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The complex circumstellar environment of supernova 2023ixf.
Zimmerman, E A; Irani, I; Chen, P; Gal-Yam, A; Schulze, S; Perley, D A; Sollerman, J; Filippenko, A V; Shenar, T; Yaron, O; Shahaf, S; Bruch, R J; Ofek, E O; De Cia, A; Brink, T G; Yang, Y; Vasylyev, S S; Ben Ami, S; Aubert, M; Badash, A; Bloom, J S; Brown, P J; De, K; Dimitriadis, G; Fransson, C; Fremling, C; Hinds, K; Horesh, A; Johansson, J P; Kasliwal, M M; Kulkarni, S R; Kushnir, D; Martin, C; Matuzewski, M; McGurk, R C; Miller, A A; Morag, J; Neil, J D; Nugent, P E; Post, R S; Prusinski, N Z; Qin, Y; Raichoor, A; Riddle, R; Rowe, M; Rusholme, B; Sfaradi, I; Sjoberg, K M; Soumagnac, M; Stein, R D.
Afiliación
  • Zimmerman EA; Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot, Israel. erezimm@gmail.com.
  • Irani I; Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot, Israel.
  • Chen P; Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot, Israel.
  • Gal-Yam A; Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot, Israel.
  • Schulze S; The Oskar Klein Centre, Department of Physics, Stockholm University, AlbaNova, Stockholm, Sweden.
  • Perley DA; Astrophysics Research Institute, Liverpool John Moores University, Liverpool, UK.
  • Sollerman J; The Oskar Klein Centre, Department of Astronomy, Stockholm University, AlbaNova, Stockholm, Sweden.
  • Filippenko AV; Department of Astronomy, University of California, Berkeley, Berkeley, CA, USA.
  • Shenar T; Departamento de Astrofísica, Centro de Astrobiología (CSIC-INTA), Madrid, Spain.
  • Yaron O; Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot, Israel.
  • Shahaf S; Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot, Israel.
  • Bruch RJ; Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot, Israel.
  • Ofek EO; School of Physics and Astronomy, Tel Aviv University, Tel Aviv, Israel.
  • De Cia A; Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot, Israel.
  • Brink TG; European Southern Observatory, Garching bei München, Germany.
  • Yang Y; Department of Astronomy, University of Geneva, Versoix, Switzerland.
  • Vasylyev SS; Department of Astronomy, University of California, Berkeley, Berkeley, CA, USA.
  • Ben Ami S; Department of Astronomy, University of California, Berkeley, Berkeley, CA, USA.
  • Aubert M; Physics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing, China.
  • Badash A; Department of Astronomy, University of California, Berkeley, Berkeley, CA, USA.
  • Bloom JS; Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot, Israel.
  • Brown PJ; Université Clermont Auvergne, CNRS/IN2P3, LPC, Clermont-Ferrand, France.
  • De K; Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot, Israel.
  • Dimitriadis G; Department of Astronomy, University of California, Berkeley, Berkeley, CA, USA.
  • Fransson C; Department of Physics and Astronomy, Texas A&M University, College Station, TX, USA.
  • Fremling C; MIT Kavli Institute for Astrophysics and Space Research, Cambridge, MA, USA.
  • Hinds K; School of Physics, Trinity College Dublin, The University of Dublin, Dublin 2, Ireland.
  • Horesh A; The Oskar Klein Centre, Department of Astronomy, Stockholm University, AlbaNova, Stockholm, Sweden.
  • Johansson JP; Caltech Optical Observatories, California Institute of Technology, Pasadena, CA, USA.
  • Kasliwal MM; Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA, USA.
  • Kulkarni SR; Astrophysics Research Institute, Liverpool John Moores University, Liverpool, UK.
  • Kushnir D; The Racah Institute of Physics, The Hebrew University of Jerusalem, Jerusalem, Israel.
  • Martin C; The Oskar Klein Centre, Department of Physics, Stockholm University, AlbaNova, Stockholm, Sweden.
  • Matuzewski M; Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA, USA.
  • McGurk RC; Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA, USA.
  • Miller AA; Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot, Israel.
  • Morag J; Cahill Center for Astronomy and Astrophysics, California Institute of Technology, Pasadena, CA, USA.
  • Neil JD; Cahill Center for Astronomy and Astrophysics, California Institute of Technology, Pasadena, CA, USA.
  • Nugent PE; W. M. Keck Observatory, Kamuela, HI, USA.
  • Post RS; Department of Physics and Astronomy, Northwestern University, Evanston, IL, USA.
  • Prusinski NZ; Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA), Northwestern University, Evanston, IL, USA.
  • Qin Y; Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot, Israel.
  • Raichoor A; Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA, USA.
  • Riddle R; Department of Astronomy, University of California, Berkeley, Berkeley, CA, USA.
  • Rowe M; Lawrence Berkeley National Laboratory, Berkeley, CA, USA.
  • Rusholme B; Post Observatory, Lexington, MA, USA.
  • Sfaradi I; Cahill Center for Astronomy and Astrophysics, California Institute of Technology, Pasadena, CA, USA.
  • Sjoberg KM; Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA, USA.
  • Soumagnac M; Department of Astronomy, University of California, Berkeley, Berkeley, CA, USA.
  • Stein RD; Caltech Optical Observatories, California Institute of Technology, Pasadena, CA, USA.
Nature ; 627(8005): 759-762, 2024 Mar.
Article en En | MEDLINE | ID: mdl-38538936
ABSTRACT
The early evolution of a supernova (SN) can reveal information about the environment and the progenitor star. When a star explodes in vacuum, the first photons to escape from its surface appear as a brief, hours-long shock-breakout flare1,2, followed by a cooling phase of emission. However, for stars exploding within a distribution of dense, optically thick circumstellar material (CSM), the first photons escape from the material beyond the stellar edge and the duration of the initial flare can extend to several days, during which the escaping emission indicates photospheric heating3. Early serendipitous observations2,4 that lacked ultraviolet (UV) data were unable to determine whether the early emission is heating or cooling and hence the nature of the early explosion event. Here we report UV spectra of the nearby SN 2023ixf in the galaxy Messier 101 (M101). Using the UV data as well as a comprehensive set of further multiwavelength observations, we temporally resolve the emergence of the explosion shock from a thick medium heated by the SN emission. We derive a reliable bolometric light curve that indicates that the shock breaks out from a dense layer with a radius substantially larger than typical supergiants.
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Texto completo: 1 Colección: 01-internacional Banco de datos: MEDLINE Idioma: En Revista: Nature Año: 2024 Tipo del documento: Article País de afiliación: Israel
Texto completo
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XML
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Texto completo: 1 Colección: 01-internacional Banco de datos: MEDLINE Idioma: En Revista: Nature Año: 2024 Tipo del documento: Article País de afiliación: Israel