World space observatory-ultraviolet
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Abstract:
The World Space Observatory UltraViolet (WSO-UV) project is an international space observatory designed for observations in the ultraviolet domain. The observatory includes a single 170 cm aperture telescope capable of high-resolution spectroscopy, long slit low-resolution spectroscopy and deep UV and optical imaging.Keywords:
Ultraviolet
Space observatory
Aperture (computer memory)
Spitzer Space Telescope
The VLT Survey Telescope (VST) is a cooperative program between the European Southern Observatory (ESO) and the INAF Capodimonte Astronomical Observatory (OAC), Naples, for the study, design, and realization of a 2.6-m wide-field optical imaging telescope to be operated at the Paranal Observatory, Chile. The VST has been specifically designed to carry out stand-alone observations in the UV to I spectral range and to supply target databases for the ESO Very Large Telescope (VLT). The telescope design, manufacturing and integration are responsibility of TWG and have been carried out on the base of a model of optimized design not only for mechanics but for all telescope subsystems. The paper is an overview on the telescope mechanical design and optimization.
Very Large Telescope
Mechanical design
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Preliminary results are presented arising from the use of the 40 inch telescope at Siding Spring Observatory for visual supernova hunting over a period of about 18 months. The use of the telescope in this way is continuing. These results are compared with the performance of my 41 cm backyard telescope over the same 18-month period, and with recently announced results from the Perth Observatory's Automated Supernova Search using their 61 cm telescope over a three-year period.
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Abstract Preliminary results are presented arising from the use of the 40 inch telescope at Siding Spring Observatory for visual supernova hunting over a period of about 18 months. The use of the telescope in this way is continuing. These results are compared with the performance of my 41 em backyard telescope over the same 18-month period, and with recently announced results from the Perth Observatory's Automated Supernova Search using their 61 em telescope over a three-year period.
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The VLT Survey Telescope (VST) is a cooperative program between the European Southern Observatory (ESO) and the INAF Capodimonte Astronomical Observatory (OAC), Naples, for the study, design, and realization of a 2.6-m wide-field optical imaging telescope to be operated at the Paranal Observatory, Chile. The VST has been specifically designed to carry out stand-alone observations in the UV to I spectral range and to supply target databases for the ESO Very Large Telescope (VLT). The telescope design, manufacturing and integration are responsibility of TWG and have been carried out on the base of a model of optimized design not only for mechanics but for all telescope subsystems. The paper is an overview on the telescope drive system characteristics.
Very Large Telescope
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Field of view
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The accuracy of optical telescope in the past was dominated by the construction of the telescope body and the precision of optical surface. This thesis fits into a larger project with a goal of controlling a flexible telescope in order to help a cheaper telescope achieve higher accuracy. In order to understand the internal motion of telescope, the goal of this thesis is to build a state space model of a two-degree-of-freedom telescope using a known star location as feedback. The model presented in this thesis may be used for the telescope simulation and the control design in the future. This project considers a light weight flexible structured telescope and uses state space formulation to model dynamic motion of the telescope since state space model is better for modeling and analyzing a multiple-inputs and multiple-outputs system. A one-degree-freedom experimental test stand is built to generate a series of telescope motion data in order to examine whether the telescope simulation model can represent a real telescope system. To record the telescope motion, a wheel encoder mounted on the azimuth motor and a LED light density sensor installed at the end of telescope body are used as feedbacks. The results show that the state space model can simulate many system dynamic behaviors as shown in the experimental result; however, it is not feasible to obtain all of telescope’s physical parameters from the system feedbacks.
Spitzer Space Telescope
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The National Observatory of Athens (N.O.A.) will install a new, advanced technology 2.3-m telescope in Greece. A favoured location for the installation of the new telescope is the top of Mount Chelmos. We present preliminary results concerning the conditions at this site. It is found that the site has a quite dark sky, a good percentage of clear nights (about 60%) and very good seeing conditions.
Mount
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The Soviet Academy of Sciences' Astrophysical Observatory in the Northern Caucasus includes the new 6 m optical telescope as well as the 600 m radio telescope Ratan (see Physics Bulletin December 1976 p535). Little information has been available in the West about the 6 m telescope but last October Professor Sir Bernard Lovell, Director of Jodrell Bank telescope, visited the observatory and found out about its design and operation from the director, Dr Kopylov, the chief designer, Dr Ioannisiani and other members of the observatory staff.
Optical telescope
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We describe the New Mexico State University (NMSU) 1 m telescope located at the Apache Point Observatory (APO), and in particular, its robotic mode of operation. Some of the issues we have encountered may be of interest to others developing similar facilities. This telescope provides a good example of the possibilities of locating a moderate‐sized university robotic research telescope at a major observatory. We find that this mode of operation provides a significant amount of productive science data on a relatively small budget.
Mode (computer interface)
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We saw in the chapter on atmospheric turbulence that the real limitation to the resolution of a ground-based telescope is not the diameter of the telescope aperture, but the atmosphere. As a result, a telescope of any diameter will rarely give an angular resolution in visible light better than 1 arcsec, which is equivalent to the diffraction limit of an aperture of about 10 cm diameter (the Fried parameter, r0, defined in section 5.4.1). This limitation has been considered so fundamental that large telescope mirrors might not even have been polished to an accuracy which could give a better resolution than this. The ideas behind the various methods of astronomical interferometry are all directed at exceeding it.
Aperture (computer memory)
Aperture synthesis
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