SN 2017gci: a nearby Type I Superluminous Supernova with a bumpy tail

Research output: Contribution to journalArticlepeer-review

Authors

  • A Fiore
  • T-W Chen
  • A Jerkstrand
  • S Benetti
  • R Ciolfi
  • C Inserra
  • E Cappellaro
  • A Pastorello
  • G Leloudas
  • S Schulze
  • M Berton
  • J Burke
  • C McCully
  • W Fong
  • L Galbany
  • M Gromadzki
  • C P Gutiérrez
  • D Hiramatsu
  • G Hosseinzadeh
  • D A Howell
  • E Kankare
  • R Lunnan
  • T E Müller-Bravo
  • D O’ Neill
  • A Rau
  • J Sollerman
  • G Terreran
  • S Valenti
  • D R Young

Colleges, School and Institutes

Abstract

We present and discuss the optical spectrophotometric observations of the nearby (z = 0.087) Type I superluminous supernova (SLSN I) SN 2017gci, whose peak K-corrected absolute magnitude reaches Mg = −21.5 mag. Its photometric and spectroscopic evolution includes features of both slow- and of fast-evolving SLSN I, thus favoring a continuum distribution between the two SLSN-I subclasses. In particular, similarly to other SLSNe I, the multiband light curves (LCs) of SN 2017gci show two re-brightenings at about 103 and 142 d after the maximum light. Interestingly, this broadly agrees with a broad emission feature emerging around 6520 Å after ∼51 d from the maximum light, which is followed by a sharp knee in the LC. If we interpret this feature as Hα, this could support the fact that the bumps are the signature of late interactions of the ejecta with a (hydrogen-rich) circumstellar material. Then we fitted magnetar- and CSM-interaction-powered synthetic LCs on to the bolometric one of SN 2017gci. In the magnetar case, the fit suggests a polar magnetic field Bp ≃ 6 × 1014 G, an initial period of the magnetar Pinitial ≃ 2.8 ms, an ejecta mass Mejecta≃9M and an ejecta opacity κ≃0.08cm2g−1⁠. A CSM-interaction scenario would imply a CSM mass ≃5M and an ejecta mass ≃12M⁠. Finally, the nebular spectrum of phase + 187 d was modeled, deriving a mass of ∼10M for the ejecta. Our models suggest that either a magnetar or CSM interaction might be the power sources for SN 2017gci and that its progenitor was a massive (⁠40M⁠) star.

Details

Original languageEnglish
Pages (from-to)2120–2139
Number of pages20
JournalMonthly Notices of the Royal Astronomical Society
Volume502
Issue number2
Early online date5 Jan 2021
Publication statusPublished - Apr 2021

Keywords

  • Transients: supernovae, supernova: general, supernovae: individual: SN 2017gci