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  Ceres’ spectral link to carbonaceous chondrites - Analysis of the dark background materials

Schäfer, M., Schäfer, T., Izawa, M. R. M., Cloutis, E. A., Schröder, S. E., Roatsch, T., et al. (2018). Ceres’ spectral link to carbonaceous chondrites - Analysis of the dark background materials. Meteoritics and Planetary Science, 53(9), 1925-1945. doi:10.1111/maps.13079.

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 Creators:
Schäfer, Michael, Author
Schäfer, Tanja1, Author              
Izawa, Matthew R. M., Author
Cloutis, Edward A., Author
Schröder, Stefan E., Author
Roatsch, Thomas, Author
Preusker, Frank, Author
Stephan, Katrin, Author
Matz, Klaus‐Dieter, Author
Raymond, Carol A., Author
Russell, Christopher T., Author
Affiliations:
1Department Planets and Comets, Max Planck Institute for Solar System Research, Max Planck Society, ou_1832288              

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 Abstract: Ceres’ surface has commonly been linked with carbonaceous chondrites (CCs) by ground‐based telescopic observations, because of its low albedo, flat to red‐sloped spectra in the visible and near‐infrared (VIS/NIR) wavelength region, and the absence of distinct absorption bands, though no currently known meteorites provide complete spectral matches to Ceres. Spatially resolved data of the Dawn Framing Camera (FC) reveal a generally dark surface covered with bright spots exhibiting reflectance values several times higher than Ceres’ background. In this work, we investigated FC data from High Altitude Mapping Orbit (HAMO) and Ceres eXtended Juling (CXJ) orbit (~140 m/pixel) for global spectral variations. We found that the cerean surface mainly differs by spectral slope over the whole FC wavelength region (0.4–1.0 μm). Areas exhibiting slopes <−10% μm−1 constitute only ~3% of the cerean surface and mainly occur in the bright material in and around young craters, whereas slopes ≥−10% μm−1 occur on more than 90% of the cerean surface; the latter being denoted as Ceres’ background material in this work. FC and Visible and Infrared Spectrometer (VIR) spectra of this background material were compared to the suite of CCs spectrally investigated so far regarding their VIS/NIR region and 2.7 μm absorption, as well as their reflectance at 0.653 μm. This resulted in a good match to heated CI Ivuna (heated to 200–300 °C) and a better match for CM1 meteorites, especially Moapa Valley. This possibly indicates that the alteration of CM2 to CM1 took place on Ceres.

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Language(s): eng - English
 Dates: 2019-04-042018
 Publication Status: Published in print
 Pages: -
 Publishing info: -
 Table of Contents: -
 Rev. Type: Peer
 Identifiers: DOI: 10.1111/maps.13079
 Degree: -

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Title: Meteoritics and Planetary Science
Source Genre: Journal
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Publ. Info: Fayetteville, AR : Meteoritical Society at the University of Arkansas, Dept. of Chemistry and Biochemistry
Pages: - Volume / Issue: 53 (9) Sequence Number: - Start / End Page: 1925 - 1945 Identifier: ISSN: 1086-9379
CoNE: https://pure.mpg.de/cone/journals/resource/954925424162