5/23/2023 0 Comments Telescope differential flexture![]() All structural systems experience some deformation with a change in applied load and a Cassegrain mounted telescope instrument will experience a continual change in gravitational load direction while tracking a celestial object.įigure 1 shows the Shane telescope fork axis (dashed line), which the telescope and instruments rotate about as a celestial object is tracked during an exposure. The effects of flexure become especially problematic during long camera exposures. Images will not reach the diffraction-limit if there is excessive flexure/deformation during the exposure, especially if there is differential flexure between the wavefront sensor, deformable mirror, and/or science imaging device. Both of these requirements dictate tighter tolerances in stability at both pupil and image conjugates. ![]() Shorter wavelengths also produce higher angular resolution at the diffraction limit (λ/D). Achieving diffraction limited results at shorter wavelengths (J-band and H-band) requires higher-spatial frequency sampling of the wavefront and a larger number of degrees of freedom on the deformable mirror. The first generation Lick 3-meter adaptive optics system was optimized for astronomical imaging and spectroscopy in K-band (2.2 microns). Other UC Observatory papers in these proceedings address items 1, 2, and 3 (see references 1 and 2.) This paper addresses item 4, improvement to the support structure and motion stages. Stiff mechanical support structure with stiff and precise motion stages to allow for easier acquisition and longer exposures. New fiber laser for producing the reference guide star Ĥ. High resolution infrared detector: Teledyne Hawaii 2RG (2K x 2K) ģ. High order wavefront correction using Boston Micromachines 32x32 actuator MEMs deformable mirror Ģ.
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