Submitted in fulfillment of the academic requirements for the Master’s Degree of Technology: Electrical Engineering – Light Current, Durban University of Technology, 2012. / The development of a transit radio telescope at the hydrogen line frequency of 1420 MHz is described. The telescope antenna uses a 5 m diameter parabolic reflector with an estimated efficiency of 50 % and an F/D ratio of 0.5. The gain of the antenna at 1420 MHz (wavelength of 21.1 cm) is approximately 35 dB with a beamwidth of approximately 3°. The antenna is mounted on a concrete beam at the first floor level, running between two 5 floor tower blocks on the Steve Biko campus of the Durban University of Technology. The majority of the components of the radio telescope antenna and receiver were designed and manufactured at the Durban University of Technology by students of the Departments of Mechanical and Electronic Engineering. The measured sensitivity of the receiver is approximately -94 dBm with a bandwidth of approximately 80 MHz. Radio sources successfully detected by the radio telescope include the Sun, the Moon, Sagittarius A, Centaurus A and Vela X.

Submitted in fulfillment of the academic requirements for the Degree Master of Engineering: Electrical: Electronic Engineering, Durban University of Technology. Durban. South Africa, 2015. / A two element correlating radio telescope interferometer is the fundamental building block of modern radio telescope aperture synthesis arrays. Early radio telescopes consisted of a single antenna, usually a dish antenna. Larger and larger antennas were constructed in order to improve the resolution of the measurement of the direction and extent of radio frequency radiation coming from the sky. Telescope resolution is fundamentally limited by the ratio of the telescope aperture to the wavelength of the received radiation. For single element radio telescopes to approach the resolution of their optical telescope counterparts, they would need to be impractically large. Mathematical analysis of correlating two element radio telescope interferometers shows that very large aperture radio telescopes can be synthesized from a number of two element interferometers. An array of two element correlating radio telescope interferometers can be used to produce a synthesized aperture equal to the largest distance between two receiving antennas in the array. Telescope arrays thus enable very high resolution since the angular resolution of a telescope is proportional to the wavelength of the received signal divided by the aperture diameter. A spread of separation distances between antenna pairs is required to produce a complete image of the radiating sources in the field of view. Modern digital signal processing techniques can be used to provide cost effective performance and flexibility in two element correlating radio telescope interferometer design. The aim of this research project was to design and construct a two element correlating radio telescope interferometer using modern digital signal processing techniques and hardware. The relevant theory has been investigated together with suitable hardware and software platforms and tools used to produce such a system. The two element correlating radio telescope interferometer produced, will be used as a platform for further investigative research into its design, performance and application. The outcome of this research project was the successful completion of a working two element correlating radio telescope interferometer. The development process has been analysed and carefully documented. Some fringe measurements for a simple single frequency radiating point source have been taken and these measurements have been analysed according to theoretical expectation. Potential for further research, using the two element correlating radio telescope interferometer produced, has been identified and discussed.

Submitted in fulfillment of the academic requirements for the Degree Master of Engineering (Electronic), Department of Electronic Engineering, Durban University of Technology, Durban, South Africa, 2016. / The proposed supervisory control and data acquisition solution is intended to gather data from all sub-systems and provide control commands related to the Indlebe Radio Telescope. Currently the control commands are executed from the command line prompt of the Skypipe software. These control commands are used to change the elevation angle of the antenna. The supervisory control and data acquisition system will be interfaced to sub-systems namely; a programmable logic controller, a weather station, an uninterruptible power supply and a camera. It will be used to manually or automatically control the elevation angle of the antenna, includes a menu structure that allows for easy navigation to the sub-systems and allows for trending, alarming, logging and monitoring of all system parameters. The proposed system will mitigate the lack of information on the existing system. A global system for mobile communication unit has also been installed to monitor the temperature within the Indlebe control room, detect a power failure and communicate this information to supervisors, using its short message service option. Implementing a solution of this nature means that all data from the various sub-systems are brought together, giving a single platform to monitor data and provide manual and automatic control functionality. Problem solving, understanding and maintenance of the system will also become easier. / D

This qualitative study is an exploratory look at family experiences at night time telescope observing events, often called star parties. Four families participated in this study which looked at their expectations, experiences and agendas as well as the roles that identity and family culture played in the negotiation of meaning. Two families who had prior experience with attending star parties were recruited ahead of time and two other families who were first time visitors were recruited on-site at the observing event. Data were collected at two star parties. At each event, one experienced family was paired with an on-site family for the purposes of facilitating conversations about expectations and prior experiences.The results of this study showed that learning is constantly occurring among families, and that star parties and family culture were mediational means for making meaning. Expectations and agendas were found to affect the families' star party experiences and differences were observed between the expectations and experiences of families based on their prior experiences with star parties. These data also showed that family members are actively negotiating their individual and family identities. These families use their cultural history together to make sense of their star party experiences; however, the meaning that families were negotiating was often focused more on developing family and individual identity rather than science content. The families in this study used the star party context as a way to connect with each other, to make sense of their prior experiences, and as raw material for making sense of future experiences.

The Richard F. Caris Mirror Lab at the University of Arizona is responsible for production of the eight 8.4 m segments for the primary mirror of the Giant Magellan Telescope, including one spare off-axis segment. We report on the successful casting of Segment 4, the center segment. Prior to generating the optical surface of Segment 2, we carried out a major upgrade of our 8.4 m Large Optical Generator. The upgrade includes new hardware and software to improve accuracy, safety, reliability and ease of use. We are currently carrying out an upgrade of our 8.4 m polishing machine that includes improved orbital polishing capabilities. We added and modified several components of the optical tests during the manufacture of Segment 1, and we have continued to improve the systems in preparation for Segments 2-8. We completed two projects that were prior commitments before GMT Segment 2: casting and polishing the combined primary and tertiary mirrors for the LSST, and casting and generating a 6.5 m mirror for the Tokyo Atacama Observatory.

QC 351 A7 no. 69 / The history of modern wide -field, high-speed catadioptric lenses is reviewed. One system comprising only spherical curves and representative of the current art for low-light-level systems is evaluated and used as a baseline design in a weight-reduction study. Five aspheric designs are computed and evaluated. It is found that the use of aspherics will permit weight reduction only in certain instances, i.e., if one element of an all-spherical design can be eliminated or if a fundamentally different configuration that is possible only with aspherics is substituted for the all-spherical configuration. Of these possibilities, the elimination of an element is the best replacement for the baseline design. The case of a highly constrained, purely refractive triplet is studied in some detail. Four designs are computed -from the all-spherical case to the most complex polynomial aspheric. It is found that, if only conic aspherics are employed, significant improvement can be obtained and the problems involved are sensibly the same as those in all-spherical designs. When complex aspherics are applied, the problem becomes surprisingly difficult, and there is some indication that a computer can deal with it better than can a human lens designer.

Les expériences d’astroparticules n’ont cessé de fleurir ces dix dernières années dans le but de connaître l’origine des rayons cosmiques et les procédés mis en œuvre dans leur accélération à des ultra-hautes énergies. Les télescopes Cherenkov tels que ANTARES détectent la lumière Cherenkov issue des muons se propageant dans l’eau de mer méditerranée. Les muons sont les produits d’interaction de neutrinos cosmiques (signal) ou atmosphériques (bruit) avec les noyaux de la terre. Pour offrir les meilleures conditions de détection de la lumière Cherenkov, et par conséquent bien reconstruire les traces des muons détectés, les détecteurs de lumière i.e les photomultiplicateurs doivent satisfaire plusieurs conditions. Le premier volet de cette thèse porte sur le développement de photomultiplicateurs utilisant le cristal comme préamplificateur de signal optique. L’avantage d’un tel procédé est la possibilité de séparer plusieurs pics photo-électrons et d’améliorer la résolution tem- porelle grâce à un fort champ électrique. La conception d’un tel prototype et la possibilité de son industrialisation à grande échelle sont développés pour la première fois dans cette thèse. Le deuxième volet s’inscrit dans la nouvelle thématique multi-messagers d’ANTARES.Un suivi avec six télescopes optiques répartis sur chaque hémisphère est déclenché lorsque ANTARES détecte un neutrino de haute énergie ou un ensemble de neutrinos coïncidents en temps et en direction. Un tel système permet d’augmenter la sensibilité de détection de neutrinos provenant de sources transitoires tels que les sursauts gamma et les Supernovæ à effondrement de cœur. Un système d’alertes neutrino est maintenant implémenté et fonctionne continument et de manière autonome sur ANTARES. Le système offre de bonnes performances; le suivi optique se déclenche dans la minute suivant la détection neutrino et l’incertitude sur la reconstruction de la trajectoire du neutrino est de 0.4◦ (valeur médiane). Une fois l’alerte reu çe par un des télescopes, celui-ci se repositionne sur la direction du neutrino et entame une série d’observations réparties sur le mois suivant l’alerte. Cette thèse a porté dans un premier temps sur l’aspect neutrino en développant le filtre sélectionnant les évènements haute énergie et multi-neutrinos. Des outils d’analyse d’images optiques ont ensuite été implémentés pour la recherche de sources transitoires. Les premiers résultats de recherche de contreparties optiques de sursauts gamma en corrélation avec un signal neutrino sont présentés. / Astroparticle experiments are being developed with the aim of resolving the mystery of cosmic rays. Questions like from where cosmic rays originate or how do they get accelerated up to ultra high energies are still unresolved. Cherenkov telescopes like ANTARES detect the Cherenkov light emitted by muons propagating in the sea water. Muons are produced by the interaction of cosmic neutrinos (signal) or atmospheric neutrinos (noise) with the Earth nuclei.In order to offer the best detection conditions of Cherenkov light, and subsequently ensure a good reconstruction quality of the muons trajectory, the light sensors i.e the photomultipliers must satisfy various conditions.The first part of this thesis focuses on the development of photomultipliers using crystals as a preamplifier of the light signal. The advantage of such a method is the possibility to separate individual photo-electrons and to enhance the temporal resolution by applying a high electric field.The design and conception as well as the possibility to produce such devices at large industrial scales is for the first time developed in this thesis.The second part of the thesis is inspired from the new multi-messenger approach in ANTARES. An optical follow-up with six telescopes spread over the two hemispheres is triggered by the detection of a high energy neutrino or a set of neutrinos coincident in time and direction. Such a system enhances the sensitivity to transient sources such as Gamma Rays Bursts (GRB) or Core Collapse Supernovae. The neutrino alert system is now fully operational. The system offers good performances; the optical follow-up starts within one minute from the neutrino detection and the median angular accuracy of the reconstructed neutrinos is 0.4$^circ$.Upon the reception of an alert, the telescopes point at the neutrino direction and start the acquisition of image series almost each night of the month following the neutrino alert. Image analysis tools have been implemented to search for optical transients; First results on the search of GRB optical counterparts correlated with a neutrino signal are presented.

Philosophiae Doctor - PhD / The next generation of radio telescopes will revolutionize cosmology by providing large three-dimensional surveys of the universe. This work presents forecasts using the technique 21cm intensity mapping (IM) combined with results from the cosmic microwave background, or mock data of galaxy surveys. First, we discuss prospects of constraining curvature independently of the dark energy (DE) model, finding that the radio instrument HIRAX will reach percent-level accuracy even when an arbitrary DE equation of state is assumed. This is followed by a study of the potential of the multi-tracer technique to surpass the cosmic variance limit, a crucial method to probe primordial non-Gaussianity and large scale general relativistic e↵ects. Using full sky simulations for the Square Kilometre Array phase 1 (SKA 1 MID) and the Large Synoptic Survey Telescope (LSST), including foregrounds, we demonstrate that the cosmic variance contaminated scenario can be beaten even in the noise free case. Finally, we derive the signal to noise ratio for the cosmic magnification signal from foreground HI intensity maps combined with background galaxy count maps. Instruments like SKA1 MID and HIRAX are highly complementary and well suited for this measurement. Thanks to the powerful design of the planned radio instruments, all results confirm their potential and promise an exciting future for cosmology.

In this thesis we studied dark matter models with strong self-interactions, typically known as self-interacting dark matter (SIDM). This kind of models constitute a promising solution to the tension between small scale structure observations and predictions assuming the standard case of collisionless cold dark matter (CDM) while keeping the success of the standard cosmological model, LambdaCDM, at large scales. The presence of strong self-interactions can increase the dark matter capture and annihilation in astrophysical objects like our sun, enhancing the potential of indirect detection signals. We used the high energy neutrinos produced by such annihilations to probe SIDM models. We established strong constraints on SIDM with velocity independent cross section by comparing the expected neutrino signal with the results of the IceCube-79 dark matter search. Also, we determined the sensitivity for the IceCube-DeepCore and PINGU detectors for SIDM with a velocity dependent self-interacting cross section (vdSIDM). Most of its relevant parameter space can be tested with the three years of data already collected by IceCube-DeepCore, complementing results from direct detection experiments and other indirect detection studies. / Nesta tese investigamos modelos de matéria escura com auto-interações fortes, conhecidos tipicamente como matéria escura auto-interagente (SIDM). Este tipo de modelos constituem uma solução promissora à tensão entre as observações de estrutura a pequena escala e as previsões assumindo o caso padrão de matéria escura fria não colisional (CDM), enquanto se mantêm o sucesso do modelo cosmológico padrão, LambdaCDM, a grandes escalas. A presença de auto-interações fortes podem aumentar a captura e a aniquilação da matéria escura em objetos astrofísicos como o nosso sol, aumentando o potencial de sinais de detecção indireta. Usamos o sinal de neutrinos de alta energia produzidos por essas aniquilações para explorar modelos de SIDM. Estabelecemos fortes vínculos em modelos de SIDM com seção de auto-interação independente da velocidade comparando o sinal de neutrinos esperado com os resultados de busca de matéria escura do IceCube-79. Também, determinamos a sensibilidade dos detectores IceCube-DeepCore e PINGU para modelos de SIDM com uma seção de auto-interação dependente da velocidade (vdSIDM). A maior parte do espaço de parâmetros de interesse pode ser testado com os três anos de dados já coletados pelo IceCube-DeepCore, complementando os resultados de experimentos de detecção direta e outras an análises de detecção indireta.

Submitted by Verena Pereira (verenagoncalves@uefs.br) on 2018-11-14T23:32:15Z No. of bitstreams: 1 Disserta??o - Dados Astron?micos_Uma proposta de implementa??o para banco de dados - VERSAO DIGITAL.pdf: 12472772 bytes, checksum: 7819133722c393f66647cb47f14700c6 (MD5) / Made available in DSpace on 2018-11-14T23:32:15Z (GMT). No. of bitstreams: 1 Disserta??o - Dados Astron?micos_Uma proposta de implementa??o para banco de dados - VERSAO DIGITAL.pdf: 12472772 bytes, checksum: 7819133722c393f66647cb47f14700c6 (MD5) Previous issue date: 2018-06-21 / Coordena??o de Aperfei?oamento de Pessoal de N?vel Superior - CAPES / With the advent of computing, the way of doing science has changed circumstantially, revolutionizing scientific research. In astronomy, telescopes now equipped with increasingly modern sensors, produce data quantities never seen before, making it impossible to exhaust all the capacity to extract knowledge from the data produced, thus presenting conditions of reuse by their peers or other purposes. The value of this data to Science lies in its unexplored potential. In this sense, this work shares the philosophy of Virtual Observatories, regarding the reuse of old data. Therefore, this dissertation is about the implementation of procedures and computational techniques that allow to organize and search for images from telescopes. Images that were found were of the exclusive period. With this, studies were developed on data structure, computational tools, algorithms and programming languages that could contribute to the development and resolution of the research problem under analysis / Com advento da Computa??o, a forma de fazer Ci?ncia mudou circunstancialmente, revolucionando a pesquisa cient?fica. Na Astronomia, os telesc?pios agora equipados com sensorescada vez mais modernos, produzem quantidades de dados nunca vista antes, tornando imposs?vel exaurir toda ? capacidade de extra??o de conhecimento dos dados produzidos, apresentando assim, condi??es de reutiliza??o pelos seus pares ou outras finalidades. O valor desses dados para a Ci?ncia est? no seu potencial n?o explorado. Nesse sentido, esse trabalho compartilha da filosofia dos Observat?rios Virtuais,no que tange ? reutiliza??o de dados antigos. Para tanto, essa disserta??o versa sobre a implementa??o de procedimentos e t?cnicas computacionais que permitem organizar e buscar imagens oriundas de telesc?pios. Imagens que se encontram foram do per?odo de exclusividade. Com isso, foram desenvolvidos estudos sobre estrutura de dados, ferramentas computacionais, algoritmos e linguagens de programa??o que pudessem contribuir com o desenvolvimento e resolu??o do problema de pesquisa em an?lise