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Euclid: VI. NISP-P optical ghosts

  • K. Paterson*
  • , M. Schirmer
  • , K. Okumura
  • , B. Venemans
  • , K. Jahnke
  • , N. Aghanim
  • , B. Altieri
  • , A. Amara
  • , S. Andreon
  • , C. Baccigalupi
  • , M. Baldi
  • , A. Balestra
  • , S. Bardelli
  • , P. Battaglia
  • , A. Biviano
  • , A. Bonchi
  • , E. Branchini
  • , M. Brescia
  • , J. Brinchmann
  • , S. Camera
  • G. Cañas-Herrera, V. Capobianco, J. Carretero, S. Casas, M. Castellano, G. Castignani, S. Cavuoti, K. C. Chambers, A. Cimatti, C. Colodro-Conde, G. Congedo, C. J. Conselice, L. Conversi, Y. Copin, F. Courbin, H. M. Courtois, A. Da Silva, R. Da Silva, H. Degaudenzi, G. De Lucia, A. M. Di Giorgio, J. Dinis, H. Dole, F. Dubath, X. Dupac, S. Dusini, A. Ealet, S. Escoffier, M. Farina, R. Farinelli, F. Faustini, S. Ferriol, F. Finelli, S. Fotopoulou, N. Fourmanoit, M. Frailis, E. Franceschi, P. Franzetti, S. Galeotta, K. George, W. Gillard, B. Gillis, C. Giocoli, J. Gracia-Carpio, B. R. Granett, A. Grazian, F. Grupp, L. Guzzo, S. V.H. Haugan, H. Hoekstra, W. Holmes, F. Hormuth, A. Hornstrup, P. Hudelot, M. Jhabvala, E. Keihänen, S. Kermiche, A. Kiessling, R. Kohley, B. Kubik, M. Kümmel, M. Kunz, H. Kurki-Suonio, A. M.C. Le Brun, D. Le Mignant, S. Ligori, P. B. Lilje, V. Lindholm, I. Lloro, G. Mainetti, D. Maino, E. Maiorano, O. Mansutti, S. Marcin, O. Marggraf, K. Markovic, M. Martinelli, N. Martinet, F. Marulli, R. Massey, H. J. Mccracken, E. Medinaceli, S. Mei, M. Meneghetti, E. Merlin, G. Meylan, A. Mora, M. Moresco, L. Moscardini, R. Nakajima, C. Neissner, R. C. Nichol, S. M. Niemi, J. W. Nightingale, C. Padilla, S. Paltani, F. Pasian, K. Pedersen, W. J. Percival, V. Pettorino, S. Pires, G. Polenta, M. Poncet, L. A. Popa, L. Pozzetti, F. Raison, R. Rebolo, A. Renzi, J. Rhodes, G. Riccio, E. Romelli, M. Roncarelli, E. Rossetti, R. Saglia, Z. Sakr, A. G. Sánchez, D. Sapone, B. Sartoris, J. A. Schewtschenko, P. Schneider, T. Schrabback, A. Secroun, E. Sefusatti, G. Seidel, M. Seiffert, S. Serrano, P. Simon, C. Sirignano, G. Sirri, L. Stanco, J. Steinwagner, P. Tallada-Crespí, D. Tavagnacco, A. N. Taylor, I. Tereno, S. Toft, R. Toledo-Moreo, F. Torradeflot, I. Tutusaus, L. Valenziano, J. Valiviita, T. Vassallo, G. Verdoes Kleijn, A. Veropalumbo, Y. Wang, J. Weller, A. Zacchei, G. Zamorani, I. A. Zinchenko, E. Zucca, V. Allevato, M. Ballardini, M. Bolzonella, E. Bozzo, C. Burigana, R. Cabanac, M. Calabrese, P. Casenove, D. Di Ferdinando, J. A.Escartin Vigo, L. Gabarra, S. Matthew, N. Mauri, R. B. Metcalf, A. A. Nucita, A. Pezzotta, M. Pöntinen, C. Porciani, V. Scottez, M. Tenti, M. Viel, M. Wiesmann, Y. Akrami, I. T. Andika, S. Anselmi, M. Archidiacono, F. Atrio-Barandela, D. Bertacca, M. Bethermin, A. Blanchard, L. Blot, S. Borgani, M. L. Brown, S. Bruton, A. Calabro, A. Cappi, F. Caro, C. S. Carvalho, T. Castro, R. Chary, F. Cogato, S. Conseil, A. R. Cooray, O. Cucciati, S. Davini, F. De Paolis, G. Desprez, A. Díaz-Sánchez, S. Di Domizio, J. M. Diego, P. Dimauro, A. Enia, Y. Fang, A. M.N. Ferguson, A. G. Ferrari, A. Finoguenov, A. Franco, K. Ganga, J. García-Bellido, T. Gasparetto, V. Gautard, E. Gaztanaga, F. Giacomini, F. Gianotti, G. Gozaliasl, A. Gregorio, M. Guidi, C. M. Gutierrez, A. Hall, W. G. Hartley, S. Hemmati, C. Hernández-Monteagudo, H. Hildebrandt, J. Hjorth, J. J.E. Kajava, Y. Kang, V. Kansal, D. Karagiannis, K. Kiiveri, C. C. Kirkpatrick, S. Kruk, J. Le Graet, L. Legrand, M. Lembo, F. Lepori, G. Leroy, J. Lesgourgues, L. Leuzzi, T. I. Liaudat, S. J. Liu, A. Loureiro, J. Macias-Perez, G. Maggio, M. Magliocchetti, F. Mannucci, R. Maoli, J. Martín-Fleitas, C. J.A.P. Martins, L. Maurin, M. Miluzio, P. Monaco, A. Montoro, C. Moretti, G. Morgante, S. Nadathur, K. Naidoo, P. Natoli, A. Navarro-Alsina, S. Nesseris, F. Passalacqua, L. Patrizii, A. Pisani, D. Potter, S. Quai, M. Radovich, P. Reimberg, I. Risso, S. Sacquegna, M. Sahlén, E. Sarpa, A. Schneider, M. Schultheis, D. Sciotti, E. Sellentin, M. Sereno, A. Shulevski, L. C. Smith, J. Stadel, K. Tanidis, C. Tao, G. Testera, R. Teyssier, S. Tosi, A. Troja, M. Tucci, C. Valieri, A. Venhola, D. Vergani, G. Verza, P. Vielzeuf, N. A. Walton
*Corresponding author for this work
  • Max Planck Institute for Astronomy
  • Institut de recherche sur les lois fondamentales de l'Univers
  • Leiden University
  • Université Paris-Sud
  • European Space Astronomy Centre
  • University of Surrey
  • Osservatorio Astronomico di Brera
  • University of Trieste
  • University of Bologna
  • Astronomical Observatory of Padua
  • Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna
  • Italian Space Agency
  • University of Naples Federico II
  • University of Porto
  • University of Turin
  • ESTEC
  • National Institute for Astrophysics
  • CIEMAT
  • RWTH Aachen University
  • Osservatorio Astronomico Roma
  • Osservatorio Astronomico di Capodimonte
  • University of Hawai'i at Mānoa
  • Instituto de Astrofísica de Canarias
  • University of Edinburgh
  • University of Manchester
  • European Space Agency/ESRIN
  • Universite Claude Bernard Lyon 1
  • ICREA
  • Institut national de physique nucléaire et de physique des particules
  • University of Lisbon
  • University of Geneva
  • Osservatorio Astronomico di Trieste
  • National Institute for Nuclear Physics
  • CNRS
  • University of Bristol
  • Ludwig Maximilian University of Munich
  • Max Planck Institute for Extraterrestrial Physics
  • University of Oslo
  • California Institute of Technology
  • Felix Hormuth Engineering
  • Institut d’Astrophysique de Paris
  • NASA Goddard Space Flight Center
  • University of Helsinki
  • Observatoire de Paris
  • SKA Organisation
  • University of Milan
  • University of Applied Sciences Northwestern Switzerland
  • University of Bonn
  • Durham University
  • Centre Pierre Binétruy
  • European Space Agency - ESA
  • Institute for High Energy Physics
  • Newcastle University
  • University of Copenhagen
  • University of Waterloo
  • French Alternative Energies and Atomic Energy Commission
  • Centre national d'études spatiales
  • Heidelberg University 
  • Universidad de Chile
  • University of Innsbruck
  • Institute of Space Studies of Catalonia
  • University of Padua
  • Technical University of Cartagena
  • Université de Toulouse
  • University of Groningen
  • University of Oxford
  • University of Salento
  • CSIC-UAM - Institute of Theoretical Physics
  • Technical University of Munich
  • Universidad de Salamanca
  • Université de Strasbourg
  • ICSC - Centro Nazionale di Ricerca in High Performance Computing
  • University of California at Irvine
  • CSIC-UC - Institute of Physics of Cantabria
  • Université Paris 7
  • University of Portsmouth
  • Aalto University
  • University of La Laguna
  • Ruhr University Bochum
  • Swinburne University of Technology
  • University of Ferrara
  • University of Cambridge
  • University of Zurich
  • Université Paris-Saclay
  • Imperial College London
  • Université Grenoble Alpes
  • Osservatorio Astrofisico Di Arcetri, Florence
  • University of Rome La Sapienza
  • CSIC - Institute of Space Sciences
  • Uppsala University
  • International School for Advanced Studies
  • Université Côte d'Azur
  • Princeton University
  • University of Genoa
  • University of Oulu
  • Simons Foundation

Research output: Contribution to journal › Journal article › Research › peer-review

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Abstract

The Near-Infrared Spectrometer and Photometer (NISP) on board Euclid includes several optical elements in its path that introduce artefacts into the data from non-nominal light paths. To ensure uncontaminated source photometry, these artefacts must be accurately accounted for. This paper focuses on two specific optical features in NISP's photometric data (NISP-P): ghosts caused by the telescope's dichroic beamsplitter, and the bandpass filters within the NISP fore-optics. Both ghost types exhibit a characteristic morphology and are offset from the originating stars. The offsets are well modelled using 2D polynomials; only stars brighter than approximately 10 magnitudes in each filter produce significant ghost contributions. The masking radii for these ghosts depend on both the source-star brightness and the filter wavelength, ranging from 20 to 40 pixels. We present the final relations and models used in the near-infrared (NIR) processing function (PF) to mask these ghosts for Euclid's Quick Data Release (Q1).

Original languageEnglish
Article numberA226
JournalAstronomy and Astrophysics
Volume707
Number of pages13
ISSN0004-6361
DOIs
Publication statusPublished - 2026

Keywords

  • Instrumentation: photometers
  • Space vehicles: instruments

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