(90377) Sedna: Investigation of Surface Compositional Variation

The dwarf planet (90377) Sedna is one of the most remote solar system objects accessible to investigations. To better constrain its surface composition and to investigate the possible heterogeneity of the surface of Sedna, several observations have been carried out at ESO-VLT with the powerful spect...

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Bibliographic Details
Published in:The Astronomical journal 2010-12, Vol.140 (6), p.2095-2100
Main Authors: Barucci, M. A, Morea Dalle Ore, C, Alvarez-Candal, A, de Bergh, C, Merlin, F, Dumas, C, Cruikshank, D
Format: Article
Language:English
Subjects:
ALCOHOLS
ALKANES
Astrophysics
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
CHALCOGENIDES
DIMETHYL SULFIDE
ENERGY TRANSFER
ETHANE
HEAT TRANSFER
HYDROCARBONS
HYDROGEN COMPOUNDS
HYDROXY COMPOUNDS
ICE
INFRARED SPECTRA
MATTER
MEASURING INSTRUMENTS
METHANE
METHANOL
MINERALS
OLIVINE
ORGANIC COMPOUNDS
ORGANIC MATTER
ORGANIC SULFUR COMPOUNDS
OXYGEN COMPOUNDS
PHOTOMETRY
Physics
PLANETS
RADIANT HEAT TRANSFER
SATELLITES
SERPENTINE
SILICATE MINERALS
SOLAR SYSTEM
SPECTRA
SPECTROMETERS
SULFIDES
SULFUR COMPOUNDS
TELESCOPES
TRACE AMOUNTS
WATER
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Summary:The dwarf planet (90377) Sedna is one of the most remote solar system objects accessible to investigations. To better constrain its surface composition and to investigate the possible heterogeneity of the surface of Sedna, several observations have been carried out at ESO-VLT with the powerful spectrometer SINFONI observing simultaneously the H and K bands. The analyzed spectra (obtained in 2005, 2007, and 2008) show a non-uniform spectral signature, particularly in the K band. Spectral modeling using the Shkuratov radiative transfer code for surface scattering has been performed using the various sets of data, including previous observations at visible wavelengths and photometry at 3.6 and 4.5 Delta *mm by the Spitzer Space Telescope. The visible and near-infrared spectra can be modeled with organic materials (triton and titan tholin), serpentine, and H2O ice in fairly significant amounts, and CH4, N2, and C2H6 in varying trace amounts. One of the spectra obtained in 2005 October shows a different signature in the K band and is best modeled with CH3OH in place of CH4, with reduced amounts of serpentine and with the addition of olivine. The compositional surface heterogeneity can give input on the past history as well clues to the origin of this peculiar, distant object.
ISSN:1538-3881
0004-6256
1538-3881
DOI:10.1088/0004-6256/140/6/2095