No description available.

<p>I investigate the interstellar medium (ISM) of two nearby, resolved galaxies, M51 (NGC 5194) and Centaurus A (Cen A; NGC 5128) using spectroscopic and photometric data from the <em>Herschel Space Observatory</em> to search for local variations of the characteristics of the ISM. I find that the average characteristics of the ISM in Cen A, a giant elliptical galaxy, are similar to those typically found in normal star forming galaxies, despite its unique morphology and classification as a radio galaxy with an active galactic nucleus (AGN). Using <em>Herschel</em> photometry I find radial trends in the dust temperature, the dust mass, and unexpectedly, the gas-to-dust mass ratio. I hypothesise that the AGN is removing nearby dust grains via dust sputtering or expulsion via jets. A comparison of Herschel spectroscopy of important cooling lines to a photon dominated region (PDR) model reveals the strength of the far-ultraviolet radiation field, <em>G</em>₀, and the hydrogen gas density, <em>n</em>, in the PDR gas within Cen A are consistent with values found in other nearby galaxies. I do not observe any obvious radial trend in these characteristics and conclude that the high inclination of Cen A may be inhibiting the identification of any impact the AGN is having on the surrounding gas.</p> <p>An investigation of the gas in M51 using a similar spectroscopic dataset as with Cen A shows for the first time that a large fraction of the observed [C II](158 μm) emission in the centre of M51 originates in diffuse ionised gas. This fraction falls off with radius out to the arm and interarm regions. I also find via PDR modelling that there is a decreasing radial trend in the values of <em>G</em>₀ and <em>n</em>, and that in the arm and interarm regions they are the same. Thus, there appears to be no difference in the physical properties of the molecular clouds in the arm and interarm regions of the galaxy. The results of this thesis contribute to further understanding the characteristics of the ISM of nearby galaxies, as well as the evolution of the ISM in galaxies containing an AGN.</p> / Doctor of Philosophy (PhD)

Galaxy formation is a complex, nonlinear process that occurs over scales that span orders of magnitude in space and time. Of the many phenomena taking place within a galaxy, supernovae (SN) are among the most important. SN heat, stir, and eject gas from the galaxy. This has profound impact on the galaxy's evolution over cosmic time. Numerical simulations of galaxies must often include models for feedback from SN. We present a new model for SN feedback that captures the effects of previously ignored physics: thermal conduction. Massive stars form in clusters, allowing their SN ejecta to merge into a superbubble, which can vent from the disc to drive a high-entropy galactic outflow. Thermal conduction determines how much mass is mixed into this superbubble. We use this to study SN feedback in galaxy evolution, and come to four major conclusions. First, superbubbles drive stronger galactic outflows in compared to past models of SN feedback. Second, these outflows are key to both preventing the overproduction of stars and the formation of too-massive central bulges. High redshift outflows eject starforming gas, and preferentially remove bulge forming gas. Third, we show that SN cannot prevent runaway star formation in galaxies more massive than our own $(M_{halo}>10^{12}\;\rm{M_\odot})$. In these galaxies, SN are unable to prevent transport of gas towards the centre of the galaxy. These results suggest a transition between regulation from stars to regulation from supermassive black holes occurs at roughly this mass. Finally, we use our simulated galaxies to show recent observations of the Radial Acceleration Relation (RAR) are consistent with $\Lambda$CDM cosmology. The RAR ties galaxy kinematics to baryonic mass, in a tight, universal scaling relation. While this has been claimed as potential evidence of exotic new physics, we show this same tight relation occurs for galaxies formed in $\Lambda$CDM. / Thesis / Doctor of Philosophy (PhD)

Thesis. 1976. Ph.D.--Massachusetts Institute of Technology. Dept. of Earth and Planetary Science. / Microfiche copy available in Archives and Science. / Vita. / Bibliography: leaves 129-133. / by A. Colbert Reisz. / Ph.D.

Polarimetric CCD images of HII regions were obtained using a rotating polarizer device designed, built, and used in conjunction with the Spectral Line Imaging Camera (SLIC) at Virginia Tech's Martin Observatory in Giles County, Virginia. The SLIC uses a narrow bandpass interference filter coupled with a 58 mm camera lens and cryogenically cooled CCD camera to image diffuse, extended H-alpha emission over a 10° angular extent. A rotating polarizer device was placed in front of the H-alpha filter with images recorded at every 45° with respect to a fiducial setting. Stoke's parameters and were obtained and polarization maps of selected HII regions were created. Maps of the Monoceros supernova remnant and the Rosette Nebula (NGC 2237-9) were made in an attempt to detect polarization by selective extinction in H light. While this was not detected, polarization by scattering in a dust shell around the Rosette Nebula (NGC 2237-9) was observed. Scattered continuum light from the central star cluster NGC 2244 in the H-alpha bandpass was ruled out. Using Celnik's (1985) map of extinction across the Rosette Nebula at the H wavelength, coupled with Serkowski's empirical relationship between maximum polarization and color excess, it was shown that the maximum degree of polarization seen in the Rosette Nebula should be no more than 3% to 4%. The polarization observed in this project reaches values as high as 10%. It was found that a correlation exists between the H-alpha intensity and infrared emission by dust grains in all four IRAS waveband images in the suspected scattering region of the Rosette Nebula. A radial comparison between [SII] images and H-alpha images in the region of high polarization showed that the H-alpha intensity in that region is dominated by scattered H-alpha light from the Rosette Nebula. A single scattering model was constructed in an effort to predict the observed polarization. The model used parameters based on 21 cm observations by Kuchar and Bania (1993) of the HI shell which surrounds the HII region of the Rosette Nebula. The single scattering model can not accurately predict the degree of polarization. It was concluded that a multiple scattering model is required. A spatial comparison of the 12 m emission with the degree of polarization strongly suggested that multiple scattering is important in describing the observed radial behavior of polarization. Polarization images of regions in Cygnus were obtained. A polarization map of the North America Nebula (NGC 7000) and surroundings reveals a large amount of polarization. The map reveals that scattering of H-alpha light from the North America Nebula is the most likely cause of polarization in these images. From the analysis in this thesis, I conclude that in the northwest quadrant, at radial distances greater than 40 from the center of the Rosette Nebula, the observed H-alpha intensity is due to scattered H light from the nebula itself. This implies that, in H-alpha , the Rosette Nebula appears slightly larger than it actually is. With evidence of polarization by scattered H supported by the polarization map of the North America Nebula (NGC 7000), it is concluded that other HII regions may very well appear larger in H-alpha than they actually are. Thus, scattered H-alpha light may account for a small part of the more extended warm ionized medium as well. / Ph. D.

De nos jours environ 200 molécules ont été observées dans le milieu interstellaire, environ 75% d'entre elles sont carbonées et 25% sont des hydrocarbures. Les grains de poussières contiennent également du carbone en grande quantité. La présence du carbone dans la majorité des molécules et dans les grains de poussières s'explique par son abondance et sa capacité à former des liaisons. Il est donc crucial de les étudier d'un point de vue astrochimique. Dans une première partie, ce travail présente les mesures des rapports de branchement et des énergies dissipées sous forme d'énergie cinétique dans les fragments neutres lors d'une collision à haute vitesse, des molécules carbonées suivantes : SiC, AlC, AlCH, C ₂ O, CN, CH ₂ et CH. Ces mesures ont été obtenues grâce au dispositif expérimental AGAT. Ce dernier est installé à demeure auprès de l'accélérateur Tandem d'Orsay. Il permet la collision molécule-atome en cinématique inverse et la détection 100% efficace de tous les fragments émis, y compris les neutres. Dans une seconde partie, l'effet de l'ajout ou la correction de nouveaux rapports de branchement d'hydrocarbures est discuté, sur la modélisation de la chimie de deux objets célèbres : la région de photo-dissociation de la nébuleuse de la Tête de Cheval et le nuage moléculaire TMC-1. Ces deux objets sont bien connus pour leur richesse en molécules observées. Ces nouveaux rapports de branchement diminuent les abondances calculées des espèces de la phase gazeuse, déjà trop basses par rapport aux observations. Une hypothèse stipule que des hydrocarbures sont dégagés dans la phase gazeuse via les grains de poussières carbonés. Suite à cette hypothèse, pour la première fois, les effets de l'incorporation de réactions de photo-production d'hydrocarbures par les grains de carbone amorphes hydrogénés ont été étudiés, sur la chimie de la phase gazeuse de la nébuleuse de la Tête de Cheval. L'ajout de ces réactions resserre l'écart entre la modélisation et les observations. / Nowadays, about 200 molecules have been observed in the interstellar medium, about 75% are carbon molecules and 25% hydrocarbons. Dust grains also contain carbon in large quantities. The presence of carbon in the majority of molecules of the gaseous phase and in the dust is due to its abundance and its ability to form bonds. So, it is crucial to study the carbon in an astrochemical point of view.In the first part, this work presents measurements of branching ratios and energy dissipated as kinetic energy in neutral fragments which are emitted in a high speed collision, of the following carbon molecules: SiC, AlC, AlCH, C ₂ O, CN, CH ₂ and CH. These measurements were obtained from the experimental setup AGAT. This setup is permanently installed at the Tandem Orsay facility. It allows molecule-atom collisions and 100% effective detection of all the transmitted fragments, including neutral ones.In the second part, the effect of the addition or correction of new hydrocarbon branching ratios is discussed, by modeling of chemistry of two famous objects: the photo-dissociation region of the Horsehead nebula and the molecular cloud TMC-1. Both objects are well known for their numerous observed molecules. These new branching ratios reduce the calculated abundances of species in the gas phase, even though these abundances were already too low compared to the observations. A hypothesis states that hydrocarbons are released into the gas phase via the carbonaceous interstellar dust. Following this assumption, for the first time, the effects of the incorporation of photo-production reactions of hydrocarbons from the hydrogenated amorphous carbons were studied on the chemistry of the gaseous phase of the Horsehead nebula. The addition of these reactions narrows the gap between modeling and observations.

L'objectif principal de mon travail de thèse est de comprendre les processus qui agissent sur la poussière pendant le couplage entre le milieu interstellaire galactique et le milieu intra-amas. Ce processus est d'intérêt particulier dans les phénomènes violents comme les interactions galaxie-galaxie ou le "Ram Pressure Stripping" causé par la chute d'une galaxie vers le centre de l'amas.Initialement, je me suis concentré sur le problème de la destruction de la poussière et le processus de chauffage, en re-visitant les modèles présents en littérature. J'ai particulièrement insisté sur les cas des environnements extrêmes comme le gaz chaud de type coronale (e.g., IGM, ICM, HIM) et les chocs interstellaires générés par les supernovae. Sous ces conditions les petits grains sont détruits rapidement et les gros grains sont chauffés par les collisions avec les électrons énergétiques, en rendent la distribution spectral d'énergie de la poussière très différente de ce qu'on observe dans le milieu interstellaire diffus.Pour tester nos modèles j'ai les appliqués au cas d'une galaxie en interaction, NGC 4438. Les données Herschel de cette galaxie indiquent la présence de la poussière avec une température plus élevée de ce qu'on s'attendait.Avec une analyse à plusieurs longueurs d'onde on montre que cette poussière chaude semble être dans un gaz ionisé et chaud et donc subir à la fois le chauffage collisionnel et la destruction des petits grains.De plus, je me suis focalisé sur l'énigme de longue date à propos de la différence entre les échelles de temps de destruction et formation de la poussière dans la Voie Lactée. Basées sur l'efficacité de destruction de la poussière dans les chocs interstellaires, les estimations précédentes portent à une durée de vie de la poussière plus courte que l'échelle de temps typique de sa formation dans les étoiles AGB. En utilisant un modèle de poussière récent et les dernières estimations pour l'évolution de la poussière, on a réévalué la durée de vie de la poussière dans notre Galaxie. Finalement, j'ai tourné mon attention au phénomène de "Ram Pressure Stripping''. La galaxie ESO 137-001 représente un des meilleurs cas pour étudier cet effet. Sa longue queue H2 intégrée dans une queue de gaz chaud et ionisé soulève des questions sur son possible arrachement de la galaxie ou sa formation en aval dans la queue. Basé sur des récentes simulations numériques, j'ai montré que la formation des molécules de H2 sur la surface des grains dans la queue est un scénario viable. / The main goal of my PhD study is to understand the dust processing that occurs during the mixing between the galactic interstellar medium and the intracluster medium. This process is of particular interest in violent phenomena such as galaxy-galaxy interactions or the "Ram Pressure Stripping'' due to the infalling of a galaxy towards the cluster centre.Initially, I focus my attention to the problem of dust destruction and heating processes, re-visiting the available models in literature. I particularly stress on the cases of extreme environments such as a hot coronal-type gas (e.g., IGM, ICM, HIM) and supernova-generated interstellar shocks. Under these conditions small grains are destroyed on short timescales and large grains are heated by the collisions with fast electrons making the dust spectral energy distribution very different from what observed in the diffuse ISM.In order to test our models I apply them to the case of an interacting galaxy, NGC 4438. Herschel data of this galaxy indicates the presence of dust with a higher-than-expected temperature.With a multi-wavelength analysis on a pixel-by-pixel basis we show that this hot dust seems to be embedded in a hot ionised gas therefore undergoing both collisional heating and small grain destruction.Furthermore, I focus on the long-standing conundrum about the dust destruction and dust formation timescales in the Milky Way. Based on the destruction efficiency in interstellar shocks, previous estimates led to a dust lifetime shorter than the typical timescale for dust formation in AGB stars. Using a recent dust model and an updated dust processing model we re-evaluate the dust lifetime in our Galaxy. Finally, I turn my attention to the phenomenon of "Ram Pressure Stripping''. The galaxy ESO 137-001 represents one of the best cases to study this effect. Its long H2 tail embedded in a hot and ionised tail raises questions about its possible stripping from the galaxy or formation downstream in the tail. Based on recent hydrodynamical numerical simulations, I show that the formation of H2 molecules on the surface of dust grains in the tail is a viable scenario.

A Pequena Nuvem de Magalhães (PNM) é uma galáxia irregular e rica em gás, que juntamente com a Grande Nuvem de Magalhães (GNM) orbita a Via Láctea (VL). Elas formam um sistema triplo em constante interação. A PNM possui metalicidade baixa, e consequentemente seu meio interestelar (MI) apresenta propriedades particularmente diferentes das observadas para o MI da Galáxia. Mais do que isso, a importância do campo magnético em escalas galácticas vem sendo evidenciada cada vez mais. Então, o objetivo desta dissertação foi estudar a estrutura do campo magnético na PNM, e sua relação com componentes do MI desta galáxia. Para este fim, utilizamos dados de polarimetria no óptico, obtidos no Cerro Tololo Inter American Observatory. Construímos um catálogo polarimétrico que contém 7.207 estrelas em 28 campos distribuídos nas secções Nordeste e da Asa da PNM. Os mapas de polarização traçam o campo magnético no plano do céu diretamente, e pode-se obter sua intensidade utilizando o método de Chandrasekhar & Fermi. A partir do catálogo polarimétrico gerado neste trabalho, conseguimos observar que o campo magnético na PNM possui direção bastante irregular, porém é provável a existência de dois padrões em larga escala o primeiro alinhado com a Ponte pan-Magelânica e o segundo alinhado com a Barra da PNM. Obtivemos para o campo magnético regular Bcéu = (1,84 ± 0,11) uG e para o campo turbulento dB = (2,920 ± 0,098) uG. Esse resultado evidencia que na PNM o campo aleatório domina com relação ao de larga escala, justificando a observação de uma configuração tão irregular para os vetores de polarização. Correlacionando os mapas de polarização com estruturas presentes no MI da PNM, pudemos verificar a presença de diversos shells que podem possuir campos magnéticos da ordem de algumas dezenas de uG. Também foi possível observar ambientes onde o campo regular parece ter sido destruído pela turbulência e outros onde ele pode ainda não ter tido tempo de se formar. Derivamos a relação entre polarização e avermelhamento, e obtivemos como resultado que ela é da ordem de P/Av ~ 2, o que indica que na PNM a eficiência para polarização pode ser menor do que na Galáxia, talvez devido a alta turbulência e/ou ao fato de que nela o campo regular é muito baixo. Por fim, a partir da estimativa para as densidades de energia do campo magnético e para o movimento de rotação e de turbulência do gás, pudemos mostrar que o campo magnético possui importância dinâmica para PNM, sendo a componente turbulenta a maior responsável pela pressão magnética. / The Small Magellanic Cloud (SMC) is a gas rich irregular galaxy which, together with the Large Magellanic Cloud (LMC), orbit the Milky Way (MW). They form a triple system in constant interaction. The SMC is a metal poor galaxy and, due to this, its interstellar medium (ISM) presents different properties from the Galaxy\'s ISM. In addition to that, the importance of magnetic fields on galactic scales is being recognized nowadays. Therefore, the aim of this project was to study the magnetic field structure of the SMC and its relationship with other components of SMC\'s ISM. For this purpose we have used starlight optical polarimetric data, obtained at Cerro Tololo Inter-American Observatory. We have constructed a polarization catalog containing a total of 7,207 stars in 28 fields in the Northeast/Wing sections of the SMC. The polarimetric vector maps trace the ISM magnetic field component in the plane of the sky and one can estimate its intensity towards a given region using the Chandrasekhar & Fermi method. Making use of the polarimetric catalog from this work, we have found that the magnetic field in the SMC, although varying from region to region, nevertheless shows two large scale patterns - the first one aligned with the Magellanic Bridge and a second one aligned with the SMC\'s Bar. We derived for the regular sky-projected magnetic field a value of Bsky = (1.84 ± 0.11) uG, and for the turbulent magnetic field dB = (2.920 ± 0.098) uG. These results evidence that in the SMC the random field prevails over the large scale field, which explains the irregular configuration of the polarization vectors often seen. Correlating the polarization maps with structures present on the SMC\'s ISM, we could identify the presence of several shells which may have magnetic fields up to a few tens uG. It was also possible to observe environments where the regular field seems to have been destroyed due to turbulence, and others where it seems that the large scale magnetic field has not enough time to be formed. Studying the relationship with polarization and reddening, we have obtained a value for P/Av ~ 2, which may indicate that the polarization efficiency in the SMC is smaller than in the Galaxy, perhaps due to a higher turbulence and/or because of a smaller regular magnetic field. Lastly, we have estimated the energy density for the magnetic field and for the rotation and turbulent gas motions. We showed that the magnetic field is dynamically important in the SMC\'s ISM, and that the turbulent component is the largest contributor to the magnetic pressure.

Os cianopoliinos (HCnN, n = 1, 3, 5, ...) e seus isômeros, os isocianopoliinos (HCn-1NC), constituem duas famílias de moléculas já identificadas no meio interestelar. No intuito de auxiliar a detecção e investigar a formação destas moléculas neste ambiente, foram obtidas as geometrias, as constantes rotacionais, os momentos de dipolo, as frequências vibracionais e as intensidades fundamentais de infravermelho em níveis MP2/cc-pVTZ (n = 1 a 17), CCSD/cc-pVDZ (n = 1 a 13) e CCSD/cc-pVTZ (n = 1 a 7). Além disso, foi empregado o modelo de partição em carga - fluxo de carga - fluxo de dipolo, CFCFD, em termos dos multipolos atômicos advindos da Teoria Quântica de Átomos em Moléculas, QTAIM, para compreender os efeitos do tamanho da cadeia sobre as propriedades elétricas destas moléculas, como suas intensidades de infravermelho. Os resultados indicam que o nível CCSD/cc-pVTZ é o que melhor descreve as propriedades mencionadas para os menores cianopoliinos e isocianopoliinos. Contudo, devido à demanda computacional, é preciso optar entre os níveis MP2/cc-pVTZ e CCSD/cc-pVDZ para abordar espécies maiores. Assim, os momentos de dipolo destes maiores cianopoliinos são mais bem descritos pelo nível MP2/cc-pVTZ, enquanto CCSD/cc-pVDZ é mais indicado para tal propriedade em respectivos isocianopoliinos. Por sua vez, as intensidades de infravermelho destas famílias apresentam melhor concordância com dados experimentais quando determinadas em nível CCSD/cc-pVDZ. Além disso, tanto para cianopoliinos quanto para isocianopoliinos, o aumento do tamanho das cadeias resulta num incremento das intensidades do estiramento CH, o que é explicado por variações no fluxo de carga eletrônica. O estiramento das ligações triplas CC centrais é o modo mais intenso em grandes cianopoliinos, o que também se deve ao fluxo de carga observado. Ademais, o espectro dos isocianopoliinos apresenta um número maior de bandas relevantes na região de estiramento de ligações triplas CC. Um estudo também foi conduzido, onde foram estimados os dados termodinâmicos, as geometrias do estado de transição e as constantes de velocidade da reação HCnN &rarr; HCn-1NC (n = 1 a 9) para temperaturas entre 298,15 e 3000 K. Os níveis B3LYP/aug-cc-pVsZ, MPW1K/aug-cc-pVsZ (s = Q) e CCSD(T)/aug-cc-pVmZ (m = T e Q) foram adotados em um tratamento composto para as reações com n = 1, 3 e 5, enquanto as reações com n = 7 e 9 foram investigadas de forma semelhante, porém com s = T e m = D e T. O método B3LYP foi o que apresentou melhor desempenho comparado ao MPW1K na determinação de frequências e geometrias. Os resultados indicam que esta reação é exotérmica no sentido em que os cianopoliinos são formados e, portanto, é mais fácil de ocorrer em ambientes mais frios do meio interestelar. Por outro lado, suas constantes de velocidade no sentido direto e inverso tendem a ser de mesma magnitude em temperaturas elevadas, indicando que estes ambientes mais quentes são mais propícios para detecção de isocianopoliinos. Por fim, equações parametrizadas foram ajustadas para reproduzir nossos dados de constantes de velocidade das reações com n = 1 até 9 dentro do intervalo de temperaturas considerado. / Cyanopolyynes (HCnN, n = 1, 3, 5, ...) and their isomers, isocyanopolyynes (HCn-1NC), constitute two families of molecules already identified in the interstellar medium. In order to provide data for their detection and to investigate the formation of these molecules in this environment, geometries, rotational constants, dipole moments, vibrational frequencies and infrared fundamental intensities were obtained at MP2/cc-pVTZ (n = 1 to 17), CCSD/cc-pVDZ (n = 1 to 13) and CCSD/cc-pVTZ (n = 1 to 7) levels. Furthermore, the partition model in charge - charge flux - dipole flux, CFCFD, from atomic multipoles given by the Quantum Theory of Atoms in Molecules, QTAIM, was applied to understand the effects of chain size on electrical properties of these molecules, such as intensities. Results indicate that the best description of the properties mentioned is achieved at the CCSD/cc-pVTZ level for smaller cyanopolyynes and isocyanopolyynes. However, due to computational demand, one needs to choose between MP2/cc-pVTZ and CCSD/cc-pVDZ levels to deal with larger species. In this sense, the dipole moments of large cyanopolyynes are better described by the MP2/cc-pVTZ level, while CCSD/cc-pVDZ is indicated for such property in respective isocyanopolyynes. In addition, the infrared intensities of both families from CCSD/cc-pVDZ calculations are in better accordance with experimental data. Moreover, chain size increases of cyanopolyynes and isocyanopolyynes result in intensity increments of CH stretching, which is explained by electronic charge flux changes. The stretching of central CC triple bonds is the strongest mode for large cyanopolyynes and this is also due to charge flux. A study was also conducted, in which thermodynamic data, transition state geometries and rate constants of the reaction HCnN &rarr; HCn-1NC (n = 1 to 9) were estimated for temperatures between 298.15 and 3000 K. B3LYP/aug-cc-pVsZ, MPW1K/aug-cc-pVsZ (s = Q) and CCSD(T)/aug-cc-pVmZ (m = T and Q) were adopted in a combined treatment for reactions with n = 1, 3 and 5, while reactions with n = 7 and 9 were investigated in a similar way, but with s = T and m = D and T. Frequencies and geometry data from the B3LYP method exhibited a better performance than MPW1K. The results indicated that this reaction is exothermic in the direction that leads to cyanopolyynes, and therefore it is easier to occur in colder environments of the interstellar medium. On the other hand, rate constants of forward and reverse reactions tend to show the same magnitude at higher temperatures, indicating these warmer environments are more amenable to detection of isocyanopolyynes. Finally, parameterized equations were fitted to reproduce our rate constant data for reactions with n = 1 to 9 in the temperature range considered.

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.