<i>Euclid</i> preparation

We compared the performance of the flat-sky approximation and Limber approximation for the clustering analysis of the photometric galaxy catalogue of Euclid . We studied a 6-bin configuration, representing the first data release (DR1), and a 13-bin configuration, representing the third and final data release (DR3). We find that the Limber approximation is sufficiently accurate for the analysis of the wide bins of DR1. Instead, the 13 bins of DR3 cannot be modelled accurately with the Limber approximation. Instead, the flat-sky approximation is accurate to below 5% in recovering the angular power spectra of galaxy number counts in both cases and can be used to simplify the computation of the full power spectrum in harmonic space for the data analysis of DR3.

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Publication Details

Journal
Astronomy and Astrophysics
Published
2025-12-18
DOI
https://doi.org/10.1051/0004-6361/202557773
Primary Topic
Galaxies: Formation, Evolution, Phenomena
Type
article
Field-Weighted Citation Impact
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article

Euclid preparation

F Passalacqua, Lilian Blot, P. Tallada-Crespí, S Sacquegna et al.
Astronomy and Astrophysics
Galaxies: Formation, Evolution, Phenomena
article

Euclid preparation

F Passalacqua, Lilian Blot, P. Tallada-Crespí, S Sacquegna, O. Marggraf, G. Riccio, A. Pisani, J.-L. Starck, A. Amara, J. Martín-Fleitas, K. Pedersen, E Merlin, I Tereno, E. Gaztanaga, D. Sapone, G de Lucia, J. Weller, J. García-Bellido, G. Meylan, N. Martinet, G. Seidel, S Bardelli, E. Romelli, F. Marulli, S. Nadathur, A. Venhola, G. Sirri, C. Giocoli, M. Martinelli, E. Zucca, M. Baldi, P. Tallada-Crespí, S Dusini, S. Davini, X. Dupac, Carmencita David Padilla, H. Kurki-Suonio, Patrice Simon, J. F. Macías–Pérez, K. Ganga, D. Paoletti, A Renzi, G. Rodighiero, M. Viel, J.J Diaz, M. G. Lattanzi, E. Sellentin, G. Desprez, F Faustini, E Medinaceli, Daniele Bertacca, G. Maggio, M. Radovich, J Hjorth, L. Gabarra, F. Pasian, A. Navarro-Alsina, J Le Graet, M. Jhabvala, P. Schneider, A Enia, A Troja, C. Colodro-Conde, B. Joachimi, G. Leroy, S Bruton, M. Moresco, S. Paltani, B. R. Granett, T. Castro, S. Farrens, F Dubath, V. Scottez, N Auricchio, M. Poncet, G. Sirri, J. Carretero, A Kiessling, S Toft, Simon Conseil, N Tessore, D. Potter, M Ballardini, B Gillis, A. Da Silva, S Quai, A. Cimatti, J. Kim, I. Tutusaus, M Lembo, G. Morgante, B Sartoris, I Risso, R. Maoli, S. Marcin, F. Torradeflot, G. Mainetti, Fabio Lepori, S. Pires, S. Escoffier, S. Casas, K. George, William L. Matthewson, W. Gillard, M Sahlén, C. Kirkpatrick, E. Maiorano, Marco Bonici, R. B. Metcalf, K. M. George, Marcelo Farina, F. Raison, Sergey Kruk, M. Pöntinen, E. Sefusatti, Ruth Durrer, M. Béthermin, Chihiro Tao, K. Jahnkę, B. Altieri, A. Secroun, F. Hormuth, S. Camera, Ken Paterson, V. Kansal, S Anselmi, J. Weller, S. Ligori, M. Archidiacono, L. Legrand, Kogieleum Naidoo, F. Giacomini, C. Valieri, A. Zacchei, H. Degaudenzi, E. Franceschi, M Calabrese, L. Stanco, R Teyssier, R. Cabanac, Frank Grupp, V Capobianco, M. Miluzio, A. Cappi, G Cañas-Herrera, J. Gracia-Carpio, S. Mei, C Giocoli, R. Saglia, Z. Sakr, K Tanidis, K. Kiiveri, E. Bozzo, V. Pettorino, B. Morin, L. Conversi, G. Castignani, N. Mauri, T. Vassallo, E. Keihänen, E Branchini, S. Cavuoti, G. Gozaliasl, H. Dole, G Polenta, P. Bergamini, D. Vergani, Yongshui Kang, Shoubaneh Hemmati, Y Mellier, L. Corcione, J. Steinwagner, F Caro, E Sarpa, S. Ferriol, O. Mansutti, A Veropalumbo, M. Frailis, C. Burigana, M Brescia, S Nesseris, L. Patrizii, Y. Akrami, S. Kermiche, F. Atrio‐Barandela, A. Calabro, F. Cogato, D Sciotti, S. Tosi, Yang Wang, Yiming Fang, L. Maurin, Antonio Franco, D Karagiannis, G. Testera, Alessandra Silvestri, S Alvi, F. Gianotti, A Biviano, M. Magliocchetti, M. Roncarelli, M Kunz, V. Gautard, S.-M. Niemi, A. Grazian, A. Finoguenov, D. Maino, M. Tucci, F. Lacasa, M. Tenti, S Serrano, X. Dupac, M. Maturi, D. Di Ferdinando, A. Schneider, P Battaglia, G Congedo, C Porciani, L. Valenziano, F. Vernizzi, G. Zamorani, M. Wiesmann, R. Kohley, J. Rhodes, V. Lindholm, M. Fumana, G Morgante, B. Kubik, I. Lloro, S. Andreon, P Monaco, C. Hernández-Monteagudo, J Valiviita, M. Sereno, V. F. Cardone, A Mora, G Verza, W. N. Holmes, S. Borgani, J. Lesgourgues, C. Baccigalupi, F. Finelli, R. Rebolo
article en

Abstract

We compared the performance of the flat-sky approximation and Limber approximation for the clustering analysis of the photometric galaxy catalogue of Euclid . We studied a 6-bin configuration, representing the first data release (DR1), and a 13-bin configuration, representing the third and final data release (DR3). We find that the Limber approximation is sufficiently accurate for the analysis of the wide bins of DR1. Instead, the 13 bins of DR3 cannot be modelled accurately with the Limber approximation. Instead, the flat-sky approximation is accurate to below 5% in recovering the angular power spectra of galaxy number counts in both cases and can be used to simplify the computation of the full power spectrum in harmonic space for the data analysis of DR3.

Astronomy and AstrophysicsVol. 707
Université Claude Bernard Lyon 1 (FR), Institut polytechnique de Grenoble (FR), University of Geneva (CH), Institució Catalana de Recerca i Estudis Avançats (ES), Leiden University (NL), California Institute of Technology (US), University of Copenhagen (DK), Centre National de la Recherche Scientifique (FR), Goddard Space Flight Center (US), Université Libre de Bruxelles (BE), University of Hawaii System (US), Jet Propulsion Laboratory (US), Université Toulouse III - Paul Sabatier (FR), Consejo Superior de Investigaciones Científicas (ES), University of Bonn (DE), Scuola Internazionale Superiore di Studi Avanzati (IT), University of Padua (IT), University of Lisbon (PT), University of Salento (IT), University of Waterloo (CA), Universidad de La Laguna (ES), University of Groningen (NL), Université Fédérale de Toulouse Midi-Pyrénées (FR), Lyon College (US), Université Catholique de Lille (FR), Universidade do Porto (PT), Perimeter Institute (CA), Royal Holloway University of London (GB), University of Oslo (NO), Universidad de Salamanca (ES), Institute for High Energy Physics (ES), University of Milan (IT), Durham University (GB), Universität Innsbruck (AT), University of Saint Joseph (US), Princeton University (US), University of Ferrara (IT), University of Zurich (CH), University of California, Irvine (US), Université Paris Cité (FR), Aix-Marseille Université (FR), Heidelberg University (DE), University of Cambridge (GB), Commissariat à l'Énergie Atomique et aux Énergies Alternatives (FR), Université Paris Sciences et Lettres (FR), Université Paris-Saclay (FR), Centre National d'Études Spatiales (FR), Helsinki Institute of Physics (FI), Astronomical Observatory of Rome (IT), Korea Astronomy and Space Science Institute (KR), Trieste Astronomical Observatory (IT), Institut d'Astrophysique de Paris (FR), Astronomical Observatory of Capodimonte (IT), European Space Agency (FR), Laboratoire AstroParticule et Cosmologie (FR), Observatoire astronomique de Strasbourg (FR), Brera Astronomical Observatory (IT), University of Surrey (GB), FHNW University of Applied Sciences and Arts Northwestern Switzerland (CH), United Kingdom Space Agency (GB), Universidad Politécnica de Cartagena (ES), Sorbonne Université (FR), University of Oxford (GB), Park University (US), Osservatorio astronomico di Bologna (IT), Astrophysique, Instrumentation et Modélisation (FR), Institute of Astrophysics and Space Sciences (PT), ARC Centre of Excellence for Dark Matter Particle Physics (AU), Sorbonne Paris Cité (FR), Max Planck Institute for Extraterrestrial Physics (DE), Institut d'Estudis Espacials de Catalunya (ES), European Space Astronomy Centre (ES), Istituto Nazionale di Fisica Nucleare, Sezione di Lecce (IT), Istituto Nazionale di Fisica Nucleare, Sezione di Torino (IT), Institute for Space Astrophysics and Planetology (IT), Institut d'Astrophysique Spatiale (FR), Max Planck Institute for Astrophysics (DE), International University of Beirut (LB), Institut Català de Ciències del Clima (ES), Istituto Nazionale di Fisica Nucleare, Sezione di Padova (IT), Osservatorio Astrofisico di Torino (IT), Royal Observatory (GB), Istituto Nazionale di Fisica Nucleare, Sezione di Ferrara (IT), SKA Observatory (GB), Istituto Nazionale di Fisica Nucleare, Sezione di Napoli (IT), Centro de Astrofísica da Universidade do Porto (PT), Max Planck Institute for Astronomy (DE), Institute of Space Sciences (ES), Laboratoire de Physique Théorique (FR), DAWN Center for Independent Living (US), Centre for Theoretical Physics and Astrophysics (UZ), Istituto di Radioastronomia di Bologna (IT), Kavli Institute for the Physics and Mathematics of the Universe (JP), Federico II University Hospital (IT), Unidades Centrales Científico-Técnicas (ES), Mathematical Institute of the Slovak Academy of Sciences (SK), Institute of Astronomy (RU), FZU ‒ Institute of Physics of the Academy of Sciences of the Czech Republic (CZ), Collurania Teramo Observatory (IT), Institute of Theoretical Physics (CN), Istituto Nazionale di Fisica Nucleare, Sezione di Genova (IT), Observatoire de la Côte d’Azur (FR), CEA Paris-Saclay (FR), Naples Anesthesia & Physician Associates (US), Instituto de Astrofísica de Canarias (ES), Felix Scholarship (GB), Institut National de Physique Nucléaire et de Physique des Particules (FR), Astronomical Institute of the Slovak Academy of Sciences (SK), Istituto Nazionale di Fisica Nucleare, Sezione di Milano (IT), Institute of Space Science - INFLPR Subsidiary (RO), Computing Center (RU), Centre de Calcul de l’Institut National de Physique Nucléaire et de Physique des Particules (FR), Osservatorio Astronomico della Regione Autonoma Valle d'Aosta (IT), Astronomy and Space (AU), Istituto Nazionale di Fisica Nucleare, Sezione di Bologna (IT), Port d'Informació Científica (ES), Istituto Nazionale di Fisica Nucleare, Sezione di Trieste (IT), Institute for Fundamental Physics of the Universe (IT), Instituto de Física de Cantabria (ES), Flatiron Health (United States) (US), Astronomical Observatory (RS), St. Joseph Medical Center (US), Istituto Nazionale di Fisica Nucleare, Sezione di Roma I (IT), Osservatorio Astronomico di Padova (IT), Institut de Physique Théorique (FR), European Space Research Institute (IT), Institut de Recherche sur les Lois Fondamentales de l'Univers (FR), Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (ES), Institut de Recherche en Astrophysique et Planétologie (FR), Infrared Processing and Analysis Center (US), Osservatorio di Astrofisica e Scienza dello Spazio, Flatiron Institute (US), European Space Research and Technology Centre (NL), University College London (GB), École Polytechnique Fédérale de Lausanne (CH), University of Turin (IT), Swinburne University of Technology (AU), Case Western Reserve University (US), Technical University of Munich (DE), University of Portsmouth (GB), University of Chile (CL), Heidelberg Institute for Theoretical Studies (DE), Ludwig-Maximilians-Universität München (DE), University of Genoa (IT), Sapienza University of Rome (IT), University of the Western Cape (ZA), National Institute for Astrophysics (IT), RWTH Aachen University (DE), Université Grenoble Alpes (FR), University of Bologna (IT), Technical University of Denmark (DK), University of Edinburgh (GB), Aalto University (FI)
Openalex Percentile: Top 72%
Galaxies: Formation, Evolution, Phenomena
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