Andreas GlindemannJ. AlgomedoRodrigo AmesticaP. BallesterB. BauvirErich BuguenoS. CorreiaFrancisco DelgadoF. DelplanckeF. DériePh. DuhouxE. Di FolcoA. GennaiBruno GilliP. GiordanoP. GittonStéphane GuisardNico HousenAlexis HuxleyP. KervellaM. KiekebuschBetrand KoehlerSamuel LévêqueAntonio LonginottiSerge MénardiS. MorelFrancesco ParesceT. Phan DucA. RichichiM. SchöllerM. TarenghiAnders WallanderM. WittkowskiRainer Wilhelm
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Very Large Telescope
The Very Large Telescope (VLT) Observatory on Cerro Paranal (2635 m) in Northern Chile is approaching completion. After the four 8-m Unit Telescopes (UT) individually saw first light in the last years, two of them were combined for the first time on October 30, 2001 to form a stellar interferometer, the VLT Interferometer. The remaining two UTs will be integrated into the interferometric array later this year, so that any two UTs can be used for interferometry. In this article, we will describe the subsystems of the VLTI and the planning for the following years.
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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 mechanical design and optimization.
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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.
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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.
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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.
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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.
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Two interferometric instruments at ESO's Very Large Telescope Interferometer (VLTI), MIDI and AMBER which operate in the mid‐infrared (8–13 μm) and the near‐infrared (JHK) respectively, have proven to be powerful tools to probe the circumstellar environment of evolved stars. Their spectro‐interferometric capability enables us to observe objects with spectral and spatial information disentangled. VLTI observations confirm our pictures on the circumstellar environment of cool evolved stars in some cases but bring about entirely unexpected pictures for other cases. Here, we present particularly our recent results obtained with VLTI/MIDI.
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Infrared telescope
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