Home > Research > Publications & Outputs > Evidence for Extended Hydrogen-Poor CSM in the ...

Links

Text available via DOI:

View graph of relations

Evidence for Extended Hydrogen-Poor CSM in the Three-Peaked Light Curve of Stripped Envelope Ib Supernova

Research output: Contribution to Journal/MagazineJournal article

Published
  • Yossef Zenati
  • Qinan Wang
  • Alexey Bobrick
  • Lindsay DeMarchi
  • Hila Glanz
  • Mor Rozner
  • Armin Rest
  • Brian D Metzger
  • Raffaella Margutti
  • Sebastian Gomez
  • Nathan Smith
  • Silvia Toonen
  • Joe S Bright
  • Colin Norman
  • Ryan J Foley
  • Alexander Gagliano
  • Julian H Krolik
  • Stephen J Smartt
  • Ashley V Villar
  • Gautham Narayan
  • Ori Fox
  • Katie Auchettl
  • Daniel Brethauer
  • Alejandro Clocchiatti
  • Sophie V Coelln
  • Deanne L Coppejans
  • Andris Doroszmai
  • Maria Drout
  • Wynn Jacobson-Galan
  • Bore Gao
  • Ryan Ridden-Harper
  • Charles Donald Kilpatrick
  • Tanmoy Laskar
  • David Matthews
  • Sofia Rest
  • Ken W Smith
  • Candice McKenzie Stauffer
  • Michael C Stroh
  • Louis-Gregory Strolger
  • Giacomo Terreran
  • Justin D R Pierel
  • Anthony L Piro
Close
<mark>Journal publication date</mark>14/07/2022
<mark>Journal</mark>arXiv
Publication StatusPublished
<mark>Original language</mark>English

Abstract

We present multi-band ATLAS photometry for SN 2019tsf, a stripped-envelope Type Ib supernova (SESN). The SN shows a triple-peaked light curve and a late (re-)brightening, making it unique among stripped-envelope systems. The re-brightening observations represent the latest photometric measurements of a multi-peaked Type Ib SN to date. As late-time photometry and spectroscopy suggest no hydrogen, the potential circumstellar material (CSM) must be H-poor. Moreover, late (>150 days) spectra show no signs of narrow emission lines, further disfavouring CSM interaction. On the contrary, an extended CSM structure is seen through a follow-up radio campaign with Karl G. Jansky Very Large Array (VLA), indicating a source of bright optically thick radio emission at late times, which is highly unusual among H-poor SESNe. We attribute this phenomenology to an interaction of the supernova ejecta with spherically-asymmetric CSM, potentially disk-like, and we present several models that can potentially explain the origin of this rare Type Ib supernova. The warped disc model paints a novel picture, where the tertiary companion perturbs the progenitors CSM, that can explain the multi-peaked light curves of SNe, and here we apply it to SN 2019tsf. This SN 2019tsf is likely a member of a new sub-class of Type Ib SNe and among the recently discovered class of SNe that undergo mass transfer at the moment of explosion