A dual-stage co-phase correction device for splicing telescopes

Abstract

The invention discloses a two-stage co-phase correction device for splicing telescopes. Aiming at the characteristic that co-phase correction is difficult for sub-mirrors of splicing telescopes, the co-phase correction device is designed to realize the large stroke and high height of each sub-mirror of splicing telescopes. Accurate spatial positioning achieves the purpose of cophase correction and improves the imaging quality of spliced ​​telescopes. It includes a coarse adjustment level driver, a coarse adjustment level support plate, a fine adjustment level driver, a fine adjustment level support plate, a coarse adjustment level lateral load unloading device, and a fine adjustment level lateral load unloading device. The whole device is corrected through two stages of coarse adjustment and fine adjustment, so that the sub-mirror can meet the precise positioning in space, and realize the co-phase correction of the sub-mirror.

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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