The peculiar mass-loss history of SN 2014C as revealed through AMI radio observations

Research output: Contribution to journalArticle

  • External authors:
  • G E Anderson
  • A Horesh
  • KP Mooley
  • AP Rushton
  • R P Fender
  • T. D. Staley
  • P J {Hancock}
  • MA Perez-Torres
  • Y. Perrott
  • RM Plotkin
  • Magaretha L. Pretorius
  • C Rumsey
  • D. J. Titterington

Abstract

We present a radio light curve of supernova (SN) 2014C taken with the Arcminute Microkelvin Imager (AMI) Large Array at 15.7 GHz. Optical observations presented by Milisavljevic et al. demonstrated that SN 2014C metamorphosed from a stripped- envelope Type Ib SN into a strongly interacting Type IIn SN within 1 year. The AMI light curve clearly shows two distinct radio peaks, the second being a factor of 4 times more luminous than the rst peak. This double bump morphology indicates two distinct phases of mass-loss from the progenitor star with the transition between density regimes occurring at 100-200 days. This reinforces the interpretation that SN 2014C exploded in a low density region before encountering a dense Hydrogen-rich shell of circumstellar material that was likely ejected by the progenitor prior to the explosion. The AMI ux measurements of the rst light curve bump are the only
reported observations taken within 50 to 125 days post-explosion, before the blast-wave encountered the Hydrogen shell. Simplistic synchrotron self-absorption (SSA) and free-free absorption (FFA) modelling suggest that some physical properties of SN 2014C, such as the mass-loss rate, are consistent with the properties of other Type Ibc and IIn SNe. However, our single frequency data does not allow us to distinguish between these two models, which implies they are likely too simplistic to describe the complex environment surrounding this event. Lastly, we present the precise radio location of SN 2014C obtained with eMERLIN, which will be useful for future VLBI observations of the SN.

Bibliographical metadata

Original languageEnglish
JournalMonthly Notices of the Royal Astronomical Society
Early online date24 Dec 2016
DOIs
StatePublished - 2017