[Previous] | [Session 87] | [Next]
C. J. Stockdale (Marquette University), S. D. Van Dyk (IPAC/Cal Tech), K. W. Weiler (NRL), N. Panagia (STScI), R. A. Sramek (NRAO), B. Paczynski (Princeton), M. P. Rupen (NRAO)
Evidence has been accruing that long-duration GRBs may be associated with some extreme Type Ic supernovae (SNe). Theoretically, GRBs originate from directed, relativistic jets. Their afterglows, particularly in the radio, are seen as their beamed jets, while remaining collimated, decelerate and expand significantly once they become non-relativistic. Yet, most GRB jets will not be pointed along our line-of-sight, with detectable \gamma- or X-ray emission, but may still be associated with a SN Ic. In this case, recent predictions have been made that the decelerating jet and counterjet should produce detectable radio emission for several SNe Ibb or Ic per year within 200 Mpc, depending on the jet angle relative to the line-of-sight. Furthermore, the jet angle determines how long after the outburst/explosion radio emission will be detected, even >>1 yr for nearby SNe Ib/c. We have tested this intriguing possibility by observing a significant sample of SNe, with 1 yr \lesssim age \lesssim 10 yr, within 100 Mpc. Preliminary results of this survey will be presented along with their implications.
The author(s) of this abstract have provided an email address for comments about the abstract: christopher.stockdale@marquette.edu
[Previous] | [Session 87] | [Next]
Bulletin of the American Astronomical Society, 35#5
© 2003. The American Astronomical Soceity.