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• W85276688 abstract "This paper presents a telescope design that should meet the stringent specifications for the Millimeter Array antennas. The most critical specifications are 25 μm surface accuracy, 0.8 arcsec pointing precision, and the ability to switch between two source separated by 1.5° in less than 1.5 s. The major design concepts employed to attain the required performance for a 10-m diameter antenna are a spaceframe backup structure supported at a radius of 3.3 m, a wide base mount with a wheel and track azimuth bearing, low thermal expansion materials, and an independent pointing reference structure. I. INTRODUCTION The National Radio Astronomy Observatory (NRAO) is in the process of designing and developing the components for a Millimeter Array (MMA) which will consist of upward of 50 antennas located on a 5,000 m altitude site in the Atacama desert in Chile. The science goals range from detection of the weakest sources at frequencies as high as 950 GHz to imaging wide fields with good fidelity and high dynamic range at 300 GHz. These goals demand that the antennas perform significantly better than the current generation of millimeter and sub-millimeter telescopes. The baseline design is for 10-m diameter telescopes with conventional Cassegrain optics, but with very exacting performance specifications. The most demanding specifications are the wave front error, pointing accuracy and fast position switching capability. The wave front error should correspond to an effective surface error of less than 25 μm RMS. The telescope must point with an accuracy of better than 0.8 arcsec RMS. It must also be able to slew to a new position 1.5° away and settle to within 3 arcsec in less than 1.5 s. These specifications must be met under most day and night conditions at the high altitude site in Chile. The high surface accuracy is driven by the need to image wide fields at 1-mm wavelength as well as the need for high aperture efficiency at 0.3-mm wavelength. These same goals also drive the 0.8 arcsec pointing requirement. The fast position switching will allow for a very fast cycle time between observations of the target source and a nearby phase calibrator, allowing removal of a large part of the phase errors caused by fluctuations in the atmosphere. This paper describes an antenna design concept to meet the stringent MMA specifications at an affordable cost. The design uses features that have been proven to work in existing telescopes and draws upon ideas proposed by other millimeter antenna designers. The innovative concepts presented by Dietmar Plathner have been particularly important in inspiring us in the direction this design has taken (1). The proposed telescope design is shown in Figure 1. The primary and secondary reflectors and elevation tipping structure are described in the next section. Section III describes the mount including the rotating azimuth structure with a wheel and track azimuth bearing. The independent pointing reference system is described in section IV. A possible transporter configuration in presented in Section V." @default.
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• W85276688 title "A Design for a Precision 10-m Sub-Millimeter Antenna" @default.
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