Thesis (MScEng (Electrical and Electronic Engineering))--University of Stellenbosch, 2011. / ENGLISH ABSTRACT: The Square Kilometre Array (SKA) is an international project to build the world’s largest and most sensitive radio telescope interferometer. It will consist of thousands of antennas distributed over many kilometers, with the hosting country being either South Africa or Australia. Various pathfinders have been initiated to demonstrate the technologies needed to implement the SKA. The astronomy community has defined five Key Science Projects (KSP), which are the drivers for the SKA. The science goals determine the technical requirements needed to design SKA systems. Many years of planning and development are still needed in order to meet to the requirements of such a large and complex project. This thesis aims to present the various SKA pathfinder systems in terms of their application to the SKA key science projects, with main focus that of pulsar observations. In order to achieve this, a thorough overview of basic radio astronomy principles and techniques is presented, followed by a detailed look at the various pathfinders. Throughout the work, aspects of pulsar observations are given particular attention with the goal of designing optimal systems for the SKA. / AFRIKAANSE OPSOMMING: Die Square Kilometre Array (SKA) is ’n internasionale projek om die wêreld se grootste en mees sensitiewe radio teleskoop interferometer te bou. Dit sal bestaan uit duisende antennas versprei oor etlike kilometers, met die gasheer land óf Suid-Afrika óf Australië. Verskeie koersbepalers is geïnisieer om die tegnologie te demonstreer wat benodig is om die SKA te implementeer. Die astronomie gemeenskap het vyf sleutel wetenskap projekte (KSP) gedefinieër wat dien as die drywers vir die SKA. Die wetenskap doelwitte bepaal die tegniese vereistes wat nodig is om SKA stelsels to ontwerp. Talle jare van beplanning en ontwikkeling word steeds benodig om te voldoen aan die vereistes van so ’n groot en komplekse projek. Hierdie tesis het ten doel die aanbieding van verskeie SKA koersbepaler stelsels in terme van hulle aanwending tot die SKA sleutel wetenskap projekte, met hoof fokus op die van pulsar waarnemings. Om dit te behaal, word ’n deeglike oorsig van basiese radio astronomie beginsels en tegnieke aangebied, gevolg deur ’n gedetailleerde kyk na die verskeie koersbepalers. Regdeur die werk word spesifieke aandag gegee aan aspekte van pulsar waarnemings met die doel om optimale stelsels vir die SKA te ontwerp.

Le cinquième télescope (CT5) du réseau H.E.S.S. (High Energy Stereoscopic System) a été inauguré en 2012. H.E.S.S. est destiné à l’observation du ciel austral dans le domaine des rayons γ et CT5, dont le seuil est d’environ 30 GeV, a permis la détection du pulsar de Vela après 24 heures d’observations. Certains scénarios de gravitation quantique (QG) prédisent une violation d’invariance de Lorentz (LIV). Celle-ci se manifeste par l’ajout de termes ∝(E/EQG)n aux relations de dispersion du photon, où E est l’énergie du quanta de lumière, EQG l’énergie caractéristique des processus de QG et n l’ordre de la correction. Cette dépendance en énergie peut être testée par des mesures de temps de vol entre photons reçus de sources astrophysiques variables (noyaux actifs de galaxies), transitoires (sursauts γ) ou encore périodiques (pulsars). Cette thèse présente l’analyse des données recueillies par CT5 sur le pulsar de Vela. Une méthode de maximum de vraisemblance ayant déjà montré sa robustesse sur d’autres types de sources a été adaptée au cas du pulsar de Vela. Aucune déviation des relations de dispersion standard n’est observée, par conséquent des limites sont placées sur EQG. La plus contraignante est obtenue pour une correction linéaire superluminique aux relations de dispersion EQG > 7.0×1015 GeV. / The fifth telescope (CT5) of the H.E.S.S. array (High Energy Stereoscopic System) was inaugurated in 2012. H.E.S.S. is designed to scrutinize the southern γ ray sky and CT5, whose threshold is about 30 GeV, allowed the Vela pulsar detection in 24 hours observation time. Some quantum gravity (QG) scenarios predict a violation of Lorentz invariance (LIV). This could manifest by additional terms ∝(E/EQG)n to the photon dispersion relations, where E is the light quantum energy, EQG the typical scale at which QG processes are expected to occur and n the order of the correction. This energy dependence could be tested by time of flight measurements between photons emitted from variable (active galactic nuclei), transient (gamma ray bursts) or periodical (pulsars) astrophysical sources. This thesis presents the analysis of the CT5 collected data from the Vela pulsar. A maximum likelihood method already successfully applied to other source species has been adapted here to the Vela pulsar. No deviation from standard photon dispersion relations is observed, therefore limits have been placed on EQG. The most restrictive result has been obtained for a superluminal linear correction to the dispersion relations EQG > 7.0×1015 GeV.

A new digital receiver was built for the Ooty Radio Telescope (ORT). This new digital receiver system functionally replaces many systems custom-built for various applications at ORT. The thesis presents the receiver design, tests conducted, contributions made, revisions to the receiver architecture and future scopes. The novelty of the receiver design is in treating the ORT as an array of 22 antenna elements. Simulation studies were carried out to analyze the array performance of ORT. The IF signals are digitized and processed by a combination of multiple FPGAs and computers. Major transport of data in the receiver is through high speed serial communication. Programs were developed for configuration, control, data acquisition and off-line analysis. The functionality of the proposed digital receiver was verified through laboratory tests. The proposed receiver enables several new modes of operation of the ORT and field tests were carried out to verify these features of the system. These tests are briefly described below. The radio waves received on earth from celestial sources are extremely weak and their presence can only be detected by sensitive receivers associated with large radio telescopes. The resulting vulnerability of such observations to the ever increasing presence of radio frequency interference has prompted us to to develop new procedures to identify RFI at ORT through time and frequency domain analysis. The digital receiver has also been used in carrying out RFI study at ORT module level for the first time. Our study demonstrates that a major challenge to realizing the full potential of the ORT will be to detect weakly interfering RFI features and occasionally appearing RFI spikes and correct for their contamination in the observations. The examples provided by our analysis of data collected using the digital receiver are very useful for interpreting the data obtained during sensitive spectral line observations and has already enabled several new studies, the most notable being a sensitive recombination line survey conducted using our digital receiver at ORT as part of another research work. A spectral line emission detection procedure using our receiver has been evolved and an example result obtained by observing a region is presented in the thesis. Formation of phased array of ORT modules using the digitized IF signal is discussed and its implementation is verified through observation of celestial sources. An important requirement for proper phasing of the array is the calibration of differential delay/phase variations across the modules of the ORT, for which a powerful method was implemented based on the cross correlation of signals arriving at the 22 modules. This new method employs Hilbert Transform technique to introduce phase information in the sampled signal and the estimated delay and phase corrections are found to be consistent and repeatable. An interplanetary scintillation observation was made with the phased array and the resultant fluctuation spectra obtained are presented. Several pulsar observations and continuum sources have been observed and the results are presented. Another notable feature of the proposed digital receiver is the enhanced field of view which will lead to a reduced observing time observing extended regions. The improved spectral and temporal resolutions have also been demonstrated by the observations presented in the thesis. In particular, the single pulse observations of pulsars reported in the thesis were enabled by the high time resolution supported by the receiver.. The present work also demonstrated the digital beam formation with ORT modules in arbitrary directions. The digitally synthesized beam was compared within the first null positions of the central analog beam (beam-7) of ORT and the result is reported in the thesis. The new digital receiver enabled all the above mentioned analyses which were carried out for the first time at ORT. The results of the field trials emphasized the need for future observations to include RFI monitoring and characterization as part of the observing strategy and continuously evolve the algorithms for RFI mitigation by using different statistical signatures of the celestial signals. The need for providing a layer of buffering and preprocessing before the final beam formation or correlation is emphasized. To facilitate such development in the future, the final operational system provides for software based correlator which can be developed using the algorithms presented in this thesis. This transforms our original target of a reconfigurable platform to a much more flexible re-programmable platform. In particular, this simplifies the application of windowing functions and polyphase filters to control the beam shapes to (a) reduce beam dilution effects and, (b) to enhance RFI rejection by side lobe suppression. Such techniques can be used to reduce spectral leakage and reduce the effect of RFI on adjacent frequency channels in critical observations. Our receiver is adequate for realizing the maximum potential of the IF signals entering the receiver room. Any further enhancement of the ORT spectral coverage and instantaneous sky coverage will require telescope's front end modification and digitization of signals at the RF stage. The real time processing capabilities can be further enhanced by using multi-core processors and multi gigabit ethernet interfaces that are starting to appear as commodity hardware. Thus the present work opens up several new avenues for future work.

In recent years there has been an increasing demand for real-time streaming applications that handle large volumes of data with low latency. Examples of such applications include real-time monitoring and analytics, electronic trading, advertising, fraud detection, and more. In a streaming pipeline the first step is ingesting the incoming data events, after which they can be sent off for processing. Choosing the correct tool that satisfies application requirements is an important technical decision that must be made. This thesis focuses entirely on the data ingestion part by evaluating three different platforms: Apache Kafka, Apache Pulsar and Redis Streams. The platforms are compared both on characteristics and performance. Architectural and design differences reveal that Kafka and Pulsar are more suited for use cases involving long-term persistent storage of events, whereas Redis is a potential solution when only short-term persistence is required. They all provide means for scalability and fault tolerance, ensuring high availability and reliable service. Two metrics, throughput and latency, were used in evaluating performance in a single node cluster. Kafka proves to be the most consistent in throughput but performs the worst in latency. Pulsar manages high throughput with low message sizes but struggles with larger message sizes. Pulsar performs the best in overall average latency across all message sizes tested, followed by Redis. The tests also show Redis being the most inconsistent in terms of throughput potential between different message sizes

Le satellite Fermi a été lancé le 11 juin 2008, avec à son bord le Large Area Telescope (LAT). Le LAT est un télescope sensible au rayonnement ? de 20 MeV à plus de 300 GeV. Avant la mise en service du LAT, six pulsars jeunes et énergétiques étaient connus dans le domaine ? . Le nombre de détections de pulsars par le LAT prédit avant lancement était de plusieurs dizaines au moins. Le LAT permettait également l’étude des pulsars milliseconde (MSPs), jamais détectés avec certitude à très haute énergie jusqu’alors. Cette thèse aborde dans un premier temps la campagne de chronométrie des pulsars émetteurs radio et/ou X, candidats à la détection par le LAT, en collaboration avec les grands radiotélescopes et télescopes X. Cette campagne a permis la recherche de signaux ? pulsés avec une grande sensibilité. En outre, la plupart des MSPs galactiques ont été suivis dans le cadre de cette campagne, sans biais de sélection a priori sur cette population d’étoiles. Pour la première fois, des pulsations ont été détectées pour huit MSPs galactiques au-dessus de 100 MeV. Quelques bons candidats à une détection prochaine apparaissent. Une recherche similaire a été conduite pour des MSPs d’amas globulaires, sans succès à présent. L’analyse des courbes de lumière et des propriétés spectrales des huit MSPs détectés révèle que leur rayonnement ? est relativement similaire à celui des pulsars ordinaires, et est vraisemblablement produit dans la magnétosphère externe. Cette découverte suggère que certaines sources non-identi?ées sont des MSPs, pour l’instant inconnus. / The Fermi observatory was launched on June 11, 2008. It hosts the Large Area Telescope (LAT), sensitive to ? -ray photons from 20 MeV to over 300 GeV. Before the LAT began its activity, six young and energetic pulsars were known in ? rays. At least several tens of pulsar detections by the LAT were predicted before launch. The LAT also allowed the study of millisecond pulsars (MSPs), never ?rmly detected in ? rays before Fermi. This thesis ?rst presents the pulsar timing campaign for the LAT, in collaboration with large radiotelescopes and X-ray telescopes, allowing for high sensitivity pulsed searches. Furthermore, it lead to quasi-homogeneous coverage of the galactic MSPs, so that the search for pulsations in LAT data for this population of stars was not affected by an a priori bias. We present a search for pulsations from these objects in LAT data. For the ?rst time, eight galactic MSPs have been detected as sources of pulsed ? -ray emission over 100 MeV. In addition, a couple of good candidates for future detection are seen. A similar search for globular cluster MSPs has not succeeded so far. Comparison of the phase-aligned ? -ray and radio light curves, as well as the spectral shapes, leads to the conclusion that their ? -ray emission is similar to that of normal pulsars, and is probably produced in the outer-magnetosphere. This discovery suggests that many unresolved ?-ray sources are unknown MSPs.

L'objectif de cette thèse est d'étudier différents aspects microscopiques et macroscopiques liés à la présence de superfluidité dans les étoiles à neutrons. Dans un premier temps, nous avons calculé des configurations stationnaires d'étoiles à neutrons superfluides en rotation, en relativité générale, basées sur l'utilisation d'équations d'état réalistes. A l'aide de ces configurations d'équilibre, nous avons ensuite développé un modèle simple de glitch, en relativité générale, vu comme un transfert de moment cinétique entre les neutrons superfluides et les particules chargées constituant l'étoile. Cela nous a permis d'obtenir des temps caractéristiques de montée qui pourront être comparés à de futures observations précises de glitches afin d'apporter de meilleures contraintes sur l'intérieur de ces étoiles. Enfin, nous nous sommes également intéressés à la dynamique des vortex superfluides, en présence de tubes de flux, dans le cas où les protons dans le coeur des étoiles formeraient un supraconducteur de type II. / The aim of this thesis is to study different aspects, both microscopic and macroscopic, associated with the presence of a large amount of superfluid matter inside neutron stars. First, we computed stationary configurations of rotating superfluid neutron stars, in general relativity, using realistic equations of state. Based on these equilibrium configurations, we then developed a simple model of pulsar glitches, in general relativity, seen as angular momentum transfers between the superfluid neutrons and the charged particles composing the star. This enables us to infer spin-up time scales that could be compared with future accurate glitch observations, in order to get some constraints on the interior of neutron stars. Finally, we also focused on the dynamics of superfluid vortex lines, accounting for the presence of fluxtubes, if the protons are forming a type II superconductor in the core of neutron stars.

This thesis is focussed on the Molonglo Observatory Synthesis Telescope (MOST), reporting on two primary areas of investigation. Firstly, it describes the recent upgrade of the MOST to perform an imaging survey of the southern sky. Secondly, it presents a MOST survey of the Vela supernova remnant and follow-up multiwavelength studies. The MOST Wide Field upgrade is the most significant instrumental upgrade of the telescope since observations began in 1981. It has made possible the nightly observation of fields with area ~5 square degrees, while retaining the operating frequency of 843 MHz and the pre-existing sensitivity to point sources and extended structure. The MOST will now be used to make a sensitive (rms approximately 1 mJy/beam) imaging survey of the sky south of declination -30&deg. This survey consists of two components: an extragalactic survey, which will begin in the south polar region, and a Galactic survey of latitudes |b| &lt 10&deg. These are expected to take about ten years. The upgrade has necessitated the installation of 352 new preamplifiers and phasing circuits which are controlled by 88 distributed microcontrollers, networked using optic fibre. The thesis documents the upgrade and describes the new systems, including associated testing, installation and commissioning. The thesis continues by presenting a new high-resolution radio continuum survey of the Vela supernova remnant (SNR), made with the MOST before the completion of the Wide Field upgrade. This remnant is the closest and one of the brightest SNRs. The contrast between the structures in the central pulsar-powered nebula and the synchrotron radiation shell allows the remnant to be identified morphologically as a member of the composite class. The data are the first of a composite remnant at spatial scales comparable with those available for the Cygnus Loop and the Crab Nebula, and make possible a comparison of radio, optical and soft X-ray emission from the resolved shell filaments. The survey covers an area of 50 square degrees at a resolution of 43&quot x 60&quot, while imaging structures on scales up to 30'. It has been used for comparison with Wide Field observations to evaluate the performance of the upgraded MOST. The central plerion of the Vela SNR (Vela X) contains a network of complex filamentary structures. The validity of the imaging of these filaments has been confirmed with Very Large Array (VLA) observations at 1.4 GHz. Unlike the situation in the Crab Nebula, the filaments are not well correlated with H-alpha emission. Within a few parsec of the Vela pulsar the emission is much more complex than previously seen: both very sharp edges and more diffuse emission are present. It has been postulated that one of the brightest filaments in Vela X is associated with the X-ray feature (called a `jet') which appears to be emanating from the region of the pulsar. However, an analysis of the MOST and VLA data shows that this radio filament has a flat spectral index similar to another more distant filament within the plerion, indicating that it is probably unrelated to the X-ray feature.

Les observations XMM-Newton et Chandra en X de trois amas globulaires galactiques (NGC 2808, NGC 4372 et M 22) sont présentées et analysées. Elles sont complétées par des observations dans le visible, l'ultraviolet, l'infrarouge et le domaine radio afin d'identifier les sources X liées à ces amas globulaires. Les observations X ont permis de détecter 16 sources liées à NGC 2808 et 18 sources liées à M 22 qui sont principalement des binaires serrées. Cette population élevée de binaires aurait un rôle important à jouer dans le ralentissement de l'effondrement du cœur de ces amas globulaires. Une binaire X de faible masse en quiescence contenant une étoile à neutrons a été détectée dans NGC 2808 et aucune source de ce type n'est détectée dans M 22 et NGC 4372. Ces résultats sont en accord avec la corrélation déjà observée entre le nombre de ces objets et le taux de rencontre d'étoiles dans le cœur des amas globulaires. Un déficit possible de sources X dans NGC 2808 semble indiquer que le taux de rencontre n'est pas le seul paramètre intervenant dans la production des sources X et la métallicité de l'amas pourrait aussi avoir une influence. À partir des rapports X/UV et d'observations spectroscopiques, nous proposons différentes approches afin de résoudre le problème du déficit d'éruptions de variables cataclysmiques déjà observé dans les amas globulaires. Ces approches consistent à déterminer si les variables cataclysmiques des amas globulaires sont en majorité magnétiques ou si elles ont un taux d'accrétion faible. Enfin, les observations permettent d'apporter une limite supérieure d'environ 400 masses solaires si un trou noir de masse intermédiaire se trouvait dans NGC 2808.

L'expérience H.E.S.S. (High Energy Stereoscopic system) a pour objectif l'observation du ciel austral en rayons gamma de très haute énergie. L'observatoire, constitué de quatre télescopes fonctionnant en stéréoscopie et situé en Namibie, est un des plus performants au monde. Enregistrant des données depuis 2003, c'est l'instrument idéal pour l'observation du plan galactique et la détection des nombreuses sources qui s'y trouvent. Trois méthodes d'analyse ont été mises en place, s'appuyant sur différentes propriétés des gerbes électromagnétiques issues de l'interaction des gamma avec l'atmosphère. L'objectif premier de cette thèse était de combiner les informations issues de ces trois méthodes pour la sélection des événements et la reconstruction de la direction et de l'énergie des gamma. La nouvelle analyse, appelée Xeff, apporte un gain significatif sur la qualité de la sélection et sur la précision de reconstruction de l'énergie et de la direction. L'analyse Xeff a été utilisée pour l'étude de nébuleuses de pulsar telles que Vela X, G0.9+0.1 et MSH 15-52. De nouveaux résultats ont été mis en évidence concernant l'extension de la source (Vela X) ou la forme spectrale (G0.9+0.1 et MSH 15-52) grâce à de nouvelles observations et à l'efficacité de l'analyse mise en place. Dès 2010, l'expérience rentrera dans une nouvelle phase avec l'achèvement d'un cinquième télescope, dédié à l'observation des rayons gamma à partir de quelques dizaines de GeV. Les tests mis en place pour l'étalonnage des photomultiplicateurs et les résultats obtenus sont décrits dans le manuscrit.

This thesis is focussed on the Molonglo Observatory Synthesis Telescope (MOST), reporting on two primary areas of investigation. Firstly, it describes the recent upgrade of the MOST to perform an imaging survey of the southern sky. Secondly, it presents a MOST survey of the Vela supernova remnant and follow-up multiwavelength studies. The MOST Wide Field upgrade is the most significant instrumental upgrade of the telescope since observations began in 1981. It has made possible the nightly observation of fields with area ~5 square degrees, while retaining the operating frequency of 843 MHz and the pre-existing sensitivity to point sources and extended structure. The MOST will now be used to make a sensitive (rms approximately 1 mJy/beam) imaging survey of the sky south of declination -30&deg. This survey consists of two components: an extragalactic survey, which will begin in the south polar region, and a Galactic survey of latitudes |b| &lt 10&deg. These are expected to take about ten years. The upgrade has necessitated the installation of 352 new preamplifiers and phasing circuits which are controlled by 88 distributed microcontrollers, networked using optic fibre. The thesis documents the upgrade and describes the new systems, including associated testing, installation and commissioning. The thesis continues by presenting a new high-resolution radio continuum survey of the Vela supernova remnant (SNR), made with the MOST before the completion of the Wide Field upgrade. This remnant is the closest and one of the brightest SNRs. The contrast between the structures in the central pulsar-powered nebula and the synchrotron radiation shell allows the remnant to be identified morphologically as a member of the composite class. The data are the first of a composite remnant at spatial scales comparable with those available for the Cygnus Loop and the Crab Nebula, and make possible a comparison of radio, optical and soft X-ray emission from the resolved shell filaments. The survey covers an area of 50 square degrees at a resolution of 43&quot x 60&quot, while imaging structures on scales up to 30'. It has been used for comparison with Wide Field observations to evaluate the performance of the upgraded MOST. The central plerion of the Vela SNR (Vela X) contains a network of complex filamentary structures. The validity of the imaging of these filaments has been confirmed with Very Large Array (VLA) observations at 1.4 GHz. Unlike the situation in the Crab Nebula, the filaments are not well correlated with H-alpha emission. Within a few parsec of the Vela pulsar the emission is much more complex than previously seen: both very sharp edges and more diffuse emission are present. It has been postulated that one of the brightest filaments in Vela X is associated with the X-ray feature (called a `jet') which appears to be emanating from the region of the pulsar. However, an analysis of the MOST and VLA data shows that this radio filament has a flat spectral index similar to another more distant filament within the plerion, indicating that it is probably unrelated to the X-ray feature.