The following samples are measured using Micro-IR and Micro-Raman spectroscopy complemented by FESEM/EDX analyses:

1) Cometary Samples (Stardust/Wild 2 samples)

Particles collected by the Stardust spacecraft during its flyby of comet 81P/Wild 2 on 2 January 2004 and successfully returned back to Earth on 15 January 2006.

(e.g. Rotundi et al., Meteoritics & Planetary Science 43, Nr 1/2, 367–397, 2008; Rotundi et al., Meteoritics & Planetary Science 1–26, 2014).

2) Meteoric dust (DUSTER)

DUSTER (Dust in the Upper Stratosphere Tracking Experiment and Retrieval) was designed to intercept, onboard stratospheric balloons, the nanometer to micrometer meteoric dust from these events for laboratory analyses while it is still in the upper stratosphere. We have available micro IR and micro Raman spectra of dust from the upper stratosphere, classified as uncontaminated meteoric dust particles.

(e.g. Rietmeijer et al., Icarus 266, 217–234, 2016).

3) Cometary Analogs (used to calibrate GIADA instrument onboard Rosetta/ESA mission)

The analogs include: (1) anhydrous silicate minerals [forsterite and fayalite, enstatite, melilite, alkali-feldspar andanorthite, (2) hydrated layer silicates (kaolinite, serpentine, talc), (3) pyrrhotite, (4)corundum.

Four size fractions, viz. 500–250 micron, 250–100 micron, 100–50 micron, 50–20 micron, for each analog mineral.

In addition, selected analog minerals, were coated with carbon layer, and/or with a layer of sodium hexafluorosilicate (Na2SiF6) crystals representing comet water-ice for what concerns the optical properties.

(e.g. Ferrari et al., Planetary andSpaceScience, 101, 53–64, 2014)

  • sshade/databases/comeda/samples.txt
  • Last modified: 2018/01/18 10:14
  • by Bernard Schmitt