Martian Analogues Emissivity Spectra From the Berlin Emissivity Database (BED)

Details Martian Analogues Emissivity Spectra From the Berlin Emissivity Database (BED) Martian Analogues Emissivity Spectra From the Berlin Emissivity Database (BED)

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufm.p23c0064m&link_type=abstract

American Geophysical Union, Fall Meeting 2006, abstract #P23C-0064

Physics

3934 Optical, Infrared, And Raman Spectroscopy, 5400 Planetary Sciences: Solid Surface Planets, 5464 Remote Sensing, 5470 Surface Materials And Properties, 6225 Mars

Scientific paper

Remote sensing infrared spectroscopy is the principal field of investigation for planetary surfaces composition. Past, present and future missions to bodies in the solar system include in their payload instruments measuring the emerging radiation in the infrared range. For the interpretation of the measured data an emissivity spectral library of planetary analog materials is needed. The Berlin Emissivity Database (BED) currently contains emissivity spectra of plagioclase and potassium feldspars, low Ca and high Ca pyroxenes, olivine, elemental sulphur, and Martian analogue minerals, measured in the wavelength range from 7 to 22 microns as a function of particle size. For each sample we measured the spectra of four particle size separates ranging from 0 to 250 microns. The device we used is built at DLR (Berlin) and is coupled to a Fourier transform infrared spectrometer (Bruker IFS 88), purged with dry air and equipped with a cooled detector (MCT). All spectra were acquired with a spectral resolution of 4 cm-1. We present here the results of our analysis on well knew and characterized Martian analogue minerals: JSC Mars-1, Salten Skov, and Palagonite from Mauna Kea, Hawaii. We are currently working to upgrade our emissivity facility. A new spectrometer (Bruker VERTEX 80v) and new detectors will allow us to measure the emissivity of samples in the wavelength range from 1 to 50 microns, even in a vacuum environment.

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