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Crouzet N., et al. |
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Title |
Towards ASTEP+, a two-color photometric telescope at Dome C, Antarctica |
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Conference - International - Communication |
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2020 |
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SPIE Astronomical Telescopes + Instrumentation (AS20), online, 14-18 December 2020 |
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Paper 11447-23 |
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1066 |
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Bachelor's thesis |
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7831 |
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Ricaud, P., Del Guasta M., Bazile E., Azouz N., Lupi A., Durand P., Attié J.-L., Veron D., Guidard V., Grigioni P. |
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Supercooled Liquid Water Cloud observed, analysed and modelled at the Top of the Planetary Boundary Layer above Dome C |
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Communication |
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2020 |
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Antarctica, SCAR, Visio, Hobart, Australia, August 2020 |
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910 |
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7839 |
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Philippe Ricaud, Paolo Grigioni, Romain Roehrig, Pierre Durand, Dana E. Veron |
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Trends in Atmospheric Humidity and Temperature above Dome C |
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Communication |
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2020 |
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Antarctica Evaluated from Observations and Reanalyses, SCAR, Visio, Hobart, Australia, August 2020. |
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7840 |
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Barbero A. Grilli R., Blouzon C., Caillon N., Savarino, J. |
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New Observations to Better Constrain NOx (NO + NO2) Concentrations on the Antarctic Plateau and to Resolve the Ambiguity in the NO2:NO Ratio |
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Communication |
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2020 |
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AGU Fall Meeting 2020, 1-17 December 2020 San Francisco, USA |
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High southern latitude regions present specificities that are highly relevant for studying the climate in connection with the atmospheric chemistry. Contrary to regions of the rest of the world, Antarctica is still considered as a pristine environment not yet influenced by predominant anthropogenic emissions (with the notable exceptions of GHG) and thus represents the last continental-size natural laboratory. Polar snow-air-radiation interactions and the specific oxidant character of the polar atmosphere are key in order to decipher the right information buried in the ice and the current chemical stability of the polar atmosphere. Previous Antarctic campaigns have shown atmospheric similarities between the Antarctic Plateau (at Dome C, Concordia) and other regions. However, several differences are yet to be explained: the large NO2:NO ratios previously found in ambient air indicates the existence of an unknown source of NO2 above the Antarctic Plateau. These observations question either the reliability of previous measurements or the lack of our understanding of the NOx chemistry. Novel optical instruments based on the incoherent broadband cavity enhanced absorption spectroscopy technique (IBBCEAS) were developed. The instruments can measure simultaneously NO2, NOx and NO with detection limits of 11, 10 and 21 ppt, respectively (1σ) within 22 minutes of measurements. The two compact and transportable instruments were deployed during the 2019/20 Dome C summer campaign. Atmospheric measurements together with flux chamber experiments were performed for determining the snowpack NOx emissions and the NO2:NO ratio. The observations seem to differ from the conclusions of the previous Antarctic campaigns. Assuming steady state and maximum radiations, the theoretical NO2:NO ratio from the period observed in December was calculated to be 0.38 ± 0.15 and 0.31 ± 0.12 in January. The instruments measured a ratio close to steady state in December (0.25 ± 0.25) while the ratio observed in January (1.248 ± 0.792) indicates the presence of a strong NO oxidant or an unknown source of NO2. Flux chamber experiments on different types of snow were done during this campaign, and the results will help deepen our knowledge of Antarctic atmospheric chemistry. |
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7864 |
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Ishino S., Hattori S., Savarino J., Legrand M., Albalat E., Albarède F., Preunkert S., Jourdain B., Yoshida N. |
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Title |
Homogeneous sulfur isotope signature in East Antarctica and implication for sulfur source shifts through the last glacial-interglacial cycle |
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Communication |
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2020 |
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The Geochemical Society of Japan |
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1177 |
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7865 |
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Casado M., Leroy-Dos C., Fourre E., Favier V., Agosta C., Arnaud L., Prié F., Akers P., Janssen L., Savarino J., Landais A. |
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Water vapor isotopic signature along the EAIIST traverse |
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Communication |
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2020 |
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EGU General Assembly, 19-30 April 2021 |
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yes |
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7868 |
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Author |
Sara Aoroli |
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Calibration and exploitation of an automatic spectral albedometer to estimate near-surface snow SSA time series |
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Master 2 |
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2020 |
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1110 |
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7891 |
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C Engrand, E Charon, H Le- Roux, M Marinova, J Duprat, E Dartois, B Guérin, J Rojas, L Delauche, M Godard, D Troadec |
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Title |
Evidence of irradiation in interplanetary space in minerals from an ultracarbonaceous Antarctic micrometeorites (UCAMM) |
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Peer-reviewed symposium |
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2020 |
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Lunar and Planetary Science Conference |
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Introduction: Ultracarbonaceous Antarctic Micrometeorites (UCAMMs) are dominated by N-rich polyaromatic organic matter exhibiting large D enrichments [1-5]. The high abundance of organic matter exhibiting large D enrichment suggests a cometary origin for UCAMMs [1-3]. Three kinds of organic matter are identified in UCAMMs, with different nitrogen abundances and highly variable concentrations of small (typically 30-500 nanometer) mineral aggregates embedded in the organic matter [5-8]. We focus here on a mineral assemblage embedded in one UCAMM that exhibits evidence of ion irradiation, to get insight on the formation and evolution of this cometary particle. Sample and methods: A fragment of UCAMM DC06-06-43 (hereafter DC06-43) was carbon coated, observed by SEM/EDX, and a 100 nm thick FIB section of this fragment was made at IEMN Lille. The size of the initial UCAMM before fragmentation was ~ 25 x 30 µm. After STXM-XANES analysis, the mineralogy of the sample was investigated by TEM at UMET Lille using a FEI Tecnai G2 20 at 200 kV and FEI TITAN Themis at 300 kV [9]. Results : TEM examination reveals a large assemblage of crystalline minerals at the center of the DC06-43 UCAMM fragment, surrounded by organic matter (Figure 1) [9]. The assemblage consists of µm-to subµm sized Mg-rich pyroxenes, a large “triskell”-shaped Fe-sulfide, a few Mg-rich olivines, and minor Si-Al-Carich amorphous pockets and Fe-Ni metal. About 28 crystalline pyroxenes are identified whereas only 5 olivine crystals are observed in the section. GEMS are present embedded in the organic matter, close to the crystalline assemblage. We identified irradiation features (rims and tracks) in pyroxene grains. No rims or tracks were found in olivine. We observed irradiated rims around six pyroxenes at the top of the section (Figure 1, light blue labels). One pyroxene shows a continuous irradiated rim (Figure 2 top). Rim thicknesses range from 20 to 100 nm, with an average of 60 ± 20 nm (1σ) (Figure 2 bottom). Fe-rich deposits are occasionally found on top of irradiated rims. EDX mappings and profiles show that the rims are strongly depleted in Mg (Figure 3). The average track density in pyroxene grains measured over an area of 4.5 x 10-8 cm 2 is 1.3 x 10 10 cm-2 with one value at 3.8 x 10 9 cm-2 , the other values ranging from 9.5 x 10 9 to 3.2 x 10 10 cm-2 (Figure 4). Irradiation track lengths |
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1120 |
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7909 |
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B Guérin, C Engrand, C Le Guillou, H Leroux, J Duprat, E Dartois, S Bernard, K Ben- Zerara, J Rojas, M Godard, L Delauche, D Troadec |
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Title |
STEM and STXM-XANES analysis of FIB sections of Ultracarbonaceous Antarctic Micrometeorites (UCAMMs) |
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Peer-reviewed symposium |
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2020 |
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Lunar and Planetary Science Conference, id 2117 |
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51 |
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2117 |
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Introduction: Ultracarbonaceous Antarctic Micrometeorites (UCAMMS) are extraterrestrial dust particles containing large amount of carbonaceous material with elevated D/H ratios [1] and high N/C atomic ratio (up to 0.2)[2]. UCAMMS are rare (~ 1% of the particles in the Concordia meteorite collection) but they have been identified in several collection of interplanetary dust [3, 4]. They are most probably of cometary origin. Here, we studied the association of organic matter and minerals by scanning transmission X-ray microscopy (STXM-XANES) coupled with scanning transmission electronic microscopy (TEM/STEM). Samples and Methods: The UCAMMs studied here were collected in the Antarctic snow, close to the Concordia station at Dome C [3]. FIB sections of 8 UCAMMs (DC06-18, DC06-41, DC06-43, DC06-65, DC06-308, DC06-139, DC16-30, DC16-309) were analyzed using synchrotron based STXM-XANES at the carbon, nitrogen and oxygen K-edges. The FIB sections were subsequently analyzed with transmission electron microscopy (TEM/STEM) using a FEI Tecnai G2 20 and a FEI TITAN Themis 300 [5, 6]. Peak identification of STXM-XANES spectra are based on [7]. XANES spectra are processed and quantified using Quantorxs method [8] and quantification of STEM EDS spectra has been realized using Hyperspy software [9]. Here, we mainly present results obtained on two recently identified UCAMMs (DC06-308 and DC16-309) and compare them with previous observations [1, 5, 6]. Results: The STXM-XANES analysis reveals 3 types of organic matter (OM) characterized by different carbon speciation. Figure 1 shows type I OM in blue and type II OM in green, both having spectra close to that of chondritic insoluble organic matter (IOM). The main peaks of type I and II OMs are found around 284.8 eV (aromatic and olefinic groups (C=C)), 286.4 eV (ketone and phenol C=O) and 288.4 eV (carboxyl O=C-O). Type II OM exhibits similar functional groups as type I OM but the first peak position is shifted to 285 eV, indicating a stronger contribution of the aromatic groups. The atomic N/C ratio of types I/II OMs range between 0.01 and 0.05 (1σ=0.02) similar to those of chondritic IOM. The type III, in red on Figure 1 exhibits larger differences. The main peak is at 286.4 eV (C≡N nitrile), a small peak at 284.8 eV (alkene |
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7910 |
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Y. Kebukawa, M. Zolensly, J. Mathurin, E. Dartois, C. Engrand, J. Duprat, A. Deniset-Besseau, A. Dazzi, M. Fries, T. Ohigashi, D. Wakabayashi, S. Yamashita, Y. Takeichi, Y. Takahashi, M. Kondo, M. Ito, Y. Kodama, Z. Rahman, K. Kobayashi |
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Organic matter in the Aguas Zarcas (CM2) meteorite: high abundance of aliphatic carbon in metal-rich lithology |
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Peer-reviewed symposium |
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2020 |
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Lunar and Planetary Science Conference, id 1349 |
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51 |
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1614 |
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1120 |
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