Active optics correction forces for the VST 2.6m primary mirror

P. Schipani; F. Perrotta; L. Marty

doi:10.1117/12.670532

6 July 2006 Active optics correction forces for the VST 2.6m primary mirror

P. Schipani, F. Perrotta, L. Marty

Proceedings Volume 6273, Optomechanical Technologies for Astronomy; 62733A (2006) https://doi.org/10.1117/12.670532
Event: SPIE Astronomical Telescopes + Instrumentation, 2006, Orlando, Florida , United States

Abstract

In active optics systems obviously a fundamental role is played be the choice of polynomials to describe the primary mirror deformations. The well known Zernike polynomials are widely used because of their immediate interpretation in terms of optical aberrations. Nevertheless in an active optics correction system context, the choice of the so called "minimum energy modes" as the polynomials to represent the mechanical deformations is best justified by their derivation from mechanical properties. This is the approach followed for the 2.6m primary mirror of the VST telescope, to be hosted on top of the Cerro Paranal ESO observatory. The calibration forces to compensate a given amount of each aberration mode are computed and discussed.

Citation Download Citation

P. Schipani, F. Perrotta, and L. Marty "Active optics correction forces for the VST 2.6m primary mirror", Proc. SPIE 6273, Optomechanical Technologies for Astronomy, 62733A (6 July 2006); https://doi.org/10.1117/12.670532

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