Radio observations reveal unusual circumstellar environments for some TYPEIbc supernova progenitors

Abstract

We present extensive radio observations of the nearby TypeIbc supernovae (SNeIbc) 2004cc, 2004dk, and 2004gq spanning Δt 8-1900days after explosion. Using a dynamical model developed for synchrotron emission from a slightly decelerated shock wave, we estimate the velocity and energy of the fastest ejecta and the density profile of the circumstellar medium. The shock waves of all three supernovae are characterized by non-relativistic velocities of and associated energies of E (2-10) × 1047erg, in line with the expectations for a typical homologous explosion. Smooth circumstellar density profiles are indicated by the early radio data and we estimate the progenitor mass-loss rates to be (wind velocity, vw = 103 km s-1). These estimates approach the saturation limit () for line-driven winds from Wolf-Rayet stars, the favored progenitors of SNeIbc including those associated with long-duration gamma-ray bursts. Intriguingly, at later epochs all three supernovae show evidence for abrupt radio variability that we attribute to large density modulations (factor of 3-6) at circumstellar radii of r (1-50) × 1016cm. If due to variable mass loss, these modulations are associated with progenitor activity on a timescale of 10-100years before explosion. We consider these results in the context of variable mass-loss mechanisms including wind clumping, metallicity-independent continuum-driven ejections, and binary-induced modulations. It may also be possible that the SN shock waves are dynamically interacting with wind termination shocks; however, this requires the environment to be highly pressurized and/or the progenitor to be rapidly rotating prior to explosion. The proximity of the density modulations to the explosion sites may suggest a synchronization between unusual progenitor mass loss and the SN explosion, reminiscent of TypeIIn supernovae. This study underscores the utility of radio observations for tracing the final evolutionary stage(s) of SN progenitor systems. © 2012. The American Astronomical Society. All rights reserved..