Investigation of the Origin of 2008TC3 Through Spectral Analysis of F-type Asteroids and Lab Spectra of Almahata Sitta and Mineral Mixtures

Details Investigation of the Origin of 2008TC3 Through Spectral Analysis of F-type Asteroids and Lab Spectra of Almahata Sitta and Mineral Mixtures Investigation of the Origin of 2008TC3 Through Spectral Analysis of F-type Asteroids and Lab Spectra of Almahata Sitta and Mineral Mixtures

Oct 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010dps....42.1331f&link_type=abstract

American Astronomical Society, DPS meeting #42, #13.31; Bulletin of the American Astronomical Society, Vol. 42, p.1059

Astronomy and Astrophysics

Astronomy

Scientific paper

We are analyzing lab spectra of simulated ureilite meteorites along with observations of F-type asteroids in an attempt to characterize the spectral features of ureilite type meteorites. We have processed spectra from twelve F-type asteroids that are potential sources of 2008 TC3. A comparative study of the lab mixtures, Almahata Sitta, F-type asteroids, and 2008 TC3 is underway. We are attempting to use these data to connect the Almahata Sitta meteorites and their parent asteroid, 2008 TC3, with a specific class of asteroids.
Spectra of seven main-belt, F-type, low albedo asteroids were observed with the 2.2m telescope at Calar Alto using the CAFOS low resolution spectrograph in R-400 (0.47-1.1 µm) and B-100 (0.32-0.58 µm) modes. Targets were selected from Jenniskens et al (2010), and the data are currently being processed. The Kast Double Spectrograph was used at the Shane 3-m Telescope at LICK observatory to take spectra of five more F-type asteroids. Additional data will be taken in July 2010 with IRTF and SpeX low-resolution spectrographs in the near-infrared (1-2.5 µm) region.
Reflectance spectra of simulated ureilites comprised of mixtures of olivine, pyroxene and fine-grained carbon are being acquired from 0.35-2.5 µm using an ASD spectrometer at 2 nm spectral sampling. We will attempt to characterize ureilite spectral properties using Gaussian modeling (Sunshine et al. 1993) and analysis of the band centers and depths due to the olivine and pyroxene minerals observed in spectra of the Almahatta Sitta samples (Hiroi et al. 2010).
Hiroi, T et al. 2010. Meteoritics and Planetary Science, in press.
Jenniskens, P et al. 2010. Meteoritics and Planetary Science, in review.
Sunshine, J. M. et al. 1993. Icarus. 105, 79-91.

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