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SN 2008S erupted in early 2008 in the grand design spiral galaxy NGC 6946. The progenitor was detected by Prieto et al. in  Spitzer Space Telescope  images taken over the four years prior to the explosion, but was not detected in deep optical images, from which they inferred a self‐obscured object with a mass of about  10 M ⊙  . We obtained  Spitzer  observations of SN 2008S 5 days after its discovery, as well as coordinated Gemini and  Spitzer  optical and infrared observations 6 months after its outburst.  We have constructed radiative transfer dust models for the object before and after the outburst, using the same   r  −2   density distribution of pre‐existing amorphous carbon grains for all epochs and taking light travel time effects into account. We rule out silicate grains as a significant component of the dust around SN 2008S. The inner radius of the dust shell moved outwards from its pre‐outburst value of 85 au to a post‐outburst value of 1250 au, attributable to grain vaporization by the light flash from SN 2008S. Although this caused the circumstellar extinction to decrease from   A V  = 15  before the outburst to 0.8 after the outburst, we estimate that less than 2 per cent of the overall circumstellar dust mass was destroyed.  The total mass‐loss rate from the progenitor star is estimated to have been  0.5–1.0 × 10 −4  M ⊙  yr −1  . The derived dust‐mass‐loss rate of  5 × 10 −7  M ⊙  yr −1   implies a total dust injection into the interstellar medium of up to  0.01 M ⊙   over the suggested duration of the self‐obscured phase. We consider the potential contribution of objects like SN 2008S to the dust enrichment of galaxies.

The destruction and survival of dust in the shell around SN 2008S