What Fraction of Type II Supernovae Produce Dust and Why?

Details What Fraction of Type II Supernovae Produce Dust and Why? What Fraction of Type II Supernovae Produce Dust and Why?

Feb 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007noao.prop..146c&link_type=abstract

NOAO Proposal ID #2007A-0146

Physics

Scientific paper

We propose to continue our successful program studying the evolution of Type II supernovae (SNe) spectra at late times, 300-600 days after the initial explosion when dust typically condenses in the ejecta. Therefore, we are proposing to obtain new GMOS-S spectroscopy and g'r'i imaging of seven bright type II SNe. The spectra of these SNe will be sampled five times at approximately 50-day intervals in these windows: 300-350, 350-400, 400-450, 450-500, 500-550 days. It is challenging to obtain observations of SNe 500 days after peak brightness when they have faded by 6 magnitudes, but we have shown, using Gemini/GMOS, that monitoring the evolution of H-alpha and [O I] emission-line profiles in Type II SNe is a very sensitive technique for detecting new dust forming in the ejecta. These observations will double the sample of type II SNe in which dust formation has been studied. This increased sample is needed to understand several perplexing questions. First, what fraction of type II SNe produce dust? We now have a well documented case in SN 2002hh of a type II SN that does not seem to have produced any dust. Second, the relationship between dust production and global galactic properties such as metallicity can only be investigated with a larger sample. Finally, there is a wide range (300-550 days), even in the few SNe studied, in the time after peak brightness when dust forms in the ejecta. What conditions of the SNe ejecta affect the time of dust formation?

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