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Tshenye, Thapelo Obed. "Quality control of astronomical CCD observations." Master's thesis, University of Cape Town, 2007. http://hdl.handle.net/11427/4409.
Повний текст джерелаEves, Benjamin Alistair Curtis. "Observations of magnetically driven events in astronomical systems." Thesis, Open University, 2005. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.434234.
Повний текст джерелаMartin, Didier Dieudonné Elisabeth. "Development of superconducting tunnel junction arrays for astronomical observations." Enschede : University of Twente [Host], 2007. http://doc.utwente.nl/58049.
Повний текст джерелаSpreitzer, Teresa. "Construction and operation of a cloud detector to assist astronomical observations." Thesis, McGill University, 2003. http://digitool.Library.McGill.CA:80/R/?func=dbin-jump-full&object_id=80879.
Повний текст джерелаHepworth, James Haydn. "Systems Development of a Two-Axis Stabilised Platform to Facilitate Astronomical Observations." Master's thesis, University of Cape Town, 2018. http://hdl.handle.net/11427/29449.
Повний текст джерелаTravouilon, Tony Physics Faculty of Science UNSW. "Measurements of optical turbulence on the Antarctic Plateau and their impact on astronomical observations." Awarded by:University of New South Wales. Physics, 2005. http://handle.unsw.edu.au/1959.4/20852.
Повний текст джерелаCarvalho, Fernando Pedro. "'Powellsnakes' : a fast Bayesian approach to discrete object detection in multi-frequency astronomical data sets." Thesis, University of Cambridge, 2014. https://www.repository.cam.ac.uk/handle/1810/245147.
Повний текст джерелаIsaak, Katherine Gudrun. "Low-noise instrumentation and astronomical observations of high-redshift objects in submillimetre wavelengths." Thesis, University of Cambridge, 1995. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.364389.
Повний текст джерелаRojas, Folkers Eduardo. "Evaluation, design, and construction of the Wallace Astrophysical Observatory Camera for astronomical observations." Thesis, Massachusetts Institute of Technology, 2009. http://hdl.handle.net/1721.1/54464.
Повний текст джерела"May 2008." Cataloged from PDF version of thesis.
Includes bibliographical references (p. 53-54).
The goal of this thesis is to upgrade the scientific capabilities of the 24" Cassegrain reflector telescope at the George R. Wallace, Jr. Astrophysical Observatory (Wallace Observatory), part of Massachusetts Institute of Technology (MIT). The upgrade consists of evaluating, designing and constructing the Wallace Astrophysical Observatory Camera (WAOcam), optimized for 24" telescope. A full 3D model of the 24" telescope and dome was created to find the size restrictions for WAOcam. An optical model was also developed to maximize the field of view of the camera detector. WAOcam was designed using SolidWorks (3D modeling Software), the parts files from the designing process were also used to machine the instrument. The manufacturing of the WAOcam involved using the following: Computer Numerical Control (CNC) lathe, CNC mill, drill press, and a Waterjet (cutting machine). The manufacturing process also required learning of Omax (software for the Waterjet) and MasterCam 9.1 (software for the CNC lathe and CNC mill). The resulting product is WAOcam, which consists of three modules: 1) vacuum dewar (houses a CCD detector), 2) shutter (controls when light hits the camera detector), and 3) filter wheel (modifies the light before hitting the detector). The remaining work left on the WAOcam is the installation of two additional modules: 1) a four port instrument rotator and 2) a field rotator. This upgrade will allow for occultation observations, strip scanning surveys, and Kuiper Belt Object (KBOs) astrometry to be obtained using the 24" telescope.
by Folkers Eduardo Rojas.
S.B.
PENNING, WILLIAM ROY. "INVESTIGATIONS OF LONG-PERIOD DQ HERCULIS STARS." Diss., The University of Arizona, 1986. http://hdl.handle.net/10150/188161.
Повний текст джерелаSYKES, MARK VINCENT. "INFRARED ASTRONOMICAL SATELLITE OBSERVATIONS OF ASTEROID DUST BANDS AND COMETARY DUST TRAILS (COLLISIONS, DEBRIS, SOLAR SYSTEM)." Diss., The University of Arizona, 1986. http://hdl.handle.net/10150/183974.
Повний текст джерелаJeffers, Sandra Victoria. "Surface brightness distributions of late-type stars." Thesis, University of St Andrews, 2005. http://hdl.handle.net/10023/12941.
Повний текст джерелаLaag, Edward Aric. "Observations of starburst galaxies science and supporting technology /." Diss., [Riverside, Calif.] : University of California, Riverside, 2009. http://proquest.umi.com/pqdweb?index=0&did=1957320791&SrchMode=2&sid=2&Fmt=2&VInst=PROD&VType=PQD&RQT=309&VName=PQD&TS=1268854875&clientId=48051.
Повний текст джерелаIncludes abstract. Available via ProQuest Digital Dissertations. Title from first page of PDF file (viewed March 16, 2010). Includes bibliographical references. Also issued in print.
Chantzos, Johanna [Verfasser], and Paola [Akademischer Betreuer] Caselli. "High resolution spectroscopy of molecules of astrophysical interest and radio astronomical observations of star forming regions / Johanna Chantzos ; Betreuer: Paola Caselli." München : Universitätsbibliothek der Ludwig-Maximilians-Universität, 2020. http://d-nb.info/1209472864/34.
Повний текст джерелаNeyskens, Pieter. "Exploring S stars: stellar parameters, abundances and constraints on the s-process from a new grid of model atmospheres." Doctoral thesis, Universite Libre de Bruxelles, 2014. http://hdl.handle.net/2013/ULB-DIPOT:oai:dipot.ulb.ac.be:2013/209358.
Повний текст джерелаThe dredge-up of carbon and s-process elements into the AGB atmosphere causes an important chemical anomaly among them: initial oxygen-rich stars (M stars) are transformed into carbon-rich stars (C stars). As a consequence, a group of oxygen-rich AGB stars exists which makes the transition between M and C stars. These transition stars are classified as S.
Although AGB stars are identified as producers of heavy elements, their nucleosynthesis and mixing processes are weakly constrained due to large uncertainties on their estimated temperature, gravity and chemical composition. Stronger constraints on the atmospheric parameter space, hence interior processes, of AGB stars can be obtained by investigating the atmosphere of S stars. Since they are transition objects on the AGB, they trace the rise of the s-process. S stars are less numerous than C stars, but their optical spectra are brighter making it easier to identify atomic and molecular lines. Therefore, S stars belong to the most interesting objects along the AGB to perform this task.
From a practical point of view, the spectra of S stars are extremely difficult to study since they are dominated by different, overlapping molecular bands, and the spectral shape may vary strongly from star to star due to their transition status. Therefore, tailored model atmospheres for S stars are of utmost importance to understand the spectroscopic, and even photometric, changes in terms of variations in the atmospheric parameters. A comparison between the models and observations aims not only at constraining the atmospheric parameter space of S stars, it will also test the reliability of 1D state-of-the-art model atmospheres for such complex stars.
From an evolutionary point of view, the S-star family is contaminated with stars who gained their atmospheric enrichment in heavy elements from a companion star. Evidences were found that these binary S stars are not at all located on the AGB, hence, they are labelled as extrinsic S stars while S stars on the AGB are labelled as intrinsic. The difference in evolutionary stages between intrinsic and extrinsic S stars was already found 20 years ago, however, a separation in terms of surface temperature, gravity and chemical composition is not well-established due to the lack of S-star model atmospheres. Such a distinction in atmospheric parameters will facilitate the discovery of these intruders and even help to calibrate stellar evolutionary models of single and binary stars.
To achieve these goals, the first step consists in the construction of a grid of model atmospheres for S stars. The grid will be used to quantify the influence of atmospheric parameters on the model structure and emergent flux. These results will be analyzed to derive precise atmospheric parameters of observed S stars, using a set of well-defined photometric and spectroscopic indices. Once the best model atmosphere has been selected for all observed S stars, their atmospheric parameters will be discussed in view of their evolutionary stage. The best-fitting model atmosphere will also be used to derive abundances from spectral syntheses. The abundance profiles are compared with stellar evolution model prediction to constrain nucleosynthesis and mixing processes inside S stars. Derived abundances of unstable elements will be used to estimate, for the first time, the age of AGB stars. Finally, their abundance profile will be discussed as a function of their time spent on the AGB.
Doctorat en Sciences
info:eu-repo/semantics/nonPublished
Clark, Stephen J. "The intuitive and the intellectual aspects of personal compositional voice and its complex and intuitive processes in relation to astronomical observations and elementary and advanced performers /." View thesis, 2008. http://handle.uws.edu.au:8081/1959.7/38730.
Повний текст джерелаA thesis submitted in partial fulfilment of the requirements for the degree of Doctor of Philosophy awarded by the School of Communication Arts, College of Arts, University of Western Sydney. Includes bibliography.
Trahin, Boris. "Étalonnage de l'échelle des distances dans l'ère Gaia : les étoiles pulsantes RR Lyrae et Céphéides." Thesis, Paris Sciences et Lettres (ComUE), 2019. http://www.theses.fr/2019PSLEO018.
Повний текст джерелаPulsating stars are used to determine distances in the Universe owing to the relation between their pulsation period and absolute magnitude. The calibration of this period-luminosity relation is performed through the determination of independant distances, in particular with the parallax of pulsation method. However, the accuracy of this method is still mainly limited by the projection factor, a parameter used to convert radial velocities measured from spectroscopy into the true pulsating velocity of the star. The objective of this thesis is to use the SPIPS (Spectro-Photo-Interferometry of Pulsating Stars) algorithm to precisely determine this p-factor. Based on the parallax of pulsation approach, this code allows to obtain a better precision on the fundamental parameters of a pulsating star, thanks to a simultaneous modeling of the observables (spectroscopy, photometry and interferometry). Using this method while fixing an independent distance estimate allowed me to retrieve the value of the p-factor. In view of a large scale use of the SPIPS code, I first did an important work of optimization and data collection. These catalogs as well as various observations I made throughout these three years (with among others the PIONIER instrument of the VLTI) allowed me to create a complete and heterogeneous database of more than 300 stars. I then apply the SPIPS algorithm to a large sample of stars using the parallaxes from the second data release of the Gaia satellite. Using these parallaxes, I was first able to accurately calculate the p-factor of some RR Lyrae type variables. Applied to a larger sample of Cepheids, the SPIPS code allowed me to determine a linear relation between the p-factor and the pulsation period, resulting in a new calibration of the period-luminosity relation. These promising results of the SPIPS code suggest that the future releases of the Gaia satellite will unveil the nature of the p-factor, bringing the parallax of pulsation method to the forefront of in the calibration of the distance scale and the determination of the Hubble constant
饒勇 and Yong Rao. "The astronomical observation system of 12" telescope: its automatic control system and astronomical application." Thesis, The University of Hong Kong (Pokfulam, Hong Kong), 1997. http://hub.hku.hk/bib/B31214587.
Повний текст джерелаRao, Yong. "The astronomical observation system of 12" telescope : its automatic control system and astronomical application /." Hong Kong : University of Hong Kong, 1997. http://sunzi.lib.hku.hk/hkuto/record.jsp?B1877698X.
Повний текст джерелаJiang, Feng. "Capturing event metadata in the sky : a Java-based application for receiving astronomical internet feeds : a thesis presented in partial fulfilment of the requirements for the degree of Master of Computer Science in Computer Science at Massey University, Auckland, New Zealand." Massey University, 2008. http://hdl.handle.net/10179/897.
Повний текст джерелаCourt, A. J. "Hard X-ray astronomy from balloon altitudes." Thesis, University of Southampton, 1987. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.377796.
Повний текст джерелаMiret, Roig Núria. "COSMIC-DANCE : A comprehensive census of nearby star forming regions." Thesis, Bordeaux, 2020. http://www.theses.fr/2020BORD0327.
Повний текст джерелаUnderstanding how stars form is one of the fundamental questions which astronomy aims to answer. Currently, it is well accepted that the majority of stars form in groups and that their predominant mechanism of formation is the core-collapse. However, several mechanisms have been suggested to explain the formation of substellar objects, and their contribution is still under debate. The main goal of this thesis is to determine the initial mass function, the mass distribution of stars at birth time, in different associations and star-forming regions. The mass function constitutes a fundamental observational parameter to constrain stellar and substellar formation theories since different formation mechanisms predict different fraction of stellar and substellar objects. We used the Gaia Data Release 2 catalogue together with ground-based observations from the COSMIC-DANCe project to look for high probability members via a probabilistic model of the distribution of the observable quantities in both the cluster and background populations. We applied this method to the 30 Myr open cluster IC 4665 and the 1 - 10 Myr star-forming region Upper Scorpius (USC) and r Ophiuchi (r Oph). We found very rich populations of substellar objects which largely exceed the numbers predicted by core-collapse models. In USC, where our sensitivity is best, we found a large number of free-floating planets and we suggest that ejection from planetary systems must have a similar contribution than core-collapse in their formation. The age is a fundamental parameter to study the formation and evolution of stars and is essential to accurately convert luminosities to masses. For that, we also presented a strategy to study the dynamical traceback age of young local associations through an orbital traceback analysis. We applied this method to determine the age of the b Pictoris moving group and in the future, we plan to apply it to other regions such as USC. The members we identified with the membership analysis are excellent targets for follow-up studies such as a search for discs, exoplanets, characterisation of brown dwarfs and free-floating planets. I this thesis, we presented a search for discs hosted by members of IC 4665 and we found six excellent candidates to be imaged with ALMA or the JWST. The tools we developed, are ready to be used in other regions such as USC and r Oph, where we expect to find a larger number of disc-host stars
Leverington, David. "The cost and citation-based effectiveness of observational astronomical facilities since 1958." Thesis, Open University, 1997. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.363964.
Повний текст джерелаBellagamba, Fabio <1983>. "Testing future weak lensing surveys through simulations of observations." Doctoral thesis, Alma Mater Studiorum - Università di Bologna, 2012. http://amsdottorato.unibo.it/4762/.
Повний текст джерелаSasyn, Jan. "Staniční testování Mobilního automatizovaného astronomického systému." Master's thesis, Vysoké učení technické v Brně. Fakulta stavební, 2013. http://www.nusl.cz/ntk/nusl-226224.
Повний текст джерелаSantiago, Arthur Vinícius Resek. "O potencial da observação no ensino de astronomia: o estudo do conceito de energia." Universidade de São Paulo, 2015. http://www.teses.usp.br/teses/disponiveis/81/81131/tde-10092015-155110/.
Повний текст джерелаIn view of the strong relationship between Astronomy and Physics the proposed research aims to focus on a teaching activity that starts from the sky observation with an understanding motivation that lies beyond admiration and bewilderment and that may lead to the elaboration of school Physics concepts. The research deals with the investigation of a way of developping the concept of energy, starting from astronomical observations where students take active part in their learning process. A didactic sequence was elaborated and applied to secondary school students at a São Paulo public school. The objective was to motivate students to observe a celestial phenomenom, namely lunar craters, in order to build up the concept of mechanical energy in a process with the following steps: observation, obtention of related and adequate data, possible hypothesis and verification with a school laboratory controlled experiment. All activities were recorded in audio or video and with the aid of transcriptions a textual discursive analysis was effected. This analysis enabled a qualification of observations under several points of view as well as disclosing conceptions that were expressed in an atempt to model, in the school laboratory, a possible cause for the observed craters. The role played by the teacher during the whole process was essential as a moderator; his attention to follow the students argumentation and drive activities seems to have secured learning results. Vigotski theory was considered for interpreting results respect to construction of concepts. As results were obtained classes of observations made by the students, leaving a Primary Observation, evolving into a Qualified Observation. And what are the relationships that are established to investigate a problem that the mechanical energy concept create meaning to the student, relations between quantities and the concept, to the third degree of relationship, between concept and phenomenon.
Daigle, Olivier. "Spectro-imagerie optique à faible flux et comparaison de la cinématique Hα et HI d'un échantillon de galaxies proches". Aix-Marseille 1, 2010. http://www.theses.fr/2010AIX10141.
Повний текст джерелаA new EMCCD (Electron multiplying Charge Coupled Device) controller is presented. It allows the EMCCD to be used for photon counting by drastically taking down its dominating source of noise : the clock induced charges. A new EMCCD camera was built using this controller. It has been characterized in laboratory and tested at the observatoire du mont Mégantic. When compared to the previous generation of photon counting cameras based on intensifier tubes, this new camera renders the observation of the galaxies kinematics with an integral field spectrometer with a Fabry-Perot interferometer in Ha light much faster, and allows fainter galaxies to be observed. The integration time required to reach a given signal-to-noise ratio is about 4 times less than with the intensifier tubes. Many applications could benefit of such a camera: fast, faint flux photometry, high spectral and temporal resolution spectroscopy, earth-based diffraction limited imagery (lucky imaging), etc. Technically, the camera is dominated by the shot noise for flux higher than 0. 002 photon/pixel/image. The 21 cm emission line of the neutral hydrogen (HI) is often used to map the galaxies kinematics. The extent of the distribution of the neutral hydrogen in galaxies, which goes well beyond the optical disk, is one of the reasons this line is used so often. However, the spatial resolution of such observations is limited when compared to their optical equivalents. When comparing the HI data to higher resolution ones, some differences were simply attributed to the beam smearing of the HI caused by its lower resolution. The THINGS (The HI Nearby Galaxy Survey) project observed many galaxies of the SINGS (Spitzer Infrared Nearby Galaxies Survey) project. The kinematics of THINGS will be compared to the kinematic data of the galaxies obtained in Ha light. The comparison will try to determine whether the sole beam smearing is responsible of the differences observed. The results shows that intrinsic dissimilarities between the kinematical tracers used are responsible of some of the observed disagreements. The understanding of theses differences is of a high importance as the dark matter distribution, inferred from the rotation of the galaxies, is a test to some cosmological models
Jalovecký, Martin. "Analýza přesnosti výsledků astronomického určení polohy." Master's thesis, Vysoké učení technické v Brně. Fakulta stavební, 2012. http://www.nusl.cz/ntk/nusl-225609.
Повний текст джерелаMarinoni, Silvia <1975>. "Procedures of quality control and data analysis of multi-site ground-based observations for the absolute flux calibration of Gaia." Doctoral thesis, Alma Mater Studiorum - Università di Bologna, 2011. http://amsdottorato.unibo.it/3707/.
Повний текст джерелаGarcia, Garcia Carlos. "Theories of gravitation confronted with cosmological observations." Doctoral thesis, Universitat de Barcelona, 2020. http://hdl.handle.net/10803/670878.
Повний текст джерелаEsta tesis estudia la energía oscura, un tema central en la Cosmología Moderna, desde diferentes puntos de vista. Cubre desde modelos y parametrizaciones, hasta aproximaciones de la likelihood de observaciones de la Estructura a Gran Escala del Universo (LSS), vitales para constreñir los modelos, como para nuestro estudio de la tensión en S8. El modelo estudiado es el de energía oscura de α-attractors, que reproduce las observaciones actuales al poder asemejarse a una constante cosmológica. Inspirado en la clase de modelos de inflación favorecidos por Planck, α-attractors, enlaza el periodo de inflación y energía oscura mediante el mismo campo escalar. Afortunadamente, las misiones futuras podrían diferenciarlo de ΛCDM con hasta 3σ de confianza. No obstante, aprovechar al máximo los datos futuros requiere un formalismo que nos permita comprobar la viabilidad de los modelos eficientemente, como una parametrización acotada observacional y teóricamente. Mostramos el caso de w0-wa para quintaesencia de tipo thawing, que reproduce los observables desde recombinación hasta hoy, si se eligen apropiadamente. Construidas sus distribuciones de probabilidad bajo condiciones puramente teóricas, nos permiten restringir las cotas observacionales a la zona teóricamente motivada. Este trabajo es una muestra de cómo podemos trabajar con teorías muy generales como Horndeski. Pero las cotas observacionales dependen también de una correcta estimación de su likelihood. Por ello, hemos desarrollado (e implementado en NaMaster, del LSST DESC) la Narrow Kernel Approximation (NKA) para la parte gausiana (causalmente no conectada) de la covarianza de los pseudo-Cl de LSS. Ésta permite obtener con exactitud las cotas en los parámetros cosmológicos, al tiempo que reduce el coste computacional de O(lmax⁶) (cómputo exacto) a O(lmax3). Claramente, el cómputo exacto es inviable para las observaciones futuras de LSS que resolverán escalas muy pequeñas. La NKA nos ha permitido empezar a estudiar el origen de la tensión en S8 reportada por KiDS-450. Con datos de LSS de DES y del CMB de Planck, pretendemos obtener la evolución temporal de S8 y compararla con la dada por los datos de KiDS-450. En resumen, esta tesis ha trabajado en modelos de energía oscura y desarrollado métodos precisos para comprobar su viabilidad de manera eficiente. Además, se ha acercado a los datos y desarrollado la NKA que permite estimar precisamente la likelihood para LSS; permitiéndonos estudiar el origen de la tensión en el parámetro S8.
Simon, Paula Cristina da Silva Gonçalves. "Ensino de astronomia para os anos iniciais : uma proposta a partir da observação da lua." Universidade Federal de São Carlos, 2016. https://repositorio.ufscar.br/handle/ufscar/9062.
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This research presents results of an investigation of educational pedagogy done with a group of second grade students from an Elementary School. The investigation involved observations of the Moon and educational activities used to teach about Moon phases. An overview of the academic literature on the teaching of the theme of the Moon and its phases was conducted, with a bibliographical review of theses and dissertations, journal articles, papers presented at selected conferences, and some international papers on this topic. From the literature review, it was found that there are few studies that actually address of how observation of the Moon in the sky can be used to effectively teach Moon phases to elementary school students. In this study, students observed and recorded the appearance of the Moon and its place in the sky through drawings. The drawings included the position of the Moon relative to the horizon and used observations made at the school and at their homes during part of a lunar month. Using these initial Moon observations and the student drawings, there were discussions in the classroom designed to consolidate student knowledge. In this research, the data were obtained through interviews, class records, and student observations notebooks. A control group was not used. The researcher was also the teacher of the class where the research was developed. The student observations made it possible for the students to perceive the Moon's apparent motion, as well as its change of appearance over several nights. Through classroom discussions centered on the observations, it was clear that the observations helped develop student concept knowledge of Moon phases that would be difficult to develop from classroom experiences that did not include observations. This experiential connection from the observation of the Moon fostered a relationship with the knowledge implied to the reality of nature. For the initial years, in the Astronomy teaching, this is an important link that can promote the learning of such contents, from the senses of the child and the teacher intervention in a flexible and open way.
Esta pesquisa apresenta resultados de uma investigação desenvolvida com uma turma de alunos do segundo ano do Ensino Fundamental envolvendo a observação da Lua. Inicialmente, com o objetivo de apresentar um panorama das pesquisas sobre o tema Lua e suas fases, foi feita uma revisão bibliográfica a partir de teses e dissertações, artigos de periódicos, trabalhos apresentados em eventos selecionados e alguns trabalhos internacionais. Como resultado, verificou-se que poucos são os trabalhos que utilizam a observação da Lua no céu como parte da metodologia para o ensino e a aprendizagem do tema. Como objetivo de pesquisa, foi proposta e estudada uma metodologia na qual os alunos observaram e registraram a Lua por meio de desenhos, incluindo o horizonte, na escola e em suas casas, ao longo de parte de uma lunação. Priorizando a observação do céu, a partir dos desenhos, houve discussões em sala que foram conduzidas objetivando a sistematização do conhecimento. Com uma pesquisa experimental, sem grupo de controle, os dados foram obtidos por meio de entrevistas, registros de aulas e cadernos de observações dos alunos. A pesquisadora também foi a professora da turma onde a pesquisa foi desenvolvida. A observação do céu possibilitou a percepção pelos alunos do movimento aparente da Lua, bem como sua mudança de aspecto ao longo de várias noites. Por meio das discussões em sala de aula, com o uso dos registros, foi evidenciado que o conhecimento da observação desenvolve um saber a partir da vivência que transcende os limites dados ao conteúdo em sala de aula, possibilitando discussões pouco valorizadas no ensino da Lua e suas fases. Essa conexão experiencial a partir da observação da Lua fomenta uma relação com o conhecimento implicado à realidade da natureza. Para os anos iniciais, no ensino de Astronomia, esta é uma vinculação importante que pode promover a aprendizagem de tais conteúdos, a partir dos sentidos da criança e da intervenção docente de modo flexível e aberto.
Bretones, Paulo Sergio. "A astronomia na formação continuada de professores e o papel da racionalidade pratica para o tema da observação do ceu." [s.n.], 2006. http://repositorio.unicamp.br/jspui/handle/REPOSIP/287062.
Повний текст джерелаTese (doutorado) - Universidade Estadual de Campinas, Instituto de Geociencias
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Resumo: Este trabalho analisa o avanço propiciado por um projeto de fonnação continuada para professores do ensino fundamental com o tema observação do céu em Astronomia, levando-se em conta as especificidades do conhecimento, o referencial do professor reflexivo e as práticas de tutoria. Para isto, foi realizado um curso de Astronomia para professores de Ciências e Geografia de 5' a 8' séries, com 46 horas, promovido em 2002 pelo Instituto Superior de Ciências Aplicadas (ISCA) em Limeira. Após o curso foi estabelecido um grupo de estudos e realizadas cinco reuniões.Os dados foram obtidos por meio de avaliações, entrevistas, relatos dos participantes e registros das aulas e reuniões. São apresentados movimentos de sugestões de atividades extrac1asse, ações pessoais dos participantes sem seus alunos, relatos de ações extrac1asse e desenvolvimento de conteúdos astronômicos em aula, ações na prática pedagógica e reflexões dos participantes junto ao professor/pesquisador na avaliação de tais movimentos.Foram investigadas as mobilizações em ações e concepções dos participantes e o papel da, racional idade prática ao longo do programa.Verificou-se que o tema da observação do céu tem caracteristicas específicas na Astronomia que levam a uma prática escolar também específica em que os conteúdos e procedimentos por serem calcados na observação e sua representação solicitam uma prática escolar baseada na racionalidade prática. Mesmo um curso de fonnação de professores baseado inicialmente na racionalidade técnica, ao dar conta da observação do céu, adentra na racionalidade prática e no desenvolvimento próprio de princípios que norteiam a aquisição e o ensino dos conhecimentos referentes à observação do céu. Também se verificou que, para a observação do céu, o modelo da racionalidade prática no referencial do professor reflexivo e ações de tutoria levam à aquisição de conhecimentos, mudanças de concepções e ações extraclasse. Evidenciaram-se os aspectos da prática como ponto de partida, eixo e sua relação com a teoria. Particularmente ao conteúdo de movimento diário da esfera celeste, estabeleceram-se os princípios de relação da altura do pólo com a latitude geográfica, obliqüidade, continuidade do movimento, circularidade, tridimencionalidade e ciclicidade. Também se evidenciaram os aspectos de criatividade e desenvolvimento do pensamento prático dos participantes, com fatores que levam à caracterização de saberes plurais, que têm temporal idade e mostrando que a aquisição de conhecimento é seletiva, ou seja, situada e hierarquizada
Abstract: This work analyzes the advance spread by a project il! the continuing education training of high school teachers who teach the fundamentaIs of Astronomical sky observation, taking into account specitic knowledge, the reflective teacher &amework and tutoring practice.Base on this, a 46 hour Astronomy course was offered to Science and Geography teachers in the four last years of high school organized in 2002 by the Instituto Superior de Ciências Aplicadas in Limeira, Brazil. Following the course a study group was established and tive meetings were held.The data was obtained through assessments, interviews, and accounts by the teachers and records from the classes and meetings. Examples are: suggestions, personal actions of the teachers without their students, accounts of extracurricular activities and development of astronomical contents in class, actions in the pedagogical practices and reflections of the teachers with the teacher/researcher towards the assessment of such changes are shown.The actions and conceptual changes and the role of the practical rationality were then investigated. It was established that sky observation has specitic features that lead to an equally specific school practice, in which the contents and procedures based on observations and their representation point towards a more practical rationality. Even in a training course for teachers based on technical rationality, the introduction of sky observation deepens the practical rationality and the development of principIes that guide the acquisition and the teaching of knowledge about sky observation.It was also established that for sky observation the model of practical rationality, within the reflective teacher theoretical &amework and tutorial actions, leads to knowledge acquisition, conceptual changes and extracurricular activities.It was clear that the aspects of practice act as starting point, axis, and a relation with the theory. In particularly with regard to the daily motion of celestial sphere content, the principIes of relation of the elevation of the celestial pole to geographic latitude was established, obliquity, continuity of motion, circularity, tri-dimensionality and cyclicity. AIso established were the aspects of creativity and development of practical thinking of the participants, with factors that lead to the characterization of pluraIs knowledge, that have temporality and show that the knowledge acquisition is selective or situated and hierarchical
Doutorado
Doutor em Ensino e História de Ciências da Terra
Aleksic, Jelena. "Optimized DarkMatter Searches in Deep Observations of Segue 1 with MAGIC." Doctoral thesis, Universitat Autònoma de Barcelona, 2013. http://hdl.handle.net/10803/117858.
Повний текст джерелаThere is an impressive amount of evidence, on all scales, favouring the existence of dark matter - an invisible, non-baryonic component of the Universe that accounts for almost 85% of its total mass density. Although its existence was for the first time postulated more than 80 years ago, the nature of dark matter still remains a mystery. Finding and understanding the answer to this question is one of the most important and exciting tasks of modern science. In the context of our current cosmological view of the Universe, dark matter is considered to be a new type of massive particle, that interacts weakly with ordinary matter and radiation. In addition, this new particle is most likely cold, non-baryonic, produced thermally in the early Universe and stable on cosmological scales. Our search for dark matter particle is carried out in parallel by three different approaches: detection of dark matter produced in colliders, direct detection of dark matter scattering off ordinary matter in underground experiments, and indirect search with space and ground-based observatories for Standard Model particles created in dark matter annihilation or decay. This last strategy is the subject of this Thesis. Results presented here are from indirect searches for dark matter in dwarf spheroidal galaxy Segue 1, carried out with the Imaging Air Cherenkov Telescopes called MAGIC. The objective is to recognize highly energetic photons, produced in annihilation or decay of dark matter particles, by some characteristic spectral features unique for gamma rays of dark matter origin. An dedicated analysis approach, called the full likelihood method, has been developed to optimize the sensitivity of the analysis for such dark matter signatures. The outline of the Thesis could be summarized as follows: • Chapter 1 introduces the dark matter paradigm: what are the astrophysical and cosmological evidence supporting the existence of dark matter, and how can they be reconciled with our current image of the evolution of the Universe. The Chapter ends with review of some of the best motivated candidates for dark matter particle, with detailed discussion about those that are of particular interest for this work. • Chapter 2 is devoted to dark matter searches. It begins with presentation of different strategies currently employed by various experiments and their most worth noting results, to continue with more detailed description of indirect searches. Special attention is devoted to the highly energetic photons as search messengers: what signal should be expected, where to look for it and with which instruments. • Chapter 3 introduces this work's tool for dark matter searches - the MAGIC Telescopes. Chapter is divided into two parts: one, describing the technical properties of the system, and the other, characterizing its standard analysis chain. • Chapter 4 presents the original scientific contribution of this work - the development of the full likelihood approach, an analysis method optimized for recognition of spectral features expected from photons of dark matter origin. First, the method is introduced, then characterized for the pre-defined sets of conditions and its performance evaluated for particular spectrum examples. • Chapter 5 brings the results of this work. First, the motivation behind the Segue 1 galaxy as the optimal dark matter candidate for searches with MAGIC is presented. Then, details of the carried observations and data reduction are summarized. This is followed by the full likelihood analysis of the data. Finally, this Chapter ends with the constraints obtained from this work for different models of dark matter annihilation decay. Brief summary of the most relevant points of this Thesis is presented in Conclusions.
Oliveira, Fabiana Andrade de [UNESP]. "Investigando o desenvolvimento de práticas reflexivas de professores em um curso de formação continuada em astronomia voltado à observação do céu." Universidade Estadual Paulista (UNESP), 2016. http://hdl.handle.net/11449/145005.
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Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES)
A presença de dificuldades associadas ao ensino de astronomia nas escolas, a falta de contato de professores com esta Ciência durante a formação inicial e a necessidade de formar indivíduos cientes a respeito do céu noturno, levaram a necessidade de um curso de formação continuada com ênfase na observação do céu. Esta pesquisa envolve o estudo de um curso de formação continuada em astronomia com relação ao desenvolvimento profissional reflexivo de professores. Nesse sentido, buscamos responder à questão principal: Que indícios do desenvolvimento de práticas reflexivas emergem durante um curso de formação continuada em astronomia? Com efeito, os movimentos realizados em prol de um diálogo entre teoria e prática deram-se a partir do trabalho colaborativo entre os professores e pesquisadora, sendo o processo reflexivo sustentado sob três aspectos: uma situação prática desses professores, reflexões em coletivo e apresentação de pesquisas acadêmicas sobre ensino de astronomia. Os dados foram constituídos a partir de um questionário e grupos focais realizados em dois encontros com os professores. Apoiando-se metodologicamente na Análise de Conteúdo, os resultados apontam para indícios da contribuição do curso com relação ao desenvolvimento de práticas reflexivas. Dessa forma, ultimamos que as condições de reflexão em coletivo mostraram-se efetivas ao permitir que situações reais de ensino fossem discutidas e estudadas entre os pares, possibilitando também o envolvimento dos professores nas decisões em relação ao curso. Alguns deles acreditam que as teorias não atendem às suas necessidades formativas, uma vez que estão distantes dos problemas que vivenciam na prática. Em contrapartida, outros professores entendem que há fatores limitantes quanto às condições de estudo e melhorias profissionais. Na visão de alguns professores as atividades práticas desenvolvidas ao longo dos encontros foram relevantes, pois consistem em estratégias e metodologias que viabilizam a abordagem da astronomia no contexto da sala de aula. Os resultados desta pesquisa mostram que os professores apresentam preocupações de ordem prática, relacionadas ao contexto da sala de aula e à aprendizagem dos alunos.
There are some difficulties associated with the teaching of astronomy in schools, the lack of contact of teachers with this Science during initial formation and the need to train individuals aware of the night sky, led to the need for a continuing education course with emphasis on watching the sky. This research involves the study of a continuing astronomy training course in relation to the reflective professional development of teachers. In this sense, we seek to answer the main question: What signs of the development of reflexive practices emerge during a course of continuing formation in astronomy? In fact, the movements carried out in favor of a dialogue between theory and practice were based on collaborative work between teachers and researcher, and the reflexive process was sustained under three aspects: a practical situation of these teachers, reflections in collective and presentation of Academic research on astronomy teaching. The data were constituted from a questionnaire and focus groups conducted in two meetings with the teachers. By supporting methodologically in Content Analysis, the results point to indications of the course's contribution to the development of reflective practices. Thus, we conclude that the conditions of collective reflection have proved to be effective in allowing real teaching situations to be discussed and studied among peers, thus enabling the involvement of teachers in decisions related to the course. Some of them believe that the theories do not meet their training needs, since they are far from the problems they experience in practice. On the other hand, other teachers understand that there are limiting factors regarding the conditions of study and professional improvements. In the view of some teachers, the practical activities developed during the meetings were relevant, since they consist of strategies and methodologies that enable the approach of astronomy in the context of the classroom. The results of this research show that teachers present practical concerns related to the context of the classroom and student learning.
Añez, López José Ignacio. "Observational and theoretical perspective of massive star formation." Doctoral thesis, Universitat de Barcelona, 2021. http://hdl.handle.net/10803/671784.
Повний текст джерелаEn esta tesis, pretendemos contribuir a explicar el proceso de formación de estrellas masivas prestando especial atención al papel del campo magnético. Para ello, realizaremos un análisis multiescala con una doble aproximación, teórica y observacional. Por un lado investigaremos el proceso de acrecimiento a través de un disco de acrecimiento entorno a una estrella de alta masa. a) El papel del campo magnético en el proceso de fragmentación: el caso de G14.225-0.506 En este primer trabajo, estudiamos la fragmentación de una nube oscura infrarroja que presenta una estructura filamentaria y dos hubs. Prestaremos especial atención al campo magnético presente en el entorno de los hubs y trataremos de relacionarlo con los distintos niveles de fragmentación que presentan estos hubs. Para poder llevar a cabo este estudio presentamos el resultado de las observaciones del CSO a 350 masas solares, hacia ambos hubs, Norte y Sur, en la nube oscura infrarroja G14.225-0.506 (desde aquí G14.2). También mostramos el análisis de la polarización y gradiente de intensidad haciendo uso del método desarrollado por (Koch et al. 2012, Koch et al. 2012b). b) El modelado del disco de acrecimiento entorno a la protoestrella masiva GGD 27-MM1 En este segundo proyecto, descendemos hasta escalas de discos de acrecimiento para entender como las estrellas masivas se forman y evolucionan. En este trabajo hemos usado observaciones de ALMA a una longitud de onda de 1.14 mm con muy alta resolución angular (aproximadamente 40 mili-segundos de arco) que resuelven el disco entorno a la estrella masiva GGD27-MM1. El disco se dispone perpendicularmente al espectacular chorro de 10 pc de longitud que emana de la fuente, conocido como HH80-81. Motivados por el parecido de este sistema a los que encontramos en baja masa, hemos modelado la emisión del disco haciendo uso de los modelos desarrollados por D'Alessio et al. 2006 para estrellas de baja masa.
Cea, del Pozo Elsa de. "Some observational and theoretical aspects of cosmic-ray diffusion." Doctoral thesis, Universitat Autònoma de Barcelona, 2011. http://hdl.handle.net/10803/51003.
Повний текст джерелаThis Thesis deals with certain aspects on cosmic-ray diffusion. It is divided in two parts, one describes phenomenological models of cosmic-ray diffusion, and the other presents observations taken with the MAGIC experiments and simulations of the future Cherenkov Telescope Array (CTA). In the first part, the generally accepted theory for cosmic-ray diffusion is introduced. Supernova remnants (SNRs) are believed to be the more likely scenarios of cosmic-ray acceleration, considering both hadronic and leptonic processes. The mechanism for particle acceleration in each SNR is assumed to be diffusive shock acceleration (DSA). To obtain the observational confirmation of proton and nuclei acceleration, and distinguish it from leptonic emission, the effects of multiple messengers produced by secondary particles must be isolated. Following this, a model for the neighborhood of the SNR IC443 is developed, explaining the high energy phenomenology: cosmic rays escape from the remnant, the most energetic ones reach first the molecular cloud located in front of it and the least energetic ones still remain confined on the shell of the SNR. The results are confronted with the latest observations that are obtained from this source. The apparent displacement between high and very high energy detected sources is explained thanks to this model. Moreover, a multi-frequency and multi-messenger model (i.e., photons from the whole electromagnetic spectrum and neutrinos) for the diffuse emission coming from the starburst galaxy M82 is presented. The gamma-ray predictions are compared to the posterior detections in the energy range between the giga- and the tera-electronvolts of the starburst galaxies M82 and NGC 253, observed by the satellite Fermi and the ground-based experiments H.E.S.S. and VERITAS. The model explains rather satisfactorily these detections at high and very high energy. In the second part of the Thesis, the technique for the gamma-ray detection at ground level through Cherenkov radiation is described. This Cherenkov technique is used in the MAGIC experiment, among others. Some of the observations taken by the student with this telescope facility are presented as part of this Thesis. First, the upper limits to the gamma-ray flux coming from two sources in the region of the SNR G65.1+0.6 when observed with MAGIC-I are shown. These two sources were previously detected by the Milagro experiment and are associated with two bright sources in the Fermi catalog. One of the possible explanations is that these sources are two pulsars powering the pulsar wind nebula that surrounds them. Furthermore, preliminar results of the stereo observations (using the two MAGIC telescopes) of the SNR IC443 are presented. The goal for these observations is performing an energy-dependent morphological study. So far, the obtained number of hours is not enough, although new observations are planned for the near future. Finally, some simulations for the future CTA are presented for the first time, together with several spectral studies regarding interesting scientific cases. In particular, those studies are focused on objects that have been already mentioned in this Thesis, like the SNR IC443 and the starburst galaxies M82 and NGC 253, and also on molecular clouds that are illuminated by cosmic rays which escaped from nearby SNRs. The CTA observatory represents the future of the ground-based gamma-ray observations, and it is likely to include every collaboration from the existing telescope facilities nowadays. The energy range will be widened, the sensitivity will be one order of magnitude improved and the angular resolution will be enhanced respect to the existing experiments up to now. Thus, the present Thesis is just the tip of the iceberg of what is yet to come.
Martín, Rodríguez Jonatan. "Theory & observations of the PWN-SNR complex." Doctoral thesis, Universitat Autònoma de Barcelona, 2014. http://hdl.handle.net/10803/283894.
Повний текст джерелаSoler, Daniel Rutkowski. "Astronomia no currículo do Estado de São Paulo e nos PCN: um olhar para o tema observação do céu." Universidade de São Paulo, 2012. http://www.teses.usp.br/teses/disponiveis/81/81131/tde-25022013-133229/.
Повний текст джерелаThe activity of observing the Sky is very important to obtain information about the vast majority of celestial objects, particularly those from outside our Solar System: there are no technological means nowadays that allow us to obtain such information on-site, whether through robotic probes or by manned spacecraft. Under this view, it is therefore important to offer children and teenagers the opportunity to participate in didactic activities of the Sky Observation, thus allowing them to have a first systematic contact with the Sky, consequently and essentially with the whole Universe that exists outside our planet. In this work we are concerned particularly with the teaching about the Sky Observation: we are interested in dealing with proposals about teaching, in which one teaches \'how to observe the Sky\'. Our main object of study is the current Curriculum of the State of São Paulo, more specifically the Teacher\'s textbooks, which constitute the set of educational materials related to such Curriculum. In this dissertation we propose to evaluate the didactic activities of Sky Observation that are proposed in the Teacher\'s textbooks for the discipline of Science in Elementary School and for Physics in High School. This evaluation was made from two viewpoints. First, the analysis was about the content present in the activities, which were compared with the National Curriculum Parameters by means of Concept Maps. The second point of the evaluation was made regarding the structure of activities. To support this analysis, a study was done with some research of the area of Astronomy Teaching from which we listed 6 dimensions related to the proposition of didactic activities about Sky Observation - \"Objects and observable phenomena\"; \"Conditions of observation, planning and preparation\", \"Audience, context and audience interactivity\", \"Main objectives of observation\"; \"Records of observations\"; and \"Types of observation and instruments\" - which were treated as important parameters in building such proposals, then being used as analytical categories of those present in the textbooks of the Curriculum of the State. The main results show that the contents linked to the practice of Sky Observation, both the PCN and the Curriculum of the State are significantly similar, even the restricted theme of Sky Observation to elementary schools. Moreover, the activities of the Sky Observation in the textbook seem to have internal consistency and tend to contemplate the results of research in Astronomy Education.
Domingo, Santamaría Eva. "(gamma)-ray emission from regions of star formation: Theory and observations with the MAGIC Telescope." Doctoral thesis, Universitat Autònoma de Barcelona, 2006. http://hdl.handle.net/10803/3374.
Повний текст джерелаTras una evaluación fenomenológica positiva de que la emisión de rayos gamma procedente de galaxias con elevada actividad en formación estelar (como las llamadas starburst o las galaxias ultra luminosas en el infrarrojo) esté cerca de la sensibilidad de los actuales detectores de rayos gamma, se han desarrollado y presentado modelos detallados de la emisión difusa multifrecuencia procedente de los dos mejores candidatos, NGC 253 y Arp 220. Se predice que ambas galaxias serán detectables para GLAST, el próximo satélite de rayos gamma con una sensibilidad sin precedentes, y por HESS y MAGIC, los actuales telescopios Cherenkov con mayor sensibilidad, en caso de que éstos dediquen suficiente tiempo de observación a estas galaxias.
En la parte teórica de la tesis se describe también un modelo que propone la emisión de importantes flujos de rayos gamma en regiones de formación estelar dentro de nuestra Galaxia, como serían las asociaciones de estrellas jóvenes del tipo OB. El modelo considera la emisión de rayos gamma a energías cercanas a los TeV mediante interacciones hadrónicas en el sí de vientos estelares de algunas de las estrellas de la asociación, prediciendo a la vez que la emisión a bajas energías está sustancialmente suprimida debido al efecto de modulación que la población de rayos cósmicos primarios sufre al penetrar en el viento estelar. Se discuten brevemente los mejores candidatos entre las asociaciones OB galácticas conocidas.
Finalmente, la tesis recoge un primer análisis de los datos tomados por el Telescopio MAGIC durante la observación de dos regiones de formación estelar. Por una parte, la galaxia ultra luminosa en el infrarrojo más cercana, Arp 220. Por otra parte, TeV J2032+4130, que aún hoy en día sigue siendo una fuente no identificada, y cuyo origen se ha relacionado con la poderosa asociación estelar Cygnus OB2 en repetidas ocasiones. Ninguna de las observaciones ha implicado detección, en consecuencia, se han impuesto límites superiores al flujo de rayos gamma procedente de las fuentes observadas. Sin embargo, a pesar de las pocas horas de observación incluidas en el presente análisis, los límites superiores impuestos por el Telescopio MAGIC para la fuente TeV J2032+4130 están prácticamente al nivel del flujo que el experimento HEGRA detectó para dicha fuente, de manera que un análisis extendido al conjunto completo de datos disponibles, así como futuras observaciones de más larga exposición con el Telescopio MAGIC, podrían proveer resultados interesantes.
Was the aim of this thesis to study the possibility that regions with important activity in star formation may appear as sources of gamma-rays for the current and near future gamma-ray detectors, both ground and space-satellite based.
After a phenomenological positive evaluation of the fact that the gamma-ray emission from galaxies prone of star formation processes (as starburst or ultra luminous infrared galaxies) may be close to the flux sensitivities of the current gamma-ray telescopes, detailed models of the multiwavelength diffuse emission from the two best candidates, NGC 253 and Arp 220, have been presented. It is predicted that they will be detectable by GLAST, the next largest gamma-ray satellite, and by HESS and MAGIC, the current more sensitive Cherenkov Telescopes, in case enough observation time is devoted.
On the other hand, within this thesis it is described a model which proposes the emission of important fluxes of gamma-rays from regions of star formation within our Galaxy, as the stellar association of young OB stars. The model considers the emission of gamma-rays close to TeV energies by hadronic interactions within the stellar winds of some of the stars of the association, predicting at the same time that the emission at lower energies is substantially suppressed due to the modulation effects that the incoming population of primary cosmic rays suffers when penetrating the winds. The best candidates among the galactic OB associations are briefly discussed.
Finally, a first analysis of the data taken by the MAGIC Telescope when observing two of these regions of star formation is described. On one hand, the closest ultra luminous infrared galaxy, Arp 220. On the other, TeV J2032+4130, which is still an unidentified source whose origin has been several times related to the powerful stellar OB association Cygnus OB2. Any of both observations has implied detection, and upper limits to the gamma-ray flux have been imposed. However, although the few hours of observation included in the present analysis, the MAGIC upper limits for TeV J2032+4130 are nearly at the level of the flux detected by the HEGRA experiment, so an analysis extended to the complete set of data available as well as deeper observations of this source with the MAGIC Telescope can provide promising results.
Marcote, Martin Benito. "Non-thermal emission from high-energy binaries through interferometric radio observations." Doctoral thesis, Universitat de Barcelona, 2015. http://hdl.handle.net/10803/336664.
Повний текст джерелаLas binarias de alta energía son sistemas que producen emisión de rayos X y/o rayos gamma, debido a la presencia de un entorno suficientemente energético como para acelerar partículas hasta velocidades relativistas. Sólo tres tipos de binarias han sido detectadas en rayos gamma de forma persistente: binarias con colisión de vientos, binarias de rayos X de alta masa o binarias de rayos gamma. Todas ellas involucran una estrella masiva (con una masa superior a 8 veces la masa solar) y a otra estrella masiva o a un objeto compacto. Esta tesis está centrada en el estudio de la emisión radio de estos sistemas a través de observaciones con radio interferómetros. Se han estudiado dos binarias de rayos gamma a bajas frecuencias (LS 5039 y LS I +61 303), obteniendo sus curvas de luz y espectros. Éstos nos han permitido determinar propiedades físicas de la región emisora, como el campo magnético, la tasa de pérdida de masa, o la velocidad de expansión de dicha región. También hemos revelado la presencia del efecto Razin en la parte absorbida del espectro de LS 5039, siendo la primera vez que se detecta en una binaria de rayo gamma. Además, se ha detectado por primera vez una binaria de rayos gamma, LS I +61 303, a una frecuencia tan baja como 150 MHz. También se ha estudiado la binaria de rayos gamma HESS J0632+057 con observaciones radio de muy alta resolución, aunque la misma no ha sido detectada. Se ha descubierto una nueva binaria con colisión de vientos, HD 93129A, a través de observaciones radio de muy alta resolución y observaciones ópticas. Por último, se han llevado a cabo observaciones radio de dos fuentes que eran candidatas a ser binarias de rayos gamma.
Moldón, Vara Francisco Javier. "Structure and nature of gamma-ray binaries by means of VLBI observations." Doctoral thesis, Universitat de Barcelona, 2012. http://hdl.handle.net/10803/96996.
Повний текст джерелаEn los últimos años se ha producido una mejora significativa de los instrumentos que permiten observar fenómenos astrofísicos en rayos gamma de alta y muy alta energía. Gracias a estos avances, se ha podido detectar emisión de rayos gamma en sistemas binarios. Tan sólo seis sistemas binarios han sido clasificados como estrellas binarias de rayos gamma (tres de ellos aún son candidatos). Estos sistemas producen chorros de material relativista que a su vez producen grandes cantidades de energía en todo el espectro electromagnético, desde ondas radio hasta emisión de rayos gamma hasta energías del teraelectronvolt (TeV). Estos chorros se desplazan a alta velocidad produciendo estructuras en escalas de varias unidades astronómicas (UA). Estas estructuras pueden ser observadas directamente mediante técnicas de interferometría radio de muy larga línea de base (VLBI). En esta tesis nos centramos en el estudio de las propiedades morfológicas y astrométricas de binarias de rayos gamma observadas mediante VLBI. De las seis binarias conocidas, se han observado cinco de ellas. Los resultados principales son los siguientes. Se ha detectado estructura extendida en escalas de 120 UA en el sistema binario PSR B1259-63. Esta ha sido la primera evidencia observacional de que púlsares jóvenes no acretantes interaccionando con estrellas jóvenes pueden producir emisión radio extendida. Se ha descubierto que la emisión del sistema LS 5039 muestra cambios periódicos en su morfología, que son estables en escalas de varios años. También se ha determinado el movimiento propio de este sistema y se ha obtenido su trayectoria galáctica en el pasado. Se ha confirmado que el sistema LS I +61 303 muestra variabilidad orbital periódica, aunque presenta cambios significativos en ciertas fases orbitales. Se ha encontrado un desplazamiento del pico de la emisión a varias frecuencias, así como un cambio en sus posiciones relativas. Se ha descubierto emisión extendida procedente de la fuente de rayos gamma HESS J0632+057, y se ha confirmado inequívocamente su asociación con el sistema binario MWC 148. Por último, no se ha encontrado contrapartida radio a la fuente de rayos gamma AGL 2241+4454, cuya contrapartida óptica ha sido propuesta en el sistema MWC 656. Estos resultados permiten sentar las bases de la estructura en escalas de varias UA de los sistemas binarios de rayos gamma, así como su comportamiento en función de la fase orbital. Las características comunes halladas en estos sistemas ha permitido encontrar enlaces observacionales entre estos sistemas, dando consistencia a este particular grupo de estrellas que presentan emisión en rayos gamma.
Molina, Lumbreras Edgar. "Modeling and observations of relativistic outflows in high-energy binary systems." Doctoral thesis, Universitat de Barcelona, 2021. http://hdl.handle.net/10803/672686.
Повний текст джерелаA la nostra Galàxia, existeixen sistemes binaris formats per un objecte compacte i una estrella companya típicament no degenerada que emeten a freqüències des de ràdio fins a raigs gamma. Les interaccions entre l'estrella i l'objecte compacte poden resultar en el llançament d'outflows de plasma originats al voltant de l'objecte compacte, els quals poden adquirir velocitats properes a la de la llum. Quan l'estrella companya és molt massiva, aquesta genera un fort vent estel·lar que interacciona amb els outflows i els afecta tant dinàmicament com radiativa. El principal objectiu d'aquesta tesi des del punt de vista teòric és l'estudi de les interaccions entre els outflows de sistemes binaris i el vent estel·lar d'una companya massiva. Per això, hem desenvolupat una sèrie de models semi- analítics que donen una visió completa d'aquestes interaccions en diferents tipus d'escenaris. Els resultats de la modelització teòrica inclouen prediccions per a les distribucions espectrals d'energia i corbes de llum, així com mapes ràdio per a l'emissió a gran escala dels outflows. En relació a la part observacional, aquesta tesi es focalitza en l'anàlisi de l'emissió potencial de raigs gamma de molt alta energia de la binària MAXI J1820+070, observada amb els telescopis MAGIC. Els resultats observacionals consisteixen en un estudi multifreqüència de la font de ràdia a raigs gamma. Tot i que la font no es detecta per sobre dels 100 MeV, els resultats obtinguts permeten limitar les propietats d'un emissor potencial de raigs gamma a MAXI J1820+070. En conclusió, aquesta tesi profunditza en el coneixement de les interaccions entre el vent estel·lar i els outflows de sistemes binaris d'altes energies. També es conclou que les observacions en raigs gamma de sistemes binaris permeten limitar de manera important les propietats dels outflows, fins i tot quan les fonts no son detectades.
Tescaro, Diego. "TeV γ-ray observation of nearby Active Galactic Nuclei with the MAGIC telescope: exploring the high energy region of the multiwavelength picture." Doctoral thesis, Universitat Autònoma de Barcelona, 2010. http://hdl.handle.net/10803/3428.
Повний текст джерелаLa tesis sigue con tres capítulos que discuten las técnicas experimentales para elestudio de los rayos gamma.La técnicas de detección de rayos gamma, y los distintos tipos de detectores, sonanalizados primero (capitulo 4), prestando una atención especial a la explicación de latécnica de detección conocida como "IACT". Los telescopios MAGIC (capitulo 5) y susubsecuente cadena de análisis de datos (capitulo 6) son el tema de los siguientes capítulos, siendo los datos experimentales de la tesis tomados con precisamente estedetector (en el marco de trabajo de la colaboración MAGIC).
Los dos capítulos siguientes relatan los resultados astrofísicos obtenidos durante la miinvestigación doctoral.Las medidas del flujo de rayos gammas en la banda "VHE" (muy alta energía) desdetres famosos objetos astrofísicos (extra-galácticos), Markarian 421 y Markarian 501, enel marco de las mas completas campañas multifrecuencias realizadas en esto objetos (capitulo 7), y Messier 87, durante una fase muy activa en la banda de energía gamma(capitulo 8).
Finalmente dos apéndices describen las dos mas relevantes tareas técnicas en queestuve involucrado durante mi doctorado. La primera es el desarrollo de una nueva técnica de análisis por los datos de MAGIC,técnica que usa el tiempo de llegada de las señales ademas de su intensidad (apéndiceA). La segunda es el desarrollo del software de adquisición de datos para el telescopioMAGIC-II (apéndice B), el segundo telescopio del sistema de detección conocido ahoracomo: 'MAGIC Florian Goebel Telescopes'.
The first three chapters of this thesis provide an introduction to the relevant physics topics discussed, starting from the basic notions and open questions about the Cosmic Rays (chapter 1), going through the achievements of the young branch of Astrophysics known as gamma-ray Astronomy (chapter 2), and focusing finally on the astrophysicalobjects which are the subject of this thesis: the Active Galactic Nuclei (chapter 3).
We propose then three chapters that discuss the experimental approach to the subject.The gamma-ray detection techniques and the type of detectors are first discussed(chapter 4), paying special attention to the explanation of the IACT technique.The MAGIC telescope(-s) (chapter 5) and its data analysis procedure (chapter 6) arethen discussed in detail, since the astrophysical measurements shown on this thesis areobtained in this framework.
The next two chapters report on the physics results obtained in the course of my research. The measurement of the VHE gamma-ray flux of three famous extragalactic sources,namely Markarian 421 and Markarian 501, in the context of the up to date mostcomplete multiwavelength campaigns ever organized on this type of objects (chapter 7),and Messier 87 during an important flaring activity (chapter 8).
Finally, two appendices describe the most relevant technical developments to which Iwas committed during my PhD.The first is the development of a novel method for the analysis of the MAGIC telescopedata which makes use of the time information in the Cherenkov images (appendix A).The second is the development of the data acquisition software for MAGIC-II (appendix B), the second telescope of the 'MAGIC Florian Goebel Telescopes' array.
Costa, Gleice Kelen Dornelles. "A observação do céu nos livros didáticos de ciências aprovados no PNLD/2017." Universidade de São Paulo, 2018. http://www.teses.usp.br/teses/disponiveis/81/81131/tde-23112018-142104/.
Повний текст джерелаObservation of the cosmos dates back to antiquity, and its perpetual presence in basic education is defended by researchers. The observational character can be used as a didactic strategy for the student to enhance the perception of their astronomical environment, being able to recognize phenomena that are part of their daily life, either with or without the use of instruments. However, direct sky observation activities require time (times and schedules of events) and locations (outdoors, outside the classroom) that contrast from the traditional school system, in addition to required atmosphere conditions. This research intends to analyze and understand the nature of the activities when observing the sky while in Elementary School, in the discipline of Sciences for the final years, through textbook study. This material constitutes an element of significant importance within the school context, influencing the work of the teacher and student activity, both at school and at home. Nine collections of science textbooks, distributed nationally through the National Textbook Program / 2017, were analyzed. The analysis was subsidized by the construction of a set of elements considered fundamental for the implementation of an activity of observation of the sky in the school, present in the works of researchers in the area of education in Astronomy. These elements make up the structure of the set of observational activities that range in time from moments before, during and after the sky observation activity. In this way, eight categories were constructed and subsidized the analysis: Material, Pre-observation, Strategies to observe and follow stars or phenomena, Nature of observation, Post-observation, Space, Subsidies and Complements. In the analysis, it was noticed that topics of Astronomy are concentrated in the books of sixth year, and that they occupy a considerable bulk of it, while noting that contents of other areas of education include Biology, Physics, Geosciences, Chemistry. Astronomy topics disappear in the seventh and eighth years and return in the ninth year, usually within Gravitation. The presence of observation are also implemented almost exclusively in the sixth year, which are focused on short periods of time, thereby making it difficult to perceive cyclical phenomena promoting contemplative observations. In addition, these exercises are usually intended to be carried out outside of the school grounds, making it difficult for the teacher to participate, and requiring greater student autonomy. Although the activities of observation are present in the LD, they are still far from the proposals made by the researchers of the area that suggest systematic observations for a better understanding, becoming the own experiences, in which the learning occurs in the time of the phenomenon and also own of each student
Carvalho, Tassiana Fernanda Genzini de. "Da divulgação ao ensino: um olhar para o céu." Universidade de São Paulo, 2016. http://www.teses.usp.br/teses/disponiveis/81/81131/tde-06102016-113657/.
Повний текст джерелаCultural-historical psicology appeared early in the 20th century, in the Soviet Union, based mainly on marxist principles relative to the human gender. Its main contribution shows that the relation between man and the world is not a direct consequence of uninterested observation, it is not a simple stimulus-reaction situation, but it is mediated by activity within a social context. The activity concept does not have the common sense meaning but it is inserted in the Activity Theory that was based on the work of Vigotski, Leontiev and other authors. According to this theory, activity is always motivated by a human necessity that is built up socially by means of actions connected to well defined objectives and by operations connected to concrete realization conditions. In this work we studied the evolution of human beings in relation to the sky and how the \"sky observation\" activity has been transforming nature and the very essence of man, as a singular perspective. Under this point of view we can explain curricular documents, research on astronomy teaching and teaching activities for \"sky observation\" elaborated by education professionals, as a particular perspective of the history of this action in astronomy teaching. We noticed that this subject is becoming more important in educational proposals and that curricula as well as investigators and teachers admit the importance of sky observation for building up of human beings; however in spite of appearing in curricular proposals and in the \"sky observation\" research content it is still not a reality in school practice, probably because of rather unfavorable conditions ,such as teachers inadequate formation and the lack of materials and infrastructure that are essential for school room work. We made an analysis relating logical historical progress about sky concepts and about the \"sky teaching object\", in search of the essence of this concept along its development. We suggest a teaching proposal based on empirical results of our investigation about teachers knowledge and the possibility of teaching astronomy as proposed by curricula. We hope this proposal may enable students to acquire the human culture developed in the course of history besides developing their potential as human beings in a universal perspective that enables the construction of a feeling from theoretical ideas in an abstract to concrete ascension motion, as defined by the theory on which this work is based.
López, Coto Rubén. "Very-high-energy -ray observations of pulsar wind nebulae and cataclysmic variable stars with MAGIC and development of trigger systems for IACTs." Doctoral thesis, Universitat Autònoma de Barcelona, 2015. http://hdl.handle.net/10803/299795.
Повний текст джерелаThe history of astronomy is as ancient as the reach of our written records. All the human civilizations have been interested in the study and interpretation of the night sky and its objects and phenomena. These observations were performed with the naked eye until the beginning of the 17th century, when Galileo Galilei started to use an instrument recently developed called telescope. Since then, the range of accessible wavelengths has been increasing, with a burst in the 20th century with the developing of instruments to observe them: antennas (radio and submillimeter), telescopes (optical, IR) and satellites (UV, X-rays and soft gamma rays). The last wavelength range accessed was the Very-High-Energy (VHE) gamma rays. At this range fluxes are so low that it is not possible to use space-based instruments with typical collection areas of O(1) m2. We must resort to the imaging atmospheric Cherenkov technique, which is based on the detection of the flashes of Cherenkov light that VHE gamma rays produce when they interact with the Earth’s atmosphere. The field is very young, with the first source discovered in 1989 by the pioneering Whipple telescope. It is very dynamic with more than 150 sources detected to date, most of them by MAGIC, HESS and VERITAS, that make up the current generation of instruments. Finally, the field is also very promising, with the preparation of a next generation of imaging atmospheric Cherenkov telescopes: CTA, that is expected to start full operation in 2020. The work presented in this thesis comprises my e orts to take the ground-based -ray astronomy one step forward. Part I of the thesis is an introduction to the nonthermal universe, the imaging atmospheric Cherenkov technique and the Imaging Atmospheric Cherenkov Telescopes (IACTs) MAGIC and CTA. Part II deals with several ways to reduce the trigger threshold of IACTs. This includes the simulation, characterization and test of an analog trigger especially designed to achieve the lowest possible energy threshold with the LSTs of CTA. Together with this work, the trigger of the MAGIC telescopes was improved. We have simulated, tested and commissioned a new concept of stereoscopic trigger. This new system, that uses the information of the position of the showers on each of the MAGIC cameras, is dubbed “Topo-trigger”. The scientific fraction of the thesis deals with galactic sources observed with the MAGIC telescopes. In Part III, I talk about the analysis of the VHE -ray emission of Pulsar Wind Nebulae (PWNe): the discovery of VHE -ray emission from the puzzling PWN 3C 58, the likely remnant of the SN 1181 AD and the weakest PWN detected at VHE to date; the characterization of the VHE tail of the Crab nebula by observing it at the highest zenith angles; and the search for an additional inverse Compton component during the Crab nebula flares reported by Fermi-LAT in the synchrotron regime. Part IV is concerned with searches for VHE -ray emission of cataclysmic variable stars. I studied, on a multiwavelength context, the VHE -ray nature of the previously claimed pulsed -ray emission of the cataclysmic variable AE Aqr. I also performed observations of novae and a dwarf nova to pinpoint the acceleration mechanisms taking place in this kind of objects and to discover a putative hadronic component of the soft -ray emission. A conclusion chapter summarizes all the work performed and lists prospects related with the topics treated in this thesis.
Fors, Aldrich Octavi. "New Observational Techniques and Analysis Tools for Wide Field CCD Surveys and High Resolution Astrometry." Doctoral thesis, Universitat de Barcelona, 2006. http://hdl.handle.net/10803/745.
Повний текст джерелаIn the first part of the thesis a wavelet-based adaptive image deconvolution algorithm (AWMLE) has been applied to two sets of survey type CCD data: QUasar Equatorial Survey Team project(QUEST and Near-Earth Space Surveillance Terrestrial(NESS-T). Richardson-Lucy image deconvolution has also been used with Flagstaff Transit Telescope (FASTT)imagery. Both the obtaining and performance of those images were accomplished by following a new methodology which includes accurate image calibration, source detection and centering, and correct assessment procedures of the performance of the deconvolution. Results show that AWMLE deconvolution can increase limiting magnitude up to 0.6 mag and improve limiting resolution 1 pixel with respect to original image. These studies have been conducted in the context of programs dedicated to macrolensing search (QUEST) and NEOs discovery(NESS-T). Finally, astrometric accuracy of FASTT images have not been found to change significantly after deconvolution. In the same way, no positional bias towards the centre of the pixel has been observed.
In the second part of the thesis a new observational technique based on CCD fast drift scanning has been proposed, implemented and assessed for lunar occultations (LO) and speckle interferometry observations.
In the case of LO, the technique yielded positive detection of binaries up to 2 milliarcseconds of projected separation and stellar diameters measurements in the 7 milliarcsecond regime. The proposed technique implies no optical or mechanical additional adjustments and can be applied to nearly all available full frame CCDs. Thus, it enables all kind of professional and high-end amateur observatories for LO work. Complementary to this work, a four-year LO program (CALOP) at Calar Alto Observatory spanning 71.5 nights of observation and 388 recorded events has been conducted by means of CCD and MAGIC IR array cameras at OAN 1.5m and CAHA 2.2m telescopes. CALOP results include the detection of one triple system and 14 new and 1 known binaries in the near-IR, and one binary in the visible. Their projected separations range from 90 to 2 milliarcseconds with brightness ratios up to 1:35 in the K band. Several angular diameters have been also measured in the near-IR. The performance of CALOP has been calibrated in terms of limiting magnitude (K down to 9.0) and limiting angular resolution (1-3 milliarcseconds).
In addition, the binary detection probability of the program has found to be about 4%. Finally, a new wavelet-based method for extracting and characterizing LO lightcurves in an automated fashion was proposed, implemented and applied to CALOP database. This pipeline addresses the need of disposing of preliminary results in immediate basis for future programs which will provide larger number of events.
In the case of speckle interferometry, CCD fast drift scanning technique has been validated with the observation of four binary systems with well determined orbits. The results of separation, position angle and magnitude difference are in accordance with published measurements by other observers and predicted orbits. Error estimates for these have been found to be 0.017 arcseconds, 1.5 degrees and 0.34 mag, respectively. These are in the order of other authors and can be considered as successful for a first trial of this technique.
Finally, a new approach for calibrating speckle transfer function from the binary power spectrum itself has been introduced. It does not require point source observations, which gives a more effective use of observation time. This new calibration method appears to be limited to zenith angles above 30 degrees when observing with no refraction compensation devices.
En aquest treball s'han dissenyat i desenvolupat una sèrie de noves tècniques observacionals i eines d'anàlisi de dades en dues àrees ben diferenciades. D'una banda, la deconvolució d'imatges CCD de gran camp (tipus survey). D'altra banda, l'astrometria d'alta resolució, i en particular les tècniques observacionals d'ocultacions lunars i interferometria speckle.
Quant a la primera, s'han aplicat dos algorismes de deconvolució (màxima versemblança Richardson-Lucy (MLE) i la seva variant adaptativa basada en wavelets (AWMLE)) a dades de tres projectes survey: el Flagstaff Transit Telescope (FASTT), el QUasar Equatorial Survey Team (QUEST) i el Near-Earth Space Surveillance Terrestrial (NESS-T). Els tres han vist restringida la seva magnitud i resolució límits a causa del mètode d'adquisició drift scanning (per a FASTT i QUEST) o la molt curta relació focal de l'instrument (NESS-T). S'ha proposat i implementat una nova metodologia per a l'aplicació de l'AWMLE i MLE per a les anteriors imatges. Aquesta permet avaluar la millora aportada per la deconvolució en termes d'increment de magnitud i resolució límits. A més, resulta del tot general i és exportable a altres dades survey. Els resultats obtinguts mostren que AWMLE permet aconseguir un increment en la magnitud límit de 0.6 mag i una millora en la resolució límit d'1.0 pixel. A més, s'ha comprovat que tals tendències són assimtòticament independents a partir d'un nombre d'iteracions suficientment gran. Paral·lelament, s'ha comprovat que la deconvolució MLE sobre dades FASTT no afecta significativament a la precisió astromètrica ni introdueix cap biaix posicional cap al centre del píxel.
Quant a les ocultacions lunars, s'ha ideat, desenvolupat, implementat i avaluat una nova tècnica d'observació CCD per a ocultacions lunars. Éstà basada en el mètode d'adquisició "drift scanning" i permet mostrejar la intensitat de l'objecte ocultat cada 2ms. La tècnica permet a pràcticament qualsevol observatori (professional o amateur) afrontar programes d'ocultacions lunars amb propòsits de contribució científica. Paral·lelament, s'ha portat a terme un programa d'observació d'ocultacions lunars (anomenat CALOP) que durant 4 anys i 71.5 nits s'ha portat a terme a l'Observatorio Astronómico de Calar Alto, operant tant en el visible amb CCD com en l'IR amb la càmera MAGIC. Com a resultat, s'han aconseguit mesurar 3 diàmetres estel·lars de l'ordre de 7 mil.lisegons d'arc i detectar 15 nous sistemes binaris i un triple amb separacions angulars de fins a 2 mil.lisegons d'arc. Finalment, s'ha desenvolupat i implementat un nou algorisme de reducció automàtica d'ocultacions basat en wavelets. Tal algorisme ha estat aplicat satisfactòriament en la reducció del conjunt d'ocultacions (400) registrades en el programa CALOP, i permet afrontar la reducció de futures campanyes d'observació massiva.
Quant a la interferometría speckle, s'ha ideat, desenvolupat, implementat i avaluat una nova tècnica d'observació CCD per a aquest tipus d'observacions d'alta resolució espacial. Éstà basada en el mètode d'adquisició drift scanning i permet mostrejar la intensitat de l'objecte dins de l'interval de coherència atmosfèrica. S'ha validat amb la mesura de 4 sistemes binaris d'òrbita coneguda. Els resultats de separació angular, angle de posició i diferència de magnitud estan d'acord amb els publicats per autors anteriors. La tècnica permet a pràcticament qualsevol observatori (professional o amateur) afrontar programes "speckle" amb propòsits de contribució científica. Finalment, s'ha ideat, implementat i validat una nova tècnica de autocalibració de dades speckle que permet estalviar temps d'observació.
Juráň, Jakub. "Vývoj systému řízení astronomického dalekohledu s možností sledování družic." Master's thesis, Vysoké učení technické v Brně. Fakulta elektrotechniky a komunikačních technologií, 2018. http://www.nusl.cz/ntk/nusl-377003.
Повний текст джерелаBuxton, Michelle Maree. "Optical and infrared observations of low-mass X-ray binaries with black hole candidates." Phd thesis, 2002. http://hdl.handle.net/1885/148662.
Повний текст джерелаLamb, Masen. "On the calibration and use of Adaptive Optics systems: RAVEN observations of metal-poor stars in the Galactic Bulge and the application of focal plane wavefront sensing techniques." Thesis, 2017. https://dspace.library.uvic.ca//handle/1828/8368.
Повний текст джерелаGraduate