Results from the preliminary examination of Stardust samples obtained using various spectroscopic methods will be presented

Bajt, S.

Baratta, G. A.

Borg, J.

Brucato, J.

Burchell, M. J.

Colangeli, L.

d'Hendecourt, L.

Djouadi, Z.

Ferrini, G.

Flynn, G.

Franchi, A.

Fries, M.

Grady, M.

Graham, G.

Grossemy, F.

Kearsley, A.

Keller, L. P.

Matrajt, G.

Mennella, V.

Nittler, L.

Palumbo, M. E.

Rotundi, A.

Wopenka, B.

Zolensky, M.

English

Open Research Online 

Open Research OnlineThe Open University’s repository of research publicationsand other research outputsInfrared, UV/VIS and Raman Spectroscopy of CometWild-2 Samples Returned by the Stardust MissionConference or Workshop ItemHow to cite:Keller, L. P.; Bajt, S.; Baratta, G. A.; Borg, J.; Brucato, J.; Burchell, M. J.; Colangeli, L.; d’Hendecourt, L.;Djouadi, Z.; Ferrini, G.; Flynn, G.; Franchi, A.; Fries, M.; Grady, M.; Graham, G.; Grossemy, F.; Kearsley, A.; Matrajt,G.; Mennella, V.; Nittler, L.; Palumbo, M. E.; Rotundi, A.; Wopenka, B. and Zolensky, M. (2006). Infrared, UV/VISand Raman Spectroscopy of Comet Wild-2 Samples Returned by the Stardust Mission. In: 37th Lunar and PlanetaryScience Conference, 13-17 Mar 2006, Houston, Texas, USA.For guidance on citations see FAQs.c© [not recorded]Version: [not recorded]Link(s) to article on publisher’s website:http://www.lpi.usra.edu/meetings/lpsc2006/pdf/2062.pdfCopyright and Moral Rights for the articles on this site are retained by the individual authors and/or other copyrightowners. For more information on Open Research Online’s data policy on reuse of materials please consult the policiespage.oro.open.ac.ukINFRARED, UV/VIS AND RAMAN SPECTROSCOPY OF COMET WILD-2 SAMPLES RETURNED BY THE STARDUST MISSION.  L. P. Keller1, S. Bajt2, G. A. Baratta3, J. Borg4, J. Brucato3, M. Burchell5, L. Colangeli3, L. d'Hendecourt4, Z. Djouadi4, G. Ferrini3, G. Flynn6, I. A. Franchi7, M. Fries8, M. M. Grady7, G. Graham2, F. Grossemy4, A. Kearsley9, G. Matrajt10, V. Mennella3, L. Nittler8, M. E. Palumbo3, A. Rotundi11, B. Wopenka12 and M. Zolen-sky1. 1NASA-JSC, Houston, TX 77058, 2LLNL, Livermore, Ca 94550, 3Instituto Nazionale di Astrofisica INAF, 4Institut d’ Astrophysique Spatiale, IAS, 5Univ. Kent, 6SUNY-Plattsburgh, 7Open Univ., 8Carnegie Institute, Wash., 9Natural History Museum, 10Univ. Wash., Seattle, 11Univ. Naples “Parthenope”, 12Wash. Univ., St. Louis. (Lindsay.P.Keller@jsc.nasa.gov).  Introduction.  The Stardust spacecraft collected dust samples of the Kuiper belt comet 81P Wild-2 in aerogel and returned them to Earth January 15, 2006.  Preliminary examination (PE) of the collected dust will include teams focused on mineralogy [1], chemical composition [2], isotopic measure-ments [3], organic analysis [4], cratering [5] and spectroscopic properties.  The main PE science goals are to provide an initial charac-terization of the returned samples with an emphasis on the capture process and its ef-fects on the samples, a comparison of Star-dust samples to other meteoritic materials, and the abundance of presolar materials in the Stardust samples.  The science objectives of the Spectros-copy team are to obtain spectroscopic data on Stardust particles through infrared (IR), UV/Vis and Raman measurements of parti-cles in aerogel, extracted particles, keystones, and microtome thin sections.  These data will be used to answer fundamental science ques-tions about the nature of the samples, but will also serve as preliminary mineralogical data to guide follow-on measurements that will be performed in the other preliminary examina-tion teams.  Because of their non-destructive nature, these spectroscopic measurements will occur early in the PE.  Infrared Spectroscopy.  Determine the IR characteristics of as many particles or por-tions of particles as possible in order to ascer-tain: 1) the nature of the indigenous 3.4 μm organic feature, is it detected and can it be differentiated/deconvolved from the contami-nated aerogel?  How does it compare to fea-tures observed in interplanetary dust particles (IDPs) and to astronomical measurements of comets and interstellar dust? 2) the shape and fine structure within the10 μm silicate fea-ture.   Overlap with the strong Si-O stretching vibration from the aerogel will complicate this analysis, but we hope to determine if the feature is dominated by amorphous silicates such as those observed in IDPs and comets and whether or not crystalline silicates (e.g. olivine, pyroxene, clays) are present, 3) the presence of secondary (alteration) phases.  Deep Impact results suggest that IR observa-tions of Stardust particles should be evaluated for the presence of hydrated materials (water bands at 3 and 6 μm) and carbonates (6.8 μm and other resonances) and 4) the detection of crystalline features in the far-IR (20-100 μm) region where crystalline silicates and other minerals have strong bands that can be used both for phase analysis and phase chemistry.  It has been demonstrated that these far-IR measurements can be obtained in situ on par-ticles in aerogel keystones [6].  UV/VIS spectroscopy. Determine the UV/Vis spectrum of extracted particles across the wavelength range from 200–850 nm, in order to observe whether or not there is an absorbance present that can be compared with the 217.5 nm interstellar absorption band; make qualitative analyses of the presence of organic molecules within the grains, and as-sign bond identities; assess the relative abun-Lunar and Planetary Science XXXVII (2006) 2062.pdfdances of hydrated and anhydrous minerals within grains on the basis of OH features.  Raman Spectroscopy.  Obtain Raman spectra from individual extracted particles and from particles in aerogel [e.g. 7-12].  Raman spectra of Stardust particles are ex-pected to be characteristic for both the "dis-orderd carbonaceous materials" (i.e., organic components) and various minerals. The team will try to characterize the nature of the car-bonaceous materials (i.e., aromatic, aliphatic, etc.) using the position, width, and relative intensity of the first- and second-order Raman bands. The Raman spectra of most silicates and oxides have very narrow bands, which are strong and very specific for a given min-eral. Nevertheless, they potentially can be obscured by the strong Raman bands from carbonaceous materials or by fluorescence effects. As long as the Raman spectra for the minerals can be successfully obtained, how-ever, they will complement and build on the IR data, and they will allow very detailed in situ mineralogical analyses of individual Stardust particles and to understand the inter-action of the particles with the aerogel from the capture event.  Mapping of the particles will afford some information on the spatial distribution and proportion of phases within larger particles (>3 μm).  References.  [1] Zolensky, M. et al. (2006) this volume. [2] Flynn, G. J. et al. (2006) this volume. [3] McKeegan, K. D. et al. (2006) this volume. [4] Sandford, S. A. et al. (2006) this volume. [5] Horz, F. et al. (2006) this volume. [6] Keller, L. P., Flynn, G. J. and Westphal, A. (2003) MAPS, 38, #5288. [7] Burchell, M. J. et al. (2001) MAPS, 36, 209. [8] Burchell, M. J.  et al. (2004) J. Raman Spectroscopy, 35, 249. [9] Burchell, M. J. et al. (2006) Identification of Minerals and Meteoritic Materials via Raman Techniques after Capture in Hypervelocity Impacts on Aerogel, MAPS, accepted. [10] Fries M. et al. (2004) LPS XXXV, #2139. [12] Ferrini, G. et al. (2005) Workshop on Dust in Planetary Systems, #4043.  Part of this work was performed under the auspices of the U.S. Department of Energy by the University of California Lawrence Liver-more National Laboratory under Contract No. W-7405-ENG-48.  Lunar and Planetary Science XXXVII (2006) 2062.pdf

Infrared, UV/VIS and Raman Spectroscopy of Comet Wild-2 Samples Returned by the Stardust Mission

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Infrared, UV/VIS and Raman Spectroscopy of Comet Wild-2 Samples Returned by the Stardust Mission

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