Infrared Study of Supernova Dust and Ejecta

Details Infrared Study of Supernova Dust and Ejecta Infrared Study of Supernova Dust and Ejecta

May 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006sptz.prop30292m&link_type=abstract

Spitzer Proposal ID #30292

Computer Science

Scientific paper

We propose to continue our Spitzer study of supernovae (SNe). Our first goal is to investigate core-collapse supernovae (CCSNe) as the major source of dust in the universe, past or present. Direct evidence in support of this is still very sparse. Warm grains emit most strongly in the mid-IR and so is the ideal wavelength range for following dust condensation in the ejecta or possibly in a cool, dense shell at the ejecta/progenitor wind interface. Alternatively, such radiation may arise from IR light echo emission from progenitor-wind dust. Discrimination between condensing dust and pre-existing circumstellar dust can be deduced from the mid-IR spectral energy distribution and evolution. Our Spitzer data have already provided evidence of dust IR emission in several CCSNe. In one case (SN 2002hh), an IR-echo seems to dominate. In Cycle 3, we propose to continue our monitoring program of some exceptionally nearby CCSNe during the phase (550 to 1000 days) when ejecta dust condensation is expected to peak. Our second goal is to test explosion models for all SN types by measuring the intensity and, where possible, the evolution of late-epoch fine-structure (FS) lines and molecular features. By comparison with our spectral synthesis models we shall test explosion-model-sensitive predictions of abundances. Most of the FS lines arise from ground state transitions and so, compared with optical/near-IR spectra, are much less sensitive to temperature and density uncertainties. However they are only accessible in the mid-IR and provide the most useful abundance measurements at late times when the ejecta are optically thin. Ground-based mid-IR observations at such late epochs are almost impossible. From data obtained in Cycles 1 & 2 we are building up a unique picture of the mid-IR behaviour of supernovae in the nebular phase. In Cycle 3 we shall enhance this study by monitoring the closest thermonuclear and core-collapse supernovae that have occurred since the launch of Spitzer.

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