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The lowest-metallicity type II supernova from the highest-mass red supergiant progenitor

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  • معلومة اضافية
    • Contributors:
      Laboratoire d'Astrophysique de Marseille (LAM); Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS); Dark Cosmology Centre (DARK); Niels Bohr Institute [Copenhagen] (NBI); Faculty of Science [Copenhagen]; University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU)-Faculty of Science [Copenhagen]; University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU); Department of Physics [Pittsburgh]; Carnegie Mellon University [Pittsburgh] (CMU); Oskar Klein Centre [Stockholm]; Stockholm University; Institute IMDEA Materials [Madrid]; Institute IMDEA Materials; Federal Institute for Geosciences and Natural Resources (BGR); Aberystwyth University; Astrophysics Research Centre [Belfast] (ARC); Queen's University [Belfast] (QUB); Institut Lavoisier de Versailles (ILV); Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS); University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH)-Faculty of Science [Copenhagen]; University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH)
    • بيانات النشر:
      Nature Publishing Group, 2018.
    • الموضوع:
      2018
    • نبذة مختصرة :
      Red supergiants have been confirmed as the progenitor stars of the majority of hydrogen-rich type II supernovae. However, while such stars are observed with masses >25M$_\odot$, detections of >18M$_\odot$ progenitors remain elusive. Red supergiants are also expected to form at all metallicities, but discoveries of explosions from low-metallicity progenitors are scarce. Here, we report observations of the type II supernova, SN 2015bs, for which we infer a progenitor metallicity of $\leq$0.1Z$_\odot$ from comparison to photospheric-phase spectral models, and a Zero Age Main-Sequence mass of 17-25M$_\odot$ through comparison to nebular-phase spectral models. SN 2015bs displays a normal 'plateau' light-curve morphology, and typical spectral properties, implying a red supergiant progenitor. This is the first example of such a high mass progenitor for a 'normal' type II supernova, suggesting a link between high mass red supergiant explosions and low-metallicity progenitors.
      Accepted for publication in Nature Astronomy. Archive submission includes main text plus one table and three figures, together with Supplementary Information with an additional 12 figures and five tables
    • File Description:
      application/pdf; text
    • ISSN:
      2397-3366
    • الرقم المعرف:
      10.1038/s41550-018-0458-4⟩
    • الرقم المعرف:
      10.1038/s41550-018-0458-4
    • Rights:
      OPEN
    • الرقم المعرف:
      edsair.doi.dedup.....70361d93b4bdb413859de996efae3f34