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近年来,三维成像光谱技术主要是发展和采用积分视场单元方法,即将枧场内的展源目标连续切割成若干单元,重新排列后进入光谱仪器,同时获得展源的高分辨率三维数据立方体(x,y和λ).相对于传统的技术方法,这种基于积分枧场单元的三维成像光谱技术进行一次观测可以同时获取天体各处的二维空间信息和光谱信息.采用积分视场单元虽然在光谱数据处理上会带来很多困难,但由于其在观测时间和效率上具有明显的优点,因此值得采用.该文简要介绍了三维成像光谱技术的原理;评述了目前实现三维成像光谱的三种不同类型的技术系统:小透镜阵系统、光纤加小透镜阵系统、像切分器系统,重点介绍了像切分器系统的有关情况;最后展望了三维成像光谱技术在天文学上的应用. 相似文献
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《天文学进展》2017,(2)
中国丽江积分视场光纤光谱仪(China Lijiang Integral Field Unit,简称CHILI)是中国第一台用于夜天文观测的科学级积分视场光纤光谱仪,安装在丽江天文观测站2.4 m光学望远镜上。CHILI运输到中国前,在美国德克萨斯大学奥斯汀分校(University of Texas at Austin)进行了实验室测试。本次实验主要针对CHILI的蓝端,主要测试内容有本底、平场、暗场和波长定标。为了明确知道谱线在像素位置上的精准波长和CHILI探测器的分辨能力,对测试数据进行了波长定标和光谱分辨能力的计算。结果显示,CHILI蓝端的波长范围约为3 500～5 300,在此波长范围内,光谱分辨本领FW H M■5,其对应的光谱分辨率R=λ/?λ约为600～1 000,符合CHILI预期要求。 相似文献
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宽视场多目标光谱仪具有宽波段、多分辨率模式和高通光效率的特点,是极大望远镜终端仪器使用率最高的通用型仪器. 30 m级望远镜的宽视场多目标光谱仪因体量和成本急剧增加而面临重要挑战,同时天文学的不断发展对天文新技术的发展提出了更高的要求,尤其是多个巡天项目对于多目标光谱后随观测的迫切需求.综述了几类宽视场多目标光谱仪的发展现状,介绍了国际3架30 m望远镜宽视场多目标光谱仪概念设计的最新进展和仪器特点,着重介绍了中国参与研制的30 m望远镜(TMT)中的宽视场多目标光谱仪的相关进展. 相似文献
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主要介绍了抚仙湖1 m新真空太阳望远镜(the 1-meter New Vacuum Solar Telescope,NVST)6 m水平式近红外光谱仪的安装过程和实测结果。主要讨论内容是光路设计特点、光学系统的装调以及利用该光谱仪对活动区NOAA 11662黑子进行的初步近红外光谱实测(波长1.56μm附近)。成功观测到由黑子强磁场造成的Fe I 1.56μm谱线裂变现象,并初步估算了磁场强度。该光谱的成功装调和使用,充分实现了对9 m光谱仪光学系统的整体检测,为9 m光谱仪的安装调试提供了宝贵的经验和参考。 相似文献
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8~10m级光学／红外望远镜的高分辨率光谱仪 总被引：1，自引：0，他引：1
介绍并比较了KeckSubaruVLTHET及Gemini中的5架8～10m天文望远镜的高分辨率光谱仪,分析这些仪器与2～4m级望远镜的阶梯光栅光谱仪或Coude光谱仪相比所采用的新设计思想和新技术. 相似文献
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讨论了如何将SOPC技术用于大天区多目标光纤光谱天文望远镜(LAMOST)项目的低分辨率光谱仪IP控制核的设计,并在NIOSⅡ软核基础上设计实现了光谱仪IP控制核。整个IP控制核主要分为底层电机控制单元和通信单元两部分。通过工业以太网,远程控制计算机可以方便地控制低分辨率光谱仪,使其完成指定动作。也可以从本地控制计算机上实行控制。设计中采用将步进电机控制器封装成IP再复用的方法,大大缩短了研发时间,减少错误的发生。通信控制中串口通信和以太网可以互为冗余,保证了通信的顺利进行。 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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大天区面积多目标光纤光谱望远镜(Large Sky Area Multi-object Optical Spectroscopic Telescope,LAMOST)是目前国际上口径最大、视场最宽、光谱获取率最高的大型施密特望远镜,通过借助并行可控式双回转光纤定位系统,其焦面系统上的4 000根光纤可以在数分钟内按预定天体坐标快速精确地对准各自观测目标并进行精调。望远镜观测时每一个光纤单元定位情况的好坏直接决定接收天体光谱的质量,然而目前针对光纤定位精度情况仅有的信息就是定位时光纤单元步进电机驱动情况的反馈,是一个内部信息,并不全面,无法给出每一个光纤单元的实际定位精度情况。因此需要搭建一个可用于LAMOST现场的检测系统,在望远镜观测间隙,在前置光源照明条件下,可以第一时间获取焦面板光纤单元定位图像,快速分析之后,检测出定位误差较大的光纤单元,由此决定进一步观测处理措施,以保证观测光谱的有效性和准确率。 相似文献
9.
《天文研究与技术》2016,(2)
1 m新真空太阳望远镜(New Vacuum Solar Telescope,NVST)是国内用于对太阳进行观测和研究的大型科研设备,针对太阳活动区光谱观测的需求,在现有的大色散光谱仪及多波段光谱仪基础上,设计了光谱扫描设备,并基于C#设计了一套观测控制系统软件,实现扫描设备的运动控制和观测数据的采集。进行光谱扫描观测时,计算机控制扫描设备步进运动,并利用图像采集卡通过Camera Link总线采集CCD/CMOS相机的探测数据,基于多线程技术采集观测数据,将采集的图像数据存储成FITS(Flexible Image Transport System)文件,并将光谱图像数据处理成灰度图像用于软件界面监视。此套软件已用于1 m太阳望远镜光谱扫描观测,测试结果满足预期功能需求,为后续观测系统功能升级提供了良好的扩展性。 相似文献
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We describe the scheme and design features of the new IFU unit (Integral Field Unit) meant to perform integral-field spectroscopy as a part of SCORPIO-2 focal reducer, which is mounted in the prime focus of the 6-m telescope of the Special Astrophyscial Observatory of the Russian Academy of Sciences. The design of the unit is based on the principle of the formation of array spectra using a lens raster combined with optical fibers. The unit uses a rectangular raster consisting of 22×22 square 2-mm diameter lenses. The image of the object is transferred by an optical system with a 23× magnification from the focal plane of the telescope to the plane of the lens raster. The image scale is —0.″75/lens and the field of view of the instrument has the size of 16.″5 × 16.—52. The raster also contains two extra 2 × 7 lens arrays to acquire the night-sky spectra whose images are offset by ±3′from the center. Optical fibers are used to transform micropupil images into two pseudoslits located at the IFU collimator entrance. When operating in the IFU mode a set of volume phase holographic gratings (VPHG) provides a spectral range of 4600–7300 Å and a resolution λ/δλ of 1040 to 2800. The quantum efficiency of SCORPIO-2 field spectroscopy is 6–13% depending on the grating employed.We describe the technique of data acquisition and reduction using IFU unit and report the results of test observations of the Seyfert galaxyMrk 78 performed on the 6-m telescope of the Special Astrophysical Observatory of the Russian Academy of Sciences. 相似文献
15.
Yong Zhao Zhou Fan Juan-Juan Ren Liang Ge Xiao-Ming Zhang Hong-Bin Li Hui-Juan Wang Jian-Feng Wang Peng Qiu Xiao-Jun Jiang 《天文和天体物理学研究(英文版)》2018,(9)
The Beijing Faint Object Spectrograph and Camera(BFOSC) is one of the most important instruments operating in conjunction with the 2.16-m telescope at Xinglong Observatory. Every year there are~20 SCI-papers published based on observational data acquired with this telescope. In this work,we have systemically measured the total efficiency of the BFOSC that operates as part of the 2.16-m reflector, based on observations of two ESO flux standard stars. We have obtained the total efficiencies of the BFOSC instrument of different grisms with various slit widths in almost all ranges, and analyzed factors which effect the efficiency of this telescope and spectrograph. For astronomical observers, the result will be useful for them to select a suitable slit width, depending on their scientific goals and weather conditions during observations. For technicians, the result will help them to systemically identify the real efficiency of the telescope and spectrograph, and to further improve the total efficiency and observing capacity of the telescope technically. 相似文献
16.
During the last three decades an observational approach has been applied at the Byurakan Astrophysical Observatory to the problems of the evolution of astronomical bodies and systems. In contradiction to the traditional point of view, assuming that the processes of condensation are dominant in the Universe, this approach makes use of the observed predominance of expansions, ejections, and explosions.In the past, the observational approach has led to the prediction of an expansion of some stellar associations confirmed later by the analysis of observations. It became clear that the stellar associations are very young systems where the star-formation process is still continuing. The new approach has also led to the concept of the activity of galactic nuclei. The observational approach considers as a phenomenon of primary importance the formation of nebulae as a consequence of the activity of dense bodies (nebulae surrounding the novae, planetary nebulae, supernova remnants, cometary nebulae, and the diffuse nebulae in OB-associations).The new approach in application to the early stages of stellar evolution is discussed. The T Tauri-stage is considered as a phase following the more dense protostellar state. The flare stars are regarded as the next phase of evolution. The phenomena of fuors (FU Ori-type brightenings) can be considered as an expression of the same tendency (the transformation of dense matter into a rarefied state). 相似文献
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The role of magnetic fields in the dynamical evolution of galaxies and of the interstellar medium (ISM) is not well understood, mainly because such fields are difficult to directly observe. Radio astronomy provides the best tools to measure magnetic fields: synchrotron radiation traces fields illuminated by cosmic-ray electrons, while Faraday rotation and Zeeman splitting allow us to detect fields in all kinds of astronomical plasmas, from lowest to highest densities. Here, we describe how fundamental new advances in studying magnetic fields, both in our own Milky Way and in other nearby galaxies, can be made through observations with the proposed Square Kilometre Array. Underpinning much of what we propose is an all-sky survey of Faraday rotation, in which we will accumulate tens of millions of rotation measure measurements toward background radio sources. This will provide a unique database for studying magnetic fields in individual Galactic supernova remnants and Hii regions, for characterizing the overall magnetic geometry of our Galaxy’s disk and halo, and for understanding the structure and evolution of magnetic fields in galaxies. Also of considerable interest will be the mapping of diffuse polarized emission from the Milky Way in many narrow bands over a wide frequency range. This will allow us to carry out Faraday tomography of the Galaxy, yielding a high-resolution three-dimensional picture of the magnetic field within a few kpc of the Sun, and allowing us to understand its coupling to the other components of the ISM. Finally, direct synchrotron imaging of a large number of nearby galaxies, combined with Faraday rotation data, will allow us to determine the magnetic field structure in these sources, and to test both the dynamo and primordial field theories for field origin and amplification. 相似文献
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P. Abolmasov 《New Astronomy》2011,16(2):138-146
For a long time, the well-known supercritically accreting binary SS433 is being proposed as a prototype for a class of hypothetical bright X-ray sources that may be identified with the so-called Ultraluminous X-ray sources (ULXs) in nearby galaxies or at least with part of them. Like SS433, these objects should be associated with optical nebulae, powered by both radiation of the central source and its wind or jet activity. Indeed, around many ULXs, bright optical nebulae (ULX Nebulae, ULXNe) are found. Here, we use SS433 as a prototype for the power source creating the nebulae around ULXs. Though many factors are important such as the structure of the host star-forming region and the possible supernova remnant formed together with the accreting compact object, we show that most of the properties of ULXNe may be explained by an SS433-like system evolving for up to about one million years in a constant-density environment. The basic stages of evolution of a ULX Nebula include a non-spherical HII-region with a central cavity created by non-radiative shock waves, an elongated or bipolar shock-powered nebula created by jet activity and a large-scale quasi-spherical bubble. 相似文献
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In several nearby L ∼ L* early‐type galaxies, recent observations at large radii have shown indications of a lack of dark matter, substantially at odds with the prediction from the Cold Dark Matter (CDM) hierarchical merger models. Here we discuss a pilot observational project for the study of the internal kinematical and dynamical properties of this remarkable sample of galaxies. Using the VIMOS‐IFU in its high spectral resolution mode, it would be possible to investigate the regions up to ∼1.2 Re, taking advantage of the much larger field of view and telescope diameter. This will allow to disclose the presence of any kinematical substructures which could affect the conclusion on the mass modeling and definitely clarify the inner structure of this particular class of early‐type galaxies. (© 2004 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim) 相似文献
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A. Hughes L. Staveley-Smith S. Kim M. Wolleben M. Filipovi&#; 《Monthly notices of the Royal Astronomical Society》2007,382(2):543-552
We present a mosaic image of the 1.4-GHz radio continuum emission from the Large Magellanic Cloud (LMC) observed with the Australia Telescope Compact Array (ATCA) and the Parkes Telescope. The mosaic covers with an angular resolution of 40 arcsec, corresponding to a spatial scale of ∼10 pc in the LMC. The final image is suitable for studying emission on all scales between 40 arcsec and the surveyed area. In this paper, we discuss (i) the characteristics of the LMC's diffuse and compact radio continuum emission, (ii) the fraction of the emission produced by thermal processes and the implied star formation rate in the LMC and (iii) variations in the radio spectral index across the LMC. Two non-standard reduction techniques that we used to process the ATCA visibility data may be of interest for future wide-field radio continuum surveys. The data are open to the astronomical community and should be a rich resource for studies of individual objects such as supernova remnants, H ii regions and planetary nebulae as well as extended features such as the diffuse emission from synchrotron radiation. 相似文献