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Bound star clusters observed in a lensed galaxy 460 Myr after the Big Bang.
Adamo, Angela; Bradley, Larry D; Vanzella, Eros; Claeyssens, Adélaïde; Welch, Brian; Diego, Jose M; Mahler, Guillaume; Oguri, Masamune; Sharon, Keren; Hsiao, Tiger Yu-Yang; Xu, Xinfeng; Messa, Matteo; Lassen, Augusto E; Zackrisson, Erik; Brammer, Gabriel; Coe, Dan; Kokorev, Vasily; Ricotti, Massimo; Zitrin, Adi; Fujimoto, Seiji; Inoue, Akio K; Resseguier, Tom; Rigby, Jane R; Jiménez-Teja, Yolanda; Windhorst, Rogier A; Hashimoto, Takuya; Tamura, Yoichi.
  • Adamo A; Astronomy Department, Stockholm University and Oskar Klein Centre, Stockholm, Sweden. angela.adamo@astro.su.se.
  • Bradley LD; Space Telescope Science Institute (STScI), Baltimore, MD, USA.
  • Vanzella E; Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, INAF, Bologna, Italy.
  • Claeyssens A; Astronomy Department, Stockholm University and Oskar Klein Centre, Stockholm, Sweden.
  • Welch B; Department of Astronomy, University of Maryland, College Park, MD, USA.
  • Diego JM; Astrophysics Science Division, Code 660, NASA Goddard Space Flight Center, Greenbelt, MD, USA.
  • Mahler G; Instituto de Física de Cantabria, CSIC-UC, Santander, Spain.
  • Oguri M; STAR Institute, Liège, Belgium.
  • Sharon K; Centre for Extragalactic Astronomy, Durham University, Durham, UK.
  • Abdurro'uf; Institute for Computational Cosmology, Durham University, Durham, UK.
  • Hsiao TY; Center for Frontier Science, Chiba University, Chiba, Japan.
  • Xu X; Department of Physics, Graduate School of Science, Chiba University, Chiba, Japan.
  • Messa M; Department of Astronomy, University of Michigan, Ann Arbor, MI, USA.
  • Lassen AE; Space Telescope Science Institute (STScI), Baltimore, MD, USA.
  • Zackrisson E; Center for Astrophysical Sciences, Department of Physics and Astronomy, The Johns Hopkins University, Baltimore, MD, USA.
  • Brammer G; Space Telescope Science Institute (STScI), Baltimore, MD, USA.
  • Coe D; Center for Astrophysical Sciences, Department of Physics and Astronomy, The Johns Hopkins University, Baltimore, MD, USA.
  • Kokorev V; Department of Physics and Astronomy, Northwestern University, Evanston, IL, USA.
  • Ricotti M; Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA), Northwestern University, Evanston, IL, USA.
  • Zitrin A; Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, INAF, Bologna, Italy.
  • Fujimoto S; Astronomy Department, Stockholm University and Oskar Klein Centre, Stockholm, Sweden.
  • Inoue AK; Instituto de Física, Departamento de Astronomia, Universe Federal do Rio Grande do Sul, Porto Alegre, Brazil.
  • Resseguier T; Observational Astrophysics, Department of Physics and Astronomy, Uppsala University, Uppsala, Sweden.
  • Rigby JR; Swedish Collegium for Advanced Study, Uppsala, Sweden.
  • Jiménez-Teja Y; Cosmic Dawn Center (DAWN), Copenhagen, Denmark.
  • Windhorst RA; Niels Bohr Institute, University of Copenhagen, Copenhagen, Denmark.
  • Hashimoto T; Space Telescope Science Institute (STScI), Baltimore, MD, USA.
  • Tamura Y; Center for Astrophysical Sciences, Department of Physics and Astronomy, The Johns Hopkins University, Baltimore, MD, USA.
Nature ; 632(8025): 513-516, 2024 Aug.
Article en En | MEDLINE | ID: mdl-38914113
ABSTRACT
The Cosmic Gems arc is among the brightest and highly magnified galaxies observed at redshift z ≈ 10.2 (ref. 1). However, it is an intrinsically ultraviolet faint galaxy, in the range of those now thought to drive the reionization of the Universe2-4. Hitherto the smallest features resolved in a galaxy at a comparable redshift are between a few hundreds and a few tens of parsecs (pc)5,6. Here we report JWST observations of the Cosmic Gems. The light of the galaxy is resolved into five star clusters located in a region smaller than 70 pc. They exhibit minimal dust attenuation and low metallicity, ages younger than 50 Myr and intrinsic masses of about 106M⊙. Their lensing-corrected sizes are approximately 1 pc, resulting in stellar surface densities near 105M⊙ pc-2, three orders of magnitude higher than typical young star clusters in the local Universe7. Despite the uncertainties inherent to the lensing model, they are consistent with being gravitationally bound stellar systems, that is, proto-globular clusters. We conclude that star cluster formation and feedback likely contributed to shaping the properties of galaxies during the epoch of reionization.
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Texto completo: 1 Banco de datos: MEDLINE Idioma: En Año: 2024 Tipo del documento: Article
Texto completo
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PubMed Links
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Texto completo: 1 Banco de datos: MEDLINE Idioma: En Año: 2024 Tipo del documento: Article