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望远镜终端
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  “望远镜终端”译为未确定词的双语例句
     Reform of Telescopic Terminal System for the Fine-Heliograph at Gan-Yu Station of Purple Mountain Observatory and Recent New Solar-Observations
     紫金山天文台赣榆观测站精细结构望远镜终端系统改造及最新观测结果
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     The interface of filter on 1M Telescope of Yunnan Observatory was controled by the hand before. It was not convenient for use.
     云台1m RCC望远镜终端滤光片接口原设计为手动切换,因滤光片远离操作控制设备,使用很不方便。
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  相似匹配句对
     Terminal Sales Modes of Jewelry
     终端突围
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     A Telescope A Dumb
     望远镜·哑巴
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     Artificial Intelligence Terminal
     智能终端
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     internal focusing telescope;
     可调焦望远镜 ;
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     Reform of Telescopic Terminal System for the Fine-Heliograph at Gan-Yu Station of Purple Mountain Observatory and Recent New Solar-Observations
     紫金山天文台赣榆观测站精细结构望远镜终端系统改造及最新观测结果
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  telescope instrument
It is a single mode, dispersed fringes, three telescope instrument.
      
The attitude control system is tightly coupled with guide telescope instrument to provide the precise pointing required by the payload.
      
The boxes show the approximate detection limits for each telescope/instrument.
      


In this paper, the resolution requirements of the image-detecting devices attached to a telescope, especially those of the electrographic cameras, and their developments in some countries as well as the question on the preferred types of devices to be developed, are discussed.For image-detecting devices designed to achieve limiting resolution in ground-based astronomical observations the seeing disk is the fundamental limiting factor, and for electro-graphic cameras using superconducting magnet even the optical...

In this paper, the resolution requirements of the image-detecting devices attached to a telescope, especially those of the electrographic cameras, and their developments in some countries as well as the question on the preferred types of devices to be developed, are discussed.For image-detecting devices designed to achieve limiting resolution in ground-based astronomical observations the seeing disk is the fundamental limiting factor, and for electro-graphic cameras using superconducting magnet even the optical telescope itself becomes the limiting agent as well. The modulation tansfer function (MTF) of an astronomical image-detecting system, T(K), is given by the following expression T(K)=T(K)1 . T(K)2 . T(K)3 . T(K)4[1] Where T(K)1 = The MTF of astronomical seeing;T(K)2=The MTF of the telescopic optical system; T(K)3=TheMTF of electron-optical system for image-detecting devices; T(K)4=The MTF of the plate for image detecting-devices. Here it is clear that the limiting spatial frequency that can be imaged reliably by the system occurs at the lowest spatial frequency for which one of the component MTF's reaches zero. Obviously, proper matching between the limiting resolutions of various components in the image-detecting system for astronomical observations is of basic importance. Therefore, the attempt to achieve resolutions as high as possible for image detecting devices, especially the attempt to use superconducting electro-magnet focusing camera, is hardly advisable.From table 2, a comparison between electrographic cameras using roomtemperature magnet and those using superconducting, magnet shows that the former is better than the latter. We think the roomtemperature electro-magnet focusing camera may be the best one in all photo-electronic image devices for ground based astronomical observations.

本文着重分析了光学天文观测对于望远镜终端图象接收器件,特别是电子照相器件的分辨率要求,讨论了合理选择器件研制课题的问题和国外的研制情况。

The serious effects of turbulence of the Earth atmosphere can be overcome so that the diffraction-limited resolution imaging of a large ground-based astronomical telescope can be achieved by the speckle imaging techniques. The original data required in these techniques are a series of the short-exposure speckle images recorded with a speckle image detection system attached to the telescope. In comparison with the requirements for the original data, structure and properties of the new speckle image detection-system...

The serious effects of turbulence of the Earth atmosphere can be overcome so that the diffraction-limited resolution imaging of a large ground-based astronomical telescope can be achieved by the speckle imaging techniques. The original data required in these techniques are a series of the short-exposure speckle images recorded with a speckle image detection system attached to the telescope. In comparison with the requirements for the original data, structure and properties of the new speckle image detection-system built at Yunnan Observatory are introduced. Some practical observation results got with this system showed that the requirements can be basically satisfied.

斑点成象技术能有效地消除地球大气湍流的不良影响,实现地基大型天文望远镜的衍射受限分辨率成象,其所需的原始数据是天文目标及参考星的一系列的短曝光斑点象,它们取自望远镜的终端设备:斑点象探测系统。文中对比该技术对原始数据的要求:介绍了云南天文台研制的新型斑点象探测系统的结构和性能。实际观测结果表明,该系统基本能满足要求。

A Faint Object Spectrograph and Camera (FOSC) for 1-meter telescope in Yunnan Observatory is introduced in this paper.It is a focal reduced camera type instrument and is mounted at the Cassegrain focus of 1-m telescope in Yunnan Observatory.The FOSC can be used in four different modes:direct imaging,long slit spectroscopy,slitless spectroscopy and coronography,and it is efficient and flexible.The optics design for the camera and for the spectrograph are shown.The light from the f/13.3 Cassegrain focus of the...

A Faint Object Spectrograph and Camera (FOSC) for 1-meter telescope in Yunnan Observatory is introduced in this paper.It is a focal reduced camera type instrument and is mounted at the Cassegrain focus of 1-m telescope in Yunnan Observatory.The FOSC can be used in four different modes:direct imaging,long slit spectroscopy,slitless spectroscopy and coronography,and it is efficient and flexible.The optics design for the camera and for the spectrograph are shown.The light from the f/13.3 Cassegrain focus of the 1-m telescope is collimated by collimating lens then passes to the camera and images on the CCD detector.In the wavelegth range of 404.6nm-766.5nm, the image quality is 0.5″ in diameter which encircles 80% of the energy in the 10′ of the field.Four modes are as follows:1Direct Imaging:It is a focal reduced camera with a field of 10′.The focal ratio is f/7.The standard filters of B?V?R?I are mounted for selection.2Slitless Spectroscopy Mode:A direct vision prism is inserted into the parallel beam of the focal reduced camera to become a slitless spectroscopy.The dispersion of this slitless spectroscopy is 100nm/mm in 486.1nm.3Long Slit Spectroscopy:The long slits are available to do spectroscopy with the direct vision prism.There are three slits mounted on a wheel in the Cassegrain focus.The slit size is 40mm×65μm(~1″),40mm×100μm(~1.5″),40mm×150μm(~2.25″),respectively.4Coronography Mode:A special plate is mounted on the slits wheel which is in the area of Cassegrain focus.The coronograph image can be obtained and the faint nebulosity around bright objects would be imaged with this mode.

云南天文台1m望远镜终端之一的暗天体分光仪和照相机具有4种运行模式:缩焦照相机、无缝多目标光谱仪、有缝光谱仪和星冕仪。这4种运行模式能在几分钟的时间内相互转换,高效快速和灵活方便。该仪器的光学质量优秀,光学系统消像差,特别是消色差。由于光学系统消色差,所成像的低色散光谱在404.6~766.5nm全波段尖锐平直。在多色测光时,各测光波段的像面位置不变,同时兼有大视场的优点,可提高测光精度和测光效率。

 
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