<i>Euclid</i> : Early Release Observations – Interplay between dwarf galaxies and their globular clusters in the Perseus galaxy cluster

We present an analysis of globular clusters (GCs) of dwarf galaxies in the Perseus galaxy cluster that explores the relationship between dwarf galaxy properties and their GCs. Our focus is on GC numbers ( N GC ) and GC half-number radii ( R GC ) around dwarf galaxies, and their relations with host galaxy stellar masses ( M * ), central surface brightnesses ( μ 0 ), and effective radii ( R e ). This work is unique due to its large sample size and the absence of pre-selection based on μ 0 and R GC for dwarf galaxies. Interestingly, we find that at a given stellar mass, R GC is almost independent of the host galaxy μ 0 and R e , while R GC / R e depends on μ 0 and R e . Lower surface brightness and diffuse dwarf galaxies show R GC / R e ≈ 1, while higher surface brightness and compact dwarf galaxies show R GC / R e ≈ 1.5–2. This means that for dwarf galaxies of similar stellar mass, the GCs have a similar median extent; however, their distribution is different from the field stars of their host. Additionally, low surface brightness and diffuse dwarf galaxies on average have a higher N GC than high surface brightness and compact dwarf galaxies at any given stellar mass. We also find that ultra-diffuse galaxies (UDGs) and non-UDGs in the sample have a similar R GC , while UDGs have a smaller R GC / R e (typically less than one) and a three to four times higher N GC than non-UDGs. Furthermore, when examining nucleated versus non-nucleated dwarf galaxies, we found that for M * &gt; 10 8 M ⊙ , nucleated dwarf galaxies seem to have a smaller R GC and R GC / R e , with no significant differences seen between their N GC except at M * &lt; 10 8 M ⊙ , where the nucleated dwarf galaxies tend to have a higher N GC . Lastly, we explored the stellar-to-halo mass ratio (SHMR) of dwarf galaxies (halo mass based on N GC ) and conclude that the Perseus cluster dwarf galaxies follow the expected SHMR at z = 0 extrapolated down to M * = 10 6 M ⊙ .

Authors

Institutions

Publication Details

Journal
Astronomy and Astrophysics
Published
2025-09-23
DOI
https://doi.org/10.1051/0004-6361/202554667
Citations
7
Primary Topic
Galaxies: Formation, Evolution, Phenomena
Type
article
Field-Weighted Citation Impact
8.08
Controls
|||
ALL TIME
JAN
FEB
MAR
APR
MAY
JUN
JUL
AUG
SEP
OCT
article

Euclid : Early Release Observations – Interplay between dwarf galaxies and their globular clusters in the Perseus galaxy cluster

D Sapone, K. George, S Pires, L. K. Hunt et al.
7 citations
Astronomy and Astrophysics
Galaxies: Formation, Evolution, Phenomena
8.08
article

Euclid : Early Release Observations – Interplay between dwarf galaxies and their globular clusters in the Perseus galaxy cluster

D Sapone, K. George, S Pires, L. K. Hunt, L. Moscardini, M. Roncarelli, J. Graciá‐Carpio, Will J. Percival, V. Lindholm, A. Grazian, P. Tallada-Crespí, F. Pasian, Y. Mellier, N. Auricchio, William Bon, J. Martín-Fleitas, D. Le Mignant, I Tereno, I. Hook, F. Dubath, D. Bonino, M Castellano, J. H. Knapen, S. Ferriol, C. Giocoli, H. Bouy, S Dusini, S. Casas, N. A. Hatch, C. Padilla, F. Torradeflot, G. Zamorani, A. Ferré-Mateu, A Renzi, P. Schneider, F Courbin, M. Jhabvala, F. Grupp, O Marggraf, G. Mainetti, F Faustini, J. Román, Alberto Basset, J Steinwagner, G Castignani, Andrea Bonchi, T. Saifollahi, B Altieri, A. Kiessling, S. Andreon, G Polenta, S. V. H. Haugan, C.J. Conselice, J.-C. Cuillandre, C. Neissner, R. Laureijs, I. Tutusaus, S. Paltani, J. Hoar, M. Moresco, F. Raison, E. Zucca, R. Saglia, K Pedersen, M. Poncet, G. De Lucia, C. Colodro-Conde, J. Valiviita, J. Weller, A. Biviano, M Kümmel, Matthias Kluge, M. Hilker, P. Tallada-Crespí, N. Aghanim, M Frailis, J. Carretero, M. Martinelli, S. Escoffier, J Brinchmann, W. Holmes, E Keihänen, A. Tsyganov, E. Maiorano, M Baldi, A. Lançon, J Rhodes, E. Medinaceli, M. Béthermin, E. Branchini, A. Balestra, M. Farina, S. Camera, Sergio Serrano, J. Weller, H Kurki-Suonio, M. Cantiello, G. Seidel, M Fumana, R. Farinelli, S Paltani, A. Zacchei, E. Franceschi, J.A Schewtschenko, K Jahnke, L. Stanco, ENRIQUE GAZTAÑAGA, C. Stone, C. Tortora, I Lloro, V Capobianco, Antonio M. Mora, C Giocoli, A Biviano, G. Congedo, M Schirmer, S. Andreon, F Hormuth, S. Mei, K. C. Chambers, L. Conversi, A da Silva, B Gillis, R. Nakajima, S Galeotta, Karina Voggel, P. Bergamini, R Massey, Sune Toft, J. M. Diego, M Kunz, O. Mansutti, A.G. Sánchez, Michel Poulain, P. B. Lilje, E Merlin, G Meylan, N. Martinet, P.-A Duc, A Veropalumbo, A.M.C Le Brun, M. Cropper, C. Burigana, M Brescia, S Cavuoti, S. Kermiche, O. Lahav, H. M. Courtois, M. Mondelin, Yi Wang, G. Riccio, Rubén Sánchez-Janssen, M Urbano, M. D. Seiffert, S. Maurogordato, B. Sartoris, M. Bolzonella, V. Pettorino, E. Romelli, L. A. Popa, P Battaglia, D. Carollo, L. Valenziano, Z Sakr, S Bardelli, H. Degaudenzi, V. Scottez, C. Baccigalupi, A. Cimatti, B. Kubik, Y. Ascasíbar, H. Hoekstra, S. Fotopoulou, M. N. Bremer, S.-M Niemi, M.N Le, C. A. J. Duncan, S Ligori, M. Douspis, R. Rebolo, F. Marleau, D Bagot
article en
7 citations

Abstract

We present an analysis of globular clusters (GCs) of dwarf galaxies in the Perseus galaxy cluster that explores the relationship between dwarf galaxy properties and their GCs. Our focus is on GC numbers ( N GC ) and GC half-number radii ( R GC ) around dwarf galaxies, and their relations with host galaxy stellar masses ( M * ), central surface brightnesses ( μ 0 ), and effective radii ( R e ). This work is unique due to its large sample size and the absence of pre-selection based on μ 0 and R GC for dwarf galaxies. Interestingly, we find that at a given stellar mass, R GC is almost independent of the host galaxy μ 0 and R e , while R GC / R e depends on μ 0 and R e . Lower surface brightness and diffuse dwarf galaxies show R GC / R e ≈ 1, while higher surface brightness and compact dwarf galaxies show R GC / R e ≈ 1.5–2. This means that for dwarf galaxies of similar stellar mass, the GCs have a similar median extent; however, their distribution is different from the field stars of their host. Additionally, low surface brightness and diffuse dwarf galaxies on average have a higher N GC than high surface brightness and compact dwarf galaxies at any given stellar mass. We also find that ultra-diffuse galaxies (UDGs) and non-UDGs in the sample have a similar R GC , while UDGs have a smaller R GC / R e (typically less than one) and a three to four times higher N GC than non-UDGs. Furthermore, when examining nucleated versus non-nucleated dwarf galaxies, we found that for M * &gt; 10 8 M ⊙ , nucleated dwarf galaxies seem to have a smaller R GC and R GC / R e , with no significant differences seen between their N GC except at M * &lt; 10 8 M ⊙ , where the nucleated dwarf galaxies tend to have a higher N GC . Lastly, we explored the stellar-to-halo mass ratio (SHMR) of dwarf galaxies (halo mass based on N GC ) and conclude that the Perseus cluster dwarf galaxies follow the expected SHMR at z = 0 extrapolated down to M * = 10 6 M ⊙ .

Astronomy and AstrophysicsVol. 703
Université Claude Bernard Lyon 1 (FR), 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 Nottingham (GB), Université de Bordeaux (FR), 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), University of Oslo (NO), Institut Universitaire de France (FR), Institute for High Energy Physics (ES), University of Milan (IT), Universität Innsbruck (AT), University of Saint Joseph (US), Université Côte d'Azur (FR), Université Paris Cité (FR), Aix-Marseille Université (FR), Heidelberg University (DE), Université de Lille (FR), 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), Observatoire de Paris (FR), 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), University of Bristol (GB), Sorbonne Université (FR), Park University (US), Osservatorio astronomico di Bologna (IT), Astrophysique, Instrumentation et Modélisation (FR), Laboratoire Univers et Théories (FR), Institute of Astrophysics and Space Sciences (PT), Max Planck Institute for Extraterrestrial Physics (DE), Institut d'Estudis Espacials de Catalunya (ES), Centre de physique des particules de Marseille (FR), Laboratoire d’Astrophysique de Marseille (FR), Laboratoire d'Astrophysique de Bordeaux (FR), Istituto Nazionale di Fisica Nucleare, Sezione di Torino (IT), Institute for Space Astrophysics and Planetology (IT), Institut d'Astrophysique Spatiale (FR), 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), SKA Observatory (GB), Istituto Nazionale di Fisica Nucleare, Sezione di Napoli (IT), Max Planck Institute for Astronomy (DE), Institute of Space Sciences (ES), Laboratoire de Physique Théorique (FR), DAWN Center for Independent Living (US), Lagrange Laboratory (FR), Istituto di Radioastronomia di Bologna (IT), Château Gombert (FR), Federico II University Hospital (IT), Unidades Centrales Científico-Técnicas (ES), 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), 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), Geophysical Division of the Earth Science Institute of the Slovak Academy of Sciences (SK), Engineering Science Analysis (United States) (US), Astronomy and Space (AU), Istituto Nazionale di Fisica Nucleare, Sezione di Bologna (IT), Port d'Informació Científica (ES), Institute for Fundamental Physics of the Universe (IT), Institute of Nuclear Physics of Lyon (FR), St. Joseph Medical Center (US), Istituto Nazionale di Fisica Nucleare, Sezione di Roma I (IT), Osservatorio Astronomico di Padova (IT), Bristol Robotics Laboratory (GB), Mila - Quebec Artificial Intelligence Institute (CA), European Space Research Institute (IT), 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, Institut de Physique des 2 Infinis de Lyon (FR), European Space Research and Technology Centre (NL), University College London (GB), UK Astronomy Technology Centre (GB), École Polytechnique Fédérale de Lausanne (CH), University of Turin (IT), Lancaster University (GB), University of Chile (CL), Université de Montréal (CA), Heidelberg Institute for Theoretical Studies (DE), Ludwig-Maximilians-Universität München (DE), University of Genoa (IT), National Institute for Astrophysics (IT), RWTH Aachen University (DE), University of Bologna (IT), University of California, Berkeley (US), Technical University of Denmark (DK), University of Edinburgh (GB)
Openalex Percentile: Top 3%
Galaxies: Formation, Evolution, Phenomena
8.08
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.