30m环形干涉望远镜

简要介绍了云南天文台对下一代地面大型天文光学望远镜进行的初步研究，依据这些研究结果我们提出研制一个新概念的大型地面望远镜：30m环形干涉望远镜（Ringy Interferometric Telescope），它既有单口径望远镜那样的直接成像能力和分辨率，又可以进行综合孔径模式的高分辨率成像，该计划显著地不同于经典的地面大型望远镜，对其中关键技术的研究正在积极进行之中。     

8~10m级光学／红外望远镜的高分辨率光谱仪

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.     

WSO-UV—ultraviolet mission for the next decade

The World Space Observatory UltraViolet (WSO–UV) is an international space mission devoted to UV spectroscopy and imaging. The observatory includes a 170 cm aperture telescope capable of high-resolution and long slit low-resolution spectroscopy, and deep UV and optical imaging. The observatory is designed for observations in the ultraviolet domain where most of astrophysical processes can be efficiently studied with unprecedented capability.     

New telescopes in China

This paper covers the main aspects of three new optical telescopes: a 1.26 m aperture one for use in the infrared, a 1.56 m aperture one for astrometry, and a 2.16 m reflector for general astrophysical work. It also briefly mentions the 13.7 m telescope designed for the mm wavelength band, the first VLBI in China and the meter wavelength aperture synthesis telescope. All these telescopes, optical and radio, are now being built in China.Paper presented at the IAU Third Asian-Pacific Regional Meeting, held in Kyoto, Japan, between 30 September–6 October, 1984.     

Robotic telescopes for high energy astrophysics in Ondřejov

We report on two small aperture robotic telescopes called BART and D50 operated in Ondřejov. Both telescopes are capable of automatic observation of gamma ray burst (GRB) optical afterglows. Coordinates of GRBs are taken from alerts distributed via Internet. Telescopes observe other interesting high energy sources when there is not any alert. The smaller telescope BART has aperture D = 254 mm. The bigger telescope D50 has a primary mirror of diameter D = 500 mm. Both telescopes are controlled by free software package RTS2 and are accessible through Internet. We describe the two telescopes and related software and show some results such as our first observed optical counterpart of GRB.     

Large-aperture telescopes in the problems of near-Earth astronomy

Telescopes with aperture higher than 3 m and with travel rate of optical axis of more than 4 angular degrees per second are examined. These telescopes are used for estimating the situation in near-Earth space. Up to now, there are three telescopes with such parameters: SOR, AMOS, SST (all in the United States). A telescope of the same class with aperture of 3.12 m (information telescope TI-3.12) is under completion at Altai Optical Laser Center. The main technical performances of the TI-3.12 telescope are described in the paper. Current problems are defined and ways for their solution are presented.     

ESO and European astronomy: four decades of reciprocity

This paper describes and discusses some key facts in the early history of the European Southern Observatory: the founding phase leading to the establishment of the “nucleus” of telescopes in Chile, the role and impact of the “parallel line” of national telescopes, the mission of ESO and the impact of the organisation as a maecenas to European astronomy. With specific focus on the foundation of A & A as a refereed journal foregoing page charges, the support of national telescopes of all classes, the allotment of telescope time on the sole basis of proposal quality, the free travel and technical support, the free distribution of “The Messenger”, the development and free distribution of MIDAS, and the personal dedication of some early foster persons.     

观测天体光谱的纤维光学方法及2.16m望远镜实用系统

本文描述了近年来广泛发展起来的天体物理实测技术中的一项重要进展——纤维光学分光技术方法在天体光谱观测中的应用及2.16m望远镜实用系统的特点和初步应用结果     

Past and future of ESO

In 1964, the European Southern Observatory (ESO) came into being as a response to the need of European astronomers for access to large telescopes in good observing conditions. The original plan called for a 3.6 m telescope in addition to a number of smaller instruments. The 3.6 m telescope took some 12 years to build, while ESO headquarters moved from Hamburg to CERN to Garching near Munich, and during the times of office of three Directors General, and it was built on La Silla in Chile, where superior sites had been found. After 1982, when Italy and Switzerland joined the original six member countries, ESO was able to expand by building the 3.5 m New Technology Telescope, and ultimately planning and constructing the VLT on Paranal. At present ESO is a stable organization that has been successful in its original aims, and in view of new plans can look forward in confidence.     

Characteristics of small-sized space debris objects using Terskol observatory measurements

The Zeiss-2000 telescope of the International Center for Astronomic and Medico-Ecological Research, National Academy of Sciences of Ukraine (Terskol observatory), with a 2-meter aperture is the largest optical instrument in Europe that is regularly used for investigating space debris in the vicinity of the geostationary orbit. One of the main objectives is to detect and characterize small fragments of space debris that are difficult to approach for other telescopes. During each photometric night, we usually detect four to five unknown fragments of 17th to 20th magnitude. This article provides orbital parameters and physical characteristics of several small-sized fragments of space debris that were detected during observations at Terskol observatory in 2014–2015.     

基于光学辅助指向测量的太赫兹望远镜指向误差模型研究

针对太赫兹波段天文点源目标较少, 指向测量相对困难的特点, 研究了利用与太赫兹天线共轴的小型光学望远镜来辅助太赫兹望远镜指向测量以及建立指向误差修正模型的方法. 依托紫金山天文台1.2 m斜轴式太赫兹天线开展了光学辅助指向测量的实验研究, 利用一台安装在天线背架上的100mm口径折射式光学望远镜获得了优于2$''$的指向测量精度. 此外, 通过对斜轴天线的结构分析以及大气折射和本地恒星时(Local Sidereal Time, LST)偏差等误差来源的分析, 建立了包含23个误差项的斜轴式光学指向修正模型, 实现了约3$''$的拟合精度. 最后, 借助高精度数字摄影测量对光电轴一致性进行了标定, 并针对其对指向模型精度的影响进行了讨论. 研究成果将为南极5 m太赫兹望远镜(The 5m Dome A Terahertz Explorer, DATE5)及其他太赫兹望远镜提供指向测量和指向修正模型方面的技术参考.     

Toward high spatial resolution in solar observations

To achieve high spatial resolution capability for IR solar observations, we suggest the use of a special mask placed before the entrance aperture of large conventional optical telescopes. Such a mask would match well the resolution of a non-redundant array and would provide safe operation of a large telescope used for solar observations. The proposed solution has the additional advantage of relatively low cost because already-existing optical telescopes are used.     

天文高分辨像复原技术检测地基天文光学望远镜成像质量

在天文高分辨像复原技术的基础上，根据谱比法较准确地测量视宁度参数r0后，计算得到大气系统的平均短曝光传递函数，从而把大气湍流对检测结果的影响从综合成像系统中分离了出来。利用望远镜摄取大量目标源的短曝光像(斑点图)作为原始数据，通过分析这些含有望远镜衍射极限分辨率信息的斑点图，实现天文光学望远镜系统点扩展函数(PSF)中低频信息的重建，得到半峰全宽(FWHM)和80％的能量集中度(EE)。     

A novel design for a giant Arecibo-type spherical radio telescope with an active main reflector

A novel design for a giant spherical radio telescope is proposed. Instead of a fixed spherical reflecting surface such as with the 305-m Arecibo telescope, the illuminated portion of the reflecting surface is made to fit a paraboloid of revolution in real time by active control. A simple feed can thus be used, enabling the realization of broad bandwidth and full polarization. The actual design utilizes a karst depression which gives a spherical surface of 300-m radius, having an opening of 500-m diameter. The illuminated aperture is chosen to be 300 m, and the focal ratio is 0.46–0.48. With this geometry and the simple feeding system, a giant telescope with large sky coverage can be achieved at low cost. When the illuminated aperture is limited to 70–100 m, the area trackable can be extended to about 10° above the horizon.     

The NST: First results and some lessons for ATST and EST

In January 2009, first light observations with the NST (New Solar Telescope) in Big Bear Solar Observatory (BBSO) were made. NST has a 1.7 m primary with a 1.6 m clear aperture. First observational results in TiO and Hα are shown and discussed. The NST primary mirror is the most aspheric telescope mirror deployed to date. The NST is early in its commissioning, and the plans for this phase will be sketched. Lessons learned in building and implementing the NST are germane for the ATST and EST telescopes and will be discussed. The NST has an off‐axis Gregorian configuration consisting of a parabolic primary, heat‐stop, elliptical secondary and diagonal flats. The focal ratio of the primary mirror is f/2.4. The working wavelength range covers from 0.4 to 1.7 µm in the Coudé Lab beneath the telescope and all wavelengths including the far infrared at the Nasmyth focus on the dome floor (© 2010 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

The beginnings, from Lipperhey to Huygens and Cassini

The first century of telescopic astronomy can be divided into two periods. During the first, from 1609 to ca. 1640, observations were made with a simple “Dutch” or “Galilean” telescope with a concave eyepiece. Galileo made all his discoveries with this instrument. Its limited field of view, however, made magnifications of more than about 20 impractical, and therefore this instrument’s limit had been reached within a few years. During the second period, ca. 1640–ca. 1700, the simple astronomical telescope came into use, almost immediately augmented with a field lens and an erector lens (the latter used only for terrestrial purposes). Magnifications were increased by increasing the focal lengths of objectives, and this quickly led to very long telescopes, often used without a tube. The astronomical discoveries made possible by this form of the instrument were, however, made with instruments of relatively modest lengths. By the end of the century, very long telescopes fell out of use, while shorter ones were adapted for measurements. Further discoveries became possible only with the reflecting telescope in the second half of the eighteenth century.     

Statistical estimates of fundamental constraints on the use of commercial CCD cameras in TV guide systems of large optical telescopes

The parameters of TV guide cameras of the BTA and Zeiss-1000 telescopes are analyzed. The formation of optical images by the “atmosphere + telescope” system is analyzed with allowance for the laws of photoelectron statistics in order to justify the applicability of commercial CCD cameras in the guiding systems of large optical telescopes. The analysis focuses on the estimates of fundamental constraints imposed on the method of TV observations of the sky through a turbulent atmosphere. The possible ways of reducing the main constraining factors in the case of the use of highly sensitive commercially produced CCDs in TV guide cameras are outlined.     

Re-testing the JET-X Flight Module No. 2 at the PANTER facility

The Joint European X-ray Telescope (JET-X) was the core instrument of the Russian Spectrum-X- γ space observatory. It consisted of two identical soft X-ray (0.3–10 keV) telescopes with focusing optical modules having a measured angular resolution of nearly 15 arcsec. Soon after the payload completion, the mission was cancelled and the two optical flight modules (FM) were brought to the Brera Astronomical Observatory where they had been manufactured. After 16 years of storage, we have utilized the JET-X FM2 to test at the PANTER X-ray facility a prototype of a novel X-ray polarimetric telescope, using a Gas Pixel Detector (GPD) with polarimetric capabilities in the focal plane of the FM2. The GPD was developed by a collaboration between INFN-Pisa and INAF-IAPS. In the first phase of the test campaign, we have re-tested the FM2 at PANTER to have an up-to-date characterization in terms of angular resolution and effective area, while in the second part of the test the GPD has been placed in the focal plane of the FM2. In this paper we report the results of the tests of the sole FM2, using an unpolarized X-ray source, comparing the results with the calibration done in 1996.     

The Spectrum-UV Mission: an International Ultraviolet Observatory

The Spectrum-UV Mission is an ultraviolet space observatory, scheduled to be launched at the break of the century into a 7-day, highly excentric orbit aboard a Spectrum Series platform. The Observatory is endowed with a 170-cm aperture telescope and a focal plane instrument complement for spectroscopy and imaging in the 912 to 3600 range. The results of an advanced feasibility study, being carried out in the four partecipating Countries (Germany, Italy, Russia and Ukraine) are presented.