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Sökning: WFRF:(Itagaki Koichi)

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1.
  • Hosseinzadeh, Griffin, et al. (författare)
  • Short-lived Circumstellar Interaction in the Low-luminosity Type IIP SN 2016bkv
  • 2018
  • Ingår i: Astrophysical Journal. - : American Astronomical Society. - 0004-637X .- 1538-4357. ; 861:1
  • Tidskriftsartikel (refereegranskat)abstract
    • While interaction with circumstellar material is known to play an important role in Type. IIn supernovae (SNe), analyses of the more common SNe IIP and IIL have not traditionally included interaction as a significant power source. However, recent campaigns to observe SNe within days of explosion have revealed narrow emission lines of high-ionization species in the earliest spectra of luminous SNe II of all subclasses. These flash ionization features indicate the presence of a confined shell of material around the progenitor star. Here we present the first low-luminosity (LL) SN to show flash ionization features, SN 2016bkv. This SN peaked at M-V = -16 mag and has Ha expansion velocities under 1350 km s(-1) around maximum light, placing it at the faint/slow end of the distribution of SNe IIP (similar to SN 2005cs). The light-curve shape of SN 2016bkv is also extreme among SNe IIP. A very strong initial peak could indicate additional luminosity from circumstellar interaction. A very small fall from the plateau to the nickel tail indicates unusually large production of radioactive nickel compared to other LL SNe IIP. A comparison between nebular spectra of SN. 2016bkv and models raises the possibility that SN. 2016bkv is an electron-capture supernova.
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2.
  • Hosseinzadeh, Griffin, et al. (författare)
  • The Early Light Curve of SN 2023bee : Constraining Type Ia Supernova Progenitors the Apian Way
  • 2023
  • Ingår i: Astrophysical Journal Letters. - 2041-8205 .- 2041-8213. ; 953:1
  • Tidskriftsartikel (refereegranskat)abstract
    • We present very early photometric and spectroscopic observations of the Type Ia supernova (SN Ia) 2023bee, starting about 8 hr after the explosion, which reveal a strong excess in the optical and nearest UV (U and UVW1) bands during the first several days of explosion. This data set allows us to probe the nature of the binary companion of the exploding white dwarf and the conditions leading to its ignition. We find a good match to the Kasen model in which a main-sequence companion star stings the ejecta with a shock as they buzz past. Models of double detonations, shells of radioactive nickel near the surface, interaction with circumstellar material, and pulsational delayed detonations do not provide good matches to our light curves. We also observe signatures of unburned material, in the form of carbon absorption, in our earliest spectra. Our radio nondetections place a limit on the mass-loss rate from the putative companion that rules out a red giant but allows a main-sequence star. We discuss our results in the context of other similar SNe Ia in the literature.
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