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Euclid preparation: XI. Mean redshift determination from galaxy redshift probabilities for cosmic shear tomography

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DOI

  • O. Ilbert, Aix-Marseille Université
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  • S. De La Torre, Aix-Marseille Université
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  • N. Martinet, Aix-Marseille Université
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  • A. H. Wright, Ruhr University Bochum
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  • S. Paltani, University of Geneva
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  • C. Laigle, Sorbonne Université
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  • I. Davidzon, Københavns Universitet
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  • E. Jullo, Aix-Marseille Université
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  • H. Hildebrandt, Ruhr University Bochum
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  • D. C. Masters, California Institute of Technology
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  • A. Amara, University of Portsmouth
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  • C. J. Conselice, Manchester University
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  • S. Andreon, Osservatorio Astronomico di Brera
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  • N. Auricchio, Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna
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  • R. Azzollini, University College London
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  • C. Baccigalupi, University of Trieste, International School for Advanced Studies, National Institute for Nuclear Physics, Osservatorio Astronomico di Trieste
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  • A. Balaguera-Antolinez, University of La Laguna, Instituto Astrofisico de Canarias
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  • M. Baldi, Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna, University of Bologna, National Institute for Nuclear Physics
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  • A. Balestra, Astronomical Observatory of Padua
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  • S. Bardelli, Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna
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  • R. Bender, Ludwig Maximilian University of Munich, Max Planck Institute for Extraterrestrial Physics
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  • A. Biviano, University of Trieste, Osservatorio Astronomico di Trieste
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  • C. Bodendorf, Max Planck Institute for Extraterrestrial Physics
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  • D. Bonino, National Institute for Astrophysics
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  • S. Borgani, University of Trieste, National Institute for Nuclear Physics, Osservatorio Astronomico di Trieste
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  • A. Boucaud, Université de Paris
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  • E. Bozzo, University of Geneva
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  • E. Branchini, National Institute for Nuclear Physics, Roma Tre University, Osservatorio Astronomico Roma
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  • M. Brescia, Osservatorio Astronomico di Capodimonte
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  • C. Burigana, National Institute for Nuclear Physics, University of Ferrara, Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna
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  • R. Cabanac, Université de Toulouse
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  • S. Camera, National Institute for Astrophysics, National Institute for Nuclear Physics, University of Turin
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  • V. Capobianco, National Institute for Astrophysics
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  • A. Cappi, Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna, Observatoire de la Cote d'Azur
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  • C. Carbone, Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna
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  • J. Carretero, Institute for High Energy Physics
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  • C. S. Carvalho, University of Lisbon
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  • S. Casas, Universite Paris-Saclay
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  • F. J. Castander, CSIC, Institute of Space Studies of Catalonia
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  • M. Castellano, Osservatorio Astronomico Roma
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  • G. Castignani, Swiss Federal Institute of Technology Lausanne
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  • S. Cavuoti, Osservatorio Astronomico di Capodimonte, University of Naples Federico II, National Institute for Nuclear Physics
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  • A. Cimatti, University of Bologna, Osservatorio Astrofisico Di Arcetri, Florence
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  • R. Cledassou, CNES Centre National d'Etudes Spatiales
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  • C. Colodro-Conde, Instituto Astrofisico de Canarias
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  • G. Congedo, University of Edinburgh
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  • L. Conversi, European Space Agency/ESRIN, European Space Astronomy Centre
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  • Y. Copin, Universite Claude Bernard Lyon 1
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  • L. Corcione, National Institute for Astrophysics
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  • A. Costille, Aix-Marseille Université
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  • J. Coupon, University of Geneva
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  • H. M. Courtois, Universite Claude Bernard Lyon 1
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  • M. Cropper, University College London
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  • J. Cuby, Aix-Marseille Université
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  • A. Da Silva, University of Lisbon
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  • H. Degaudenzi, University of Geneva
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  • D. Di Ferdinando, National Institute for Nuclear Physics
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  • F. Dubath, University of Geneva
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  • C. Duncan, University of Oxford
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  • X. Dupac, European Space Astronomy Centre
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  • S. Dusini, National Institute for Nuclear Physics
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  • A. Ealet, Universite Claude Bernard Lyon 1
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  • M. Fabricius, Ludwig Maximilian University of Munich, Max Planck Institute for Extraterrestrial Physics
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  • S. Farrens, Universite Paris-Saclay
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  • P. G. Ferreira, University of Oxford
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  • F. Finelli, Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna, National Institute for Nuclear Physics
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  • P. Fosalba, CSIC, Institute of Space Studies of Catalonia
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  • S. Fotopoulou, University of Bristol
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  • E. Franceschi, Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna
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  • P. Franzetti, Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna
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  • S. Galeotta, Osservatorio Astronomico di Trieste
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  • B. Garilli, Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna
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  • W. Gillard, Aix-Marseille Université
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  • B. Gillis, University of Edinburgh
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  • C. Giocoli, Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna, University of Bologna, National Institute for Nuclear Physics
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  • G. Gozaliasl, University of Helsinki
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  • J. Gracia-Carpio, Max Planck Institute for Extraterrestrial Physics
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  • F. Grupp, Ludwig Maximilian University of Munich, Max Planck Institute for Extraterrestrial Physics
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  • L. Guzzo, Osservatorio Astronomico di Brera, University of Milan, National Institute for Nuclear Physics
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  • S. V.H. Haugan, University of Oslo
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  • W. Holmes, Jet Propulsion Laboratory, California Institute of Technology
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  • F. Hormuth, von Hoerner & Sulger GmbH
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  • K. Jahnke, Max Planck Institute for Astronomy
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  • E. Keihanen, University of Helsinki
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  • S. Kermiche, Aix-Marseille Université
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  • A. Kiessling, Jet Propulsion Laboratory, California Institute of Technology
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  • C. C. Kirkpatrick, University of Helsinki
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  • M. Kunz, University of Geneva
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  • H. Kurki-Suonio, University of Helsinki
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  • S. Ligori, National Institute for Astrophysics
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  • P. B. Lilje, University of Oslo
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  • I. Lloro, ASTRON
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  • D. Maino, Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna, University of Milan, National Institute for Nuclear Physics
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  • E. Maiorano, Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna
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  • O. Marggraf, University of Bonn
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  • K. Markovic, Jet Propulsion Laboratory, California Institute of Technology
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  • F. Marulli, Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna, University of Bologna, National Institute for Nuclear Physics
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  • R. Massey, University of Durham
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  • M. Maturi, Heidelberg University 
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  • N. Mauri, University of Bologna, National Institute for Nuclear Physics
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  • S. Maurogordato, Observatoire de la Cote d'Azur
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  • H. J. McCracken, Sorbonne Université
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  • E. Medinaceli, Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna
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  • S. Mei, Université de Paris, PSL Research University
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  • R. Benton Metcalf, University of Bologna, Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna
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  • M. Moresco, Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna, University of Bologna
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  • B. Morin, Universite Paris-Saclay
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  • L. Moscardini, Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna, University of Bologna, National Institute for Nuclear Physics
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  • E. Munari, Osservatorio Astronomico di Trieste
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  • R. Nakajima, University of Bonn
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  • C. Neissner, Institute for High Energy Physics
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  • S. Niemi, University College London
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  • J. Nightingale, University of Durham
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  • C. Padilla, Institute for High Energy Physics
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  • F. Pasian, Osservatorio Astronomico di Trieste
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  • L. Patrizii, National Institute for Nuclear Physics
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  • K. Pedersen
  • R. Pello, Aix-Marseille Université
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  • V. Pettorino, Universite Paris-Saclay
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  • S. Pires, Universite Paris-Saclay
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  • G. Polenta, Italian Space Agency
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  • M. Poncet, CNES Centre National d'Etudes Spatiales
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  • L. Popa, Institute for Space Sciences
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  • D. Potter, University of Zurich
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  • L. Pozzetti, Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna
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  • F. Raison, Max Planck Institute for Extraterrestrial Physics
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  • A. Renzi, National Institute for Nuclear Physics, University of Padova
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  • J. Rhodes, Jet Propulsion Laboratory, California Institute of Technology
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  • G. Riccio, Osservatorio Astronomico di Capodimonte
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  • E. Romelli, Osservatorio Astronomico di Trieste
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  • M. Roncarelli, Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna, University of Bologna
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  • E. Rossetti, University of Bologna
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  • R. Saglia, Ludwig Maximilian University of Munich, Max Planck Institute for Extraterrestrial Physics
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  • A. G. Sanchez, Max Planck Institute for Extraterrestrial Physics
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  • D. Sapone, Universidad de Chile
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  • P. Schneider, University of Bonn
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  • T. Schrabback, University of Bonn
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  • V. Scottez, Sorbonne Université
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  • A. Secroun, Aix-Marseille Université
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  • G. Seidel, Max Planck Institute for Astronomy
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  • S. Serrano, CSIC, Institute of Space Studies of Catalonia
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  • C. Sirignano, National Institute for Nuclear Physics, University of Padova
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  • G. Sirri, National Institute for Nuclear Physics
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  • L. Stanco, National Institute for Nuclear Physics
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  • F. Sureau, Universite Paris-Saclay
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  • P. Tallada Crespa, CIEMAT
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  • M. Tenti, National Institute for Nuclear Physics
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  • H. I. Teplitz, California Institute of Technology
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  • I. Tereno, University of Lisbon
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  • R. Toledo-Moreo, Technical University of Cartagena. Spain
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  • F. Torradeflot, CIEMAT
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  • A. Tramacere, University of Geneva
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  • E. A. Valentijn, University of Groningen
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  • L. Valenziano, Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna, National Institute for Nuclear Physics
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  • J. Valiviita, University of Helsinki, University of Jyväskylä
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  • T. Vassallo, Ludwig Maximilian University of Munich
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  • Y. Wang, California Institute of Technology
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  • N. Welikala, University of Edinburgh
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  • J. Weller, Ludwig Maximilian University of Munich, Max Planck Institute for Extraterrestrial Physics
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  • L. Whittaker, Manchester University, University College London
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  • A. Zacchei, Osservatorio Astronomico di Trieste
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  • G. Zamorani, Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna
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  • J. Zoubian, Aix-Marseille Université
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  • E. Zucca, Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna

The analysis of weak gravitational lensing in wide-field imaging surveys is considered to be a major cosmological probe of dark energy. Our capacity to constrain the dark energy equation of state relies on an accurate knowledge of the galaxy mean redshift ⟨ z⟩. We investigate the possibility of measuring ⟨ z»with an accuracy better than 0.002(1  +  z) in ten tomographic bins spanning the redshift interval 0.2  <  z  <  2.2, the requirements for the cosmic shear analysis of Euclid. We implement a sufficiently realistic simulation in order to understand the advantages and complementarity, as well as the shortcomings, of two standard approaches: the direct calibration of ⟨ z»with a dedicated spectroscopic sample and the combination of the photometric redshift probability distribution functions (zPDFs) of individual galaxies. We base our study on the Horizon-AGN hydrodynamical simulation, which we analyse with a standard galaxy spectral energy distribution template-fitting code. Such a procedure produces photometric redshifts with realistic biases, precisions, and failure rates. We find that the current Euclid design for direct calibration is sufficiently robust to reach the requirement on the mean redshift, provided that the purity level of the spectroscopic sample is maintained at an extremely high level of > 99.8%. The zPDF approach can also be successful if the zPDF is de-biased using a spectroscopic training sample. This approach requires deep imaging data but is weakly sensitive to spectroscopic redshift failures in the training sample. We improve the de-biasing method and confirm our finding by applying it to real-world weak-lensing datasets (COSMOS and KiDS+VIKING-450).

OriginalsprogEngelsk
ArtikelnummerA117
TidsskriftAstronomy and Astrophysics
Vol/bind647
Antal sider21
ISSN0004-6361
DOI
StatusUdgivet - mar. 2021

Bibliografisk note

Publisher Copyright:
© Euclid Collaboration 2021.

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