Neste trabalho são apresentados os resultados obtidos no desenvolvimento de um sistema especificado para realizar testes na caracterização de dispositivos fotodetectores como fotodiodos de avalanche. O sistema de ensaios elaborado pretende auxiliar com na caracterização da fotodetecção em dispositivos de acoplamento de cargas com multiplicação de elétrons (EMCCD). O objetivo deste trabalho é avaliar o desempenho dos dispositivos fotodetectores para caracterizar os parâmetros mais significativos no processo da transdução óptica de modo a colaborar no projeto da eletrônica embarcada de controle e leitura da informação contida no EMCCD. A tecnologia da multiplicação dos elétrons em dispositivos CCD e diodos de avalanche têm aplicações importantes na vigilância de ambiente de luminosidade reduzida, astronomia, além de outras aplicações de imagens científicas incluindo as de baixo nível de bioluminescência para identificação de drogas e aplicações da engenharia genética. Para efeito de avaliação do desempenho do sistema fotodetector foi necessário desenvolver uma infra-estrutura para ter controle adequado da temperatura de operação do EMCCD. Foram nomeadas as opções com uma montagem de resfriamento com células Peltier e uma opção por criogenia resfriada com nitrogênio líquido. Os resultados obtidos são úteis na detecção de sinais luminosos ultrafracos minimizando o ruído do detector na aquisição de imagens com o auxilio da instrumentação de um filtro óptico sintonizável que será integrado no telescópio SOAR de 4 metros, instalado no Chile, para observações melhoradas com óptica adaptativa. / This work presents the results obtained in the development of a system specified to perform tests in the characterization of photo-detectors devices such as avalanche photodiodes. The test system is prepared to contribute to the characterization of the photo-detection in charge-coupled devices with electron multiplication (EMCCD). The objective of this study is to evaluate the performance of photo-detectors devices to characterize the most significant parameters in the optic transduction in order to collaborate in the project of an embedded electronic system for controlling and reading the information contained with the EMCCD. The technology of the electron multiplication in CCD devices and avalanche diodes has important applications in monitoring the environment of low light, astronomy and other scientific imaging applications including the low level of bioluminescence for the identification of drugs and applications of genetic engineering. For purposes of assessing the performance of the photo-detector it was necessary to develop an infrastructure to have proper control of the operating temperature of the EMCCD. Options were named with a montage of Peltier cell cooling and a choice of cryogenically cooled with liquid nitrogen. The results are useful in the detection of ultra weak light signals while minimizing detector noise during the acquisition of images from instrument comprising an optical tunable filter, that will be integrated into SOAR 4 meters telescope, installed in Chile, for observations improved with adaptive optics.

This thesis investigates various active control aspects of large aperture telescopes; both Earth-based and space telescopes are considered.The first part proposes a concept of piezoelectric adaptive thin shell reflector for future space telescopes; it exhibits excellent areal density and stowability, and thus, paves the way to future large aperture space telescopes. Controlling the surface figure of spherical or parabolic shell with in-plane stresses induced by a piezoelectric layer raises two problems: (i) Doubly curved shells are significantly stiffer than flat plates (especially for the optical modes associated with hoop strains) and (ii) When using segmented electrodes with different voltages, the surface figure is subject to edge fluctuations with a characteristic length depending on the reflector curvature R_c and thickness t according to sqrt(R_ct). Accurate surface figure corrections require that the electrode size D_e satisfies D_e<sqrt(R_ct). This results in a very large number of electrodes, leading to ill-conditioning in the Jacobian matrix of the system; to solve this, a hierarchical approach is proposed to inverse the Jacobian, based on Saint-Venant's principle. This chapter also proposes a petal configuration which aims at reducing the hoop stiffness and improving the foldability of the reflector. A small scale technology demonstrator has been manufactured in the framework of the ESA-GSTP project Multilayer Adaptive Thin Shell Reflectors for Future Space Telescopes (MATS). The demonstrator includes a polymer substrate (PEEK) and a spin-coated PVDF-TrFE piezoelectric layer activated by independent electrodes; it is used to validate the manufacturing process and the independent actuation of the electrodes.The second part deals with control-structure interaction in flat deformable mirrors for Adaptive Optics. The problem arises because of the increasing size of AO mirrors, leading to lower resonance frequencies, and the control bandwidth requirements to achieve a good wavefront error compensation. This chapter studies the conditions for spillover instability and highlights the main parameters controlling the phenomenon: the ratio between the control bandwidth and the resonance frequency and the modal damping. Two methods for damping augmentation are discussed, one passive, using inductive shunting of piezoelectric elements, and the other active, using the wavefront sensor and the array of control actuators as a modal filter.The third part focuses on the field stabilization control of the tip/tilt mirror under wind disturbances of the E-ELT telescope (a distinctive feature of the E-ELT as compared to other smaller telescopes is that it will be a wind-limited instead of a seeing-limited telescope). A literature survey is conducted of the spectral content of the wind disturbances on large telescopes, with a special attention on the high frequency decay rate. The analysis confirms the adequacy of a decoupled design of the field stabilization (M5) control loop. However, the reaction torques necessary to control the tip/tilt mirror M5 have been found to depend critically on the asymptotic decay rate of the wind tilt disturbance. These torques act as a disturbance on the telescope structure and, if the wind disturbance does not decay fast enough with the frequency (a>-3), it may generate significant wavefront errors in the primary mirror M1, in a frequency range (30-100Hz) which may be difficult to eliminate by Adaptive Optics. / Doctorat en Sciences de l'ingénieur et technologie / info:eu-repo/semantics/nonPublished

Neste trabalho são apresentados os resultados obtidos no desenvolvimento de um sistema especificado para realizar testes na caracterização de dispositivos fotodetectores como fotodiodos de avalanche. O sistema de ensaios elaborado pretende auxiliar com na caracterização da fotodetecção em dispositivos de acoplamento de cargas com multiplicação de elétrons (EMCCD). O objetivo deste trabalho é avaliar o desempenho dos dispositivos fotodetectores para caracterizar os parâmetros mais significativos no processo da transdução óptica de modo a colaborar no projeto da eletrônica embarcada de controle e leitura da informação contida no EMCCD. A tecnologia da multiplicação dos elétrons em dispositivos CCD e diodos de avalanche têm aplicações importantes na vigilância de ambiente de luminosidade reduzida, astronomia, além de outras aplicações de imagens científicas incluindo as de baixo nível de bioluminescência para identificação de drogas e aplicações da engenharia genética. Para efeito de avaliação do desempenho do sistema fotodetector foi necessário desenvolver uma infra-estrutura para ter controle adequado da temperatura de operação do EMCCD. Foram nomeadas as opções com uma montagem de resfriamento com células Peltier e uma opção por criogenia resfriada com nitrogênio líquido. Os resultados obtidos são úteis na detecção de sinais luminosos ultrafracos minimizando o ruído do detector na aquisição de imagens com o auxilio da instrumentação de um filtro óptico sintonizável que será integrado no telescópio SOAR de 4 metros, instalado no Chile, para observações melhoradas com óptica adaptativa. / This work presents the results obtained in the development of a system specified to perform tests in the characterization of photo-detectors devices such as avalanche photodiodes. The test system is prepared to contribute to the characterization of the photo-detection in charge-coupled devices with electron multiplication (EMCCD). The objective of this study is to evaluate the performance of photo-detectors devices to characterize the most significant parameters in the optic transduction in order to collaborate in the project of an embedded electronic system for controlling and reading the information contained with the EMCCD. The technology of the electron multiplication in CCD devices and avalanche diodes has important applications in monitoring the environment of low light, astronomy and other scientific imaging applications including the low level of bioluminescence for the identification of drugs and applications of genetic engineering. For purposes of assessing the performance of the photo-detector it was necessary to develop an infrastructure to have proper control of the operating temperature of the EMCCD. Options were named with a montage of Peltier cell cooling and a choice of cryogenically cooled with liquid nitrogen. The results are useful in the detection of ultra weak light signals while minimizing detector noise during the acquisition of images from instrument comprising an optical tunable filter, that will be integrated into SOAR 4 meters telescope, installed in Chile, for observations improved with adaptive optics.

L’ELT (Extremely Large Telescope), est un télescope de diamètre 39 m en cours de réalisation par l’Observatoire Européen Austral (ESO). Pour pouvoir tirer pleinement parti de sa taille, ses instruments seront équipés de systèmes d’Optique Adaptative (OA) qui compenseront la turbulence atmosphérique. Ces systèmes d’OA requièrent l’utilisation d’étoiles guides laser afin de maximiser la couverture du ciel. Les étoiles guides laser sont générées par laser accordé sur une résonance d’atome de sodium présents dans une couche d’une épaisseur de 10 km et située à environ 90 km d’altitude. Une étoile laser est donc un cylindre lumineux dans la haute atmosphère, allumé par la relaxation des atomes. L’analyse de front d’onde à l’aide de ces étoiles artificielles souffrent de limitations connues. De plus, sur un télescope de la taille de l’ELT, leur utilisation est compliquée par l’effet de perspective qui provoque un allongement de l’étoile guide lorsqu’elle est vue d’un point éloigné de son point de lancement au sol : le cylindre n’est plus vu par une section circulaire, mais sur le côté. Sur un télescope de 39m, l’élongation de l’étoile peut alors atteindre jusqu’à 20 secondes d’arc, à comparer avec le diamètre du cylindre qui est déterminé par la turbulence, soit de l’ordre d’une seconde d’arc. La variabilité de l’épaisseur, de l’altitude et de la distribution de densité de la couche de sodium ont alors un impact sur la mesure du front d’onde.L’étude de ce problème, qui porte à la fois sur les algorithmes de mesure et le design des analyseurs de front d’onde, a donné lieu à de nombreux travaux s’appuyant sur des simulations et des tests en laboratoire. Le but de cette thèse a été d’étudier cette question à l’aide de données expérimentales obtenues sur le ciel. Ces données ont été enregistrées grâce au démonstrateur d’OA CANARY, situé sur le télescope William Herschel sur l’île de la Palma aux Canaries. CANARY a été développé par le LESIA, en collaboration avec l’Université de Durham; le laser et son télescope d’émission ont été fournis et opéré par l’ESO. Lors de cette expérience, l'allongement extrême des étoiles laser qui sera observé sur l'ELT a été reproduit en plaçant le télescope d’émission à environ 40m du télescope William Herschel. Le front d'onde a ensuite été mesuré sur l’étoile laser allongée ainsi crée.Les travaux effectués pendant cette thèse ont consisté en la préparation de l’instrument et en particulier de l’analyseur de front d’onde de l’étoile laser, la réalisation des observations et le traitement des données résultant de ces dernières. L’analyse de ces données a permis de construire un budget d’erreur de la mesure de front d’onde sur étoile laser allongée. Grâce à ce budget d’erreur, les performances de différents algorithmes de mesure ont été comparées, ainsi que leur comportement face à la variabilité du profil de sodium et des conditions de turbulence. Enfin, différentes configurations d’analyseurs ont été extrapolées, ce qui a permis d’établir des limites sur leur design dans le cadre de l’ELT. / The ELT (Extremely Large Telescope) is a telescope whose diameter is 39 m currently under construction by the European Southern Observatory (ESO). In order to fully benefit from its size, ELT instruments will be equipped with Adaptive Optics (AO) systems to compensate the atmospheric turbulence. These AO systems require the use of Laser Guides Stars (LGS) in order to have as large a sky coverage as possible. LGS are generated using a laser tuned on a resonant frequency of sodium atoms contained in a layer approximately 90km high and 10 km thick. Therefore, a LGS is a luminous cylinder in the high atmosphere, lighted by sodium atoms relaxation. Wavefront sensing on these artificial stars suffers from known limitations. On a telescope the size of the ELT, their use is further complicated by the perspective effect which causes an elongation of the LGS when it is seen from a point distant from its launch position : the cylinder is no longer seen by its circular section, but on the side. On a 39m telescope, the elongation can reach up to 20 arcseconds, which is large compared to to the diameter of the cylinder determined by the turbulence, that is about 1 arcsecond. Variability of the thickness, height and density distribution of the sodium layer then have an impact on wavefront sensing. The study of this problem, which concerns both sensing algorithms and wavefront sensor design, has already been the subject of many work relying on simulations and laboratory experiments. This thesis aims at studying this question using experimental data obtained on sky. These data were acquired using the AO demonstrator CANARY, placed on the William Herschel Telescope (WHT) on the island of La Palma in the Canaries Island. CANARY was developed by LESIA in collaboration with Durham University; the laser and its launch telescope were supplied and operated by ESO. In this experiment, the extreme elongation of LGS as will be seen on the ELT was reproduced by placing the launch telescope 40 m away from the William Herschel Telescope. The wavefront was the measured on the elongated LGS thus created. The studies led during this thesis consisted in the preparation of the instrument and in particular the LGS Wavefront Sensor (WFS), the realisation of the observations and processing on the data obtained. Analysis of these data allowed to build an error breakdown of wavefront sensing on the elongated LGS. Thanks to this error breakdown, performances of different measurement algorithms where compared, as well as their behaviour according to the variability of the sodium profile and the turbulence conditions. Finally, different wavefront sensor designs were extrapolated which allowed to establish limits on their designs for the ELT.

The purpose of this research was to investigate detect and monitor laser-tissue interactions at threshold and potentially sub-threshold levels of injury. High resolution imaging modalities can provide a deeper understanding of candidate biomarkers disease and injury at the molecular, cellular, and tissue-levels which can be used to identify and diagnose early stages disease and damage. In addition, multi-scale and multi-modal imaging have also been used to identify inherent biomarkers of retinal disease and injury. Monitoring tissue changes can be mapped back to biological changes at the cellular and sub-cellular level. Diseases often alter tissue on the ultra-structural level yet retinal clinical diagnosis often monitor changes in tissue at the organ level. If injury and disease is detected and diagnosed during an “early” stage of development, treatments and drug interventions may prevent further spread of the pathology. Non-invasive imaging is expected to be a valuable tool for in vivo medical research as well as for the diagnosis and management of disease. In addition to developing new imaging tools and techniques to image the retina, the identification of inherent biomarkers of disease and health using diagnostic methods are almost equally as important. Using the inherent optical properties of retinal tissue, we can non- invasively quantify differences in the absorption and reflection of light to gauge the risk for visual disability or worse yet irreversible vision loss as a result of retinal disease and chronic light exposure. The research presented with in this dissertation is three separate studies aimed at identifying light injury and potential biomarkers indicating the risk of light mediated development of disease. / text

The thesis details the design and characterization of an innovative optical tweezer system. Optical tweezers provide a relatively new technique for non-contact manipulation of micron-scale particles. They employ a laser beam to hold such particles at the laser’s focus. Optical tweezers are used for many scientific purposes, such as: measuring the mechanical properties of bio-molecules, cell and molecule sorting, stiction-less micro-manipulators, and fundamental research in physics. Typically, trap location has been controlled using steer-mirrors or spatial light modulators, operating without beam quality feedback. Here, an innovative trap control system has been developed, featuring a closed-loop adaptive optics system. The prototype system employs a deformable mirror and wavefront sensor to control trap position in three dimensions, while simultaneously removing beam aberrations. The performance of this system is investigated in terms of controllable range of trap motion, trap stiffness, and trap position stability.

In the last decade, adaptive optics systems have been implemented on all the major ground based telescopes and have proven reliable tools for correcting the image to near the diffraction limit. However, the correction from these systems is limited to a narrow field of view. This dissertation address the challenges of widening the corrected field of single conjugate adaptive optics by properly using statistical information on the optical turbulence profile of the atmosphere above the telescope, and by optimizing the trade-off between image quality and field of view. Altair is the facility adaptive optics system for the 8-meter Gemini North telescope and marks the historical beginning of wide field adaptive optics. Its performance evaluation in Part One is the first on-sky comparison of sparse field images from an altitude-conjugated and a ground-conjugated deformable mirror. All of the other basic aspects of Altair's performance are characterized for use by the Gemini community to plan observations. We also study and report. on techniques for extrapolating the edge of the deformable mirror, a critical step in altitude-conjugated mode. In Part Two we develop a point spread function model for Ground Layer Adaptive Optics (GLAO) that is based on analytic forms of the phase power spectral density. This model has been used for feasibility studies of GLAO on Gemini, and the Thirty Meter Telescope (TMT), currently the most advanced extremely large telescope project. The TMT will be an adaptive telescope that has science goals for the huge 81 square arcminute field of the Wide Field Optical Spectrograph (WFOS). We will show that WFOS-GLAO provides useful gains and will operate in the very wide GLAO (VWGLAO) regime, which has no additional overhead for seeing improved operation. To identify the VWGLAO regime we use statistical turbulence profile models and examine anisoplanatism in terms of image quality metrics relevant to the science that GLAO will likely assist. The VWGLAO regime is where there are useful gains over the theoretical seeing limit for wide field science that measure data collection efficiency as proportional to the product of image quality and the field of view (solid angle). We also show that for many cases VWGLAO will not be impacted by lag anisoplanatism nor by wavefront sensor noise.

Nous allons assister au cours de la prochaine décennie, à la première lumière des nouveaux Extremely Large Telescopes. Leur grande taille (de 25 à 39 m de diamètre) permet d’augmenter à la fois leur sensibilité et leur résolution angulaire. Cependant, la résolution angulaire d'un télescope terrestre, est toujours limitée par la turbulence atmosphérique. Pour pallier à ce problème, les grands télescopes sont désormais équipés d'instruments d’Optique Adaptative (OA). L’OA est une technique qui permet d’analyser les effets de la turbulence et de les compenser en temps réel à l’aide de miroirs déformables. En complément, la plupart des télescopes de la génération 8-10 m sont maintenant équipés de systèmes d’étoiles lasers qui permettent d’augmenter la proportion du ciel pouvant bénéficier d’une correction par OA: on parle alors d'Optique Adaptative Grand Champ (OAGC). Malgré les excellentes performances de ces systèmes, la correction apportée aux images reste partielle et des résidus de correction limitent encore leur qualité. Pour extraire les meilleurs résultats scientifiques des images issues de l'OAGC, il est donc essentiel d'optimiser les outils de réduction et d'analyse de données. La première partie de cette thèse détaille une analyse astrophysique de données OAGC ayant pour but d'étudier la formation des étoiles massives dans un environnement extra-galactique. Au delà des résultats scientifiques nouveaux, cette étude a permis de mettre en évidence les termes d'erreur limitant l'analyse scientifique de données OAGC. La seconde partie de cette thèse est dédiée au développement d'un nouvel outil de correction de la distorsion permettant de réduire ces termes d'erreurs. / The next decade will see the first light of the new Extremely Large Telescopes. Their large diameter (from 25 to 39 meters across), increases both their sensitivity and their angular resolution. However, angular resolution of all sizes ground-based telescope is always strongly limited by the atmospheric turbulence. To tackle this problem and fully exploit their capabilities, large optical telescopes are now indissociable of their Adaptive Optics (AO) instruments. AO is a technic that consists in analyzing the effects of turbulence on the wavefront and compensating for it in real time, thanks to one or several deformable mirrors in order to restore the initial angular resolution of optical telescopes. In addition, most of the 8-10 meters telescopes are supplied with laser guide stars systems in order to increase the portion of the sky that can benefit for such an AO correction. Such systems are called Wide Field AO (WFAO). However, despite the excellent performance of such systems, the correction performed is not perfect and some residuals still limit the image quality. In order to get the best science results out of the WFAO images, dedicated and optimized reduction and analyses tools are needed. The first part of this document present an astrophysics analyses of WFAO images aiming to study massive star formation in an extra-galactic environment. In addition to new science results, the study carried out on these observations has enable to highlight the critical parameters that limit the scientific analyses of Wide Field AO data. The second part of this document is dedicated to the development of a new distorsion correction tool that aims to reduce these error terms.

Les télécommunications optiques en espace libre sont capables d'autoriser des débits de plusieurs dizaines de gigabits par seconde. Pour traiter ces débits en bénéficiant des techniques développées dans le cadre de l'optique fibrée, il est souhaitable d'injecter le faisceau reçu dans une fibre monomode. Ainsi, l'optique adaptative est proposée pour limiter les pertes d'injection induites par la dégradation de la qualité du faisceau propagé à travers la turbulence atmosphérique.Dans ce travail nous considérons un lien entre un satellite et une station de réception au sol. En élévation haute lorsque les perturbations d'amplitude peuvent être moyennées en augmentant la taille de la pupille la correction de la phase par optique adaptative (OA) classique peut être suffisante. Mes travaux dans ce cadre portent sur la mise en œuvre expérimentale de l'optimisation du couplage entre un système d'OA classique et une fibre monomode, en corrigeant les aberrations différentielles entre la voie de mesure de la surface d'onde et la voie d'injection du signal corrigé par OA. Le travail accompli dans l'objectif de cette mise en œuvre, se résume par les tâches suivantes : Définition d'une méthode d'optimisation automatique de l'injection par contrôle d'un seul miroir déformable pour la correction conjointe des perturbations rapides de la phase et des aberrations différentielles quasi-statiques ; Étude numérique de l'implantation de la méthode définie par simulation end-to-end ; Mise en œuvre de la méthode en laboratoire sur le banc BOA en modélisant la turbulence atmosphérique par des écrans de phase en rotation et validation du fonctionnement de l'optimisation de l'injection en boucle fermée ; Application de la méthode sur le banc ODISSEE à l'OCA puis fermeture de la boucle sur un signal optique émis par le satellite japonais SOCRATE.Par ailleurs, le lien satellite doit être opérationnel sur une durée maximale. Pour cela, le système doit fonctionner même dans le cas où le satellite est bas sur l'horizon et donc lorsque la portion d'atmosphère traversée par le faisceau est épaisse. Dans ces conditions particulières, les perturbations induites par les fluctuations de l'indice de l'air sont plus fortes que pour l'observation astronomique, donc la correction simultanée de la phase et de l'amplitude est indispensable pour atteindre le taux d'injection désiré (> 50 %). La deuxième partie de la thèse se place dans ce cadre et est consacrée à l'étude de l'implantation expérimentale d'une approche innovante de la correction de la phase et de l'amplitude fondée sur l'utilisation d'un Mach-Zehnder en optique intégrée. Le travail réalisé dans cette partie comporte les points suivants : Élaboration du principe de la correction par un Mach-Zehnder et proposition d'un dispositif généralisé à N voies ; Étude analytique de la correction par le dispositif proposé ; Développement d'un algorithme de contrôle fondé sur l'architecture proposée en optique intégrée ;• Validation numérique du fonctionnement par simulation end-to-end ; Conception d'un prototype pour la validation expérimentale du concept. / Free space optical communications are able to allow rates of several tens of gigabits/s. In order to process these flows and benefit from the techniques developed in the context of fiber optics, it is desirable to inject the received beam into a single mode fiber. In this case, adaptive optics is proposed to limit the injection losses induced by the degradation of the beam quality caused by the atmospheric turbulence.In this thesis, we consider a link between a satellite and a ground receiving station.For high elevations when amplitude perturbations can be averaged by increasing the size of the pupil and the correction of the phase is sufficient by conventional adaptive optics (AO), this work deals with the experimental implementation of the coupling optimization between a conventional AO and a single mode fiber, by correcting the non common path aberrations between the measurement path of the wave front and the injection path of the corrected signal. The accomplished work in this context is summarized by the following tasks: definition of an automatic injection optimization method by controlling a single deformable mirror for the parallel correction of fast phase disturbance and quasi-static differential aberrations; numerical study of the implementation of the proposed method defined end-to-end simulations ; implementation of the method in the laboratory on the BOA bench, modeling the atmospheric turbulence by rotating phase screens, and validation of the injection optimization in closed loop ; application of the method on the ODISSEE bench at the OCA and closing of the loop on a laser signal emitted by the Japanese satellite SOCRATE.Besides, the link must be operational for a maximum duration. Indeed, the system must operate even when the satellite is low on the horizon and, therefore, when the crossed portion of atmosphere is thick. In these particular conditions, the disturbances induced by the air index fluctuations are stronger than for astronomical observations, so that, the simultaneous correction of the phase and the amplitude is essential to reach the desired injection ratio (> 50 %). Based on this analysis, the second part of this thesis focuses on the study of the experimental implementation of an innovative approach of a phase and amplitude correction based on using an integrated Mach-Zehnder. The work done in this part consists in the following points : elaboration of correction principle by a Mach-Zehnder and proposition of a generalized device with N channels ; theoretical analysis of the superposition by the proposed device ; development of a control algorithm based on the architecture proposed in integrated optics ; numerical validation of operation by end-to-end simulations ; design of the prototype for the experimental validation of the concept in the laboratory.

L'hippocampe, structure cérébrale située dans le lobe temporal, est au coeur de la gestion de nombreuses fonctions cognitives comme l'encodage des informations spatiotemporelles ou encore la mémoire épisodique. A l'heure actuelle, l'hippocampe est étudié via de nombreuses méthodes notamment l'imagerie de fluorescence qui, utilisée sur des animaux éveillés, permet d'accéder au fonctionnement du réseau neuronal. Malgré cela, une sous-région : le gyrus denté a encore un rôle mal élucidé car profondément enfoui dans le cerveau. Son étude permettrait d'apporter de nouveaux éléments sur le fonctionnement de l'hippocampe. De part sa profondeur d’environs 1 mm, son imagerie demeure très difficile. En effet, la diffusion ainsi que les aberrations optiques introduites par les couches successives de matière dégradent fortement la qualité d'imagerie. Pourtant l'optique adaptative, une technique héritée de l'astronomie, pourrait changer cela. En l'intégrant à un microscope bi-photon, il serait possible de compenser les aberrations optiques introduites par le cerveau et ainsi d'arriver à effectuer l'imagerie in vivo du gyrus denté. Durant ma thèse, j'ai donc travaillé à la conception complète tant du point de vue matériel que logiciel d'un microscope bi-photon adapté à l'imagerie in vivo et équipé d'un dispositif de correction de front d'onde. J'ai également développé une méthode d'optimisation prometteuse basée sur l'approche modale de la correction des aberrations optiques couplée à l'utilisation d'une métrique adaptée à l'imagerie non-linéaire en profondeur. Enfin, j'ai pu appliquer cette méthode dans des conditions in vitro et in vivo permettant de montrer son efficacité. / The hippocampus, a cortical structure located in the temporal lobe, is at the heart of the management of many cognitive functions such as spatiotemporal information encoding or episodic memory. At present, the hippocampus is studied through many methods including fluorescence imaging, and used on awake animals, allows access for the study of the neural network function. Despite this, a sub-region: the dentate gyrus has still a poorly elucidated role because it is deeply buried in the brain. His study would bring new elements on the hippocampus functioning. Due to its depth of about 1 mm, its imagery remains very difficult. Indeed, scattering as well as optical aberrations introduced by the successive layers of matter strongly degrade the imaging quality. Yet adaptive optics, a technique inherited from astronomy, could change that. By integrating it into a bi-photon microscope, it would be possible to compensate optical aberrations introduced by the brain and thus to achieve the in vivo imaging of the dentate gyrus. During my PhD, I worked on the complete design both in hardware and software of a bi-photon microscope suitable for in vivo imaging and equipped with a wavefront correction device. I also developed a promising optimization method based on the modal approach of optical aberration correction coupled with the use of a metric adapted to nonlinear depth imaging. Finally, I was able to apply this method in in vitro and in vivo conditions to show its effectiveness.