共查询到19条相似文献,搜索用时 250 毫秒
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对低纬子午环的仪器误差作了分类,包括制造误差、安装误差、仪器重力变形和热变形的影响,还分别列出了各种误差测量设备的制造误差、安装误差、读数零点偏差及其漂移的影响。文中强调了在该仪器误差修正中,不建立和使用任何误差模型,而是采用实时测定值,并且特别注意消除系统误差的影响,在这基础上,才能通过重复采数来压缩随机误差的影响。 相似文献
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测定天文大气折射和建立电磁波折射延迟实测模型(Ⅲ)-专用测量仪器 总被引:1,自引:0,他引:1
针对用天文大气折射测定值,建立随观测站和随方位而异的电磁波折射延迟改正模型的高精度要求,提出了新的仪器误差理论,其主要内容是允许仪器误差存在,并看成是不断变化的,采用相应的测量方法作实时的测定和修正,同时消除仪器的各种变形和误差的影响,排除观测数据中的各种系统误差来源,并达到提高单次测定精度目的;文中还针对不同纬度的观测站、多方位、从天顶直到低空的观测需要,给出了仪器总体结构的安排,和采用视频CCD作为接收器的终端设计方案,也给出了各种仪器误差的测定方法和测量装置的设计要求。 相似文献
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叙述了低纬子午环在研制中没有对加工提出苛刻的高精度要求的原因,分析了仪器在目前状态下,仪器方位指向、水平轴指向和望远镜光轴指向的实际精度,论述了克服这些指向误差影响,提高观测精度的基本思路,以及仪器研制成功的关键所在。 相似文献
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本文讨论了在利用卯酉圈观测方法绝对测定观测点瞬时纬度的过程中,仪器定向误差、周日光行差和大气折射的高次项对所得结果的影响。研究结果表明,仪器定向误差的高次项影响在可观测天顶距范围内都是比较大的,必须在结果中加以改正。而周日光行差和大气折射的影响一般不大,在精度要求的范围内可以忽略。 相似文献
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低纬子午环配备科学CCD的必要性和可行性 总被引:1,自引:1,他引:0
从基本天体测量学科的发展趋势和低纬子午环的课题目标出发,叙述了该仪器配备科学CCD的必要性和对仪器性能的相应要求,并根据仪器的各种误差的测定方法和测定精度的分析,论述了该仪器配备科学CCD后对天体位置作高精度绝对测定的可行性,文中还提出了对配备科学CCD的总体要求。 相似文献
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本文根据基本天体测量的主要任务和目前发展趋势的要求 ,以及低纬子午环配备CCD后的观测精度、效率和极限星等 ,提出了该仪器长期观测的课题目标 ,包括建立实用的准惯性天球参考架和动力学参考架 ,为太阳系动力学研究 ,为银河系结构和运动学研究 ,为某些天体物理课题研究的需要 ,提供有用的观测数据 ,为本地的地震预报和天文地震研究提供参考数据。在甚长基线射电干涉测量技术和空间测量技术迅速发展的时代 ,地面光学天体测量仍具有其不可取代的优势 ,只要能高精度地测定仪器的各种误差 ,消除仪器重力变形和热变形的影响 ,并尽可能消除由地球大气因素引起的系统误差影响 ,取得与空间测量平均而言可比的观测精度 ,两者相互配合 ,取长补短 ,就能更好地为上述诸多课题目标开展观测和研究 ,促进天体测量学和有关学科的发展 ,文中对这些要求的实现作了必要的叙述。 相似文献
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有限元分析技术在空间太阳望远镜结构设计中的应用 总被引:2,自引:0,他引:2
有限元分析技术是现代工程领域中进行结构分析的一种数值方法,已经广泛应用于天文仪器设计。它可使设计者了解被设计对象相应的特性,发现强度或刚度等方面的薄弱点,从而改进和优化设计。以空间太阳望远镜主桁架和主镜室的设计为例,从几何建模、单元划分入手,对静力学分析、模态分析、动态响应和热分析等各方面在空间太阳望远镜设计中的应用进行了阐述;分析了有限元分析存在的误差、产生的原因以及如何减少误差;叙述了有限元分析技术应用于天文仪器尤其是空间天文仪器的发展趋势。 相似文献
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Minoru Ando Tetsuya Nagata Shuji Sato Makoto Watanabe Kunio Itoh Toshihide Kawai Hidehiko Nakaya Yoshiharu Namba Takeshi Takezawa 《Experimental Astronomy》2002,13(3):119-134
We constructed a wide field cryogenic telescope (WFCT) containing a whole Ritchey-Chrétien system and a focal plane array
in a cryostat for near infrared observations to cover the field of view of 0.4°. The telescope has a primary mirror of 220
mm and an engineering grade 256 × 256 InSb array. The optical components such as two mirrors, filters, spiders, and radiation
shield tube are cooled down to 180 K as well as the InSb array to 35 K by a mechanical refrigerator. We show the results of
the background surface brightnesses and the limiting magnitudes at 3.3 and 3.67 μm measured at Sutherland, South Africa. We
describe the on-going upgrade of this instrument, equipped with a 1024 × 1024 ALADDIN InSb science grade array.
This revised version was published online in July 2006 with corrections to the Cover Date. 相似文献
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We have developed a method to measure the mirror reflectivity of telescopes. While it is relatively easy to measure the local reflectivity of the mirror material, it is not so straightforward to measure the amount of light that it focuses in a spot of a given diameter. Our method is based on the use of a CCD camera that is fixed on the mirror dish structure and observes simultaneously part of the telescope’s focal plane and the sky region around its optical axis. A white diffuse reflecting disk of known reflectivity is fixed in the telescopes focal plane. During a typical reflectivity measurement the telescope is directed to a selected star. The CCD camera can see two images of the selected star, one directly and another one as a spot focused by the mirror on the white disk. The ratio of the reflected starlight integrated by the CCD from the white disk to the directly measured one provides a precise result of the product of (mirror area × mirror reflectivity). 相似文献
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2.4m天文望远镜光学系统的设计及副镜检验的几种可能方案 总被引:1,自引:0,他引:1
详细说明了 2 .4m天文望远镜分别采用主镜焦比f/1 .5和f/3时光学系统的设计 :针对主镜焦比为f/3的凸非球面副镜 ,阐述了运用 4种不同检验方案的设计结果 ;重点介绍了计算全息法。并对几种方案作了比较 相似文献
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Hartmut W. Hoeness Rudolf Mueller Erich W. Rodeck Friedrich B. Siebers 《Astrophysics and Space Science》1989,160(1-2):193-197
For about 20 years SCHOTT has been supplying the glass ceramic ZERODUR, a material with very low thermal expansion. Besides many other applications, ZERODUR is excellently suited for the manufacture of mirror substrates for telescopes. About 80% of all telescopes in the western world with mirror diameters >1.8 m have been equipped with ZERODUR during the last 10 years. The development of modern astronomical telescopes is aimed at larger primary mirrors and lighter secondary mirrors.New techniques have been developed by SCHOTT for manufacture of thin monolithic mirror blanks of more than 8 m in diameter. The development of thin meniscus shaped shells using the spin-casting technique was successfully completed last year. During a test production several mirror substrates up to 4.1 m in diameter and down to 57 mm in thickness could be produced. The know-how has been acquired for the fabrication of mirror substrates of more than 8 m in diameter by the spin-casting technique.SCHOTT has also performed considerable developmental work in the field of lightweighted ZERODUR mirror substrates which can be generated using different techniques: forming of the lightweighted structure during casting, fusion of individual components to a total structure and lightweighting of a massive block by various mechanical machining methods.Paper presented at the Symposium on the JNLT and Related Engineering Developments, Tokyo, November 29–December 2, 1988.Registered trademark of SCHOTT Glaswerke, Mainz. 相似文献
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《Chinese Astronomy and Astrophysics》2004,28(3):356-366
A configuration for the Future Giant Telescope is proposed. It is a 30m telescope with segmented primary mirror and alt-azimuth mounting. The aspherical f/1.2 primary mirror is made up of 1095 partial annular submirrors. The optical system includes a Nasmyth system, a coude system and a wide field system. The Nasmyth system has a novel design with four mirrors and provides a ∼10 arcmin field of diffraction-limited images, a much larger field than can be obtained by the traditional Nasmyth system. Several diffraction-limited observations each over a small field, can be carried out simultaneously. By applying active optics to change the shape, tip, tilt and piston of the submirrors, thereby to effect a new aspherical surface of the primary, excellent quality images can be obtained for the coude system and the wide field system. The wide field system has a field of 25 arcmin, the focal surface is only slightly curved and the atmospheric dispersion could be corrected. The tolerances of the surface shape and position for the submirrors, and the telescope mounting and structure are also discussed. The innovations in this configuration should have a general significance for future giant telescopes. 相似文献
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本文提出一种新的反射镜轻量化方案。此方案在结构特征和减重比例上接近蜂窝结构,减重效果比背面开孔的镜子和拱形镜要好得多;同时又可避免蜂窝镜的制造难度。另外,本文还就此方案在空间太阳望远镜(SST)的相关跟踪摆镜上的应用进行探讨,给出了主要结构参数和镜面变形分析结果,其结果表明,此轻量化平面镜能满足SST的使用要求。 相似文献
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Rosalind Hopwood Trevor Fulton Edward T. Polehampton Ivan Valtchanov Dominique Benielli Peter Imhof Tanya Lim Nanyao Lu Nicola Marchili Chris P. Pearson Bruce M. Swinyard 《Experimental Astronomy》2014,37(2):195-205
Emission from the Herschel telescope is the dominant source of radiation for the majority of SPIRE Fourier transform spectrometer (FTS) observations, despite the exceptionally low emissivity of the primary and secondary mirrors. Accurate modelling and removal of the telescope contribution is, therefore, an important and challenging aspect of FTS calibration and data reduction pipeline. A dust-contaminated telescope model with time invariant mirror emissivity was adopted before the Herschel launch. However, measured FTS spectra show a clear evolution of the telescope contribution over the mission and strong need for a correction to the standard telescope model in order to reduce residual background (of up to 7 Jy) in the final data products. Systematic changes in observations of dark sky, taken over the course of the mission, provide a measure of the evolution between observed telescope emission and the telescope model. These dark sky observations have been used to derive a time dependent correction to the telescope emissivity that reduces the systematic error in the continuum of the final FTS spectra to ~0.35 Jy. 相似文献