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JWST detection of a supernova associated with GRB 221009A without an r-process signature.

التفاصيل البيبلوغرافية
العنوان: JWST detection of a supernova associated with GRB 221009A without an r-process signature.
المؤلفون: Blanchard PK; Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA), Northwestern University, Evanston, IL USA., Villar VA; Center for Astrophysics | Harvard & Smithsonian, Cambridge, MA USA., Chornock R; Department of Astronomy, University of California, Berkeley, CA USA., Laskar T; Department of Physics & Astronomy, University of Utah, Salt Lake City, UT USA.; Department of Astrophysics/IMAPP, Radboud University, Nijmegen, The Netherlands., Li Y; Department of Astronomy & Astrophysics, The Pennsylvania State University, University Park, PA USA.; Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA USA., Leja J; Department of Astronomy & Astrophysics, The Pennsylvania State University, University Park, PA USA.; Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA USA.; Institute for Computational & Data Sciences, The Pennsylvania State University, University Park, PA USA., Pierel J; Space Telescope Science Institute, Baltimore, MD USA., Berger E; Center for Astrophysics | Harvard & Smithsonian, Cambridge, MA USA., Margutti R; Department of Astronomy, University of California, Berkeley, CA USA.; Department of Physics, University of California, Berkeley, CA USA., Alexander KD; Department of Astronomy/Steward Observatory, Tucson, AZ USA., Barnes J; Kavli Institute for Theoretical Physics, University of California, Santa Barbara, CA USA., Cendes Y; Center for Astrophysics | Harvard & Smithsonian, Cambridge, MA USA., Eftekhari T; Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA), Northwestern University, Evanston, IL USA., Kasen D; Department of Physics, University of California, Berkeley, CA USA., LeBaron N; Department of Astronomy, University of California, Berkeley, CA USA., Metzger BD; Department of Physics and Columbia Astrophysics Laboratory, Columbia University, New York, NY USA.; Center for Computational Astrophysics, Flatiron Institute, New York, NY USA., Muzerolle Page J; Space Telescope Science Institute, Baltimore, MD USA., Rest A; Space Telescope Science Institute, Baltimore, MD USA., Sears H; Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA), Northwestern University, Evanston, IL USA.; Department of Physics and Astronomy, Northwestern University, Evanston, IL USA., Siegel DM; Institute of Physics, University of Greifswald, Greifswald, Germany.; Department of Physics, University of Guelph, Guelph, Ontario Canada., Yadavalli SK; Center for Astrophysics | Harvard & Smithsonian, Cambridge, MA USA.
المصدر: Nature astronomy [Nat Astron] 2024; Vol. 8 (6), pp. 774-785. Date of Electronic Publication: 2024 Apr 12.
نوع المنشور: Journal Article
اللغة: English
بيانات الدورية: Publisher: Springer Nature Country of Publication: England NLM ID: 101738506 Publication Model: Print-Electronic Cited Medium: Internet ISSN: 2397-3366 (Electronic) Linking ISSN: 23973366 NLM ISO Abbreviation: Nat Astron Subsets: PubMed not MEDLINE
أسماء مطبوعة: Original Publication: [London] : Springer Nature, [2017]-
مستخلص: Identifying the sites of r-process nucleosynthesis, a primary mechanism of heavy element production, is a key goal of astrophysics. The discovery of the brightest gamma-ray burst (GRB) to date, GRB 221009A, presented an opportunity to spectroscopically test the idea that r-process elements are produced following the collapse of rapidly rotating massive stars. Here we present James Webb Space Telescope observations of GRB 221009A obtained +168 and +170 rest-frame days after the gamma-ray trigger, and demonstrate that they are well described by a SN 1998bw-like supernova (SN) and power-law afterglow, with no evidence for a component from r-process emission. The SN, with a nickel mass of approximately 0.09  M ⊙ , is only slightly fainter than the brightness of SN 1998bw at this phase, which indicates that the SN is not an unusual GRB-SN. This demonstrates that the GRB and SN mechanisms are decoupled and that highly energetic GRBs are not likely to produce significant quantities of r-process material, which leaves open the question of whether explosions of massive stars are key sources of r-process elements. Moreover, the host galaxy of GRB 221009A has a very low metallicity of approximately 0.12  Z ⊙ and strong H 2 emission at the explosion site, which is consistent with recent star formation, hinting that environmental factors are responsible for its extreme energetics.
Competing Interests: Competing interestsThe authors declare no competing interests.
(© The Author(s) 2024.)
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فهرسة مساهمة: Keywords: High-energy astrophysics; Time-domain astronomy; Transient astrophysical phenomena
تواريخ الأحداث: Date Created: 20240624 Latest Revision: 20240625
رمز التحديث: 20240625
مُعرف محوري في PubMed: PMC11189819
DOI: 10.1038/s41550-024-02237-4
PMID: 38912294
قاعدة البيانات: MEDLINE
الوصف
تدمد:2397-3366
DOI:10.1038/s41550-024-02237-4