1. Infrared Spectroscopy of Minerals from Primitive Meteorites: An IR Snapshot of an Early Solar System. A. Morlok 1,4, M. Koehler 2,4, O.N. Menzies 3,4, M. M. Grady 1,4 1 The Natural History Museum, London 2 Institut fuer Planetologie, Muenster 3 Imperial College, London 4 IARC

2. © European Southern Observatory Astronomical Infrared Spectra

3. Formation of a Solar System © Bill Hartmann

4. Primitive Meteorites: Components Calcium-Aluminum Rich InclusionsChondrules and Matrix Mainly Silicates, e.g.: Olivine (Mg,Fe) 2 SiO 4 Pyroxene (Mg,Fe)SiO 3 ‘Glass’ Highly refractory phases, e.g.: Corundum Al 2 O 3 Hibonite CaAl 12 O 19 Melilite Ca 2 MgSi 2 O 7 Ca 2 Al 2 SiO 7

5. What ? ? (Mid-)infrared spectra from sub- micron dust clouds, young solar systems, circumstellar discs etc. obtained with earth and space based telescopes Mid-infrared analysis of sub- micron powder of mineral separates and components, from primitive meteorites for comparison with these astronomical spectra Aim: Comparison of laboratory infrared data of minerals and components with astronomical spectra © European Southern Observatory

6. Challenges -Sample Preparation: -’Pure’ grains/material needed  But primitive meteorites are very fine grained, most mineral grains <<100  m -Characterization: What are we actually measuring ? -Preparation of tiny grains for identification, measurement of chemical composition, estimation of homogeneity -Infrared Measurements -Small amounts of material (~ng)  Difficult to prepare/handle  Danger of artefacts -Generally: Efficiency of process – each individual grain counts !

7. Sample Preparation Cleaning with Isopropanol and Deionised Water Picking Embedding Polishing Characterisation Separation Grinding FT-IR Analysis (at last) Separation Sample

8. How: FT-IR Techniques (Microscope) -Perkin Elmer AutoImage FT-IR microscope system for mid-infrared: 4000cm -1 to 650cm -1 (2.5  m to ~16  m), spectral resolution 4cm -1 Transmission/ Absorbance Source Sample Detector +High Quality +Common -Thin Samples Needed Reflectance Source Sample Detector +Easy&Fast -(Less Common) ATR Source Sample Detector +High Quality -Artefacts -Resolution

9. Results: Enstatites from Primitive Meteorites I TW Hya  -Pictoris Enstatite (En 99 ) From Primitive Meteorite

10. Results: Enstatites from Primitive Meteorites

11. Compact, Melilite/Spinel-rich Inclusion (Vigarano CV3.3) Wark- Lovering Rim: Diopside, Forsterite, Spinel Interior: Melilite, Spinel Material Separated ‘In Situ’ from Polished Thick Section A 8910 12 13 mm 11 TW Hya  -Pictoris

12. Conclusions & Outlook -Analyses over a wider range of wavelengths needed (far IR !) -Systematic analysis of all types of components like CAI and chondrules -Effects of environment (temperature…) and size and so … -Mid-infrared spectra of components and minerals from primitive chondrites can be easily measured with a variety of techniques -Preliminary comparison with astronomical spectra shows potential -But much more work has to be done ….