228 results on '"D'Aversa, E."'
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2. Moons and Jupiter Imaging Spectrometer (MAJIS) on Jupiter Icy Moons Explorer (JUICE)
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Poulet, F., Piccioni, G., Langevin, Y., Dumesnil, C., Tommasi, L., Carlier, V., Filacchione, G., Amoroso, M., Arondel, A., D’Aversa, E., Barbis, A., Bini, A., Bolsée, D., Bousquet, P., Caprini, C., Carter, J., Dubois, J.-P., Condamin, M., Couturier, S., Dassas, K., Dexet, M., Fletcher, L., Grassi, D., Guerri, I., Haffoud, P., Larigauderie, C., Le Du, M., Mugnuolo, R., Pilato, G., Rossi, M., Stefani, S., Tosi, F., Vincendon, M., Zambelli, M., Arnold, G., Bibring, J.-P., Biondi, D., Boccaccini, A., Brunetto, R., Carapelle, A., Cisneros González, M., Hannou, C., Karatekin, O., Le Cle’ch, J.-C., Leyrat, C., Migliorini, A., Nathues, A., Rodriguez, S., Saggin, B., Sanchez-Lavega, A., Schmitt, B., Seignovert, B., Sordini, R., Stephan, K., Tobie, G., Zambon, F., Adriani, A., Altieri, F., Bockelée, D., Capaccioni, F., De Angelis, S., De Sanctis, M.-C., Drossart, P., Fouchet, T., Gérard, J.-C., Grodent, D., Ignatiev, N., Irwin, P., Ligier, N., Manaud, N., Mangold, N., Mura, A., Pilorget, C., Quirico, E., Renotte, E., Strazzulla, G., Turrini, D., Vandaele, A.-C., Carli, C., Ciarniello, M., Guerlet, S., Lellouch, E., Mancarella, F., Morbidelli, A., Le Mouélic, S., Raponi, A., Sindoni, G., and Snels, M.
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- 2024
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3. Milliarcsecond astrometry for the Galilean moons using stellar occultations
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Morgado, B. E., Gomes-Júnior, A. R., Braga-Ribas, F., Vieira-Martins, R., Desmars, J., Lainey, V., D'aversa, E., Dunham, D., Moore, J., Baillié, K., Herald, D., Assafin, M., Sicardy, B., Aoki, S., Bardecker, J., Barton, J., Blank, T., Bruns, D., Carlson, N., Carlson, R. W., Cobble, K., Dunham, J., Eisfeldt, D., Emilio, M., Jacques, C., Hinse, T. C., Kim, Y., Malacarne, M., Maley, P. D., Maury, A., Meza, E., Oliva, F., Orton, G. S., Pereira, C. L., Person, M., Plainaki, C., Sfair, R., Sindoni, G., Smith, M., Sussenbach, E., Stuart, P., Vrolijk, J., and Winter, O. C.
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Astrophysics - Earth and Planetary Astrophysics ,Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
A stellar occultation occurs when a Solar System object passes in front of a star for an observer. This technique allows the determination of sizes and shapes of the occulting body with kilometer precision. Also, this technique constrains the occulting body's positions, albedos, densities, etc. In the context of the Galilean moons, these events can provide their best ground-based astrometry, with uncertainties in the order of 1 mas ($\sim$ 3 km at Jupiter's distance during opposition). We organized campaigns and successfully observed a stellar occultation by Io (JI) in 2021, one by Ganymede (JIII) in 2020, and one by Europa (JII) in 2019, with stations in North and South America. Also, we re-analyzed two previously published events, one by Europa in 2016 and another by Ganymede in 2017. Then, we fit the known 3D shape of the occulting satellite and determine its center of figure. That resulted in astrometric positions with uncertainties in the milliarcsecond level. The positions obtained from these stellar occultations can be used together with dynamical models to ensure highly accurate orbits of the Galilean moons. These orbits can help plan future space probes aiming at the Jovian system, such as JUICE by ESA and Europa Clipper by NASA, and allow more efficient planning of flyby maneuvers., Comment: 19 pages, 25 figures, Accepted on March 14, 2022 for publication in The Astronomical Journal
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- 2022
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4. Saturn's icy satellites investigated by Cassini -- VIMS. V. Spectrophotometry
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Filacchione, G., Ciarniello, M., D'Aversa, E., Capaccioni, F., Clark, R. N., Buratti, B. J., Helfenstein, P., Stephan, K., and Plainaki, C.
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Astrophysics - Earth and Planetary Astrophysics - Abstract
Albedo, spectral slopes, and water ice band depths maps for the five midsized saturnian satellites Mimas, Enceladus, Tethys, Dione, and Rhea have been derived from Cassini-Visual and Infrared Mapping Spectrometer (VIMS) data. The maps are systematically built from photometric corrected data by applying the Kaasalainen-Shkuratov model (Kaasalainen et al., 2001, Shkuratov et al., 2011}. In this work a quadratic function is used to fit phase curves built by filtering observations taken with incidence angle $i\le70^\circ$, emission angle $e\le70^\circ$, phase angle $10^\circ \le g \le 120^\circ$, and Cassini-satellite distance $D \le 100.000$ km. This procedure is systematically repeated for a subset of 65 VIMS visible and near-infrared wavelengths for each satellite. The average photometric parameters are used to compare satellites' properties and to study their variability with illumination conditions changes. We derive equigonal albedo, extrapolated at g=0$^\circ$, not including the opposition effect, equal to 0.63$\pm$0.02 for Mimas, 0.89$\pm$0.03 for Enceladus, 0.74$\pm$0.03 for Tethys, 0.65$\pm$0.03 for Dione, 0.60$\pm$0.05 for Rhea at 0.55 $\mu$m. The knowledge of photometric spectral response allows to correct individual VIMS spectra used to build maps through geolocation. Maps are rendered at a fixed resolution corresponding to a $0.5^\circ \times 0.5^\circ$ bin on a longitude by latitude grid resulting in spatial resolutions of 1.7 km/bin for Mimas, 2.2 km/bin for Enceladus; 4.7 km/bin for Tethys; 4.5 km/bin for Dione; 6.7 km/bin for Rhea. These spectral maps allow establishing relationships with morphological features and with endogenic and exogenic processes capable to alter satellites' surface properties through several mechanisms..., Comment: 60 pages, 16 figures, 6 tables. Accepted for publication on Icarus journal
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- 2021
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5. Observation of the Southern Polar cap during MY34-36 with ExoMars-TGO NOMAD LNO
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Ruiz Lozano, L., Oliva, F., Karatekin, Ö., Bellucci, G., Dehant, V., D'Aversa, E., Carrozzo, F.G., Schmidt, F., Cruz Mermy, G., Thomas, I.R., Vandaele, A.C., Daerden, F., Ristic, B., Patel, M.R., and López-Moreno, J.-J.
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- 2024
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6. Properties of a Martian local dust storm in Atlantis Chaos from OMEGA/MEX data
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Oliva, F., Geminale, A., D'Aversa, E., Altieri, F., Bellucci, G., Carrozzo, F. G., Sindoni, G., and Grassi, D.
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Astrophysics - Earth and Planetary Astrophysics - Abstract
In this study we present the analysis of the dust properties of a local storm imaged in the Atlantis Chaos region on Mars by the OMEGA imaging spectrometer on March 2nd 2005. We use the radiative transfer model MITRA to study the dust properties at solar wavelengths between 0.5 {\mu}m and 2.5 {\mu}m and infer the connection between the local storm dynamics and the topography. We retrieve maps of effective grain radius (reff), optical depth at 9.3 {\mu}m ({\tau}9.3) and top altitude (ta) of the dust layer. Our results show that large particles (reff = 1.6 {\mu}m) are gathered in the centre of the storm (lat=33.5{\deg} S; lon=183.5 W{\deg}), where the optical depth is maximum ({\tau}9.3 > 7.0) and the top altitude exceeds 18 km. Outside the storm, we obtain {\tau}9.3 < 0.2, in agreement with the estimates derived from global climate models (GCM). We speculate that a low thermal inertia region at the western border of Atlantis Chaos is a possible source of the dust storm. Moreover, we find evidence that topography plays a role in confining the local storm in Atlantis Chaos. The vertical wind component from the GCM does not provide any hint for the triggering of dust lifting. On the other hand, the combination of the horizontal and vertical wind profiles suggests that the dust, once lifted, is pushed eastward and then downward and gets confined within the north-east ridge of Atlantis Chaos. (continues in article)
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- 2017
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7. Jupiter's Hotspots as observed by JIRAM-Juno: limb darkening in thermal infrared.
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Grassi, D, Mura, A, Adriani, A, Sindoni, G, Atreya, S K, Fletcher, L N, Orton, G S, Plainaki, C, Tosi, F, Biagiotti, F, Olivieri, A, Castagnoli, C, D'Aversa, E, Migliorini, A, Moirano, A, Noschese, R, Piccioni, G, Sordini, R, and Bolton, S
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NATURAL satellite atmospheres ,NATURAL satellites ,JUNO (Space probe) ,PLANETARY atmospheres ,INFRARED imaging ,ALBEDO - Abstract
The Jupiter InfraRed Auroral Mapper (JIRAM) instrument onboard the Juno spacecraft performed repeated observations of Jupiter's North Equatorial Belt (NEB) around the time of 12th Juno pericenter passage on 2018 April 1. The data consist of thermal infrared images and show, among other atmospheric features, two bright Hotspots on the boundary between the NEB and the Equatorial Zone. Night-time images of the same areas at different emission angles were used to constrain the trend of the limb-darkening function. Comparison with simulated observations, computed for different emission angles, total opacities, single scattering albedo ω
0 , and asymmetry parameter g suggests that ω0 ∼ 0.90 ± 0.05 and g ∼ 0.37 ± 0.15 provide best match with data. Subsequently, we computed the ω0 and g resulting from different size distributions, taking into account the complex refractive indices of ammonium hydrosulfide (NH4 SH) by Howett et al. [2007] and Ferraro et al. [1980]. Only the former data set is marginally consistent with JIRAM observations. Similarly, ammonia and hydrazine barely reproduce the experimental data. Tholin, although not usually considered a realistic component for Jupiter's aerosols, provides a better match for particle radii between 0.7 and 1 μm, both as a pure material as well as a thick coating over NH4 SH cores. Notably, this radius range is consistent with the mean radius of aerosols as estimated by Ragent et al. [1998] on the basis of Galileo entry probe data. Comparison with literature suggests that similar results can be achieved by a large variety of contaminants bearing C–N bounds. [ABSTRACT FROM AUTHOR]- Published
- 2024
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8. Regions of interest on Ganymede's and Callisto's surfaces as potential targets for ESA's JUICE mission
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Stephan, K., Roatsch, T., Tosi, F., Matz, K.-D., Kersten, E., Wagner, R., Molyneux, P., Palumbo, P., Poulet, F., Hussmann, H., Barabash, S., Bruzzone, L., Dougherty, M., Gladstone, R., Gurvits, L.I., Hartogh, P., Iess, L., Wahlund, J.-E., Wurz, P., Witasse, O., Grasset, O., Altobelli, N., Carter, J., Cavalié, T., d'Aversa, E., Della Corte, V., Filacchione, G., Galli, A., Galluzzi, V., Gwinner, K., Hauber, E., Jaumann, R., Krohn, K., Langevin, Y., Lucchetti, A., Migliorini, A., Piccioni, G., Solomonidou, A., Stark, A., Tobie, G., Tubiana, C., Vallat, C., and Van Hoolst, T.
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- 2021
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9. A database of aerosols and gases coefficients for VIS-NIR radiative transfer in the Solar System planetary atmospheres
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Oliva, F., D'Aversa, E., Liberti, G.L., Sindoni, G., Altieri, F., and Castelli, E.
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- 2019
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10. Properties of a Martian local dust storm in Atlantis Chaos from OMEGA/MEX data
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Oliva, F., Geminale, A., D'Aversa, E., Altieri, F., Bellucci, G., Carrozzo, F.G., Sindoni, G., and Grassi, D.
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- 2018
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11. Analysis of IR-bright regions of Jupiter in JIRAM-Juno data: Methods and validation of algorithms
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Grassi, D., Ignatiev, N.I., Sindoni, G., d'Aversa, E., Maestri, T., Adriani, A., Mura, A., Filacchione, G., Dinelli, B.M., Noschese, R., Cicchetti, A., Piccioni, G., Turrini, D., Tosi, F., Moriconi, M.L., Olivieri, A., Plainaki, C., Amoroso, M., Atreya, S.K., Orton, G.S., and Bolton, S.
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- 2017
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12. Observation of the Southern Polar cap during MY34-36 with ExoMars-TGO NOMAD LNO
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Ruiz Lozano, L., primary, Oliva, F., additional, Karatekin, Ö., additional, Bellucci, G., additional, Dehant, V., additional, D'Aversa, E., additional, Carrozzo, F.G., additional, Schmidt, F., additional, Cruz Mermy, G., additional, Thomas, I.R., additional, Vandaele, A.C., additional, Daerden, F., additional, Ristic, B., additional, Patel, M.R., additional, and López-Moreno, J.-J., additional
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- 2023
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13. CO concentration in the upper stratosphere and mesosphere of Titan from VIMS dayside limb observations at 4.7 µm
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Fabiano, F., López Puertas, M., Adriani, A., Moriconi, M.L., D’Aversa, E., Funke, B., López-Valverde, M.A., Ridolfi, M., and Dinelli, B.M.
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- 2017
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14. Deciphering sub-micron ice particles on Enceladus surface
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Scipioni, F., Schenk, P., Tosi, F., D'Aversa, E., Clark, R., Combe, J.-Ph., and Ore, C.M. Dalle
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- 2017
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15. Clouds and hazes vertical structure of a Saturn's giant vortex from Cassini/VIMS-V data analysis
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Oliva, F., Adriani, A., Moriconi, M.L., Liberti, G.L., D'Aversa, E., and Filacchione, G.
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- 2016
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16. In vivo susceptibility to energy failure parkinsonism and LRRK2 kinase activity
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Novello, S, Mercatelli, D, Albanese, F, Domenicale, C, Brugnoli, A, D'Aversa, E, Vantaggiato, S, Dovero, S, Murtaj, V, Presotto, L, Borgatti, M, Shimshek, D, Bezard, E, Moresco, R, Belloli, S, Morari, M, Novello S., Mercatelli D., Albanese F., Domenicale C., Brugnoli A., D'Aversa E., Vantaggiato S., Dovero S., Murtaj V., Presotto L., Borgatti M., Shimshek D. R., Bezard E., Moresco R. M., Belloli S., Morari M., Novello, S, Mercatelli, D, Albanese, F, Domenicale, C, Brugnoli, A, D'Aversa, E, Vantaggiato, S, Dovero, S, Murtaj, V, Presotto, L, Borgatti, M, Shimshek, D, Bezard, E, Moresco, R, Belloli, S, Morari, M, Novello S., Mercatelli D., Albanese F., Domenicale C., Brugnoli A., D'Aversa E., Vantaggiato S., Dovero S., Murtaj V., Presotto L., Borgatti M., Shimshek D. R., Bezard E., Moresco R. M., Belloli S., and Morari M.
- Abstract
The G2019S mutation of LRRK2 represents a risk factor for idiopathic Parkinson's disease. Here, we investigate whether LRRK2 kinase activity regulates susceptibility to the environmental toxin 1-methyl-4-phenyl-1,2,5,6-tetrahydropyridine (MPTP). G2019S knock-in mice (bearing enhanced kinase activity) showed greater nigro-striatal degeneration compared to LRRK2 knock-out, LRRK2 kinase-dead and wild-type mice following subacute MPTP treatment. LRRK2 kinase inhibitors PF-06447475 and MLi-2, tested under preventive or therapeutic treatments, protected against nigral dopamine cell loss in G2019S knock-in mice. MLi-2 also rescued striatal dopaminergic terminal degeneration in both G2019S knock-in and wild-type mice. Immunoblot analysis of LRRK2 Serine935 phosphorylation levels confirmed target engagement of LRRK2 inhibitors. However, MLi-2 abolished phosphoSerine935 levels in the striatum and midbrain of both wild-type and G2019S knock-in mice whereas PF-06447475 partly reduced phosphoSerine935 levels in the midbrain of both genotypes. In vivo and ex vivo uptake of the 18-kDa translocator protein (TSPO) ligand [18F]-VC701 revealed a similar TSPO binding in MPTP-treated wild-type and G2019S knock-in mice which was consistent with an increased GFAP striatal expression as revealed by Real Time PCR. We conclude that LRRK2 G2019S, likely through enhanced kinase activity, confers greater susceptibility to mitochondrial toxin-induced parkinsonism. LRRK2 kinase inhibitors are neuroprotective in this model.
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- 2022
17. Titan’s surface spectra at the Huygens landing site and Shangri-La
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Rannou, P., Toledo, D., Lavvas, P., D’Aversa, E., Moriconi, M.L., Adriani, A., Le Mouélic, S., Sotin, C., and Brown, R.
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- 2016
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18. Removal of atmospheric features in near infrared spectra by means of principal component analysis and target transformation on Mars: I. Method
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Geminale, A., Grassi, D., Altieri, F., Serventi, G., Carli, C., Carrozzo, F.G., Sgavetti, M., Orosei, R., D’Aversa, E., Bellucci, G., and Frigeri, A.
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- 2015
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19. Martian CO2 Ice Observation at High Spectral Resolution With ExoMars/TGO NOMAD
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Oliva, F., primary, D’Aversa, E., additional, Bellucci, G., additional, Carrozzo, F. G., additional, Ruiz Lozano, L., additional, Altieri, F., additional, Thomas, I. R., additional, Karatekin, O., additional, Cruz Mermy, G., additional, Schmidt, F., additional, Robert, S., additional, Vandaele, A. C., additional, Daerden, F., additional, Ristic, B., additional, Patel, M. R., additional, López‐Moreno, J.‐J., additional, and Sindoni, G., additional
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- 2022
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20. Milliarcsecond Astrometry for the Galilean Moons Using Stellar Occultations
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Morgado, B. E., primary, Gomes-Júnior, A. R., additional, Braga-Ribas, F., additional, Vieira-Martins, R., additional, Desmars, J., additional, Lainey, V., additional, D’aversa, E., additional, Dunham, D., additional, Moore, J., additional, Baillié, K., additional, Herald, D., additional, Assafin, M., additional, Sicardy, B., additional, Aoki, S., additional, Bardecker, J., additional, Barton, J., additional, Blank, T., additional, Bruns, D., additional, Carlson, N., additional, Carlson, R. W., additional, Cobble, K., additional, Dunham, J., additional, Eisfeldt, D., additional, Emilio, M., additional, Jacques, C., additional, Hinse, T. C., additional, Kim, Y., additional, Malacarne, M., additional, Maley, P. D., additional, Maury, A., additional, Meza, E., additional, Oliva, F., additional, Orton, G. S., additional, Pereira, C. L., additional, Person, M., additional, Plainaki, C., additional, Sfair, R., additional, Sindoni, G., additional, Smith, M., additional, Sussenbach, E., additional, Stuart, P., additional, Vrolijk, J., additional, and Winter, O. C., additional
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- 2022
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21. Oxygen airglow emission on Venus and Mars as seen by VIRTIS/VEX and OMEGA/MEX imaging spectrometers
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Migliorini, A., Altieri, F., Zasova, L., Piccioni, G., Bellucci, G., Cardesín Moinelo, A., Drossart, P., D’Aversa, E., Carrozzo, F.G., Gondet, B., and Bibring, J.-P.
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- 2011
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22. Jupiter’s hot spots: Quantitative assessment of the retrieval capabilities of future IR spectro-imagers
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Grassi, D., Adriani, A., Moriconi, M.L., Ignatiev, N.I., D'Aversa, E., Colosimo, F., Negrão, A., Brower, L., Dinelli, B.M., Coradini, A., and Piccioni, G.
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- 2010
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23. FAILURE AS PART OF THE ENTREPRENEURIAL PROCESS. AN EXPLORATORY CONTENT ANALYSIS OF WHAT ENTREPRENEURS SAY ABOUT IT
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Aversa, E., Pisoni, A., and Onetti, A.
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- 2021
24. Regions of interest on Ganymede's and Callisto's surfaces as potential targets for ESA's JUICE mission
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Stephan, Katrin, Roatsch, Thomas, Tosi, F., Matz, K-D, Kersten, Elke, Wagner, Roland, Molyneux, Philippa, Palumbo, P., Poulet, F., Hussmann, H., Barabash, S., Bruzzone, L., Dougherty, Michele K., Gladstone, R., Gurvits, L. I., Hartogh, P., Iess, L., Wahlund, J.-E., Wurz, P, Witasse, O., Grasset, O, Altobelli, N., Carter, J., Cavalie, T., D'Aversa, E., Della Corte, V., Filacchione, G., Galli, A., Galluzzi, V., Gwinner, Klaus, Hauber, Ernst, Jaumann, R., Krohn, Katrin, Langevin, Y., Lucchetti, A, Migliorini, A., Piccioni, G., Solomonidou, A., Stark, Alexander, Tobie, G., Tubiana, C, Vallat, C., Van Hoolst, T., and JUICE, SWT Team
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Ganymede ,Callisto ,JUICE - Published
- 2021
25. What we program is not what we get: Importance of measuring the P-wave sensing offset in DDD pacemakers
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Aversa, E., Chirife, R., Sztyglic, E., Mazzetti, H., Mascheroni, O., and Tentori, M.C.
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- 2011
26. Characterization of Titan's Ontario Lacus region from Cassini/VIMS observations
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Moriconi, M.L., Lunine, J.I., Adriani, A., D'Aversa, E., Negrao, A., Filacchione, G., and Coradini, A.
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Nitriles -- Chemical properties ,Sediments (Geology) -- Chemical properties ,Image processing -- Chemical properties ,Methane -- Chemical properties ,Image processing -- Equipment and supplies ,Image processor ,Astronomy ,Earth sciences - Abstract
To link to full-text access for this article, visit this link: http://dx.doi.org/10.1016/j.icarus.2010.07.023 Byline: M.L. Moriconi (a), J.I. Lunine (b)(e), A. Adriani (b), E. D'Aversa (b), A. Negrao (b)(c), G. Filacchione (d), A. Coradini (b) Keywords: Titan; Satellites, Surfaces; Infrared observations; Image processing Abstract: Liquid hydrocarbons were long predicted on Titan's surface before the RADAR instrument onboard Cassini detected lakes poleward of 70[degrees]N in July 2006. Before that the Cassini Imaging Science Subsystem (ISS) observed a lake-like feature in the South Pole, named Ontario Lacus, in July 2004. Here we analyze one observation of Ontario Lacus taken by the Visual and Infrared Mapping Spectrometer (VIMS) on 2007 December 5, during the T 38 flyby. This is the best spatially resolved image of a Titan lake to date by an imaging spectrometer, and has been previously reported in Brown et al. (Brown, R.H., Soderblom, L.A., Soderblom, J.M., Clark, R.N., Jaumann, R., Barnes, J.W., Sotin, C., Buratti, B., Baines, K.H., Nicholson, P.D. [2008]. Nature 454, 607-610) and in Barnes et al. (Barnes, J.W. et al. [2009]. Icarus 201, 217-225). The observing geometry and our data processing will be explained, followed by a discussion of the main characteristics of the image. The analyzed image covers a small portion of Ontario Lacus and shows what appears from RADAR data to be a region of modest slope ('ramp') adjacent to the dark lake itself. Our analysis of 5.0[mu]m spectral data suggests that the previously reported absorption feature of ethane seen at shorter wavelengths may be produced by damp sediments adjacent to the main liquid basin. The latter appears to be absorbing all of the photons incident upon it in the 5[mu]m spectral region and shows no discernible absorption features. A characterization of the basin composition and morphology is developed with the help of ISS and RADAR observations. The simplest model consistent with the data is an optically deep lake surrounded by a region in which ethane, propane, possibly methane, and other, less volatile hydrocarbons and nitriles are present mixed into spectroscopically neutral sediments. The dominance of relatively low vapor pressure organics outside the lake itself suggests a retreat of Ontario Lacus associated with evaporation on seasonal or longer timescales, consistent with analysis of RADAR and ISS images. Author Affiliation: (a) Institute of Atmospheric Science and Climate-CNR, Via Fosso del Cavaliere 100, I-00133 Rome, Italy (b) IFSI-INAF, Via Fosso del Cavaliere 100, I-00133 Rome, Italy (c) Escola Superior de Tecnologia e Gestao de Leiria, Campus 2, Morro do Lena-Alto do Vieiro, P-2411 Leiria, Portugal (d) IASF-INAF, Via Fosso del Cavaliere 100, I-00133 Rome, Italy (e) Department of Physics, University of Rome Tor Vergata, Via della Ricerca Scientifica 1, 00133 Roma, Italy Article History: Received 15 October 2009; Revised 22 July 2010; Accepted 27 July 2010
- Published
- 2010
27. O.sub.2 1.27[mu]m emission maps as derived from OMEGA/MEx data
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Altieri, F., Zasova, L., D'Aversa, E., Bellucci, G., Carrozzo, F.G., Gondet, B., and Bibring, J.-P.
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Astronomy ,Earth sciences - Abstract
To link to full-text access for this article, visit this link: http://dx.doi.org/10.1016/j.icarus.2009.07.022 Byline: F. Altieri (a), L. Zasova (b), E. D'Aversa (a), G. Bellucci (a), F.G. Carrozzo (a), B. Gondet (c), J.-P. Bibring (c) Keywords: Mars; Atmosphere; Atmosphere; Composition; Spectroscopy Abstract: We present a method to derive the 2D maps of the O.sub.2 (a.sup.1 [DELTA].sub.g) airglow emission at 1.27[mu]m from the OMEGA/MEx nadir observations. The OMEGA imaging capabilities allow monitoring the 2D distribution, daily and seasonal variation of the O.sub.2 emission intensities with a detection limit of 4 MR. The highest values, of the order of [approximately equal to]31 MR, are found on the south pole for 11h Atmospheric waves crossing the terminator on the southern polar regions are observed for the first time during the MY28 early spring. The spatial scale of the waves ranges from 100 to 130km, and the intensity fluctuations are of the order of 4MR. This study confirms the high potentiality of O.sub.2 (a.sup.1 [DELTA].sub.g) day glow as a passive tracer of the martian atmosphere dynamics at high latitudes. Author Affiliation: (a) IFSI - INAF, Via del Fosso del Cavaliere 100, 00133 Rome, Italy (b) Space Research Institute, 84/32 Profsoyuznaya Str., 117997 Moscow, Russia (c) Institut d'Astrophysique Spatiale, BAcentst. 121, Universite Paris-Sud, 91405 Orsay Cedex, France Article History: Received 22 July 2008; Revised 18 June 2009; Accepted 6 July 2009
- Published
- 2009
28. Mapping of water frost and ice at low latitudes on Mars
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Carrozzo, F.G., Bellucci, G., Altieri, F., D'Aversa, E., and Bibring, J.-P.
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Clouds ,Mars (Planet) ,Ice ,Geology ,Astronomy ,Earth sciences - Abstract
To link to full-text access for this article, visit this link: http://dx.doi.org/10.1016/j.icarus.2009.05.020 Byline: F.G. Carrozzo (a), G. Bellucci (a), F. Altieri (a), E. D'Aversa (a), J.-P. Bibring (b) Keywords: Mars; Mineralogy; Ices; Frost; Spectroscopy Abstract: This paper reports on mapping of water frost and ice on Mars, in the range of latitudes between 30[degrees]S and 30[degrees]N. The study has been carried out by analysing 2485 orbits acquired during almost one martian year by the Mars Express/OMEGA imaging spectrometer. Water frost/ice is identified by the presence of [approximately equal to]1.5[mu]m, [approximately equal to]2[mu]m and [approximately equal to]3.0[mu]m absorptions. Although the orbits analysed in this study cover all seasons, water frost/ice is observed only near the aphelion seasons, at Ls=19[degrees] and at Ls=98-150[degrees]. Water frost/ice is detected mainly on the southern hemisphere between 15[degrees]S and 30[degrees]S latitude while it has not been identified within 15[degrees]S-15[degrees]N. In the northern hemisphere, the water frost/ice detection is complicated by the presence of clouds. Usually, water frost/ice is found in shadowed areas, while in few cases it is exposed to the sunlight. This indicates a clear relationship with the local illumination conditions on the slopes which favour the water frost/ice deposition on the surface when the temperatures are very low. OMEGA observations span from 10 to 17LT and the frost/ice is detected mainly between 15 and 16LT, with practically no detection before 13LT. We think this is due to the fact that the 10-12LT observations occur at large distances and it is not a local time effect. A thermal model is used to determine the deposition conditions on the sloped surfaces where water frost/ice has been found. There, daily atmospheric saturation does not occur on pole facing 10-25[degrees] slopes with current water vapour abundances but only by assuming values greater than 40pr[mu]m. Moreover, the water frost/ice is not detected during the northern winter, even if the thermal model foresees daily saturation on 25[degrees] slopes. Author Affiliation: (a) Istituto Nazionale di Astrofisica - Istituto Fisica Spazio Interplanetario (IFSI), Via del Fosso del Cavaliere 100, 00133 Rome, Italy (b) Institut d'Astrophysique Spatiale (IAS), BAcentstiment 121, Universite Paris Sud, 91405 Orsay Cedex, France Article History: Received 12 January 2009; Revised 4 May 2009; Accepted 23 May 2009
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- 2009
29. Analysis of night-side dust activity on comet 67P observed by VIRTIS-M: a new method to constrain the thermal inertia on the surface
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Rinaldi, G., Formisano, M., Kappel, D., Capaccioni, F., Bockelée-Morvan, D., Cheng, Y.-C., Vincent, J.-B., Deshapriya, P., Arnold, G., Capria, M., Ciarniello, M., D’Aversa, E., D'aversa, E, De Sanctis, M., Doose, L., Erard, S., Federico, C., Filacchione, G., Fink, U., Leyrat, C., Longobardo, A., Magni, G., Migliorini, A., Mottola, S., Naletto, G., Raponi, A., Taylor, F., Tosi, F., Tozzi, G., Salatti, M., IASI (IASI), Consiglio Nazionale delle Ricerche (CNR), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Istituto di Astrofisica Spaziale e Fisica cosmica - Roma (IASF-Roma), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institute of Astronomy [Taiwan] (IANCU), National Central University [Taiwan] (NCU), Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique et Mécanique Textiles (LPMT), ENSITM-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Matériaux et nanosciences d'Alsace (FMNGE), Institut de Chimie du CNRS (INC)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), IASF-Roma - Istituto di Astrofisica Spaziale e Fisica cosmica - Roma, Lunar and Planetary Laboratory [Tucson] (LPL), University of Arizona, Instituto de Estudos Avançados (IEAV), Institut, DLR Institute of Planetary Research, German Aerospace Center (DLR), Centro di Ateneo di Studi e Attività Spaziali 'Giuseppe Colombo' (CISAS), Universita degli Studi di Padova, INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto di Fisica dello Spazio Interplanetario (IFSI), Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-ENSITM-Matériaux et Nanosciences Grand-Est (MNGE), Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de la Santé et de la Recherche Médicale (INSERM)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de la Santé et de la Recherche Médicale (INSERM)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Padova = University of Padua (Unipd), and Bockelée-Morvan, Dominique
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Asteroiden und Kometen ,67P/Churyumov-Gerasimenko -infrared ,010504 meteorology & atmospheric sciences ,Comet ,Imaging spectrometer ,Coma (optics) ,Astrophysics ,[SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph] ,01 natural sciences ,general -comets ,Mantle (geology) ,[SDU] Sciences of the Universe [physics] ,comet ,0103 physical sciences ,Thermal ,comets ,individual ,infrared: planetary systems ,010303 astronomy & astrophysics ,planetary systems ,ComputingMilieux_MISCELLANEOUS ,0105 earth and related environmental sciences ,Physics ,[PHYS]Physics [physics] ,Jet (fluid) ,Range (particle radiation) ,[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph] ,comets: general ,Leitungsbereich PF ,comets: individual: 67P/Churyumov-Gerasimenko ,Astronomy and Astrophysics ,Plume ,13. Climate action ,Space and Planetary Science ,[SDU]Sciences of the Universe [physics] ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] - Abstract
On 2015 July 18, near perihelion at a heliocentric distance of 1.28 au, the Visible InfraRed Thermal Imaging Spectrometer (VIRTIS-M) on board the Rosetta spacecraft had the opportunity of observing dust activity in the inner coma with a view of the night side (shadowed side) of comet 67P/Churyumov-Gerasimenko. At the time of the measurements we present here, we observe a dust plume that originates on the far side of the nucleus. We are able to identify the approximate location of its source at the boundary between the Hapi and Anuket regions, and we find that it has been in darkness for some hours before the observation. Assuming that this time span is equal to the conductive time scale, we obtain a thermal inertia in the range 25–36 W K−1 m−2 s−1/2. These thermal inertia values can be used to verify with a 3D finite-element method (FEM) numerical code whether the surface and subsurface temperatures agree with the values found in the literature. We explored three different configurations: (1) a layer of water ice mixed with dust beneath a dust mantle of 5 mm with thermal inertia of 36 J m−2 K−1 s−0.5; (2) the same structure, but with thermal inertia of 100 J m−2 K−1 s−0.5; (3) an ice-dust mixture that is directly exposed. Of these three configurations, the first seems to be the most reasonable, both for the low thermal inertia and for the agreement with the surface and subsurface temperatures that have been found for the comet 67P/Churyumov-Gerasimenko. The spectral properties of the plume show that the visible dust color ranged from 16 ± 4.8%/100 nm to 13 ± 2.6%/100 nm, indicating that this plume has no detectable color gradient. The morphology of the plume can be classified as a narrow jet that has an estimated total ejected mass of between 6 and 19 tons when we assume size distribution indices between −2.5 and −3.
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- 2019
30. Martian CO2 Ice Observation at High Spectral Resolution With ExoMars/TGO NOMAD.
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Oliva, F., D'Aversa, E., Bellucci, G., Carrozzo, F. G., Ruiz Lozano, L., Altieri, F., Thomas, I. R., Karatekin, O., Cruz Mermy, G., Schmidt, F., Robert, S., Vandaele, A. C., Daerden, F., Ristic, B., Patel, M. R., López‐Moreno, J.‐J., and Sindoni, G.
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ICE clouds ,MARTIAN atmosphere ,MARTIAN surface ,TRACE gases ,ICE ,DUST storms - Abstract
The Nadir and Occultation for MArs Discovery (NOMAD) instrument suite aboard ExoMars/Trace Gas Orbiter spacecraft is mainly conceived for the study of minor atmospheric species, but it also offers the opportunity to investigate surface composition and aerosols properties. We investigate the information content of the Limb, Nadir, and Occultation (LNO) infrared channel of NOMAD and demonstrate how spectral orders 169, 189, and 190 can be exploited to detect surface CO2 ice. We study the strong CO2 ice absorption band at 2.7 μm and the shallower band at 2.35 μm taking advantage of observations across Martian Years 34 and 35 (March 2018 to February 2020), straddling a global dust storm. We obtain latitudinal‐seasonal maps for CO2 ice in both polar regions, in overall agreement with predictions by a general climate model and with the Mars Express/OMEGA spectrometer Martian Years 27 and 28 observations. We find that the narrow 2.35 μm absorption band, spectrally well covered by LNO order 189, offers the most promising potential for the retrieval of CO2 ice microphysical properties. Occurrences of CO2 ice spectra are also detected at low latitudes and we discuss about their interpretation as daytime high altitude CO2 ice clouds as opposed to surface frost. We find that the clouds hypothesis is preferable on the basis of surface temperature, local time and grain size considerations, resulting in the first detection of CO2 ice clouds through the study of this spectral range. Through radiative transfer considerations on these detections we find that the 2.35 μm absorption feature of CO2 ice clouds is possibly sensitive to nm‐sized ice grains. Plain Language Summary: The Nadir and Occultation for MArs Discovery (NOMAD) instrument aboard the ExoMars/Trace Gas Orbiter spacecraft is conceived for the study of non‐abundant gaseous species in the atmosphere of Mars. Nevertheless, we investigate its capability to observe the Martian surface, suspended dust and CO2 ice clouds. We verify that part of the signal registered by the instrument contains information on the presence of CO2 ice on the surface of Mars. We produce maps that predict the seasonal condensation/sublimation of the ice that are in general good agreement with a Mars climate model and with observations acquired by the OMEGA instrument aboard the Mars Express spacecraft. The data we study also observed a dust storm that globally enveloped the planet in 2018, allowing us to deduce that the dust in the atmosphere strongly affects the capability to detect the ice on the surface. Finally, we also find that some observations are compatible with CO2 ice clouds made of extremely small crystals (dimensions of some millionths of millimeters) that have never been observed by studying such specific part of the signal registered by NOMAD. Key Points: Martian surface CO2 ice detection at high spectral resolution with Trace Gas Orbiter/Nadir and Occultation for MArs DiscoveryGeneral good agreement of the seasonal surface CO2 ice maps with Mars Express/OMEGA observations and with Mars Climate Database predictionsCO2 ice clouds detection through the 2.35 micron CO2 ice absorption band, likely sensitive to a population of nm‐sized ice grains [ABSTRACT FROM AUTHOR]
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- 2022
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31. Saturn's icy satellites investigated by Cassini-VIMS I. Full-disk properties: 350-5100 nm reflectance spectra and phase curves
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Filacchione, G., Capaccioni, F., McCord, T.B., Coradini, A., Cerroni, P., Bellucci, G., Tosi, F., D'Aversa, E., Formisano, V., Brown, R.H., Baines, K.H., Bibring, J.P., Buratti, B.J., Clark, R.N., Combes, M., Cruikshank, D.P., Drossart, P., Jaumann, R., Langevin, Y., Matson, D.L., Mennella, V., Nelson, R.M., Nicholson, P.D., Sicardy, B., Sotin, C., Hansen, G., Hibbitts, K., Showalter, M., and Newman, S.
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Cassini (Space probe) -- Observations ,Satellites -- Observations ,Saturn (Planet) -- Observations ,Astronomy ,Earth sciences - Abstract
Saturn's icy satellites are among the main scientific objectives of the Cassini-VIMS (Visual and Infrared Mapping Spectrometer) experiment. This paper contains a first systematic and comparative analysis of the full-disk spectral properties of Dione, Enceladus, Epimetheus, Hyperion, Iapetus, Mimas, Phoebe, Rhea and Tethys as observed by VIMS from July 2004 to June 2005. The disk integrated properties (350-5100 nm reflectance spectra and phase curves at 550-2232 nm) and images of satellites are reported and discussed in detail together with the observed geometry. In general, the spectra in the visible spectral range are almost featureless and can be classified according to the spectral slopes: from the bluish Enceladus and Phoebe to the redder Iapetus, Hyperion and Epimetheus. In the 1000-1300 nm range the spectra of Enceladus, Tethys, Mimas and Rhea are characterized by a negative slope, consistent with a surface largely dominated by water ice, while the spectra of Iapetus, Hyperion and Phoebe show a considerable reddening pointing out the relevant role played by darkening materials present on the surface. In between these two classes are Dione and Epimetheus, which have a fiat spectrum in this range. The main absorption bands identified in the infrared are the 1520, 2020, 3000 nm [H.sub.2]O/OH bands (for all satellites), although Iapetus dark terrains show mostly a deep 3000 nm band while the 1520 and 2020 nm bands are very faint. In this spectral range, the Iapetus spectrum is characterized by a strong reddening. The C[O.sub.2] band at 4260 nm and the Fresnel ice peak around 3100 nm are evident only on Hyperion, Phoebe and Iapetus. The phase curves at 550 and at 2232 nm are reported for all the available observations in the 0[degrees]-144[degrees] range; Rhea shows an opposition surge at visible wavelengths in the 0.5[degrees]-1.17[degrees] interval. The improvement on the retrieval of the full-disk reflectance spectra can be appreciated by a direct comparison with ground-based telescopic data available from literature. Finally, data processing strategies and recent upgrades introduced in the VIMS-V calibration pipeline (flat-field and destriping-despiking algorithm) are discussed in appendices. Keywords: Saturn, satellites; Spectroscopy; Infrared observations; Image processing
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- 2007
32. TITAN’S GROUND REFLECTANCE RETRIEVAL FROM CASSINI-VIMS DATA TAKEN DURING THE JULY 2ND, 2004 FLY-BY AT 2 AM UT
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Adriani, A., Moriconi, M. L., Liberti, G. L., Gardini, A., Orosei, R., D’Aversa, E., Filacchione, G., and Coradini, A.
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- 2005
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33. Observations of non-LTE emission at 4-5 microns with the planetary Fourier spectrometer abord the Mars Express mission
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Formisano, V., Maturilli, A., Giuranna, M., D'Aversa, E., and Lopez-Valverde, M.A.
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Astronomy ,Earth sciences - Abstract
To link to full-text access for this article, visit this link: http://dx.doi.org/10.1016/j.icarus.2005.12.022 Byline: V. Formisano (a), A. Maturilli (a), M. Giuranna (a), E. D'Aversa (a), M.A. Lopez-Valverde (b) Keywords: Mars; Mars; atmosphere; Atmospheres; composition Abstract: We report on PFS-MEX (Planetary Fourier Spectrometer on board Mars Express) limb observations of the non-Local Thermodynamic Equilibrium emission by CO and CO.sub.2 isotopic molecules. The CO emission is observed peaking at altitudes lower than the CO.sub.2 emission peak. Two orbits have been considered, which explore latitudes from 75 to 15[degrees] N, located in local time at 11:30 and 06:40, and with L.sub.s=138[degrees] and 168[degrees], respectively. In general in the season considered (northern summer) the emission intensity increases going to lower latitudes. The peak emission height is also decreasing with decreasing latitude. The CO.sub.2 isotopic molecules are emitting radiance out of proportion with respect to the normal isotopic abundance, which surely indicates a strong contribution from a large number of much weaker CO.sub.2 bands, a result that will demand careful theoretical modeling. By comparison with Hitran data base we can identify, among the emitting bands, the second hot band for the 626 and 636 molecule, while for the 628 and 627 emission from the third hot bands are very possible. Other minor bands or lines are also observed in emission for the first time in Mars. In one of the two orbits considered, the orbit 1234 of MEX, we also observe at altitudes 80-85 km scattered radiation, with indication of CO.sub.2 ice aerosols as scattering centers. At the same altitude the Pathfinder descending measurements show a temperature that allows CO.sub.2 condensation. Pathfinder measurements were at 03:00 local time, while our observations are for orbit 1234 showing CO.sub.2 ice signature at 11:30 local time. These non-LTE limb emissions, with their unprecedented spectral resolution in this portion of the near infrared and their sensitivity and geographical coverage, will represent in our opinion an excellent data set for testing current theoretical models of the martian upper atmosphere. Author Affiliation: (a) Istituto di Fisica dello Spazio Interplanetario IFSI-INAF, Via del Fosso del Cavaliere 100, 00113 Roma, Italy (b) Instituto de Astrofisica de Andalucia (CSIC), Apdo. 3004, 18080 Granada, Spain Article History: Received 23 May 2005; Revised 20 December 2005
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- 2006
34. Cassini/VIMS observation of an Io post-eclipse brightening event
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Bellucci, G., D'Aversa, E., Formisano, V., Cruikshank, D., Nelson, R.M., Clark, R.N., Baines, K.H., Matson, D., Brown, R.H., McCord, T.B., Buratti, B.J., and Nicholson, P.D.
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Cassini (Space probe) -- Observations ,Satellites -- Observations ,Infrared astronomy ,Astronomy ,Earth sciences - Abstract
During the Cassini-Jupiter flyby, VIMS observed Io at different phase angles, both in full sunlight and in eclipse. By using the sunlight measurements, we were able to produce phase curves in the visual through all the near infrared wavelengths covered by the VIMS instrument (0.85-5.1 [micro]m). The phase angle spanned from ~2[degrees] to ~120[degrees]. The measurements, done just after Io emerged from Jupiter's shadow, show an increase of about 15% in Io's reflectance with respect to what would be predicted by the phase curve. This behavior is observed at wavelengths > 1.2 [micro]m. Moreover, just after emergence from eclipse an increase of about 25% is observed in the depth of S[O.sub.2] frost bands at 4.07 and 4.35 [micro]m. At 0.879 < [lambda] < 1.04 [micro]m the brightening is 10-24%. Below [lambda] = 0.879 [micro]m the brightening, if present, should be less than the precision of our measurements (~5%). Apparently, these observations are not explained neither by a diverse spatial distribution of S[O.sub.2] on the Io' surface nor by atmospheric S[O.sub.2] condensation on the surface during the eclipse. Keywords: Io; Atmosphere; Infrared observations: Satellites of Jupiter
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- 2004
35. Cassini'-VIMS at Jupiter: solar occultation measurements using Io
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Formisano, V, D'Aversa, E., Bellucci, G., Baines, K.H., Bibring, J.P., Brown, R.H., Buratti, B.J., Capaccioni, F., Cerroni, P., Clark, R.N., Coradini, A., Cruikshank, D.P., Drossart, P., Jaumann, R., Langevin, Y., Matson, D.L., McCord, T.B., Mennella, V., Nelson, R.M., Nicholson, P.D., Sicardy, B., Sotin, C., Chamberlain, M.C., Hansen, G., Hibbits, K., Showalter, M., and Filacchione, G.
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Jupiter (Planet) -- Research ,Astronomy ,Earth sciences - Abstract
We report unusual and somewhat unexpected observations of the jovian satellite Io, showing strong methane absorption bands. These observations were made by the Cassini VIMS experiment during the Jupiter flyby of December/January 2000/2001. The explanation is straightforward: Entering or exiting from Jupiter's shadow during an eclipse, Io is illuminated by solar light which has transited the atmosphere of Jupiter. This light, therefore becomes imprinted with the spectral signature of Jupiter's upper atmosphere, which includes strong atmospheric methane absorption bands. Intercepting solar light refracted by the jovian atmosphere, Io essentially becomes a 'mirror' for solar occultation events of Jupiter. The thickness of the layer where refracted solar light is observed is so large (more than 3000 km at Io's orbit), that we can foresee a nearly continuous multi-year period of similar events at Saturn, utilizing the large and bright ring system. During Cassini's 4-year nominal mission, this probing technique should reveal information of Saturn's atmosphere over a large range of southern latitudes and times. Keywords: Occultations; Jupiter; Infrared observations
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- 2003
36. Composition of Titan's surface from Cassini VIMS
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McCord, T.B., Hansen, G.B., Buratti, B.J., Clark, R.N., Cruikshank, D.P., D’Aversa, E., Griffith, C.A., Baines, E.K.H., Brown, R.H., Dalle Ore, C.M., Filacchione, G., Formisano, V., Hibbitts, C.A., Jaumann, R., Lunine, J.I., Nelson, R.M., and Sotin, C.
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- 2006
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37. Large Abundances of Polycyclic Aromatic Hydrocarbons in Titan's Upper Atmosphere
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Lopez-Puertas, M, Dinelli, B. M, Adriani, A, Funke, B, Garcia-Comas, M, Moriconi, M. L, D'Aversa, E, Boersma, C, and Allamandola, L. J
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Lunar And Planetary Science And Exploration - Abstract
In this paper, we analyze the strong unidentified emission near 3.28 micron in Titan's upper daytime atmosphere recently discovered by Dinelli et al.We have studied it by using the NASA Ames PAH IR Spectroscopic Database. The polycyclic aromatic hydrocarbons (PAHs), after absorbing UV solar radiation, are able to emit strongly near 3.3 micron. By using current models for the redistribution of the absorbed UV energy, we have explained the observed spectral feature and have derived the vertical distribution of PAH abundances in Titan's upper atmosphere. PAHs have been found to be present in large concentrations, about (2-3) × 10(exp 4) particles / cubic cm. The identified PAHs have 9-96 carbons, with a concentration-weighted average of 34 carbons. The mean mass is approx 430 u; the mean area is about 0.53 sq. nm; they are formed by 10-11 rings on average, and about one-third of them contain nitrogen atoms. Recently, benzene together with light aromatic species as well as small concentrations of heavy positive and negative ions have been detected in Titan's upper atmosphere. We suggest that the large concentrations of PAHs found here are the neutral counterpart of those positive and negative ions, which hence supports the theory that the origin of Titan main haze layer is located in the upper atmosphere.
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- 2013
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38. Photometric modelling and VIS-IR albedo maps of Rhea from Cassini-VIMS
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Filacchione, G, primary, Ciarniello, M, additional, D’Aversa, E, additional, Capaccioni, F, additional, Cerroni, P, additional, Buratti, B J, additional, Clark, R N, additional, Stephan, K, additional, and Plainaki, C, additional
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- 2020
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39. Dust composition in the innermost coma of comet 67P from the VIRTIS-M spectra: Organic features detection
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Rinaldi, G., D'Aversa, E., Bockelee-Morvan, D., Raponi, A, Capaccioni, F., Ciarniello, M., Filacchione, G., De Sanctis, M. C., Oliva, F., Kappel, David, Longobardo, A, Tosi, F., Capria, M., and Taylor, F.
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Asteroiden und Kometen ,Rosetta ,Comet 67P ,Dust ,VIRTIS - Abstract
The Rosetta/ESA spacecraft followed the comet 67P/Churyumov-Gerasimenko from 2014 August (3.6 au pre-perihelion) to 2016 September (3.6 au post-perihelion). This offered a unique opportunity to analyze the time evolution of the dust properties in the inner coma. Onboard Rosetta, the Visual Infrared and Thermal Imaging Spectrometer (VIRTIS-M) acquired spectra of the dust coma in the spectral range 0.25 to 5 μm.
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- 2019
40. Detection of Crystalline and Fine-grained Calcic Plagioclases on Vesta
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Palomba, E., D'Aversa, E., Longobardo, A., Dirri, F., Orton, G., Sindoni, G., Oliva, F., Carrozzo, G., Sato, Takao M., Aoki, Shohei, and Kasaba, Yasumasa
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Physics ,Solar System ,Infrared astronomy ,010504 meteorology & atmospheric sciences ,Astronomy and Astrophysics ,engineering.material ,01 natural sciences ,Regolith ,Astrobiology ,Meteorite ,Space and Planetary Science ,Asteroid ,Absorption band ,0103 physical sciences ,engineering ,Plagioclase ,010303 astronomy & astrophysics ,Achondrite ,0105 earth and related environmental sciences - Abstract
著者人数: 11名, Accepted: 2019-06-26, 資料番号: SA1190057000
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- 2019
41. Water Vapor Vertical Profiles on Mars in Dust Storms Observed by TGO/NOMAD
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Aoki, Shohei, Vandaele, Ann Carine, Daerden, Frank, Villanueva, Geronimo L., Liuzzi, Giuliano, Thomas, Ian R., Erwin, Justin T., Trompet, L., Robert, S., Neary, L., Viscardy, S., Ristic, Bojan, Patel, Manish R., Bellucci, Giancarlo, Bauduin, S., López-Moreno, José Juan, Alonso-Rodrigo, G., Fussen, D., Bolsée, D., Carrozzo, G., Clancy, R. Todd, Cloutis, E., Crismani, M., Da Pieve, F., D'Aversa, E., Kaminski, J., Depiesse, C., Garcia-Comas, M., Etiope, G., Fedorova, A.A., Funke, Bernd, Geminale, A., Gérard, Jean-Claude, Giuranna, M., Karatekin, O., Gkouvelis, L., González-Galindo, F., Holmes, J., Hubert, B., Mumma, M.J., Ignatiev, N.I., Kasaba, Y., Kass, D., Kleinböhl, A., Lanciano, O., Lefèvre, F., Lewis, S., López-Puertas, M., Schneider, Nicholas, Nakagawa, H., Hidalgo López, Ana, Mahieux, A., Mason, J., Mege, D., Neefs, E., Novak, R.E., Oliva, F., Sindoni, G., Piccialli, A., Renotte, E., Ritter, B., Willame, Y., Schmidt, F., Smith, M.D., Teanby, N.A., Thiemann, E., Trokhimovskiy, A., Auwera, J.V., Wolff, M.J., Clairquin, R., Whiteway, J., Wilquet, V., Wolkenberg, P., Yelle, R., del Moral Beatriz, A., Barzin, P., Beeckman, B., Cubas, J., BenMoussa, A., Berkenbosch, S., Orban, A., Biondi, D., Bonnewijn, S., Candini, G.P., Giordanengo, B., Gissot, S., Gomez, A., Hathi, B., Zafra, J.J., Leese, M., Maes, J., Pastor-Morales, M., Mazy, E., Mazzoli, A., Meseguer, J., Morales, R., Perez-grande, I., Queirolo, C., Ristic, R., Gomez, J.R., Saggin, B., Samain, V., Sanz Andres, A., Altieri, F., Sanz, R., Simar, J.-F., Thibert, T., the NOMAD team, López-Valverde, M. A., Hill, Brittany, Belgian Science Policy Office, European Space Agency, Ministerio de Ciencia e Innovación (España), European Commission, UK Space Agency, Agenzia Spaziale Italiana, Ministerio de Ciencia, Innovación y Universidades (España), Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles), National Aeronautics and Space Administration (US), and Canadian Space Agency
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010504 meteorology & atmospheric sciences ,Storm ,Atmosphere of Mars ,Mars Exploration Program ,Atmospheric sciences ,01 natural sciences ,Trace gas ,Atmosphere ,Geophysics ,Space and Planetary Science ,Geochemistry and Petrology ,Dust storm ,Earth and Planetary Sciences (miscellaneous) ,Environmental science ,Hadley cell ,Water vapor ,0105 earth and related environmental sciences - Abstract
It has been suggested that dust storms efficiently transport water vapor from the near-surface to the middle atmosphere on Mars. Knowledge of the water vapor vertical profile during dust storms is important to understand water escape. During Martian Year 34, two dust storms occurred on Mars: a global dust storm (June to mid-September 2018) and a regional storm (January 2019). Here we present water vapor vertical profiles in the periods of the two dust storms (Ls = 162–260° and Ls = 298–345°) from the solar occultation measurements by Nadir and Occultation for Mars Discovery (NOMAD) onboard ExoMars Trace Gas Orbiter (TGO). We show a significant increase of water vapor abundance in the middle atmosphere (40–100 km) during the global dust storm. The water enhancement rapidly occurs following the onset of the storm (Ls~190°) and has a peak at the most active period (Ls~200°). Water vapor reaches very high altitudes (up to 100 km) with a volume mixing ratio of ~50 ppm. The water vapor abundance in the middle atmosphere shows high values consistently at 60°S-60°N at the growth phase of the dust storm (Ls = 195°–220°), and peaks at latitudes greater than 60°S at the decay phase (Ls = 220°–260°). This is explained by the seasonal change of meridional circulation: from equinoctial Hadley circulation (two cells) to the solstitial one (a single pole-to-pole cell). We also find a conspicuous increase of water vapor density in the middle atmosphere at the period of the regional dust storm (Ls = 322–327°), in particular at latitudes greater than 60°S. ©2019. American Geophysical Union. All Rights Reserved., S. A. is >Charge de Recherches> of the F.R.S.-FNRS. ExoMars is a space mission of the European Space Agency and Roscosmos. The NOMAD experiment is led by the Royal Belgian Institute for Space Aeronomy (IASBBIRA), assisted by Co-PI teams from Spain (IAA-CSIC), Italy (INAF-IAPS), and the United Kingdom (Open University). This project acknowledges funding by the Belgian Science Policy Office, with the financial and contractual coordination by the European Space Agency Prodex Office (PEA 4000103401 and 4000121493), by the Spanish MICINN through its Plan Nacional and by European funds under grants PGC2018-101836-B-I00 and ESP2017-87143-R (MINECO/FEDER), as well as by UK Space Agency through grants ST/R005761/1, ST/P001262/1, ST/R001405/1, and ST/S00145X/1 and Italian Space Agency through grant 2018-2-HH.0. The IAA/CSIC team acknowledges financial support from the State Agency for Research of the Spanish MCIU through the >Center of Excellence Severo Ochoa> award for the Instituto de Astrofisica de Andalucia (SEV-2017-0709). This work was supported by the Belgian Fonds de la Recherche Scientifique-FNRS under grant numbers 30442502 (ET_HOME) and T.0171.16 (CRAMIC) and Belgian Science Policy Office BrainBe SCOOP Project. U.S. investigators were supported by the National Aeronautics and Space Administration. Canadian investigators were supported by the Canadian Space Agency. The results retrieved from the NOMAD measurements used in this article are available on the BIRA-IASB data repository: http://repository.aeronomie.be/?doi= 10.18758/71021054 (Aoki et al., 2019).
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- 2019
42. VIS-IR Albedo and Spectral Indicators Maps of Saturn’s Icy Satellites Surfaces by Cassini/VIMS
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Filacchione, G., Ciarniello, Mauro, D’Aversa, E., Capaccioni, F., Cerroni, P., Buratti, B, Clark, R., Stephan, Katrin, Lunine, J., and Plainaki, C.
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Planetengeologie ,Eismonde - Published
- 2019
43. Experimental Tests Results of Traspiration Cooling Subscale Injector Head in the frame of LYRA Program
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TERRACCIANO, A., GELAIN, R., BIANCHI, G., LIUZZI, D., SCARPINO, D., RUDNYKH, M., DRIGO, D., ARIONE, L., PELLEGRINI, R., and D'AVERSA, E.
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SPACE PROPULSION ,COMBUSTION CHAMBERS ,CRYOGENIC PROPULSION ,ADDITIVE MANUFACTURING - Abstract
In the frame of the LYRA Program, funded by the Italian Space Agency, the LM-10-MIRA engine has been successfully tested. The engine has a vacuum thrust of 10-tons and has been developed by a joint Avio-KBKhA propulsion team in the frame of a dedicated ASI-Roscosmos inter-agencies agreement. After the experimental test campaign, further improvement for flight application have been identified, including the improvement of the efficiency and new technologies for of injector head manufacturing. The `lesson learned\' allowed ASI to promote further activities in collaboration with Avio. In particular, two main activities have been developed, the first one aimed to reduce the methane line pressure drop and the second one related to the optimization of the methane/oxygen interfaces. The results have been implemented on a subscale version of the injector head. The present work describes the improvements obtained and confirmed by the results of the subscale experimental test campaign.
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- 2019
- Full Text
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44. Observing regions of interest on Ganymede and Callisto with JUICE
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Tosi, F., Stephan, Katrin, Palumbo, P., Piccioni, G., Langevin, Y., Altieri, F., Carter, J., Cremonese, G., D’Aversa, E., Della Corte, V., Filacchione, G., Galuzzi, V., Lucchetti, A., Massironi, M., Migliorini, A., Poulet, F., and Roatsch, Thomas
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Planetengeologie ,JUICE - Published
- 2019
45. Fourth meeting of the European Neurological Society 25–29 June 1994 Barcelona, Spain: Abstracts of Symposia and free communications
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Harms, L., Bock, A., JÄnisch, W., Valdueza, J., Weber, J., Link, I., De Keyser, J., Goossens, A., Wilczak, N., Vedeler, C., Bjorge, L., Uvestad, E., Conti, G., Williams, K., Ginsberg, L., Rafique, S., Rapoport, S. I., Gershfeld, N. L., De La Meilleure, G., Crevits, L., Faiss, J. H., Heye, N., Blanke, J., Sackmann, A., Kastrup, O., Doornbos, R., van der Worp, H. B., Kappelle, L. J., Bar, P. R., Davie, C. A., Barker, G. J., Brenton, D., Miller, D. H., Thompson, A. J., Block, F., Schwarz, M., Delodovici, L., Baruzzi, F., Bonaldi, G., Dario, A., Marra, A., Mercuri, A., Dworzak, F., Cavallari, P., Confalonieri, P., Zuffi, M., Antozzi, C., Cornelio, F., Baldissera, F., Chassande, B., Ameri, A., Eymard, B., Poisson, M., Vérier, A., Brunet, P., Congia, S., Murgia, P. L., Cannas, A., Borghero, G., Uselli, S., Mellino, G., Ferrai, R., Lampis, R., Massa, R., Muzzetto, B., Giannini, F., Rossi, S., Cioni, R., d'Aniello, C., Guarneri, A., Battistini, N., Ceriani, F., Del Santo, A., Poloni, M., Campo, J. F., Iglesias, F., Guitera, M. V., Farinas, C., Pascual, J., Leno, C., Berciano, J., Thorpe, I. W., Kendall, B. E., McDonald, W. I., Moulignier, A., Dromer, F., Baudrimont, M., Dupont, B., Gozlan, J., El Amrani, M., Petit, J. C., Roullet, E., Sterzi, R., Causaran, R., Protti, A., Riva, M., Erminio, F., Arena, O., Villa, F., Maccagnano, E., Miletta, M., Spinelli, F., Ben-Hur, T., Weidenfeldl, J., Rao, N. S., Chari, C. C., Laforet, P., Matheron, S., Adams, D., Chemouilli, Ph., Desi, M., Said, G., Davous, P., Lionnet, F., Pulik, M., Genet, P., Rozenberg, F., Cartier, L. M., Castillo, J. L., Cea, J. G., Villagra, R., de Saint Martin, L., Mahieux, F., Manifacier, M. J., Mattos, K., Queiros, C., Publio, L., Vinhas, V., PeÇanha-Martins, A. C., Melo, A., Liska, U., Zifko, U., Budka, H., Drlicek, M., Grisold, W., Kaufmann, R., Kaiser, R., Czygan, M., Gomes, I., Jones, N., Cunha, S., EmbiruÇu, E. Katiane, Vieira, V., Araujo, I., Alexandra, M., Ferreira, A., Goes, J., Chemouilli, P., Israel-Biet, Masson, H., Lacroix, C., Gasnault, J., Hildebrandt-Müller, B., Oschmann, P., Krack, P., Willems, W. R., Dorndorf, W., Freitas, V., Bittencourt, A., Fernandes, D., Nascimento, M. H., Severo, M., Moraes, D., Muller, M., Hasert, K., Merkelbach, S., Schimrigk, K., van Oosten, B. W., Lai, M., Polman, C. H., Bertelsmann, F. W., Hodgkinson, S., Cabre, P. H., Volpe, L., Smadja, D., Vernant, J. P., Villaroya, H., Violleau, K., Younes-Chennoufi, A. Ben, Baumann, N., Villanueva-Hemandez, P., Ballabriga, J., Basart, E., Arbizu, T. X., Perez-Serra, J., Vinuels, F., Giron, J. M., Castilla, J. M., Redondo, L., Izquierdo, G., Lauer, K., Henneberg, A., Bittmann, N., Link, D., Wollinsky, K. H., Mobner, R., Fassbender, K., Kuhnen, J., Schwartz, A., Hennerici, M., Miller, A., Lider, O., Abramsky, O., Weiner, H. L., Offner, H., Vanderbark, A. A., Paoino, E., Fainardi, E., Addonizio, M. C., Ruppi, P., Tola, M. R., Granieri, E., Carreras, M., Sazdovitch, V., Joutel, A., Verdier-taillefer, M. H., Heinzlef, O., Radder, C., Tournier-Lasserve, E., Brenner, R. E., Munro, P. M. G., Williams, S. C. R., Bell, J. D., Hawkins, C. P., Filippi, M., Campi, A., Dousset, V., Canal, N., Comi, G., Zhu, J., Weber, F., Retska, R., List, J., Zhang, L., Brock, M., Taphoorn, M. J. B., Heimans, J. J., van der Veen, E. A., Karim, A. B. M. F., Sarazin, M., Argentino, N., Delattre, J. Y., Derkinderen, P., Buchwald, B., Schroter, G., Serve, G., Franke, C. H., Conrad, B., Kitchen, N. D., Thomas, D. G. T., Forman, A. D., Ang, Kie- Kian, Price, R., Stephens, C., Salmaggi, A., Nermni, R., Silvani, A., Forno, M. G., Luksch, R., Boiardi, A., Grzelec, H., Fryze, C., Nowacki, P., Zdziarska, B., Sanson, M., Merel, P., Richard, S., Rouleau, G., Thomas, G., Olsen, N. K., Pfeiffer, P., Egund, N., Bentzen, S. M., Johannesen, L., Mondrup, K., Rose, C., Zyluk, B., Wondrusch, E., Berger, O., Fast, N., Jellinger, K., Lindner, K., Urman, A., Thibault, J. L., Duyckaerts, Ch., Strik, H., Muller, B., Richter, E., Krauseneck, P., Steinbrecher, A., Schabet, M., Hess, C., Bamberg, M., Dichgans, J., Counsell, C. E., McLeod, M., Grant, R., Creel, G. B., Claus, D., Sieber, E., Engelhardt, A., Rechlin, T., Thierauf, P., Neubauer, U., Peresson, M., Di Giovacchino, G., Romani, G. L., Di Silverio, F., Danek, A., Kuffner, M., Hoermann, R., Schopohl, J., Laska, M., Heye, B., Zangaladze, A. T., Valls-SoIè, J., Cammarota, A., Alvarez, R., Tolosa, E., Hallett, M., Ulbricht, D., Ganslandt, O., Kober, H., Vieth, J., Grummich, P., Pongratz, H., Brigel, C., Fahlbusch, R., Serra, F. P., Palma, V., Nolfe, G., Buscaino, G. A., Rothstein, T. L., Gibson J. M., Morrison P. M., Collins A. D., Eiselt, M., Wagnur, H., Zwiener, U., Schindler, T., Efendi, H., Ertekin, C., Erfas, M., Larsson, L. E., Sirin, H., AraÇ, N., Toygar, A., Demir, Y., Seddigh, S., Vogt, T. H., Hundemer, H., Visbeck, A., Pastena, L., Faralli, F., Mainardi, G., Gagliardi, R., Linden, D., Berlit, P., Lopez, O. L., Becker, J. T., Jungreis, C., Brenner, R., Rezek, D., Dekesky, S. T., Estol, C., Boller, F., Fernandez, J. M., Mederer, S., Batlle, J., Turon, A., Codina, A., Hitzenberger, P., Vila, N., Valls-SolÇ, J., Chamorro, A., Pouget, J., Schmied, A., Morin, D., Azulay, J. Ph., Vedel, J. P., Montalt, J., Escudero, J., Barona, R., Campos, A., Varli, K., Ertem, E., Uludag, B., Yagiz, A., Privorkin, Z., Steinvil, Y., Kott, E., Combarros, O., Sanchez-Pernaute, R., Orizaola, P., Mokrusch, Th., Kutluaye, E., Selcuki, D., Ertikin, C., Zettl, U., Gold, R., Harvey, G. K., Hartung, H. P., Toyka, K. V., Wokke, J. H. J., Oey, P. L., Ippel, P. F., Jansen, G. H., Franssen, H., Toyooka, K., Fujimura, H., Ueno, S., Yoshikawa, H., Yorifuji, S., Yanagihara, T., Talamon, C., Tzourio, C., Kiefer, R., Jung, S., Toyka, K., Ruolt, I., Tranchant, C., Mohr, M., Warter, J. M., Younger, D. S., Rosoklija, G., Hays, A. P., Kurita, R., Hasegawa, O., Matsumto, M., Komiyama, A., Nara, Y., Oueslati, S., Belal, S., Turki, I., Ben Hamida, C., Hentati, F., Ben Hamida, M., Kwiecinski, H., Krolicki, L., Domzal-Stryga, A., Dellemijn, P. L. I., van Deventer, P., van Moll, B., Drogendijk, T., Vecht, Ch. J., Nemni S., Amadio, Fazio, R., Galardin, G., Delodovici, M. L., Peghi, E., Monticelli, M. L., Sessa, A., Viguera, M. L., Palomar, M., Gamez, J., Cervera, C., Navarro, C., Serena, J., Duran, I., Fernandez, A. L., Comabella, M., Nos, C., Rio, J., Montalban, J., Navarro, X., Verdu, E., Darbra, S., Buti, M., Mrabet, A., Fredj, M., Gouider, R., Tounsi, H., Khalfallah, N., Haddad, A., Dbaiss, T., Ghnassia, R., Rouillet, E., Chedru, F., Porsche, H., Strenge, H., Li, S. W., Young, Y. P., Garcia, A. A., Baron, P., Scarpini, E., Bianchi, R., Conti, A., Livraghi, S., Rees, J. H., Gregson, N. A., Hughes, R. A. C., Sedano, M. J., Calleja, J., Canga, E., Bahou, Y., Biary, N., Al Deeb, S. M., Guern, E. L. E., Gugenheim, M., Tardieu, S., Aisonobe, T. M., Agid, Y., Bouche, P., Brice, A., Rautenstrauss, B., Nelis, E., Grehl, H., Van Broeckhoven, C., Pfeiffer, R. A., Liehr, T., Ganzmann, E., Gehring, C., Neundörfer, B., Geremia, L., Doronzo, R., Sacilotto, G., Sergi, P., Pastorino, G. C., Scarlato, G., Planté-Bordeneuve, V., Mantel, A., Baas, F., Moser, H., Antonini, A., Psylla, M., Günther, I., Vontobell, P., Beer, H. F., Leenders, K. L., Chaudhuri, K. Ray, Parker, J., Pye, I. F., Millac, P. A. H., Abbott, R. J., Sutter, M., Albani, C., de Rijk, M. C., Breteler, M. M. B., Graveland, G. A., van der Mechè, F. G. A., Hofman, A., Keipes, M., Hilger, Ch., Diederich, N., Metz, H., Hentges, F., Pollak, P., Benabid, A. L., Limousin, P., Hoffmann, D., Benazzouz, A., Perret, J., Laihinen, A., Rinne, J. O., Ruottinen, H., Nagren, K., Lehikoinen, P., Oikonen, V., Ruotsalainen, U., Rinne, U. K., Cocozza, S., Pizzuti, A., Cavalcanti, F., Monticelli, A., Pianese, L., Redolfi, E., Paiau, F., Di Donato, S., Pandolfo, M., Palau, F., Monros, E., De Michele, G., Smeyers, P., Lopez-ArLandis, J., Uilchez, J., Filla, A., Genis, D., Matilla, T., Volpini, V., Blanchs, M. I., Davalos, A., Molins, A., Rosell, J., Estivill, X., De Jonghe, P., Smeyers, G., Krols, L., Mercelis, R., Hazan, J., Weissenbach, J., Martin, J. J., Warner, T. A. T., Williams, L., Orb, A. S., Harding, A. E., Giunti, P., Sweeney, M. G., Spadaro, M., Jodice, C., Novelletto, A., Malaspina, P., Frontali, M., Salmon, E., Gregoire, Del Fiore, Comar, Franck, G., Scheltens, P. H., Siegfried, K., Dartigues, E., De Deyn, P., Horn, R., Nelson, I., Hanna, M. G., Morgan-Hughes, J. A., Collinge, J., Palmer, M. S., Campbell, T., Mahal, S., Sidle, K., Humphreys, C., Tavitian, B., Pappata, S., Jobert, A., Crouzel, A. M., DiGiamberardino, L., Steimetz, G., Barbanti, P., Fabbrini, G., Salvatore, M., Buzzi, M. G., Di Piero, V., Petraroli, R., Sbriccoli, A., Pocchiari, M., Macchi, G., Lenzi, G. L., Spiegel, R., Maguire, P., Schmid, W., Ott, A., Bots, M. L., Grobbe, D. E., Hofman, A., Howard, R. S., Russell, S., Losseff, N., Hirsch, N. P., Couderc, R., Bailleul, S., Nargeot, M. C., Touchon, J., Picot, M. C., Rizzo, M., Watson, G., McGehee, D., Dingus, T., Kappos, L., Radü, E. W., Haas, J., Hartard, C. H., Spuler, S., Yousry, T., Voltz, R., Scheller, A., Holler, E., Hohlfeld, R., Scolding, N. J., Sussman, J., Kolar, O. J., Farlow, M. R., Rice, P. H., Zipp, F., Sotgiu, S., Weiss, E. H., Wekerle, H., Chalmers, R., Robertson, N., Compston, D. A. S., Martino, G., Clementi, E., Brambilla, E., Moiola, L., Martinelli, V., Colombo, B., Poggi, A., Rovaris, M., Grimaldi, L. M. E., Roth, M. P., Descoins, P., Ballivet, S., Ruidavets, J. B., Waubant, E., Nogueira, L., Cambon-Thomsen, A., Clanet, M., Leppert, D., Hauser, S., Lugaresi, A., Tartaro, A., D'aurelio, P., Befalo, L. L. O., Thomas, A., Malatesta, G., Gambi, D., Benedikz, J. E. G., Magnusson, H., Poser, C. M., Guomundsson, G., Bates, T. E., Davies, S. E. C., Clark, J. B., Landon, D. N., ùther, J. R., Rautenberg, W., Overgaard, K., Sereghy, T., Pedersen, H., Boysen, G., Diez-Tejedor, E., Carceller, F., Gutierrez, M., Lopez-Pajares, R., Roda, J. M., Chandra, B., Ricart, W., Gonzalez-Huix, F., Molina, A., Rundek, T., Demarin, V., De Reuck, J., Boon, P., Decoq, D., Strijckmans, K., Goethals, P., Lemahieu, I., Nibbio, A., Chabriat, H., Vahedi, K., Nagy, T., Verin, M., Mas, J. L., Julien, J., Ducrocq, X., Iba-Zizen, M. T., Cabanis, E. A., Bousser, M. G., Rolland, Y., Landgraf, F., Bompais, B., Lemaitre, M. H., Edan, G., Vorstrup, S., Knudsen, L., Olsen, K. Skovgaard, Videbaek, C., Schroeder, T., van Gijn, J., Jansen, H. M. L., Pruim, J., Paans, A. M. J., Willemsen, A. T. M., Hew, J. M., vd Vliet, A. M., Haaxma, R., Vaalburg, W., Minderhoud, J. M., Korf, J., Soudain, S. E., Ho, T. W., Mishu, B., Li, C. Y., Nachainkin, I., Gao, C. Y., Cornblath, D. R., Griffin, J. W., Asbury, A. K., Blaser, M. J., McKhann, G. M., Ho, T., Macko, C., Xue, P., Stadlan, E. M., Ramos-Alvarez, M., Valenciano, L., Visser, L. H., van der Meché, F. G. A., van Darn, P. A., Meulstee, J., Schmitz, P. I. M., Jacobs, B., Oomes, P. G., Kleyweg, R. P., Jacobs, B. C., Endtz, H. P., van Doorn, P. A., van der Mech, F. G. A., Van den Berg, L. H., Mollee, I., Logtenberg, T., Thomas, P. K., Plant, G., Baxter, P. J., Luis, R. Santiago, Matsumoto, M., Notermans, N. C., Wokke, J. H. J., Lokhorst, H. M., van der Graaf, Y., Jennekens, F. G. I., Azulay, J. P., Bille-Turg, F., Valentin, P., Farnarier, G. G., Pellissier, J. F., Serratrice, G., Quasthoff, S., Schneider, U., Grafe, P., Hilkens, P. H. E., Moll, J. W. B., van der Burg, M. E. L., Planting, A. S. T., van Putten, W. L. J., van den Bent, M. J., Birklein, F., Spitzer, A., Lang, E., Neundorfer, B., Diehl, R. R., Lücke, D., Smith, G. D. P., Mathias, C. J., Serra, J., Campera, M., Ochoa, J. L., Ray Chaudhuri, K., Pavitt, D., Alam, M., Handwerker, H. O., Bleasdale-Barr, K., Smith, G., Murray, N. M. F., Hawkins, P., Pepys, M., Gellera, C., DiDonato, S., Taroni, F., Uncini, A., Di Muzio, A., Servidei, S., Silvestri, G., Lodi, R., Iotti, S., Barbiroli, B., Morrissey, S. P., Borruat, F. X., Francis, D., Mosely, I., Hansen, H. C., Helmke, K., Kunze, K., Sadzot, B., Maquet, P., Lemaire, Plenevaux, Damhaut, Sommer, C., Myers, R. R., Berta, E., Mantegazza, R., Argov, Z., Shapira, Y., Wirguin, I., Beuuer, J., Franke, C., Roberts, M., Willison, H., Vincent, A., Newsom-Davis, J., Morrison, K. E., Damels, R., Francis, M., Campbell, L., Davies, K. E., Kohler, W., Bucka, C., Hertel, G., Kanovsky, P., Auer, D., Ackermann, H., Klose, U., Naegele, Th., Bien, S., Voigt, K., Fink, G. R., Stephan, K. M., Wise, R. J. S., Mullatti, N., Hewer, L., Frackowiak, R. S. J., Weiller, C. S., Rijnites, M., Jueptner, M., Bauermann, T., Krams, M., Diener, H. C., van Walderveen, M. A. A., Barkhof, F., Hommes, O. R., Valk, J., Willmer, J. P., Guzman, D. A., Passingham, R. E., Silbersweig, D., Ceballos-Baumann, A., Frith, C. D., Frackowiak, R., Lucas, C. H., Goullard, L., Marchau, M. J., Godefroy, O., Rondepierre, P. H., Chamas, E., Mounier-Vehier, F., Leys, D., Renato, J., Verdugo, M. S. C., Campero, M., Jose, L., Ochoa, D. S. C., Vivancos, F., Tejedor, E. Diez, Martinez, N., Roda, J., Frank, A., Barreiro, P., Satoh, Y., Nagata, K., Maeda, T., Hirata, Y., YalÇinerner, B., Ozkara, C., Ozer, F., Ozer, S., Hanoglu, L., Zunker, P., Pozo, J. L., Oberwittler, C., Schick, A., Buschmann, H. -Ch., Ringelstein, E. Bernd, Lara, M., Anzola, G. P., Magoni, M., Volta, G. Dalla, Tarasov, A., Feigin, V., Beaudry, M. G., Carrier, S., Chicoutimi, Henriques, I. L., Bogoussslavsky, J., van Melle, G., Mathieu, J., Perusse, L., Allard, P., Prevost, C., Cantin, L., Bouchard, J. M., De Braekeleer, M., Agbo, C., Neau, J. P., Tantot, A. M., Dary-Auriol, M., Ingrand, P., Gil, R., Baltadjiev, D., Zekin, D., Sabey, K., Gennaula, C. P., Pope, B. A., Caparros-Lefebvre, D., Girard-Buttaz, I., Pruvo, J. P., Petit, H., Hipola, D., Martin, M., Giménez-Roldan, S., Ivanez, V., Japaridze, G., Carrasco, J. L., Picomell, I., Herranz, J. L., Macias, J. A., Nieto, M., Noya, M., Oller, L., Kiteva-Trencevska, G., Delgado, M. R., Liu, H., Luengo, A., Parra, J., Colas, J., Fernandez, M. J., Manzanares, R., Kornhuber, M. E., Malashkhia, V., Orkodashili, G., Martinez, M., Bonaventura, I., Porta, G., Martinez, I., Fernandez, A., Aguilar, M., Masnou, P., Drouet, A., Dreyfus, M., Cartron, J., Morel-Kopp, M. C., Tchernia, G., Kaplan, C., Lammers, M. W., Hekster, Y. A., Keyser, A., Meinardi, H., Renier, W. O., Boon, P. A. J. M., Have, M. D., Kint, B., Cruz, P., Cadilha, A., Almeida, R., Goncalves, M., Pimenta, M., Ramos, L. M. P., Polder, T. W., Broere, C. A., Polman, L., Rother, I., Rother, M., Schlaug, G., Arnold, S., Holthausen, H., Wunderlich, G., Ebner, A., Luders, H., Witte, O. W., Seitz, R. J., Serra, L. L., Gallicchio, B., Rotondi, F., Wieshmann, U., Meierkord, H., Sabev, K., Di Carlo, V., Gueguen, B., Derouesné, Ch., Ancri, D., Bourdel, M. C., Guillou, S., Aliaga, R., Chornet, M. A., Rodrigo, A., Pascual, A. Pascual -Leone, Catala, M. D., Pascual-Leone, A., Benbadis, S. R., Dinner, D. S., Chelune, G. J., Lüders, H. O., Piedmonte, M. R., Blanco, T., Lopez, M. P., Romero, B., Deltoro, A., Pascual, A., Pascual, Leone, Bolgert, F., Josse, M. O., Tassan, P., Touze, E., Laplane, D., Godenberg, F., Brizioli, E., Del Gobbo, M., Pelliccioni, G., Scarpino, O., Durak, H., Damlacik, G., Tunca, Z., Fidaner, H., Yurekli, Y., Yemez, B., Kaygisiz, A., Anllo, E. A., Esperet, E., Giovagnoli, A. R., Casazza, M., Spreafico, R., Avanzini, G., Mascheroni, S., Vecchio, I., Tornali, C., Antonuzzo, A., Grasso, A. A., Bella, R., Pennisi, G., Raffaele, R., Broeckx, J., Schildermans, F., Hospers, W., Deberdt, W., Carney, J. M., Aksenova, M., Chen, M. S., Juncadella, M., Busquets, N., De la Fuente, I., Rodriguez, A., Rubio, F., Soler, R., Khati, C., Pillon, B., Deweer, B., Malapani, C., Malichard, N., Dubois, B., Rancurel, G., Lopez, D. L., Jungreia, G., DeKosky, S. T., Boiler, F., Weiller, C., Rijntjes, M., Mueller, S. P., Maguire, E. A., Burke, E. T., Staunton, H., Phillips, J., Rousseaux, M., Pena, J., Bertran, I., Santacruz, P., Lopez, R., Catafau, A., Lomena, F., Blesa, R., Rampello, L., Nicoletti, A., Cabaret, M., Lesoin, F., Steinling, M., Tournev, I., Maier-Hauff, K., Schroeder, M., Wolf, A., Cochin, J. P., Noel, I., Augustin, P., Auzou, P., Hannequin, D., Maria, V., Lopez-Bresnahan, Danielle, D. M., Antin-Ozerkis B. A., Bartels, E., Rodiek, S. O., Flugel, K. A., Campos, D. M., Salas-Puig, J., Del Rio, J. Sanhez, Vidal, J. A., Lahoz, C. H., Eraksoy, M., Barlas, O., Barlas, M., Bayindir, C., Ozcan, H., Birbamer, G., Gerstenbrand, F., Felber, S., Luz, G., Aichner, F., Seidel, G., Kaps, M., Hutzelmann, A., Gerriets, T., Kruggel, F., Martin, P. J., Gaunt, M. E., Abbot, R. J., Naylor, A. R., Meary, E., Dilouya, A., Meder, J. F., De Recondo, J., Lebtahi, R., Neff, K. W., Meairs, S., Viola, S., Matta, E., Aquilone, L., Rise, I. R., Authier, F. J., Kondo, H., Ghnassia, R. T., Degos, J. D., Gherardi, R. K., Bardoni A., Ciafaloni E., Comi G. P., Bresolin N., Robotti M., Moggio M., Rigoletto C., Roses A., Scarlato G., Castelli, E., Turconi, A., Bresolin, N., Perani, D., Felisari, G., Chariot, P., de Pinieux, G., Astier, A., Jacotot, B., Gherardi, R., Fischer-Gagnepain, V., Louboutin, J. P., Crespo, F., Florea-Strat, A., Fromont, G., Sabourin, J. -C., Gonano, E. -F., Moroni, I., Prelle, A., Iannaccone, S., Quattrini, A., deRino, F., Sessa, M., Golzi, V., Smirne, S., Nemni, R., Turpin, J. C., Lucotte, G., Jacobs, S. C. J. M., Willems, P. W. A., Bootsma, A. L., Lasa, A., Calaf, M., Baiget, M., Gallano, B., Fichter-Gagnepain, V., Mazzucchelli, F., D'Angelo, M. G., Velicogna, M., Bet, L., Comi, G. P., Bordoni, A., Gonano, E. F., Bazzi, P., Rapuzzi, S., Moggio, M., Fagiolari, G., Ciscato, P., Messina, A., Battistel, A., Ryniewicz, B., Sangla, I., Desnuelle, C., Paquis, V., Cozzone, P. J., Bendahan, D., Sturenburg, H. J., Kohncke, G., Castellli, E., Linssen, W., Stegeman, D., Binkhorst, R., Notermans, S., Jaspert, A., Fahsold, R., de Munain, A. Lopez, Cobo, A., Martorell, L., Poza, J. J., Navarrete Palau, D., Emparanza, J. I., Sanchez-Roy, R., Vilchez, J. J., Hernandez, M., Tena, J. Garcia, Perla, C., Koutroumanidis, M., Papathanasopoulos, P., Papadimitriou, A., Papapetropoulos, T. H., Divari, R., Hadjigeorgiou, G. M., Anastasopoulos, I., Sansone, V., Rotondo, G., Meola, G., Rigoletto, C., Messina, S., Szwabowska-Orzeszko, E., Jozwiak, S., Michalowicz, R., Szaplyko, W., Petrella, M. A., Della Marca, G., Masullo, G., Mennuni, G. F., Kompf, D., Wascher, E., Verleger, R., Kaido, M., Soga, F., Toyooka, H., Bayon, C., Rubio, J., Carlomagno, S., Parlato, V., Santoro, A., Lavarone, A., Bonavita, V., Pentore, R., Venneri, A., Pasquier, F., Lebert, F., Grymonprez, L., Lefebvre, C., Van der Linden, M., Derouesné, C., Renault, B., Lacomblez, L., Homeyer, P., Ouss, L., Neuman, E., Malbezin, M., Barrandon, S., Guez, D., Stevens, M., van Swieten, J. C., Franke, C. L., Sanchez, A., Castellvirel, S., Mila, M., Jimenez, D., Pallesta, F., Ruiz, P. J. Garcia, Barrio, A., Barroso, T., Benitez, J., de Yebenes, J. Garcia, Manubens, J. M., Martinez-Lage, J. M., Larumbe, R., Muruzabal, J., Lacruz, F., Quesada, Pedro, Gallego, J., Ferini-Strambi, L., Marcone, A., Garancini, P., Tedesi, B., Jacob, B., Rozewicz, L., Langdon, D., Davie, C., Ron, M., Thompson, A., Koepp, M. J., Hansen, M. L., Guldin, B., Pressler, R. M., Ried, S., Scholz, C., Monaco, F., Gianelli, M., Schiavalla, M. P., Naldi, P., Cantello, R., Torta, R., Verze, L., Mutani, R., Knott, H., Ferbert, A., Schulze-Bonhage, A., Aust, W., Di Mascio, R., Marchioli, R., Vitullo, F., Di Pasquale, A., Sciulli, L., Kramer, V., Tognoni, G., Santacruz, P., Lopez, R., Marti, M. J., Charques, I., Catafau, A., Lomeila, F., Peila, J., Bertran, I., Blesa, R., Krendel, D. A., Costiga, D. A., Koeppen, S., Korn, W. M., Brugge, S., Schmitz, D., Scheulen, M. E., King, R. H. M., Robertson, A. M., Thomas, P. K., Kerkhofs, A., Vermersch, P., Dereeper, O., Daems Monpeun, C., Parent, M., Deplanque, D., Petit, H., Campero, M., Serra, J., Ochoa, J. L., Martinez-Matos, J. A., Montero, J., Olivé, M., Rene, R., Vidaller, A., Gugenheim, M., Gouider, R., Le Guern, E., Brice, A., Agid, Y., Bouche, P., Grisold, W., Ziflo, U., Drlicek, M., Budka, H., Jellinger, K., Zielinski, C. H., Ginsberg, L., King, R. H. M., Workman, J., Platts, A. D., Thomas, P. K., Gherardi, R. K., Florea-Strat, A., Poron, F., Sabourin, J. -C., Fazio, R., Nemni, R., Franceschi, M., Lorenzetti, I., Rinaldi, L., Canal, N., Weilbach, F. X., Sennlaub, A., Jung, S., Gold, R., Toyka, K. V., Hartung, H. P., Giegerich, G., Ellie, E., Vital, A., Steck, A. J., Vital, C., Julien, J., Doneda, P., Pizzul, S., Scarpini, E., Chiodi, P., Ramacci, M. T., Livraghi, S., Maimone, D., Annunziata, P., Salvadori, C., Guazzi, G. C., Arne-Bes, M. C., Delisle, M. B., Fabre, N., Hurtevent, J. F., Bes, A., Baudoin-Martin, D., Laborde, E., Viallet, F., Creisson, C., Crespi, V., Bogliun, G., Marzorati, L., Zincone, A., D'Angelo, L., Liberani, A., Merlini, M., Rivolta, R., Creange, A., Sabourin, J. -C., Theodorou, I., Gherardi, R. K., Conti, A. M., Malosio, M. L., Baron, P. L., Scarlato, G., Chorao, R., Rosas, M. J., Leite, I., Callea, L., Donati, E., Bargnani, C., Bud, M., Verdu, E., Navarro, X., Braun, S., Einius, S., Poindron, P., Warier, J. M., Bradley, J., Bekkelund, S. I., Torbergsen, T., Mellgren, S. I., Carlomagno, S., Parlato, V., Santoro, A., Lavarone, A., Boller, F., Bonavita, V., Engelhardt, A., Lörler, H., Robeck, S., Kluglein, C., Comi, G., Avoledo, V., Locatelli, T., Leocani, L., Galardi, G., Magnani, G., Medaglini, S., Chkhikvishvili, T. S., Zangaladze, A., Bratoeva, M., Kovachev, P., Chavdarov, D., Artemis, N., Karacostas, D., Milonas, I., Arpa, J., Lopez-Pajares, R., Cruz-Matinez, A., Sarria, J., Palomo, F., Alonso, M., Rodriguez-Al-barino, A., Lacasa, T., Nos, J., Barreiro, P., Martinez, A. Cruz, Villoslada, C., Alons, M., Taghavy, A., Hamer, H., Kratzer, A., Dethy, S., Pauwels, T., Monclus, M., Luxen, A., Goldman, S., Ziegler, M., Crambes, O., Ragueneau, I., Arnaud, F., Zappia, M., Montesanti, R., Colao, R., Palmieri, A., Branca, D., Nicoletti, G., Rizzo, M., Parlato, G., Quattrone, A., Vanacore, N., Zuchegna, P., Bonifati, V., Meco, G., Scholz, J., Friedrich, H. -J., Rohl, A., Ulm, G., Vieregge, P., Savettieri, G., Rocca, W. A., Meneghini, F., Grigoletto, F., Morgante, L., Reggio, A., Salemi, G., Di Pierri, R., OzckmekÇi, S., Ertan, S., Yeni, N., Apaydin, H., Erkol, G., Kiziltan, G., Denktas, F., Ranoux, D., de Recondo, J., Ostergaard, L., Werdelin, L., Odin, P., Lindvall, O., Dupont, E., Christensen, P. B., Boisen, E., Jensen, N. B., Schmiegelow, M., Ingwersen, S. H., Matias-Guiu, J., Canet, T., Falip, R., Martin, R., Galiano, L., Voloshin, M. Y., Burchinskaya, L. F., Cabrera-Valdivia, F., Jimenez-Jimenez, F. J., Molina, J. A., Fernandez-Calle, P., Vazquez, A., Canizares-Liebana, F., Larumbe-Lobalde, S., Ayuso-Peralta, L., Rabasa, M., Codoceo, R., Arrieta, F. J., Aguilar, M. V., Jorge-Santamaria, A., Martinez-Para, M. C., Alarcon, J., Mateo, D., Gimenez-Roldan, S., Gencheva, E., Tzonev, T. z., Georgiev, G., Petkova, P., Gasparini, M., Vanacore, N., Meco, N. G., de la Sierra, G., Aguado, F., Revilla, M., Varela, L., Rico, H., Feve, A., N'Guyen, J. P., Bathien, N., Fenelon, G., Veroust, J., Cesaro, P., Egersbach, G., Hattig, H., Schelosky, L., Wissel, J., Poewe, W., Durif, F., Albuisson, E., Debilly, B., Tournilhac, M., Magnani, C., Mocellini, C., Soffietti, R., Schiffer, D., Cardozo, A., Cruz-Sanchez, F. F., Falip, L., Potagas, G., Ziegler, M., Rondot, P., Bonifati, V., Fabrizio, E., Meco, G., Bostantjopoulou, S., Katsarou, Z., Kyriazis, G., Baas, H., Demisch, L., Esser, A., Zoeller, F., Burklin, F., Harder, S., Fischer, P. A., Arcusa, M. J., Hermandez, S., Claramonte, F. J., Pascual, A. Pascual- Leone, Alonso, M. D., Catata, M. D., Alessandri, A., Giustini, P., Dufour, A., Ciusani, E., Nespolo, A., Roelcke U., Radu E. W., von Ammon K., Maguire R. P., Leenders K. L., Radionova, M., Chavdarov, D., Bratoeva, M., Tzekov, Ch., Pietrangeli, A., Bove, L., Pace, A., Falqui, L., Jandolo, B., Potemkowski, A., Muller B., Reinhard I., Krone A., Warmuth M., Brocker E. M., Krauseneck P., Meyding-Lamadé, U., Krieger, D., Sartor, K., Hacke, W., Maugard-Louboutin, C., Fayet, G., Sagan, C., Martin, S., Ménégalli, D., Lajat, Y., Resche, F., Koriech, O. M., Al Moutaery, K., Yaqub, B., Jochens, R., Wolters, A., Venz, S., Cordes, M., Hecht, B. K., Chatel, M., Gaudray, P., Turc-Carel, C., Gioanni, J., Ayraud, N., Hecht, F., Rumbach, L., Racadot, E., Bataillard, M., Billot, M., Pariset, J., Wijdenes, J., Montalban, Rio J., Tintoré, M., Galan, I., Acarin, N., Rapaport, S., Huberman, M., Shechtcr, D., Karabudak, R., Kilinc, M., Boyacigil, S., Cila, A., Polo, J. M., Setien, S., Sanchez, R., Figols, J., Zubimendi, A., Nadareishvili, Z. G., Massot, R., Marés, R., Gallecho, F., Richart, C., Hernandez, M. A., Garcia, M. R., Lorenzo, J. N., Leon, C., Muros, M., Togores, J., Kutluk, K., Damlacik, G. A., Tekinsoy, B., Obuz, O., Baklan, B., Idiman, E., Genc, K., Zielasek, J., Schmidt, B., Liew, F. Y., Gulay, Z., Yulug, N., Wong, K. S., Wong, T. W., Yu, T. S., Kay, R., Poupon, R., Giral, P., Roberti, C., Zanette, E. M., Chiarotti, F., Brusa, L., Cerbo, R., Prusinski, A., Pondal, M., Canton, R., Dominigo, Erodriguez J., Pereira Monteino J. M., Pereira Monteino X., Pardo, J., Carroacedo, A., Barros, F., Lema, M., Castillo, J., Melchor, A., Montiel, I., Guiu, J. Matias, Kloss, T. M., Keidel, M., Jacob, M., Idiman, F., Idman, E., Ozturk, V., Metin, E., Yilmaz, M., Gerard, J. M., Bouton, R., Decamps, D., Herbaut, A. G., Delecluse, F., Cavenaile, M., Divano, L., Chazot, G., Boureau, F., Emile, J., Bertin, L., d'Allens, H., Ferro, J. M., Costa, I., Carletto, F., Catarci, T., Padovani, A., Iandolo, B., Bartoli, M., Bonamini, M., Pulcinelli, F., Pignatelli, P., Russo, M., Gazzaniga, P. P., Barros, J., Pinheiro, J., Correia, A. P., Monteiro, J. M. Pereira, Alvarez-Cermeno, J. C., Avello, G., Sastre, J. L., Vecino, A., Cesar, J. M., Leone, M., Stankov, B., D'Amico, D., Maltempo, C., Moschian, F., Fraschini, F., Bussone, G., Molto, J. M., Fernandez, E., Fernandez, A. Morento, Barreiro, A., Siclia, J., Castejon, P., Mihout, B., Malberin, M., Salzman, V., Bogousslavsky, J., Meneghetti, G., Baracchini, C., Bozzato, G., Marini, B., Mendel, T., Czlonkowska, A., Pasierski, T., Szwed, H., Marta-Moreno, J., Lopez-Delval, J., Mostacero, E., Morales, F., Mahagne, M. H., Rogopoulos, A., Bertrand, F., Bedoucha, P., Lanteri-Minet, M., Riva, D., Zorzi, C., Milani, N., Vajsar, J., Ronen, G., Macgregor, D., Becker, L., Susseve, J., Seidl, Z., Faber, J., Obenberger, J., Springer, R., Bax, R. T., Eckardt, T., Czettritz, G. V., Emmrich, P., Vlaski-Jekic, S., Petrova, V., Cherninkova, S., Gudeva, T., Tzekov, C., Devoti, M., Franceschetti, S., Mientus, S., Vienna, P., Vashtang, Y., Tazir, M., Assami, S., Oulbani, D., Kaci Ahmed, M. Ait, Andersen, G., Vestergaard, K., Riis, J. O., Chavdarov, D., Corbo, M., Previtali, S., Allen, R. R., McKay, W. C., Rowbotham, M. 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B., Roelcke, U., von Ammon, K., Pellikka, R., Lucking, C. H., Walon, C., Boucquey, D., -Van Rijckevorsel, K. Harmant, Lannoy, N., Verellen-Dunoulin, Ch., Liszka, U., Cavaletti, G., Casati, B., Kolig, C., Bogliun, G., Marzorati, L., Johannsen, L., Chio, A., Ruda, R., Vigliani, M. C., Sciolla, R., Seliak, D., Hoang-Xuang, K., Villanueva, J. A., Montalban, X., Arboix, A., Colosimo, C., Albanese, A., Hughes, A. J., de Bruin, V., Lees, A. J., Kowalski, J. W., Banfi, S., Santoro, L., Perretti, A., Castaldo, I., Barbieri, F., Campanella, G., Bhatia, K. P., Mardsen, C. D., de Bruin, V. S., Machedo, C., Ceballos-Baumann, D., Marsden, C. D., Brooks, D. B. J., Wennlng, G. K., Quinn, N., McDonald, W. l., Warner, T. T., Bain, P. C., Davis, M. B., Conway, D., Shaunak, S., O'Sullivan, E., Crawford, T., Lawden, M., Blunt, S., Rapoport, A., Sarova-Pinchas, I., de Beyl, D. Zegers, Mavroudakis, N., Blanc, S., Godinot, C., Lenoir, G., Barkhof, M. S. F., Tas, M. W., Baron, P. L., Constantin, C., Cassatella, M. A., Langdon, D. W., Webb, S., Gasparini, P., Zeviani, A., Kidd, D., Mammi, S., Cahalon, L., Hershkoviz, R., Lahat, N., Wallach, D., Annunziata, P., Martino, T., Maimone, D., Guazzi, G. C., Porrini, A. M., Dell'Arciprete, L., Rothwell, P. M., Stewart, R. R. C., Cull, R. E., Willmes, K., Poeck, K., Russell, D., Braekken, S. K., Brucher, R., Svennevig, J., Hermesl, M., Bruckmann, H., Biraben, A., Sliwka, U., Meyer, B., Schondube, F., Noth, J., Lavenu, I., Lammers, C., Waldecker, B., Haberbosch, W., Stam, J., Schneider, R., Gautier, J. C., Berlit, T. P., Fauser, B., Kuhne, D., Geraud, G., Danielli, A., Larrue, V., Bes, A., Timmerman, E., Bono, F., Bruni, A. C., Valalentino, P., Montesi, M. P., Talerico, G., Zappia, M., Sabatelli, M., Quattrone, A., Pareyson, D., Lorenzetti, D., Sghirlanzoni, A., Castellotti, B., Lupski, J. R., Archidiacono, N., Antonacci, R., Marzella, R., Rocchi, M., Samuel, D., Goulon-Goeau, C., Costa, P. P., Bismuth, H., Said, G., De Jongh P., Lofgren A., Timmerman V., Vance J. M., Van Broeckhoven C., Martin J. -J., Martinez, A. Cruz, Bort, S., Arpa, J., Misra, P., King, R. H. M., Badhia, K., Anderson, M., Caballo, A., Vichez, J., Gabriel, J. M., Erne, B., Miescher, G. C., Ulrich, J., Vital, A., Vital, C., Steck, A., Petry, K., Labatut, I., Hilmi, S., Ellie, E., Ferrini-Strambi, L., Zucconl, M., Marchettini, P., Palazzi, S., Oehlschlager, M., Pepinsky, R. B., Gemignani, F., Marbini, A., Pavesi, G., Di Vittorio, S., Manganelli, P., Mancia, D., Vermersh, P., Roche, J., Durocher, A. M., Dewailly, Ph., Dettmers, C., Fink, G., Lemon, R., Stephan, K., Passingham, D., Weder, B., Knorr, U., Huang, Y., Butterfield, D. A., Peris, M. L., Peiro, C., Pascual, A. Pascual-Leone, Bottini, G., Folnegovic-Smalc, V., Knezevic, S., Bokonjic, R., Ersmark, B., Torres, M. Gonzalez, Guiraud-Chaumeil, B., Haugaard, K., Jovicic, A., Chr, Lang, Levic, Z., Parra, C. Martinez, Ochoa, J. Patrignani, Titlbach, O., Wikkelso, C., Caparros-Lefevre, D., Debachy, B., Verier, A., Cantinho, G., Santos, A. I., Godinho, F., Bagunya, J., Roig, T., Ensenyat, A., Santiag, O., Trabucchi, H., De Leo, D., Koch, Ch., Zeumer, H., Matkovic, Z., Morris, P., Donaghy, M., Köhler, W., Kammer, T., Röther, J., Navon, R., Fontaine, B., Wu, Y., Capdevila, A., Guardiola, M. J., van Dijk, G. W., Notermans, N. C., Kruize, A. A., Kater, L., Bertelt, C., Hesse, S., Friedrich, H., Mauritz, K. -H., Giron, L. T., Watanabe, I. S., Ewing, D., Koepp, M., Lempert, T., Sander, B., Kauerz, U., Mehdorn, H. M., Hezel, J., Eickhoff, W., Kryst, T., Timsit, S., Gardeur, D., Reis, Mitermayer Galvao dos, Secor, E., Filho, A. Andrade, Silva, M. Cardoso, Santos, S. R. Silveira, Vasilaski, G., Reis, E. A. dos, Velupillai, P., Harn, D. A., Tigera, J. Garcia, Dreke, R. Martinez, Crespo, R. Piedra, Besses, C., Acin, P., Massons, J., Florensa, L., Oliveres, M., Sans-Sabrafen, J., Wicklein, E. M., Pleiffer, G., Kunre, K., Dieterich, M., Brandt, Th., Guarino, M., Stracciari, A., Pazzaglia, P., D'Alessandro, R., Santilli, I., Donato, M., The European Velnacrine Study Group, The Dutch Guillain-Barré study group, The COP-1 Multicenter Clinical and Research Group Study, and European Study Group
- Published
- 1994
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46. Water Vapor Vertical Profiles on Mars in Dust Storms Observed by TGO/NOMAD
- Author
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Belgian Science Policy Office, European Space Agency, Ministerio de Ciencia e Innovación (España), European Commission, UK Space Agency, Agenzia Spaziale Italiana, Ministerio de Ciencia, Innovación y Universidades (España), Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles), National Aeronautics and Space Administration (US), Canadian Space Agency, Aoki, Shohei, Vandaele, Ann Carine, Daerden, Frank, Villanueva, Geronimo L., Liuzzi, Giuliano, Thomas, Ian R., Erwin, Justin T., Trompet, L., Robert, S., Neary, L., Viscardy, S., Hathi, B., Zafra, J.J., Leese, M., Maes, J., Pastor-Morales, M., Mazy, E., Mazzoli, A., Meseguer, J., Morales, Rafael, Pérez Grande, Isabel, Ristic, Bojan, Queirolo, C., Ristic, R., Gomez, J.R., Saggin, B., Smith, M.D., Samain, V., Sanz Andres, A., Altieri, F., Sanz, R., Simar, J.-F., Patel, Manish R., Thibert, T., the NOMAD team, López-Valverde, M. A., Hill, Brittany, Bellucci, Giancarlo, Bauduin, S., López-Moreno, José Juan, Alonso-Rodrigo, G., Fussen, D., Bolsée, D., Carrozzo, G., Clancy, R. Todd, Cloutis, E., Crismani, M., Da Pieve, F., D'Aversa, E., Kaminski, J., Depiesse, C., Garcia-Comas, M., Etiope, G., Fedorova, A.A., Funke, Bernd, Geminale, A., Gérard, Jean-Claude, Giuranna, M., Karatekin, O., Gkouvelis, L., González-Galindo, F., Holmes, J., Hubert, B., Mumma, M.J., Ignatiev, N.I., Kasaba, Y., Kass, D., Kleinböhl, A., Lanciano, O., Lefèvre, F., Lewis, S., López-Puertas, M., Schneider, Nicholas, Nakagawa, H., Hidalgo López, Ana, Mahieux, A., Mason, J., Mege, D., Neefs, E., Novak, R.E., Oliva, F., Sindoni, G., Piccialli, A., Renotte, E., Ritter, B., Willame, Y., Schmidt, F., Teanby, N.A., Thiemann, E., Trokhimovskiy, A., Auwera, J.V., Wolff, M.J., Clairquin, R., Whiteway, J., Wilquet, V., Wolkenberg, P., Yelle, R., del Moral Beatriz, A., Barzin, P., Beeckman, B., Cubas, J., BenMoussa, A., Berkenbosch, S., Orban, A., Biondi, D., Bonnewijn, S., Candini, G.P., Giordanengo, B., Gissot, Samuel, Gomez, A., Belgian Science Policy Office, European Space Agency, Ministerio de Ciencia e Innovación (España), European Commission, UK Space Agency, Agenzia Spaziale Italiana, Ministerio de Ciencia, Innovación y Universidades (España), Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles), National Aeronautics and Space Administration (US), Canadian Space Agency, Aoki, Shohei, Vandaele, Ann Carine, Daerden, Frank, Villanueva, Geronimo L., Liuzzi, Giuliano, Thomas, Ian R., Erwin, Justin T., Trompet, L., Robert, S., Neary, L., Viscardy, S., Hathi, B., Zafra, J.J., Leese, M., Maes, J., Pastor-Morales, M., Mazy, E., Mazzoli, A., Meseguer, J., Morales, Rafael, Pérez Grande, Isabel, Ristic, Bojan, Queirolo, C., Ristic, R., Gomez, J.R., Saggin, B., Smith, M.D., Samain, V., Sanz Andres, A., Altieri, F., Sanz, R., Simar, J.-F., Patel, Manish R., Thibert, T., the NOMAD team, López-Valverde, M. A., Hill, Brittany, Bellucci, Giancarlo, Bauduin, S., López-Moreno, José Juan, Alonso-Rodrigo, G., Fussen, D., Bolsée, D., Carrozzo, G., Clancy, R. Todd, Cloutis, E., Crismani, M., Da Pieve, F., D'Aversa, E., Kaminski, J., Depiesse, C., Garcia-Comas, M., Etiope, G., Fedorova, A.A., Funke, Bernd, Geminale, A., Gérard, Jean-Claude, Giuranna, M., Karatekin, O., Gkouvelis, L., González-Galindo, F., Holmes, J., Hubert, B., Mumma, M.J., Ignatiev, N.I., Kasaba, Y., Kass, D., Kleinböhl, A., Lanciano, O., Lefèvre, F., Lewis, S., López-Puertas, M., Schneider, Nicholas, Nakagawa, H., Hidalgo López, Ana, Mahieux, A., Mason, J., Mege, D., Neefs, E., Novak, R.E., Oliva, F., Sindoni, G., Piccialli, A., Renotte, E., Ritter, B., Willame, Y., Schmidt, F., Teanby, N.A., Thiemann, E., Trokhimovskiy, A., Auwera, J.V., Wolff, M.J., Clairquin, R., Whiteway, J., Wilquet, V., Wolkenberg, P., Yelle, R., del Moral Beatriz, A., Barzin, P., Beeckman, B., Cubas, J., BenMoussa, A., Berkenbosch, S., Orban, A., Biondi, D., Bonnewijn, S., Candini, G.P., Giordanengo, B., Gissot, Samuel, and Gomez, A.
- Abstract
It has been suggested that dust storms efficiently transport water vapor from the near-surface to the middle atmosphere on Mars. Knowledge of the water vapor vertical profile during dust storms is important to understand water escape. During Martian Year 34, two dust storms occurred on Mars: a global dust storm (June to mid-September 2018) and a regional storm (January 2019). Here we present water vapor vertical profiles in the periods of the two dust storms (Ls = 162–260° and Ls = 298–345°) from the solar occultation measurements by Nadir and Occultation for Mars Discovery (NOMAD) onboard ExoMars Trace Gas Orbiter (TGO). We show a significant increase of water vapor abundance in the middle atmosphere (40–100 km) during the global dust storm. The water enhancement rapidly occurs following the onset of the storm (Ls~190°) and has a peak at the most active period (Ls~200°). Water vapor reaches very high altitudes (up to 100 km) with a volume mixing ratio of ~50 ppm. The water vapor abundance in the middle atmosphere shows high values consistently at 60°S-60°N at the growth phase of the dust storm (Ls = 195°–220°), and peaks at latitudes greater than 60°S at the decay phase (Ls = 220°–260°). This is explained by the seasonal change of meridional circulation: from equinoctial Hadley circulation (two cells) to the solstitial one (a single pole-to-pole cell). We also find a conspicuous increase of water vapor density in the middle atmosphere at the period of the regional dust storm (Ls = 322–327°), in particular at latitudes greater than 60°S. ©2019. American Geophysical Union. All Rights Reserved.
- Published
- 2019
47. NOMAD, an Integrated Suite of Three Spectrometers for the ExoMars Trace Gas Mission: Technical Description, Science Objectives and Expected Performance
- Author
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Vandaele, Ann Carine, López-Moreno, José Juan, Patel, Manish R., Bellucci, Giancarlo, Daerden, Frank, Ristic, Bojan, Robert, S., Thomas, Ian R., Wilquet, V., Allen, M., Alonso-Rodrigo, G., Altieri, F., Aoki, Shohei, Bolsée, D., Clancy, T., Cloutis, E., Depiesse, C., Drummond, R., Fedorova, A., Formisano, V., Funke, Bernd, González-Galindo, F., Geminale, A., Gérard, Jean-Claude, Giuranna, M., Hetey, L., Ignatiev, N., Kaminski, J., Karatekin, O., Kasaba, Y., Leese, M., Lefèvre, F., Lewis, S. R., López-Puertas, Manuel, López-Valverde, M. A., Mahieux, A., Mason, J., McConnell, J., Mumma, M., Neary, L., Neefs, E., Renotte, E., Rodriguez-Gomez, J., Sindoni, G., Smith, M., Stiepen, A., Trokhimovsky, A., Vander Auwera, J., Villanueva, Geronimo L., Viscardy, S., Whiteway, J., Willame, Y., Wolff, Michael T., Patel, M., D’aversa, E., Fussen, D., García Comas, Maia, Hewson, W., McConnel, J., Novak, R., Oliva, F., Piccialli, A., Aparicio del Moral, Beatriz, Barzin, P., BenMoussa, A., Berkenbosch, S., Biondi, D., Bonnewijn, S., Candini, G. P., Clairquin, R., Cubas, J., De-Lanoye, S., Giordanengo, B., Gissot, S., Gomez, A., Maes, J., Mazy, E., Mazzoli, A., Meseguer, J., Morales, Rafael, Orban, A., Pastor, Carmen, Perez-Grande, I., Queirolo, C., Saggin, B., Samain, V., Sanz Andres, A., Sanz Mesa, Rosario, Simar, J.-F., Thibert, T., Jerónimo, José María, The NOMAD Team, Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), School of Physical Sciences [Milton Keynes], Faculty of Science, Technology, Engineering and Mathematics [Milton Keynes], The Open University [Milton Keynes] (OU)-The Open University [Milton Keynes] (OU), Space Science and Technology Department [Didcot] (RAL Space), STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC)-Science and Technology Facilities Council (STFC), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Jet Propulsion Laboratory (JPL), California Institute of Technology (CALTECH)-NASA, Instituto Universitario de Microgravedad 'Ignacio Da Riva' (IDR), Universidad Politécnica de Madrid (UPM), Space Science Institute [Boulder] (SSI), Department of Geography [Winnipeg], University of Winnipeg, Space Research Institute of the Russian Academy of Sciences (IKI), Russian Academy of Sciences [Moscow] (RAS), Laboratoire de Physique Atmosphérique et Planétaire (LPAP), Université de Liège, Institute of Geophysics [Warsaw], Polska Akademia Nauk = Polish Academy of Sciences (PAN), Royal Observatory of Belgium [Brussels] (ROB), Tohoku University [Sendai], PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Fonds National de la Recherche Scientifique [Bruxelles] (FNRS), York University [Toronto], NASA Goddard Space Flight Center (GSFC), Centre Spatial de Liège (CSL), Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], Service de Chimie Quantique et Photophysique, Université libre de Bruxelles (ULB), Catholic University of America, Belgian Science Policy Office, European Space Agency, Ministerio de Ciencia e Innovación (España), European Commission, UK Space Agency, Agenzia Spaziale Italiana, and Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles)
- Subjects
010504 meteorology & atmospheric sciences ,Solar occultation ,education ,Physique atomique et moléculaire ,Exploration of Mars ,01 natural sciences ,Occultation ,law.invention ,Orbiter ,Mars atmosphere ,law ,0103 physical sciences ,Nadir ,Chimie ,natural sciences ,010303 astronomy & astrophysics ,Spectroscopy ,0105 earth and related environmental sciences ,Remote sensing ,Ultraviolet ,Martian ,Astronomy and Astrophysics ,Dust ,Atmosphere of Mars ,Mars Exploration Program ,Nadir observations ,ExoMars ,Trace gas ,[SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM] ,Spectroscopie [électromagnétisme, optique, acoustique] ,13. Climate action ,Space and Planetary Science ,Visible ,Environmental science ,Infrared ,Methane ,Composition - Abstract
Open Access This article is distributed under the terms of the Creative Commons Attribution 4.0 International License (http://creativecommons.org/licenses/by/4.0/), The NOMAD (“Nadir and Occultation for MArs Discovery”) spectrometer suite on board the ExoMars Trace Gas Orbiter (TGO) has been designed to investigate the composition of Mars’ atmosphere, with a particular focus on trace gases, clouds and dust. The detection sensitivity for trace gases is considerably improved compared to previous Mars missions, compliant with the science objectives of the TGO mission. This will allow for a major leap in our knowledge and understanding of the Martian atmospheric composition and the related physical and chemical processes. The instrument is a combination of three spectrometers, covering a spectral range from the UV to the mid-IR, and can perform solar occultation, nadir and limb observations. In this paper, we present the science objectives of the instrument and explain the technical principles of the three spectrometers. We also discuss the expected performance of the instrument in terms of spatial and temporal coverage and detection sensitivity.© 2018, The Author(s)., The NOMAD experiment is led by the Royal Belgian Institute for Space Aeronomy (IASB-BIRA), assisted by Co-PI teams from Spain (IAA-CSIC), Italy (INAF-IAPS), and the United Kingdom (Open University). This project acknowledges funding by the Belgian Science Policy Office (BELSPO), with the financial and contractual coordination by the ESA Prodex Office (PEA 4000103401, 4000121493), by Spanish MICINN through its Plan Nacional and by European funds under grant ESP2015-65064-C2-1-P (MINECO/FEDER), as well as by UK Space Agency through grants ST/R005761/1, ST/P001262/1, ST/R001405/1 and ST/R001405/1 and Italian Space Agency through grant 2018-2-HH.0. The research was performed as part of the >Excellence of Science> project >Evolution and Tracers of Habitability on Mars and the Earth> (30442502). SA acknowledge support from the FNRS, Be.
- Published
- 2018
48. The dust coma environment of 67P/Churyumov-Gerasimenko as observed by VIRTIS
- Author
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Rinaldi, G., Bockelee-Morvan, D., Ciarniello, M., Tozzi, G., Fink, U., Doose, L., Capaccioni, F., Della Corte, Vincenzo, Fulle, M., Rotundi, A., Filacchione, G., Taylor, F.W., Kappel, David, Erard, S., Leyrat, C., Raponi, A., D'Aversa, E., Ivanovski, S., Capria, M. T., Longobardo, A, Palomba, E., Tosi, F., Migliorini, A., and Salatti, M.
- Subjects
Comet 67P ,Dust ,Coma ,VIRTIS - Published
- 2018
49. NOMAD, an Integrated Suite of Three Spectrometers for the ExoMars Trace Gas Mission: Technical Description, Science Objectives and Expected Performance
- Author
-
Vandaele, A. C., López-Moreno, José Juan, Patel, M. R., Bellucci, G., Daerden, F., Ristic, B., Robert, S., Thomas, I. R., Wilquet, V., Allen, M., Alonso-Rodrigo, G., Altieri, F., Aoki, S., Bolsée, D., Clancy, T., Cloutis, E., Depiesse, C., Drummond, R., Fedorova, A., Formisano, V., Funke, Bernd, González-Galindo, F., Geminale, A., Gérard, Jean-Claude, Giuranna, M., Hetey, L., Ignatiev, N., Kaminski, J., Karatekin, O., Kasaba, Y., Leese, M., Lefèvre, F., Lewis, S. R., López-Puertas, Manuel, López-Valverde, M. A., Mahieux, A., Mason, J., McConnell, J., Mumma, M., Neary, L., Neefs, E., Renotte, E., Rodriguez-Gomez, J., Sindoni, G., Smith, M., Stiepen, A., Trokhimovsky, A., Vander Auwera, J., Villanueva, G., Viscardy, S., Whiteway, J., Willame, Y., Wolff, Michael T., Patel, M., D’aversa, E., Fussen, D., García Comas, Maia, Hewson, W., McConnel, J., Novak, R., Oliva, F., Piccialli, A., Aparicio del Moral, Beatriz, Barzin, P., BenMoussa, A., Berkenbosch, S., Biondi, D., Bonnewijn, S., Candini, G. P., Clairquin, R., Cubas, J., De-Lanoye, S., Giordanengo, B., Gissot, S., Gomez, A., Maes, J., Mazy, E., Mazzoli, A., Meseguer, J., Morales, Rafael, Orban, A., Pastor, Carmen, Perez-Grande, I., Queirolo, C., Saggin, B., Samain, V., Sanz Andres, A., Sanz Mesa, Rosario, Simar, J.-F., Thibert, T., Jerónimo, José María, The NOMAD Team, Belgian Science Policy Office, European Space Agency, Ministerio de Ciencia e Innovación (España), European Commission, UK Space Agency, Agenzia Spaziale Italiana, and Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles)
- Subjects
Mars atmosphere ,Solar occultation ,Visible ,Dust ,Infrared ,Methane ,ExoMars ,Nadir observations ,Spectroscopy ,Composition ,Ultraviolet - Abstract
Open Access This article is distributed under the terms of the Creative Commons Attribution 4.0 International License (http://creativecommons.org/licenses/by/4.0/) The NOMAD (“Nadir and Occultation for MArs Discovery”) spectrometer suite on board the ExoMars Trace Gas Orbiter (TGO) has been designed to investigate the composition of Mars’ atmosphere, with a particular focus on trace gases, clouds and dust. The detection sensitivity for trace gases is considerably improved compared to previous Mars missions, compliant with the science objectives of the TGO mission. This will allow for a major leap in our knowledge and understanding of the Martian atmospheric composition and the related physical and chemical processes. The instrument is a combination of three spectrometers, covering a spectral range from the UV to the mid-IR, and can perform solar occultation, nadir and limb observations. In this paper, we present the science objectives of the instrument and explain the technical principles of the three spectrometers. We also discuss the expected performance of the instrument in terms of spatial and temporal coverage and detection sensitivity.© 2018, The Author(s). The NOMAD experiment is led by the Royal Belgian Institute for Space Aeronomy (IASB-BIRA), assisted by Co-PI teams from Spain (IAA-CSIC), Italy (INAF-IAPS), and the United Kingdom (Open University). This project acknowledges funding by the Belgian Science Policy Office (BELSPO), with the financial and contractual coordination by the ESA Prodex Office (PEA 4000103401, 4000121493), by Spanish MICINN through its Plan Nacional and by European funds under grant ESP2015-65064-C2-1-P (MINECO/FEDER), as well as by UK Space Agency through grants ST/R005761/1, ST/P001262/1, ST/R001405/1 and ST/R001405/1 and Italian Space Agency through grant 2018-2-HH.0. The research was performed as part of the >Excellence of Science> project >Evolution and Tracers of Habitability on Mars and the Earth> (30442502). SA acknowledge support from the FNRS, Be.
- Published
- 2018
50. Photometric-Corrected Albedo Maps of Tethys by Cassini-VIMS
- Author
-
Filacchione, G., Ciarniello, M., D'Aversa, E., Capaccioni, F., Cerroni, P., Buratti, B.J., Clark, R. N., Stephan, Katrin, and Plainaki, C.
- Subjects
VIMS ,Cassini ,Photometrie ,Tethys - Published
- 2018
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