本文關(guān)鍵詞： 光學(xué)裝調(diào) 光軸 像質(zhì) 彎沉 靈敏度矩陣　出處：《中國科學(xué)院研究生院(云南天文臺(tái))》2016年碩士論文　論文類型：學(xué)位論文

【摘要】：一架設(shè)計(jì)先進(jìn)、加工精準(zhǔn)的大型光學(xué)望遠(yuǎn)鏡,工廠測試質(zhì)量合格后在使用地點(diǎn)安裝時(shí),必須再經(jīng)調(diào)校、檢測,保證望遠(yuǎn)鏡仍舊符合設(shè)計(jì)、使用要求。本文僅討論元件精準(zhǔn)的大型望遠(yuǎn)鏡調(diào)校及檢測問題。對(duì)于大型天文望遠(yuǎn)鏡,如果光學(xué)成像部件(如主鏡和副鏡)有些許的離心或傾斜,都會(huì)引起光軸的偏移,既會(huì)給望遠(yuǎn)鏡指向、跟蹤帶來困擾,還會(huì)造成有效視場丟失。同時(shí)我們發(fā)現(xiàn),當(dāng)離心與傾斜同時(shí)存在且保持特定關(guān)系時(shí),它們可以互相補(bǔ)償,而不太嚴(yán)重破壞望遠(yuǎn)鏡的綜合成像質(zhì)量;因此傳統(tǒng)的以綜合像質(zhì)為最終評(píng)估標(biāo)準(zhǔn)的檢測方法是不完備的。研究了計(jì)算機(jī)輔助裝調(diào)的方法,其過程是:像差測試、模型計(jì)算給出鏡面的調(diào)整方向和量值、調(diào)整鏡面位置;迭代這個(gè)過程直到像質(zhì)達(dá)標(biāo)。在這個(gè)過程中,以模型的正確性保障收斂結(jié)果的正確性和唯一性。一米紅外太陽望遠(yuǎn)鏡(New Vacuum Solar Telescope,簡稱NVST)是目前國際領(lǐng)先水平的真空太陽望遠(yuǎn)鏡,NVST位于云南省昆明市約70公里的撫仙湖東北岸老鷹地(東經(jīng)102°57′11″,北緯24°34′47″),該臺(tái)址擁有世界一流的大氣視寧度,光學(xué)系統(tǒng)為修正的格里高利(Gregorian)系統(tǒng),可對(duì)太陽磁流場高分辨率光譜和成像觀測,觀測波段為0.3μm~2.5μm。本文以NVST為例,討論了在主副鏡的安裝調(diào)校中存在空間的位置與方向誤差,但在綜合像質(zhì)仍舊達(dá)到衍射極限的前提下,考查誤差對(duì)光軸、視場帶來的影響,從而確定光軸穩(wěn)定性是判定大型望遠(yuǎn)鏡裝調(diào)結(jié)果的一項(xiàng)必檢指標(biāo)。
[Abstract]:A large optical telescope of advanced design and precise processing must be adjusted and tested when it is installed in the place of use after the factory has qualified the test quality to ensure that the telescope still conforms to the design. Requirements for use. This paper deals only with the calibration and detection of large telescopes with precise components. For large telescopes, optical imaging components (such as primary and secondary mirrors) that are slightly centrifuged or tilted will cause the deviation of the optical axis. It can cause problems with telescope pointing and tracking, as well as the loss of effective field of view, and we have found that when centrifugation and tilt exist at the same time and have a specific relationship, they can compensate each other. However, the integrated imaging quality of the telescope is not seriously damaged, so the traditional detection method based on the integrated image quality as the final evaluation standard is not complete. The computer-aided adjustment method is studied, and the process is as follows: aberration testing. The model calculation gives the direction and magnitude of the mirror, adjusts the position of the mirror, iterates the process until the image quality is up to standard. The correctness of the model ensures the correctness and uniqueness of the convergence results. The 1-meter infrared solar telescope Vacuum Solar Telescopeis a leading international vacuum solar telescope located about 70 kilometers in Kunming, Yunnan Province. The Eagle Land on the east coast of Xianhu (102 擄5711 "E, 24 擄3447" N) has world class atmospheric visibility. The optical system is a modified Gregorian system, which can be used to observe the high-resolution spectrum and imaging of the solar magnetic flow field. The observation band is 0.3 渭 m ~ (2.5 渭 m). In this paper, taking NVST as an example, the position and direction errors of the space in the installation and adjustment of the primary and secondary mirror are discussed. However, on the premise that the synthetic image quality still reaches the diffraction limit, the influence of the error on the optical axis and the field of view is examined, thus determining the stability of the optical axis is a necessary index to judge the adjustment results of large telescopes.
【學(xué)位授予單位】：中國科學(xué)院研究生院(云南天文臺(tái))
【學(xué)位級(jí)別】：碩士
【學(xué)位授予年份】：2016
【分類號(hào)】：P111.41

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