PI: Kelsie Krafton, Louisiana State U., firstname.lastname@example.org
Address: 233-B Nicholson Hall, LSU, Baton Rouge LA, 70803 USA
CoI: Geoffrey Clayton, Louisiana State U.
CoI: Michael J Barlow, University College of London
CoI: Antonia Bevan, University College of London
CoI: Roger Wesson, University College of London
CoI: Ilse De Looze, University College of London
Title: Observations of CCSNe to Look for Dust Production
Abstract: Studies in the last 10 years of dust formation in core-collapse supernovae (CCSNe) have found only small amounts, ~10^-3 solar masses during the first three years after the explosion. This is far less than the amount needed to account for the large masses of dust seen in some high redshift galaxies. However, the discovery of up to one solar mass of cold dust in the ejecta of SN 1987A, confirmed by ALMA, has caused a complete re-evaluation of dust formation in CCSNe. It has been suggested that the CCSNe are continuously forming dust so that by the time they are about 25 years old they will have dust masses similar to SN 1987A. However, there is a wide time gap between the CCSNe that have been studied recently and SN 1987A. We plan to use the high sensitivity of Gemini/GMOS to obtain spectra of a large sample of 11 CCSNe, between 6 and 60 yr after explosion, to test this hypothesis. All of the SNe have previously been observed spectroscopically, and should be bright enough to get high S/N emission spectra. The line profiles in our sample's spectra will be modeled with our new radiative transfer code DAMOCLES to derive ejecta dust masses by fitting observed asymmetries and extended scattering wings. The simultaneous modelling of emission lines spanning from 470 to 740 nm, in order to cover [OIII] 4959,5007, [OI] 6300,6363, [OII] 7319,7330, and the Balmer series, can be used to constrain the properties and ejecta locations of the dust grains formed. Solving the mystery of the large dust mass in SN 1987A will be an important step toward understanding the mechanisms of dust formation, and will help to understand the large dust masses found in early galaxies.
Program Type: Standard/Extragalactic
Run 1 (2018A): GEM-SQ/GMOSS -- 11.27hrs band 3 (GS-2018A-Q-311 )
National Optical Astronomy Observatory, 950 North Cherry Avenue, P.O. Box 26732, Tucson, Arizona 85726, Phone: (520) 318-8000, Fax: (520) 318-8360