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Optical studies of SN 2009jf: a Type Ib supernova with an extremely slow decline and aspherical signature

Authors

  • D. K. Sahu,

    Corresponding author
    1. Indian Institute of Astrophysics, Koramangala, Bangalore 560034, India
      E-mail: dks@iiap.res.in (DKS); uday@iiap.res.in (UKG); gca@iiap.res.in (GCA); nomoto@astron.s.u-tokyo.ac.jp (KN)
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  • U. K. Gurugubelli,

    Corresponding author
    1. Indian Institute of Astrophysics, Koramangala, Bangalore 560034, India
    2. Joint Astronomy Programme, Indian Institute of Science, Bangalore 560012, India
      E-mail: dks@iiap.res.in (DKS); uday@iiap.res.in (UKG); gca@iiap.res.in (GCA); nomoto@astron.s.u-tokyo.ac.jp (KN)
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  • G. C. Anupama,

    Corresponding author
    1. Indian Institute of Astrophysics, Koramangala, Bangalore 560034, India
      E-mail: dks@iiap.res.in (DKS); uday@iiap.res.in (UKG); gca@iiap.res.in (GCA); nomoto@astron.s.u-tokyo.ac.jp (KN)
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  • K. Nomoto

    Corresponding author
    1. Institute for the Physics and Mathematics of the Universe, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
      E-mail: dks@iiap.res.in (DKS); uday@iiap.res.in (UKG); gca@iiap.res.in (GCA); nomoto@astron.s.u-tokyo.ac.jp (KN)
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E-mail: dks@iiap.res.in (DKS); uday@iiap.res.in (UKG); gca@iiap.res.in (GCA); nomoto@astron.s.u-tokyo.ac.jp (KN)

ABSTRACT

Optical UBVRI photometry and medium-resolution spectroscopy of the Type Ib supernova SN 2009jf, during the period from ∼ −15 to +250 d, with respect to the B maximum are reported. The light curves are broad, with an extremely slow decline. The early post-maximum decline rate in the V band is similar to SN 2008D; however, the late-phase decline rate is slower than other Type Ib supernovae studied. With an absolute magnitude of MV=−17.96 ± 0.19 at peak, SN 2009jf is a normally bright supernova. The peak bolometric luminosity and the energy deposition rate via the 56Ni 56Co chain indicate that ∼0.17+0.03−0.03 M of 56Ni was ejected during the explosion. The He i 5876 Å line is clearly identified in the first spectrum of day ∼ −15, at a velocity of ∼16 000 km s−1. The [O i] 6300–6364 Å line seen in the nebular spectrum has a multipeaked and asymmetric emission profile, with the blue peak being stronger. The estimated flux in this line implies that ≳1.34 M oxygen was ejected. The slow evolution of the light curves of SN 2009jf indicates the presence of a massive ejecta. The high expansion velocity in the early phase and broader emission lines during the nebular phase suggest it to be an explosion with a large kinetic energy. A simple qualitative estimate leads to the ejecta mass of Mej= 4–9 M and kinetic energy EK= 3–8 × 1051 erg. The ejected mass estimate is indicative of an initial main-sequence mass of ≳20–25 M.

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