Thesis (MScEng)--Stellenbosch University, 2011. / ENGLISH ABSTRACT: A new type of wideband lters, with tunability in both the centre frequency and bandwidth, is presented in this thesis. These lters are based on perturbed ring-resonators in cascade, while varactor diodes are used for electronic tuning. The Karoo Array Telescope (KAT-7) requires a front-end lter that has the ability for ne-tuning the response after fabrication, in order to obtain the designed ltering response. Not only are tune-all characteristics required, but also wide bandwidth, at passband, high selectivity and implementation in microstrip technology. In this thesis an extensive investigation of both tunable and wideband lters is done, in order to nd a possible solution for the KAT-7 speci cations. Following this investigation, it is concluded that no suitable design approach for tune-all wideband lters, implemented in microstrip, exists in current literature. Therefore, this thesis proposes a new type of lter along with the development of a complete design procedure. Two lters are designed with this procedure to achieve the required passband from 1.2 to 1.95 GHz (i.e. a fractional bandwidth of 49%). In the rst lter design, with a network consisting of 4 cascaded ltering-sections, the centre frequency is 5% tunable and the bandwidth 17.5%. With the second lter consisting of 6 cascaded ltering-sections, higher selectivity is achieved but with lower return loss. Here the centre frequency is 8.5% tunable and the bandwidth 18.8%. The theoretical results are validated with the fabrication of both lters. This design is very unique in that it achieves wide bandwidth, is realisable in microstrip and most importantly is tunable in both the centre frequency and bandwidth. An advantage of this design procedure is that full wave simulations are minimal, due to the complete circuit models used for optimisation. / AFRIKAANSE OPSOMMING: 'n Nuwe soort van wye-band lters, met verstelbaarheid in beide senter frekwensie en bandwydte, word voorgelê in hierdie tesis. Hierdie lters is gebaseer op versteurde ringresoneerders in kaskade, terwyl varaktordiodes gebruik word vir elektroniese verstelling. Die Karoo Array Telescope (KAT-7) vereis 'n voorkant lter wat die vermoë het vir die instemming van die respons na fabrikasie, sodat die geontwerpde lter respons behaal kan word. Nie net word verstel-als eienskappe vereis nie, maar ook wye bandwydte, plat deurlaatband, hoë selektiwiteit en implimentering in mikrostrook tegnologie. In hierdie tesis is 'n veelomvattende ondersoek gedoen van beide verstelbare en wyeband lters, sodat 'n moontlike oplossing vir die KAT-7 spesi kasies gevind kan word. Na aanleiding van hierdie ondersoek, is die gevolgtrekking dat daar geen gepaste ontwerp benadering vir verstel-als wye-band lters, wat geïmplimenteer is in mikrostrook, in huidige literatuur bestaan nie. Daarom stel hierdie tesis, saam met die ontwikkeling van 'n volledige ontwerp prosedure, 'n nuwe tipe lter voor. Twee lters is ontwerp met hierdie prosedure om die vereiste deurlaatband vanaf 1.2 tot 1.95 GHz (dit is 'n fraksionele bandwydte van 49%) te behaal. In die eerste lter ontwerp, met 'n netwerk wat uit 4 kaskade lter-seksies bestaan, is die senter frekwensie 5% verstelbaar en die bandwydte 17.5%. Met die tweede lter bestaande uit 6 kaskade lter-seksies, word hoër selektiwiteit behaal maar met laer eggoverswakking. Hier is die senter frekwensie 8.5% verstelbaar en die bandwydte 18.8%. Die teoretiese resultate is geldig bewys deur die fabrikasie van albei lters. Hierdie ontwerp is baie uniek in dat dit wye bandwydte behaal, is realiseerbaar in mikrostrook en mees belangrikste dat dit verstelbaar is in beide senter frekwensie en bandwydte. 'n Voordeel van hierdie prosedure is dat heelgolf simulasies minimaal is, a.g.v. die volledige stroombaan modelle wat gebruik word vir optimering.

Dark matter is now accepted as an integral part of our universe, and galaxy dynamics have long provided the most convincing observational evidence for dark matter. Spiral galaxies have traditionally been used for these studies because of their more simple kinematics, however elliptical galaxies need to be understood as well. In this dissertation I present deep long-slit spectroscopy from the University of Texas’ Hobby-Eberly Telescope for a sample of elliptical galaxies. For a subsample of galaxies I fit axisymmetric orbit-superposition models with a range of dark halo density profiles. I find that all three galaxies modeled require a significant dark halo to explain their motions. However, the shape of the dark halo is not the expected NFW profile, but rather a profile with a flat central slope. I also discuss the galaxy masses, anisotropies, and stellar mass-to-light ratios. / text

L’imagerie 3γ est une technique innovante d’imagerie médicale nucléaire qui est étudiée au laboratoire SUBATECH. Elle repose sur la localisation tridimensionnelle d’un radioisotope émetteur (β+, γ), le 44Sc, à l’aide d’un télescope Compton au xénon liquide. Le lieu de désintégration de ce radioisotope est obtenu par l’intersection de la ligne de réponse, construite à partir de la détection des deux photons de 511 keV issus de l’annihilation d’un positron, et du cône déterminé à partir du troisième photon. Un prototype de petite dimension XEMIS1 (XEnon Medical Imaging System) a été développé afin de faire la preuve expérimentale de la faisabilité de l’imagerie à 3γ. Les résultats de ce prototype sont très promoteurs en terme de résolution en énergie, de pureté du xénon liquide et de faible bruit électronique. La simulation Monte Carlo est un outil indispensable pour accompagner la R&D et évaluer les performances de la nouvelle technique d’imagerie proposée. Les travaux rapportés dans cette thèse concernent le développement de la simulation du système d’imagerie 3γ avec GATE (Geant4 Application for Tomographic Emission). De nouvelles fonctionnalités ont été implémentées dans GATE afin de simuler un détecteur de type TPC (Time Projection Chamber). Nous avons effectué une simulation du prototype XEMIS1 et obtenu des résultats en bon accord avec nos données expérimentales. La prochaine étape du projet consiste à construire une caméra cylindrique au xénon liquide pour l’imagerie du petit animal. Les résultats des simulations de cette caméra présentés dans cette thèse montrent la possibilité de localiser chaque désintégration le long de la ligne de réponse avec une très bonne précision et une bonne sensibilité de détection. Des premières images de fantômes simples, réalisées évènements par événements, et après reconstruction tomographiques ont également présentées. / Nuclear medical 3γ imaging is an innovative technique which is studied at the SUBATECH laboratory. It isbased on the three-dimensional localization of a (β+, γ) radioisotope emitter, the 44Sc, by using a liquid xenon Compton telescope. The position of the disintegration of this radioisotope is obtained by the intersection of the line of response, built by the detection of two 511 keVphotons from the annihilation of a positron, and the cone determined by the third photon. A small prototype XEMIS1 (XEnon Medical Imaging System) was developed to demonstrate experimentally the feasibility of 3γ imaging. The results of this prototype are quite encouraging in terms of energy resolution, purity of liquid xenon and electronic noise. The Monte Carlo simulation is an indispensable tool to support the R&D and to evaluate the new proposed technique of imaging ; this thesis work is to develop the simulation of 3γ imaging system by using GATE (Geant4 Application for Tomographic Emission). New functionalities have been added to GATE to simulate a TPC (Time Projection Chamber) detector. We performed a simulation of XEMIS1 prototype and obtained results in good agreement with our experimental data. The next step of the project is to build a full liquid xenon cylindrical camera for the small animal imaging. The results presented in this thesis of the simulations of this camera demonstrate the ability to locate every decayalong the line of response with very good accuracy and good detection sensitivity. The first direct images of simple phantoms, realized event by event, and after tomographic reconstruction are also presented.

Le besoin tant en haute qualité d'imagerie qu'en structures légères est l'un des principaux moteurs pour la conception des télescopes spatiaux. Un contrôle efficace du front d'onde va donc devenir indispensable dans les futurs grands observatoires spatiaux, assurant une bonne performance optique tout en relâchant les contraintes sur la stabilité globale du système. L'optique active consiste à contrôler la déformation des miroirs, cette technique peut être utilisée afin de compenser la déformation des grands miroirs primaires, afin de permettre l'utilisation d'instrument reconfigurable ou afin de fabriquer des miroirs asphériques avec le polissage sous contraintes. Dans ce manuscrit, la conception de miroirs actifs dédiés à l'instrumentation spatiale est présentée. Premièrement, un système compensant la déformation d'un grand miroir allégé dans l'espace est conçu et ses performances sont démontrées expérimentalement. Avec 24 actionneurs, le miroir MADRAS (Miroir Actif Déformable et Régulé pour Applications Spatiales) effectuera une correction efficace du front d'onde dans un relais de pupille du télescope. Deuxièmement, un harnais de déformation pour le polissage sous contraintes des segments du télescope géant européen de 39 m (E-ELT) est présenté. La performance du procédé est prédite et optimisée avec des analyses éléments finis et la production en masse des segments est considérée. Troisièmement, deux concepts originaux de miroirs déformables avec un nombre minimal d'actionneurs ont été développés. VOALA (Variable Off-Axis parabola) est un système à trois actionneurs et COMSA (Correcting Optimized Mirror with a Single Actuator) est un système à un actionneur. / The need for both high quality images and light structures is one of the main driver in the conception of space telescopes. An efficient wave-front control will then become mandatory in the future large observatories, ensuring the optical performance while relaxing the specifications on the global system stability. Consisting in controlling the mirror deformation, active optics techniques can be used to compensate for primary mirror deformation, to allow the use of reconfigurable instruments or to manufacture aspherical mirror with stress polishing. In this manuscript, the conception of active mirrors dedicated to space instrumentation is presented. Firstly, a system compensating for large lightweight mirror deformation in space, is designed and its performance are experimentally demonstrated. With 24 actuators, the MADRAS mirror (Mirror Actively Deformed and Regulated for Applications in Space) will perform an efficient wave-front correction in the telescope's pupil relay. Secondly, a warping harness for the stress polishing of the 39 m European Extremely Large Telescope segments is presented. The performance of the process is predicted and optimized with Finite Element Analysis and the segments mass production is considered. Thirdly, two original concepts of deformable mirrors with a minimum number of actuators have been developed. The Variable Off-Axis parabola (VOALA) is a 3-actuators system and the Correcting Optimized Mirror with a Single Actuator (COMSA) is a 1-actuator system.

Os aglomerados globulares (GCs) são laboratórios essenciais no estudo da formação e evolução quimiodinâmica da Via Láctea, pois formaram-se durante os episódios iniciais de formação estelar das galáxias. Na última década, evidências observacionais fotométricas e espectroscópicas têm desafiado o paradigma clássico da formação dos GCs em um episódio único de formação estelar, dando origem ao debate sobre as múltiplas populações estelares. Com o objetivo de explorar esse fenômeno, o programa do Telescópio Espacial Hubble GO-13297 (UV Legacy Survey of Galactic Globular Clusters, PI G. Piotto) obteve fotometria para 57 GCs com os filtros UV/azul F275W, F336W e F438W (WFC3/UVIS), sensíveis às variações nas abundâncias de CNO e, portanto, capazes de distinguir múltiplas populações ao longo dos diagramas cor-magnitude. Combinados com fotometria anterior nos filtros do óptico F606W e F814W (programa GO-10775, PI A. Sarajedini), eles formam uma base de dados fotométricos sem precedentes para GCs. Este trabalho expõe a análise de sete desses aglomerados, sendo seis do Bojo Galáctico (NGC 6304, NGC 6624, NGC 6637, NGC 6652, NGC 6717 e NGC 6723) e um localizado no Halo interno para referência (NGC 6362). A amostra é representativa dos dois picos na distribuição de metalicidades dos GCs do Bojo, em [Fe/H] ~ -0.5 e -1.0. Adotou-se métodos homogêneos para a separação das múltiplas populações nos diferentes estágios evolutivos e para o ajuste de isócronas, com o intuito de analisar comparativamente os dois grupos de metalicidade e verificar se ocorre alguma diferença de idades detectável entre as múltiplas populações. Algoritmos de classificação com aprendizado de máquina, e métodos utilizando estatística Bayesiana (máxima verossimilhança e MCMC) foram implementados e uma ferramenta em Python, nomeada SIRIUS, foi desenvolvida pelo grupo. Os resultados apontam para uma tendência de idades maiores (~ 13 Gyr) para os GCs mais pobres em metais com ramo horizontal azul, comparado com 12.0-12.5 Gyr para os outros GCs. Os resultados para as múltiplas populações indicam idades ligeiramente mais altas para a primeira geração em geral, mas com diferenças menores que 400 Myr comparado com a segunda geração. O resultado de 13.14 +0.25/-0.43 Gyr para o aglomerado NGC 6717 surpreende pois este é o aglomerado menos massivo da amostra, com maior fração de estrelas da primeira geração e com um ramo horizontal azul estendido: aspectos que o colocam como um dos objetos mais velhos da Galáxia. Esses resultados são bastante relevantes, com impactos diretos nos cenários de formação das partes centrais da Galáxia. / The globular clusters (GCs) are fundamental laboratories to study the formation and chemodynamical evolution of the Milky Way, as they formed during the initial episodes of star formation in galaxies. In the last decade, photometric and spectroscopic observational results have challenged the classical paradigm of GCs formation in a single star formation burst, giving rise to the debate about multiple stellar populations. With the purpose of better explore this phenomenon, the Hubble Space Telescope GO-13297 program (UV Legacy Survey of Galactic Globular Clusters, PI: G. Piotto) obtained photometry for 57 GCs with the UV/blue filters F275W, F336W and F438W (WFC3/UVIS), sensitive to variations in CNO abundances, and consequently able to distinguish multiple populations along the color-magnitude diagrams. Combined with previous photometry in the optical filters F606W and F814W (GO-10775 program, PI A. Sarajedini), they provide an unprecedented photometric database for GCs. This work presents the analysis of seven of these clusters, six of them from the Galactic Bulge (NGC 6304, NGC 6624, NGC 6637, NGC 6652, NGC 6717 and NGC 6723) and one located in the inner Halo for reference purposes (NGC 6362). This sample is representative of the two peaks in the metallicity distribution of Bulge GCs, with [Fe/H] ~ -0.5 and -1.0. We adopted homogeneous methods to the separation of multiple populations in the different evolutionary stages and to the isochrone fitting, with the purpose of analyze comparatively the two metallicity groups, and check whether there occurs any detectable age difference between the multiple populations. Classification algorithms with machine learning, and methods using Bayesian statistics (maximum likelihood and MCMC) were implemented and a Python tool, named SIRIUS, was developed by the group. The results point to a trend of larger ages (~ 13 Gyr) for the more metal-poor clusters with a blue horizontal branch, compared with 12.0-12.5 Gyr for the other GCs. The results for the multiple populations indicate slightly larger ages for the first generation in general, but with differences lower than 400 Myr compared with the second generation. The result of 13.14 +0.25/-0.43 Gyr for the cluster NGC 6717 is surprising because this is the least massive cluster of the sample, with the highest fraction of first generation stars and with a blue horizontal branch: features that place it as one of the oldest objects in the Galaxy. These results are quite relevant, with direct impacts on the formation scenarios of the innermost regions of the Galaxy.

Diese Arbeit beschreibt die Suche nach relativistischen magnetischen Monopolen mit dem AMANDA Detektor. Die Methoden der Simulation und der Untergrundseparation werden erläutert. Keine Spuren mit der Signatur eines magnetischen Monopols wurden gefunden. Das sich ergebende Flusslimit von 0.61x10^-16 1/(cm^2 sr s) für Monopole, die sich nahe der Lichtgeschwindigkeit bewegen, liegt um einen Faktor 3-4 besser als die Ergebnisse vergleichbarer Untergrundexperimente und einen Faktor 16 unterhalb der Grenze, die aus der beobachteten Stabilität der galaktischen Magnetfelder liegt. / This thesis describes the search for relativistic magnetic monopoles with the AMANDA detector. The methods of their simulation and their separation from the background are given. No tracks with the signature of a magnetic monopoles are found, resulting in an upper limit on the flux of 0.61x10^-16 1/(cm^2 sr s) for monopoles with velocities close to the speed of light. This is better by a factor of 3-4 compared to results from other underground detectors and a factor of 16 below the limit derived from the observed stability of the galactic magnetic fields.

im Postscript-Format

La métrologie fondamentale est la garante de la pérennité des systèmes de mesure et est en charge de fournir les étalons de références. En ce qui concerne la métrologie des rayonnements ionisants et, en particulier la métrologie des neutrons, des détecteurs étalons sont utilisés pour caractériser les champs de références, en énergie et en fluence. Les dosimètres ou détecteurs de particules sont étalonnés. Cette thèse présente le développement d’un spectromètre neutron candidat au statut d’étalon primaire pour la caractérisation de champs neutroniques dans la gamme 5-20 MeV. Le spectromètre utilise le principe du télescope à protons de recul comme moyen de détection ; la technologie CMOS, au travers de trois capteurs de positions, est mise à profit pour réaliser la trajectographie du proton de recul. Un détecteur Si(Li) est en charge de la mesure de l’énergie résiduelle du proton. Les simulations des dispositifs, réalisées sous MCNPX, ont permis d’estimer les performances du dispositif et de valider la procédure de reconstruction de l’énergie des champs neutroniques. Une étape essentielle de caractérisation des éléments du télescope et en particulier des capteurs CMOS est également proposée afin de garantir la validité de mesures expérimentales postérieures. Les tests réalisés aussi bien en champs mono-énergétiques qu’en champs étendus témoignent des très bonnes performances du système. La quantification des incertitudes indiquent une mesure de l’énergie avec une précision de plus de 1.5 % pour une résolution de moins de 6 %. La mesure de la fluence neutronique est quand a elle réalisée avec une incertitude de 4 à 6 %. / The fundamental metrology is responsible for the sustainability of the measurement systems and handles to supply the reference standards. Concerning the metrology of ionizing radiations and, in particular the neutron metrology, detectors standards are used to characterize reference fields, in terms of energy and fluence. The dosimeters or particle detectors are calibrated on these reference fields. This thesis presents the development of a neutron spectrometer neutron candidate to the status of primary standard for the characterization of neutron fields in the range from 5 to 20 MeV. The spectrometer uses the recoil proton telescope as detection principle; the CMOS technology, through three sensor positions, is taking advantage to realize the tracking of protons. A Si(Li) detector handles the measure of the residual proton energy. The device simulations, realized under MCNPX, allow to estimate its performances and to validate the neutron energy reconstruction. An essential step of characterization of the telescope elements and in particular of CMOS sensors is also proposed to guarantee the validity of posterior experimental measurements. The tests realized as well in mono-energy fields as in radionuclide source show the very good performances of the system. The quantification of uncertainties indicates an energy estimation with 1.5 % accuracy and a resolution of less than 6 %. The fluence measurement is performed with an uncertainty about 4 to 6%.

We show some preliminary 10-37 micron high-resolution spectra taken with the Spitzer Space Telescope in 2008-9 of Mira variables distributed across the M, S and C chemical subclasses. Our entire Spitzer sample of 25 galactic Miras was observed from two to several times during this observing campaign and all have simultaneously measured near-infrared interferometric diameters acquired using the Palomar Testbed Interferometer. Because our sources are very bright for Spitzer IRS (typically 5-100 Janskys), we have excellent signal to noise and for many sources see marked changes in overall flux levels as a function of phase. Further, we are able to identify many strong emission lines and emission features due to silicate and carbon dusts and molecular constituents. We introduce the sample and the design of our experiment, discuss the data reduction required for such bright sources using Spitzer, show several examples of spectra with phase and discuss some preliminary findings. Finally, we discuss future steps for Paper II, to be presented later in the year.

The main objective of this research is to design, simulate, and evaluate telescope array-based receiver architectures for the inter-planetary optical communication links, which is able to provide broadband data support for future deep-space and universe exploration missions. The major aspects of this research are as follows: (1) evaluation and performance comparison of telescope arrays-based receiver with a large, monolithic telescope-based receiver, (2) mathematical modeling and analysis of the impact of various limiting factors (i.e., background noise, atmospheric turbulence, synchronization and tracking errors) on the performance of optical array receiver, (3) design and evaluation of subsystems and adaptive signal processing algorithms for the mitigation of the above-mentioned deleterious effects, and (4) development of an end-to-end simulation and analysis platform for an optical communication link between a transmitter in Mars orbit and an Earth-based array receiver after integration of the proposed sub-systems. In the second part of this research, I aim to extend the analysis to the free-space, short-range, terrestrial optical communication links. In this part, the objective is the development of the efficient simulation tools for the analysis of receiver performance and optical beam propagation through turbulent atmospheric channel. In the experimental part of the research, the investigation of the use of adaptive optics (AO) subsystems for turbulence and background noise compensation in the deep-space optical communication links will be carried out.