Статті в журналах: "Telescopes"

1

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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2

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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3

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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4

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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5

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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6

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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7

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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8

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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9

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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10

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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11

Li, X., X. Yuan, B. Gu, S. Yang, Z. Li, and F. Du. "CHINESE ANTARCTIC ASTRONOMICAL OPTICAL TELESCOPES." Revista Mexicana de Astronomía y Astrofísica Serie de Conferencias 51 (April 13, 2019): 135–38. http://dx.doi.org/10.22201/ia.14052059p.2019.51.23.

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Due to its superb seeing conditions, the Antarctica plateau is widely considered to be an excellent astronomical site. The long periods of uninterrupted darkness at polar sites such as Dome A provide a possibility of continuous observation for more than three months, which is quite suitable for time-domain astronomy. Since 2008, several wide-field optical photometric telescopes, including Chinese Small Telescope ARray (CSTAR), two of the Three Antarctic Survey Telescopes (AST3), have been deployed on Dome A. Science with these telescopes covers variable stars, supernovas, exoplanets, etc. For the remoteness of the Antarctic plateau, these telescopes are designed to observe autonomously and operate remotely via satellite communication. As for future plan, Kunlun Dark Universe Survey Telescope (KDUST), a 2.5-meter optic/infrared telescope, is being proposed as one of the two major facilities of Chinese Antarctic Observatory.

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12

HUGHES, S. B. "INITIAL STEREO ANALYSIS OF MRK 421 FROM THE VERITAS TELESCOPES." International Journal of Modern Physics A 22, no. 14n15 (June 20, 2007): 2461–67. http://dx.doi.org/10.1142/s0217751x07036816.

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VERITAS (Very Energetic Radiation Imaging Telescope Array System), an array of ground-based gamma-ray telescopes in southern Arizona, USA, has been taking data in hardware stereo mode since March, 2006. The April–May 2006 dark run provided a large set of data from two telescopes on the known blazar Markarian (Mrk) 421. An initial analysis produced a light curve and preliminary cuts showing the two telescope array's angular resolution to be 0.19°. The remaining two VERITAS telescopes will be brought online by January, 2007.

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13

Song, Su. "Evolutions and Principles of Space and Radio Telescope." Highlights in Science, Engineering and Technology 72 (December 15, 2023): 47–52. http://dx.doi.org/10.54097/8r8fyx84.

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Contemporarily, various types of telescopes have been proposed as tools for cosmology observation. This study discusses main types of telescopes, i.e., space and radio telescopes people used to observe universe and gives deep description and comparison between them. Radio telescope is the telescope which can receive radio waves from the outer space and can detect waves in different wavelengths besides visible light. It has a long history, as radio telescope is built on Earth and relatively easier for people to make it, but the drawback is that radio telescope may be disturbed by nature conditions easily, even a small change in the strength of wind or the thickness of atmosphere can make a huge difference to the result. While space telescope is different. The first space telescope is Hubble Space Telescope, which is launched in 1990, thus the history of space telescope is relatively short. Compared with radio telescope, space telescope has its own advantage: since it works in space, changing nature conditions in Earth will not affect its precision, and some cancan work without the impact of infrared radiation of the Earth. However, the repair and maintenance cost are problems as it is difficult for people to go to space and fix the broken parts regularly. This paper can help people have a better understanding of these types of telescopes which are used frequently in observation for the universe.

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14

Pramudya, Yudhiakto, A. R. Dhimas Prayoga Jullyantama, M. Khairul Ardi, Cintha Ayu Wandira, and Muchlas. "Observational Technique Development and Instruments Status in Observatorium Universitas Ahmad Dahlan." Journal of Physics: Conference Series 2773, no. 1 (June 1, 2024): 012014. http://dx.doi.org/10.1088/1742-6596/2773/1/012014.

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Abstract The Observatorium Universitas Ahmad Dahlan (UAD) is an urban telescope located in close proximity to city lights. Light pollution monitoring is performed using a Sky Quality Meter and an All Sky Camera, revealing a maximum Night Sky Brightness (NSB) value of 18 mag/arcsec2. A 17-inch Planewave Telescope housed in a 5-meter dome is used to image nebulae and galaxies. Portable telescopes are used to observe the crescent moon, with the use of a buffle and stacking techniques enabling daytime imaging. Lunar elongation and altitude data were obtained to assess the telescope’s capabilities and site feasibility.

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15

Strassmeier, Klaus G., Thomas Granzer, Michael Weber, Manfred Woche, Emil Popow, Arto Järvinen, Janos Bartus, et al. "The STELLA Robotic Observatory on Tenerife." Advances in Astronomy 2010 (2010): 1–11. http://dx.doi.org/10.1155/2010/970306.

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The Astrophysical Institute Potsdam (AIP) and the Instituto de Astrofísica de Canarias (IAC) inaugurated the robotic telescopes STELLA-I and STELLA-II (STELLar Activity) on Tenerife on May 18, 2006. The observatory is located on the Izaña ridge at an elevation of 2400 m near the German Vacuum Tower Telescope. STELLA consists of two 1.2 m alt-az telescopes. One telescope fiber feeds a bench-mounted high-resolution echelle spectrograph while the other telescope feeds a wide-field imaging photometer. Both scopes work autonomously by means of artificial intelligence. Not only that the telescopes are automated, but the entire observatory operates like a robot, and does not require any human presence on site.

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16

Zhou, Weimin. "Analysis of the Observations for Three Telescopes: EHT, FAST and LBTI." Highlights in Science, Engineering and Technology 88 (March 29, 2024): 278–85. http://dx.doi.org/10.54097/9k8yw745.

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As technology continuously advances, the telescope technologies available to humans are becoming increasingly refined, leading to the discovery of an ever-growing number of phenomena using these telescopes. This allows for a deeper understanding of the universe one inhabits, with more astronomical phenomena receiving scientific explanations. This article primarily seeks to broaden our knowledge in this area by describing three distinct astronomical telescopes. It introduces the components and detection principles of the Event Horizon Telescope (EHT), FAST, and the Large Binocular Telescope Interferometer (LBTI). Additionally, this study delves into the primary research objectives, pivotal scientific domains, and ongoing projects of these three telescopes. Moreover, at the conclusion of each section, this study discusses their recent observational results or some noteworthy astronomical phenomena. According to the three examples presented in this article, the aim is to enhance people's understanding of astronomical telescopes and to inspire more individuals to take an interest in the advancements of astrophysics.

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17

Liu, Xuan, Junhong Deng, King Fai Li, Mingke Jin, Yutao Tang, Xuecai Zhang, Xing Cheng, Hong Wang, Wei Liu, and Guixin Li. "Optical telescope with Cassegrain metasurfaces." Nanophotonics 9, no. 10 (April 10, 2020): 3263–69. http://dx.doi.org/10.1515/nanoph-2020-0012.

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AbstractThe Cassegrain telescope, made of a concave primary mirror and a convex secondary mirror, is widely utilized for modern astronomical observation. However, the existence of curved mirrors inevitably results in bulky configurations. Here, we propose a new design of the miniaturized Cassegrain telescope by replacing the curved mirrors with planar reflective metasurfaces. The focusing and imaging properties of the Cassegrain metasurface telescopes are experimentally verified for circularly polarized incident light at near infrared wavelengths. The concept of the metasurface telescopes can be employed for applications in telescopes working at infrared, Terahertz, and microwave and even radio frequencies.

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18

Turner, Michael S. "Extremely large telescopes at risk." Science 382, no. 6673 (November 24, 2023): 857. http://dx.doi.org/10.1126/science.adm9964.

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Images of the cosmos from the Hubble Space Telescope and the James Webb Space Telescope have awed the public and astronomers alike. Until the Hubble, breakthroughs in astronomy came from big telescopes on mountain-top observatories—discoveries that include the expansion of the Universe and planets orbiting other stars. A new generation of extremely large ground-based telescopes is under development, which, when paired with space-based observatories, will produce even more remarkable discoveries about our Universe.

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19

Williams, Richard J., and James Mulherin. "The Development of Advanced-Technology Automated/Robotic Telescope Systems and the Future of Small-Telescope Astronomy." International Astronomical Union Colloquium 183 (2001): 95–101. http://dx.doi.org/10.1017/s0252921100078672.

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AbstractDuring the 1990s groups at universities around the world developed small working automated/robotic telescopes that proved the feasibility of using such systems for education and research projects. A few of the more successful projects such as the Bradford Robotic Observatory in the United Kingdom and the University of Iowa’s Automated Telescope Facility (AFT) and Iowa Robotic Observatory (IRO) programs proved how useful and powerful these systems can be in practice. This paper describes how one company, Torus Technologies, developed hardware and software technologies to create the most advanced integrated small automated/robotic telescope systems in the world. These systems were designed from the “bottom up” to be automated/robotic telescopes capable of operating an entire observatory including domes, CCD cameras, and other peripheral equipment.Automated/robotic telescopes can play a major role in enabling small colleges and universities, especially in developing countries, to actively participate in serious “hands on” research and education projects that otherwise would not be practical. A commercially available affordable, high-precision, and proven turnkey automated/robotic small telescope system capable of operating remotely via the Internet is crucial for bringing this technology into widespread use. Today Torus Technologies telescopes are installed at locations worldwide as primary instruments for research programs, discovery and monitoring programs, and education programs. This paper describes some of the current applications for using these telescopes and how these telescope systems will be used in the future in standalone installations and in global networks.

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20

Hall, A., I. L. Bailey, L. S. Kekelis, T. W. Raasch, and G. L. Goodrich. "Retrospective Survey to Investigate Use of Distance Magnifiers for Travel." Journal of Visual Impairment & Blindness 81, no. 9 (November 1987): 418–23. http://dx.doi.org/10.1177/0145482x8708100906.

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Seventy-eight subjects from the Western Blind Rehabilitation Center at the Palo Alto Veterans Administration Hospital and 34 subjects from the U.C. Berkeley Low Vision Center were surveyed to investigate the use of distance magnifiers for travel. Information is reported regarding demographic characteristics, vision characteristics, usual travel patterns, characteristics of telescopes used by the subjects, telescope training, and travel habits with telescopic devices, along with similarities and differences between the two groups.

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21

Bedding, T. R., J. M. Beckers, M. Faucherre, N. Hubin, B. Koehler, O. von der Lühe, F. Merkle, and N. Zhu. "The VLT Interferometer." Symposium - International Astronomical Union 158 (1994): 143–50. http://dx.doi.org/10.1017/s0074180900107454.

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One of the observing modes available with the ESO Very Large Telescope will be coherent combination of the light received by up to four 8 m unit telescopes and several 1.8 m auxiliary telescopes. The location of the main telescopes is fixed, while auxiliary telescopes can be moved among some 30 observing stations. The locations of these stations were chosen to augment the (u, v) coverage of the unit telescopes as well as to function as an independent interferometric array.The 8 m telescopes will be equipped with adaptive optics to correct for seeing-induced wavefront aberrations. This wavefront correction will be complete at near-infrared wavelengths, giving the interferometer very high sensitivity in this spectral regime. This paper gives a brief description of the VLT Interferometer and an update on its status.

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22

Zeldovich, Lina. "A Golden Eye in the Sky." Mechanical Engineering 145, no. 6 (November 29, 2023): 24–29. http://dx.doi.org/10.1115/1.2023-nov1.

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Abstract The James Webb Telescope is NASA’s largest and most complex orbiting observatory to date. Ten years in the making at a price tag of nearly $10 billion, Webb was designed to not only go where no other telescopes have gone before, but also see things no other telescopes have been able to see. This is the story of the engineering underpinning this new space telescope.

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23

Davis, John. "Commission 9: Instruments and Techniques (Instruments et Techniques)." Transactions of the International Astronomical Union 21, no. 1 (1991): 41–52. http://dx.doi.org/10.1017/s0251107x00009780.

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The period covered by this report has seen significant progress in the development of the new generation of telescopes with apertures in the 8 m plus range. The period has encompassed the major construction phase of the 10 m Keck Telescope, witnessed the commissioning of the European Southern Observatory’s (ESO) New Technology Telescope and the approval of funding for the ESO Very Large Telescope (VLT). Significant progress has been achieved in developing the necessary technology for manufacturing and figuring large mirrors. There have been major expansions of activity in the areas of active control of telescope optics and adaptive optics, and in high angular resolution interferometry with several new groups entering both fields. The use of optical fibers, particularly in the area of multiple-object spectroscopy, has continued to grow. Several telescopes can now be operated remotely and the control systems of new telescopes are being designed to facilitate remote operation.

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24

Jhetam, Siddeeqa, and Khathutshelo P Mashige. "Effects of spectacles and telescopes on visual function in students with oculocutaneous albinism." African Health Sciences 20, no. 2 (July 22, 2020): 758–67. http://dx.doi.org/10.4314/ahs.v20i2.28.

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Purpose: To investigate the effects of spectacle and telescope corrections on visual acuity (VA), contrast sensitivity (CS) and reading rates (RR) in students with oculocutaneous albinism (OCA). Methods: An observational study design was conducted on 81 students with OCA. Distance and near VA, CS and RR were measured without correction, with spectacle correction and with a combination of spectacle correction and telescopes. Results: The mean distance and near VA values with a combination of spectacle correction and telescopes were significantly better than those without correction and with spectacle correction alone (p = 0.01). Mean CS values achieved with spectacles alone were significantly better than those obtained with a combination of spectacles and telescopes (p = 0.01). There was no significant difference between logCS values obtained without correction compared to those obtained with a combination of spectacle correction and telescopes. There were no significant differences between RR values obtained with a combination of spectacles and telescopes and those without and with spectacle correction alone (all p > 0.05). Conclusion: This article provides valuable information to eye care practitioners on the effects of spectacles and telescopes on visual acuity, contrast sensitivity and reading rate in students with OCA. Keywords: Oculocutaneous albinism; visual acuity; telescope; contrast sensitivity; reading rate.

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25

Bennett, J. A. "Book Review: Telescopic Curiosities: Unusual Telescopes." Journal for the History of Astronomy 24, no. 4 (November 1993): 306. http://dx.doi.org/10.1177/002182869302400409.

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26

Mack, Peter, John Stein, and Wonyong Han. "ACE FlexGrid Telescope Flexure and Pointing Software." International Astronomical Union Colloquium 183 (2001): 111–12. http://dx.doi.org/10.1017/s0252921100078696.

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AbstractWe describe ACE FlexGrid, a telescope flexure and pointing model based on an empirical grid of reference points. This software is valid for all types of telescopes and is especially suited to robotic telescopes which repeatedly observe the same object.

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27

Ofek, E. O., S. Ben-Ami, D. Polishook, E. Segre, A. Blumenzweig, N. L. Strotjohann, O. Yaron, et al. "The Large Array Survey Telescope—System Overview and Performances." Publications of the Astronomical Society of the Pacific 135, no. 1048 (June 1, 2023): 065001. http://dx.doi.org/10.1088/1538-3873/acd8f0.

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Abstract The Large Array Survey Telescope (LAST) is a wide-field visible-light telescope array designed to explore the variable and transient sky with a high cadence. LAST will be composed of 48, 28 cm f/2.2 telescopes (32 already installed) equipped with full-frame backside-illuminated cooled CMOS detectors. Each telescope provides a field of view (FoV) of 7.4 deg2 with 1.″25 pix−1, while the system FoV is 355 deg2 in 2.9 Gpix. The total collecting area of LAST, with 48 telescopes, is equivalent to a 1.9 m telescope. The cost-effectiveness of the system (i.e., probed volume of space per unit time per unit cost) is about an order of magnitude higher than most existing and under-construction sky surveys. The telescopes are mounted on 12 separate mounts, each carrying four telescopes. This provides significant flexibility in operating the system. The first LAST system is under construction in the Israeli Negev Desert, with 32 telescopes already deployed. We present the system overview and performances based on the system commissioning data. The B p 5σ limiting magnitude of a single 28 cm telescope is about 19.6 (21.0), in 20 s (20 × 20 s). Astrometric two-axes precision (rms) at the bright-end is about 60 (30) mas in 20 s (20 × 20 s), while absolute photometric calibration, relative to GAIA, provides ∼10 millimag accuracy. Relative photometric precision, in a single 20 s (320 s) image, at the bright-end measured over a timescale of about 60 minutes is about 3 (1) millimag. We discuss the system science goals, data pipelines, and the observatory control system in companion publications.

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28

Mandat, Dusan, Toshihiro Fujii, Max Malacari, John Farmer, Xiaochen Ni, Paolo Privitera, Justin Albury, et al. "Atmospheric monitoring with the Fluorescence detector Array of Single-pixel Telescopes." EPJ Web of Conferences 197 (2019): 02002. http://dx.doi.org/10.1051/epjconf/201919702002.

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The Fluorescence detector Array of Single-pixel Telescopes (FAST) is a proposed low-cost, largearea, next-generation experiment for the detection of ultrahigh-energy cosmic rays (UHECRs) via the atmospheric fluorescence technique. Two FAST telescopes are currently installed and operating at the Black Rock Mesa site of the Telescope Array Experiment in Utah, USA. Knowledge of the properties of the atmosphere above the detector is of utmost importance for the analysis and reconstruction of the energy and trajectory of UHECRs measured with an atmospheric fluorescence telescope. The FAST experiment uses all sky camera (FASCam) and sky quality monitor (SQM) for the detection of clouds and quantification of the night-sky background light in the field-of-view of the telescopes. Measurements of a vertically-fired ultra-violet laser at a distance of 21 km from the FAST telescopes are used to infer the transparency of the atmosphere above the detector through comparison with simulations.

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29

Blalock, Todd, Brian Myer, Brittany Cox, and Jessica Nelson. "The Manufacturing of a Multi-surface Monolithic Telescope with Freeform Surfaces." EPJ Web of Conferences 215 (2019): 06004. http://dx.doi.org/10.1051/epjconf/201921506004.

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Monolithic multi-surface telescopes combined with freeform optical surfaces provide improvements in optical performance in a smaller footprint as compared to systems with spherical surfaces, while providing superior mechanical stability to traditional telescope assemblies. Three different monolithic telescope concepts, in different configurations and optical performance were produced as proof of concepts. The results of the telescopes are presented as well as the unique manufacturing and testing challenges to produce these monolithic optical systems.

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30

Kuyk, T. "Telescopic Low Vision Aids with Motorized and Auto Focuses." Journal of Visual Impairment & Blindness 90, no. 4 (July 1996): 333–40. http://dx.doi.org/10.1177/0145482x9609000408.

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Prototypes of motorized-focus telescopes (MFTs) and of a 4X auto-focus telescope (AFT) were constructed, and 22 users of hand-focus telescopes (HFTs) were trained to use them for near-distance and intermediate-distance tasks. Despite the lack of differences in performance with the MFT, AFT, and HFT, the subjects’ ratings on 9 of 10 aspects of telescope performance were significantly higher for the AFT and MFT than for the HFT.

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31

Zhao, Yong, Yingqiang Wang, Fei He, Zhonghua Yao, Zhaojin Rong, and Yong Wei. "A Simplified Pointing Model for Alt-Az Telescopes." Applied Sciences 13, no. 20 (October 12, 2023): 11238. http://dx.doi.org/10.3390/app132011238.

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The telescope pointing model plays a crucial role in characterizing and explaining the inaccuracies in the telescope’s pointing. It uses mathematical models to express these errors and suggests methods to calibrate and rectify them. By employing the pointing model, one can gain a deeper understanding of the discrepancies in the telescope’s pointing accuracy at various positions and orientations. This article introduces the establishment and validation of a simplified pointing model for correcting the pointing errors of an alt-az telescope. The traditional telescope pointing model, with its complex formulas, makes it difficult to quickly apply for the calibration of the telescope’s pointing. This method utilizes two-dimensional surface fitting to obtain the telescope’s pointing error function, enabling a rapid determination of the telescope’s pointing model, which is then validated on the Planetary Atmospheric Spectroscopic Telescope (PAST). Using this method, the azimuth axis and altitude axis errors (root mean square error—RMSE) of the PAST telescope are 6.8 arcs and 3.8 arcs, respectively.

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32

Hofmann, Werner. "Intercalibration of Cherenkov telescopes in telescope arrays." Astroparticle Physics 20, no. 1 (October 2003): 1–3. http://dx.doi.org/10.1016/s0927-6505(03)00137-3.

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33

Ekers, R. D. "Review of Linked Array Instruments." Highlights of Astronomy 8 (1989): 551–52. http://dx.doi.org/10.1017/s1539299600008297.

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At cm wavelengths aperture synthesis radio-telescopes (arrays of linked antennas which synthesize an image of the sky with high angular resolution) are now becoming the dominant astronomical research tool. Major new facilities such as the VLA are in full operation, others such as the Australia Telescope are nearing completion and a number of telescopes designed to form images in real time have been converted to operate in the aperture synthesis mode (e.g. MOST, Bologna Cross). See Napier et al. (1983) for a review of modern synthesis telescopes. The high resolution, sensitivity and freedom from confusion have led the aperture synthesis telescopes into very diverse astronomical applications.

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34

Watson, F. G. "Multi-Fibre Spectroscopy with Schmidt Telescopes." International Astronomical Union Colloquium 148 (1995): 70–80. http://dx.doi.org/10.1017/s0252921100021734.

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AbstractLarge Schmidt telescopes are peculiarly well-suited to multifibre spectroscopy. The extent to which the small aperture is compensated by the wide field is illustrated by the fact that the total photon throughput of the 1.2 m UK Schmidt Telescope (UKST) is almost identical to that of the 3.9 m Anglo-Australian Telescope (AAT) in its new 2-degree field (2dF) mode. In the implementation of the technique, Schmidt telescopes have a number of practical advantages, while there is no shortage of scientific problems that can be addressed. However, the instrumentation required to capitalize fully on this potential is costly and, because Schmidts are perceived as “small” telescopes with a specialist following, the required funding is likely to remain elusive.

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35

Zheng, Binwen. "Comparison and Demonstration of the Principle and Applications for the State-of-art Astrophysical Telescopes." Highlights in Science, Engineering and Technology 38 (March 16, 2023): 37–44. http://dx.doi.org/10.54097/hset.v38i.5693.

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With the rapid development of the technique for optics engineering, the telescope has developed rapidly with great performances (i.e., higher resolution), which exhibits great potential in cosmology detection. On this basis, this paper compares and demonstrates the basic principle as well as the state-of-art applications and observations of two typical telescopes, i.e., the Arecibo and Fast. According to the analysis, the later constructed FAST largely expands the searching parameters which offer a path for higher signal-noise ratio. However, it should be noted that ground-based telescopes do have some shortcomings and defects. The revision suggestions are also proposed in order to better upgrade the performances of the telescopes. These results shed light on guiding further exploration of future telescope construction.

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36

Wu, Shengyin, Shouguan Wang, Yukuan Mao, and Yan Su. "Trying to Enlarge the Sky Coverage of the FAST." International Astronomical Union Colloquium 182 (2001): 249–53. http://dx.doi.org/10.1017/s0252921100001068.

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AbstractThe proposed FAST project is a novel giant spherical radio telescope, with active elements which form a temporary paraboloid to track radio objects in the sky. Efforts have been made to extend the limited sky coverage that is a characteristic disadvantage of Arecibo-style radio telescopes. Three measures under investigation are introduced in this paper. The expected performance of the telescope is described, and a brief comparison is made with some of the largest existing radio telescopes.

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37

Kuzin S.V., Bogachev S.A., Erkhova N.F., Pertsov A.A., Loboda I.P., Reva A.A., Kholodilov A.V., et al. "Solar VUV telescope for nanosatellites." Technical Physics 92, no. 13 (2022): 2021. http://dx.doi.org/10.21883/tp.2022.13.52216.115-21.

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Within the Universat program, a set of solar vacuum ultraviolet (VUV) telescopes has been developed for deployment on 6U nanosatellites. Telescopes are designed to get images of the solar corona. The spectral ranges of observations is considered, the characteristics of the nanosatellite from the point of view of the observations feasibility are opmized, the optical scheme of the telescope and VUV multilayer mirrors coatings and thin-film filters are modelled. Keywords: Nanosatellite, VUV, telescope, solar corona.

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38

Nekola, Martin, René Hudec, Martin Jelínek, Petr Kubánek, Jan Štrobl, and Cyril Polášek. "BART: The Czech Autonomous Observatory." Advances in Astronomy 2010 (2010): 1–5. http://dx.doi.org/10.1155/2010/103986.

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The High Energy Astrophysics group of the stellar department of the Astronomical Institute in Ondřejov operates two small aperture robotic telescopes called BART and D50. Both telescopes are capable of making automatic followup observation of gamma-ray burst optical counterparts. This paper deals with the smaller telescope BART.

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39

Hippler, Stefan. "Adaptive Optics for Extremely Large Telescopes." Journal of Astronomical Instrumentation 08, no. 02 (May 29, 2019): 1950001. http://dx.doi.org/10.1142/s2251171719500016.

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Adaptive Optics (AO) has become a key technology for the largest ground-based telescopes currently under, or close to beginning of, construction. AO is an indispensable component and has basically only one task, that is to operate the telescope at its maximum angular resolution, without optical degradations resulting from atmospheric seeing. Based on three decades of experience using AO usually as an add-on component, all extremely large telescopes and their instrumentation are designed for diffraction limited observations from the very beginning. This paper illuminates various approaches of the ELT, the Giant Magellan Telescope (GMT), and the Thirty-Meter Telescope (TMT), to fully integrate AO in their designs. The paper concludes with a brief look into the requirements that high-contrast imaging poses on AO.

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40

Iyer, Aditya Arun, Gautham Manuru Prabhu, Tanay Gupta, Shrey Deshmukh, and Rushit Rivankar. "Exploring Design Optimisation Techniques of a Radio Telescope Using Fixed Costing Constraints." Journal of Physics: Conference Series 2571, no. 1 (October 1, 2023): 012031. http://dx.doi.org/10.1088/1742-6596/2571/1/012031.

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Abstract Cost optimization is a common problem encountered in the design of telescopes. This paper comprehensively discusses various radio telescope designs worldwide, focusing on their design and utilities. It contextualizes the Pulsar data challenge and subsequently discusses and develops a mathematical model for designing radio telescopes. The model assumes a fixed-cost budget. This paper expands current ideas of modeling the system using figure-of-merit equations and optimizing them based on a fixed budget to obtain optimal and affordable radio telescope designs.

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41

Jeon, Young-Beom, Chow-Choong Ngeow, and James M. Nemec. "Ground-based photometry for 42 Kepler-field RR Lyrae stars." Proceedings of the International Astronomical Union 9, S301 (August 2013): 427–28. http://dx.doi.org/10.1017/s1743921313014889.

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AbstractFollow-up (U)BVRI photometric observations have been carried out for 42 RR Lyrae stars in the Kepler field. The new magnitude and color information will complement the available extensive high-precision Kepler photometry and recent spectroscopic results. The photometric observations were made with the following telescopes: 1-m and 41-cm telescopes of Lulin Observatory (Taiwan), 81-cm telescope of Tenagra Observatory (Arizona, USA), 1-m telescope at the Mt. Lemmon Optical Astronomy Observatory (LOAO, Arizona, USA), 1.8-m and 15-cm telescopes at the Bohyunsan Optical Astronomy Observatory (BOAO, Korea) and 61-cm telescope at the Sobaeksan Optical Astronomy Observatory (SOAO, Korea). The observations span from 2010 to 2013, with ~200 to ~600 data points per light curve. Preliminary results of the Korean observations were presented at the 5th KASC workshop in Hungary. In this work, we analyze all observations. These observations permit the construction of full light curves for these RR Lyrae stars and can be used to derive multi-filter Fourier parameters.

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42

Bloch, Jeffrey. "EUV Astrophysics with ALEXIS: The Wide View." International Astronomical Union Colloquium 152 (1996): 7–14. http://dx.doi.org/10.1017/s0252921100035685.

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The Array of Low Energy X-ray Imaging Sensors (ALEXIS) satellite is Los Alamos’ pathfinding small space mission achieving low cost and rapid development time for its technology demonstration and science goals. The ALEXIS satellite contains the ALEXIS telescope array, which consists of six EUV/ultrasoft X-ray telescopes utilizing normal incidence multilayer mirrors, microchannel plate detectors, and thin UV rejecting filters. Each telescope is tuned to a relatively narrow bandpass centered at either 130, 171, or 186 angstroms. Each telescope has a 33° field-of-view, and a resolution of ~ 0.25°. With each 50 s rotation of the satellite, the telescopes scan most of the anti-solar hemisphere of the sky. The spacecraft is controlled exclusively from a ground station located at Los Alamos.This paper discusses the characteristics and performance of the ALEXIS telescopes and the results from the mission in spite of the damage incurred to the spacecraft at launch.

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43

Jacoby, G. H. "Research programmes, productivity, and usage statistics for the 0.9m telescopes at Kitt Peak." Symposium - International Astronomical Union 118 (1986): 237–39. http://dx.doi.org/10.1017/s0074180900151368.

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Current research programmes using the smaller telescopes at Kitt Peak include spectroscopy, photometry, and imaging of clusters, variable stars, nebulae, and extragalactic objects. Their scientific productivity is competitive with the 4m and 2.1m telescopes. Subscription rates indicate that when advanced instrumentation is made available on a small telescope, the demand will increase significantly.

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44

Crawford, David L. "A Global Network of Small Telescopes as a Resource for Astronomical Research and Education." Highlights of Astronomy 11, no. 2 (1998): 923–26. http://dx.doi.org/10.1017/s1539299600019171.

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There is no question that relatively small telescopes are powerful tools for astronomy, just as they always have been. With the new detectors and full usage of computers, they have become even more powerful, enabling us to do with a one-meter aperture telescope today more than 4-meter or 5-meter telescopes could do only a few decades ago. And the small ones cost a lot less to build and operate than the large ones. As such, small telescopes are the main hope for observing time for the many astronomers worldwide who need them as part of their research (or educational) tools. They can make a major impact on many areas of research and will be of great value for scientific education as well. Astronomy is very interesting to students and to the general public, not just to astronomers. Furthermore, most areas of astronomical research are data poor and more telescopes are needed to effectively attack the problems. Only a very few of us have adequate telescope time for our research or educational needs.

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45

Twarog, B. A. "Stellar photometry with small telescopes." Symposium - International Astronomical Union 118 (1986): 135–47. http://dx.doi.org/10.1017/s0074180900151289.

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The dominant trend within stellar photometry in recent years has been an increase in the number of intermediate and narrow-band photometric observations, particularly with small telescopes. Recent examples illustrating the scope and emphasis of such programs are reviewed. It is concluded that with continuing improvement in detector technology and telescope automation, small telescope photometry will grow in importance.

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46

Wang, Jing-Sheng. "Newly Installed Radio and Optical Telescopes in China." Publications of the Astronomical Society of Australia 9, no. 1 (1991): 60–61. http://dx.doi.org/10.1017/s1323358000024899.

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AbstractNew radio and optical telescopes installed in recent years in China are summarised. These include the 2.16-m optical telescope, the solar magnetic field telescope, the Miyun synthesis radio telescope, the 1.26-m infrared telescope (Beijing Astronomical Observatory), the 25-m radio telescope as the first station of China’s VLBI network, the 1.56-m astrometric telescope (Shanghai Observatory), and the 13.7-m millimetre wave radio telescope.

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47

Zhang, Yajie, Ce Yu, Chao Sun, Zhaohui Shang, Yi Hu, Huiyu Zhi, Jinmao Yang, and Shanjiang Tang. "A Multilevel Scheduling Framework for Distributed Time-domain Large-area Sky Survey Telescope Array." Astronomical Journal 165, no. 3 (February 1, 2023): 77. http://dx.doi.org/10.3847/1538-3881/acac24.

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Abstract Telescope arrays are receiving increasing attention due to their promise of higher resource utilization, greater sky survey area, and higher frequency of full space-time monitoring than single telescopes. Compared with the ordinary coordinated operation of several telescopes, the new astronomical observation mode has an order of magnitude difference in the number of telescopes. It requires efficient coordinated observation by large-domain telescopes distributed at different sites. Coherent modeling of various abstract environmental constraints is essential for responding to multiple complex science goals. Also, due to competing science priorities and field visibility, how the telescope arrays are scheduled for observations can significantly affect observation efficiency. This paper proposes a multilevel scheduling model oriented toward the problem of telescope-array scheduling for time-domain surveys. A flexible framework is developed with basic functionality encapsulated in software components implemented on hierarchical architectures. An optimization metric is proposed to self-consistently weight contributions from time-varying observation conditions to maintain uniform coverage and efficient time utilization from a global perspective. The performance of the scheduler is evaluated through simulated instances. The experimental results show that our scheduling framework performs correctly and provides acceptable solutions considering the percentage of time allocation efficiency and sky coverage uniformity in a feasible amount of time. Using a generic version of the telescope-array scheduling framework, we also demonstrate its scalability and its potential to be applied to other astronomical applications.

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48

Jilek, Vlastimil, Dusan Mandat, Francesco Salamida, and Zuzana Svozilikova. "Potential for atmospheric monitoring using FAST telescopes." Journal of Physics: Conference Series 2398, no. 1 (December 1, 2022): 012015. http://dx.doi.org/10.1088/1742-6596/2398/1/012015.

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Abstract The Fluorescence detector Array of Single-pixel Telescopes (FAST) is a design for a next-generation ground-based ultra-high energy cosmic ray observatory, addressing the requirements for a large-area, low-cost detector suitable for measuring the properties of the highest energy cosmic rays with an unprecedented aperture. Three telescope prototypes are installed nearby the fluorescence telescopes of Telescope Array and one prototype is located at the Pierre Auger Observatory. Apart from detecting cosmic ray showers, the FAST prototypes offer the possibility of detecting laser pulses from atmospheric facilities such as CLF. The first part of the contribution describes the theoretical modeling of the photon scattering processes for different atmospheric models, and the raytracing of photons from the laser shot to and inside the FAST telescope. Simulations will be performed for different types of scattering conditions dependent on e.g. the size of the scattering centers or other parameters such as humidity. The ultimate goal is to create a software tool simulating the measured signals in the FAST telescopes from distant laser shots with proper treatment of light propagation trough the atmosphere and trough the detector. Such simulation toolkit for FAST prototypes at the Pierre Auger Observatory will benefit from existing attempts done for the Telescope Array site. Another part of the contribution will concern the real data of the observed CLF shots by the FAST prototypes both at the Pierre Auger Observatory and Telescope Array. Moreover, we can focus on the comparison of measured CLF shots by FAST prototype with the available data recorded by the full-scale fluorescence telescopes of the Pierre Auger Observatory.

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49

Richtsmeier, William J., and Richard L. Scher. "Telescopic Laryngeal and Pharyngeal Surgery." Annals of Otology, Rhinology & Laryngology 106, no. 12 (December 1997): 995–1001. http://dx.doi.org/10.1177/000348949710601202.

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Surgery of the hypopharynx and larynx has traditionally been performed with either direct, unaided vision or the operating microscope. We proposed to extend the surgical capability provided by angled Hopkins telescopes to the larynx and hypopharynx. Forty-eight cases in which rigid telescopes were employed primarily for intervention were reviewed. We found significant advantages of the telescopic system when performing procedures on surfaces that were not 90° from the observer, such as the walls of the hypopharynx, the petiole of the epiglottis, the ventricle, and the posterior commissure. Both 30° and 70° telescopes were found useful, but required complementary instruments. The potassium titanyl phosphate laser's flexible fiber provided a distinct advantage in resecting lesions that presented on vertical surfaces. Telescopes also permitted the use of large instruments designed for intraperitoneal and intrathoracic surgery that blocked the view of the operating microscope. Telescopic pharyngeal and laryngeal visualization allowed surgical procedures complementary to more traditional forms of endoscopic surgery.

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50

Gomez, E. L. "Las Cumbres Observatory: Building a global telescope network from the ground up." Proceedings of the International Astronomical Union 10, H16 (August 2012): 646. http://dx.doi.org/10.1017/s1743921314012678.

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AbstractLas Cumbres Observatory Global Telescope Network (LCOGT) are building a global network of telescopes which will be available to both professional scientists and the science curious public. This telescope network will be global and so will the community, therefore all aspects of the endeavour must be online and self-sustaining - from the observing software to the analysis tools. During 2012 LCOGT have deployed the first 1-meter telescopes, and launched a citizen science project using LCOGT data, Agent Exoplanet, as well as many other online resources for anyone to use as they explore astronomy.

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