The next generation of large telescones currently in the planning stage will be exposed to higher wind loading due to the cost cutting reduction of dome size in relation to aperture. Thin actively figured mirrors and tighter pointing requirements increase their sus-ceptibility to the general wind loading including higher frguency componants. The figure control and pointing servo loops will require wider bandwidth and higher gain to maintain gool optical performance. To design these servo loops requires knowledge of the wind power spectra to assess loop stability and correction performance. Wind data was collected from several different observing sites. The measurements were made with a Pitot tube anemometer mounted on a tower at the leading edge of a site and four differential pressure sensors mounted across the mirror plane. Anemometer measurements were made at two different elevations to provide site wind vs. elevation extrapolation data. Hundred second measurements, with the data sampled at 50 Hz, were made. Fourier Transforms of the data cover a frequency range of 0.02 to 25 Hz.
"Wind Loading Of Large Astronomical Telescopes", Proc. SPIE 0332, Advanced Technology Optical Telescopes I, (4 November 1982); doi: 10.1117/12.933521; https://doi.org/10.1117/12.933521