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Artigos de revistas sobre o tema "Telescopes"

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Autor: Grafiati

Publicado: 4 de junho de 2021

Última modificação: 10 de março de 2023

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1

Tokunaga, A. T., C. Ftaclas, J. R. Kuhn e 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.

2

Kim, Sang Chul. "Paper Productivity of Ground-based Large Optical Telescopes from 2000 to 2009". Publications of the Astronomical Society of Australia 28, n.º 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.

3

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.

4

Li, Yuqiao. "State-of-art Facilities and Prospect of Radio Telescopes". Highlights in Science, Engineering and Technology 5 (7 de julho de 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.

5

Porter, F. I., J. M. White, J. Goldberg, J. L. Demer e A. Koval. "Predicting Successful Low Vision Rehabilitation with Telescopic Spectacles". Journal of Visual Impairment & Blindness 86, n.º 1 (janeiro de 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.

6

Burton, Michael G., John W. V. Storey e Michael C. B. Ashley. "Science Goals for Antarctic Infrared Telescopes". Publications of the Astronomical Society of Australia 18, n.º 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.

7

Li, X., X. Yuan, B. Gu, S. Yang, Z. Li e F. Du. "CHINESE ANTARCTIC ASTRONOMICAL OPTICAL TELESCOPES". Revista Mexicana de Astronomía y Astrofísica Serie de Conferencias 51 (13 de abril de 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.

8

HUGHES, S. B. "INITIAL STEREO ANALYSIS OF MRK 421 FROM THE VERITAS TELESCOPES". International Journal of Modern Physics A 22, n.º 14n15 (20 de junho de 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.

9

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.

10

Liu, Xuan, Junhong Deng, King Fai Li, Mingke Jin, Yutao Tang, Xuecai Zhang, Xing Cheng, Hong Wang, Wei Liu e Guixin Li. "Optical telescope with Cassegrain metasurfaces". Nanophotonics 9, n.º 10 (10 de abril de 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.

11

Bennett, J. A. "Book Review: Telescopic Curiosities: Unusual Telescopes". Journal for the History of Astronomy 24, n.º 4 (novembro de 1993): 306. http://dx.doi.org/10.1177/002182869302400409.

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12

Williams, Richard J., e 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.

13

Bedding, T. R., J. M. Beckers, M. Faucherre, N. Hubin, B. Koehler, O. von der Lühe, F. Merkle e 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.

14

Hall, A., I. L. Bailey, L. S. Kekelis, T. W. Raasch e G. L. Goodrich. "Retrospective Survey to Investigate Use of Distance Magnifiers for Travel". Journal of Visual Impairment & Blindness 81, n.º 9 (novembro de 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.

15

Davis, John. "Commission 9: Instruments and Techniques (Instruments et Techniques)". Transactions of the International Astronomical Union 21, n.º 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.

16

Jhetam, Siddeeqa, e Khathutshelo P Mashige. "Effects of spectacles and telescopes on visual function in students with oculocutaneous albinism". African Health Sciences 20, n.º 2 (22 de julho de 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.

17

Mack, Peter, John Stein e 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.

18

Hofmann, Werner. "Intercalibration of Cherenkov telescopes in telescope arrays". Astroparticle Physics 20, n.º 1 (outubro de 2003): 1–3. http://dx.doi.org/10.1016/s0927-6505(03)00137-3.

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19

Blalock, Todd, Brian Myer, Brittany Cox e 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.

20

Kuyk, T. "Telescopic Low Vision Aids with Motorized and Auto Focuses". Journal of Visual Impairment & Blindness 90, n.º 4 (julho de 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.

21

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.

22

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.

23

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.

24

Hippler, Stefan. "Adaptive Optics for Extremely Large Telescopes". Journal of Astronomical Instrumentation 08, n.º 02 (29 de maio de 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.

25

Nekola, Martin, René Hudec, Martin Jelínek, Petr Kubánek, Jan Štrobl e 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.

26

Wu, Shengyin, Shouguan Wang, Yukuan Mao e 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.

27

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, n.º 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.

28

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.

29

Wang, Jing-Sheng. "Newly Installed Radio and Optical Telescopes in China". Publications of the Astronomical Society of Australia 9, n.º 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.

30

Jeon, Young-Beom, Chow-Choong Ngeow e James M. Nemec. "Ground-based photometry for 42 Kepler-field RR Lyrae stars". Proceedings of the International Astronomical Union 9, S301 (agosto de 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.

31

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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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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Jilek, Vlastimil, Dusan Mandat, Francesco Salamida e Zuzana Svozilikova. "Potential for atmospheric monitoring using FAST telescopes". Journal of Physics: Conference Series 2398, n.º 1 (1 de dezembro de 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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Crawford, David L. "A Global Network of Small Telescopes as a Resource for Astronomical Research and Education". Highlights of Astronomy 11, n.º 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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Zhang, Yajie, Ce Yu, Chao Sun, Zhaohui Shang, Yi Hu, Huiyu Zhi, Jinmao Yang e Shanjiang Tang. "A Multilevel Scheduling Framework for Distributed Time-domain Large-area Sky Survey Telescope Array". Astronomical Journal 165, n.º 3 (1 de fevereiro de 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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Genet, Russell M., Louis J. Boyd e Douglas S. Hall. "Variable star observations with automatic telescopes". Symposium - International Astronomical Union 118 (1986): 47–55. http://dx.doi.org/10.1017/s0074180900151009.

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Small automatic telescopes have been used for several years to make wide band, differential photometric observations of brighter variable stars. For example, a single automatic telescope located in Arizona has been used to study essentially the entire class of RS Canum Venaticorum binaries. These stars have changing spot structures that require once-a-night photometric observations - an ideal job for an automatic telescope located in the clear skies of Arizona. The operation of such automatic systems has become so routine that an “Automatic Photoelectric Telescope Service” now makes photometric observations for any institution so requesting. A list of stars is sent to the Arizona site of this service, and every three months the observational results are returned, with the cost typically being similar to the publication page charges. Currently the use of automatic telescopes is being extended to fainter stars and narrower bandwidths. For instance, a highly specialized one-meter telescope has been designed for automatic observations of Ca II K-line emissions from brighter active chromosphere stars. Further extensions of such automation seem likely.

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Richtsmeier, William J., e Richard L. Scher. "Telescopic Laryngeal and Pharyngeal Surgery". Annals of Otology, Rhinology & Laryngology 106, n.º 12 (dezembro de 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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Gomez, E. L. "Las Cumbres Observatory: Building a global telescope network from the ground up". Proceedings of the International Astronomical Union 10, H16 (agosto de 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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Soonthornthum, Boonraksar. "What Can be Done with Small Telescopes?" Transactions of the International Astronomical Union 24, n.º 3 (2001): 243–49. http://dx.doi.org/10.1017/s0251107x00000900.

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AbstractModern astronomy has developed rapidly in the last few decades. Large telescopes, several metres in diameter, have been constructed and installed at many sites around the world, in order to carry out high-quality research work at the frontiers of astronomy. In many parts of the world, only small telescopes are available, because of budgetary limitations and the stage of development of science in the country. However, much effort has been put into using these small telescopes to the best of their capabilities. A small telescope with modern detectors can do good astronomical research. Sirindhorn Observatory, Chiang Mai University, is the only observatory in northern Thailand which plays an active role in astronomical research. The major instrument is the 40-cm Cassegrain reflecting telescope with standard wide-band and intermediate band photoelectric photometers, CCD photometers and a CCD spectrograph. Because of Thailand’s hot and humid climate, the telescopes and detectors at Sirindhorn Observatory need regular maintenance. Major research at the Observatory emphasizes the study of physical propoerties and evolution of close binary systems, especially near-contact and contact binaries, by photometric techniques. Networks in this field of research have been established through national and international collaboration with some astronomical institutes in the region. A larger telescope is being developed for more efficiency in operation; it is expected to be able to serve the future development of astronomical research in Thailand.

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Chen, Yufan (Jerry). "Understanding Black Hole Imaging Based on Very Large Baseline Interferometry (VLBI)". Applied Science and Innovative Research 6, n.º 3 (15 de junho de 2022): p21. http://dx.doi.org/10.22158/asir.v6n3p21.

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In 2019, the Event Horizon Telescope made history when it captured the first known image of a blackhole. The black hole, situated in the center of the Messier 87 galaxy, is more than 55 million light-years away from earth, and was only able to be captured using Very Large Baseline Interferometry (VLBI) technology and the computational imaging technologies integrated into the Event Horizon Telescope array (The Event Horizon Telescope Collaboration, 2019). Astronomical image processing and interferometry requires the collection of radio waves using a radio telescope and analyzing that data with software. VLBI collects signals with multiple telescopes simultaneously, and the resulting data can be reduced and analyzed as data collected by a telescope with the diameter equal to the largest distance between the telescopes, thus is capable of producing an image with higher angular resolution and capturing objects further away from earth. However, due to the distance between the VLBI telescopes, algorithms are needed to fill in the hole within the collected data and reduce atmospheric noise and delays in signals (Very Long Baseline Array (VLBA)). We conduct an in depth review of the algorithm and VLBI as a whole in this paper, and hope to use our findings to further push the development of this great technology.

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Zhang, Yu Fang. "Review of Mechanical Structure of Force Actuator for Optical Astronomical Telescope". Advanced Materials Research 765-767 (setembro de 2013): 25–28. http://dx.doi.org/10.4028/www.scientific.net/amr.765-767.25.

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Reviewed the application of force actuators in the optical astronomical telescopes, and introduced the working principle, mechanical structure, performance requirements and basic components of the force actuators; then compared the advantages and disadvantages of force actuator types which commonly used in astronomical telescopes, finally, propose a outlook of the development trend of the actuator on the great telescope application requirements.

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Woillez, J., J. A. Abad, R. Abuter, E. Aller Carpentier, J. Alonso, L. Andolfato, P. Barriga et al. "NAOMI: the adaptive optics system of the Auxiliary Telescopes of the VLTI". Astronomy & Astrophysics 629 (setembro de 2019): A41. http://dx.doi.org/10.1051/0004-6361/201935890.

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Context. The tip-tilt stabilisation system of the 1.8 m Auxiliary Telescopes of the Very Large Telescope Interferometer was never dimensioned for robust fringe tracking, except when atmospheric seeing conditions are excellent. Aims. Increasing the level of wavefront correction at the telescopes is expected to improve the coupling into the single-mode fibres of the instruments, and enable robust fringe tracking even in degraded conditions. Methods. We deployed a new adaptive optics module for interferometry (NAOMI) on the Auxiliary Telescopes. Results. We present its design, performance, and effect on the observations that are carried out with the interferometric instruments.

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Wainscoat, Richard, Ken Chambers, Eva Lilly, Robert Weryk, Serge Chastel, Larry Denneau e Marco Micheli. "The Pan-STARRS search for Near Earth Objects". Proceedings of the International Astronomical Union 10, S318 (agosto de 2015): 293–98. http://dx.doi.org/10.1017/s1743921315009187.

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AbstractThe two Pan-STARRS telescopes, located on Haleakala, Maui, Hawaii, are 1.8-meter diameter telescopes equipped with 1.4 Gigapixel cameras that deliver 7 square degree fields-of-view. The first of these telescopes, Pan-STARRS1, is conducting a search for Near Earth Objects, and is currently the leading discoverer of Near Earth Objects. The second telescope, Pan-STARRS2, is nearing the end of its commissioning, and is becoming more productive.Pan-STARRS has become the leading survey for Near Earth Objects, responsible for approximately half of the NEO discoveries to date in 2015. Pan-STARRS is also the leading discoverer of new comets.

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Tlatov, Andrey. "The Forecast of Space Weather According to Ground-Based Observatories". Proceedings of the International Astronomical Union 13, S335 (julho de 2017): 362–64. http://dx.doi.org/10.1017/s174392131700881x.

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AbstractThe space weather forecast can be conditionally divided into three components: 1) The forecast of recurrent slowly varying events which are associated with the topology of a large-scale magnetic field; 2) Evaluation of fluxes of ultraviolet and extreme radiation; 3) Detecting and determining the parameters of eruptions and CME. All three components can be observed and evaluated by ground-based telescopes. In this article we describe the telescopes of the space weather service in Kislovodsk Mountain Astronomical Station. Telescope-magnetograph STOP for the forecast of recurrent events and patrol telescopes-spectrographs for detecting CME and estimating hard radiation fluxes.

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Cox, G. C. "The COAST Interferometer". Symposium - International Astronomical Union 158 (1994): 163–66. http://dx.doi.org/10.1017/s007418090010748x.

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The Cambridge Optical Aperture Synthesis Telescope (COAST) [1] will be the first instrument of its kind to exploit the techniques of aperture synthesis and closure phase to produce very high resolution (one milliarcsecond) optical images. The instrument will consist of four identical independent mobile 40 cm telescopes, and an optical building incorporating the path compensators and the fringe and acquisition and auto-guider detector systems. The present status is; there are three operational telescopes on site with two fully functional path compensator trolleys, an acquisition and auto-guider system capable of controlling up to four telescopes, correlator and a fringe detector system.

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Döhring, Thorsten, Veronika Stieglitz, Rene Hudec, Iryna Sapsai, Peter Friedrich e Vadim Burwitz. "Characterization of a lobster-eye type X-ray telescope". EPJ Web of Conferences 266 (2022): 13010. http://dx.doi.org/10.1051/epjconf/202226613010.

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Lobster-eye type X-ray telescopes use reflecting plano mirrors under grazing incidence and can observe a large field of view. As part of a Bavarian-Czech cooperation, two telescopes were build, equipped with mirrors coated with gold and iridium. Their X-ray characterization was carried out at the PANTER test facility, which simulates parallel starlight incident on the telescopes. The telescopes have an angular resolution of about 4 arc minutes in X-rays and a focal length of about 2 meters. The used X-ray mirrors reflect and focus visible light as well; their functionality in the optical regime was checked in laboratory tests. Now another test campaign will be carried out to examine the telescope resolution for real objects of the visible night sky and the imaging properties for star constellations.

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Scuderi, Salvatore. "The ASTRI Program". EPJ Web of Conferences 209 (2019): 01001. http://dx.doi.org/10.1051/epjconf/201920901001.

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The ASTRI (Astrofisica con Specchi a Tecnologia Replicante Italiana) program was born as a collaborative international effort led by the Italian National Institute for Astrophysics (INAF) to design and realize, within the Cherenkov Telescope Array (CTA) framework, an end-to-end prototype of the Small-Sized Telescope (SST) in a dual-mirror configuration (2M). While the activities concerning the characterization of the prototype are under completion, the program entered a new phase. With the final aim of contributing at the production of the SST telescopes for the CTAO Southern site, we started the development of nine telescopes based on the evolution of the ASTRI prototype design to work as pathfinder for the CTAO. Furthermore, together with the CHEC (Compact High Energy Camera) collaboration, the ASTRI team presented a proposal, that will be evaluated with other proposals, to deliver to CTAO the complete set of SST telescopes.

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Garrison, R. F. "Use of the University of Toronto Southern Observatory as support for large-telescope and satellite programmes". Symposium - International Astronomical Union 118 (1986): 69–70. http://dx.doi.org/10.1017/s0074180900151046.

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With a 60-cm telescope at an outstanding site, it is possible to coordinate observations with larger telescopes and with satellites to provide monitoring of interesting objects. The University of Toronto Southern Observatory at Las Campanas, Chile, has been involved in several such programmes, in support of large telescopes at Tololo, La Silla, and Mauna Kea, in addition to the I.U.E., EXOSAT, and other satellites.

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Mulumba, Dorcus. "Design and development of a two-dish interferometer". Proceedings of the International Astronomical Union 15, S356 (outubro de 2019): 408. http://dx.doi.org/10.1017/s1743921320003622.

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AbstractThe angular resolution and the sensitivity of a parabolic dish telescope increase with the diameter of its aperture at a given frequency. This implies that as the telescope gets larger, its resolution becomes better. However, constructing telescopes of ever increasing size is prohibitive for both technical and financial reasons. This problem is solved by using an interferometer which consists of two or more separate telescopes that combine their signals offering a resolution equivalent to the largest separation distance between the telescopes. In this work, the electric field variations from two telescopes will be obtained. The voltage signals from the two telescopes will be coherently combined in order to derive the structure of the target source of radio emission. This combination will be done by a cross-correlator, which multiplies and averages the voltage outputs V1 and V2 of the two dishes. A major challenge to be addressed in this work is to design an instrument capable of making professional-type radio astronomy measurement in a local interference environment. In this regard, the investigative part of this work will verify whether it is possible to achieve a high sensitivity enough to detect some cosmic sources where the presence of man-made interference and cost adversely influences the system. The design of an interferometer will be presented and implemented. It may also serve as a demonstrator for engineering students to gain a working knowledge of radio interferometry.

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Han, J., C. Cui, D. Fan, Y. Xu, C. Li, S. Li e L. Mi. "AN EXTENSIBLE FRAMEWORK FOR OBSERVATORY SYSTEM BASED ON DOCKER CLOUD". Revista Mexicana de Astronomía y Astrofísica Serie de Conferencias 53 (1 de setembro de 2021): 61–66. http://dx.doi.org/10.22201/ia.14052059p.2021.53.16.

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Remote observatory is playing more and more important role in scientific research, astronomy education and citizen science. With many years' development, remote observatory whether hardware or software has made great progress. It supports single telescope well and has been very mature. For high utility rate of an observatory, more and more observatories has began to run multiple telescopes to provide more observation services. But it also takes some challenges, for example how to manage telescopes, how to manage lots of observers, how to update driver or application quickly and how to realize coordination and cooperation between different telescopes. After taking into full consideration of the problems, we propose an extensible framework for observatory system based on Docker cloud. It not only could solve that challenges from multi telescopes, but also could make software application to support more hardware platform easily.