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Djmax respect update 1.083/9/2023 ![]() A final rms profile error of 0.6 mm was achieved due to the invention of an inexpensive technique of panel construction and measurement combined with the use of radio-astronomical holographic techniques to measure the telescope under actual operating conditions. The improvement of the short-wavelength performance of the Jodrell Bank Mk II radio telescope is described. Resurfacing the Jodrell Bank Mk II radio telescope The signal intensity varies accordingly to the presence of nearby population and topography of the region. The results, for which we used to make preliminary site selection, show signals from typical broadcast and telecommunication services and aeronautics applications. The data from a 3-minute pointing were recorded for both horizontal and vertical polarizations, in maxhold and average modes. ![]() The Radio Frequency Interference (RFI) measurements were carried out with a DC spectrum analyzer and directional antennas at 1.5 meter above ground, from 20 MHz to 6 GHz with full azimuth coverage. Possible locations have been narrowed down to three candidates, situated in the Northern part of Thailand, where the atmosphere is sufficiently dry and suitable for 22 and 43 GHz observations. National Astronomy Research Institute of Thailand (NARIT) has initiated a 5-year project, known as the Radio Astronomy Network and Geodesy for Development (RANGD), which includes the establishment of 40-meter and 13-meter radio telescopes. Performance of radio telescopes lies within the fact that astronomical sources are extremely weak. Radio astronomical observations have increasingly been threaten by the march of today telecommunication and wireless technology. ![]() Radio Frequency Interference Site Survey for Thai Radio Telescopes The book benefits scientists and radio/communication engineers, telescope designers and construction firms as well as telescope operators, observatory staff, but also the observing astronomer who is directly confronted with the t. Thermal Design and Thermal Behaviour of Radio Telescopes and their Enclosures reviews the design and construction principles of radio telescopes in view of thermal aspects and heat transfer with the variable thermal environment it explains supporting thermal model calculations and the application and efficiency of thermal protection and temperature control it presents many measurements illustrating the thermal behaviour of telescopes in the environment of their observatory sites. Among those, temperature influences may degrade the performance of a radio telescope through transient changes of the focus, pointing, path length and sensitivity, often in an unpredictable way. Radio telescopes as well as communication antennas operate under the influence of gravity, temperature and wind. Thermal Design and Thermal Behaviour of Radio Telescopes and their Enclosures The communication between the observer and the system, the format of data on magnetic tape and an on-line reduction of position measurements are considered. The final part introduces the architecture of the executive program in general, which has been tailored to meet the demands of the process and the hardware. The second part briefly describes the computer and its hardware. The first part of the paper deals with the process itself, the radio telescope and its operation, and the demands resulting for the control program. It is controlled by a Ferranti Argus 500 on-line computer. The instrument is the largest fully steerable antenna in the world. ![]() An on-line computer control process developed for the 100-m radio telescope of the Max-Planck-Institut fur Radioastronomie in Bonn is described.
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