<i>Euclid</i> preparation

Extragalactic globular clusters (EGCs) are an abundant and powerful tracer of galaxy dynamics and formation, and their own formation and evolution is also a matter of extensive debate. The compact nature of globular clusters means that they are hard to spatially resolve and thus study outside the Local Group. In this work we have examined how well EGCs will be detectable in images from the Euclid telescope, using both simulated pre-launch images and the first early-release observations of the Fornax galaxy cluster. The Euclid Wide Survey will provide high-spatial resolution VIS imaging in the broad I E band as well as near-infrared photometry ( Y E , J E , and H E ). We estimate that the 24 719 known galaxies within 100 Mpc in the footprint of the Euclid survey host around 830 000 EGCs of which about 350 000 are within the survey’s detection limits. For about half of these EGCs, three infrared colours will be available as well. For any galaxy within 50 Mpc the brighter half of its GC luminosity function will be detectable by the Euclid Wide Survey. The detectability of EGCs is mainly driven by the residual surface brightness of their host galaxy. We find that an automated machine-learning EGC-classification method based on real Euclid data of the Fornax galaxy cluster provides an efficient method to generate high purity and high completeness GC candidate catalogues. We confirm that EGCs are spatially resolved compared to pure point sources in VIS images of Fornax. Our analysis of both simulated and first on-sky data show that Euclid will increase the number of GCs accessible with high-resolution imaging substantially compared to previous surveys, and will permit the study of GCs in the outskirts of their hosts. Euclid is unique in enabling systematic studies of EGCs in a spatially unbiased and homogeneous manner and is primed to improve our understanding of many understudied aspects of GC astrophysics.

Authors

Institutions

Publication Details

Journal
Astronomy and Astrophysics
Published
2024-11-22
DOI
https://doi.org/10.1051/0004-6361/202450851
Citations
7
Primary Topic
Galaxies: Formation, Evolution, Phenomena
Type
article
Field-Weighted Citation Impact
2.32

Funders

Controls
|||
ALL TIME
JAN
FEB
MAR
APR
MAY
JUN
JUL
AUG
SEP
OCT
article

Euclid preparation

D Sapone, A Hall, K. George, L. K. Hunt et al.
7 citations
Astronomy and Astrophysics
Galaxies: Formation, Evolution, Phenomena
2.32
article

Euclid preparation

D Sapone, A Hall, K. George, L. K. Hunt, G. Seidel, S. S. Larsen, M. Rejkuba, M Poncet, J. Graciá‐Carpio, M. Ballardini, M. Calabrese, P. Tallada-Crespí, S Matthew, P. Hudelot, G. Riccio, G. A. Mamon, A Grazian, K. Pedersen, C. Sirignano, N. Martinet, E. Gaztanaga, R. Laureijs, I. Hook, I. Ferrero, G de Lucia, R Nakajima, M. Kunz, L. Stanco, E. Bozzo, J. Weller, C. Baccigalupi, J. H. Knapen, J. Steinwagner, M. Baldi, C. Surace, J. García-Bellido, S. Borgani, H Hildebrandt, S. Di Domizio, N. Mauri, M. Martinelli, O. Marggraf, J. F. Macías–Pérez, C. Padilla, S Dusini, P. Liebing, Y. Copin, Pierre Boldrini, A. Troja, F. Torradeflot, A. Díaz‐Sánchez, G. Gozaliasl, G. Desprez, P. Reimberg, E. Munari, G Verza, C.J.A.P. Martins, Abdurrouf, A.R. Cooray, V. Capobianco, J Hjorth, T. Schrabback, L. Gabarra, T. Saifollahi, S. Cavuoti, A. Kiessling, S. V. H. Haugan, D. Vergani, R. Massey, T. Vassallo, R. Scaramella, C.J. Conselice, J.-C. Cuillandre, Antoine Blanchard, M. Kümmel, G. Castignani, Valérie Gautard, R. Toledo-Moreo, S Bruton, M. Moresco, M. Baes, V. Scottez, J. Brinchmann, G Congedo, G Sirri, L Moscardini, M. Kilbinger, P. Lonare, T. Castro, Elisabeth Sola, D. Bonino, J.W Nightingale, J. J. E. Kajava, A. Veropalumbo, J. Carretero, L. Valenziano, S Toft, M. A. Raj, C Colodro-Conde, E. Romelli, C. Burigana, A. M. Di Giorgio, L. Conversi, H. Degaudenzi, O. Mansutti, I.A Zinchenko, G. Zamorani, I Risso, F. Marulli, B. De, V. Allevato, J. Väliviita, W. Gillard, R. Kohley, D. Karagiannis, S. Escoffier, L Blot, B. Gillis, M Sahlén, F. Dubath, E. Maiorano, R. B. Metcalf, J. Rhodes, F. Fornari, A. Hornstrup, E. Medinaceli, O. Ilbert, M. Pöntinen, A. Cappi, A. Lançon, D Scott, M. Béthermin, D. Carollo, K. Jahnkę, A. M. N. Ferguson, A. Secroun, M. Farina, F. Mannucci, M. Magliocchetti, F. Pasian, V. Kansal, S Anselmi, S. Ligori, Achille Nucita, M. Cantiello, L. Legrand, R. Farinelli, F. Giacomini, S. Galeotta, F. Raison, R. B. Metcalf, E. Franceschi, E. A. Valentijn, A. Cimatti, S. Casas, P.‐A. Duc, P. Gómez-Álvarez, M. Bolzonella, E. Merlin, R Teyssier, M. Roncarelli, N. A. Walton, R Saglia, S Farrens, Y. Mellier, G Cañas-Herrera, S. Paltani, M. Castellano, K. Markovič, R. Cabanac, S. Ferriol, S. Maurogordato, D. Potter, Z. Sakr, C. Giocoli, S. Mei, M Schirmer, V. Pettorino, K. C. Chambers, F Hormuth, F. Finelli⋆, J. Dinis, V. Lindholm, R. Rébolo, E. Sefusatti, P.-F Rocci, M. Sereno, M. Cropper, E. Keihänen, Anthony Calabro, B. Sartoris, C. Bodendorf, P. Schneider, N. Auricchio, M. Frailis, M. Fumana, A. Spurio Mancini, Karina Voggel, P. Bergamini, S Camera, P. Šimon, S. Andreon, C. Carbone, F. Annibali, S. Kermiche, H.I Teplitz, Michel Poulain, P. B. Lilje, Chiara Moretti, M. Paolillo, S. Serrano, G. Polenta, L.A. Popa, S. Contarini, E. Rossetti, M. Viel, A Pezzotta, R. Carlberg, E. Zucca, M Brescia, E. Branchini, C. S. Carvalho, Alejandro S. Borlaff, L. Pozzetti, Y. Akrami, F Grupp, H. M. Courtois, R. C. Nichol, K. Jahnkę, Yun Wang, S. Tosi, A. Da Silva, L. Maurin, Rubén Sánchez-Janssen, M Urbano, I. Lloro, I. Tutusaus, S. Pires, G. Meylan, C. C. Kirkpatrick, W. Holmes, C. Porciani, V. Popa, K. Ganga, D. Di Ferdinando, I. Tereno, G Morgante, A. Schneider, S Bardelli, F. Courbin, A. Renzi, H. Kurki‐Suonio, M. Wiesmann, M. Tenti, X. Dupac, G. Maggio, C. Neissner, J.A. Escartin Vigo, A Biviano, B. Kubik, H. Dole, M. Tucci, P Monaco, G. Testera, H. Hoekstra, S. Fotopoulou, A. Loureiro, S.-M. Niemi, L. Patrizii, F. Marleau
article en
7 citations

Abstract

Extragalactic globular clusters (EGCs) are an abundant and powerful tracer of galaxy dynamics and formation, and their own formation and evolution is also a matter of extensive debate. The compact nature of globular clusters means that they are hard to spatially resolve and thus study outside the Local Group. In this work we have examined how well EGCs will be detectable in images from the Euclid telescope, using both simulated pre-launch images and the first early-release observations of the Fornax galaxy cluster. The Euclid Wide Survey will provide high-spatial resolution VIS imaging in the broad I E band as well as near-infrared photometry ( Y E , J E , and H E ). We estimate that the 24 719 known galaxies within 100 Mpc in the footprint of the Euclid survey host around 830 000 EGCs of which about 350 000 are within the survey’s detection limits. For about half of these EGCs, three infrared colours will be available as well. For any galaxy within 50 Mpc the brighter half of its GC luminosity function will be detectable by the Euclid Wide Survey. The detectability of EGCs is mainly driven by the residual surface brightness of their host galaxy. We find that an automated machine-learning EGC-classification method based on real Euclid data of the Fornax galaxy cluster provides an efficient method to generate high purity and high completeness GC candidate catalogues. We confirm that EGCs are spatially resolved compared to pure point sources in VIS images of Fornax. Our analysis of both simulated and first on-sky data show that Euclid will increase the number of GCs accessible with high-resolution imaging substantially compared to previous surveys, and will permit the study of GCs in the outskirts of their hosts. Euclid is unique in enabling systematic studies of EGCs in a spatially unbiased and homogeneous manner and is primed to improve our understanding of many understudied aspects of GC astrophysics.

Astronomy and AstrophysicsVol. 693
Université Claude Bernard Lyon 1 (FR), Institut polytechnique de Grenoble (FR), University of Geneva (CH), University of Rome Tor Vergata (IT), Leiden University (NL), California Institute of Technology (US), Uppsala University (SE), University of Copenhagen (DK), Ames Research Center (US), Centre National de la Recherche Scientifique (FR), University of Minnesota (US), European Southern Observatory (DE), Institute of Space Sciences (ES), University of Hawaii System (US), Jet Propulsion Laboratory (US), University of Helsinki (FI), 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 British Columbia (CA), University of Trieste (IT), University of Salento (IT), Radboud University Nijmegen (NL), University of Turku (FI), Universidad de La Laguna (ES), Stockholm University (SE), Queen Mary University of London (GB), Kavli Institute for the Physics and Mathematics of the Universe (JP), University of Groningen (NL), Université Fédérale de Toulouse Midi-Pyrénées (FR), Université Catholique de Lille (FR), Universidade do Porto (PT), Royal Holloway University of London (GB), Saint Joseph University (LB), University of Oslo (NO), University of Toronto (CA), Institute for High Energy Physics (ES), University of Milan (IT), Durham University (GB), Universität Innsbruck (AT), Princeton University (US), University of Ferrara (IT), Université Côte d'Azur (FR), University of Zurich (CH), University of California, Irvine (US), Aarhus University (DK), 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), Agenzia Spaziale Italiana (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), University of Surrey (GB), University of Manchester (GB), Institute for High Performance Computing and Networking (IT), CEA Grenoble (FR), Universidad Politécnica de Cartagena (ES), Ghent University (BE), University of Bristol (GB), Sorbonne Université (FR), University of Oxford (GB), Técnicas Reunidas (Spain) (ES), Astrophysique, Instrumentation et Modélisation (FR), Janssen (France) (FR), Laboratoire Univers et Théories (FR), Institute of Astrophysics and Space Sciences (PT), ARC Centre of Excellence for Dark Matter Particle Physics (AU), Max Planck Institute for Extraterrestrial Physics (DE), Institut d'Estudis Espacials de Catalunya (ES), European Space Astronomy Centre (ES), Centre de physique des particules de Marseille (FR), Istituto Nazionale di Fisica Nucleare, Sezione di Lecce (IT), Laboratoire d’Astrophysique de Marseille (FR), Istituto Nazionale di Fisica Nucleare, Sezione di Torino (IT), Institute for Space Astrophysics and Planetology (IT), Institut d'Astrophysique Spatiale (FR), 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), Istituto Nazionale di Fisica Nucleare, Sezione di Napoli (IT), Centro de Astrofísica da Universidade do Porto (PT), Max Planck Institute for Astronomy (DE), Bay Area Environmental Research Institute (US), CEA Cadarache (FR), Lagrange Laboratory (FR), Istituto di Radioastronomia di Bologna (IT), Château Gombert (FR), Université Bourgogne Franche-Comté (FR), Collurania Teramo Observatory (IT), Istituto Nazionale di Fisica Nucleare, Sezione di Genova (IT), Observatoire de la Côte d’Azur (FR), CEA Paris-Saclay (FR), Instituto de Astrofísica de Canarias (ES), Institut National de Physique Nucléaire et de Physique des Particules (FR), Danish Gas Technology Centre (Denmark) (DK), Istituto Nazionale di Fisica Nucleare, Sezione di Milano (IT), Laboratoire de Physique Subatomique et de Cosmologie (FR), Institute of Space Science - INFLPR Subsidiary (RO), Osservatorio Astronomico della Regione Autonoma Valle d'Aosta (IT), 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), Institute of Nuclear Physics of Lyon (FR), Flatiron Health (United States) (US), Istituto Nazionale di Fisica Nucleare, Sezione di Roma I (IT), Osservatorio Astronomico di Padova (IT), 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, Fondazione ICSC Centro Nazionale di Ricerca in High Performance Computing, Big Data e Quantum Computing, Flatiron Institute (US), Institut de Physique des 2 Infinis de Lyon (FR), European Space Research and Technology Centre (NL), University College London (GB), Imperial College London (GB), UK Astronomy Technology Centre (GB), École Polytechnique Fédérale de Lausanne (CH), University of Turin (IT), Swinburne University of Technology (AU), New York University (US), Case Western Reserve University (US), University of Portsmouth (GB), Universidad Autónoma de Madrid (ES), Saint Mary's University (CA), Lancaster University (GB), Université de Strasbourg (FR), University of Chile (CL), Heidelberg Institute for Theoretical Studies (DE), University of Naples Federico II (IT), The University of Tokyo (JP), Ludwig-Maximilians-Universität München (DE), University of Genoa (IT), Newcastle University (GB), Sapienza University of Rome (IT), University of the Western Cape (ZA), National Institute for Astrophysics (IT), RWTH Aachen University (DE), Université Grenoble Alpes (FR), Ruhr University Bochum (DE), Netherlands Institute for Radio Astronomy (NL), University of Bologna (IT), Universitat Politècnica de Catalunya (ES), Technical University of Denmark (DK), University of Oulu (FI), University of Edinburgh (GB), Aalto University (FI)
National Aeronautics and Space Administration, Ministerio de Ciencia, Innovación y Universidades, European Space Agency, European Commission, Agence Nationale de la Recherche, Magyar Tudományos Akadémia, Agenzia Spaziale Italiana, National Astronomical Observatory of Japan, Agenția Spațială Română, Norsk Romsenter, Fundação para a Ciência e a Tecnologia, European Regional Development Fund, Agencia Estatal de Investigación
Openalex Percentile: Top 12%
Galaxies: Formation, Evolution, Phenomena
2.32
DOIOpen Access PDFOpenAlex
AI Navigator

Ask Laika to Summarize, Analyze, and Connect papers live on the map.

Summarize Papers & Methodologies

Extract key findings, datasets, and comparative methods across publications.

Benchmark Rankings & Visual Analytics

Rank top research institutions, authors, funders, topics, and journals by Field-Weighted Citation Impact (FWCI) and paper volume with instant charts.

Connect Distant Disciplines

Bridge topological clusters on the map to find hidden collaborative intersections.