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Добірка наукової літератури з теми "Telescopes"

Автор: Grafiati

Опубліковано: 4 червня 2021

Оновлено: 1 серпня 2024

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Статті в журналах з теми "Telescopes"

Tokunaga, A. T., C. Ftaclas, J. R. Kuhn, and P. Baudoz. "High Dynamic Range and the Search for Planets." Symposium - International Astronomical Union 211 (2003): 487–96. http://dx.doi.org/10.1017/s0074180900211200.

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General arguments for optimized coronagraphy in the search for planets are presented. First, off-axis telescopes provide the best telescopic platforms for use with coronagraphy, and telescope fabrication technology now allows the fabrication of such telescopes with diameters of up to 6.5 m. We show that in certain circumstances a smaller telescope with an off-axis primary has a signal-to-noise advantage compared with larger Cassegrain telescopes. Second, to fully exploit the advantages of the coronagraph for suppressing stray light, it is necessary to use a high Strehl ratio adaptive optics system. This can be best achieved initially with modest aperture telescopes of 3–4 m in diameter. Third, application of simultaneous differential imaging and simultaneous polarimetric techniques are required to reach the photon-limit of coronagraphic imaging. These three developments, if pursued together, will yield significant improvements in the search for planets.

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Liu, Yi, Changqing Feng, Ingrid-Maria Gregor, Adrian Herkert, Lennart Huth, Marcel Stanitzki, Yao Teng, and Chenfei Yang. "ADENIUM — A demonstrator for a next-generation beam telescope at DESY." Journal of Instrumentation 18, no. 06 (June 1, 2023): P06025. http://dx.doi.org/10.1088/1748-0221/18/06/p06025.

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Abstract High-resolution beam telescopes for charged particle tracking are one of the most important and equally demanding infrastructure items at test beam facilities. The main purpose of beam telescopes is to provide precise reference track information of beam particles to measure the performance of a device under test (DUT). In this report the development of the ADENIUM beam telescope (ALPIDE sensor based DESY Next test beam Instrument) as a demonstrator and prototype for a next-generation beam telescope is presented. The ADENIUM beam telescope features up to six pixelated reference planes framed by plastic scintillators for triggering. ADENIUM is capable of replacing the currently used EUDET-type beam telescopes without impacting existing DUT implementations due to the integration of the telescope DAQ into EUDAQ2. In this report the concept and design of the ADENIUM telescope as well as its performance are discussed. The telescope's pointing resolution is determined in different configurations. For an optimal setup at a momentum of 5.6 GeV with an ALPIDE as DUT, a resolution better than 3 μm has been extracted. No rate limitations have been observed at the DESY II test beam.

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Lu, Zhiyi. "Analysis of the Principle and State-of-art Applications of Astronomical Telescope." Highlights in Science, Engineering and Technology 72 (December 15, 2023): 83–89. http://dx.doi.org/10.54097/4kna8f33.

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Astronomical telescopes have been instrumental in enhancing our comprehension of the cosmos since ancient eras. This study explores these remarkable instruments' principles and state-of-art applications, tracing their development from early refracting telescopes to modern space and ground-based telescopes. The primary focus is to analyze the imaging principles of optical and radio telescopes and showcase their significance in capturing high-resolution observations of celestial objects. It also highlights recent achievements made by advanced telescopes, including the James Webb Space Telescope and the Event Horizon Telescope, which have provided unprecedented clarity and insights into distant galaxies, exoplanets, and supermassive black holes. This research presents breakthrough achievements made by advanced telescopes such as the James Webb Space Telescope and the Event Horizon Telescope in revealing distant galaxies, exoplanets, and supermassive black holes. Despite the limitations in astronomical telescope research, such as errors, atmospheric interference, and high costs, the paper emphasizes a promising future. Through technological advancements, international collaboration, and cost-effective space telescopes, astronomical research is expected to make significant progress. In summary, these results provide a comprehensive analysis of astronomical telescopes, enriches the frontiers of astronomy, underscores the importance of international cooperation, and offer essential guidance for the future development of astronomy.

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Chen, Siyu. "Comparisons of Two Types of Astronomical Telescopes: Terrestrial Telescopes and Space Telescopes." Theoretical and Natural Science 2, no. 1 (February 20, 2023): 75–80. http://dx.doi.org/10.54254/2753-8818/2/20220166.

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In the field of astrophysics and cosmology, astronomical telescopes are the main and key tool for observing and capturing information of celestial bodies. Generally, there are two types of telescopes, i.e., terrestrial telescopes and space telescopes. This study will be mainly focused on the differences and similarities between the two types mentioned above. According to the analysis, the ground telescope is larger and collect data with processing instead of real picture. The space telescope, on the other hand, is smaller but hard to repair, which is able to send back the real pictures of the space. The research aims of this investigation are helping the further researchers to have better understanding to the two different types of telescopes and offering a guideline for them to choose the more appropriate resources to use for the future research. These results shed light on guiding further exploration of different types of telescopes and pave a path for the future inventions of the telescopes.

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Kim, Sang Chul. "Paper Productivity of Ground-based Large Optical Telescopes from 2000 to 2009." Publications of the Astronomical Society of Australia 28, no. 3 (2011): 249–60. http://dx.doi.org/10.1071/as11011.

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AbstractWe present an analysis of the scientific (refereed) paper productivity of the current largest (diameter > 8m) ground-based optical (and infrared) telescopes during the ten-year period from 2000 to 2009. The telescopes for which we have gathered and analysed the scientific publication data are the two 10-m Keck telescopes, the four 8.2-m Very Large Telescopes (VLT), the two 8.1-m Gemini telescopes, the 8.2-m Subaru telescope, and the 9.2-m Hobby–Eberly Telescope (HET). We have analysed the numbers of papers published in various astronomical journals produced by using these telescopes. While the total numbers of papers from these observatories are largest for the VLT, followed by Keck, Gemini, Subaru, and HET, the number of papers produced by each component of the telescopes is largest for Keck, followed by VLT, Subaru, Gemini, and HET. In 2009, each telescope of the Keck, VLT, Gemini, Subaru, and HET observatories produced 135, 109, 93, 107, and 5 refereed papers, respectively. We have shown that each telescope of the Keck, VLT, Gemini, and Subaru observatories is producing 2.1 ± 0.9 Nature and Science papers annually and these papers make up 1.7 ± 0.8% of all refereed papers produced by using each of those telescopes. Extending this relation, we propose that this ratio of the number of Nature and Science papers to the total number of refereed papers that will be produced by future extremely large telescopes (ELTs) will remain similar. From a comparison of the publication trends of the above telescopes, we suggest that (i) having more than one telescope of the same kind at the same location and (ii) increasing the number of instruments available at the telescope are good ways to maximize the paper productivity.

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Pech, Miroslav, Justin Albury, Jose A. Bellido, John Farmer, Toshihiro Fujii, Petr Hamal, Pavel Horvath, et al. "Simulation of the optical performance of the Fluorescence detector Array of Single-pixel Telescopes." EPJ Web of Conferences 210 (2019): 05014. http://dx.doi.org/10.1051/epjconf/201921005014.

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The Fluorescence detector Array of Single-pixel Telescopes (FAST) is a proposed large-area, next-generation experiment for the detection of ultra-high energy cosmic rays via the atmospheric fluorescence technique. The telescope’s large field-of-view (30 ×30) is imaged by four 200 mm photomultiplier-tubes at the focal plane of a segmented spherical mirror of 1.6 m diameter. Two prototypes are installed and taking data at the Black Rock Mesa site of the Telescope Array experiment in central Utah, USA. We present the process used for optimization of the optical performance of this compact and low-cost telescope, which is based on a simulation of the telescope’s optical point spread function.

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Hong, Yiduo. "Working principle of the radio telescope and the study of the sun." Theoretical and Natural Science 12, no. 1 (November 17, 2023): 172–76. http://dx.doi.org/10.54254/2753-8818/12/20230461.

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Radio telescopes can help people observe celestial bodies far away from people, which is conducive for astronomers to observe and draw the trend of celestial transformations. The use of radio telescopes allows scholars to study and understand celestial bodies to a new height. At present, the more famous are the Webb Space Telescope in the United States, the Hubble Space Telescope and China's Tianyan. In the case of the eye of Heaven in Guizhou, China, the surface of the eye is covered by a metal layer one millimeter thick, so it can not withstand excessive pressure, and the maintenance personnel need to attach themselves to a giant helium balloon to reduce their weight, the whole process is so careful to ensure the safety of the precision instrument. So there are still some limitations in the development of radio telescopes. This paper will focus on the working principle of the radio telescope, the development of the radio telescope and techniques for observing the sun with radio telescopes, summarize the achievements of the radio telescope so far and the areas that need to be improved. To better understand radio telescopes.

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Li, Yuqiao. "State-of-art Facilities and Prospect of Radio Telescopes." Highlights in Science, Engineering and Technology 5 (July 7, 2022): 201–7. http://dx.doi.org/10.54097/hset.v5i.743.

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The radio telescopes play a crucial role in astrophysical observations; hence it is necessary to discuss about the significance, structure, and applications of radio telescope and analyse the difference between the state-of-art radio telescopes (FAST and SKA) based on present information. Specifically, the background and present conditions as well as the history of radio telescopes will be introduced initially. Subsequently, the significance of radio telescope will be explained, including structure and application of radio telescopes. Subsequently, the doubts on FAST and SKA and strengths of them will be clarified. Eventually, the problems and limitations about radio telescope and the future prospect will be discussed. Overall, these results shed light on offering suggestions for future development of galaxy and cosmology observations.

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Porter, F. I., J. M. White, J. Goldberg, J. L. Demer, and A. Koval. "Predicting Successful Low Vision Rehabilitation with Telescopic Spectacles." Journal of Visual Impairment & Blindness 86, no. 1 (January 1992): 29–32. http://dx.doi.org/10.1177/0145482x9208600116.

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Although telescopic spectacles magnify the retinal image and should improve functional vision, many low vision patients are unable to use them. The authors found that involuntary head movements and the reduction of acuity with imposed head motion differentiated successful from unsuccessful telescope users and that success was related to the age at which telescopes were first used.

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Burton, Michael G., John W. V. Storey, and Michael C. B. Ashley. "Science Goals for Antarctic Infrared Telescopes." Publications of the Astronomical Society of Australia 18, no. 2 (2001): 158–65. http://dx.doi.org/10.1071/as01026.

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AbstractOver the past few years, site-testing at the South Pole has revealed conditions that are uniquely favourable for infrared astronomy. In particular, the exceptionally low sky brightness throughout the near and mid-infrared leads to the possibility of a modest-sized telescope achieving comparable sensitivity to that of existing 8–10 metre class telescopes. An 8 metre Antarctic telescope, if constructed, would yield performance that would be unrivalled until the advent of the NGST. In this paper we review the scientific potential of infrared telescopes in Antarctica, and discuss their complementarity with existing 8–10 metre class telescopes and future proposed space telescopes. In particular, we discuss the role that a 2 metre class infrared telescope plays in future plans for the development of an observatory on the Antarctic plateau.

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Більше джерел

Дисертації з теми "Telescopes"

Mawson, Neil R. "Small telescopes installed at the Liverpool Telescope." Thesis, Liverpool John Moores University, 2013. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.604296.

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The Small Telescopes Installed at the Liverpool Telescope (STILT) have been in operation since March 2009, collecting wide field data from their position, at the Liverpool Telescope on La Palma. The system consists of a set of two wide field imaging cameras, known as SkycamT and SkycamZ. They provide fields of view of 21x210 and Ix 1 0, along with limits of 12th and 18th in R-band magnitude. The work in this thesis describes the methodology used to create an image analysis pipeline and database to store the photometric results contained in the images produced by these cameras. Such a database is capable of providing invaluable data for the study of many stellar and transient sources. The optimisation of the camera software, as well as modifications to the hardware of the cameras are presented, along with a discussion of the imaging methodologies used in the creation of the data pipeline, which involved specific setup for the case of wide field imaging. For the pipeline, the method for photometric calibration and the overall process structure will be presented along with the schema of the database, and the justifications for these choices. Work has also been carried out to define the performance of the system in a photometric, astrometric and computational sense. The resulting datasets contains: SkycamZ SkycamT Images processed 272,470 315,277 Unique Objects observed 6,290,935 21,453,608 Observations 332,735,320 904,033,139 Mean observations per object 53 42

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Vaksdal, Birger. "Medium Size Telescopes in the Cherenkov Telescope Array." Thesis, KTH, Fysik, 2017. http://urn.kb.se/resolve?urn=urn:nbn:se:kth:diva-210238.

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Fernández, Barral Alba. "Extreme particle acceleration in microquasar jets and pulsar wind nebulae with the MAGIC telescopes." Doctoral thesis, Universitat Autònoma de Barcelona, 2017. http://hdl.handle.net/10803/457715.

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A lo largo de toda nuestra historia, los seres humanos nos hemos esforzado por descifrar los misterios con los que el Universo nos desafía. En nuestros humildes comienzos, esta tarea era realizada con nuestros ojos desnudos, mirando las estrellas y los planetas y preguntándonos qué tan lejos estaban y cómo se movían en el cielo nocturno. Durante muchos siglos, sólo el Universo visible fue accesible para nosotros, pero se obtuvieron logros extraordinarios a pesar de las limitadas herramientas: descubrimos, por ejemplo, que nuestro planeta no era el centro del Universo, gracias a las observaciones de Nicolaus Copernicus y su modelo heliocéntrico. Desde la época de Copernicus hasta ahora, el desarrollo de nuevas tecnologías y el avance de nuestra propia comprensión del Cosmos, nos ha permitido desentrañar mucho enigmas. Afortunadamente, esta curiosidad natural que nos lleva a mejorar nunca termina, y nos enfretamos a nuevas preguntas que desafían nuestra capacidad como científicos. En la presente tesis, me centro en una pequeña fracción de esta ciencia: la astronomía de rayos gamma. Dentro de este campo, estudio la aceleraci ón de partículas y los mecanismos de producción de rayos gamma en los jets relativistas de los denominados microcuásares y en shocks producidos en pleriones. En la Parte I de la tesis, presento una introducción al Universo no térmico, profundizando en los mecanismos de producción y absorción que gobiernan la emisión de rayos gamma. También introduzco los telescopios MAGIC, de los cuales se obtiene la mayor parte de los resultados de esta tesis. Otras técnicas de detección, como las empleadas en el Observatorio HAWC o por el satélite Fermi-LAT, son igualmente presentadas dado que sus resultados son empleados en la discusión de fuentes galácticas incluidas en esta tesis. Los logros científicos están incluidos en la Parte II y Parte II. En el primera, discuto los resultados de los tres mejores candidatos microcuásares para emitir rayos gamma a muy altas energías: Cygnus X-1, Cygnus X-3 y V404 Cygni. Investigo todos ellos haciendo uso de los datos de MAGIC durante campañas observacionales de larga duración o durante periodos de alta actividad. Por otra parte, con el fin de complementar los resultados a energías más bajas, analizo los datos de Fermi-LAT de Cygnus X-1, lo cual condujo a la detección del sistema en el régime de altas energ ías. Esto constituye la primer detección firme de rayos gamma a altas energías de un sistema binario compuesto por un agujero negro. La Parte III se centra en el estudio de pleriones. Analizo cinco fuentes pertenecientes a esta clase y contextualizo los resultados dentro del estudio de población de pleriones realizado por la Colaboración H.E.S.S.. Haciendo uso de estos resultados, se discute la importancia de la densidad de fotones en el medio circundante junto con las características de los p´ulsares alojado por estos pleriones para la emisión de rayos gamma. En esta tesis, también presento el primer trabajo conjunto entre el Observatorio HAWC y MAGIC, que abre las puertas a futuros proyectos en sinergia. La Parte IV incluye el trabajo técnico realizado durante mi tesis con el futuro CTA. Este trabajo está centrado en el hardware de la cámara de los telescopios de gran tamaño (LST, por sus siglas en inglés) del futuro instrumento CTA, que incluye el control de calidad de varios subsistemas, entre los que descatan los fotomultiplicadores, las fuentes de alimentación y el sistema de trigger. Finalmente, resumo todos los anteriormente mencionados resultados en un capítulo de conclusiones. Todo el trabajo desarrollado durante mi tesis dio lugar a siete publicaciones en revistas científicas: dos ya publicadas, dos aceptadas por la correspondiente revista y tres actualmente bajo revisión de la Colaboración de MAGIC y otras colaboraciones implicadas.
Throughout our entire history, we humans have strived to unravel the mysteries with which the deep Universe challenges us. In our humble beginnings, this task was performed with our naked eyes, by gazing at the stars and planets and wondering how far away they were and how they moved in the night sky. For many centuries, only the visible Universe was reachable for us, but extraordinary achievements were accomplished despite the limited tools: we discovered, for example, that our planet was not the center of the Universe, owing to Nicolaus Copernicus’ observations and his heliocentric model. From Copernicus’ epoch up to now, the development of new technologies and the advancement of our own understanding of the Cosmos, allowed us to disentangle many riddles. Fortunately, this natural curiosity that leads us to improve never ends, and we face new questions that challenge our capacity as scientists. In the present thesis, I focus on a small fraction of this science: the gamma-ray astronomy. Within this field, I study particle acceleration and gamma-ray production mechanisms inside the relativistic jets displayed by the so-called microquasars and the shocks produced in Pulsar Wind Nebulae (PWNe). In Part I of the thesis I present an introduction to the non-thermal Universe, delving into the mechanisms of production and absorption that govern the gamma-ray emission. I also introduce the MAGIC telescopes, from which the bulk of results in this thesis are obtained. Other detection techniques, such as those used by the HAWC Observatory and the Fermi-LAT satellite, are also introduced as results from both of them are used in the discussion of galactic sources included in this thesis. The scientific achievements are encompassed in Part II and Part III. In the former, I discuss results from the three best microquasar candidates to emit Very-High-Energy (VHE) gamma rays: Cygnus X-1, Cygnus X-3 and V404 Cygni. I investigate them making use of MAGIC data during long-term campaigns or under flaring periods. Furthermore, in order to complement results at lower energies, I analyze Fermi-LAT data of Cygnus X-1, leading to the detection of the system in the High Energy (HE) regime. This constitutes the first firmly gamma-ray detection on a Black Hole (BH) binary system. Part III is focused on the study of PWNe. I analyze five sources of this type and set the results in the context of the TeV PWN population study performed by the High Energy Stereoscopic System (H.E.S.S.) Collaboration. Along with these results, I discuss the importance of the target photon field together with characteristic features of the pulsars hosted by these PWNe to emit gamma rays. In this thesis, I also present the first joint work between the HAWC Observatory and MAGIC, which opens the door to future synergy projects. In Part IV, I present the technical work performed during my thesis for the future Cherenkov Telescope Array (CTA) instrument. I focus on the camera hardware for the Large Size Telescope (LST), working on the Quality Control (QC) for several subsystems, among which the Photomultiplier Tubes (PMTs), power supplies and trigger mezzanines stand out. Finally, I summarize all the aforementioned results in a conclusion chapter. All the work developed during my thesis led to seven publications in scientific journals: two of them already published, two accepted by the corresponding journal and three currently under the revision of MAGIC and all implicated collaborations.

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Witzemann, Amadeus. "Cosmology with next generation radio telescopes." University of the Western Cape, 2019. http://hdl.handle.net/11394/6936.

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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.

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O'Dougherty, Stefan, and Stefan O'Dougherty. "Quasi-Optical Spherical Balloon Telescopes." Diss., The University of Arizona, 2018. http://hdl.handle.net/10150/626762.

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Astronomy constantly pushes the limits of technology in order to decipher the workings of the Universe. There is a constant need for higher resolution observations across a wide range of wavelengths, at preferably a minimal cost. The terahertz regime (lambda=100 um to lambda=1000 um) covers a region of the electromagnetic spectrum that is blocked by Earth's atmosphere, which limits observations to high altitude plane and balloon telescopes and space telescopes. These current options limit the resolution achievable due to the size of telescopes that can be launched. This dissertation investigates a new approach, the Large Balloon Reflector (LBR), where a 20 meter diameter spherical balloon can be inflated and used as a 10 meter telescope inside a larger carrier balloon. Detailed in this dissertation are design considerations for the terahertz regime and a series of scaled versions of this balloon concept where I work to develop on-axis spherical corrector designs. Chapters 1 through 6 focus on the LBR designs and their variants, including investigations for a 3 meter rooftop proof of concept model, a 5 meter test flight model, and the final 20 meter LBR. The successful modeling and proof of concepts from the LBR studies then prompted an investigation into a Terahertz Space Telescope (TST), a proposed 20 meter inflatable telescope adapted from the LBR technology. Starting with Chapter7, this dissertation explores the application of using 1 meter diameter inflatable balloons as rapidly deployable communications satellites from standard CubeSats. The concept, design and test results of an electronically steerable line feed antenna array are presented which allows for instantaneous, non mechanical pointing of a 10 GHz signal within a 500 km ground footprint. Alternative uses of the 1 meter inflatable balloon CubeSat are also discussed, such as low cost astronomical galactic plane surveys.

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Bou, Cabo Manuel. "Acoustics for underwater neutrino telescopes." Doctoral thesis, Universitat Politècnica de València, 2011. http://hdl.handle.net/10251/10989.

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En esta tesis se tratan diferentes aspectos de la acústica presente en un telescopio submarino de neutrinos, principalmente en dos vertientes: en el sistema de posicionamiento acústico utilizado para la monitorización de las posiciones de los módulos ópticos presentes a lo largo del detector, así como en sistemas para detección acústica de neutrinos, técnica que actualmente está en fase de estudio. Todos los estudios realizados están enmarcados dentro de dos colaboraciones europeas para el diseño, construcción y operación de telescopios submarinos de neutrinos: Antares (en fase de operación) y KM3NET (en fase de diseño). Objetivos. Los objetivos de este trabajo pueden resumirse en los siguientes aspectos: - Estudios y análisis del sistema de posicionamiento acústico de Antares. Desarrollo del software para la para la automatización del procesado de los datos de dicho sistema e incorporación de los resultados en la base de datos del experimento. Análisis de los datos proporcionados por dicho sistema con el fin de validar su correcto funcionamiento. - Diseño y desarrollo del sistema de posicionamiento acústico para KM3NeT, telescopio unas 20 veces más grande que Antares. - Estudios para la evaluación de la generación acústica paramétrica para el desarrollo de un calibrador compacto capaz de generar señales tipo neutrino útiles en sistemas de detección acústica. Elementos de la metodología a destacar. Cabe destacar aquí que el trabajo se ha desarrollado en el marco de dos colaboraciones internacionales: ANTARES y KM3NeT, financiados con fondos europeos y nacionales. Por su contexto y el carácter de las actividades realizadas ha sido necesaria la formación en distintos campos: telescopios de neutrinos y astropartículas, pero también en otras áreas como la acústica submarina. Además, se ha desarrollado diversas capacidades y destrezas en diversos ámbitos: en instrumentación, en aplicaciones informáticas, en análisis de datos, etc. Más concretamente, se ha trabajado en aplicaciones informáticas para los desarrollos y análisis en ANTARES.
Bou Cabo, M. (2011). Acoustics for underwater neutrino telescopes [Tesis doctoral no publicada]. Universitat Politècnica de València. https://doi.org/10.4995/Thesis/10251/10989
Palancia

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Kern, Pierre. "Optique adaptative et grands telescopes." Paris 7, 1990. https://tel.archives-ouvertes.fr/tel-00714946.

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Severement limite par la turbulence atmospherique, les grands telescopes au sol ne sont pas capables d'atteindre leur limite de resolution intrinseque de maniere directe. En fonctionnement normal, ils ne peuvent pas resoudre plus de details, aux longueurs d'ondes du visible et du proche infrarouge qu'un telescope de quelques decimetres de diametre. La technique d'optique adaptative decrite ici, offre l'avantage sur les autres techniques, d'un traitement du front d'onde avant la detection du signal. Lorsque la detection n'est pas limitee par le bruit propre du signal incident ce traitement permet d'ameliorer significativement le rapport signal sur bruit. La correction est realisee par un miroir deformable dont les comandes sont calculees a partir des mesures des perturbations de la surface d'onde. Les limitations de cette instrumentation sont donnees par le nombre d'actuateurs du miroir, la precision de la mesure du front d'onde, liee au flux disponible pour realiser la mesure, et a la bande passante de l'asservissement. Cette bande passante est surtout liee a la frequence d'echantillonnage du signal d'erreur, et a la vitesse de calcul dans la boucle d'asservissement. Nous donnons la description d'un instrument teste en observatoire au cours de l'automne 1989. Le front d'onde corrige au moyen d'un miroir deformable de 19 actuateurs, a permis d'obtenir en temps reel, des images limitees par la diffraction pour des longueurs d'onde superieures a 2,2 m, au foyer coude du telescope de 1,52 m de l'ohp. La mesure de la perturbation est realisee par un analyseur de shack-hartmann de 55 sous-pupilles pour echantillonner le signal a une frequence de 100 hz. La bande passante obtenue est de 9 hz en boucle ouverte a 0 db. Les resultats qui sont presentes illustrent l'interet de cette technique pour l'imagerie infrarouge en astronomie

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Petrushevska, Tanja. "Supernovae seen through gravitational telescopes." Doctoral thesis, Stockholms universitet, Fysikum, 2017. http://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-141633.

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Galaxies, and clusters of galaxies, can act as gravitational lenses and magnify the light of objects behind them. The effect enables observations of very distant supernovae, that otherwise would be too faint to be detected by existing telescopes, and allows studies of the frequency and properties of these rare phenomena when the universe was young. Under the right circumstances, multiple images of the lensed supernovae can be observed, and due to the variable nature of the objects, the difference between the arrival times of the images can be measured. Since the images have taken different paths through space before reaching us, the time-differences are sensitive to the expansion rate of the universe. One class of supernovae, Type Ia, are of particular interest to detect. Their well known brightness can be used to determine the magnification, which can be used to understand the lensing systems. In this thesis, galaxy clusters are used as gravitational telescopes to search for lensed supernovae at high redshift. Ground-based, near-infrared and optical search campaigns are described of the massive clusters Abell 1689 and 370, which are among the most powerful gravitational telescopes known. The search resulted in the discovery of five photometrically classified, core-collapse supernovae at redshifts of 0.671<z<1.703 with significant magnification from the cluster. Owing to the power of the lensing cluster, the volumetric core-collapse supernova rates for 0.4 ≤ z < 2.9 were calculated, and found to be in good agreement with previous estimates and predictions from cosmic star formation history. During the survey, two Type Ia supernovae in A1689 cluster members were also discovered, which allowed the Type Ia explosion rate in galaxy clusters to be estimated. Furthermore, the expectations of finding lensed supernovae at high redshift in simulated search campaigns that can be conducted with upcoming ground- and space-based telescopes, are discussed. Magnification from a galaxy lens also allows for detailed studies of the supernova properties at high redshift that otherwise would not be possible. Spectroscopic observations of lensed high-redshift supernovae Type Ia are of special interest since they can be used to test for evolution of the standard candle nature of these objects. If systematic redshift-dependent properties are found, their utility for future surveys could be challenged. In the thesis it is shown that the strongly lensed and very distant supernova Type Ia PS1-10afx at z=1.4, does not deviate from the well-studied nearby and intermediate populations of normal supernovae Type Ia. In a different study, the discovery of the first resolved multiply-imaged gravitationally lensed supernova Type Ia is also reported.

At the time of the doctoral defense, the following papers were unpublished and had a status as follows: Paper 3: Manuscript. Paper 4: Manuscript.

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Andersen, Geoff. "Holographic correction of aberrated telescopes /." Title page, abstract and contents only, 1996. http://web4.library.adelaide.edu.au/theses/09PH/09pha544.pdf.

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Thrall, Michael L. "Orbit determination of highly eccentric orbits using a RAVEN telescope." Thesis, Monterey, Calif. : Springfield, Va. : Naval Postgraduate School ; Available from National Technical Information Service, 2005. http://library.nps.navy.mil/uhtbin/hyperion/05Sep%5FThrall.pdf.

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Thesis (M.S. in Space Systems Operations)--Naval Postgraduate School, September 2005.
Thesis Advisor(s): Kyle T. Alfriend, Don A. Danielson. Includes bibliographical references (p. 33). Also available online.

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Книги з теми "Telescopes"

Bender, Lionel. Telescopes. New York: Gloucester Press, 1991.

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Bender, Lionel. Telescopes. London: Gloucester, 1991.

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Manly, Peter L. Unusual telescopes. Cambridge: Cambridge University Press, 1991.

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English, Neil. Space Telescopes. Cham: Springer International Publishing, 2017. http://dx.doi.org/10.1007/978-3-319-27814-8.

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Chinnici, Ileana, ed. Merz Telescopes. Cham: Springer International Publishing, 2017. http://dx.doi.org/10.1007/978-3-319-41486-7.

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English, Neil. Classic Telescopes. New York, NY: Springer New York, 2013. http://dx.doi.org/10.1007/978-1-4614-4424-4.

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Panel, Anglo-Australian Observatory Schmidt Telescope. The future use of the UK Schmidt Telescope: A report. [Epping, N.S.W., Australia: Anglo-Australian Observatory], 1995.

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Tucker, Wallace H. The cosmic inquirers: Modern telescopes and their makers. Cambridge, Mass: Harvard University Press, 1986.

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Kitchin, C. R. Telescopes and techniques: An introduction to practical astronomy. London: Springer, 1995.

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1934-, Brown Robert A., Ford H. C, Space Telescope Science Institute (U.S.), and United States. National Aeronautics and Space Administration., eds. Report of the HST Strategy Panel: A strategy for recovery : the results of a special study, August-October 1990. Baltimore, Md: Space Telescope Science Institute, 1991.

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Частини книг з теми "Telescopes"

Gross, Herbert, Fritz Blechinger, and Bertram Achtner. "Telescopes." In Handbook of Optical Systems, 723–864. Weinheim, Germany: Wiley-VCH Verlag GmbH & Co. KGaA, 2015. http://dx.doi.org/10.1002/9783527699247.ch8.

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Redfern, Gregory I. "Telescopes." In The Patrick Moore Practical Astronomy Series, 55–76. Cham: Springer International Publishing, 2020. http://dx.doi.org/10.1007/978-3-030-45943-7_4.

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Bennett, Jim. "Telescopes." In A Companion to the History of Science, 530–42. Hoboken, NJ, USA: John Wiley & Sons, Inc., 2016. http://dx.doi.org/10.1002/9781118620762.ch37.

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Schilizzi, Richard T., Ronald D. Ekers, Peter E. Dewdney, and Philip Crosby. "Large Radio Telescopes and the Emergence of the SKA, 1957–1993." In The Square Kilometre Array, 13–46. Cham: Springer International Publishing, 2024. http://dx.doi.org/10.1007/978-3-031-51374-9_2.

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AbstractThe SKA is the culmination of radio telescope design development in the decades prior to 1990. This chapter surveys the earlier telescopes and traces the origins of the ideas behind the SKA design.

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Mullaney, James. "Refracting Telescopes." In The Patrick Moore Practical Astronomy Series, 27–33. New York, NY: Springer New York, 2013. http://dx.doi.org/10.1007/978-1-4614-8733-3_4.

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Mullaney, James. "Reflecting Telescopes." In The Patrick Moore Practical Astronomy Series, 35–46. New York, NY: Springer New York, 2013. http://dx.doi.org/10.1007/978-1-4614-8733-3_5.

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Mullaney, James. "Catadioptric Telescopes." In The Patrick Moore Practical Astronomy Series, 47–53. New York, NY: Springer New York, 2013. http://dx.doi.org/10.1007/978-1-4614-8733-3_6.

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Phillips, Thomas G., Stephen Padin, and Jonas Zmuidzinas. "Submillimeter Telescopes." In Planets, Stars and Stellar Systems, 283–313. Dordrecht: Springer Netherlands, 2013. http://dx.doi.org/10.1007/978-94-007-5621-2_7.

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EkersCSIRO Fellow, Ron, and Thomas L. Wilson. "Radio Telescopes." In Planets, Stars and Stellar Systems, 315–59. Dordrecht: Springer Netherlands, 2013. http://dx.doi.org/10.1007/978-94-007-5621-2_8.

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Lemaire, Philippe, Bernd Aschenbach, and John F. Seely. "Space telescopes." In Observing Photons in Space, 183–210. New York, NY: Springer New York, 2013. http://dx.doi.org/10.1007/978-1-4614-7804-1_9.

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Тези доповідей конференцій з теми "Telescopes"

Renero-C., Francisco-J., Octavio Cardona-N., Roberto Cardona-N., Sergio Vázquez-M., Alejandro Cornejo-R., Carlos Islas-G., and Jorge Romero-A. "Fabrication of the SubReflector for the Large Millimeter Telescope (Gran Telescopio Milimétrico)." In Optical Fabrication and Testing. Washington, D.C.: Optica Publishing Group, 1998. http://dx.doi.org/10.1364/oft.1998.otuc.5.

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Astronomers use telescopes to study the universe in the different spectrum regions. The dimensions of telescopes, to research in the millimeter region, are too big. Thus, fabrication of such instruments is a challenge work. The “Gran Telescopio Milimétrico (Large Millimeter Telescope, which will be called LMT) is a Cassegrain Telescope, which diameter of the primary reflector is 50 meters and the subreflector is a hyperbolic surface which diameter is 2.57 meters, and it is been developed to observe in the millimeter region. The subrelector surface must be fabricated with an accuracy of 13 µm (rms). Furthermore, the subreflector must achieve the so-called wobbling, meaning that the subreflector cannot be so heavy, but enough stiff to be wobbled. In this work, we describe the fabrication technique for the subreflector.

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Oldenettel, Jerry R. "Mirror and dome seeing measurements at AMOS." In Adaptive Optics for Large Telescopes. Washington, D.C.: Optica Publishing Group, 1992. http://dx.doi.org/10.1364/aolt.1992.amc5.

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While the effect of mirror and dome temperatures on seeing quality has been the subject of several recent laboratory experiments (1,2,3), no data from working telescope systems has been published. In this paper, I present data collected on telescopes of two different designs located at the Maui Space Surveillance Site located near the 10,000 foot summit of Haleakala Volcano on Maui, HI. The 1.6 meter aperture AMOS telescope is a closed tube Cassegrain design which tends to trap mirror generated turbulence and channel it along the telescope line of site. The 1.2 meter aperture MOTIF telescope is an open truss Cassegrain design with a short tube which extends about 1 meter above the mirror. The telescopes are housed in separate 15 meter domes located about 50 meters apart.

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Iye, Masanori, and Eiji Nishihara. "Differential Dome Seeing Monitor." In Adaptive Optics for Large Telescopes. Washington, D.C.: Optica Publishing Group, 1992. http://dx.doi.org/10.1364/aolt.1992.amd1.

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The evaluation and control of atmospheric turbulence in the upper atmosphere and around the telescope environment are growing concerns, since these are the last limiting factors in improving the imaging quality of large ground based telescopes. The adaptive optics is naturally a recent topical dynamic approach to control the optical wavefront aberration using a real time servo system. Another line of pains-taking efforts have been made to improve the thermal environment more favorable to telescopes. They are, for example, 1) reducing the thermal mass and thermal time constant of mirrors, telescope structure, and dome structure, 2) removing unneseccary heat sources and cooling the dome against daylight heating, 3) flushing the trapped warm air inside the telescope enclosure, and so on.

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Merkle, Fritz, and Norbert Hubin. "Adaptive Optics for the ESO Very Large Telescope." In Adaptive Optics for Large Telescopes. Washington, D.C.: Optica Publishing Group, 1992. http://dx.doi.org/10.1364/aolt.1992.atua4.

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Adaptive optics is one of the main features of the Very Large Telescope (VLT) of the European Southern Observatory (ESO). The VLT consists of an array of four 8 meter telescopes arranged in a quadrilateral configuration (see Figure 1). These four telescopes can be operated individually, in a so-called incoherent combined mode (mainly for high resolution spectroscopy), and in a coherently combined mode as a long baseline interferometer to achieve highest spatial resolution in the milliarcsecond range. In order to increase the performance and flexibility in use of the VLT in the interferometric mode, two to four mobile telescopes of the two meter class will be added to the array. Each telescope will be equipped with adaptive optics systems for real-time correction of atmospheric turbulence effects.

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Kim, Daewook, Jonathan W. Arenberg, Yuzuru Takashima, Art Palisoc, and Christopher Walker. "SALTUS Probe Class Space Mission: Enabled by 20-m Inflatable Mirror." In CLEO: Applications and Technology. Washington, D.C.: Optica Publishing Group, 2022. http://dx.doi.org/10.1364/cleo_at.2022.aw4i.2.

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SALTUS (Single Aperture Large Telescope for Universe Studies) is a mid/far-infrared telescope concept utilizing a 20-m scale inflatable mirror antenna. The light-weight mirror utilizes a membrane architecture that has been developed and characterized specifically for space-based applications. The telescope's end-to-end optical design and optimization process unleashes the unprecedented photon collecting power of a large space aperture. A series of inflatable mirror prototypes have been designed, manufactured, and tested. These tests confirmed the optical performance of the apertures under space-like conditions. This paradigm changing approach will allow the realization of a new generation of space telescopes far larger than can be achieved utilizing conventional technologies.

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Beckers, Jacques M. "Requirements for Adaptive Optics in Large Astronomical Telescopes." In Adaptive Optics for Large Telescopes. Washington, D.C.: Optica Publishing Group, 1992. http://dx.doi.org/10.1364/aolt.1992.atua1.

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The incorporation of adaptive optics in large astronomical telescopes to provide diffraction limited imaging promises to revolutionize ground based optical astronomy in the next decade. The gains are especially impressive for large aperture telescopes where the large increase in diameter D results both in a decrease of the area of the telescope point spread function proportional to D2 and in an increase in collected photons within that smaller area of D2. The availability of adaptive optics will thus pay off handsomely in many astronomical uses of large telescopes.

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Martin, H. M. "Innovative Optics for Giant Telescopes." In Optical Fabrication and Testing. Washington, D.C.: Optica Publishing Group, 1996. http://dx.doi.org/10.1364/oft.1996.ofd.1.

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The present decade is an unprecedented period of expansion in the collective power of ground-based optical and infrared telescopes worldwide. No fewer than 13 telescopes between 6.5 m and 10 m in diameter--all larger than the most powerful telescope available before 1990--will be completed by roughly the year 2000. Some of these telescopes are designed with specific scientific goals in mind, such as high-resolution infrared imaging and spectroscopy, while others are multi-purpose instruments designed to serve the needs of an astronomical community whose observations have been limited by collecting area and resolving power for several decades. The projects are listed below.

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Leviton, Douglas B., Geraldine A. Wright, Roger J. Thomas, Joseph M. Davila, and Gabriel L. Epstein. "Performance comparison of two Wolter Type II telescopes in the vacuum ultraviolet." In Space Optics for Astrophysics and Earth and Planetary Remote Sensing. Washington, D.C.: Optica Publishing Group, 1991. http://dx.doi.org/10.1364/soa.1991.mf8.

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The SERTS-A and SERTS-C solar telescopes are examples of Wolter Type II glancing incidence telescopes built for flight1,2 on sounding rockets to study active regions on the sun in the extreme ultraviolet wavelength range 24-45 nm. Improvements in computer-controlled polishing technology at GSFC have led to the SERTS-C telescope which has substantially improved throughput and angular resolution in that wavelength range over the earlier SERTS-A. While both telescopes are diffraction-limited in the visible, preventing an obvious selection of the better telescope for flight, laboratory results in the far ultraviolet were used to make the selection and flight data are shown to illuminate these advances.

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Miao, C. H. "Design of Array Systems Using Shared Symmetry." In International Lens Design. Washington, D.C.: Optica Publishing Group, 1990. http://dx.doi.org/10.1364/ild.1990.lwb4.

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The design of multiple aperture array systems intended to cover a relatively wide field of view requires the appropriate combination of individual telescopes feeding a central collecting telescope system. In addition, specific aberration correction and scaling relations between the individual telescopes and the collecting telescope must be maintained. Of necessity there are at lease two optical axes that must be considered in such designs, with rotated symmetries dependent upon the position of each telescope in the array, practical systems should contain a minimum number of components in order to maintain high transmission, leading to the desirable sharing of components between the symmetries of the telescopes and such array designs, and examines the implications of adding aspheric correctors attached to the collector symmetry to the individual components of the telescope array. Two design approaches, one using collecting Mersenne telescopes and a second using four mirror telescopes are compared, the effect of changing primary mirror relative aperture and system length upon the symmetry and order of aberrations arising from the use of eccentric aspheric is explained, and some of the subtle limitations of correcting techniques applicable to adding decentered aspheric to optical design programs as special surfaces are discussed.

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Max, Claire E. "Laser Guide Stars and Large Astronomical Telescopes." In Adaptive Optics for Large Telescopes. Washington, D.C.: Optica Publishing Group, 1992. http://dx.doi.org/10.1364/aolt.1992.afa2.

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Звіти організацій з теми "Telescopes"

Halyo, Valerie. Diamond Pixel Luminosity Telescopes. Office of Scientific and Technical Information (OSTI), December 2014. http://dx.doi.org/10.2172/1166638.

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Hyde, R. A. ,. LLNL. Large aperture Fresnel telescopes/011. Office of Scientific and Technical Information (OSTI), July 1998. http://dx.doi.org/10.2172/304513.

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Swanson, W. P. Aperture of two-counter telescopes. Office of Scientific and Technical Information (OSTI), April 1988. http://dx.doi.org/10.2172/5997515.

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Ma, Binzhong. Research on Large Astronomical Telescopes,. Fort Belvoir, VA: Defense Technical Information Center, July 1995. http://dx.doi.org/10.21236/ada297609.

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Baltz, E. Kaluza-Klein Dark Matter, Electrons and Gamma Ray Telescopes. Office of Scientific and Technical Information (OSTI), December 2004. http://dx.doi.org/10.2172/839776.

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Pollard, Eric L., and Christopher H. Jenkins. Shape Memory Alloy Deployment of Membrane Mirrors for Spaceborne Telescopes. Fort Belvoir, VA: Defense Technical Information Center, January 2005. http://dx.doi.org/10.21236/ada443511.

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Jefferies, Stuart M., and Douglas A. Hope. Advancing the Surveillance Capabilities of the Air Force's Large-Aperature Telescopes. Fort Belvoir, VA: Defense Technical Information Center, March 2014. http://dx.doi.org/10.21236/ada605833.

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Anheier, Norman C., and Cliff S. Chen. A New Approach to Space Situational Awareness using Small Ground-Based Telescopes. Office of Scientific and Technical Information (OSTI), December 2014. http://dx.doi.org/10.2172/1171901.

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Marois, C. High Resolution Imaging of Satellites with Ground-Based 10-m Astronomical Telescopes. Office of Scientific and Technical Information (OSTI), January 2007. http://dx.doi.org/10.2172/1036840.

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Lloyd-Hart, M., and T. McMahon. Adaptive Optics for the 6.5 m MMT Conversion, Development of Very High Resolution Imaging with Adaptive Optics for Large Telescopes, and Advanced Adaptive Optics for the World's Largest Telescopes. Fort Belvoir, VA: Defense Technical Information Center, April 2001. http://dx.doi.org/10.21236/ada387632.

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