Two-stage co-phase correction device for spliced telescope

Abstract

The invention discloses a two-stage co-phase correction device for a spliced telescope, and aims to design the co-phase correction device aiming at the characteristic of difficulty in co-phase correction of sub-mirrors of the spliced telescope so as to realize large-stroke high-precision spatial positioning of each sub-mirror of the spliced telescope, achieve the purpose of co-phase correction andimprove the imaging quality of the spliced telescope. The device comprises a coarse adjustment stage driver, a coarse adjustment stage supporting plate, a fine adjustment stage driver, a fine adjustment stage supporting plate, a coarse adjustment stage transverse load unloading device and a fine adjustment stage transverse load unloading device. According to the whole device, through coarse adjustment and fine adjustment two-stage correction, the sub-mirror can meet space accurate positioning, and sub-mirror co-phase correction is achieved.

Description

technical field [0001] The invention relates to the technical field of co-phase correction of spliced ​​telescopes, in particular to a two-stage co-phase correction device for spliced ​​telescopes. Background technique [0002] As an important tool for astronomical research, telescopes have been developed for hundreds of years. Today, driven by the hot issues in astronomical research, astronomical telescopes are developing in the direction of strong light-gathering ability, high-resolution, and full-band. Building a telescope with a larger aperture has always been the goal of astronomers. However, the increase in the aperture of the primary mirror of the telescope will increase its manufacturing cost and technical difficulty. In this regard, scientists have proposed to use spliced ​​mirrors as the main mirror of the telescope. The 8-10m class ground-based telescopes that have been built so far such as KECK1 and KECK2, and the tens of meter class telescopes under constructi...

AI Technical Summary

Problems solved by technology

[0007] However, for the expandable spliced ​​primary mirror telescope, the common phase correction schemes adopted in the above-mentioned typical spliced ​​primary mirror telescope have their shortcomings, mainly including the following points: (1) the axial dimensions of the above-mentioned schemes It is too large to meet the index requirements of the expandable splicing telescope; (2) on the observation band, unlike the telescopes mentioned in Table 1, the working band of the telescope is the visible light band, according to the requirements of splicing mirrors and mirrors. The correction accuracy needs to be above 0.05λ, and the above-mentioned solutions cannot meet the accuracy requirements; (3) The telescope adopts the electronic scanning mode, which requires the device to be able to tilt quickly

It can be seen from the above that the existing solutions cannot meet the needs of the expandable splicing primary mirror telescope in terms of device volume, adjustment accuracy, and tilt speed.

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