共查询到18条相似文献，搜索用时 125 毫秒
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光学近红外相机CASCAM(Chinese Academy of Sciences．Camera)采用光学CCD和近红外阵列HAWMH-1(HgCdTe Astronomical Wide Area Infrared Imaging)探测器，配备兴隆2．16m望远镜可同时进行光学、近红外成像和偏振观测。CASCAM的机械系统主要包括光学箱、真空箱以及致冷设计。其中光学箱是相机光学系统和探测器的载体，同时防止来自光学箱外部的红外热辐射；真空箱位于光学箱外部，它是整个系统的机械支撑，保证相机有良好的真空密封性能，并和真空泵、冷冻机一起构成了相机的致冷系统。 相似文献
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LAMOST是一个大视场兼大口径的中星仪式望远镜,其光学系统是反射Schmidt系统。为克服Schmidt系统长镜筒（二倍焦距）的整体运动所引起的各种困难,采用了特殊的装置,即球面主镜固定不动,由非球面改正板的转动完成对被观测目标的瞄准和跟踪。使大视场和大口径的兼备成为可能。因而AMOST在观测过程中的成像情况与一般的望远镜不同,其焦面、改正板的位置和面形,都随观测天区和时间而变化,另外还有视场旋转和大气折射的影响。本文提出了用光轴稍微倾斜放置的球面代替最佳焦面的方法,并详细叙述了对LAMOST实际观测过程中,光学系统成像情况动态模拟分析的方法和结果。进一步证明了这种特殊的光学系统的可行性。 相似文献
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给出红外点源IRAS 20231 3440附近恒星形成区近红外．JHK’和H2成像观测结果，以及与该IRAS点源成协的近红外点源IRS1的K波段分光观测结果．．JHK’观测显示该区域存在嵌埋的年轻星天体，H2窄波段观测揭示了若干个氢分子发射结点，其中有几个结点排列成线形，暗示分子氢喷流的存在．喷流的北部与已知观测的分子外流成协，表明二者之间存在联系．喷流的走向提示IRS1可能是其激发源，对IRS1的K波段分光观测给出了进一步的证据．从近红外、MSX及IRAS资料估计出IRS1的能谱分布，表明它是一个处于ClassI状态的中等质量的年轻星天体． 相似文献
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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。 相似文献
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1m红外太阳塔是我国未来重点发展的地面太阳观测设备，本文的所有工作均围绕着与此相关的红外波段太阳观测技术方法展开。1．针对望远镜实验平台－云台太阳光谱仪，建立了光谱仪分光流量,工用多种实验手段验证了其可靠性。利用该模型计算了Fe Ⅰ1.56μm红外太阳光 谱的分光流量，分析了实验观测的可行性及改进方案。2．针对探测器实验平台－PtSi红外焦平面阵列相机，建立了FeⅠ1.56μm光谱观测信噪比模型，模拟了各种噪声对观测的影响。在此基础上，在国内首次成功进行了FeⅠ1.56μm红外太阳光谱的面阵观测实验。3．在红外观测实验所处的高背景低对比度条件下，讨论了红外太阳光谱观测的图像处理方法，分析了观测中出现的干涉条纹的来源及解决办法，初步建立起了一整套红外太阳光谱与成像的定标方法和图像处理方法。4．首次利用PVA材料，设计研制了一套FeⅠ1.56μm近红外Stokes参量偏振仪，并将该偏振仪安装在美国国立天文台McMath望远镜上进行了观测实验。针对一太阳黑子，通过扫描进行了二维的Stokes参量观测。同时建立了一套从Stokes参量反演磁矢量场的方法，并将反演的结果与怀柔太阳磁场望远镜的观测结果进行了比对。5．针对1m红外太阳塔的太阳光谱仪系统，给出了垂直多波段光谱仪和红外大色散光谱仪的光、机初步设计。6．针对1m红外太阳塔的科学目标，提出了多波段光谱仪探测器系统方案，对红外大色散光谱仪所使用的红外探测器也进行了初步方案设计。 相似文献
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本文作者用北京天文台兴隆站２．１６米望远镜及卡焦ＣＣＤ摄谱仪，观测到一颗红移为１．６６的类星体，讨论了该望远镜卡焦摄谱系统的总体光效率。 相似文献
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中国科学院云南天文台1 m新真空太阳望远镜(New Vacuum Solar Telescope,NVST)是我国在太阳物理和空间科学对太阳进行光学和近红外观测的主力设备,主要科学目标是高精度、高时空分辨率的太阳磁场测量。1 m新真空太阳望远镜采用机械扫描偏振观测方式,由于光学系统的结构特性导致望远镜在跟踪太阳的过程中不可避免地引入了随时间变化的偏振效应,因此在进行偏振观测时需要进行系统定标,整个系统由定标单元、分析单元和探测器组成,其间涉及的多个运动部件均有复杂精密的运动要求。针对偏振定标过程和偏振观测过程中各光学器件的运动需求,给出了定标单元和分析单元的控制要求,实现了不同观测模式下各部件的运动要求。基于TCP/IP协议的远程控制方案,集成了采用串口通讯的各商用驱动控制器,开发了一套在.NET架构下的定标单元控制软件和相应的用户界面,并预留了观测控制系统接口。性能测试表明,系统符合观测要求,现已投入使用,为后续的偏振观测奠定了基础。 相似文献
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E. H. Geyer K. Jockers N. N. Kiselev G. P. Chernova 《Astrophysics and Space Science》1996,239(2):259-274
For observations of solar system objects an imaging polarimeter has been constructed as an auxiliary instrument for a f/15 focal reducer. With this instrument simultaneous measurement of theQ andU Stokes parameters is possible. It contains no moving parts such as a moving /2 retarder. The polarizer consists of two Wollaston prisms which are combined to form a single optical element. Their polarization angles differ by 45°. This compound polarizer is placed in the exit pupil of the afocal telescope-collimator system of the focal reducer and splits the exit pupil into halves. In this way four polarized beams with E-vector orientations 0°, 90°, 45°, and 135° emerge from the exit pupil. These are intercepted by the camera lens of the focal reducer system and imaged simultaneously on the CCD detector. With a properly designed field mask at the Cassegrain focus, the four beams are imaged without overlap.As a demonstration of the capabilities of this quadruple-beam Wollaston-prism polarimeter, we present observations of comet Tanaka-Machholz 1992 X in May 1992. The advantages, shortcomings, and possible improvements of the instrument are discussed.based on observations obtained at Hoher List Observatorypresently at Astronomical Observatory of Khar'kiv University, Sumskaya Street 35, 310022 Khar'kiv, Ukraine 相似文献
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A. Akhperjanian R. Kankanian V. Sahakian A. Heusler C.-A. Wiedner H. Wirth 《Experimental Astronomy》1998,8(2):135-152
The raytracing technique was used to derive a suitable design for the HEGRA system of Cherenkov telescopes, which is at present commissioned at La Palma. The reflectors with a diameter of 3.9 m consist of 30 spherical mirrors with focal lengths in the range of 4.88 – 4.94 m. It is shown that 93% of the photons from the Cherenkov light emitted by an extended air shower are contained in the camera pixels, 0.25° in diameter, for the full field of view of = ± 2.5°. The optical performance of the HEGRA design is compared to other layouts. 相似文献
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S. P. Willner 《Experimental Astronomy》1994,3(1-4):147-148
A camera design with only four lens elements gives good imaging performance at a working focal ratio of f/4.4. 相似文献
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T. A. Lozinskaya A. V. Moiseev N. Yu. Podorvanyuk A. N. Burenkov 《Astronomy Letters》2008,34(4):217-230
We have investigated the structure, kinematics, and emission spectrum of the ionized gas in the synchrotron superbubble in the irregular galaxy IC 10 based on observations with the 6-m Special Astrophysical Observatory telescope with the SCORPIO focal reducer in three modes: direct imaging in the [S II] λ(6717 + 6731) Å lines, long-slit spectroscopy, and spectroscopy with a scanning Fabry-Perot interferometer. We have identified a bright (in the [S II] lines) filamentary optical shell and determined its expansion velocity, mass, and kinetic energy. The nature of the object is discussed. 相似文献
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Roberto Viotti Cesare D. La Padula Domenico Nanni Agostino Vignato 《Astrophysics and Space Science》2001,276(1):81-88
We present the basic concepts of the two-mirror, three-reflection optical system (2MTRT), and discuss the important benefits of such a system for space projects: wide ( 2°) correctedand unvignetted FOV, without the use of refractive optics for thefield correction, planarity of the focal surface for an optimizedinstallation of wide area detectors, easy telescope adjustement, small volume and little mass.We also report the results of optical tests made with a 30 cm prototype,equipped with a 2k × 2k CCD camera, and give examples of scientific programmes which can be performed from space and in hostile terrestrial sites such as the Antarctic Plateau. 相似文献
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K. Kawata T. K. Sako M. Ohnishi M. Takita Y. Nakamura K. Munakata 《Experimental Astronomy》2017,43(1):1-17
ASTRI SST-2M is one of the prototypes of the small size class of telescopes proposed for the Cherenkov Telescope Array. Its optical design is based on a dual-mirror Schwarzschild-Couder configuration, and the camera is composed by a matrix of monolithic multipixel silicon photomultipliers managed by ad-hoc tailored front-end electronics. This paper describes the procedures for the gain calibration on the ASTRI SST-2M. Since the SiPM gain depends on the operative voltage and the temperature, we adjust the operative voltages for all sensors to have equal gains at a reference temperature. We then correct gain variations caused by temperature changes by adjusting the operating voltage of each sensor. For that purpose the SiPM gain dependence on operating voltage and on temperature have been measured. In addition, we present the calibration procedures and the results of the experimental measurements to evaluate, for each pixel, the parameters necessary to make the trigger uniform over the whole focal plane. 相似文献
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The Automated Patrol Telescope is a wide-field CCD imaging telescope of novel design. The telescope is a converted Baker-Nunn satellite tracking camera that has undergone extensive modification to its optical, mechanical and electronic systems. Telescope operation is entirely under computer control, and the instrument is to be used for a variety of astronomical survey and monitoring projects. 相似文献