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2. Evidence for interstellar origin of seven dust particles collected by the Stardust spacecraft

Author

Westphal, Andrew J., Stroud, Rhonda M., Bechtel, Hans A., Brenker, Frank E., Butterworth, Anna L., Flynn, George J., Frank, David R., Gainsforth, Zack, Hillier, Jon K., Postberg, Frank, Simionovici, Alexandre S., Sterken, Veerle J., Nittler, Larry R., Allen, Carlton, Anderson, David, Ansari, Asna, Bajt, Saša, Bastien, Ron K., Bassim, Nabil, Bridges, John, Brownlee, Donald E., Burchell, Mark, Burghammer, Manfred, Changela, Hitesh, Cloetens, Peter, Davis, Andrew M., Doll, Ryan, Floss, Christine, Grün, Eberhard, Heck, Philipp R., Hoppe, Peter, Hudson, Bruce, Huth, Joachim, Kearsley, Anton, King, Ashley J., Lai, Barry, Leitner, Jan, Lemelle, Laurence, Leonard, Ariel, Leroux, Hugues, Lettieri, Robert, Marchant, William, Ogliore, Ryan, Ong, Wei Jia, Price, Mark C., Sandford, Scott A., Tresseras, Juan-Angel Sans, Schmitz, Sylvia, Schoonjans, Tom, Schreiber, Kate, Silversmit, Geert, Solé, Vicente A., Srama, Ralf, Stadermann, Frank, Stephan, Thomas, Stodolna, Julien, Sutton, Stephen, Trieloff, Mario, Tsou, Peter, Tyliszczak, Tolek, Vekemans, Bart, Vincze, Laszlo, Von Korff, Joshua, Wordsworth, Naomi, Zevin, Daniel, and Zolensky, Michael E.

Published
2014

3. INTERSTELLAR DUST: Evidence for interstellar origin of seven dust particles collected by the Stardust spacecraft

Author

Westphal, Andrew J., Stroud, Rhonda M., Bechtel, Hans A., Brenker, Frank E., Butterworth, Anna L., Flynn, George J., Frank, David R., Gainsforth, Zack, Hillier, Jon K., Postberg, Frank, Simionovici, Alexandre S., Sterken, Veerle J., Nittler, Larry R., Allen, Carlton, Anderson, David, Ansari, Asna, Bajt, Saša, Bastien, Ron K., Bassim, Nabil, Bridges, John, Brownlee, Donald E., Burchell, Mark, Burghammer, Manfred, Changela, Hitesh, Cloetens, Peter, Davis, Andrew M., Doll, Ryan, Floss, Christine, Grün, Eberhard, Heck, Philipp R., Hoppe, Peter, Hudson, Bruce, Huth, Joachim, Kearsley, Anton, King, Ashley J., Lai, Barry, Leitner, Jan, Lemelle, Laurence, Leonard, Ariel, Leroux, Hugues, Lettieri, Robert, Marchant, William, Ogliore, Ryan, Jia Ong, Wei, Price, Mark C., Sandford, Scott A., Sans Tresseras, Juan-Angel, Schmitz, Sylvia, Schoonjans, Tom, Schreiber, Kate, Silversmit, Geert, Solé, Vicente A., Srama, Ralf, Stadermann, Frank, Stephan, Thomas, Stodolna, Julien, Sutton, Stephen, Trieloff, Mario, Tsou, Peter, Tyliszczak, Tolek, Vekemans, Bart, Vincze, Laszlo, Von Korff, Joshua, Wordsworth, Naomi, Zevin, Daniel, and Zolensky, Michael E.

Published
2014
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4. Stardust Interstellar Preliminary Examination V: XRF Analyses of Interstellar Dust Candidates at ESRF ID13

Author

Brenker, Frank E, Westphal, Andrew J, Simionovici, Alexandre S, Flynn, George J, Gainsforth, Zack, Allen, Carlton C, Sanford, Scott, Zolensky, Michael E, Bastien, Ron K, and Frank, David R

Subjects
Astrophysics
Abstract

Here, we report analyses by synchrotron X-ray fluorescence microscopy of the elemental composition of eight candidate impact features extracted from the Stardust Interstellar Dust Collector (SIDC). Six of the features were unambiguous tracks, and two were crater-like features. Five of the tracks are so-called midnight tracks that is, they had trajectories consistent with an origin either in the interstellar dust stream or as secondaries from impacts on the Sample Return Capsule (SRC). In a companion paper reporting synchrotron X-ray diffraction analyses of ISPE candidates, we show that two of these particles contain natural crystalline materials: the terminal particle of track 30contains olivine and spinel, and the terminal particle of track 34 contains olivine. Here, we show that the terminal particle of track 30, Orion, shows elemental abundances, normalized to Fe, that are close to CI values, and a complex, fine-grained structure. The terminal particle of track 34, Hylabrook, shows abundances that deviate strongly from CI, but shows little fine structure and is nearly homogenous. The terminal particles of other midnight tracks, 29 and 37, had heavy element abundances below detection threshold. A third, track28, showed a composition inconsistent with an extraterrestrial origin, but also inconsistent with known spacecraft materials. A sixth track, with a trajectory consistent with secondary ejecta from an impact on one of the spacecraft solar panels, contains abundant Ce and Zn. This is consistent with the known composition of the glass covering the solar panel. Neither crater-like feature is likely to be associated with extraterrestrial materials. We also analyzed blank aerogel samples to characterize background and variability between aerogel tiles. We found significant differences in contamination levels and compositions, emphasizing the need for local background subtraction for accurate quantification.

Published
2014
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5. Stardust Interstellar Preliminary Examination VII: Synchrotron X-Ray Fluorescence Analysis of Six Stardust Interstellar Candidates Measured with the Advanced Photon Source 2-ID-D Microprobe

Author

Allen, Carlton C, Anderson, David, Bastien, Ron K, Brenker, Frank E, Flynn, George J, Frank, David, Gainsforth, Zack, Sandford, Scott A, Simionovici, Alexandre S, and Zolensky, Michael E

Subjects
Astrophysics
Abstract

The NASA Stardust spacecraft exposed an aerogel collector to the interstellar dust passing through the solar system. We performed X-ray fluorescence element mapping and abundance measurements, for elements 19 < or = Z < or = 30, on six "interstellar candidates," potential interstellar impacts identified by Stardust@Home and extracted for analyses in picokeystones. One, I1044,3,33, showed no element hot-spots within the designated search area. However, we identified a nearby surface feature, consistent with the impact of a weak, high-speed particle having an approximately chondritic (CI) element abundance pattern, except for factor-of-ten enrichments in K and Zn and an S depletion. This hot-spot, containing approximately 10 fg of Fe, corresponds to an approximately 350 nm chondritic particle, small enough to be missed by Stardust@Home, indicating that other techniques may be necessary to identify all interstellar candidates. Only one interstellar candidate, I1004,1,2, showed a track. The terminal particle has large enrichments in S, Ti, Cr, Mn, Ni, Cu, and Zn relative to Fe-normalized CI values. It has high Al/Fe, but does not match the Ni/Fe range measured for samples of Al-deck material from the Stardust sample return capsule, which was within the field-of-view of the interstellar collector. A third interstellar candidate, I1075,1,25, showed an Al-rich surface feature that has a composition generally consistent with the Al-deck material, suggesting that it is a secondary particle. The other three interstellar candidates, I1001,1,16, I1001,2,17, and I1044,2,32, showed no impact features or tracks, but allowed assessment of submicron contamination in this aerogel, including Fe hot-spots having CI-like Ni/Fe ratios, complicating the search for CI-like interstellar/interplanetary dust.

Published
2014
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6. Section 3.12: Focusing methods: K-B mirrors, zone plates, capillaries, etc. for spectroscopy

Author

Simionovici, Alexandre S., Lemelle, Laurence, Schroer, Christian, Institut des Sciences de la Terre (ISTerre), Institut national des sciences de l'Univers (INSU - CNRS)-Institut de recherche pour le développement [IRD] : UR219-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Gustave Eiffel-Université Grenoble Alpes (UGA), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Institut de recherche pour le développement [IRD] : UR219-Université Grenoble Alpes (UGA)-Université Gustave Eiffel-Centre National de la Recherche Scientifique (CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry]), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement [Lyon] (LGL-TPE), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon)

Subjects
[PHYS.PHYS.PHYS-CHEM-PH]Physics [physics]/Physics [physics]/Chemical Physics [physics.chem-ph], ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2020

7. Coordinated Microanalyses of Seven Particles of Probable Interstellar Origin from the Stardust Mission

Author

Westphal, Andrew J, Stroud, Rhonda M, Bechtel, Hans A, Brenker, Frank E, Butterworth, Anna L, Flynn, George J, Frank, David R, Gainsforth, Zack, Hillier, Jon K, Postberg, Frank, Simionovici, Alexandre S, Sterken, Veerle J, Allen, Carlton, Anderson, David, Ansari, Asna, Bajt, Sasa, Bastien, Ron K, Bassim, Nabil, Bridges, John, Brownlee, Donald E, Burchell, Mark, Burghammer, Manfred, Changela, Hitesh, Sandford, Scott A, and Zolensky, Michael

Subjects
Lunar And Planetary Science And Exploration
Abstract

Stardust, a NASA Discovery-class mission, was the first sample-return mission to return solid samples from beyond the Moon. Stardust was effectively two missions in one spacecraft: it returned the first materials from a known primitive solar system body, the Jupiter-family comet Wild 2; Stardust also returned a collector that was exposed to the contemporary interstellar dust stream for 200 days during the interplanetary cruise. Both collections present severe technical challenges in sample preparation and in analysis. By far the largest collection is the cometary one: approximately 300 micro g of material was returned from Wild 2, mostly consisting of approx. 1 ng particles embedded in aerogel or captured as residues in craters on aluminum foils. Because of their relatively large size, identification of the impacts of cometary particles in the collection media is straightforward. Reliable techniques have been developed for the extraction of these particles from aerogel. Coordinated analyses are also relatively straightforward, often beginning with synchrotron-based x-ray fluorescence (S-XRF), X-ray Absorption Near-Edge Spectoscopy (XANES) and x-ray diffraction (S-XRD) analyses of particles while still embedded in small extracted wedges of aerogel called ``keystones'', followed by ultramicrotomy and TEM, Scanning Transmission X-ray Microscopy (STXM) and ion microprobe analyses (e.g., Ogliore et al., 2010). Impacts in foils can be readily analyzed by SEM-EDX, and TEM analysis after FIB liftout sample preparation. In contrast, the interstellar dust collection is vastly more challenging. The sample size is approximately six orders of magnitude smaller in total mass. The largest particles are only a few pg in mass, of which there may be only approx.10 in the entire collection. The technical challenges, however, are matched by the scientific importance of the collection. We formed a consortium carry out the Stardust Interstellar Preliminary Examination (ISPE) to carry out an assessment of this collection, partly in order to characterize the collection in sufficient detail so that future investigators could make well-informed sample requests. The ISPE is the sixth PE on extraterrestrial collections carried out with NASA support. Some of the basic questions that we asked were: how many impacts are there in the collector, and what fraction of them have characteristics consistent with extraterrestrial materials? What is the elemental composition of the rock-forming elements? Is there crystalline material? Are there organics? Here we present coordinated microanalyses of particles captured in aerogel, using S-FTIR, S-XRF, STXM, S-XRD; and coordinated microanalyses of residues in aluminum foil, using SEMEDX, Auger spectroscopy, STEM, and ion microprobe. We discuss a novel approach that we employed for identification of tracks in aerogel, and new sample preparation techniques developed during the ISPE. We have identified seven particles - three in aerogel and four in foils - that are most consistent with an interstellar origin. The seven particles exhibit a large diversity in elemental composition. Dynamical evidence, supported supported by laboratory simulations of interstellar dust impacts in aerogel and foils, and numerical modeling of interstellar dust propagation in the heliosphere, suggests that at least some of the particles have high optical cross-section, perhaps due to an aggregate structure. However, the observations are most consistent with a variety of morphologies

Published
2014

8. Final Reports of the Stardust ISPE: Seven Probable Interstellar Dust Particles

Author

Allen, Carlton, Sans Tresseras, Juan-Angel, Westphal, Andrew J, Stroud, Rhonda M, Bechtel, Hans A, Brenker, Frank E, Butterworth, Anna L, Flynn, George J, Frank, David R, Gainsforth, Zack, Hillier, Jon K, Postberg, Frank, Simionovici, Alexandre S, Sterken, Veerle J, Anderson, David, Ansari, Asna, Bajt, Sasa, Bastien, Ron K, Bassim, Nabil, Bridges, John, Brownlee, Donald E, Burchell, Mark, Burghammer, Manfred, Changela, Hitesh, Cloetens, Peter, Davis, Andrew M, Doll, Ryan, Floss, Christine, Gruen, Eberhard, Heck, Philipp R, Hoppe, Peter, Hudson, (Bruce), Huth, Joachim, Kearsley, Anton, and King, Ashley J

Subjects
Lunar And Planetary Science And Exploration
Abstract

The Stardust spacecraft carried the first spaceborne collector specifically designed to capture and return a sample of contemporary interstellar dust to terrestrial laboratories for analysis [1]. The collector was exposed to the interstellar dust stream in two periods in 2000 and 2002 with a total exposure of approximately 1.8 10(exp 6) square meters sec. Approximately 85% of the collector consisted of aerogel, and the remainder consisted of Al foils. The Stardust Interstellar Preliminary Examination (ISPE) was a consortiumbased effort to characterize the collection in sufficient detail to enable future investigators to make informed sample requests. Among the questions to be answered were these: How many impacts are consistent in their characteristics with interstellar dust, with interplanetary dust, and with secondary ejecta from impacts on the spacecraft? Are the materials amorphous or crystalline? Are organics detectable? An additional goal of the ISPE was to develop or refine the techniques for preparation, analysis, and curation of these tiny samples, expected to be approximately 1 picogram or smaller, roughly three orders of magnitude smaller in mass than the samples in other small particle collections in NASA's collections - the cometary samples returned by Stardust, and the collection of Interplanetary Dust Particles collected in the stratosphere.

Published
2014

9. Determination of the Cd-bearing phases in municipal solid waste and biomass single fly ash particles using SR-[micro]XRF spectroscopy

Author

Camerani, Maria Caterina, Somogyi, Andrea, Vekemans, Bart, Ansell, Stuart, Simionovici, Alexandre S., Steenari, Britt-Marie, and Panas, Itai

Subjects
Fluorescence -- Methods, Cadmium -- Identification and classification, Fly ash -- Composition, Chemistry
Abstract

By using an excitation energy of 27.0 keV, synchrotron radiation-induced micro-X-ray fluorescence (SR-[micro]XRF) is employed to extract information regarding the composition and distribution of Cd-bearing phases in municipal solid waste (MSW) and biomass fly ashes. Significance of observation is based on statistics of totally more than 100 individual MSW and biomass fly ash particles from a fluidized bed combustion (FBC) plant. Cd concentrations in the parts-per-million range are determined. In general, although previous leaching studies have indicated Cd to be predominant in the smaller-size ash particles, in the present study Cd is more evenly distributed throughout all the particle sizes. For MSW fly ashes, results indicate the presence of Cd mainly as Cd[Br.sub.2] hot-spots, whereas for biomass fly ashes, which exhibit lower Cd[X.sub.2] concentration, a thin Cd layer on/in the particles is reported. For both ashes, Ca-containing matrixes are found to be the main Cd-bearing phases. Support for this observation is found from independent first-principles periodic density functional theory calculations. The observations are condensed into a schematic mechanism for Cd adsorption on the fly ash particles.

Published
2007

10. X-ray fluorescence tomography of individual municipal solid waste and biomass fly ash particles

Author

Camerani, Maria Caterina, Golosio, Bruno, Somogyi, Andrea, Simionovici, Alexandre S., Steenari, Britt-Marie, and Panas, Itai

Subjects
Chemistry
Abstract

Information about Cd distribution inside single municipal solid waste and biomass fly ash particles is fundamental since it affects its leachability. The internal 2D distributions of the main and trace elements in such highly inhomogeneous matrixes were successfully determined by means of the combined synchrotron radiation induced micro X-ray fluorescence ([micro]-SRXRF) and tomography ([micro]-SRXRFT) techniques. Scanning [micro]-SRXR measurements show Cd elemental distribution within single fly ash particles to be inhomogeneous, but no information can be obtained about its internal distribution. During [micro]-SRXRFT analysis, single fly ash particles are successively measured by a rotational-translational scan in a VH = 2 x 5 [micro][m.sup.2] microbeam. The 2D internal elemental distribution images, obtained by the modified simultaneous algebraic reconstruction technique algorithm, provide the size and the location of Cd-containing areas together with the location of other measurable elements. Results showed Cd concentration to be higher in the core of the fly ash particles analyzed rather than on the surface of the particles. Moreover, in both ashes, Ca-containing matrixes are found to be the main Cd-bearing phases. A possible mechanism for Cd adsorption on the fly ash particles is proposed based on the obtained results.

Published
2004

11. Stardust Interstellar Preliminary Examination III: Infrared Spectroscopic Analysis of Interstellar Dust Candidates

Author

Bechtel, Hans A, Flynn, George J, Allen, Carlton, Anderson, David, Ansari, Asna, Bajt, Sasa, Bastien, Ron K, Bassim, Nabil, Borg, Janet, Brenker, Frank E, Bridges, John, Brownlee, Donald E, Burchell, Mark, Burghammer, Manfred, Butterworth, Anna L, Changela, Hitesh, Cloetens, Peter, Davis, Andrew M, Doll, Ryan, Floss, Christine, Frank, David R, Gainsforth, Zack, Grun, Eberhard, Heck, Philipp R, Hillier, Jon K, Hoppe, Peter, Hudson, Bruce, Huth, Joachim, Hvide, Brit, Kearsley, Anton, King, Ashley J, Lai, Barry, Leitner, Jan, Lemelle, Laurence, Leroux, Hugues, Leonard, Ariel, Lettieri, Robert, Marchant, William, Nittler, Larry, Ogliore, Ryan, Ong, Wei Ja, Postberg, Frank, Price, Mark C, Sandford, Scott A, Tresseras, Juan-Angel Sans, Schmitz, Sylvia, Schoonjans, Tom, Silversmit, Geert, Simionovici, Alexandre S, Sole, Vicente A, Srama, Ralf, Stadermann, Frank J, Stephan, Thomas, Sterken, Veerle J, Stodolna, Julien, Stroud, Rhonda M, Sutton, Steven, Trieloff, Mario, Tsou, Peter, Tsuchiyama, Akira, Tyliszczak, Tolek, Vekemans, Bart, Vincze, Laszlo, Von Korff, Joshua, Westphal, Andrew J, Wordsworth, Naomi, Zevin, Daniel, and Zolensky, Michael E

Subjects
Astrophysics
Abstract

Under the auspices of the Stardust Interstellar Preliminary Examination, picokeystones extracted from the Stardust Interstellar Dust Collector were examined with synchrotron Fourier transform infrared (FTIR) microscopy to establish whether they contained extraterrestrial organic material. The picokeystones were found to be contaminated with varying concentrations and speciation of organics in the native aerogel, which hindered the search for organics in the interstellar dust candidates. Furthermore, examination of the picokeystones prior to and post X-ray microprobe analyses yielded evidence of beam damage in the form of organic deposition or modification, particularly with hard X-ray synchrotron X-ray fluorescence. From these results, it is clear that considerable care must be taken to interpret any organics that might be in interstellar dust particles. For the interstellar candidates examined thus far, however, there is no clear evidence of extraterrestrial organics associated with the track and/or terminal particles. However, we detected organic matter associated with the terminal particle in Track 37, likely a secondary impact from the Al-deck of the sample return capsule, demonstrating the ability of synchrotron FTIR to detect organic matter in small particles within picokeystones from the Stardust interstellar dust collector.

Published
2013
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13. Metals for Life in Earth & Planetary Sciences

Author

Simionovici, Alexandre S., Lemelle, Laurence, Solé, Vicente Armando, Tucoulou, Rémi, Suchéras-Marx, Baptiste, Bartolini, Annachiara, Simionovici, Alexandre, Solé, A, Schoonjans, T, Institut des Sciences de la Terre (ISTerre), Institut national des sciences de l'Univers (INSU - CNRS)-Institut de recherche pour le développement [IRD] : UR219-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Gustave Eiffel-Université Grenoble Alpes (UGA), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), European Synchrotron Radiation Facility (ESRF), Centre européen de recherche et d'enseignement des géosciences de l'environnement (CEREGE), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Collège de France (CdF (institution))-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), Muséum national d'Histoire naturelle (MNHN), and Suchéras-Marx, Baptiste

Subjects
[SDV.IB.BIO] Life Sciences [q-bio]/Bioengineering/Biomaterials, [SDU.STU.GC]Sciences of the Universe [physics]/Earth Sciences/Geochemistry, [SDU.STU.GC] Sciences of the Universe [physics]/Earth Sciences/Geochemistry, [SDV.IB.BIO]Life Sciences [q-bio]/Bioengineering/Biomaterials
Abstract

International audience; Metals are pre-requisites for life, fingerprints of life and tracers of metabolic processes of biomineralisation in living organisms. To study metals at macromolecular interaction scales requires state of the art analytical capabilities down to trace element levels and nanometer spatial resolutions. Fortunately, in the last decade, highly sensitive X-ray probes have been developed at worldwide 3rd generation synchrotron facilities. To date, a limited number of these highly specific nanoimaging probes have been deployed, and the ESRF ID16A/B and ID21 ones are among the leaders. X-rays are non (or least) destructive, noninvasive, penetrative and highly sensitive probes of solid samples and metals are their ideal targets. X-ray fluorescence has reached few tens of nm resolutions and a world record for absolute mass of e.g. 50 zg for Fe, whichcan be recognized as only about 600 atoms. Over the past decade, we have developed a multi-analyses methodology of nanoimaging mid-Z elements in low-Z matrices as a direct application to Life and/or Planetary Sciences of trace metals in biological matrices or in C/Si-based ones.X-ray fluorescence and absorption spectroscopies, deployed at the few nanometer scales, are sensitive probes but they require a re-assessment of the analytical requirements previously established at the few micron levels [1]. We will present some specific analytical developments and methodologies optimized for such applications. They are centered onto absolute quantification of metals using both the Fundamental Parameter Approximation and reference materials, after spectra analysis using the PyMCA package [2] coupled to Monte-Carlo simulations of sample compositions [3] and geometries, prerequisites for 2D/3D elemental imaging. Examples based on metal detection were applied to either environmental key organisms such as foraminifers or coccolithofores [4, 5] but also to the oldest living organisms tracedback to life's origins on Earth [1]. Finally, our search for life being also aimed at planetary and astronomical scales on exoplanets, we will present our patented methodology and sample holder [6] for Quarantine Extraterrestrial Sample Analyses (QESA) for the upcoming Returned Sample Missions from Mars and asteroids [7].[1] – L. Lemelle, A. Simionovici et al., Trends Anal. Chem. 91, 104–111, 2017.[2] – Solé, V.A., Papillon, et al., Spectrochim. Acta B, 62, 63-68, 2006.[3] – T. Schoonjans, L. Vincze, V.A. Sol_e, et al., Spectrochim. Acta B 70, 10-23, 2012.[4] – L. Lemelle, A. Bartolini, A. Simionovici, et al., Nature Comm., (in review) 2019.[5] – B. Suchéras-Marx, F. Giraud, A. Simionovici et al., Geobiology 14, 390-403, 2016.[6] – A. Simionovici and CNES, European Patent Office # EP2411791A1, 2010.[7] – A. Simionovici, L Lemelle et al., Proc. of the EAS Annual Meeting, EWASS, 2019

Published
2019

16. Wavelength-dispersive spectroscopy in the hard x-ray regime of a heavy highly-charged ion: the 1s Lamb shift in hydrogen-like gold

Author

Gaßner, Tobias, Trassinelli, Martino, Heß, Regina, Spillmann, Uwe, Banaś, Dariusz, Blumenhagen, Karl-Heinz, Bosch, Fritz, Brandau, Carsten, Chen, Weidong, Dimopoulou, Christina, Förster, Eckhart, Grisenti, Robert Evaristo, Gumberidze, Alexandre, Hagmann, Siegbert, Hillenbrand, Pierre-Michel, Indelicato, Paul, Jagodziński, Paweł, Kämpfer, Tino, Kozhuharov, Christophor, Lestinsky, Michael, Liesen, Heinz-Dieter, Litvinov, Yuri A., Loetzsch, Robert, Manil, Bruno, Märtin, Renate, Nolden, Fritz, Petridis, Nikolaos, Sanjari, Mohammad Shahab, Schulze, Kai-Sven, Schwemlein, Max, Simionovici, Alexandre S., Steck, Markus, Stöhlker, Thomas, Szabo, Csilla I., Trotsenko, Sergiy, Uschmann, Ingo, Weber, Günter, Wehrhan, Ortrud, Winckler, Nicolas, Winters, Danyal Ferdinant Alexander, Winters, Natalya, Ziegler, Eric, Beyer, Heinrich F., Gaßner, Tobias, Trassinelli, Martino, Heß, Regina, Spillmann, Uwe, Banaś, Dariusz, Blumenhagen, Karl-Heinz, Bosch, Fritz, Brandau, Carsten, Chen, Weidong, Dimopoulou, Christina, Förster, Eckhart, Grisenti, Robert Evaristo, Gumberidze, Alexandre, Hagmann, Siegbert, Hillenbrand, Pierre-Michel, Indelicato, Paul, Jagodziński, Paweł, Kämpfer, Tino, Kozhuharov, Christophor, Lestinsky, Michael, Liesen, Heinz-Dieter, Litvinov, Yuri A., Loetzsch, Robert, Manil, Bruno, Märtin, Renate, Nolden, Fritz, Petridis, Nikolaos, Sanjari, Mohammad Shahab, Schulze, Kai-Sven, Schwemlein, Max, Simionovici, Alexandre S., Steck, Markus, Stöhlker, Thomas, Szabo, Csilla I., Trotsenko, Sergiy, Uschmann, Ingo, Weber, Günter, Wehrhan, Ortrud, Winckler, Nicolas, Winters, Danyal Ferdinant Alexander, Winters, Natalya, Ziegler, Eric, and Beyer, Heinrich F.

Abstract

Accurate spectroscopy of highly-charged high-Z ions in a storage ring is demonstrated to be feasible by the use of specially adapted crystal optics. The method has been applied for the measurement of the 1s Lamb shift in hydrogen-like gold (Au+78) in a storage ring through spectroscopy of the Lyman x-rays. This measurement represents the first result obtained for a high-Z element using high-resolution wavelength-dispersive spectroscopy in the hard x-ray regime, paving the way for sensitivity to higher- order QED effects.

Published
2018

19. Dual energy nano-XRF quantification in EL-3 fragments of the Almahata Sitta TC3 asteroid

Author

Simionovici, A. S., David, G., Lemelle, Laurence, Boyet, M., Gillet, Ph, Rivard, C., El Goresy, A., Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement [Lyon] (LGL-TPE), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Lyon 1, Depot 2, Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[SDU] Sciences of the Universe [physics], [SDU]Sciences of the Universe [physics]
Published
2015

20. NanoXRF elemental mapping of Middle Jurassic (~-170Ma) coccoliths

Author

Suchéras-Marx, Baptiste, Giraud, Fabienne, Daniel, Isabelle, Simionovici, Alexandre S., Tucoulou, Rémi, Simionovici, Alexandre, Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), Institut des Sciences de la Terre (ISTerre), Institut national des sciences de l'Univers (INSU - CNRS)-Institut de recherche pour le développement [IRD] : UR219-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Gustave Eiffel-Université Grenoble Alpes (UGA), European Synchrotron Radiation Facility (ESRF), and Suchéras-Marx, Baptiste

Subjects
[SDU.STU.PG] Sciences of the Universe [physics]/Earth Sciences/Paleontology, [SDU.STU.PG]Sciences of the Universe [physics]/Earth Sciences/Paleontology
Abstract

International audience; Coccolithophores algae produce micrometric calcite platelets called coccoliths. Coccoliths geological record is continuous from their appearance 220 Ma ago until today and are found in abundant marine environment in this time interval. Hence, coccoliths have huge potential for geochemical reconstruction of paleoclimate and paleoceanography through time. We have performed nanometric XRF analysis on 3 species of Early Bajocian (Middle Jurassic) coccoliths at European Synchrotron Radiation Facility (ESRF) on the beamline ID22NI, Grenoble, France. Based on this analysis, we endeavor to have a better understanding of the chemical composition of coccoliths and thus of marine waters where they were precipitated. Samples have been collected at Cabo Mondego, Portugal, the international reference section (GSSP) for the Early Bajocian interval and they were selected based on their preservation. Beforehand, coccoliths were separated from the matrix using a picking technique and deposited on 500 nm-thick silicon nitride membranes. With an excitation beam at 17 KeV and a resolution of 100 m, we have mapped 14 elements in coccoliths, i.e., S, Cl, K, Ca, Ti, V, Cr, Mn, Fe, Cu, Zn, Br, Rb and Sr. The mapping allows the recognition of biological incorporation of elements from the diagenetic overprint. Calcium, Strontium and Manganese are biologically organized in coccoliths. Sulfur, Chlorine, Chromium, and Bromine are also homogenously incorporated without relation with the crystallographic organization of the coccolith. Conversely, Potassium, Iron, Copper, Zinc, Titanium and Rubidium are related to diagenetic processes and clays contamination. These results will (1) help in a better understanding of the chemical incorporation of elements, and (2) in the recognition of diagenetic effects on coccoliths chemistry, and finally (3) develop new paleoceanographic proxies, e.g. the Chlorine and Bromine incorporation in coccoliths for salinity reconstructions. Further analysis especially on living species will greatly help in the calibration of such a proxy.

Published
2013

21. NanoXRF cartography of Middle Jurassic (~-170 Ma) coccoliths

Author

Suchéras-Marx, Baptiste, Giraud, Fabienne, Daniel, Isabelle, Simionovici, Alexandre S., Tucoulou, Rémi, Mattioli, Emanuela, Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), Institut des Sciences de la Terre (ISTerre), Institut national des sciences de l'Univers (INSU - CNRS)-Institut de recherche pour le développement [IRD] : UR219-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Gustave Eiffel-Université Grenoble Alpes (UGA), European Synchroton Radiation Facility [Grenoble] (ESRF), and Suchéras-Marx, Baptiste

Subjects
[SDU.STU.GC]Sciences of the Universe [physics]/Earth Sciences/Geochemistry, [SDU.STU.GC] Sciences of the Universe [physics]/Earth Sciences/Geochemistry, [SDU.STU.PG] Sciences of the Universe [physics]/Earth Sciences/Paleontology, [SDU.STU.PG]Sciences of the Universe [physics]/Earth Sciences/Paleontology
Abstract

International audience; Coccolithophores, golden-brown algae, produce micrometric calcite platelets called coccoliths. Coccoliths geological record is continuous from their appearance 220 Ma ago until today. Hence, coccoliths have huge potential for geochemical reconstruction of paleoclimate and paleoceanography through time. We have performed sub-micrometric XRF analysis on 3 species of Early Bajocian (Middle Jurassic) coccoliths at European Synchrotron Radiation Facility (ESRF) on the beamline ID22NI, Grenoble, France. Based on this analysis, which had never been applied on coccoliths before, we endeavor to have a better understanding of the chemical composition of coccoliths and thus of marine waters where they were precipitated. Samples have been collected at Cabo Mondego, Portugal, the international reference section (GSSP) for the Early Bajocian interval and they were selected based on their preservation. Beforehand, coccoliths were separated from the matrix using a picking technique and deposited on 500 nm-thick silicon nitride membranes. With an excitation beam at 17 KeV and a resolution of 100 m, we have mapped 14 elements in coccoliths, i.e., S, Cl, K, Ca, Ti, V, Cr, Mn, Fe, Cu, Zn, Br, Rb and Sr. The mapping allows the recognition of biological incorporation of elements from the diagenetic overprint. Calcium, Strontium and Manganese are biologically organized in coccoliths. Sulfur, Chlorine, Chromium, and Bromine are also incorporated in coccoliths without suffering any diagenetic process. Conversely, Potassium, Iron, Copper, Zinc, Titanium and Rubidium are related to diagenetic processes and clays contamination.These results, namely the first record of sub-micrometric chemical organization documented for coccoliths, will (1) help in a better understanding of the chemical incorporation of elements, and (2) in the recognition of diagenetic effects on coccoliths chemistry, and finally (3) develop new paleoceanographic proxies, e.g. the Chlorine and Bromine incorporation in coccoliths for salinity reconstructions. Further analysis especially on living species will greatly help in the calibration of such a proxy.

Published
2011

22. Semi-quantitative analysis of bulk chondritic material using X-Ray fluorescence spectroscopy

Author

Simionovici, A. S., Hubert, A., Quitté, Ghylaine, Lemelle, Laurence, Ferroir, Tristan, Sole, A. V., Haschke, M., Laboratoire de Géodynamique des Chaines Alpines (LGCA), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut des Sciences de la Terre (ISTerre), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-PRES Université de Grenoble-Institut de recherche pour le développement [IRD] : UR219-Institut national des sciences de l'Univers (INSU - CNRS)-Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-PRES Université de Grenoble-Institut de recherche pour le développement [IRD] : UR219-Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR), Laboratoire de Sciences de la Terre (LST), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), European Synchrotron Radiation Facility (ESRF), Bruker Nano Microanalysis GmbH, Bruker AXS, Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire des Sciences de l'Univers de Grenoble [1985-2015] (OSUG [1985-2015]), Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology [2007-2019] (Grenoble INP [2007-2019])-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology [2007-2019] (Grenoble INP [2007-2019])-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut des Sciences de la Terre [2011-2015] (ISTerre [2011-2015]), Université Joseph Fourier - Grenoble 1 (UJF)-Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR)-Institut national des sciences de l'Univers (INSU - CNRS)-Institut de recherche pour le développement [IRD] : UR219-PRES Université de Grenoble-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR)-Institut de recherche pour le développement [IRD] : UR219-PRES Université de Grenoble-Centre National de la Recherche Scientifique (CNRS), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[SDU.STU.GC]Sciences of the Universe [physics]/Earth Sciences/Geochemistry, [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], [SDE.MCG]Environmental Sciences/Global Changes, [PHYS.PHYS.PHYS-GEO-PH]Physics [physics]/Physics [physics]/Geophysics [physics.geo-ph]
Abstract

73rd Annual Meeting of the Meteoritical-Society, New York, NY, July 26-30, 2010; International audience; Synchrotron radiation X-ray fluorescence (SR-XRF) is a method of choice to analyze fragile, unique meteoritic samples, requiring no sample preparation. It is a nondestructive, multielemental, quantitative method, easily coupled to diffraction and speciation for a detailed sample characterization. The composition of samples thicker than a few microns is however difficult to obtain due to the high attenuation of the characteristic X-rays resulting in non-detection of low-Z elements (Z≤ 14).

Published
2010

23. Non-desctructive X-Ray, Raman and IR Imaging of quarantined Mars return samples

Author

Simionovici, A. S., Beck, P., Lemelle, Laurence, Ferroir, T., Westphal, Andrew, Vincze, Laszlo, Schoonjans, T., Sole, A. V., Toucoulou, R., Fihman, François, Viso, Michel, Chazalnoel, Pascale, Laboratoire de Géodynamique des Chaines Alpines (LGCA), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Planétologie de Grenoble (LPG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Sciences de la Terre (LST), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley], University of California-University of California, Department of Analytical Chemistry, Universiteit Gent = Ghent University [Belgium] (UGENT), European Synchrotron Radiation Facility (ESRF), 6TEC, Centre National d'Études Spatiales [Toulouse] (CNES), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut des Sciences de la Terre (ISTerre), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-PRES Université de Grenoble-Institut de recherche pour le développement [IRD] : UR219-Institut national des sciences de l'Univers (INSU - CNRS)-Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-PRES Université de Grenoble-Institut de recherche pour le développement [IRD] : UR219-Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR), Ghent University [Belgium] (UGENT), Observatoire des Sciences de l'Univers de Grenoble [1985-2015] (OSUG [1985-2015]), Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology [2007-2019] (Grenoble INP [2007-2019])-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology [2007-2019] (Grenoble INP [2007-2019])-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut des Sciences de la Terre [2011-2015] (ISTerre [2011-2015]), Université Joseph Fourier - Grenoble 1 (UJF)-Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR)-Institut national des sciences de l'Univers (INSU - CNRS)-Institut de recherche pour le développement [IRD] : UR219-PRES Université de Grenoble-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR)-Institut de recherche pour le développement [IRD] : UR219-PRES Université de Grenoble-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), and Universiteit Gent = Ghent University (UGENT)

Subjects
[SDU.STU.GC]Sciences of the Universe [physics]/Earth Sciences/Geochemistry, [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], [SDE.MCG]Environmental Sciences/Global Changes, [PHYS.PHYS.PHYS-GEO-PH]Physics [physics]/Physics [physics]/Geophysics [physics.geo-ph]
Abstract

73rd Annual Meeting of the Meteoritical-Society : New York, NY, July 26-30, 2010; International audience; In preparation for the upcoming international Mars Sample Return mission, bringing to Earth samples containing potential biohazards, we have implemented a hyperspectral method of analysis of grains performed in BSL4 quarantine conditions,by combining several non-destructive imaging diagnostics. This methodology was tested on meteorites [1, 2] and cometary grains from the recent NASA Stardust mission [3-6].

Published
2010

25. Final reports of the Stardust Interstellar Preliminary Examination

Author

Westphal, Andrew J., Bechtel, Hans A., Brenker, Frank E., Butterworth, Anna L., Flynn, George, Frank, David R., Gainsforth, Zack, Hillier, Jon K., Postberg, Frank, Simionovici, Alexandre S., Sterken, Veerle J., Stroud, Rhonda M., Allen, Carlton, Anderson, David, Ansari, Asna, Bajt, Saša, Bastien, Ron K., Bassim, Nabil, Borg, Janet, Bridges, John, Brownlee, Donald E., Burchell, Mark J., Burghammer, Manfred, Changela, Hitesh, Cloetens, Peter, Davis, Andrew M., Doll, Ryan, Floss, Christine, Grün, Eberhard, Heck, Philipp R., Hoppe, Peter, Hudson, Bruce, Huth, Joachim, Hvide, Brit, Kearsley, Anton, King, Ashley J., Lai, Barry, Leitner, Jan, Lemelle, Laurence, Leroux, Hugues, Leonard, Ariel, Lettieri, Robert, Marchant, William, Nittler, Larry R., Ogliore, Ryan, Ong, Wei Ja, Price, Mark C., Sandford, Scott A., Tresseras, Juan-Angel Sans, Schmitz, Sylvia, Schoonjans, Tom, Silversmit, Geert, Solé, Vicente A., Srama, Ralf, Stadermann, Frank, Stephan, Thomas, Stodolna, Julien, Sutton, Steven, Trieloff, Mario, Tsou, Peter, Tsuchiyama, Akira, Tyliszczak, Tolek, Vekemans, Bart, Vincze, Laszlo, Von Korff, Joshua, Wordsworth, Naomi, Zevin, Daniel, Zolensky, Michael E., Westphal, Andrew J., Bechtel, Hans A., Brenker, Frank E., Butterworth, Anna L., Flynn, George, Frank, David R., Gainsforth, Zack, Hillier, Jon K., Postberg, Frank, Simionovici, Alexandre S., Sterken, Veerle J., Stroud, Rhonda M., Allen, Carlton, Anderson, David, Ansari, Asna, Bajt, Saša, Bastien, Ron K., Bassim, Nabil, Borg, Janet, Bridges, John, Brownlee, Donald E., Burchell, Mark J., Burghammer, Manfred, Changela, Hitesh, Cloetens, Peter, Davis, Andrew M., Doll, Ryan, Floss, Christine, Grün, Eberhard, Heck, Philipp R., Hoppe, Peter, Hudson, Bruce, Huth, Joachim, Hvide, Brit, Kearsley, Anton, King, Ashley J., Lai, Barry, Leitner, Jan, Lemelle, Laurence, Leroux, Hugues, Leonard, Ariel, Lettieri, Robert, Marchant, William, Nittler, Larry R., Ogliore, Ryan, Ong, Wei Ja, Price, Mark C., Sandford, Scott A., Tresseras, Juan-Angel Sans, Schmitz, Sylvia, Schoonjans, Tom, Silversmit, Geert, Solé, Vicente A., Srama, Ralf, Stadermann, Frank, Stephan, Thomas, Stodolna, Julien, Sutton, Steven, Trieloff, Mario, Tsou, Peter, Tsuchiyama, Akira, Tyliszczak, Tolek, Vekemans, Bart, Vincze, Laszlo, Von Korff, Joshua, Wordsworth, Naomi, Zevin, Daniel, and Zolensky, Michael E.

Published
2014

26. Evidence for interstellar origin of seven dust particles collected by the Stardust spacecraft

Author

Westphal, A. J., Stroud, R. M., Bechtel, H. A., Brenker, F. E., Butterworth, A. L., Flynn, G. J., Frank, D. R., Gainsforth, Z., Hillier, Jon K., Postberg, F., Simionovici, A. S., Sterken, V. J., Nittler, L. R., Allen, C., Anderson, D., Ansari, A., Bajt, S., Bastien, R. K., Bassim, N., Bridges, J., Brownlee, D. E., Burchell, Mark J., Burghammer, M., Changela, H., Cloetens, P., Davis, A. M., Doll, R., Floss, C., Grun, E., Heck, P. R., Hoppe, P., Hudson, B., Huth, J., Kearsley, A., King, A. J., Lai, B., Leitner, J., Lemelle, L., Leonard, A., Leroux, H., Lettieri, R., Marchant, W., Ogliore, R., Ong, W. J., Price, M. C., Sandford, S. A., Tresseras, J.-A. S., Schmitz, S., Schoonjans, T., Schreiber, K., Silversmit, G., Sole, V. A., Srama, R., Stadermann, F., Stephan, T., Stodolna, J., Sutton, S., Trieloff, M., Tsou, P., Tyliszczak, T., Vekemans, B., Vincze, L., Von Korff, J., Wordsworth, N., Zevin, D., Zolensky, M. E., Westphal, A. J., Stroud, R. M., Bechtel, H. A., Brenker, F. E., Butterworth, A. L., Flynn, G. J., Frank, D. R., Gainsforth, Z., Hillier, Jon K., Postberg, F., Simionovici, A. S., Sterken, V. J., Nittler, L. R., Allen, C., Anderson, D., Ansari, A., Bajt, S., Bastien, R. K., Bassim, N., Bridges, J., Brownlee, D. E., Burchell, Mark J., Burghammer, M., Changela, H., Cloetens, P., Davis, A. M., Doll, R., Floss, C., Grun, E., Heck, P. R., Hoppe, P., Hudson, B., Huth, J., Kearsley, A., King, A. J., Lai, B., Leitner, J., Lemelle, L., Leonard, A., Leroux, H., Lettieri, R., Marchant, W., Ogliore, R., Ong, W. J., Price, M. C., Sandford, S. A., Tresseras, J.-A. S., Schmitz, S., Schoonjans, T., Schreiber, K., Silversmit, G., Sole, V. A., Srama, R., Stadermann, F., Stephan, T., Stodolna, J., Sutton, S., Trieloff, M., Tsou, P., Tyliszczak, T., Vekemans, B., Vincze, L., Von Korff, J., Wordsworth, N., Zevin, D., and Zolensky, M. E.

Abstract

Seven particles captured by the Stardust Interstellar Dust Collector and returned to Earth for laboratory analysis have features consistent with an origin in the contemporary interstellar dust stream. More than 50 spacecraft debris particles were also identified. The interstellar dust candidates are readily distinguished from debris impacts on the basis of elemental composition and/or impact trajectory. The seven candidate interstellar particles are diverse in elemental composition, crystal structure, and size. The presence of crystalline grains and multiple iron-bearing phases, including sulfide, in some particles indicates that individual interstellar particles diverge from any one representative model of interstellar dust inferred from astronomical observations and theory.

Published
2014

28. Stardust Interstellar Preliminary Examination I: Identification of tracks in aerogel

Author

Westphal, Andrew J., primary, Anderson, David, additional, Butterworth, Anna L., additional, Frank, David R., additional, Lettieri, Robert, additional, Marchant, William, additional, Von Korff, Joshua, additional, Zevin, Daniel, additional, Ardizzone, Augusto, additional, Campanile, Antonella, additional, Capraro, Michael, additional, Courtney, Kevin, additional, Criswell, Mitchell N., additional, Crumpler, Dixon, additional, Cwik, Robert, additional, Gray, Fred Jacob, additional, Hudson, Bruce, additional, Imada, Guy, additional, Karr, Joel, additional, Wah, Lily Lau Wan, additional, Mazzucato, Michele, additional, Motta, Pier Giorgio, additional, Rigamonti, Carlo, additional, Spencer, Ronald C., additional, Woodrough, Stephens B., additional, Santoni, Irene Cimmino, additional, Sperry, Gerry, additional, Terry, Jean‐Noel, additional, Wordsworth, Naomi, additional, Yahnke, Tom, additional, Allen, Carlton, additional, Ansari, Asna, additional, Bajt, Saša, additional, Bastien, Ron K., additional, Bassim, Nabil, additional, Bechtel, Hans A., additional, Borg, Janet, additional, Brenker, Frank E., additional, Bridges, John, additional, Brownlee, Donald E., additional, Burchell, Mark, additional, Burghammer, Manfred, additional, Changela, Hitesh, additional, Cloetens, Peter, additional, Davis, Andrew M., additional, Doll, Ryan, additional, Floss, Christine, additional, Flynn, George, additional, Gainsforth, Zack, additional, Grün, Eberhard, additional, Heck, Philipp R., additional, Hillier, Jon K., additional, Hoppe, Peter, additional, Huth, Joachim, additional, Hvide, Brit, additional, Kearsley, Anton, additional, King, Ashley J., additional, Lai, Barry, additional, Leitner, Jan, additional, Lemelle, Laurence, additional, Leroux, Hugues, additional, Leonard, Ariel, additional, Nittler, Larry R., additional, Ogliore, Ryan, additional, Ong, Wei Ja, additional, Postberg, Frank, additional, Price, Mark C., additional, Sandford, Scott A., additional, Tresseras, Juan‐Angel Sans, additional, Schmitz, Sylvia, additional, Schoonjans, Tom, additional, Silversmit, Geert, additional, Simionovici, Alexandre S., additional, Solé, Vicente A., additional, Srama, Ralf, additional, Stephan, Thomas, additional, Sterken, Veerle J., additional, Stodolna, Julien, additional, Stroud, Rhonda M., additional, Sutton, Steven, additional, Trieloff, Mario, additional, Tsou, Peter, additional, Tsuchiyama, Akira, additional, Tyliszczak, Tolek, additional, Vekemans, Bart, additional, Vincze, Laszlo, additional, and Zolensky, Michael E., additional

Published
2014
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29. Coordinated Microanalyses of Seven Particles of Probable Interstellar Origin from the Stardust Mission.

Author

Westphal, Andrew J., primary, Stroud, Rhonda M., additional, Bechtel, Hans A., additional, Brenker, Frank E., additional, Butterworth, Anna L., additional, Flynn, George J., additional, Frank, David R., additional, Gainsforth, Zack, additional, Hillier, Jon K., additional, Postberg, Frank, additional, Simionovici, Alexandre S., additional, Sterken, Veerle J., additional, Allen, Carlton, additional, Anderson, David, additional, Ansari, Asna, additional, Bajt, Saˇsa, additional, Bastien, Ron K., additional, Bassim, Nabil, additional, Bridges, John, additional, Brownlee, Donald E., additional, Burchell, Mark, additional, Burghammer, Manfred, additional, Changela, Hitesh, additional, Cloetens, Peter, additional, Davis, Andrew M., additional, Doll, Ryan, additional, Floss, Christine, additional, Gru¨n, Eberhard, additional, Heck, Philipp R., additional, Hoppe, Peter, additional, Hudson, Bruce, additional, Huth, Joachim, additional, Kearsley, Anton, additional, King, Ashley J., additional, Lai, Barry, additional, Leitner, Jan, additional, Lemelle, Laurence, additional, Leonard, Ariel, additional, Leroux, Hugues, additional, Lettieri, Robert, additional, Marchant, William, additional, Nittler, Larry R., additional, Ogliore, Ryan, additional, Jia Ong, Wei, additional, Price, Mark C., additional, Sandford, Scott A., additional, Sans Tresseras, Juan-Angel, additional, Schmitz, Sylvia, additional, Schoonjans, Tom, additional, Schreiber, Kate, additional, Silversmit, Geert, additional, Solé, Vicente A., additional, Srama, Ralf, additional, Stadermann, Frank, additional, Stephan, Thomas, additional, Stodolna, Julien, additional, Sutton, Stephen, additional, Trieloff, Mario, additional, Tsou, Peter, additional, Tyliszczak, Tolek, additional, Vekemans, Bart, additional, Vincze, Laszlo, additional, Von Korff, Joshua, additional, Wordsworth, Naomi, additional, Zevin, Daniel, additional, and Zolensky, Michael E., additional

Published
2014
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30. Stardust Interstellar Preliminary Examination XI: Identification and elemental analysis of impact craters on Al foils from the Stardust Interstellar Dust Collector

Author

Stroud, Rhonda M., Allen, Carlton, Ansari, Asna, Anderson, David, Bajt, Saša, Bassim, Nabil, Bastien, Ron S., Bechtel, Hans A., Borg, Janet, Brenker, Frank E., Bridges, John, Brownlee, Donald E., Burchell, Mark J., Burghammer, Manfred, Butterworth, Anna L., Changela, Hitesh, Cloetens, Peter, Davis, Andrew M., Doll, Ryan, Floss, Christine, Flynn, George, Frank, David R., Gainsforth, Zack, Grün, Eberhard, Heck, Philipp R., Hillier, Jon K., Hoppe, Peter, Huth, Joachim, Hvide, Brit, Kearsley, Anton, King, Ashley J., Kotula, Paul, Lai, Barry, Leitner, Jan, Lemelle, Laurence, Leroux, Hugues, Leonard, Ariel, Lettieri, Robert, Marchant, William, Nittler, Larry R., Ogliore, Ryan, Ong, Wei Jia, Postberg, Frank, Price, Mark C., Sandford, Scott A., Tresseras, Juan-Angel Sans, Schmitz, Sylvia, Schoonjans, Tom, Schreiber, Kate, Silversmit, Geert, Simionovici, Alexandre S., Solé, Vicente A., Srama, Ralf, Stephan, Thomas, Sterken, Veerle J., Stodolna, Julien, Sutton, Steven, Trieloff, Mario, Tsou, Peter, Tsuchiyama, Akira, Tyliszczak, Tolek, Vekemans, Bart, Vincze, Laszlo, Westphal, Andrew J., Von Korff, Joshua, Zevin, Daniel, Zolensky, Michael E., Stroud, Rhonda M., Allen, Carlton, Ansari, Asna, Anderson, David, Bajt, Saša, Bassim, Nabil, Bastien, Ron S., Bechtel, Hans A., Borg, Janet, Brenker, Frank E., Bridges, John, Brownlee, Donald E., Burchell, Mark J., Burghammer, Manfred, Butterworth, Anna L., Changela, Hitesh, Cloetens, Peter, Davis, Andrew M., Doll, Ryan, Floss, Christine, Flynn, George, Frank, David R., Gainsforth, Zack, Grün, Eberhard, Heck, Philipp R., Hillier, Jon K., Hoppe, Peter, Huth, Joachim, Hvide, Brit, Kearsley, Anton, King, Ashley J., Kotula, Paul, Lai, Barry, Leitner, Jan, Lemelle, Laurence, Leroux, Hugues, Leonard, Ariel, Lettieri, Robert, Marchant, William, Nittler, Larry R., Ogliore, Ryan, Ong, Wei Jia, Postberg, Frank, Price, Mark C., Sandford, Scott A., Tresseras, Juan-Angel Sans, Schmitz, Sylvia, Schoonjans, Tom, Schreiber, Kate, Silversmit, Geert, Simionovici, Alexandre S., Solé, Vicente A., Srama, Ralf, Stephan, Thomas, Sterken, Veerle J., Stodolna, Julien, Sutton, Steven, Trieloff, Mario, Tsou, Peter, Tsuchiyama, Akira, Tyliszczak, Tolek, Vekemans, Bart, Vincze, Laszlo, Westphal, Andrew J., Von Korff, Joshua, Zevin, Daniel, and Zolensky, Michael E.

Published
2013

34. Stardust Interstellar Preliminary Examination XI: Identification and elemental analysis of impact craters on Al foils from the Stardust Interstellar Dust Collector

Author

Stroud, Rhonda M., primary, Allen, Carlton, additional, Ansari, Asna, additional, Anderson, David, additional, Bajt, Saša, additional, Bassim, Nabil, additional, Bastien, Ron S., additional, Bechtel, Hans A., additional, Borg, Janet, additional, Brenker, Frank E., additional, Bridges, John, additional, Brownlee, Donald E., additional, Burchell, Mark, additional, Burghammer, Manfred, additional, Butterworth, Anna L., additional, Changela, Hitesh, additional, Cloetens, Peter, additional, Davis, Andrew M., additional, Doll, Ryan, additional, Floss, Christine, additional, Flynn, George, additional, Frank, David R., additional, Gainsforth, Zack, additional, Grün, Eberhard, additional, Heck, Philipp R., additional, Hillier, Jon K., additional, Hoppe, Peter, additional, Huth, Joachim, additional, Hvide, Brit, additional, Kearsley, Anton, additional, King, Ashley J., additional, Kotula, Paul, additional, Lai, Barry, additional, Leitner, Jan, additional, Lemelle, Laurence, additional, Leroux, Hugues, additional, Leonard, Ariel, additional, Lettieri, Robert, additional, Marchant, William, additional, Nittler, Larry R., additional, Ogliore, Ryan, additional, Ong, Wei Jia, additional, Postberg, Frank, additional, Price, Mark C., additional, Sandford, Scott A., additional, Tresseras, Juan‐Angel Sans, additional, Schmitz, Sylvia, additional, Schoonjans, Tom, additional, Schreiber, Kate, additional, Silversmit, Geert, additional, Simionovici, Alexandre S., additional, Solé, Vicente A., additional, Srama, Ralf, additional, Stephan, Thomas, additional, Sterken, Veerle J., additional, Stodolna, Julien, additional, Sutton, Steven, additional, Trieloff, Mario, additional, Tsou, Peter, additional, Tsuchiyama, Akira, additional, Tyliszczak, Tolek, additional, Vekemans, Bart, additional, Vincze, Laszlo, additional, Westphal, Andrew J., additional, Von Korff, Joshua, additional, Zevin, Daniel, additional, and Zolensky, Michael E., additional

Published
2013
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38. Fluorescence microtomography using nanofocusing refractive x-ray lenses

Author

Schroer, Christian G., primary, Gunzler, Til Florian, additional, Kuhlmann, Marion, additional, Kurapova, Olga, additional, Feste, Sebastian, additional, Schweitzer, Mario, additional, Lengeler, Bruno, additional, Schroder, Walter H., additional, Drakopoulos, Michael, additional, Somogyi, Andrea, additional, Simionovici, Alexandre S., additional, Snigirev, Anatoly A., additional, and Snigireva, Irina I., additional

Published
2004
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39. Nanofocusing parabolic refractive x-ray lenses

Author

Schroer, C. G., primary, Kuhlmann, M., additional, Hunger, U. T., additional, Günzler, T. F., additional, Kurapova, O., additional, Feste, S., additional, Frehse, F., additional, Lengeler, B., additional, Drakopoulos, M., additional, Somogyi, A., additional, Simionovici, A. S., additional, Snigirev, A., additional, Snigireva, I., additional, Schug, C., additional, and Schröder, W. H., additional

Published
2003
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40. Beryllium parabolic refractive x-ray lenses

Author

Schroer, Christian G., primary, Kuhlmann, Marion, additional, Lengeler, Bruno, additional, Gunzler, Til F., additional, Kurapova, O., additional, Benner, Boris, additional, Rau, Christoph, additional, Simionovici, Alexandre S., additional, Snigirev, Anatoly A., additional, and Snigireva, Irina, additional

Published
2002
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42. New results in x-ray computed fluorescence tomography

Author

Simionovici, Alexandre S., primary, Chukalina, Marina, additional, Vekemans, B., additional, Lemelle, L., additional, Gillet, Ph., additional, Schroer, Christian G., additional, Lengeler, Bruno, additional, Schroeder, Walter H., additional, and Jeffries, Theresa, additional

Published
2002
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46. Nanofocusing Parabolic Refractive X-Ray Lenses.

Author

Schroer, C. G., Kuhlmann, M., Hunger, U. T., Günzler, T. F., Kurapova, O., Feste, S., Lengeler, B., Drakopoulos, M., Somogyi, A., Simionovici, A. S., Snigirev, A., Snigireva, I., and Warwick, T.

Subjects
X-rays, LENSES, X-ray spectra, X-ray refraction, SYNCHROTRON radiation sources, SYNCHROTRON radiation, PARTICLES (Nuclear physics), PHYSICS
Abstract

Parabolic refractive x-ray lenses with short focal distance can generate intensive hard x-ray microbeams with lateral extensions in the 100nm range even at short distance from a synchrotron radiation source. We have fabricated planar parabolic lenses made of silicon that have a focal distance in the range of a few millimeters at hard x-ray energies. In a crossed geometry, two lenses were used to generate a microbeam with a lateral size of 330nm by 110nm at 25keV in a distance of 41.8m from the synchrotron radiation source. First microdiffraction and fluorescence microtomography experiments were carried out with these lenses. Using diamond as lens material, microbeams with lateral size down to 20nm and below are conceivable in the energy range from 10 to 100keV. © 2004 American Institute of Physics [ABSTRACT FROM AUTHOR]

Published
2004
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