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Radio Monitoring of Supernova 2001ig: The First Year

Published online by Cambridge University Press:  19 September 2016

Stuart D. Ryder
Affiliation:
Anglo-Australian Observatory, P.O. Box 296, Epping, NSW 1710, Australia; sdr@aaoepp.aao.gov.au
Elaine Sadler
Affiliation:
School of Physics, University of Sydney, NSW 2006, Australia;ems@physics.usyd.edu.au
Ravi Subrahmanyan
Affiliation:
Australia Telescope National Facility, CSIRO, Locked Bag 194, Narrabri, NSW 2390, Australia;Ravi.Subrahmanyan@csiro.au
Kurt W. Weiler
Affiliation:
Naval Research Laboratory, Code 7213 Washington, DC 20375-5320, USA;Kurt.Weiler@nrl.navy.mil
Nino Panagia
Affiliation:
ESA/Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA;panagia@stsci.edu
Christopher Stockdale
Affiliation:
Naval Research Laboratory, Code 7213 Washington, DC 20375-5320, USA;Kurt.Weiler@nrl.navy.mil Physics Dept., Marquette University, P.O. Box 1881 Milwaukee, WI 53201, USA;Christopher.Stockdale@marquette.edu

Summary

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Supernova 2001ig in NGC 7424 has been observed with the Australia Telescope Compact Array at ~2 week intervals since its discovery, making this the best-studied Type IIb radio supernova since SN 1993J. We present radio light curves for frequencies from 1.4 to 20 GHz, and preliminary attempts to model the observed behavior. Since peaking in radio luminosity at 8.6 and 4.8 GHz some 1-2 months after the explosion, SN 2001ig has on at least two occasions deviated significantly from a smooth decline, indicative of interaction with a dense circumstellar medium and possibly of periodic progenitor mass-loss.

Type
Part I Supernovae: Individual
Copyright
Copyright © Springer-Verlag 2005

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