casilla 603, La Serena, ChileJ. AnnisFermi National Accelerator Laboratory, P. O. Box 500, Batavia, IL 60510, USAS. ÀvilaInstitute of Cosmology and Gravitation, University of Portsmouth, Portsmouth PO1 3FX, UKK. BechtolLSST, 933 North Cherry Avenue, Tucson, AZ 85721, USAS. L. BridleJodrell Bank Center for Astrophysics, School of Physics and Astronomy, University of Manchester, Oxford Road, Manchester M13 9PL, UKDavid BrooksDepartment of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UKE. Buckley‐GeerFermi National Accelerator Laboratory, P. O. Box 500, Batavia, IL 60510, USAD. L. BurkeKavli Institute for Particle Astrophysics and Cosmology, P. O. Box 2450, Stanford University, Stanford, CA 94305, USAA. Carnero RosellCentro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, SpainM. Carrasco KindDepartment of Astronomy, University of Illinois at Urbana-Champaign, 1002 W, Green Street, Urbana, IL 61801, USAJ. CarreteroInstitut de Física d’Altes Energies (IFAE), The Barcelona Institute of Science and Technology, Campus UAB, E-08193 Bellaterra (Barcelona), SpainF. J. CastanderInstitut d’Estudis Espacials de Catalunya (IEEC), E-08034 Barcelona, SpainR. CawthonPhysics Department, 2320 Chamberlin Hall, University of Wisconsin-Madison, 1150 University Avenue Madison, WI 53706, USAC. B. D’AndreaDepartment of Physics and Astronomy, University of Pennsylvania, Philadelphia, PA 19104, USAL. N. da CostaLaboratório Interinstitucional de e-Astronomia - LIneA, Rua Gal. José Cristino 77, Rio de Janeiro RJ - 20921-400, BrazilJ. De VicenteCentro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, SpainS. DesaiDepartment of Physics, IIT Hyderabad, Kandi, Telangana 502285, IndiaH. T. DiehlFermi National Accelerator Laboratory, P. O. Box 500, Batavia, IL 60510, USAP. DoelDepartment of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UKA. Drlica-WagnerFermi National Accelerator Laboratory, P. O. Box 500, Batavia, IL 60510, USAT. F. EiflerDepartment of Astronomy/Steward Observatory, 933 North Cherry Avenue, Tucson, AZ 85721-0065, USAA. E. EvrardDepartment of Astronomy, University of Michigan, Ann Arbor, MI 48109, USAB. FlaugherFermi National Accelerator Laboratory, P. O. Box 500, Batavia, IL 60510, USAP. FosalbaInstitut d’Estudis Espacials de Catalunya (IEEC), E-08034 Barcelona, SpainJ. FriemanFermi National Accelerator Laboratory, P. O. Box 500, Batavia, IL 60510, USAJ. García-BellidoInstituto de Fisica Teorica UAM/CSIC, Universidad Autonoma de Madrid, E-8049 Madrid, SpainE. GaztañagaInstitut d’Estudis Espacials de Catalunya (IEEC), E-08034 Barcelona, SpainR. A. GruendlDepartment of Astronomy, University of Illinois at Urbana-Champaign, 1002 W, Green Street, Urbana, IL 61801, USAJ. GschwendLaboratório Interinstitucional de e-Astronomia - LIneA, Rua Gal. José Cristino 77, Rio de Janeiro RJ - 20921-400, BrazilG. GutiérrezFermi National Accelerator Laboratory, P. O. Box 500, Batavia, IL 60510, USAW G HartleyDepartment of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UKD L HollowoodK. HonscheidCenter for Cosmology and Astro-Particle Physics, The Ohio State University, Columbus, OH 43210, USAD. J. JamesCenter for Astrophysics, Harvard and Smithsonian, 60 Garden Street, MS 42, Cambridge, MA 02138, USAK. KuehnAustralian Astronomical Optics, Macquarie University, North Ryde, NSW 2113, AustraliaN. KuropatkinFermi National Accelerator Laboratory, P. O. Box 500, Batavia, IL 60510, USAM. LimaDepartamento de Física Matemática, Instituto de Física, Universidade de São Paulo, CP 66318, São Paulo, SP 05314-970, BrazilH. LinFermi National Accelerator Laboratory, P. O. Box 500, Batavia, IL 60510, USAM. A. G. MaiaLaboratório Interinstitucional de e-Astronomia - LIneA, Rua Gal. José Cristino 77, Rio de Janeiro RJ - 20921-400, BrazilM. MarchDepartment of Physics and Astronomy, University of Pennsylvania, Philadelphia, PA 19104, USAJ. L. MarshallGeorge P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, and Department of Physics and Astronomy, Texas A&M University, College Station, TX 77843, USAP. MelchiorDepartment of Astrophysical Sciences, Princeton University, Peyton Hall, Princeton, NJ 08544, USAF. MenanteauDepartment of Astronomy, University of Illinois at Urbana-Champaign, 1002 W, Green Street, Urbana, IL 61801, USAR. L. C. OgandoLaboratório Interinstitucional de e-Astronomia - LIneA, Rua Gal. José Cristino 77, Rio de Janeiro RJ - 20921-400, BrazilA A PlazasDepartment of Astrophysical Sciences, Princeton University, Peyton Hall, Princeton, NJ 08544, USAE. S. RykoffKavli Institute for Particle Astrophysics and Cosmology, P. O. Box 2450, Stanford University, Stanford, CA 94305, USAE. SánchezCentro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, SpainV. ScarpineFermi National Accelerator Laboratory, P. O. Box 500, Batavia, IL 60510, USAS. SerranoInstitut d’Estudis Espacials de Catalunya (IEEC), E-08034 Barcelona, SpainI. Sevilla-NoarbeCentro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, SpainM. SmithSchool of Physics and Astronomy, University of Southampton, Southampton SO17 1BJ, UKM. Soares-SantosPhysics Department, Brandeis University, 415 South Street, Waltham, MA 02453, USAF. SobreiraInstituto de Física Gleb Wataghin, Universidade Estadual de Campinas, 13083-859 Campinas, SP, BrazilE. SuchytaComputer Science and Mathematics Division, Oak Ridge National Laboratory, Oak Ridge, TN 37831, USAM. E. C. SwansonNational Center for Supercomputing Applications, 1205 West Clark St., Urbana, IL 61801, USAG. TarléDepartment of Physics, University of Michigan, Ann Arbor, MI 48109, USAD. ThomasInstitute of Cosmology and Gravitation, University of Portsmouth, Portsmouth PO1 3FX, UKV. VikramArgonne National Laboratory, 9700 South Cass Avenue, Lemont, IL 60439, USA
2019en
ABI
Аннотация
ABSTRACT Wide-field imaging surveys such as the Dark Energy Survey (DES) rely on coarse measurements of spectral energy distributions in a few filters to estimate the redshift distribution of source galaxies. In this regime, sample variance, shot noise, and selection effects limit the attainable accuracy of redshift calibration and thus of cosmological constraints. We present a new method to combine wide-field, few-filter measurements with catalogues from deep fields with additional filters and sufficiently low photometric noise to break degeneracies in photometric redshifts. The multiband deep field is used as an intermediary between wide-field observations and accurate redshifts, greatly reducing sample variance, shot noise, and selection effects. Our implementation of the method uses self-organizing maps to group galaxies into phenotypes based on their observed fluxes, and is tested using a mock DES catalogue created from N-body simulations. It yields a typical uncertainty on the mean redshift in each of five tomographic bins for an idealized simulation of the DES Year 3 weak-lensing tomographic analysis of σΔz = 0.007, which is a 60 per cent improvement compared to the Year 1 analysis. Although the implementation of the method is tailored to DES, its formalism can be applied to other large photometric surveys with a similar observing strategy.
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