The Astrophysical Journal (Jan 2023)

Near-infrared and Optical Observations of Type Ic SN 2021krf: Luminous Late-time Emission and Dust Formation

  • Aravind P. Ravi,
  • Jeonghee Rho,
  • Sangwook Park,
  • Seong Hyun Park,
  • Sung-Chul Yoon,
  • T. R. Geballe,
  • Jozsef Vinkó,
  • Samaporn Tinyanont,
  • K. Azalee Bostroem,
  • Jamison Burke,
  • Daichi Hiramatsu,
  • D. Andrew Howell,
  • Curtis McCully,
  • Megan Newsome,
  • Estefania Padilla Gonzalez,
  • Craig Pellegrino,
  • Regis Cartier,
  • Tyler Pritchard,
  • Morten Andersen,
  • Sergey Blinnikov,
  • Yize Dong,
  • Peter Blanchard,
  • Charles D. Kilpatrick,
  • Peter Hoeflich,
  • Stefano Valenti,
  • Alexei V. Filippenko,
  • Nicholas B. Suntzeff,
  • Ji Yeon Seok,
  • R. Könyves-Tóth,
  • Ryan J. Foley,
  • Matthew R. Siebert,
  • David O. Jones

DOI
https://doi.org/10.3847/1538-4357/accddc
Journal volume & issue
Vol. 950, no. 1
p. 14

Abstract

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We present near-infrared (NIR) and optical observations of the Type Ic supernova (SN Ic) SN 2021krf obtained between days 13 and 259 at several ground-based telescopes. The NIR spectrum at day 68 exhibits a rising K -band continuum flux density longward of ∼2.0 μ m, and a late-time optical spectrum at day 259 shows strong [O i ] 6300 and 6364 Å emission-line asymmetry, both indicating the presence of dust, likely formed in the SN ejecta. We estimate a carbon-grain dust mass of ∼2 × 10 ^−5 M _⊙ and a dust temperature of ∼900–1200 K associated with this rising continuum and suggest the dust has formed in SN ejecta. Utilizing the one-dimensional multigroup radiation-hydrodynamics code STELLA, we present two degenerate progenitor solutions for SN 2021krf, characterized by C–O star masses of 3.93 and 5.74 M _⊙ , but with the same best-fit ^56 Ni mass of 0.11 M _⊙ for early times (0–70 days). At late times (70–300 days), optical light curves of SN 2021krf decline substantially more slowly than those expected from ^56 Co radioactive decay. Lack of H and He lines in the late-time SN spectrum suggests the absence of significant interaction of the ejecta with the circumstellar medium. We reproduce the entire bolometric light curve with a combination of radioactive decay and an additional powering source in the form of a central engine of a millisecond pulsar with a magnetic field smaller than that of a typical magnetar.

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