<i>Euclid</i> preparation

Local Universe dwarf galaxies can serve as both cosmological and mass assembly probes. Deep surveys have enabled the study of these objects down to the low surface brightness (LSB) regime. In this paper, we estimate Euclid ’s dwarf detection capabilities as well as limits of its MERge processing function (MER pipeline), which is responsible for producing the stacked mosaics and final catalogues. To do this, we injected mock dwarf galaxies in a real Euclid Wide Survey (EWS) field in the VIS band and compared the input catalogue to the final MER catalogue. The mock dwarf galaxies were generated using simple Sérsic models with structural parameters (including size and surface brightness) drawn from observed dwarf galaxy catalogues. These simulations represent an idealised case in the sense they do not account for additional factors such as ellipticity, morphology, or crowding. To characterise the detected dwarfs, we used the mean surface brightness inside the effective radius SB e (in mag arcsec −2 ). The final MER catalogues achieve a completenesses of 91% for SB e ∈ [21, 24] and 54% for SB e ∈ [24, 28]. These numbers do not take into account possible contaminants, including confusion with background galaxies at the location of the dwarfs. After taking those effects into account, they respectively became 86% and 38%. The MER pipeline performs a final local background subtraction with a small mesh size, leading to a flux loss for galaxies with R e &gt; 10″. By using the final MER mosaics and reinjecting this local background, we obtained an image in which we recover reliable photometric properties for objects under the arcminute scale. This background-reinjected product is thus suitable for the study of Local Universe dwarf galaxies. Euclid ’s data reduction pipeline serves as a test bed for other deep surveys, particularly regarding background subtraction methods, a key issue in LSB science.

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Publication Details

Journal
Astronomy and Astrophysics
Published
2025-11-14
DOI
https://doi.org/10.1051/0004-6361/202557270
Primary Topic
Galaxies: Formation, Evolution, Phenomena
Type
article
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article

Euclid preparation

R. Laureijs, L. K. Hunt, G. Seidel, M. Roncarelli et al.
Astronomy and Astrophysics
Galaxies: Formation, Evolution, Phenomena
article

Euclid preparation

R. Laureijs, L. K. Hunt, G. Seidel, M. Roncarelli, M. Martinelli, F Passalacqua, L. Moscardini, Lilian Blot, V. Lindholm, S Sacquegna, F. Pasian, A. Pisani, J.-L. Starck, Chris Carbone, J. Martín-Fleitas, G. Zamorani, A. Secroun, Leigh C. Smith, S Toft, I. Hook, A Hall, L. Stanco, C. Padilla, J. Hjorth, P. M. Sánchez-Alarcón, J. H. Knapen, E. Gaztanaga, S Bardelli, F. Raison, J. García-Bellido, D. Sapone, A. Venhola, H Hildebrandt, S. Di Domizio, M. Sereno, A. Navarro-Alsina, Francesca Lepori, A. Blanchard, Matteo Cantiello, R. Maoli, O. Cucciati, K Kiiveri, A. Loureiro, S. A. Stanford, A. Ferré-Mateu, Pietro Battaglia, D. Paoletti, M. Jhabvala, Maureen Cropper, E. Sellentin, M. Tewes, M Radovich, J. Román, Daniele Bertacca, Harry I. Teplitz, Oliver Müller, T. Kitching, S. Nadathur, F. Marulli, K Jahnke, W Holmes, C. Baccigalupi, T. Schrabback, L. Gabarra, M Miluzio, I. A. Zinchenko, T. Saifollahi, S. Mei, J Le Graet, S. Andreon, A. Grazian, A. Kiessling, G Polenta, Chunhui Tao, A Enia, A Troja, S. Andreon, J.-C. Cuillandre, Benjamin Joachimi, G. Castignani, G. Leroy, I. Tutusaus, G. Mainetti, Valérie Gautard, R. Toledo-Moreo, B. Camacho Quevedo, S Bruton, M. Moresco, M. Baes, E. Zucca, Elisabeth Sola, M. Poncet, Juan José Díaz, A. Da Silva, N. Martinet, E. Bozzo, L. Patrizii, C. Colodro-Conde, I Lloro, G. Morgante, A. Cappi, K. Ganga, H. Dole, Simon Conseil, N Tessore, M Ballardini, S. Ferriol, H. Domínguez Sánchez, S Quai, V Capobianco, A. Biviano, E Medinaceli, L. Conversi, M Lembo, B Sartoris, I Risso, K Paterson, M. Hilker, P. Tallada-Crespí, C Sirignano, J. Carretero, K. George, E Keihänen, B. Gillis, M. Castellano, G. De Lucia, M Sahlén, F. De Paolis, C. Kirkpatrick, E. Maiorano, R Ragusa, O. Marggraf, Marcelo Farina, A Calabrò, Sandor Kruk, M. Pöntinen, M Viel, C Porciani, A. Lançon, G. Meylan, M. Béthermin, E. Branchini, R. Saglia, V. Testa, F. Mannucci, S. Galeotta, V. Kansal, H Kurki-Suonio, S Borgani, L. Legrand, R. Farinelli, F. Giacomini, M Tenti, C. Valieri, Yuhong Fang, K. Pedersen, Franca Soldano, A. Biviano, E. Franceschi, A Cimatti, R. Rebolo, P.‐A. Duc, Rebecca Habas, Luca Amendola, J.M. Diego, T Castro, R Teyssier, Pierluigi Monaco, C. Giocoli, María Guidi, Elham Saremi, J. Gracia-Carpio, S. Davini, Antonio M. Mora, M.L Brown, Savvas Nesseris, D. Potter, F. Hormuth, F. Dubath, K Tanidis, C. Neissner, E. Iodice, F. Buitrago, F. Finelli⋆, T Gasparetto, M. Fumana, G. Verdoes Kleijn, S. Pires, P. Papaderos, M. Cropper, P Vielzeuf, P. C. Schneider, R. Nakajima, G. Gozaliasl, E. Romelli, Krishna Naidoo, Karina Voggel, P. Bergamini, S Camera, P. Šimon, D. Vergani, Yongshui Kang, B. Altieri, Y Mellier, J. Rhodes, F Caro, E Sarpa, G Sirri, A. A. Franco, M Kunz, O. Mansutti, R. Cabanac, F. Torradeflot, A Veropalumbo, S. Dusini, Aurel Schneider, C. Burigana, M Brescia, M. Kümmel, S Cavuoti, S. Paltani, A. Nucita, Y. Akrami, S. Kermiche, F. Atrio‐Barandela, Claudio Moretti, F. Cogato, D Sciotti, Yi Wang, Hui Kong, L. Maurin, G. Riccio, D Karagiannis, M Urbano, G Maggio, M. Magliocchetti, M. Baldi, O. Marchal, V. Pettorino, J. Valiviita, X. Dupac, M. Archidiacono, E. Merlin, D. Di Ferdinando, I. Tereno, A. Renzi, D. Carollo, J. Macias-Perez, N. Auricchio, Z Sakr, F. Courbin, H. Degaudenzi, V. Scottez, M. Tucci, M. Wiesmann, D. Maino, J. Kim, H. Dole, J.A. Escartin Vigo, B. Kubik, M Bolzonella, S. Casas, A. N. Taylor, G Verza, L Valenziano, F. Gianotti, J Lesgourgues, M. N. Bremer, M. Poulain, S.-M. Niemi, M.N Le, S Ligori, A Finoguenov, M. Walmsley, G. Congedo, F. Marleau, L. Leuzzi, J Junais
article en

Abstract

Local Universe dwarf galaxies can serve as both cosmological and mass assembly probes. Deep surveys have enabled the study of these objects down to the low surface brightness (LSB) regime. In this paper, we estimate Euclid ’s dwarf detection capabilities as well as limits of its MERge processing function (MER pipeline), which is responsible for producing the stacked mosaics and final catalogues. To do this, we injected mock dwarf galaxies in a real Euclid Wide Survey (EWS) field in the VIS band and compared the input catalogue to the final MER catalogue. The mock dwarf galaxies were generated using simple Sérsic models with structural parameters (including size and surface brightness) drawn from observed dwarf galaxy catalogues. These simulations represent an idealised case in the sense they do not account for additional factors such as ellipticity, morphology, or crowding. To characterise the detected dwarfs, we used the mean surface brightness inside the effective radius SB e (in mag arcsec −2 ). The final MER catalogues achieve a completenesses of 91% for SB e ∈ [21, 24] and 54% for SB e ∈ [24, 28]. These numbers do not take into account possible contaminants, including confusion with background galaxies at the location of the dwarfs. After taking those effects into account, they respectively became 86% and 38%. The MER pipeline performs a final local background subtraction with a small mesh size, leading to a flux loss for galaxies with R e &gt; 10″. By using the final MER mosaics and reinjecting this local background, we obtained an image in which we recover reliable photometric properties for objects under the arcminute scale. This background-reinjected product is thus suitable for the study of Local Universe dwarf galaxies. Euclid ’s data reduction pipeline serves as a test bed for other deep surveys, particularly regarding background subtraction methods, a key issue in LSB science.

Astronomy and AstrophysicsVol. 707
Université Claude Bernard Lyon 1 (FR), Institut polytechnique de Grenoble (FR), Universidad de Valladolid (ES), University of Geneva (CH), Institució Catalana de Recerca i Estudis Avançats (ES), Universidad Complutense de Madrid (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), 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), University of Turku (FI), Universidad de La Laguna (ES), Stockholm University (SE), University of Groningen (NL), Université Fédérale de Toulouse Midi-Pyrénées (FR), Université Catholique de Lille (FR), University of Oslo (NO), Universidad de Salamanca (ES), University of Toronto (CA), 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), Université Côte d'Azur (FR), 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), Arcetri Astrophysical Observatory (IT), Helsinki Institute of Physics (FI), Astronomical Observatory of Rome (IT), 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), United Kingdom Space Agency (GB), Universidad Politécnica de Cartagena (ES), Ghent University (BE), 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), 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), 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), Institute of Nuclear Physics of Lyon (FR), Flatiron Health (United States) (US), Astronomical Observatory (RS), St. Joseph Medical Center (US), Istituto Nazionale di Fisica Nucleare, Sezione di Roma I (IT), Instituto de Astrofísica de Andalucía (ES), Osservatorio Astronomico di Padova (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), University of Southampton (GB), Osservatorio di Astrofisica e Scienza dello Spazio, Flatiron Institute (US), European Space Research and Technology Centre (NL), University College London (GB), Imperial 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), Lancaster University (GB), University of Chile (CL), Heidelberg Institute for Theoretical Studies (DE), École Centrale de Lille (FR), 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 76%
Galaxies: Formation, Evolution, Phenomena
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