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Artykuły w czasopismach na temat „Cassegrain telescope”

Autor: Grafiati

Data publikacji: 3 czerwca 2025

Data aktualizacji: 31 lipca 2025

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1

Liu, Xuan, Junhong Deng, King Fai Li, et al. "Optical telescope with Cassegrain metasurfaces." Nanophotonics 9, no. 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

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2

BAQUERO, N., W. A. HERNANDEZ, and R. A. RINCON. "Diseño y construcción de un telescopio Cassegrain clásico." Orinoquia 10, no. 2 (2006): 7–12. http://dx.doi.org/10.22579/20112629.209.

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Titulo en ingles: Design and construction of a telescope classic CassegrainRESUMEN: Se presenta los resultados del trabajo de investigación aplicada y desarrollo tecnológico llevado a cabo en el taller de óptica de UNILLANOS: Diseño y construcción de un telescopio Cassegrain clásico, de 150 mm de diámetro, f/D= 20; como instrumento óptico para la observación astronómica.Palabras clave: Diseño óptico, telescopio CassegrainABSTRACT: Next are shown the scientific results of the applied investigation work and technology development accomplished in the optic laboratory of UNILLANOS: Design and cons

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3

Yue, Song, Zhe Zhang, Kunpeng Zhang, et al. "Design and Numerical Analysis of an Infrared Cassegrain Telescope Based on Reflective Metasurfaces." Nanomaterials 11, no. 11 (2021): 2904. http://dx.doi.org/10.3390/nano11112904.

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Reflective imaging systems such as Cassegrain-type telescopes are widely utilized in astronomical observations. However, curved mirrors in traditional Cassegrain telescopes unavoidably make the imaging system bulky and costly. Recent developments in the field of metasurfaces provide an alternative way to construct optical systems, possessing the potential to make the whole system flat, compact and lightweight. In this work, we propose a design for a miniaturized Cassegrain telescope by replacing the curved primary and secondary mirrors with flat and ultrathin metasurfaces. The meta-atoms, cons

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4

Sobirin, Farhan Fatwa, Satia Nugraha, Fauzia Haz, and Peberlin Sitompul. "Study of Cassegrain-type antenna for radio telescope." Journal of Physics: Conference Series 2214, no. 1 (2022): 012028. http://dx.doi.org/10.1088/1742-6596/2214/1/012028.

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Abstract There are many critical parameters in the design of a radio telescope, such as antenna gain and antenna resolution. In telecommunications, radar, and radio telescopes, an antenna is a very important component. There are many designs of the antenna, such as dipole array and parabolic antenna. Parabolic antennas also have many sub-reflector and antenna methods that control the radio wave, such as the Cassegrain type. A Cassegrain-type antenna is a parabolic antenna in which the feed antenna is mounted at or behind the surface of the main parabolic reflector dish. For the transmitter sys

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5

Haider, Y. Hammod*1 Saaid F. Hassan2 Intisar A. Naseef3. "DESIGN AND ANALYSISA ZOOM CASSEGRAIN TELESCOPE COVER MIDDLE IR REGION USING ZEMAX PROGRAM." INTERNATIONAL JOURNAL OF ENGINEERING SCIENCES & RESEARCH TECHNOLOGY 6, no. 8 (2017): 178–85. https://doi.org/10.5281/zenodo.839159.

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The goal of the project is to find an optimal design of zoom -Cassegrain telescope which is popular for amateur astronomers. Also,the objective function of the optical design is to reduce the aberrations to provide aclear image. Cassegrain telescope has been designing and analysis by using (Zemax) software. The full field of view of the objective lens angle to 0.383°, the focal length to 747,748,750 and751mm, Back focal distance BFD 41 mmand Entrance pupil diameter 218.The system consists of a fixed focal length of the objective lens, zoom eyepiece. The eyepiece continuous zoom the zoom telesc

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6

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 sy

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7

Wang, Honghao, Jianli Wang, Yuyan Cao, Tao Chen, and Hongwen Li. "Optical Pupil Shift Correction Method for Large Ground-Based Optical Telescopes." Applied Sciences 13, no. 24 (2023): 13173. http://dx.doi.org/10.3390/app132413173.

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Cassegrain telescopes with larger apertures suffer significant optical pupil shifting errors caused by gravity and temperature gradients. This study constructs an optical model of a large Cassegrain telescope and a method to calculate and compensate its shifting error. First, the optical structure is simplified by incorporating only the most relevant telescope components, and the system optics is modeled using ray tracing. A computer-aided mounting-based method for calculating the misalignment error of primary and secondary mirrors is proposed, with the spatial position change of secondary mir

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8

Tan, Alfred Yong Liang. "High-resolution solar imaging for citizen science." EPJ Web of Conferences 240 (2020): 01002. http://dx.doi.org/10.1051/epjconf/202024001002.

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High-resolution solar imaging, essential for research into the Sun is usually limited to high-end expensive telescopes found in professional observatories using adaptive optics technology. However, a Schmidt-Cassegrain Telescope (SCT) or a refractor telescope equipped with a narrow-band energy rejection filter and a suitable solar spectrum filter, employing appropriate data acquisition and post-processing techniques can provide an amateur astronomer a costeffective means to high-resolution solar imaging.

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9

Xiaodong Hu, Xiaodong Hu, Weike Wang Weike Wang, Qiang Hu Qiang Hu, et al. "Design of CASSEGRAIN telescope baffles with honeycomb entrance." Chinese Optics Letters 12, no. 7 (2014): 072901–72904. http://dx.doi.org/10.3788/col201412.072901.

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10

Stavroudis, Orestes N. "Principal surface of a Cassegrain telescope." Journal of the Optical Society of America A 11, no. 4 (1994): 1253. http://dx.doi.org/10.1364/josaa.11.001253.

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11

Florentin-Nielsen, Ralph. "The Strömgren Automatic Telescope." International Astronomical Union Colloquium 136 (1993): 213–20. http://dx.doi.org/10.1017/s0252921100007582.

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AbstractCopenhagen University Observatory operates a 52cm Cassegrain telescope at ESO, La Silla (Chile) for photoelectric photometry in a completely automatic mode. Alternatively, the telescope may be operated, remotely, from Europe. We report on the operational experience from more than four years of successful use and on the decision by ESO to establish a similar system on their photometric telescope.

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12

Journal, Baghdad Science. "Calculation of Coefficients of Cassegrain Telescope Mirrors." Baghdad Science Journal 8, no. 1 (2011): 161–67. http://dx.doi.org/10.21123/bsj.8.1.161-167.

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In the present work, a program for calculating the coefficients of the Aplanatic Cassegrain Telescope (ACT) system, free from the effects of spherical and coma aberrations, were constructed. In addition, the two-mirrors of the optical system, as aspherical surfaces, were adopted. This means, that the two-equations of the mirrors are assumed to be polynomial function of five even terms only. The numerical method, least-squares curve fitting method to calculate the two-mirror coefficients system, was adopted. For choosing the values and ratios that give the best results, Rayleigh Criterion (Rayl

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13

Hickey, David. "Construction of a 32cm Cassegrain photoelectric telescope." Symposium - International Astronomical Union 118 (1986): 91–92. http://dx.doi.org/10.1017/s0074180900151137.

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14

Ahmed, Ahmed Kamil. "Calculation of Coefficients of Cassegrain Telescope Mirrors." Baghdad Science Journal 8, no. 1 (2011): 161–67. http://dx.doi.org/10.21123/bsj.2011.8.1.161-167.

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In the present work, a program for calculating the coefficients of the Aplanatic Cassegrain Telescope (ACT) system, free from the effects of spherical and coma aberrations, were constructed. In addition, the two-mirrors of the optical system, as aspherical surfaces, were adopted. This means, that the two-equations of the mirrors are assumed to be polynomial function of five even terms only. The numerical method, least-squares curve fitting method to calculate the two-mirror coefficients system, was adopted. For choosing the values and ratios that give the best results, Rayleigh Criterion (Rayl

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15

Osman, A. M. I. "The Kottamia Observatory and Other Aspects of Astronomy in Egypt." Highlights of Astronomy 10 (1995): 670–71. http://dx.doi.org/10.1017/s1539299600012521.

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The 74-inch (1.8m) telescope of Kottamia Observatory is the largest telescope in North Africa and the Middle East. It stands on a plateau 485m above sea-level and 70km to the east of Cairo. The latitude is 25° 55’.9 N and the longitude 31° 49’.5E. The telescope is of conventional type, having Newtonian (f/4.9), Cassegrain (f/18) and coudí (f/28.9) foci; it was built by Grubb-Parsons (U.K.). The main mirror is of Duran 50 glass, and has a clear aperture of 74 inches (1.8m) and a focal length, for its paraboloidal surface, of 360 inches (9.2m). The secondary mirrors are of fused quartz. The tele

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16

Turatto, M., E. Cappellaro, and F. Sabbadin. "CCD Images of Selected Planetary Nebulae." Symposium - International Astronomical Union 131 (1989): 172. http://dx.doi.org/10.1017/s0074180900137805.

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17

Jena, Carl Zeiss. "Optical Systems for the ‘Large Imaging Telescope’ (Lite)." Symposium - International Astronomical Union 161 (1994): 93–99. http://dx.doi.org/10.1017/s007418090004715x.

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With the first demands to the LITE-project being available in summer 1992, it was obvious that the known systems such as Slevogt, Schmidt or Ritchey-Chrétien-Cassegrain did not offer an attempt at a solution.

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18

Tan, C. Y., and B. Schulz. "A Fourier method for the determination of focus for telescopes with stars." Monthly Notices of the Royal Astronomical Society 511, no. 2 (2022): 2008–20. http://dx.doi.org/10.1093/mnras/stac189.

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ABSTRACT We introduce a Fourier method (Fm) for the determination of best focus for telescopes with stars. Our method fits a power function, that we will derive in this paper, to a set of images taken as a function of focuser position. The best focus position is where the power is maximum. Fm was first tested with small refractor and Schmidt–Cassegrain telescopes. After the successful small telescope tests, we then tested Fm with a 2 m Ritchey–Chrétien–Coudé. Our tests show that Fm is immune to the problems inherent in the popular half-flux diameter method.

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19

Tezuka, Hideaki, Michitsugu Mori, Koichi Hishida, and Masanobu Maeda. "1001 Super-Long Range PIV with Cassegrain Telescope." Proceedings of the Fluids engineering conference 2005 (2005): 141. http://dx.doi.org/10.1299/jsmefed.2005.141.

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20

Obraztsov, Vladimir S., and Alexander A. Ageichik. "Alignment of Cassegrain Telescope with Epps-Shulte Focus." Key Engineering Materials 437 (May 2010): 329–33. http://dx.doi.org/10.4028/www.scientific.net/kem.437.329.

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21

Hearnshaw, J. B. "Cassegrain echelle spectroscopy with small telescopes." Symposium - International Astronomical Union 118 (1986): 371–84. http://dx.doi.org/10.1017/s0074180900151769.

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This paper comments on the growing use of cassegrain échelle spectrographs for high resolving power astronomical spectroscopy over the last two decades. Some of the theoretical and practical advantages of échelle spectrographs are outlined, as well as some of the problems that arise in their use. Design parameters of some recent échelle spectrographs in various observatories are summarised. A novel use of échelle spectrographs without a cross-dispersing element for radial velocity spectrometry is proposed. The design parameters of a fibre-fed échelle spectrograph that will achieve a resolving

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22

Martin, R. N., and J. W. M. Baars. "The Submillimeter Telescope - A Status Report." International Astronomical Union Colloquium 140 (1994): 66–67. http://dx.doi.org/10.1017/s0252921100019151.

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SummaryThe Max-Planck-Institut für Radioastronomie, Bonn and the Steward Observatory of the University of Arizona, Tucson are collaborating on the construction and operation of a dedicated submillimeter facility. The Submillimeter Telescope (SMT) is a 10 m diameter reflector surrounded by a corotating enclosure. The instrument is an alt-azimuth mounted f/13.8 Cassegrain homology telescope with two Nasmyth and bent Cassegrain foci. The SMT will have diffraction limited performance at a wavelength of 300 μm. and an operating overall figure accuracy of 15 μm rms. The primary and secondary reflect

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23

Ziener, R. "The Plate Archive of the Tautenburg Schmidt Telescope." Symposium - International Astronomical Union 161 (1994): 367–68. http://dx.doi.org/10.1017/s0074180900047677.

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The Karl-Schwarzschild-Observatorium, about 15 km away from Jena in the Tautenburg forest at 330 m above sea level, was founded in 1960. The 2m-Universal-Telescope contains three optical systems: Schmidt, Cassegrain and Coudé. The spherical primary mirror consists of Sitall (a Russian ceramic glass).

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24

Dahlmark, Lennart. "Searching for Variables, and Constructing a Slit-less Spectroscope." International Astronomical Union Colloquium 98 (1988): 111. http://dx.doi.org/10.1017/s0252921100092381.

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Methods of searching for variables using a short-focal-length (30 cm) and stereo and blink comparators were described, together with the design of a simple slit-less spectrograph suitable for a Newtonian or Cassegrain telescope.

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25

Shi-Yang, Jiang. "Several Possible Designs for BFOSC." International Astronomical Union Colloquium 149 (1995): 29–32. http://dx.doi.org/10.1017/s0252921100022636.

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AbstractVarious optical solutions are presented for the Beijing Faint Object Spectrograph and Camera of Beijing Astrophysical Observatory 2.16 m telescope. They are based either on dioptric or catoptric designs including an adaptation of the existing Cassegrain spectrograph.

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26

Reinacher, Andreas, Friederike Graf, Benjamin Greiner, et al. "The SOFIA Telescope in Full Operation." Journal of Astronomical Instrumentation 07, no. 04 (2018): 1840007. http://dx.doi.org/10.1142/s225117171840007x.

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The SOFIA telescope is a 2.5[Formula: see text]m class Cassegrain telescope with Nasmyth focus. It is the largest telescope ever integrated into an aircraft. The telescope is exposed to the stratospheric environment during the observations and the fact that the telescope’s foundation, which is a Boeing 747 SP, is vibrating and moving in all degrees of freedom (DoF) requires a highly specialized and sophisticated design. Based on the telescope of its predecessor, the Kuiper Airborne Observatory (KAO), the SOFIA telescope design had to evolve to accommodate a telescope 2.5 times the size of KAO.

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27

Lai, Wan, Zhu Neng-hong, Wang Lan-juan, Yang Zheng-hua, and Zheng Yi-jin. "The main features of the 1.56-m telescope and its status quo." Symposium - International Astronomical Union 118 (1986): 121–22. http://dx.doi.org/10.1017/s0074180900151265.

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This telescope was designed for determining the trigonometric parallaxes of faint stars. The otpical configuration is a Ritchey-Chrétien system and has only a f/10 Cassegrain focus for photographic work.The mounting is a combination of fork and yoke frame which can reduce the flexure due to gravity. A high speed digital servo-system was adopted for controlling and driving the telescope. At present some photographs of Comet Halley have been obtained.

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28

Nankivell, G. R., and N. J. Rumsey. "The optical system of the Mt John one metre telescope." Symposium - International Astronomical Union 118 (1986): 101–2. http://dx.doi.org/10.1017/s0074180900151174.

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The telescope will be used at the Cassegrain focal plane only. Two interchangeable systems of secondary optics are required to give relative apertures of: (a)f/13.5 for spectroscopy and photometry over a small field.(b)f/8 for photography over as wide a field as practicable.

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29

Hsiao, C. N., H. P. Chen, P. K. Chiu, Y. W. Lin, F. Z. Chen, and J. L. Andrew Yeh. "On the thin film optics of a Cassegrain telescope." Thin Solid Films 570 (November 2014): 471–74. http://dx.doi.org/10.1016/j.tsf.2014.04.029.

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30

Xiao, Liuping, Huajun Yang, Xiaojing Liu, Quan Xu, and Xinqiang Xiong. "New type optical Cassegrain antenna with lenses telescope system." Optik 121, no. 6 (2010): 521–25. http://dx.doi.org/10.1016/j.ijleo.2008.09.002.

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31

Soonthornthum, Boonraksar. "What Can be Done with Small Telescopes?" Transactions of the International Astronomical Union 24, no. 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. Si

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32

Roth, M., A. Herrero, R. H. Mendez, R. P. Kudritzki, K. Butler, and H. G. Groth. "The Metal-Line Spectra of Central Stars of Planetary Nebulae." Symposium - International Astronomical Union 131 (1989): 317. http://dx.doi.org/10.1017/s0074180900138653.

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We present spectral descriptions based on high-resolution spectrograms of central stars of planetary nebulae, obtained with the ESO 3,6-m telescope + CASPEC (Cassegrain Echelle Spectrograph). We make preliminary determinations of stellar photospheric metal abundances, using non-LTE model atmospheres and non-LTE line formation calculations.

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Hysom, E. J. "The Instruments of H.E. Dall." International Astronomical Union Colloquium 98 (1988): 46–47. http://dx.doi.org/10.1017/s0252921100092150.

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In 1926 Horace Dall commenced optical work, with interests covering both microscopes and telescopes. Soon (1928), he was making solid eyepieces of the Tolles type. Eventually he developed skills in making lenses of the smallest size to be incorporated into microscope objectives of the highest numerical aperture; this culminated in an objective with a N.A. of 1.92 (a record). The lenses were jewelled elements worked with diamond dust. During World War 2 he repaired all the microscope lenses damaged in the U.K. that had originated with the German firm of Leitz.Horace Dall had an exceptionally in

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34

Cohen, R. S., P. Thaddeus, and L. Bronfman. "CO survey of the Southern Milky Way." Symposium - International Astronomical Union 106 (1985): 199–202. http://dx.doi.org/10.1017/s0074180900242423.

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When the Columbia Southern Millimeter-Wave Telescope on Cerro Tololo, Chile, began operation in January 1983, one of the main goals was to make the first extensive out-of-plane survey of 2.6-mm CO emission in the Southern Milky Way. Because this telescope, a 1.2-meter Cassegrain, is a close copy of the Columbia telescope in New York – with nearly identical antenna, feed, and calibration – it will be very easy to join our northern and southern surveys to make the first homogeneous radio survey of the entire Galaxy. The Chile telescope does have one important improvement over the New York system

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35

Andrillat, Yvette, and Léo Houziaux. "Infrared Spectra of Recent Novae." International Astronomical Union Colloquium 122 (1990): 210–12. http://dx.doi.org/10.1017/s0252921100068652.

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We present CCD spectra of novae PW Vul, QS And, Herculis 87 and V1819 Cyg obtained in the wavelength range 680 to 1080 nm at the Cassegrain focus of the 193–cm telescope at the Observatoire de Haute–Provence (CNRS, France). The reciprocal dispersion is 23 nm/mm.

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Hasan, Alaa B. "A Computer Simulation of Hubble Telescope Including Eyepiece Nano- Sensors to Increase Optical Efficiency." Pakistan Journal of Medical and Health Sciences 16, no. 12 (2022): 755–58. http://dx.doi.org/10.53350/pjmhs20221612755.

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The Hubble telescope is characterized by the accuracy of the image formed in it, as a result of the fact that the surrounding environment is free of optical pollutants. Such as atmospheric gases and dust, in addition to light pollution emanating from industrial and natural light sources on the earth's surface. The Hubble telescope has a relatively large objective lens that provides appropriate light to enter the telescope to get a good image. Because of the nature of astronomical observation, which requires sufficient light intensity emanating from celestial objects (galaxies, stars, planets,

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Nakajima, Junichi, Eiichiro Otobe, Kazuhiko Nishibori, Naoki Watanabe, Kuniyuki Asuma, and Tsuneaki Daishido. "First Fringe with the Waseda FFT Radio Telescope." Publications of the Astronomical Society of Japan 44, no. 3 (1992): L35—L38. https://doi.org/10.1093/pasj/44.3.l35.

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Abstract A sixty-four-element FFT (Fast Fourier Transform) type radio interferometer has been constructed at Waseda University. Using 2 elements, we have started fringe observations of radio sources. During observations of 1991 November 10–20, we detected the fringes of Cas A and Tau A. The performance of the radio telescope, which includes backend digital processors, have been confirmed by switching observations. Each element is a 2.4-m diameter cassegrain antenna with a receiver of 200 K noise temperature. The purpose of the telescope is to survey transient radio sources.

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38

Yadoumaru, Y., A. Tajitsu, and S. Tamura. "High velocity collimated flow in a Halo Planetary Nebula, H 4-1." Symposium - International Astronomical Union 180 (1997): 288. http://dx.doi.org/10.1017/s0074180900131055.

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H 4-1, PNG 049.3+88.1 (α = 12h59m27.6s, δ = +27° 38′14″, 2000), was one of well known halo Planetary Nebulae (PNe). During our program to study the expanding characteristics of PNe, the long-slit spectroscopic observations were made by the cassegrain spectrograph of the 74 inch telescope at the Okayama Astrophysical Observatory in March 1995.

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Bin, Li, Chen Jiayi, Wang Haichao, and Huo Tengfei. "Accuracy angular measurement method in alignment process for Cassegrain telescope." Journal of Applied Optics 38, no. 6 (2017): 584–89. http://dx.doi.org/10.5768/jao201738.0603003.

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40

GUAN, Wen-lu, Feng-fu TAN, Xu JING, Zai-hong HOU, and Yi WU. "Automatic focusing of Cassegrain telescope based on environmental temperature feedback." Optics and Precision Engineering 29, no. 8 (2021): 1832–38. http://dx.doi.org/10.37188/ope.20212908.1832.

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41

Senthil Kumar, M., C. S. Narayanamurthy, and A. S. Kiran Kumar. "Design and analysis of optimum baffle for a Cassegrain telescope." Journal of Optics 45, no. 2 (2015): 180–85. http://dx.doi.org/10.1007/s12596-015-0296-z.

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García, E., J. A. López Fernández, L. De Haro, et al. "Analysis of the defocused Gaussian beam telescope on Cassegrain feeds." Microwave and Optical Technology Letters 32, no. 6 (2002): 420–23. http://dx.doi.org/10.1002/mop.10196.

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Sekiguchi, Kazuhiro, Phil Charles, Liza van Zyl, and Guy F. Woodhouse. "High-Speed Imaging and Spectro-Polarimetry with Subaru Telescope." International Astronomical Union Colloquium 190 (2004): 182–83. http://dx.doi.org/10.1017/s0252921100002074.

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AbstractWe are developing a high-speed option for the Faint Object Camera and Spectrograph (FOCAS) at the Cassegrain focus of the Subaru 8.2 meter telescope at Mauna Kea, Hawaii. FOCAS has been used for direct imaging, low-dispersion multi-object spectroscopy, imaging polarimetry and spectro-polarimetry of faint objects. The high-speed option utilizes an EEV CCD47-20 with the frame transfer operation to achieve up to ~ 0.1 sec time resolution. This paper presents a summary of the expected capability and the implementation schedule.

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Lortet, M. C., M. Heydari-Malayeri, and G. Testor. "CCD Observations of Young Stellar Associations and Multiple Systems in the Magellanic Clouds." Symposium - International Astronomical Union 116 (1986): 401–2. http://dx.doi.org/10.1017/s0074180900149277.

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The nebular and stellar observations were carried out by G. T. at the Cassegrain focus of the Danish 1.50m telescope at the ESO La Silla Observatory in August and September 1984, using a RCA CCD (512 × 320 pixels) with a pixel size of 0.47”. The frames were reduced using the VAX/MIDAS software at ESO Garching and Meudon Observatory (INVENTORY automatic program).

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Anderson, B., and R. D. Davies. "Results with the Extended MERLIN." Symposium - International Astronomical Union 158 (1994): 343–45. http://dx.doi.org/10.1017/s0074180900107867.

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A major enhancement of MERLIN completed in 1992 has led to a transformation of its capabilities. The seventh telescope added to the array is a 32-m telescope at Cambridge which provides high sensitivity on all the longest baselines where extra collecting area is especially beneficial. The 32-m telescope is a shaped primary-Cassegrain configuration which achieves an 80 percent aperture efficiency. A change from frequency to amplitude modulation in the microwave links increased the effective bandwidth from 9 to 30 MHz. This broadbanding enables the two hands of circular polarization to be transm

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Walker, A. B. C., J. Lindblom, R. B. Hoover, and T. W. Barbee. "Monochromatic X-ray and XUV Imaging with Multilayer Optics." International Astronomical Union Colloquium 102 (1988): 175–80. http://dx.doi.org/10.1017/s025292110010764x.

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AbstractThe development of techniques for the fabrication of multilayer coated mirrors which can function as energy selective X-ray and XUV mirrors at normal incidence has greatly expanded the options available to the astronomical spectroscopist. We have developed a rocket spectroheliograph which utilizes multilayer optics in three configurations: i) As Cassegrain telescopes for imaging at 256 Å (He II) and 173 Å (Fe IX, X); ii) As tertiary mirrors used with a conventional Wolter I telescope for imaging at 44 Å (Si XI, XII), 173 Å, and 256 Å; iii) As off-axis spherical mirrors for imaging at 4

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Pertenais, Martin, Coralie Neiner, Laurent Parès, Pascal Petit, Frans Snik, and Gerard van Harten. "Preliminary design of the full-Stokes UV and visible spectropolarimeter for UVMag/Arago." Proceedings of the International Astronomical Union 10, S305 (2014): 168–74. http://dx.doi.org/10.1017/s1743921315004718.

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AbstractThe UVMag consortium proposed the space mission project Arago to ESA at its M4 call. Arago is dedicated to the study of the dynamic 3D environment of stars and planets. This space mission will be equipped with a high-resolution spectropolarimeter working from 119 to 888 nm. A preliminary optical design of the whole instrument has been prepared and is presented here. The design consists of the telescope, the instrument itself, and the focusing optics. Considering not only the scientific requirements, but also the cost and size constraints to fit an M-size mission, the telescope has a 1.

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Beradze, Sopia, and Nino Kochiashvili. "Observations of Bright Massive Stars Using Small Size Telescopes." Proceedings of the International Astronomical Union 12, S329 (2016): 385. http://dx.doi.org/10.1017/s1743921317002526.

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AbstractThe size of a telescope determines goals and objects of observations. During the latest decades it becomes more and more difficult to get photometric data of bright stars because most of telescopes of small sizes do not operate already. But there are rather interesting questions connected to the properties and evolution ties between different types of massive stars. Multi-wavelength photometric data are needed for solution of some of them. We are presenting our observational plans of bright Massive X-ray binaries, WR and LBV stars using a small size telescope. All these stars, which ar

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Wang, C. J., L. X. Chen, Y. F. Fan, and D. Q. Wang. "THE CONCEPT DESIGN OF OBSERVATION CONTROL SYSTEM FOR LIJIANG 2.4-METER TELESCOPE." Revista Mexicana de Astronomía y Astrofísica Serie de Conferencias 51 (April 13, 2019): 24–29. http://dx.doi.org/10.22201/ia.14052059p.2019.51.05.

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The Lijiang 2.4-m telescope was built and opened to astronomers since 2008, now there are several instruments installed at the telescope. The control system of the 2.4-m telescope was designed to be operated in robotic mode as the Liverpool telescope, but due to many reasons it didn’t achieve robotic mode until now. After we upgraded the fold mirror by adding a rapid instrument exchanging system at the Cassegrain focus in 2012, now we can have up to 9 instruments on the telescope at the same time, but the control system for the instrument is still specific for each instrument. During the obser

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Hu, Ningsheng. "Design for a Large Transit Circle with Reflecting Optics." Symposium - International Astronomical Union 109 (1986): 421–26. http://dx.doi.org/10.1017/s0074180900076853.

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This paper describes a conceptual design for an automatic transit circle with Ritchey-Chretien Cassegrain type optics of 40 cm aperture. The instrument takes reversal observation both in the meridian and in the prime vertical. Methods of adopting active optics to achieve a stable boresight of the reflecting telescope and of automatically reversing and leveling the instrument are presented. The instrument can also be used in a theodolite mode.

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