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A recently quenched galaxy 700 million years after the Big Bang.
Looser, Tobias J; D'Eugenio, Francesco; Maiolino, Roberto; Witstok, Joris; Sandles, Lester; Curtis-Lake, Emma; Chevallard, Jacopo; Tacchella, Sandro; Johnson, Benjamin D; Baker, William M; Suess, Katherine A; Carniani, Stefano; Ferruit, Pierre; Arribas, Santiago; Bonaventura, Nina; Bunker, Andrew J; Cameron, Alex J; Charlot, Stephane; Curti, Mirko; de Graaff, Anna; Maseda, Michael V; Rawle, Tim; Rix, Hans-Walter; Del Pino, Bruno Rodríguez; Smit, Renske; Übler, Hannah; Willott, Chris; Alberts, Stacey; Egami, Eiichi; Eisenstein, Daniel J; Endsley, Ryan; Hausen, Ryan; Rieke, Marcia; Robertson, Brant; Shivaei, Irene; Williams, Christina C; Boyett, Kristan; Chen, Zuyi; Ji, Zhiyuan; Jones, Gareth C; Kumari, Nimisha; Nelson, Erica; Perna, Michele; Saxena, Aayush; Scholtz, Jan.
Afiliación
  • Looser TJ; Kavli Institute for Cosmology, University of Cambridge, Cambridge, UK. tjl54@cam.ac.uk.
  • D'Eugenio F; Cavendish Laboratory - Astrophysics Group, University of Cambridge, Cambridge, UK. tjl54@cam.ac.uk.
  • Maiolino R; Kavli Institute for Cosmology, University of Cambridge, Cambridge, UK.
  • Witstok J; Cavendish Laboratory - Astrophysics Group, University of Cambridge, Cambridge, UK.
  • Sandles L; Kavli Institute for Cosmology, University of Cambridge, Cambridge, UK.
  • Curtis-Lake E; Cavendish Laboratory - Astrophysics Group, University of Cambridge, Cambridge, UK.
  • Chevallard J; Department of Physics and Astronomy, University College London, London, UK.
  • Tacchella S; Kavli Institute for Cosmology, University of Cambridge, Cambridge, UK.
  • Johnson BD; Cavendish Laboratory - Astrophysics Group, University of Cambridge, Cambridge, UK.
  • Baker WM; Kavli Institute for Cosmology, University of Cambridge, Cambridge, UK.
  • Suess KA; Cavendish Laboratory - Astrophysics Group, University of Cambridge, Cambridge, UK.
  • Carniani S; Centre for Astrophysics Research, Department of Physics, Astronomy and Mathematics, University of Hertfordshire, Hatfield, UK.
  • Ferruit P; Department of Physics, University of Oxford, Oxford, UK.
  • Arribas S; Kavli Institute for Cosmology, University of Cambridge, Cambridge, UK.
  • Bonaventura N; Cavendish Laboratory - Astrophysics Group, University of Cambridge, Cambridge, UK.
  • Bunker AJ; Center for Astrophysics | Harvard & Smithsonian, Cambridge, MA, USA.
  • Cameron AJ; Kavli Institute for Cosmology, University of Cambridge, Cambridge, UK.
  • Charlot S; Cavendish Laboratory - Astrophysics Group, University of Cambridge, Cambridge, UK.
  • Curti M; Department of Astronomy and Astrophysics, University of California, Santa Cruz, Santa Cruz, CA, USA.
  • de Graaff A; Kavli Institute for Particle Astrophysics and Cosmology (KIPAC), Stanford University, Stanford, CA, USA.
  • Maseda MV; Department of Physics, Stanford University, Stanford, CA, USA.
  • Rawle T; Scuola Normale Superiore, Pisa, Italy.
  • Rix HW; European Space Astronomy Centre (ESAC), European Space Agency (ESA), Madrid, Spain.
  • Del Pino BR; Centro de Astrobiología (CAB), Spanish National Research Council (CSIC)-National Institute of Aerospace Technology (INTA), Madrid, Spain.
  • Smit R; Cosmic Dawn Center (DAWN), Copenhagen, Denmark.
  • Übler H; Niels Bohr Institute, University of Copenhagen, Copenhagen, Denmark.
  • Willott C; Department of Physics, University of Oxford, Oxford, UK.
  • Alberts S; Department of Physics, University of Oxford, Oxford, UK.
  • Egami E; Sorbonne Université, CNRS, UMR 7095, Institut d'Astrophysique de Paris, Paris, France.
  • Eisenstein DJ; Kavli Institute for Cosmology, University of Cambridge, Cambridge, UK.
  • Endsley R; Cavendish Laboratory - Astrophysics Group, University of Cambridge, Cambridge, UK.
  • Hausen R; European Southern Observatory, Garching bei Muenchen, Germany.
  • Rieke M; Max-Planck-Institut für Astronomie, Heidelberg, Germany.
  • Robertson B; Department of Astronomy, University of Wisconsin-Madison, Madison, WI, USA.
  • Shivaei I; European Space Agency (ESA) Office, Space Telescope Science Institute (STScI), Baltimore, MD, USA.
  • Williams CC; Max-Planck-Institut für Astronomie, Heidelberg, Germany.
  • Boyett K; Centro de Astrobiología (CAB), Spanish National Research Council (CSIC)-National Institute of Aerospace Technology (INTA), Madrid, Spain.
  • Chen Z; Astrophysics Research Institute, Liverpool John Moores University, Liverpool, UK.
  • Ji Z; Kavli Institute for Cosmology, University of Cambridge, Cambridge, UK.
  • Jones GC; Cavendish Laboratory - Astrophysics Group, University of Cambridge, Cambridge, UK.
  • Kumari N; NRC Herzberg, Victoria, British Columbia, Canada.
  • Nelson E; Steward Observatory, University of Arizona, Tucson, AZ, USA.
  • Perna M; Steward Observatory, University of Arizona, Tucson, AZ, USA.
  • Saxena A; Center for Astrophysics | Harvard & Smithsonian, Cambridge, MA, USA.
  • Scholtz J; Department of Astronomy, University of Texas at Austin, Austin, TX, USA.
Nature ; 629(8010): 53-57, 2024 May.
Article en En | MEDLINE | ID: mdl-38447669
ABSTRACT
Local and low-redshift (z < 3) galaxies are known to broadly follow a bimodal distribution actively star-forming galaxies with relatively stable star-formation rates and passive systems. These two populations are connected by galaxies in relatively slow transition. By contrast, theory predicts that star formation was stochastic at early cosmic times and in low-mass systems1-4. These galaxies transitioned rapidly between starburst episodes and phases of suppressed star formation, potentially even causing temporary quiescence-so-called mini-quenching events5,6. However, the regime of star-formation burstiness is observationally highly unconstrained. Directly observing mini-quenched galaxies in the primordial Universe is therefore of utmost importance to constrain models of galaxy formation and transformation7,8. Early quenched galaxies have been identified out to redshift z < 5 (refs. 9-12) and these are all found to be massive (M⋆ > 1010 M⊙) and relatively old. Here we report a (mini-)quenched galaxy at z = 7.3, when the Universe was only 700 Myr old. The JWST/NIRSpec spectrum is very blue (U-V = 0.16 ± 0.03 mag) but exhibits a Balmer break and no nebular emission lines. The galaxy experienced a short starburst followed by rapid quenching; its stellar mass (4-6 × 108 M⊙) falls in a range that is sensitive to various feedback mechanisms, which can result in perhaps only temporary quenching.
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Texto completo: 1 Base de datos: MEDLINE Asunto principal: Galaxias Idioma: En Revista: Nature Año: 2024 Tipo del documento: Article
Texto completo
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Texto completo: 1 Base de datos: MEDLINE Asunto principal: Galaxias Idioma: En Revista: Nature Año: 2024 Tipo del documento: Article