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Xiang, Danfeng; Wang, Xiaofeng; Lin, Weili; Mo, Jun; Lin, Han; Burke, Jamison; Hiramatsu, Daichi; Hosseinzadeh, Griffin; Howell, D. Andrew; McCully, Curtis; Valenti, Stefan; Vinkó, József; Wheeler, J. Craig; Ehgamberdiev, Shuhrat A.; Mirzaqulov, Davron; Bódi, Attila; Bognár, Zsófia; Cseh, Borbála; Hanyecz, Ottó; Ignácz, Bernadett; Kalup, Csilla; Könyves-Tóth, Réka; Kriskovics, Levente; Ordasi, András; [...]

The Peculiar Transient AT2018cow: A Possible Origin of a Type Ibn/IIn Supernova

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  • Medientyp: E-Artikel
  • Titel: The Peculiar Transient AT2018cow: A Possible Origin of a Type Ibn/IIn Supernova
  • Beteiligte: Xiang, Danfeng; Wang, Xiaofeng; Lin, Weili; Mo, Jun; Lin, Han; Burke, Jamison; Hiramatsu, Daichi; Hosseinzadeh, Griffin; Howell, D. Andrew; McCully, Curtis; Valenti, Stefan; Vinkó, József; Wheeler, J. Craig; Ehgamberdiev, Shuhrat A.; Mirzaqulov, Davron; Bódi, Attila; Bognár, Zsófia; Cseh, Borbála; Hanyecz, Ottó; Ignácz, Bernadett; Kalup, Csilla; Könyves-Tóth, Réka; Kriskovics, Levente; Ordasi, András; [...]
  • Erschienen: American Astronomical Society, 2021
  • Erschienen in: The Astrophysical Journal
  • Sprache: Nicht zu entscheiden
  • DOI: 10.3847/1538-4357/abdeba
  • ISSN: 0004-637X; 1538-4357
  • Schlagwörter: Space and Planetary Science ; Astronomy and Astrophysics
  • Entstehung:
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  • Beschreibung: <jats:title>Abstract</jats:title> <jats:p>We present our photometric and spectroscopic observations of the peculiar transient AT2018cow. The multiband photometry covers from peak to ∼70 days, and the spectroscopy ranges from 5 to ∼50 days. The rapid rise (<jats:italic>t</jats:italic> <jats:sub>r</jats:sub> ≲ 2.9 days), high luminosity (<jats:italic>M</jats:italic> <jats:sub> <jats:italic>V</jats:italic>,peak</jats:sub> ∼ −20.8 mag), and fast decline after peak make AT2018cow stand out from any other optical transients, whereas we find that its light curves show a high resemblance to those of Type Ibn supernovae. Moreover, the spectral energy distribution remains at a high temperature of ∼14,000 K at <jats:italic>t</jats:italic> &gt; 15 days after discovery. The spectra are featureless in the first 10 days, while some broad emission lines due to H, He, C, and O emerge later, with velocity declining from ∼14,000 to ∼3000 km s<jats:sup>−1</jats:sup> at the end of our observations. Narrow and weak He <jats:sc>I</jats:sc> emission lines emerge in the spectra at <jats:italic>t</jats:italic> &gt; 20 days after discovery. These emission lines are reminiscent of the features seen in interacting supernovae like the Type Ibn and IIn subclasses. We fit the bolometric light curves with a model of circumstellar interaction and radioactive decay of <jats:sup>56</jats:sup>Ni and find a good fit with ejecta mass <jats:italic>M</jats:italic> <jats:sub>ej</jats:sub> ∼ 3.16 <jats:italic>M</jats:italic> <jats:sub>⊙</jats:sub>, circumstellar medium (CSM) mass <jats:italic>M</jats:italic> <jats:sub>CSM</jats:sub> ∼ 0.04 <jats:italic>M</jats:italic> <jats:sub>⊙</jats:sub>, and ejected <jats:sup>56</jats:sup>Ni mass <jats:inline-formula> <jats:tex-math> <?CDATA ${M}_{{}^{56}\mathrm{Ni}}\sim 0.23$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjabdebaieqn1.gif" xlink:type="simple" /> </jats:inline-formula> <jats:italic>M</jats:italic> <jats:sub>⊙</jats:sub>. The CSM shell might be formed in an eruptive mass ejection of the progenitor star. Furthermore, the host environment of AT2018cow implies a connection of AT2018cow with massive stars. Combining observational properties and the light-curve fitting results, we conclude that AT2018cow might be a peculiar interacting supernova that originated from a massive star.</jats:p>
  • Zugangsstatus: Freier Zugang