HR: 0800h
AN: P21A-0209    [Abstracts]
TI: Spectral Characterization of Mars Analogues From the Berlin Emissivity Database (BED)
AU: * Maturilli, A
EM: alessandro.maturilli@dlr.de
AF: DLR - German Aerospace Center, Rutherfordstrasse 2, Berlin, 12489, Germany
AU: Helbert, J
EM: joern.helbert@dlr.de
AF: DLR - German Aerospace Center, Rutherfordstrasse 2, Berlin, 12489, Germany
AB: Several well-recognized Martian soil analogues have been classified and studied in the past years. The JSC Mars-1, collected and distributed under control of the NASA Johnson Space Center, originates from Pu\'u Nene cinder cone in Hawaii, USA. It is a palagonitic tephra (glassy volcanic ash altered at low temperatures), whose spectral features resemble the bright regions on Mars. The Salten Skov, coming from a subsurface deposit in the Midjutland region of Denmark, is a Fe-oxide precipitate with a dark red color, composed mainly of goethite, hematite and maghemite, with mineralogical and magnetic close to those of the martian soil. Montmorillonite and palagonite are other natural materials commonly referred as Martian soil analogues. We present and discuss the emissivity spectra of these analogue minerals from the Berlin Emissivity Database spectral library. The Berlin Emissivity Database (BED) currently contains also emissivity spectra of plagioclase and potassium feldspars, low Ca and high Ca pyroxenes, olivine, elemental sulfur and a lunar highland soil sample measured in the wavelength range from 3 to 50 μm as a function of particle size. For each sample we measured the spectra of four particle size separates ranging from < 25 to 250 μm. The current main setup at the Planetary Emissivity Laboratory (PEL) at DLR consist of an emissivity device built at DLR coupled to a Fourier transform infrared spectrometer (Bruker VERTEX 80v) equipped with both a cooled MTC detector and a room temperature DTGS detector. All spectra were acquired with a spectral resolution of 4 cm^{- 1}. The combination of detectors and spectrometer allows a unique wavelength coverage encompassing the whole thermal radiation range measured by spacecraft instruments. The emissivity device is currently purged with dry air, while the spectrometer is evacuated. In a future upgrade of the facility the emissivity device will be replaced by a planetary simulation chamber which can be evacuated and which allows to heat sample up to Mercury surface temperatures.
DE: 5410 Composition (1060, 3672)
DE: 5415 Erosion and weathering
DE: 5464 Remote sensing
DE: 5494 Instruments and techniques
DE: 6225 Mars
SC: Planetary Sciences [P]
MN: 2007 Fall Meeting