We investigate a new metric power spectral density (PSD),for characterizing the performance of seeing-limited large telescope such as thirty meter telescope(TMT ). As the PSD is directly related to the performance of the atmosphere which plays an important role in ground based facilities, it represents the efficiency lose due to mid and high-spatial frequency components in observing time. The metric also properly counts for the optic error of the mirror itself such as the deviations from a perfect surface, and metrology measurement errors .The metric can multiply all the errors which differentiates from the traditional ones, such as RMS. We also numerically confirm this feature for Karman model atmosphere error multiplied with the sample of our vendor and the TMT M3.Additonaly, we discuss other pertinent feature of the PSD, including its relationship to Zernike aberration ,and RMS of wave front errors.
With the development of infrared technology and material, infrared zoom system is playing an important role in the field of photoelectric observation, the demand of infrared systems is increasing rapidly. In order to satisfy the requirement of infrared tracking imaging requirements of a car optoelectronic devices, different kinds of mechanical structure has been discussed, finally, according to the character of the optical design result, cam mechanism is adopted in zoom mechanism design, ball screw has been used in focusing mechanism design. As is known to all, cam is the key part in zoom system, the static, dynamic and thermal characteristics of the cam make great effect on the system performance because of the greater impact of the car’s shaking and a larger range of temperature changes, as a result, the FEM analysis is necessary. The static performance is all right obtained by the finite element analysis results, the cam’s first -order natural frequency is 97.56 Hz by modal analysis, the deformation of cam in the temperature difference of 80 °C is no more than 0. 003 mm by thermal analysis, which means the mechanical performance of the cam is fine. at last, the focusing mechanism has been designed, and analysis of focusing mechanism precision and encoder theoretical resolving power has been done, this mechanism has the advantages of simple transmission chain and low friction, as well as reducing the transmission error, an absolute encoder is chosen to detect the displacement of the focusing mechanism, the focusing precision is 5μm, the encoder theoretical resolving power is 0.015μm. In addition, the measurements on how to suppress stray radiation have been put forward. The experiment afterward showed that the infrared zoom system performs well, which provides lot of experience in infrared zoom system design and adjustment.
In order to evaluate and test the image quality of large aperture telescope, the most directly method is adopting the collimator and test the telescope system with full aperture. Changchun Institute of Optics, Fine Mechanics and Physics (CIOMP) commenced developing the large aperture collimator for interferometric and image quality testing of meter scale optical systems under cryogenic, vacuum conditions. The aperture of the collimator which has been on the conceptual design phase is 1.5m diameter, and the optical configuration is Cassegrain, the focus is 50m. The material of reaction bonded Silicon Carbide (RB-SiC) produced by CIOMP will be used as the primary mirror substrate. And the figure accuracy of the primary mirror will be polished better than 15nm (RMS). The collimator will be working in a vacuum chamber and face down vertically to the unit under test. The application requirements, specification requirements, and some key technology are demonstrated and analysed with finite element analysis (FEA) in the paper. The feasibility, error budget, and hazards evaluation of the collimator are fulfilled by the FEA results. It demonstrated that the conceptual design meet the requirements of the 1.5m aperture vertical collimator, and could achieve the high accuracy requirements of the wavefront for the beam of light in the vacuum chamber, which the wavefront error should less than 32nm(RMS). Mechanical alignment errors induced by thermal and structural perturbations are monitored with an auto-focusing system to enable focus compensation. The ambient temperature of the collimator in chamber are controlled allowing testing while the chamber shrouds and test unit are brought to cryogenic temperatures. With the high accuracy of the wavefront, the collimator could test the image resolution, modulation transfer functions (MTFs), point spread functions (PSFs), encircled energy, wavefront error, best focus, etc. for optical systems. And the conceptual design could be consulted to other large aperture collimators.
Corrective force solving is a critical technology of the active optics. A method to solve active optics corrective force is
introduced, which is based on Householder transform of Zernike polynomial wave front fitting, this method is different
from the traditional least square method and Gram-Schmid orthogonal method, because it does not bring ill-conditioned
polynomial without constructing normal equation, so it can avoid calculation error, wave front fitting is precision. Based
on the coefficient of the Zernike polynomial and the response function of the each actuator, the stiffness matrix of the
primary mirror is built, and then adopting the damp least square method to calculate corrective force. Based on this
method, φ400m test mirror is simulated many times, the calculation result approve: if the Householder transform is
adopted, wave front fitting is precision, the result is stabilization and corrective effectiveness is better.