<i>Euclid</i> preparation

The intracluster light (ICL) permeating galaxy clusters is a tracer of the cluster assembly history and potentially a tracer of their dark matter structure. In this work, we explore the capability of the Euclid Wide Survey to detect ICL using H E -band mock images. We simulated clusters across a range of redshifts (0.3–1.8) and halo masses (10 13.9 –10 15.0 M ⊙ ) using an observationally motivated model of ICL. We identified a 50–200 kpc circular annulus around the brightest cluster galaxy (BCG) in which the signal-to-noise ratio of the ICL is maximised and used the S/N within this aperture as our figure of merit for ICL detection. We compared three state-of-the-art methods for ICL detection and found that a method that performs simple aperture photometry after high-surface brightness source masking is able to detect ICL with minimal bias for clusters more massive than 10 14.2 M ⊙ . The S/N of the ICL detection is primarily limited by the redshift of the cluster, which is driven by cosmological dimming rather than the mass of the cluster. Assuming the ICL in each cluster contains 15% of the stellar light, we forecast that Euclid will be able to measure the presence of ICL in up to ∼80 000 clusters of &gt;10 14.2 M ⊙ between z = 0.3 and 1.5 with an S/N&gt;3. Half of these clusters will reside below z = 0.75, and the majority of those below z = 0.6 will be detected with an S/N&gt;20. A few thousand clusters at 1.3&lt; z &lt;1.5 will have ICL detectable with an S/N &gt;3. The surface brightness profile of the ICL model is strongly dependent on both the mass of the cluster and the redshift at which it is observed so that the outer ICL is best observed in the most massive clusters of &gt;10 14.7 M ⊙ . Euclid will detect the ICL at a distance of more than 500 kpc from the BCG, up to z = 0.7, in several hundred of these massive clusters over its large survey volume.

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Publication Details

Journal
Astronomy and Astrophysics
Published
2025-04-04
DOI
https://doi.org/10.1051/0004-6361/202553887
Citations
6
Primary Topic
Astronomy and Astrophysical Research
Type
article
Field-Weighted Citation Impact
7.15

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article

Euclid preparation

M Viel, G. Seidel, S. Farrens, Zohreh Ghaffari et al.
6 citations
Astronomy and Astrophysics
Astronomy and Astrophysical Research
7.15
article

Euclid preparation

M Viel, G. Seidel, S. Farrens, Zohreh Ghaffari, M. Ballardini, M. Calabrese, M. Martinelli, P. Tallada-Crespí, A. Pisani, K. Pedersen, C. Sirignano, G. Zamorani, M. Brescia, E Merlin, F. Marulli, S Toft, I. Hook, C. Baccigalupi, C. Padilla, A. Blanchard, G. Meylan, M. Bolzonella, W.G Hartley, M. Schultheis, R Nakajima, J. Carretero, J. Steinwagner, Matthew Shetrone, A.G Ferrari, M. Sereno, A. Navarro-Alsina, R. Bender, O. Marggraf, N. A. Hatch, F. Durret, Patrice Simon, Paola Dimauro, Y. Copin, Alex D. Hall, P. Schneider, M Baldi, F Courbin, F Caro, A. Biviano, M. Jhabvala, F. Torradeflot, A. Díaz‐Sánchez, E Maiorano, G. Gozaliasl, E. Sellentin, F Raison, S. Bardelli, G. Desprez, T. Contini, F Faustini, A. Finoguenov, M. Magliocchetti, Alberto Basset, A. Amara, Claudio Moretti, C.J.A.P. Martins, A.R. Cooray, O. Cucciati, L. Moscardini, J Hjorth, T. Schrabback, S.J Liu, L. Gabarra, M Miluzio, T. Saifollahi, P Gómez-Álvarez, S. Mei, B Altieri, J Le Graet, A. Grazian, E. Bozzo, S. V. H. Haugan, Chunhui Tao, K Ganga, T. Vassallo, A Troja, C.J. Conselice, J.-C. Cuillandre, S. Dusini, G. Castignani, R. Toledo-Moreo, S Bruton, M. Moresco, Mark Holliman, D. Sapone, M. Meneghetti, G. De Lucia, N. Martinet, F Dubath, L. Patrizii, E. Slezak, M. Lattanzi, X Dupac, A. Veropalumbo, M. Poncet, T.I Liaudat, A. Caillat, H. Hildebrandt, S. Ferriol, S. P. Bamford, B Gillis, E. Romelli, C. Burigana, A. M. Di Giorgio, V Capobianco, H. Degaudenzi, G. Morgante, I Risso, J. Väliviita, G. Mainetti, E. Zucca, D. Karagiannis, S. Escoffier, L Blot, A. Tsyganov, Syeda Lammim Ahad, S Serrano, Maria Lembo, Yolanda Jiménez-Teja, W. Gillard, M Sahlén, F. De Paolis, Callum Bellhouse, M. Kümmel, S Casas, R. B. Metcalf, A. Hornstrup, V.F Cardone, S. Fotopoulou, E. Rossetti, E. Medinaceli, Sergey Kruk, M. Pöntinen, S. Di Domizio, R. B. Metcalf, R. Teyssier, M. Béthermin, V. Pettorino, E. Branchini, M. Farina, F. Mannucci, S. Galeotta, Claire E. Murray, V. Kansal, S Anselmi, J. Weller, S Borgani, L. Legrand, F. Grupp, M Fumana, R. Farinelli, F. Giacomini, M Tenti, C. Valieri, E. Franceschi, L. Conversi, A. Fontana, A. Cappi, Y Wang, K Jahnke, L. Stanco, ENRIQUE GAZTAÑAGA, A. Kiessling, J Martín-Fleitas, T Castro, P. Monaco, N. A. Walton, C. Giocoli, J. Gracia-Carpio, K. Markovič, I.T Andika, S. Maurogordato, S. Camera, F. Hormuth, K Tanidis, LAURENCE C. SMITH, K. C. Chambers, M. Kilbinger, D. Bonino, M. Archidiacono, F. Finelli⋆, V. Lindholm, M. Melchior, G. Verdoes Kleijn, P.-F Rocci, Jesse B. Golden-Marx, E. Keihänen, Anthony Calabro, D. Potter, P Vielzeuf, Koshy George, Krishna Naidoo, Mireia Montes, M. Frailis, R Massey, D. Vergani, A. Ellien, C. Carbone, Shoubaneh Hemmati, K. Paterson, S. Andreon, E Sarpa, S.A Stanford, J. M. Diego, G Sirri, M. Castellano, O. Mansutti, P. B. Lilje, S. Paltani, A.M.C Le Brun, Aurel Schneider, A.H. Gonzalez, I. Lloro, S Nesseris, J. Dinis, C. S. Carvalho, Alejandro S. Borlaff, S Cavuoti, L. Pozzetti, Y. Akrami, S. Kermiche, F. Atrio‐Barandela, H. M. Courtois, F. Cogato, D Sciotti, A. Da Silva, J.J Diaz, L. Maurin, G. Riccio, C. M. Gutiérrez, G. Testera, A. Jiménez Muñoz, Y. W. Kang, J.J.E Kajava, M. Roncarelli, I. Tutusaus, M Kunz, B. Sartoris, S.-M. Niemi, L. Valenziano, P. Hudelot, N Mauri, C.C Kirkpatrick, D. Di Ferdinando, J García-Bellido, I. Tereno, A Renzi, L. A. Popa, P Battaglia, V. Scottez, H. Kurki‐Suonio, M. Wiesmann, Z. Sakr, P. Liebing, N. Aghanim, V. Popa, C. Neissner, S. Pires, Jason Rhodes, J.A. Escartin Vigo, B. Kubik, R Cabanac, W. Holmes, S. Paltani, G. Polenta, R. Saglia, H. Hoekstra, A Cimatti, G Verza, A. Loureiro, M.L Brown, F. Gianotti, R. Pello, A. Mora, S. Tosi, P.G Ferreira, C Colodro-Conde, J. Lesgourgues, M Kluge, M Guidi, G. Ca nas-Herrera, C. A. J. Duncan, S Ligori, H. Böhringer, G. Congedo
article en
6 citations

Abstract

The intracluster light (ICL) permeating galaxy clusters is a tracer of the cluster assembly history and potentially a tracer of their dark matter structure. In this work, we explore the capability of the Euclid Wide Survey to detect ICL using H E -band mock images. We simulated clusters across a range of redshifts (0.3–1.8) and halo masses (10 13.9 –10 15.0 M ⊙ ) using an observationally motivated model of ICL. We identified a 50–200 kpc circular annulus around the brightest cluster galaxy (BCG) in which the signal-to-noise ratio of the ICL is maximised and used the S/N within this aperture as our figure of merit for ICL detection. We compared three state-of-the-art methods for ICL detection and found that a method that performs simple aperture photometry after high-surface brightness source masking is able to detect ICL with minimal bias for clusters more massive than 10 14.2 M ⊙ . The S/N of the ICL detection is primarily limited by the redshift of the cluster, which is driven by cosmological dimming rather than the mass of the cluster. Assuming the ICL in each cluster contains 15% of the stellar light, we forecast that Euclid will be able to measure the presence of ICL in up to ∼80 000 clusters of &gt;10 14.2 M ⊙ between z = 0.3 and 1.5 with an S/N&gt;3. Half of these clusters will reside below z = 0.75, and the majority of those below z = 0.6 will be detected with an S/N&gt;20. A few thousand clusters at 1.3&lt; z &lt;1.5 will have ICL detectable with an S/N &gt;3. The surface brightness profile of the ICL model is strongly dependent on both the mass of the cluster and the redshift at which it is observed so that the outer ICL is best observed in the most massive clusters of &gt;10 14.7 M ⊙ . Euclid will detect the ICL at a distance of more than 500 kpc from the BCG, up to z = 0.7, in several hundred of these massive clusters over its large survey volume.

Astronomy and AstrophysicsVol. 698
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), Uppsala University (SE), University of Copenhagen (DK), Ames Research Center (US), Centre National de la Recherche Scientifique (FR), Goddard Space Flight Center (US), 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 Nottingham (GB), University of Trieste (IT), 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), Universidade do Porto (PT), Saint Joseph University (LB), University of Oslo (NO), Universidad de Salamanca (ES), 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), Université Paris Cité (FR), Aix-Marseille Université (FR), Heidelberg University (DE), Université de Lille (FR), 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), FHNW University of Applied Sciences and Arts Northwestern Switzerland (CH), Institute for High Performance Computing and Networking (IT), Universidad Politécnica de Cartagena (ES), University of Florida (US), University of Bristol (GB), Sorbonne Université (FR), University of Oxford (GB), Técnicas Reunidas (Spain) (ES), Astrophysique, Instrumentation et Modélisation (FR), Janssen (France) (FR), Max Planck Institute for Physics (DE), Laboratoire Univers et Théories (FR), Valongo Observatory (BR), 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), AstroTec Holding (Netherlands) (NL), Institut d'Astrophysique Spatiale (FR), Max Planck Institute for Astrophysics (DE), 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), Lagrange Laboratory (FR), Istituto di Radioastronomia di Bologna (IT), Château Gombert (FR), Federico II University Hospital (IT), Université Bourgogne Franche-Comté (FR), 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), Istituto Nazionale di Fisica Nucleare, Sezione di Milano (IT), Laboratoire de Physique Subatomique et de Cosmologie (FR), Institute of Space Science - INFLPR Subsidiary (RO), 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), 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), Istituto Nazionale di Fisica Nucleare, Sezione di Roma I (IT), Instituto de Astrofísica de Andalucía (ES), 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), 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), Universidad Autónoma de Madrid (ES), Lancaster University (GB), Université de Strasbourg (FR), University of Chile (CL), Heidelberg Institute for Theoretical Studies (DE), Universitat de Barcelona (ES), The University of Tokyo (JP), Ludwig-Maximilians-Universität München (DE), University of Genoa (IT), University of California, Davis (US), 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 Edinburgh (GB), Aalto University (FI)
National Aeronautics and Space Administration, Ministerio de Ciencia, Innovación y Universidades, European Space Agency, Leverhulme Trust, Centre National d’Etudes Spatiales, Magyar Tudományos Akadémia, Agenzia Spaziale Italiana, National Astronomical Observatory of Japan, Agenția Spațială Română, Norsk Romsenter, Science and Technology Facilities Council, Fundação para a Ciência e a Tecnologia
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Astronomy and Astrophysical Research
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