Dark Energy Survey Year 1 results: validation of weak lensing cluster member contamination estimates from P(z) decomposition
T N VargaFakultät für Physik, Universitäts-Sternwarte, Ludwig−Maximilians Universität München, Scheinerstr. 1, D-81679 München, GermanyJoseph DeRoseDepartment of Physics, Stanford University, 382 Via Pueblo Mall, Stanford, CA 94305, USAD. GruenDepartment of Physics, Stanford University, 382 Via Pueblo Mall, Stanford, CA 94305, USAThomas McClintockBrookhaven National Laboratory, Bldg 510, Upton, NY 11973, USAS. SeitzFakultät für Physik, Universitäts-Sternwarte, Ludwig−Maximilians Universität München, Scheinerstr. 1, D-81679 München, GermanyEduardo RozoDepartment of Physics, University of Arizona, Tucson, AZ 85721, USAM. CostanziFakultät für Physik, Universitäts-Sternwarte, Ludwig−Maximilians Universität München, Scheinerstr. 1, D-81679 München, GermanyB. HoyleFakultät für Physik, Universitäts-Sternwarte, Ludwig−Maximilians Universität München, Scheinerstr. 1, D-81679 München, GermanyN. MacCrannCenter for Cosmology and Astro-Particle Physics, The Ohio State University, Columbus, OH 43210, USAA A PlazasDepartment of Astrophysical Sciences, Princeton University, 4 Ivy Lane, Princeton, NJ 08544, USAE. S. RykoffKavli Institute for Particle Astrophysics and Cosmology, PO Box 2450, Stanford University, Stanford, CA 94305, USAMelanie SimetJet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Dr., Pasadena, CA 91109, USAA von der LindenDepartment of Physics and Astronomy, Stony Brook University, Stony Brook, NY 11794, USAR.H. WechslerDepartment of Physics, Stanford University, 382 Via Pueblo Mall, Stanford, CA 94305, USAJ. AnnisFermi National Accelerator Laboratory, PO Box 500, Batavia, IL 60510, USAS. ÀvilaInstitute of Cosmology and Gravitation, University of Portsmouth, Portsmouth PO1 3FX, UKE. BertinCNRS, UMR 7095, Institut d’Astrophysique de Paris, F-75014, Paris, FranceDavid BrooksDepartment of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UKE. Buckley‐GeerFermi National Accelerator Laboratory, PO Box 500, Batavia, IL 60510, USAD. L. BurkeKavli Institute for Particle Astrophysics and Cosmology, PO Box 2450, Stanford University, Stanford, CA 94305, USAA. Carnero RosellCentro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), 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) SpainC. E. CunhaKavli Institute for Particle Astrophysics and Cosmology, PO Box 2450, Stanford University, Stanford, CA 94305, 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), Madrid, SpainS. DesaiDepartment of Physics, IIT Hyderabad, Kandi, Telangana 502285, IndiaH. T. DiehlFermi National Accelerator Laboratory, PO Box 500, Batavia, IL 60510, USAJ. P. DietrichExcellence Cluster Universe, Boltzmannstr. 2, D-85748 Garching, GermanyP. DoelDepartment of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UKA. E. EvrardDepartment of Astronomy, University of Michigan, Ann Arbor, MI 48109, USAB. FlaugherFermi National Accelerator Laboratory, PO Box 500, Batavia, IL 60510, USAP. FosalbaInstitut d’Estudis Espacials de Catalunya (IEEC), E-08034 Barcelona, SpainJ. FriemanFermi National Accelerator Laboratory, PO Box 500, Batavia, IL 60510, USAJ. García-BellidoInstituto de Fisica Teorica UAM/CSIC, Universidad Autonoma de Madrid, E-28049 Madrid, SpainE. GaztañagaInstitut d’Estudis Espacials de Catalunya (IEEC), E-08034 Barcelona, SpainD. W. GerdesDepartment of Astronomy, University of Michigan, Ann Arbor, MI 48109, USAR. 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, PO Box 500, Batavia, IL 60510, USAW G HartleyDepartment of Physics, ETH Zurich, Wolfgang-Pauli-Strasse 16, CH-8093 Zurich, SwitzerlandD L HollowoodK. HonscheidCenter for Cosmology and Astro-Particle Physics, The Ohio State University, Columbus, OH 43210, USAD. J. JamesHarvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USAT. JeltemaK. KuehnAustralian Astronomical Optics, Macquarie University, North Ryde, NSW 2113, AustraliaN. KuropatkinFermi National Accelerator Laboratory, PO Box 500, Batavia, IL 60510, USAM. LimaDepartamento de Física Matemática, Instituto de Física, Universidade de São Paulo, CP 66318, São Paulo, SP 05314-970, BrazilM. 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, USAC. J. MillerDepartment of Astronomy, University of Michigan, Ann Arbor, MI 48109, USAR. MiquelInstitució Catalana de Recerca i Estudis Avançats, E-08010 Barcelona, SpainR. L. C. OgandoLaboratório Interinstitucional de e-Astronomia - LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ - 20921-400, BrazilA. K. RomerDepartment of Physics and Astronomy, Pevensey Building, University of Sussex, Brighton BN1 9QH, UKE. SánchezCentro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), Madrid, SpainV. ScarpineFermi National Accelerator Laboratory, PO Box 500, Batavia, IL 60510, USAM. SchubnellDepartment of Physics, University of Michigan, Ann Arbor, MI 48109, USAS. SerranoInstitut d’Estudis Espacials de Catalunya (IEEC), E-08034 Barcelona, SpainI. Sevilla-NoarbeCentro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), Madrid, SpainM. SmithSchool of Physics and Astronomy, University of Southampton, Southampton SO17 1BJ, UKF. SobreiraInstituto de Física Gleb Wataghin, Universidade Estadual de Campinas, SP 13083-859 Campinas, 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, UKD. L. TuckerFermi National Accelerator Laboratory, PO Box 500, Batavia, IL 60510, USAY. ZhangFermi National Accelerator Laboratory, PO Box 500, Batavia, IL 60510, USA
2019en
ABI
Аннотация
ABSTRACT Weak lensing source galaxy catalogues used in estimating the masses of galaxy clusters can be heavily contaminated by cluster members, prohibiting accurate mass calibration. In this study, we test the performance of an estimator for the extent of cluster member contamination based on decomposing the photometric redshift P(z) of source galaxies into contaminating and background components. We perform a full scale mock analysis on a simulated sky survey approximately mirroring the observational properties of the Dark Energy Survey Year One observations (DES Y1), and find excellent agreement between the true number profile of contaminating cluster member galaxies in the simulation and the estimated one. We further apply the method to estimate the cluster member contamination for the DES Y1 redMaPPer cluster mass calibration analysis, and compare the results to an alternative approach based on the angular correlation of weak lensing source galaxies. We find indications that the correlation based estimates are biased by the selection of the weak lensing sources in the cluster vicinity, which does not strongly impact the P(z) decomposition method. Collectively, these benchmarks demonstrate the strength of the P(z) decomposition method in alleviating membership contamination and enabling highly accurate cluster weak lensing studies without broad exclusion of source galaxies, thereby improving the total constraining power of cluster mass calibration via weak lensing.
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