Near-infrared Observations Of The Type Iin Sn 2005ip: The Case For Dust Condensation

Details Near-infrared Observations Of The Type Iin Sn 2005ip: The Case For Dust Condensation Near-infrared Observations Of The Type Iin Sn 2005ip: The Case For Dust Condensation

Jan 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21349002f&link_type=abstract

American Astronomical Society, AAS Meeting #213, #490.02; Bulletin of the American Astronomical Society, Vol. 41, p.465

Astronomy and Astrophysics

Astronomy

Scientific paper

Near-infrared observations of the Type IIn SN 2005ip in NGC 2906 reveal large fluxes (>1.3 mJy) in the Ks-band over more than 900 days. While warm dust can explain the late-time Ks-band emission of SN 2005ip, the nature of the dust heating source is ambiguous. Shock heating of pre-existing dust by post-shocked gas is unlikely because the forward shock is moving too slowly to have traversed the expected dust-free cavity by the time observations first reveal the Ks emission. While an infrared light echo model correctly predicts a near-infrared luminosity plateau, heating dust to the observed temperatures of 1400-1600 K at a relatively large distance from the supernova (>1018 cm) requires an extraordinarily high early supernova luminosity ( 1 x 1011 Lsolar). The evidence instead favors condensing dust in the cool, dense shell between the forward and reverse shocks. Both the initial dust temperature and the evolutionary trend towards lower temperatures are consistent with this scenario. We infer that radiation from the circumstellar interaction heats the dust. Near and mid-infrared spectra support this scenario and reveal evidence of PAH formation. Observations of dust and PAH formation in SNe are sparse, so these results provide a rare opportunity to consider SNe Type IIn as sources of dust in our universe.

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