We present our recent process on a portable solar adaptive Optics system, which is aimed for diffraction-limited imaging
in the 1.0 ~ 5.0-μm infrared wavelength range with any solar telescope with an aperture size up to 1.6 meters. The realtime
wave-front sensing, image processing and computation are based on a commercial multi-core personal computer.
The software is developed in LabVIEW. Combining the power of multi-core imaging processing and LabVIEW parallel
programming, we show that our solar adaptive optics can achieve excellent performance that is competitive with other
systems. In addition, the LabVIEW's block diagram based programming is especially suitable for rapid development of
a prototype system, which makes a low-cost and high-performance system possible. Our adaptive optics system is
flexible; it can work with any telescope with or without central obstruction with any aperture size in the range of 0.6~1.6
meters. In addition, the whole system is compact and can be brought to a solar observatory to perform associated
scientific observations. According to our knowledge, this is the first adaptive optics that adopts the LabVIEW high-level
programming language with a multi-core commercial personal computer, and includes the unique features discussed
above.
Large-aperture segmented primary mirror has been widely used in high-resolution space telescopes. After deployment,
position error and surface error of each segmented mirror will lead inacceptable wavefront errors together. A critical
problem is how to decouple position error and surface error from exit-pupil wavefront aberrations. We proposed a
decoupling control strategy based on sensitivity matrix retrieval method. The sensitivity matrix of segmented mirror is
calculated by simulation method and a new type of orthogonal polynomials is recommended to fit wavefront aberrations
in non-circular area. First we give a simulation example to show how to decouple position errors in each degree of
freedom if there are no surface errors. Then a further simulation reveals the decoupling control process for position and
surface errors. The low order aberrations are corrected by position control actuators and high order aberrations are
corrected by figure control actuators.
Large-aperture segmented primary mirror has been widely used in
high-resolution space telescopes. In this paper, we
concentrate on the wavefront sensing and control (WFS&C) methods for a segmented primary mirror comprising a
central octagon and eight surrounding petals. As the wavefront errors have a wide dynamic range in amplitude and
spatial frequency, a multistage wavefront control algorithm is proposed. The control process is divided to five steps to
reduce the wavefront errors gradually. A simulation toolbox integrating multi-disciplinary software has been developed
to verify our WFS&C algorithms. Simulation results give a good demonstration of the feasibility of our algorithms.
KEYWORDS: Actuators, Wavefronts, Mirrors, Phase modulation, Spatial frequencies, Space telescopes, Control systems, Wavefront aberrations, James Webb Space Telescope, Telescopes
Segmented primary mirror has been widely used in high-resolution ground-based and space-based telescopes. In this
paper, we mainly discuss the wavefront control issue for a segmented primary mirror with annular-sector subaperture. In
order to balance the requirements of correction in amplitude and spatial frequency, we propose a multistage wavefront
control strategy and allocate the wavefront errors in spatial frequency domain. The power spectral density (PSD) is
calculated to obtain the spatial frequency information of wavefront aberrations. The feasibility of the control strategy is
verified by numerical simulation.
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