Method for realizing active optical system of large field survey telescope

Abstract

The invention provides a method for realizing an active optical system of a field survey telescope. The method comprises steps that: an active optical control main server sends a gravitational deformation correction instruction to an industrial computer; the active optical control main server sends an instruction for measuring a collimation error of a main focus device to the industrial computer;the active optical control main server sends an instruction for performing a preliminary correction on the collimation error of the main focus device to a collimation control unit of the main focus device of the industrial computer, thereby performing active optical correction on a field survey telescope. The method is simple and efficient. After corrected by the active optical system, the axial positioning error is expected to reach 0.002 mm, the eccentric error is expected to be within 0.02 mm, and the tilt error is expected to be within 0.001 degrees after the main focus device is corrected. Without considering the influence of seeing, the wavefront error RMS is within 0.05, the overall image quality mean is controlled below 5 microns, and the image quality degradation is controlled within 5% after correcting the gravitational deformation and thermal deformation of a main mirror by the active optical system.

Description

technical field [0001] The invention belongs to the technical field of optical systems, and in particular relates to a method for realizing an active optical system of a large-field survey telescope. Background technique [0002] An automated survey telescope is a type of telescope. It is suitable for observing extended celestial bodies and performing sky survey observations. With the birth of new concepts in the 1980s, in order to enhance the light-gathering ability of the telescope, the diameter of the primary mirror should be more than 4 meters. Obviously, the above-mentioned traditional methods of maintaining image quality and preventing lens deformation due to gravity Restrictions by price and structural weight no longer apply. In order to improve the image quality of large and medium-sized telescopes, the built-in optical correction components automatically adjust the image quality during the observation process, and these correction components work at relatively low...

AI Technical Summary

Problems solved by technology

With the birth of new concepts in the 1980s, in order to enhance the light-gathering ability of the telescope, the diameter of the primary mirror should be more than 4 meters. Obviously, the above-mentioned traditional methods of maintaining image quality and preventing lens deformation due to gravity Limitations by price and structural weight no longer apply

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