Dust Signatures from Late-time Infrared and Optical Observations of SN 1998S

Details Dust Signatures from Late-time Infrared and Optical Observations of SN 1998S Dust Signatures from Late-time Infrared and Optical Observations of SN 1998S

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aspc..342..337p&link_type=abstract

1604-2004: Supernovae as Cosmological Lighthouses, ASP Conference Series, Vol. 342, Proceedings of the conference held 15-19 Jun

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We present late-time IR (1-5 µm) and optical observations of the type IIn SN 1998S up to about 1200 days post-explosion. The shape and evolution of the Hα and He I 1.083 µm line profiles indicate a powerful interaction with a massive progenitor wind and provide evidence of dust condensation within the ejecta. 1.5-2.5 µm spectra and HKL'M' photometry reveal strong IR emission due to hot dust in the ejecta and/or circumstellar medium (CSM). For the origin of the IR emission we favour dust condensation (at least 10^{-3} M_{sun}) in a cool dense shell (CDS) as the main IR source but do not rule out a contribution from the CSM. The late-time evolution of the intrinsic (K-L') colour of type II supernovae (SNe) may be a potentially useful tool for determining the presence or absence of a massive CSM around their progenitors.

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