LSST structural design

Warren B. Davison; Mario H. Rascon; Brian Cuerden; Jacques Sebag; Chuck Claver; Gary Muller; Larry Daggert

doi:10.1117/12.552233

29 September 2004 LSST structural design

Warren B. Davison, Mario H. Rascon, Brian Cuerden, Jacques Sebag, Chuck Claver, Gary Muller, Larry Daggert

Proceedings Volume 5495, Astronomical Structures and Mechanisms Technology; (2004) https://doi.org/10.1117/12.552233
Event: SPIE Astronomical Telescopes + Instrumentation, 2004, Glasgow, United Kingdom

Abstract

The Large Synoptic Survey Telescope (LSST) is an 8-meter class telescope with a proposed field of view between 3.0 and 3.5 degrees. The scientific goals of the survey establish a cadence that sets the telescope performance. The proposed cadence of the LSST telescope will typically require movements and settling of the telescope of approximately 3 degrees in 5 seconds. This dictates a high bandwidth to the telescope servo and thus a high locked rotor resonant frequency. In this study, the structure must accommodate three optical surfaces, the 8.4-meter primary, the 3-meter class secondary, and a 5-meter class tertiary in a long-tube configuration. The instrument must be accommodated in a "Trapped Focus" in the middle of the telescope. This imposes very stringent requirements on the structure and drives. This structure will require performance beyond the existing class of 8-meter telescopes. This can be achieved with the C-ring and azimuth platform concept demonstrated with the Large Binocular Telescope. The structure requires a low rotational inertia and a very high locked rotor resonant frequency at all angles of the sky. This is a challenging problem that can be overcome with this innovative solution.

Citation Download Citation

Warren B. Davison, Mario H. Rascon, Brian Cuerden, Jacques Sebag, Chuck Claver, Gary Muller, and Larry Daggert "LSST structural design", Proc. SPIE 5495, Astronomical Structures and Mechanisms Technology, (29 September 2004); https://doi.org/10.1117/12.552233

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