<i>Euclid</i>: Early Release Observations

Intracluster light (ICL) provides a record of the dynamical interactions undergone by clusters, giving clues on cluster formation and evolution. Here, we analyse the properties of ICL in the massive cluster Abell 2390 at redshift z = 0.228. Our analysis is based on the deep images obtained by the Euclid mission as part of the Early Release Observations in the near-infrared ( Y E , J E , H E bands), using the NISP instrument in a 0.75 deg 2 field. We subtracted a point–spread function (PSF) model and removed the Galactic cirrus contribution in each band after modelling it with the DAWIS software. We then applied three methods to detect, characterise, and model the ICL and the brightest cluster galaxy (BCG): the CICLE 2D multi-galaxy fitting; the DAWIS wavelet-based multiscale software; and a mask-based 1D profile fitting. We detect ICL out to 600 kpc. The ICL fractions derived by our three methods range between 18% and 36% (average of 24%), while the BCG+ICL fractions are between 21% and 41% (average of 29%), depending on the band and method. A galaxy density map based on 219 selected cluster members shows a strong cluster substructure to the south-east and a smaller feature to the north-west. Ellipticals dominate the cluster's central region, with a centroid offset from the BCG by about 70 kpc and distribution following that of the ICL, while spirals do not trace the entire ICL but rather substructures. The comparison of the BCG+ICL, mass from gravitational lensing, and X-ray maps show that the BCG+ICL is the best tracer of substructures in the cluster. Based on colours, the ICL (out to about 400 kpc) seems to be built by the accretion of small systems ( M ∼10 9.5 M ⊙ ), or from stars coming from the outskirts of Milky Way-type galaxies ( M ∼10 10 M ⊙ ). Though Abell 2390 does not seem to be undergoing a merger, it is not yet fully relaxed, since it has accreted two groups that have not fully merged with the cluster core. We estimate that the contributions to the inner 300 kpc of the ICL of the north-west and south-east subgroups are 21% and 9%, respectively.

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Journal
Astronomy and Astrophysics
Published
2025-05-05
DOI
https://doi.org/10.1051/0004-6361/202554460
Citations
6
Primary Topic
Galaxies: Formation, Evolution, Phenomena
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article
Field-Weighted Citation Impact
6.93
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article

Euclid: Early Release Observations

K. George, M Poncet, Will J. Percival, G. Riccio et al.
6 citations
Astronomy and Astrophysics
Galaxies: Formation, Evolution, Phenomena
6.93
article

Euclid: Early Release Observations

K. George, M Poncet, Will J. Percival, G. Riccio, J.-L. Starck, D. Le Mignant, M. Brescia, E Merlin, F. Marulli, R Nakajima, J Brinchmann, B. Joachimi, J. Weller, G. Meylan, J. Steinwagner, N. Aghanim, I. Lloro, Guillaume Mahler, E Rossetti, N. A. Hatch, F. Durret, Paola Dimauro, F. Courbin, Y. Copin, A Renzi, M. Jhabvala, S. Bardelli, F Faustini, Alberto Basset, B Sartoris, M Schirmer, V. Scottez, C. Baccigalupi, T. Schrabback, A. Secroun, T. Saifollahi, B Altieri, A. Grazian, S. Maurogordato, H Degaudenzi, G Polenta, S. V. H. Haugan, S Marcin, T. Vassallo, R. Scaramella, S. Andreon, C.J. Conselice, J.-C. Cuillandre, G. Castignani, M Castellano, R. Toledo-Moreo, J. Hoar, M. Moresco, D. Sapone, G. De Lucia, J.W Nightingale, F Dubath, E. Slezak, A. Veropalumbo, N Auricchio, G. Sirri, J. Carretero, W. Holmes, A. Caillat, S. Ferriol, S. P. Bamford, E. Romelli, A. M. Di Giorgio, I. Tutusaus, A. Cimatti, H Kurki-Suonio, Matthias Kluge, C Sirignano, P. Schneider, A. Bonchi, M. Martinelli, S. Casas, E. Maiorano, A. Tsyganov, Syeda Lammim Ahad, S Serrano, L. Moscardini, Yolanda Jiménez-Teja, B. Gillis, E. Medinaceli, Callum Bellhouse, M. Kümmel, A. Hornstrup, R Ragusa, V.F Cardone, E Sefusatti, M Baldi, A. Balestra, K. Jahnkę, M. Farina, L. Guzzo, S Dusini, S. Ligori, G. Seidel, S Paltani, S. Galeotta, F. Raison, E. Franceschi, P. Tallada-Crespí, Y Wang, L. Stanco, K. Pedersen, A. Kiessling, Konrad H. Kuijken, Frank Grupp, R Gavazzi, V Capobianco, Y. Mellier, C Giocoli, K. Markovič, S. Camera, F. Hormuth, S. Mei, D. Bonino, V. Lindholm, R. Rébolo, Jesse B. Golden-Marx, L. Conversi, M. Cropper, E. Keihänen, E Branchini, M Roncarelli, S. Cavuoti, Mireia Montes, M. Melchior, M. Frailis, V. Pettorino, P. Bergamini, R Massey, A. Ellien, C. Carbone, S. Kermiche, H.I Teplitz, J. M. Diego, M Kunz, O. Mansutti, P. B. Lilje, A. Amara, A.N. Taylor, L.A. Popa, S. Paltani, G. Mainetti, A.H. Gonzalez, C. Burigana, J. Dinis, L. Pozzetti, P. Gómez-Alvarez, H. M. Courtois, R. C. Nichol, A. Da Silva, O. R. Williams, M. D. Seiffert, A Biviano, S.-M. Niemi, S. Paltani, L. Valenziano, P. Hudelot, V. Pettorino, C Neissner, D. Maino, O. Marggraf, I. Tereno, P Battaglia, Z Sakr, J. Rhodes, R. Laureijs, M. Bolzonella, H. Dole, F Torradeflot, B. Kubik, Y. Ascasíbar, X. Dupac, R. Saglia, N Martinet, G. Congedo, S. Fotopoulou, A. Mora, C Colodro-Conde, H. Hoekstra, C. A. J. Duncan
article en
6 citations

Abstract

Intracluster light (ICL) provides a record of the dynamical interactions undergone by clusters, giving clues on cluster formation and evolution. Here, we analyse the properties of ICL in the massive cluster Abell 2390 at redshift z = 0.228. Our analysis is based on the deep images obtained by the Euclid mission as part of the Early Release Observations in the near-infrared ( Y E , J E , H E bands), using the NISP instrument in a 0.75 deg 2 field. We subtracted a point–spread function (PSF) model and removed the Galactic cirrus contribution in each band after modelling it with the DAWIS software. We then applied three methods to detect, characterise, and model the ICL and the brightest cluster galaxy (BCG): the CICLE 2D multi-galaxy fitting; the DAWIS wavelet-based multiscale software; and a mask-based 1D profile fitting. We detect ICL out to 600 kpc. The ICL fractions derived by our three methods range between 18% and 36% (average of 24%), while the BCG+ICL fractions are between 21% and 41% (average of 29%), depending on the band and method. A galaxy density map based on 219 selected cluster members shows a strong cluster substructure to the south-east and a smaller feature to the north-west. Ellipticals dominate the cluster's central region, with a centroid offset from the BCG by about 70 kpc and distribution following that of the ICL, while spirals do not trace the entire ICL but rather substructures. The comparison of the BCG+ICL, mass from gravitational lensing, and X-ray maps show that the BCG+ICL is the best tracer of substructures in the cluster. Based on colours, the ICL (out to about 400 kpc) seems to be built by the accretion of small systems ( M ∼10 9.5 M ⊙ ), or from stars coming from the outskirts of Milky Way-type galaxies ( M ∼10 10 M ⊙ ). Though Abell 2390 does not seem to be undergoing a merger, it is not yet fully relaxed, since it has accreted two groups that have not fully merged with the cluster core. We estimate that the contributions to the inner 300 kpc of the ICL of the north-west and south-east subgroups are 21% and 9%, respectively.

Astronomy and AstrophysicsVol. 698
Université Paris Cité (FR), Commissariat à l'Énergie Atomique et aux Énergies Alternatives (FR), Centre National d'Études Spatiales (FR), Institut d'Astrophysique de Paris (FR), Laboratoire AstroParticule et Cosmologie (FR), Observatoire astronomique de Strasbourg (FR), Astrophysique, Instrumentation et Modélisation (FR), Centre de physique des particules de Marseille (FR), Laboratoire d’Astrophysique de Marseille (FR), Institut d'Astrophysique Spatiale (FR), Lagrange Laboratory (FR), Château Gombert (FR), Observatoire de la Côte d’Azur (FR), CEA Paris-Saclay (FR), Centre de Calcul de l’Institut National de Physique Nucléaire et de Physique des Particules (FR), Institute of Nuclear Physics of Lyon (FR), Institut de Recherche en Astrophysique et Planétologie (FR), Institut de Physique des 2 Infinis de Lyon (FR)
Openalex Percentile: Top 3%
Galaxies: Formation, Evolution, Phenomena
6.93
DOIOpen Access PDFOpenAlex
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