In this paper, wide-field adaptive optics systems for ground-based solar telescopes are discussed. The features of constructing adaptive optics systems based on layer- and object-oriented approaches are considered. It is shown that the optimal adaptive optics system for the Large Solar Vacuum Telescope (LSVT) should be created on the basis of optical conjugation of deformable mirrors with turbulent layers of the atmosphere, the system for determining wavefront aberrations should be based on the use of a set of a narrow field of view sensors conjugated with telescope aperture, as well as a multi-directional wavefront sensor for turbulence tomography, designed on the basis of an object-oriented approach (measurements of wavefront aberrations in different directions). The schemes of pupil imagers that provide optical conjugation of the LSVT wavefront sensor with heights of 3 km as well as the upper atmospheric levels are considered. Direct optical conjugation of the Shack-Hartmann sensor with a turbulent layer is limited by a height of about 3 km (due to significant vignetting).
A multi-cascade adaptive optical system for imaging and image stabilization for the Large Solar Vacuum Telescope is described. This system was created in 2017 by specialists of the V.E. Zuev Institute of Atmospheric Optics SB RAS, Tomsk, with the technical support of the Institute of Solar-Terrestrial Physics SB RAS, Irkutsk. The system has been tested at the Large Solar Vacuum Telescope (Baikal Astrophysical Observatory) and demonstrated its efficiency. Along with the first cascade of adaptive image stabilization by a tip-tilt corrected mirror, this system employs the second imaging cascade based on correction with a flexible mirror controlled by a specialized wavefront sensor, as well as the third cascade for real-time post-detector processing of video camera frames. Reliable experimental data confirming the efficiency of the multi-cascade adaptive system for image formation and stabilization have been obtained. Three highrate digital video cameras recording simultaneously digital images with rates from 300 to 980 frames per second were used to test the system. The mirror correcting wavefront tilts and operating in a closed optical feedback loop was controlled by the specially developed software including the fast correlation tracking algorithm. The post-detector digital imaging was performed with a special software for processing of video camera frames in real time with the use of modern high-speed parallel algorithms based on the Intel MKL and IPP libraries.
The article proposes a design of sensor of optical distortions in a wide field of view for the adaptive optical system of the Large Solar Vacuum Telescope. The calculation of the optical scheme of the sensor based on the use of two wavefront sensors was performed. The working field of view of the adaptive system with an additional sensor for determining the distortions of the wavefront is 120 arc sec. Adjusting the field of view of each Shack-Hartmann sensor up to 30 arc sec is provided by field diaphragms. It is shown that for the used second imager, the quality of subimages remains high, the standard deviation is λ /80.
This paper describes the features of the two-mirror adaptive system for correcting atmospheric disturbances of the Large Solar Vacuum Telescope, developed with allowance for the correction of instrumental vibrations of telescopes in a wide amplitude-frequency range with an open siderostat supply mirror. Correction of the general slopes of the light wave front and its deformations is carried out separately. The adaptive optical system is designed to work with extended light sources (the Sun), which have a low contrast of image details.
Developed according to quasi-Ritchey–Chretien, the AZT-33VM telescope is designed for up to 2.8-deg wide-field survey observations; it has inner position of the focal plane and the prefocal lens corrector installed at 0.12 of the equivalent focal length from the image plane. Classic methods to calculate direct stray light protection system in two-mirror systems allow us to find the optimal configuration of the baffles providing minimum obscuration of the entrance pupil. The design of stray light protection baffles for a future large rectangular detector 260 × 124 mm was proposed. The baffles were calculated from axisymmetric condition in a plane passing through the system centerline and a point of the detector perimeter. Using the ray-tracing method, we simulated optimized baffles for a rectangular detector. We assessed obscuration of the entrance pupil with an optimal design baffle as well their advantages for the modulation transfer function.
The ground-based 0.36m mirror coronagraph with super-polished off-axis parabolic primary mirror for solar
applications has developed and build now. Optical system design, technology of scattering level measurement of
primary mirror surface and the method of adjustment are described. Also presents the constructions of heat-stop, Lyot-stop
assemblies and truss. The kit of spectral equipment and detectors for actual solar astrophysics tasks is discussed.
Two-mirrors aplanatic optical design for amateur telescopes up to 0.5m class is described. The optical system is low cost,
easy for adjusting, fast and large field of view can be used for visual and astrophotography. The method for calculation
of baffles for straight light protection is described. The optical performances and sample shots for the builted device are
presented.
Keywords: two-mirrors system, all-reflecting schmidt system, aplanatic system, protection from straight light, baffles,
obscuration, wide-field, telescopes for amateurs.
The devices and components of adaptive optical system ANGARA, which is developed for image correction in the Big
solar vacuum telescope (BSVT) at Baykal astrophysical observatory are described. It is shown that the use of
modernized adaptive system on BSVT not only reduces the turbulent atmospheric distortions of image, but also gives a
possibility to improve the telescope developing new methods of solar observations. A high precision Shack-Hartmann
wavefront (WF) sensor has been developed on the basis of a low-aperture off-axis diffraction lens array. The device is
capable of measuring WF slopes at array sub-apertures of size 640X640 μm with an error not exceeding 4.80 arc.sec.
Also the modification of this sensor for adaptive system of solar telescope using extended scenes as tracking objects,
such as sunspot, pores, solar granulation and limb, is presented. The software package developed for the proposed WF
sensors includes three algorithms of local WF slopes estimation (modified centroids, normalized cross-correlation and
fast Fourier-demodulation), as well as three methods of WF reconstruction (modal Zernike polynomials expansion,
deformable mirror response functions expansion and phase unwrapping), that can be selected during operation with
accordance to the application.
The design sophistication of optical instruments with low level instrumental (including diffraction) scattered illumination is very interesting not only for solar asrophysics. The construction of a laboratory installation for measuring intensity of a diffractio-swcattered illumination in a shadow of darkening system of a coronagraph with an exterior eclipse surveyed is described. The method of measuring, permitting to minimize influecing of a light, scattered from interior surfaces of installation is offered. Measuring of intensity of a diffraction-scattered illumination in a shadow of the single disk with different lateral views of edge is conducted. From the obtained experimental data follows that the change of the shape of scattering edge of exterior darkening system can essentially reduce intensity of a diffraction-scattered illumination in the field of an entrance pupil of an external occulted coronagraph.
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