Multiwavelength observations of the Type IIb supernova 2009mg

Authors

  • S. R. Oates,

    Corresponding author
    1. Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Dorking, Surrey RH5 6NT
      E-mail: sro@mssl.ucl.ac.uk
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  • A. J. Bayless,

    1. Space Science and Engineering, Division 15, Southwest Research Institute, Building 263, 6220 Culebra Road, San Antonio, TX 78238, USA
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  • M. D. Stritzinger,

    1. Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark
    2. Department of Astronomy, The Oskar Klein Centre, Department of Astronomy, Stockholm University, AlbaNova, 10691 Stockholm, Sweden
    3. Carnegie Observatories, Las Campanas Observatory, La Serena, Chile
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  • T. Prichard,

    1. Space Science and Engineering, Division 15, Southwest Research Institute, Building 263, 6220 Culebra Road, San Antonio, TX 78238, USA
    2. Department of Astronomy and Astrophysics, Pennsylvania State University, 104 Davey Laboratory, University Park, PA 16802, USA
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  • J. L. Prieto,

    1. Department of Astrophysical Sciences, Princeton University, Peyton Hall, Princeton, NJ 08544, USA
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  • S. Immler,

    Corresponding author
    1. Department of Astronomy, University of Maryland, College Park, MD 20742, USA
    2. Astrophysics Science Division, Code 660.1, NASA Goddard Space Flight Centre, 8800 Greenbelt Road, Greenbelt, MD 20771, USA
    3. Centre for Research and Exploration in Space Science and Technology Code 668.8 8800, Greenbelt Road Goddard Space Flight Centre, Greenbelt, MD 20771, USA
      Hubble, Carnegie-Princeton Fellow.
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  • P. J. Brown,

    1. Department of Physics & Astronomy, University of Utah, 115 South 1400 East #201, Salt Lake City, UT 84112, USA
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  • A. A. Breeveld,

    1. Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Dorking, Surrey RH5 6NT
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  • M. De Pasquale,

    1. Department of Physics and Astronomy, University of Nevada, Las Vegas 4505 S. Maryland Parkway, Las Vegas, NV 89154, USA
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  • N. P. M. Kuin,

    1. Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Dorking, Surrey RH5 6NT
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  • M. Hamuy,

    1. Departamento de Astronomía, Universidad de Chile, Santiago, Chile
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  • S. T. Holland,

    1. Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
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  • F. Taddia,

    1. Department of Astronomy, The Oskar Klein Centre, Department of Astronomy, Stockholm University, AlbaNova, 10691 Stockholm, Sweden
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  • P. W. A. Roming

    1. Space Science and Engineering, Division 15, Southwest Research Institute, Building 263, 6220 Culebra Road, San Antonio, TX 78238, USA
    2. Department of Astronomy and Astrophysics, Pennsylvania State University, 104 Davey Laboratory, University Park, PA 16802, USA
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  • This paper includes data gathered with the 6.5-m Magellan telescopes located at Las Campanas Observatory, Chile, and the Gemini Observatory, Cerro Pachon, Chile (Gemini Programmes GS-2009B-Q-9, GS-2009B-Q-40 and GS-2009B-Q-67).

E-mail: sro@mssl.ucl.ac.uk

Hubble, Carnegie-Princeton Fellow.

ABSTRACT

We present Swift Ultra-Violet Optical Telescope and X-Ray Telescope (XRT) observations, and visual wavelength spectroscopy of the Type IIb supernova (SN) 2009mg, discovered in the Sb galaxy ESO 121-G26. The observational properties of SN 2009mg are compared to the prototype Type IIb SNe 1993J and 2008ax, with which we find many similarities. However, minor differences are discernible including SN 2009mg not exhibiting an initial fast decline or u-band upturn as observed in the comparison objects, and its rise to maximum is somewhat slower leading to slightly broader light curves. The late-time temporal index of SN 2009mg, determined from 40 d post-explosion, is consistent with the decay rate of SN 1993J, but inconsistent with the decay of 56Co. This suggests leakage of γ-rays out of the ejecta and a stellar mass on the small side of the mass distribution. Our XRT non-detection provides an upper limit on the mass-loss rate of the progenitor of inline image. Modelling of the SN light curve indicates a kinetic energy of inline image, an ejecta mass of inline image and a 56Ni mass of 0.10 ± 0.01 M.

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