L’étude du comportement des composantes des intérieurs planétaires dans des conditions extrêmes de pression (megabar) et température (milliers de Kelvin) est essentielle afin de construire des modèles fiables décrivant l’évolution et la structure des planètes. Dans ce travail, nous avons étudié plusieurs composantes par compression par choc laser sur les installations LULI2000 (France) et GEKKO XII (Japon).Nous avons employé des chocs décroissants pour étudier des conditions de haute-pression / haute-température. Afin d’accéder à des conditions de température modérée, nous avons utilisé des techniques de pre-compression statique (couplage compression par choc — cellules à enclumes de diamant) et dynamique (génération de doubles chocs).Nous avons étudié l’équation d’état des mélanges eau-ethanol-ammoniac et de l’eau et ammoniac purs, d’intérêt pour la description des intérieurs des planètes géantes de glace. L’étude de l’ammoniac a été particulièrement délicate en raison de sa forte réactivité et donc de la complexité du design des cibles ; nous présentons les premières données obtenues par choc laser, dans un domaine de pression jamais exploré. Les données des mélanges confirment des calculs ab initio récents basés sur une approximation de mélange linéaire.Nous avons également mesuré la réflectivité des mélanges liquides et de la silice, une composante-clé des intérieurs des planètes terrestres. Nous avons ensuite estimé la conductivité électrique — un paramètre crucial pour modéliser la génération des champs magnétiques planétaires dans les intérieurs via un mécanisme dynamo — de ces composantes.Eau, ammoniac et mélanges eau-ethanol-ammoniac affichent des réflectivités différentes, ce qui suggère que l’eau pure ne peut pas être considérée comme représentative des mélanges planétaires dans les modèles dynamo.Par ailleurs, nous avons apporté une confirmation expérimentale de calculs ab initio récents selon lesquels la conductivité de la silice n’est pas monotone le long d’une ligne isotherme pour des températures modérées.Nos données supportent des calculs qui prédisent qu’une dynamo peut avoir lieu dans les océans de magma dans des super-Terres ainsi que dans la jeune Terre. / Characterising the behaviour of planetary interiors’ components at extreme conditions (megabar pressures, temperatures of a few thousand Kelvin) is essential to build reliable models describing the evolution and structure of planets. In this thesis, we investigated various components on a wide set of conditions using laser-driven shock compression techniques at the LULI2000 (France) and GEKKO XII (Japan) facilities.Single decaying shocks were employed to study high-pressure / high-temperature states. To reach moderate-temperature conditions, closer to planetary interior profiles, we employed static and dynamic pre-compression techniques coupling Diamond Anvil Cells to shock compression and generating double shocks, respectively.We studied the equation of state of water-ethanol-ammonia mixtures and of pure liquid water and ammonia, of interest for icy giant structure models. Pure ammonia measurements have been particularly challenging due to cell design complexity in reason of its reactivity; we provide the first data obtained with laser shocks, in a pressure domain up to now unexplored. Mixtures data are in agreement with recent ab initio calculations based on the linear mixing approximation.We measured the optical reflectivity of liquid mixtures and silica, a key component of rocky planets’ interiors. From reflectivity data we estimated the electrical conductivity of such components — a crucial parameter for modelling the generation of planetary magnetic fields in the interiors via a dynamo mechanism.Water, ammonia, and water-ethanol-ammonia mixtures exhibit different reflectivity (hence conductivity) behaviours as a function of pressure and temperature. This suggests that pure water should not be used in dynamo models as representative of the icy mixtures.Moreover, we provide the first experimental confirmation of recent ab initio studies showing that the conductivity of silica along isothermal lines is not monotonic at moderate temperatures. Our data provide experimental support for the calculations predicting a dynamo action to occur in super-Earths’ and early Earth’s magma oceans.

L'étude de l'injection d'un fluide dans des conditions de hautes pressions reste encore aujourd'hui un challenge. Lorsque la pression critique des fluides est dépassée, l'état supercritique est atteint, faisant disparaître la distinction entre liquide et gaz. Pour ces conditions extrêmes, les données expérimentales sont peu nombreuses et nécessitent d'être consolidées. Dans cette étude, un nouveau banc d'essai a été réalisé au laboratoire CORIA dans le but d'étudier des injections non-réactives d'éthane et de propane dans une atmosphère sub- et supercritique d'azote ou d'hélium. Les données ont été collectées à partir de quatre diagnostics optiques : l'ombroscopie, la DBI, la radiographie et la CBOS. Des informations qualitatives sur la topologie des jets et de leur couche de mélange sont apportées. Des mesures quantitatives de longueur de cœur dense, d'angle d'ouverture et de densité sont complétées par une étude phénoménologique à l'aide de la théorie des mélanges binaires. / Studying a fluid flow under high-pressure conditions through reliable experiments is still nowadays a challenge. When the chamber pressure exceeds the critical pressure of working fluids the supercritical state of matter is reached and the distinction between gas and liquid becomes blurred. For such special conditions, experimental data are scarce and need to be consolidated. In the present study, a new test bench has been designed at CORIA Lab to study the non-reactive injection of ethane and propane into nitrogen or helium under sub- and supercritical conditions. Experimental data are collected from four image-based techniques : shadowgraphy, diffused backlight illumination (DBI), radiography and color background oriented schlieren (CBOS). Qualitative information on topology of the jets and their mixing layer are provided. Quantitative measurements of dense core length, jet spreading angle and density field are supported by a phenomenological study based on binary mixing theory.

Les robots et véhicules autonomes représentent le futur des modes de déplacements et de production. Les enjeux de l’avenir reposent sur la robustesse de leurs perceptions et flexibilité face aux environnements changeant et situations inattendues. Les capteurs stéréoscopiques sont des capteurs passifs qui permettent d'obtenir à la fois image et information 3D de la scène à la manière de la vision humaine. Dans ces travaux nous avons développé un système de localisation, par odométrie visuelle permettant de déterminer la position dans l'espace du capteur de façon efficace et performante en tirant partie de la carte de profondeur dense mais également associé à un système de SLAM, rendant la localisation robuste aux perturbations et aux décalages potentiels. Nous avons également développé plusieurs solutions de cartographie et interprétation d’obstacles, à la fois pour le véhicule aérien et terrestre. Ces travaux sont en partie intégrés dans des produits commerciaux. / Autonomous vehicles and robots represent the future of transportation and production industries. The challenge ahead will come from the robustness of perception and flexibility from unexpected situations and changing environments. Stereoscopic cameras are passive sensors that provide color images and depth information of the scene by correlating 2 images like the human vision. In this work, we developed a localization system, by visual odometry that can determine efficiently the position in space of the sensor by exploiting the dense depth map. It is also combined with a SLAM system that enables robust localization against disturbances and potentials drifts. Additionally, we developed a few mapping and obstacles detections solutions, both for aerial and terrestrial vehicles. These algorithms are now partly integrated into commercial products.

Ce mémoire porte sur l'étude des étoiles naines blanches de type DB, dont le spectre est dominé par les raies d’hélium neutre. Des travaux récents ont révélé que les paramètres physiques mesurés à l'aide de la méthode dite spectroscopique —notamment la température effective et la masse de l'étoile — posaient problème pour ce type de naine blanche. Nous avons dans cette étude réexaminé un des ingrédients essentiels de cette méthode, soit le calcul de profils d'élargissement Stark des raies d'hélium neutre. Ce problème fut abordé il y a 25 ans par notre groupe de recherche en utilisant la théorie standard de l'élargissement Stark. Les profils semi-analytiques calculés dans le cadre de cette théorie considèrent les électrons comme étant dynamiques et les ions statiques. Avec l'amélioration de la puissance numérique des ordinateurs, d’autres groupes de recherche ont grandement amélioré le traitement de l'élargissement Stark en produisant des simulations numériques décrivant en détail la dynamique et les interactions des perturbateurs (ions et électrons) près de l'émetteur (l'atome d'hélium dans notre cas). Ils n'ont cependant généré de tables de profils Stark, applicables au calcul de spectres synthétiques d'étoiles naines blanches, que pour deux raies de l'atome d'hélium. Dans ce mémoire, nous décrivons la conception de notre propre environnement de simulation incluant certains aspects importants considérés dans les travaux précédents (unification du traitement des ions et électrons, correction pour la dynamique des ions, transition de la contribution des électrons à l'élargissement, du coeur aux ailes du profil, intégration numérique de l'opérateur quantique d'évolution temporelle de l'hélium perturbé par un champ électrique fluctuant, correction de Debye pour la corrélation du mouvement des perturbateurs chargés, variation de densité locale et réinjection de particules) afin de mieux représenter l'environnement dynamique de l'atome d'hélium. Des étapes intermédiaires, comme la construction de l'espace de simulation et le modèle quasi-statique, nous ont permis de valider cet espace de simulation ainsi que le respect de la statistique du système. Une fois ces étapes de validation franchies, nous avons produit des grilles de profils Stark pour les deux raies les plus importantes de l'atome d'hélium dans le domaine du visible, soit He ɪ λ4471 et He ɪ λ4922, pour des températures entre 10,000 K et 40,000 K et des densités électroniques entre 1 × 10¹⁴ cm⁻³ et 6 × 10¹⁷ cm⁻³. Une comparaison avec d'autres résultats publiés démontre que nos calculs rivalisent avec les meilleurs profils obtenus dans le domaine des simulations numériques de l'élargissement Stark. L'élaboration de cet outil ouvre la voie à la création d'une nouvelle génération de modèles d'atmosphères de naines blanches qui nous permettra de raffiner l'analyse spectroscopique de ces objets. / This thesis deals with the study of white dwarf stars of the DB type, whose spectrum is dominated by neutral helium lines. Recent work has revealed that physical parameters — namely the effective temperature and the stellar mass — measured using the so-called spectroscopic technique are problematic for this type of white dwarf. In this study, we re-examine one of the essential ingredients of this method, namely the calculation of Stark broadening profiles of neutral helium lines. This problem was addressed 25 years ago by our research group using the standard Stark broadening theory. Semi-analytical profiles calculated under this theory consider electrons as dynamic and ions as static. With the improvement of computer numerical power, other research groups have significantly improved the treatment of Stark brodening by producing numerical simulations describing in detail the dynamics and interactions of the perturbers (ions and electrons) near the emitter (the helium atom in our case). However, they generated Stark profile tables, applicable to the computation of synthetic spectra for white dwarf stars, for only two lines of the helium atom. In this thesis, we describe the creation of our own simulation environment including some important aspects considered in previous work (unification of ion and electron treatment, correction for ion dynamics, transition of the electron contribution to broadening from the core to the wings of the profile, numerical integration of the quantum operator of the time evolution of helium perturbed by a fluctuating electric field, Debye correction for the correlation of the motion of charged perturbers, local density variation and particle reinjection) in order to better represent the dynamical environment of the helium atom. Intermediate steps, such as the construction of the simulation space and the quasi-static model, allowed us to validate this simulation space and the respect of the system statistics. Once these validation steps were completed, we produced grids of Stark profiles for the two most important lines of the helium atom in the optical, namely He ɪ λ4471 et He ɪ λ4922, for temperatures between 10,000 K and 40,000 K and electronic densities between 1 × 10¹⁴ cm⁻³ and 6 × 10¹⁷ cm⁻³. A comparison with other published results shows that our calculations rival the best profiles obtained in the field of numerical simulations of Stark broadening. The development of this tool paves the way for the creation of a new generation of white dwarf atmosphere models that will allow us to refine the spectroscopic analysis of these objects.

No description available.

The warm dense matter regime (WDM), defined by temperatures of a few electron volts and densities comparable with solids, is a complex state of matter where multi-body particle correlations and quantum effects play an important role in determining the overall structure and equation of state. The study of WDM states represents the laboratory analogue of the astrophysical environments found in the cores of planets and in the crusts of old stars, but also has practical applications for controlled thermonuclear fusion. Time resolved X-ray diffraction is used to study the temporal evolution of a sample from solid state towards WDM, either after irradiation with an intense proton/electron beam, in carbon samples, or direct laser illumination, in thin gold nanofoils. The electron-ion equilibration time is extracted through the use of the two-temperature model and in highly excited carbon shown to be longer than previously thought, this is attributed to strong ion-ion coupling screening the interaction (coupled mode theory). Calculation of the dynamic ion-ion structure factor is performed using orbital-free density functional theory (OF-DFT) and shown to compare well with Kohn-Sham DFT in both the static and dynamic cases. Experimental verification of these results is vital and measurement of the microscopic dynamics of warm dense aluminium have been successfully demonstrated through inelastic X-ray scattering. Using the self-seeded beam at the linear coherent light source (LCLS) scattering at a small momentum exchange allowed the first direct measurement of ion acoustic waves in WDM. This data provides the basis for a direct experimental test of many dense plasma theories through direct comparison with the ion-ion dynamic structure factor.

Doctor of Philosophy / Department of Statistics / Weixin Yao / This dissertation contains two projects that are related to varying coefficient models. The traditional least squares based kernel estimates of the varying coefficient model will lose some efficiency when the error distribution is not normal. In the first project, we propose a novel adaptive estimation method that can adapt to different error distributions and provide an efficient EM algorithm to implement the proposed estimation. The asymptotic properties of the resulting estimator is established. Both simulation studies and real data examples are used to illustrate the finite sample performance of the new estimation procedure. The numerical results show that the gain of the adaptive procedure over the least squares estimation can be quite substantial for non-Gaussian errors. In the second project, we propose a unified inference for sparse and dense longitudinal data in time-varying coefficient models. The time-varying coefficient model is a special case of the varying coefficient model and is very useful in longitudinal/panel data analysis. A mixed-effects time-varying coefficient model is considered to account for the within subject correlation for longitudinal data. We show that when the kernel smoothing method is used to estimate the smooth functions in the time-varying coefficient model for sparse or dense longitudinal data, the asymptotic results of these two situations are essentially different. Therefore, a subjective choice between the sparse and dense cases may lead to wrong conclusions for statistical inference. In order to solve this problem, we establish a unified self-normalized central limit theorem, based on which a unified inference is proposed without deciding whether the data are sparse or dense. The effectiveness of the proposed unified inference is demonstrated through a simulation study and a real data application.

Cette recherche s’intéresse à l’usage de deux variables du français traditionnellement décrites comme phonologiques : la liaison et l’élision du schwa. Ces variables sont étudiées au cours d’interactions naturelles entre trois enfants et leurs parents respectifs. Plus précisément, l’objectif de cette thèse est de décrire les particularités du discours adressé à l’enfant (DAE) au niveau de l’usage des variables phonologiques et de mesurer leur impact sur l’émergence de la production de ces mêmes variables chez l’enfant. Après la présentation du cadre théorique d’analyse et de la méthodologie de recueil, de structuration et d’analyse des données, le travail de recherche s’organise en trois parties. La première étude basée sur corpus, descriptive, a deux principaux objectifs. Dans un premier temps, il s’agit de mesurer à quelle variation les jeunes enfants sont exposés au domicile familial. Ensuite, le but est de confronter les résultats des études précédentes sur l’acquisition de la liaison, principalement obtenus à partir de tâches expérimentales, à des données issues de corpus denses d’interactions parent-enfant. Cette étude a notamment permis de relever l’influence de facteurs liés à l’usage, comme la fréquence, sur l’emploi des variables phonologiques. La seconde étude se focalise sur les caractéristiques du DAE. Les résultats présentés démontrent notamment que l’usage des variables phonologiques est modulé en DAE, et ce essentiellement à un stade précoce. Cette modulation s’atténue ensuite au cours du développement linguistique des jeunes sujets. La dernière étude de ce travail de recherche permet de mettre en relation les productions enfantines et parentales. Il apparaît que le développement de la variation phonologique va dans le sens des hypothèses émises par les modèles basés sur l’usage : la variation phonologique est à un stade précoce mémorisée à l’intérieur de constructions spécifiques, particulièrement fréquentes et saillantes dans le DAE. Celles-ci vont ensuite s’abstraire et entrer en concurrence au cours du développement, ces deux phénomènes étant particulièrement sensibles aux facteurs d’usage, notamment la fréquence d’emploi des types et des formes linguistiques. / This study deals with the usage of two French linguistic variables liaison and elision, which are traditionally described as phonological variables. They are studied during natural interactions between three children and their parents. More precisely, the aim of this thesis is to describe the specificities of the child directed speech (CDS) concerning the usage of liaison and elision to measure their impact on the emergence of these phonological variables in the speech of the children. After the presentation of the theoretical context of the study (Usage-Based Models and Construction Grammar) and the methodology used to collect, structure, and analyse the data, the research is divided into three analysis sections. The aim of the first corpus based study, a descriptive one, is twofold. The first objective is to describe the variation to which children are exposed at home. A second objective is to compare the results of previous studies on liaison acquisition, obtained mainly from experimental tasks, with data extracted from dense corpora collected during natural interactions between the children and their parents. In particular, this study shows that usage factors, including the frequency of items, influence the production of phonological variables. The second study focuses on the specificities of CDS. The results show that the usage of phonological variables is modulated in CDS, essentially at an early stage of language acquisition. Then, this modulation attenuates during the child’s development. The aim of the third study is to connect parent’s productions and children’s productions. It appears that the results concerning the development of phonological variation are in step with the assumptions provided by the usage-based models: at an early stage, the variation is memorized into specific constructions, particularly salient and frequent in CDS. Then, these constructions are abstracted and enter into competition with each other during the course of language development. The children’s productions show that these two phenomena are especially sensitive to usage factors, including type and token frequency.

Entre outubro de 2009 e dezembro de 2012, foi realizado estudo no Laboratório de Hidrologia Florestal Walter Emmerich (L.H.F.W.E.), para avaliar o potencial hidrológico dos nevoeiros e a precipitação oculta em ambiente de Floresta Ombrófila Densa Montana, na Serra do Mar, em Cunha, a leste do Estado de São Paulo. Os objetivos específicos da pesquisa foram: 1) avaliar o desempenho de coletores de água de nevoeiro; 2) verificar o potencial de coleta de água de nevoeiro no laboratório; 3) analisar o potencial de coleta de água de nevoeiro em três setores da microbacia experimental D; 4) averiguar a distribuição espacial e temporal de ocorrência dos nevoeiros na microbacia D e 5) estimar a contribuição da precipitação oculta na floresta da microbacia D. Para alcançar os três primeiros objetivos foram usados coletores passivos tipo harpa, nas formas cilíndrica e plana. Para estudar a distribuição de nevoeiros, foram feitas observações diárias de três referências visuais situadas a distâncias conhecidas no interior da microbacia D. O método da medição da precipitação efetiva foi empregado para estimar a precipitação oculta na floresta. Sobre a distribuição espacial e temporal da ocorrência de nevoeiros na microbacia D, os resultados mostraram que os episódios de nevoeiro foram mais comuns à tarde, como decorrência da brisa marítima proveniente do Oceano Atlântico. Para 61,3% do tempo, em média, foi observada a presença de nevoeiro em algum setor da microbacia, com a ocorrência dos nevoeiros diminuindo de montante para jusante da área. No que concerne ao desempenho dos equipamentos, a média de coleta diferiu de coletor para coletor, exceto entre o coletor cilíndrico descoberto e o coletor plano, que interceptaram mais água que os coletores cilíndricos cobertos. O coletor plano foi o único a interceptar água em todos os episódios amostrados. Sobre o potencial de coleta de água de nevoeiros no laboratório, concluiu-se que é reduzido e resulta da combinação de três fatores: a grande ocorrência de nevoeiros de radiação, a curta duração dos ix episódios dos nevoeiros orográficos e a baixa intensidade dos ventos na região. No que concerne ao potencial de coleta de água de nevoeiro em três setores da microbacia D, árvores localizadas próximas aos coletores funcionaram como obstáculo à livre circulação dos nevoeiros orográficos, induzindo os coletores a interceptar exíguos volumes de água. Considerando apenas os eventos de nevoeiro sem chuva, a precipitação oculta foi de 2,3 mm, correspondendo a 0,12% da precipitação pluviométrica anual. Para os eventos de chuva com a presença de nevoeiro, a precipitação oculta gerou um total de 5,1 mm de água adicional ao piso da floresta, correspondendo a 0,27% da precipitação pluviométrica. Concluiu-se que a precipitação oculta na floresta não é um processo importante para a entrada de água na microbacia D. / Between October 2009 and December 2012 a study was conducted at the Walter Emmerich Hydrologic Laboratory (LHFWE) to assess the hydrological potential of fog and occult precipitation in the Montane Dense Ombrophilous Forest environment located in the Parque Estadual da Serra do Mar - Núcleo Cunha, east of the State of São Paulo, Brazil. The specific multiple objectives of the research were: 1) evaluate the performance of passive fog collectors, 2) evaluate the potential for collecting fog water in the laboratory, 3) evaluate the potential of collecting fog water in three sectors of experimental catchment \"D\", 4) determine the spatial and temporal distributions of fog occurrence in catchment \"D\", 5) estimate the contribution of occult precipitation in the rainforest in catchment \"D\". To achieve the first three objectives, cylindrical and flat harp collectors were used. To study the spatial and temporal distributions of fog occurrence, we made daily observations of three visual references located at known distances within the catchment. Net precipitation was measured and used to estimate the occult precipitation in the rainforest. Regarding the spatial and temporal distributions of fog occurrence, the results showed that episodes of fog were more common in the afternoon as a result of the sea breeze from the Atlantic Ocean. For 61.3% of the time on average, we observed the presence of fog in some sector of the catchment, with its occurrence decreasing in areas located from upstream to downstream. Concerning the comparison of the performance of the collectors, the average volume of water collected differed from collector to collector, except between cylindrical collector uncovered and flat collector, which captured more water than the cylindrical collectors covered to prevent rainwater input. The flat collector was the only gauge to intercept water in all episodes. The high incidence of fog radiation, the short duration of orographic fog, and the low intensity of winds combined to reduce the potential for harvesting fog water in the laboratory. Regarding the potential for collecting fog water in three sectors of the catchment \"D\", xi trees located next to collectors operated as an obstacle to the free movement of orographic fog inducing gauges to intercept exiguous volumes of water. Considering only fog, but no rain, occult precipitation was 2.3 mm, corresponding to 0.12% of annual rainfall. For rainfall events with the presence of fog, occult precipitation generated a total of 5.1 mm of additional water to the floor of the forest, equivalent to 0.27% of the rainfall. It was therefore concluded that occult precipitation in rainforest did not significantly contribute to water entering catchment \"D\".

Des nuages moléculaires aux étoiles, l'ensemble des stades d'évolution des étoiles jeunes peuvent être observés dans le domaine submillimétrique. A cette fin, le télescope Herschel a observé, dans le cadre d'un relevé de la Ceinture de Gould, plusieurs nuages moléculaires. Lorsque ces nuages se fragmentent, des coeurs denses, accumulant de la poussière et du gaz, se forment et se contractent. Nous avons effectué un relevé exhaustif des coeurs denses préstellaires dans le nuage moléculaire d'Ophiuchus qui apparaissent couplés avec des structures filamentaires dans le cadre du paradigme de la formation d'étoiles au sein de filaments interstellaires. La région n'était pas connue pour être filamentaire, malgré des alignements de protoétoiles observables. Ce nuage moléculaire présente la particularité d'être soumis à une rétroaction importante venant d'étoiles actives à proximité, visible dans la structure du nuage moléculaire. Oph B-11, mise en évidence par des observations interférométriques, est un précurseur de naine brune, de masse finale trop faible pour que l'étoile produite brûle de l'hydrogène. Leur mécanisme de formation est mal connu. Il faut caractériser et observer un premier candidat pré-naine brune. Oph B-11 a été détectée à proximité d'un choc proche, que nous avons caractérisé chimiquement. De plus, à plus haute résolution avec ALMA, nous avons montré l'environnement moléculaire structuré, contraint le mécanisme de formation de ce type d'objet. Ces observations dévoilent une série de chocs dans plusieurs traceurs, coïncidant avec la détection de la pré-naine brune, favorisant le scénario gravo-turbulent pour la formation des naines brunes. / From molecular clouds to stars, every step of the evolution of young stars can be observed in the submillimetric range. The Herschel Space Telescope observed, as part of the Herschel Gould Belt Survey, many molecular clouds.When these molecular clouds are fragmenting, dense prestellar cores accumulating dust and gaz are forming and contracting. We performed a census of prestellar dense cores in the Ophiuchus Molecular Cloud, which appear to be coupled with filamentary structures, as part of the paradigm of star-formation inside insterstellar filaments. The region was not previously known as filamentary, despite the observation of protostellar alignments.This molecular could is under the heavy feedback of active stars nearby seen in the structure of the molecular cloud.Oph B-11, detected with interferometric observations, is a brown dwarf precursor, which final mass will not be important enough for the final star to burn hydrogen. Their formation mechanism is not well constrained, we must find and characterize a first candidate pre-brown dwarf.Oph B-11 was detected along a nearby shock, we characterize chemically. Moreover, higher resolution studies with ALMA show a structured molecular environment, and help us constrain the mechanism of formation of this kind of objects. These observations show a series of shocks in differents tracers, spatially coincident with the detected position of the pre-brown dwarf, in favor of the gravo-turbulent scenario for the formation of brown dwarfs.