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Supplemental material, sj-pdf-2-jhs-10.1177_17531934211027499 for Hyperselective neurectomy for the treatment of upper limb spasticity in adults and children: a prospective study by Caroline Leclercq, Anne Perruisseau-Carrier, Mathilde Gras, Paolo Panciera, Camillo Fulchignoni and Marcello Fulchignoni in Journal of Hand Surgery (European Volume)

Supplemental material, sj-pdf-1-jhs-10.1177_17531934211027499 for Hyperselective neurectomy for the treatment of upper limb spasticity in adults and children: a prospective study by Caroline Leclercq, Anne Perruisseau-Carrier, Mathilde Gras, Paolo Panciera, Camillo Fulchignoni and Marcello Fulchignoni in Journal of Hand Surgery (European Volume)

International audience

International audience

Since the Rosetta mission arrived at the comet 67P/Churyumov-Gerasimenko (67/P C-G) on August 2014, the comet nucleus has been mapped by both OSIRIS (Optical, Spectroscopic, and Infrared Remote Imaging System), and VIRTIS (Visible Infrared Thermal Imaging Spectrometer) acquiring a huge quantity of surface's images and spectra, producing the most detailed maps at the highest spatial resolution of a cometary nucleus. The OSIRIS imaging system (NAC & WAC) has a set of filters at different wavelengths from the ultraviolet (269 nm) to the near-infrared (989 nm). The OSIRIS imaging system has been the first instrument with the capability to map a comet surface at a high resolution reaching a maximum resolution of 11cm/px during the closest fly-by on February 14, 2015 at a distance of about 6 km from the nucleus surface while the VIRTIS spectro-imager (with two channels M and H) operates from 0.25 to 5m with medium and high spectral resolution. The spectral analysis on global scale from the VIRTIS data indicates that the nucleus presents different terrains covered by a very dark and dehydrated organic-rich material [1]. OSIRIS images indicate a morphologically complex and dark surface with a variety of terrain types and several intricate features [2]. The surface shows albedo variation and from the spectrophotometric analysis a large heterogeneity on the surface properties [3, 4, 5]. Limited evidences of exposed H2O ice have been found on the surface of 67/P C-G up to now [6, 7, 8], even though ices are considered to be a major constituent of cometary nuclei. The aim of this work is, taking advantage of the high resolution of the OSIRIS images, i) to detect the bright spots at all dimensions by albedo and spectral slope analyses, ii) to select those spots which could be resolved by VIRTIS and iii ) to deeply analyse the corresponding spectra. The OSIRIS analysis has been carried out on the colours and spectrophotometry of the whole 67/P C-G nucleus from images acquired since the first Rosetta bound orbits in August 2014 up to the end of 2015. The bright spots are spread everywhere on the surface. The analysis of the VIRTIS spectra on the selected positions by OSIRIS allowed us to detect eight spots with positive H2O ice signatures detection. The obtained results with the computed models will be presented and discussed. References : [1] Capaccioni et al. 2015. Science 347, DOI: 10.1126/science.aaa0628 [2] Sierks et al. 2015. Science 347, DOI: 10.1126/science.aaa1044 [3] Fornasier et al. 2015. A&A, 583, A30 [4] Ciarniello et al., 2015, A&A, 583, A31 [5] Oklay et al. 2016. A&A 586, A80 [6] Pommerol et al. 2015. A&A, 583, A25 [7] De Sanctis et al. 2015. Nature 525, 500 [8] Filacchione et al. 2016. Nature 529, 368.

Since the Rosetta mission arrived at the comet 67P/Churyumov-Gerasimenko (67/P C-G) on July 2014, the comet nucleus has been mapped by both OSIRIS (Optical, Spectroscopic, and Infrared Remote Imaging System, [1]) NAC (Narrow Angle Camera) and WAC (Wide Angle Camera) acquiring a huge quantity of surface’s images at different wavelength bands, under variable illumination conditions and spatial resolution, and producing the most detailed maps at the highest spatial resolution of a comet nucleus surface. 67/P C-G’s nucleus shows an irregular bi-lobed shape of complex morphology with terrains showing intricate features [2, 3] and a heterogeneity surface at different scales.

There is a high degree of diversity among the physical properties of asteroids and comets, known as the « small bodies » of the Solar System. In the next years several space missions will be dedicated to the physical characterization and the return of samples from primitive asteroids or to the study of the nature of an object that would have an impact with our planet. Due to the great number of objects which will never be visited by a space mission, ground based observations will be complementary to space missions. During my Ph.D. I focused on the physical characterization of two classes of Near-Earth Asteroids : i) Potentially Hazardous Asteroids (PHAs) and ii) low-delta V asteroids, easily accessible for future missions. For PHAs in particular the derived physical parameters are fundamental to model the future dynamical evolution and asses the mitigation technologies to be used in case of impact with the Earth. I also analyzed the physical properties of the target of the Dawn mission, Vesta and Ceres. Vesta is considered the parent body of the basaltic material (V-type) in the Solar System. In order to characterize the mineralogy of basaltic material I analyzed visible and near-infrared spectra for a sample of 115 V-type asteroids and I compared them with Dawn data, which orbited around Vesta in 2011-2012. I performed a mineralogical characterization of two quadrangles of Vesta, Bellicia and Floronia. I also lead a spectroscopic observational campaign at TNG to characterize Ceres’surface. I interpreted the extreme variability found as an effect of the outgassing activity on the surface of Ceres.; Un haut niveau de diversité est présent parmi les propriétés physiques des astéroïdes et des comètes, collectivement connus comme les petits corps du Système Solaire. Dans les prochaines années plusieurs missions spatiales seront dédiées à la caractérisation physique et au retour d'un échantillon provenant d'un astéroïde primitive, ou à l'étude de la nature d'un objet qui pourrait avoir un impact avec notre planète. Dans ce contexte, les observations au sol seront complémentaires aux missions spatiales. Pendant mon doctorat je me suis concentré sur la caractérisation physique de deux classes de géocroiseurs potentielles cibles des missions spatiales: i) les astéroïdes potentiellement dangereux (PHAs) et ii) les géocroiseurs facilement accessible de la Terre. Pour les PHAs surtout, les paramètres physiques dérivés sont fondamentaux pour modéliser l'évolution dynamique, et évaluer les technologies d'atténuation à utiliser en cas de risque d'impact avec la Terre. J'ai aussi étudié les propriétés physiques des cibles de la mission Dawn, Vesta et Cérès. Vesta a été considéré comme le corps parent du matériel basaltique (de type V) dans le système solaire. Pour caractériser la minéralogie du matériel basaltique j'ai analysé les données spectroscopiques dans les canaux visibles et proche infrarouge d'un grand échantillon de 115 astéroïdes de type V et je les ai comparé avec les données récupérées par la mission Dawn, qui a orbité autour de Vesta en 2011-2012. J'ai conduit une campagne d'observation spectroscopique au TNG pour caractériser la surface de Cérès. J’ai interprété l'extrême variabilité trouvée comme une éventuelle activité de dégazage à la surface de Cérès.

There is a high degree of diversity among the physical properties of asteroids and comets, known as the « small bodies » of the Solar System. In the next years several space missions will be dedicated to the physical characterization and the return of samples from primitive asteroids or to the study of the nature of an object that would have an impact with our planet. Due to the great number of objects which will never be visited by a space mission, ground based observations will be complementary to space missions. During my Ph.D. I focused on the physical characterization of two classes of Near-Earth Asteroids : i) Potentially Hazardous Asteroids (PHAs) and ii) low-delta V asteroids, easily accessible for future missions. For PHAs in particular the derived physical parameters are fundamental to model the future dynamical evolution and asses the mitigation technologies to be used in case of impact with the Earth. I also analyzed the physical properties of the target of the Dawn mission, Vesta and Ceres. Vesta is considered the parent body of the basaltic material (V-type) in the Solar System. In order to characterize the mineralogy of basaltic material I analyzed visible and near-infrared spectra for a sample of 115 V-type asteroids and I compared them with Dawn data, which orbited around Vesta in 2011-2012. I performed a mineralogical characterization of two quadrangles of Vesta, Bellicia and Floronia. I also lead a spectroscopic observational campaign at TNG to characterize Ceres’surface. I interpreted the extreme variability found as an effect of the outgassing activity on the surface of Ceres., Un haut niveau de diversité est présent parmi les propriétés physiques des astéroïdes et des comètes, collectivement connus comme les petits corps du Système Solaire. Dans les prochaines années plusieurs missions spatiales seront dédiées à la caractérisation physique et au retour d'un échantillon provenant d'un astéroïde primitive, ou à l'étude de la nature d'un objet qui pourrait avoir un impact avec notre planète. Dans ce contexte, les observations au sol seront complémentaires aux missions spatiales. Pendant mon doctorat je me suis concentré sur la caractérisation physique de deux classes de géocroiseurs potentielles cibles des missions spatiales: i) les astéroïdes potentiellement dangereux (PHAs) et ii) les géocroiseurs facilement accessible de la Terre. Pour les PHAs surtout, les paramètres physiques dérivés sont fondamentaux pour modéliser l'évolution dynamique, et évaluer les technologies d'atténuation à utiliser en cas de risque d'impact avec la Terre. J'ai aussi étudié les propriétés physiques des cibles de la mission Dawn, Vesta et Cérès. Vesta a été considéré comme le corps parent du matériel basaltique (de type V) dans le système solaire. Pour caractériser la minéralogie du matériel basaltique j'ai analysé les données spectroscopiques dans les canaux visibles et proche infrarouge d'un grand échantillon de 115 astéroïdes de type V et je les ai comparé avec les données récupérées par la mission Dawn, qui a orbité autour de Vesta en 2011-2012. J'ai conduit une campagne d'observation spectroscopique au TNG pour caractériser la surface de Cérès. J’ai interprété l'extrême variabilité trouvée comme une éventuelle activité de dégazage à la surface de Cérès.