Dust Formation in the Bright Type II SN 2007it

Details Dust Formation in the Bright Type II SN 2007it Dust Formation in the Bright Type II SN 2007it

Feb 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008noao.prop..313a&link_type=abstract

NOAO Proposal ID #2008A-0313

Physics

Scientific paper

We propose to take advantage of a recently discovered (Sep. 13, 2007), extremely bright (V=13.2), Type II supernova 2007it, to make a detailed study of its dust formation at visible, near- and mid-IR wavelengths. Because SN 2007it is so unusually bright, we should be able to follow its evolution for at least two years. This is very important because dust typically condenses in the SN ejecta approximately 300-600 days after the initial explosion. We are proposing for Long-Term Status so that we can follow SN 2007it in the 2008B and 2009A semesters as well. We are proposing to obtain new GMOS-S spectroscopy and imaging, and T-ReCS mid-IR imaging. The spectra of this SN will be sampled six times at approximately 30-day intervals covering the span of 140 to 320 days since the explosion. We have shown using Gemini that monitoring the evolution of H-alpha and [O I] emission-line profiles and IR emission in Type II SNe are very sensitive techniques for detecting new dust forming in the ejecta. With the exception of SN 1987A, observations of SNe are fragmentary, often only two spectra are available from which to infer the line profile evolution. The unusual brightness of SN 2007it and the sensitivity of Gemini/GMOS and T-ReCS will allow us to follow its evolution at regular intervals for up to 700 days. These detailed observations, beginning before dust forms and throughout the dust forming period, are needed to answer several perplexing questions concerning when and how much dust is produced by type II SNe. The observations in both the visible and IR will allow us to investigate the clumpy distribution of dust in the ejecta and better estimate the total mass of dust, which has important implications for the evolution of galaxies at high redshift.

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