Shack-Hartmann wavefront sensors are commonly used in optical alignment, ophthalmology, astronomy, adaptive optics and commercial optical testing. Wavefront error measurement yields Zernike polynomials which provide useful data for alignment correction calculations. In this thesis a practical alignment method of a helmet visor is proposed based on the wavefront error measurements. The optical system is modeled in Zemax software in order to collect the Zernike polynomial data necessary to relate the error measurements to the positioning of the visor. An artificial neural network based computer program is designed and trained with the data obtained from Zernike simulation in Zemax software and then the program is able to find how to invert the misalignments in the system. The performance of this alignment correction method is compared with the optical test setup measurements.

Las aberraciones ópticas determinan la formación de imágenes en el ojo, tanto en el proceso de la visión como en las observaciones oftalmoscópicas del fondo de ojo. La corrección total de estas aberraciones permitiría una resolución limitada sólo por la difracción en las pupilas utilizadas. Las aberraciones del ojo difieren de un sujeto a otro y no responden a modelos sencillos. En este trabajo se propone el uso de técnicas de Óptica Adaptativa para el desarrollo de un sistema experimental para la medida y corrección de las aberraciones estáticas del ojo. Estas técnicas pueden ser igualmente útiles para obtener imágenes de alta resolución de la retina, utilizarse en el diseño de lentes oftálmicas, etc. Para la medida de la función aberración de onda, se han utilizado dos métodos no invasivos aplicables al ojo humano: La Recuperación de Fase a partir de dos imágenes de Doble Paso, y el Sensor de Hartmann-Shack. Para la corrección de la aberración se ha utilizado un Modulador Espacial de Cristal Líquido.Se han desarrollado los procedimientos de control y de calibrado de estos métodos, y se estudia la viabilidad de aplicación para el ojo. Finalmente, se han realizado medidas de la aberración, mediante ambos métodos, y su posterior corrección mediante el modulador espacial de cristal líquido, en un ojo artificial y en sujetos reales. / The image formation properties of the eye are determined by the aberrations of the optics. The complete correction of the aberrations would allow diffraction-limited resolution. The aberrations of the eye are not easily modeled and are different for each subject.This thesis proposes the use of adaptive optics techniques to measure and correct the static aberrations of the eye. The principles and methods developed are useful in specific applications, i.e., high-resolution retinal imaging, ophthalmic lens design, etc.Two non-invasive methods have been used to measure the wave aberration function: Phase Retrieval Techniques from two double-pass retinal images; and the Hartmann-Shack sensor. A Liquid Crystal Spatial Light Modulator was used to adaptively correct the wave front aberration of the eye.This thesis also includes guidelines to calibrate and control the proposed techniques.Finally, experimental explorations of these methods are reported. Several results are presented, including the measure and the subsequent compensation of the wave aberration for artificial and human eyes.

Understanding and modeling seismic wave propagation is important in regional and exploration seismology. Ray tracing is a powerful and popular method for this purpose. Wavefront construction (WFC) method handles wavefronts instead of individual rays, thereby controlling proper ray density on the wavefront. By adaptively controlling rays over a wavefront, it efficiently models wave propagation. Algorithms for a quasi-P wave wavefront construction method and a new coordinate system used to generate wavefront construction mesh are proposed and tested for numerical properties and modeling capabilities. Traveltimes, amplitudes, and other parameters, which can be used for seismic imaging such as migrations and synthetic seismograms, are computed from the wavefront construction method. Modeling with wavefront construction code is applied to anisotropic media as well as isotropic media. Synthetic seismograms are computed using the wavefront construction method as a new way of generating synthetics. To incorporate layered velocity models, the model based interpolation (MBI) ray tracing method, which is designed to take advantage of the wavefront construction method as well as conventional ray tracing methods, is proposed and experimental codes are developed for it. Many wavefront construction codes are limited to smoothed velocity models for handling complicated problems in layered velocity models and the conventional ray tracing methods suffer from the inability to control ray density during wave propagation. By interpolating the wavefront near model boundaries, it is possible to handle the layered velocity model as well as overcome ray density control problems in conventional methods. The test results revealed this new method can be an effective modeling tool for accurate and effective computing.

In this paper, we present a nonlinear curvelet-based sparsity-promoting formulation for three problems related to seismic noise, namely the ’good’, corresponding to noise generated by random sampling; the ’bad’, corresponding to coherent noise for which (inaccurate) predictions exist and the ’ugly’ for which no predictions exist. We will show that the compressive capabilities of curvelets on seismic data and images can be used to tackle these three categories of noise-related problems.

No description available.

Tese (doutorado)—Universidade de Brasília, Faculdade de Tecnologia, Departamento de Engenharia Elétrica, 2008. / Submitted by Jaqueline Oliveira (jaqueoliveiram@gmail.com) on 2008-12-04T18:50:12Z No. of bitstreams: 1 TESE_2008_JanMendoncaCorrea.pdf: 1697042 bytes, checksum: 1f33d862081703c73ca93cae5ea50d48 (MD5) / Approved for entry into archive by Georgia Fernandes(georgia@bce.unb.br) on 2009-02-12T17:40:49Z (GMT) No. of bitstreams: 1 TESE_2008_JanMendoncaCorrea.pdf: 1697042 bytes, checksum: 1f33d862081703c73ca93cae5ea50d48 (MD5) / Made available in DSpace on 2009-02-12T17:40:50Z (GMT). No. of bitstreams: 1 TESE_2008_JanMendoncaCorrea.pdf: 1697042 bytes, checksum: 1f33d862081703c73ca93cae5ea50d48 (MD5) / O alinhamento de seqüências biológicas é uma das operações mais básicas em bioinformática, tendo por objetivo determinar a similaridade entre as seqüências. A solução deste problema envolve geralmente a comparação de seqüências através de programação dinâmica. Este tipo de comparação gera resultados ótimos mas possui complexidade quadrática de tempo, justificando métodos para sua aceleração em hardware como o FPGA. Na presente tese foram projetadas arquiteturas wavefront em FPGA utilizando espaço linear para três diferentes algoritmos. O primeiro algoritmo foi o de Smith-Waterman. Ele foi implementado na forma de um vetor wavefront e foi utilizado na aceleração da fase inicial de um algoritmo de alinhamento. Esta arquitetura foi capaz de recuperar o maior escore e posição em espaço linear. Esta arquitetura foi sintetizada em FPGA e o melhor resultado da arquitetura foi 246,9 vezes mais rápido que em software, demonstrando a utilidade da arquitetura. A seguir, foi projetada uma arquitetura para a recuperação do escore ótimo do algoritmo de programação dinâmica DIALIGN também em espaço linear. Foram obtidos resultados até 383,41 vezes superiores ao programa em software. Para recuperar o alinhamento ótimo no DIALIGN é necessário espaço quadrático. Assim, foi projetada uma variante do DIALIGN capaz de recuperar o alinhamento de duas seqüências em espaço linear. Após a implementação em hardware, os resultados obtidos foram até 141,38 vezes mais rápido que a implementação em software. ______________________________________________________________________________________ ABSTRACT / The alignment of biological sequences is one of the more basic operations in bioinformatics. Its purpose is to find the similarity between sequences. The solution to this problem generally involves sequence comparison through dynamic programming. This kind of comparison yields optimal results but has quadratic time complexity thus justifying its hardware acceleration in FPGA. In this thesis, linear space wavefront architectures were designed in FPGA for three different algorithms. The first algorithm was Smith-Waterman. It was implemented in a wavefront array and utilized to accelerate the initial phase of a sequence alignment algorithm. This architecture was able to retrieve the largest score and its position in linear space. It was synthesized in FPGA and the best result was 246,9 times faster than software, showing the appropriateness of the architecture. Also, an architecture to retrieve the optimal DIALIGN score in linear space was designed. The results were up to 383,41 times better than software. The retrieval of the optimal alignment for DIALIGN needs quadratic space. Therefore, a variant for the DIALIGN dynamic programming algorithm was proposed to retrieve the alignment in linear space. This variant was implemented in hardware and the results were up to 141,38 times faster than the software implementation.

Neste trabalho foi desenvolvido um novo método voltado para a caracterização de lentes térmicas em materiais fotônicos, utilizados como meios ativos no desenvolvimento de lasers. Este método baseia-se em interferometria por padrão de speckle eletrônico (ESPI), utilizando dois lasers de diodo multímodo sintonizados a diferentes freqüências. Com o ajuste desta diferença, foi possível escolher uma resolução apropriada para medirmos as variações geradas no raio de curvatura da frente de onda, relacionados ao efeito térmico. Para os nossos experimentos escolhemos uma amostra vítrea de aluminato de cálcio dopado com 4% de érbio; e potências de bombeio incidentes de até 1,76 mW do laser de bombeio. Os lasers de diodo foram sintonizados para ter um intervalo de contorno por volta de 120 m. Com o aumento da potência absorvida pela amostra, observamos a diminuição da curvatura da frente de onda incidente na CCD, devido ao aumento da potência da lente térmica gerada. Através de uma análise paraxial dos feixes, foi feita uma aproximação para obtermos os valores das lentes para cada configuração, apresentando comprimentos focais de 131,39 mm a 42,76 mm. / In this work we will develop a new method focused on the caracterization of thermal lenses effect in photonic materials used as active media in lasers design. This method is based on electronic speckle pattern interferometry (ESPI) using two multimode diode lasers tuned to different frequencies. Adjusting this difference we can achieve an appropriate resolution to measure the variability generated within the curvature radius of the wavefront due to thermal lens effect. For our experiments we chose a vitreous sample of calcium aluminate doped with 4% erbium and incident pump powers ranging to 1.76mW. The diode lasers were tuned to have a contour interval of around 120m. With addition in power absorbed by the sample, we observed a decrease in the curvature radius incident on the camera due to increased power of the thermal lens generated. Through a paraxial of the wavefront, an approach was made to obtain the values of the lenses for each configuration, with focal lengths ranging from 131.39 mm to 42.76 mm.

The submicron-aperture fiber point-diffraction interferometer (SFPDI) can be applied to realize the measurement of three-dimensional absolute displacement within large range, in which the performance of point-diffraction wavefront and numerical iterative algorithm for displacement reconstruction determines the achievable measurement accuracy, reliability and efficiency of the system. A method based on fast searching particle swarm optimization (FS-PSO) algorithm is proposed to realize the rapid measurement of three-dimensional absolute displacement. Based on the SFPDI with two submicron-aperture fiber pairs, FS-PSO method and the corresponding model of the SFPDI, the measurement accuracy, reliability and efficiency of the SFPDI system are significantly improved, making it more feasible for practical application. The effect of point-diffraction wavefront error on the measurement is analyzed. The error of point-diffraction wavefront obtained in the experiment is in the order of 1x10(-4). (the wavelength. is 532 nm), and the corresponding displacement measurement error is smaller than 0.03 mu m. Both the numerical simulation and comparison experiments have been carried out to demonstrate the accuracy and feasibility of the proposed SFPDI system, high measurement accuracy in the order of 0.1 mu m, convergence rate (similar to 90.0%) and efficiency have been realized with the proposed method, providing a feasible way to measure three-dimensional absolute displacement in the case of no guide rail.

L’imagerie d’exoplanètes est limitée par deux obstacles intrinsèques : le faible écart angulaire entre planète et étoile, et le très faible flux lumineux en provenance de la planète par rapport à la lumière de l’étoile. Le premier obstacle est surmonté par l’utilisation de très grands télescopes, de la classe des dix mètres de diamètre, et éventuellement depuis le sol de systèmes d’optique adaptative, qui permettent d’atteindre de hautes résolutions angulaires. Le deuxième obstacle est surmonté par l’utilisation de coronographes. Les coronographes sont des instruments conçus pour filtrer la lumière de l’étoile tout en laissant passer la lumière de l’environnement circumstellaire. Cependant, toute aberration optique en amont du coronographe engendre des fuites de lumière stellaire à travers le coronographe. Ces fuites se traduisent par un fouillis de tavelures dans les images scientifiques, tavelures qui cachent d’éventuelles planètes. Il est donc nécessaire de mesurer et de corriger les aberrations quasi-statiques à l’origine des tavelures. Cette thèse présente des contributions théoriques, numériques et expérimentales à la mesure et à la correction des aberrations des imageurs coronographiques. La première partie décrit le contexte et présente la méthode de la diversité de phase coronographique, un formalisme qui considère l’analyse de surface d’onde post-coronographique comme un problème inverse posé dans un cadre bayésien. La deuxième partie concerne l’imagerie depuis le sol. Elle présente tout d’abord une expression analytique permettant de modéliser l’imagerie coronographique en présence de turbulence, puis l’extension de la méthode de diversité de phase coronographique à la mesure depuis les télescopes au sol donc en présence de turbulence résiduelle, et enfin une validation en laboratoire de cette méthode étendue. La troisième partie est consacrée aux futurs imageurs spatiaux à très hauts contrastes pour lesquels il faut corriger non pas seulement la phase mais tout le champ complexe. Elle présente la validation en laboratoire de la mesure d’un champ complexe d’aberrations par diversité de phase coronographique, ainsi que des premiers résultats d’extinction de la lumière en plan focal par une méthode non linéaire, le non-linear dark hole. / Exoplanet imaging has two intrinsic limitations, namely the small angular separation between the star and the planet, and the very low light flux from the planet compared to the starlight. The first limitation is overcome by using very large telescopes of the ten-metre diameter class, and, for ground-based telescopes, adaptive optics systems, which allow high angular resolution imaging. The second limitation is overcome by using a coronagraph. Coronagraphs are optical devices which filter the starlight while granting passage to the light coming from the stellar environment. However, any optical aberration upstream of the coronagraph causes some of the starlight to leak through the coronagraph. This unfiltered starlight in turn causes speckles in the scientific images, and the light of the planets that could be there is lost among the speckles. Consequently, measurement and correction of the quasi-static aberration which generate the speckles are necessary for the exoplanet imagers to achieve their full potential. This thesis introduces theoretical, numerical, and experimental contributions to the topic of measurement and correction of the aberrations in coronagraphic imagers. The first part describes the context and introduces coronagraphic phase diversity, which is a Bayesian inverse problem formalism for post-coronagraphic wave-front sensing. The second part is focused on ground-based imaging. It introduces an analytic expression for coronagraphic imaging through turbulence, the extension of coronagraphic phase diversity to on-sky measurement through residual turbulence, and a laboratory validation of the extended method. The third part is concerned with future high-contrast space-based imagers, which will require not only phase correction, but a full complex wave-front correction. It presents the laboratory validation of coronagraphic phase diversity as a post-coronagraphic complex wave-front sensor, and first results of active contrast enhancement in the focal plane through thecreation of a non-linear dark hole.

When the light passes through optical elements it can cause deformation of wavefront light due to the damage of materials and optical aberrations. The deformation leads to unprecise imaging and deformation of an image. The diploma work mentions wavefront sensing techniques which are important for determination inappropriate errors of optical elements and the specification of their properties. The purpose of the master's thesis is to suggest and investigate wavefront sensing methods after the light passes through the optical element while using the digital micromirror device. The work deals with the topic of wavefront aberrations and geometric optical defects of optical elements. Different kinds of commercial products determined for wavefront sensing are described too.