Abstract
The SAO Submillimeter Wavelength Array is under construction and is expected to be ready for observations in 1997. It will consist of six telescopes with baselines from 9 to 470 m and resolutions as fine as 0'.'. Eight receivers will cover all bands from 180 to 900 GHz in linear polarization; two orthogonal polarizations will be available at 350 GHz. Multiyear site testing on Mauna Kea shows that the precipitable water vapor is less than 1 nun for 17% of the time, and the rms phase fluctuations on a baseline of 100 m are less than 55µm for 25% of the time. The configuration of the array will be optimized to provide nearly uniform coverage in the uy plane. The correlator spectrometer will have 105 spectral channels (8192 per baseline) and will be able to provide 0.6 MHz resolution for a total bandwidth of 4 GHz.
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Moran, J.M. (1994). The SAO Submillimeter Wavelength Array. In: Robertson, J.G., Tango, W.J. (eds) Very High Angular Resolution Imaging. International Astronomical Union / Union Astronomique Internationale, vol 158. Springer, Dordrecht. https://doi.org/10.1007/978-94-011-0880-5_4
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DOI: https://doi.org/10.1007/978-94-011-0880-5_4
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