Measurement, modeling, and adjustment of the 10.4-m-diameter Leighton telescopes

David P. Woody; Eugene Serabyn; Antony Schinckel

doi:10.1117/12.317381

31 July 1998 Measurement, modeling, and adjustment of the 10.4-m-diameter Leighton telescopes

David P. Woody, Eugene Serabyn, Antony Schinckel

Proceedings Volume 3357, Advanced Technology MMW, Radio, and Terahertz Telescopes; (1998) https://doi.org/10.1117/12.317381
Event: Astronomical Telescopes and Instrumentation, 1998, Kona, HI, United States

Abstract

The design of the Leighton telescopes and the unique techniques used in their fabrication make these telescopes particularly amenable to precise modeling and measurement of their performance. The surface is essentially a continuous membrane supported at 99 uniformly distributed nodes by a pin joint triangular grid space frame. This structure can be accurately modeled and the surface can be adjusted using low- resolution maps. Holographic measurements of the surface figure of these telescopes at the Caltech Submillimeter Observatory (CSO) and the Owens Valley Radio Observatory (OVRO) have been made over several epochs with a repeatability of 5 - 10 micrometer over the zenith angle range from 15 to 75 degrees. The measurements are consistent with the calculated gravitational distortions. Several different surface setting strategies are evaluated and the 'second order deviation from homology,' H_d, is introduced as a measure of the gravitational degradation that can be expected for an optimally adjusted surface. H_d is defined as half of the RMS difference between the deviations from homology for the telescope pointed at the extremes of its intended sky coverage range. This parameter can be used to compare the expected performance of many different types of telescopes, including off-axis reflectors and slant-axis or polar mounts as well as standard alt-az designs. Subtle asymmetries in a telescope's structure are shown to dramatically affect its performance. The RMS surface error of the Leighton telescope is improved by more than a factor of two when optimized over the positive zenith angle quadrant compared to optimization over the negative quadrant. A global surface optimization algorithm is developed to take advantage of the long term stability and understanding of the Leighton telescopes. It significantly improves the operational performance of the telescope over that obtained using a simple 'rigging angle' adjustment. The surface errors for the CSO are now less than 22 micrometer RMS over most of the zenith angle range and the aperture efficiency at 810 GHz exceeds 33%. This illustrates the usefulness of the global surface optimization procedure.

Citation Download Citation

David P. Woody, Eugene Serabyn, and Antony Schinckel "Measurement, modeling, and adjustment of the 10.4-m-diameter Leighton telescopes", Proc. SPIE 3357, Advanced Technology MMW, Radio, and Terahertz Telescopes, (31 July 1998); https://doi.org/10.1117/12.317381

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