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《天文学报》2017,(2)
云对天文观测具有重要影响,云量是衡量天文台址质量的重要指标.位于姚安天文观测站的红外云量仪,用于获取实时的全天高空间分辨率云图.结合空间碎片的实际观测,严格按照天文夜对累积1yr(2015-08-01—2016-07-31)的夜间云量数据进行统计和分析.姚安站的年平均夜间云量为4.42成,年天文可用夜为236个,其中测光夜98个,半测光夜44个,光谱夜94个.云量具有明显的两季特征:5月至10月间为雨季,云量显著增多,其中7月份观测条件最差;11月至次年4月为旱季,云量较少,每月的天文可用夜均在23个以上,其中1月份的测光夜最多,3月份的天文可用夜最多.结合云层对天文观测的威胁程度,统计不同云量的总时间和每月的云量分布情况,评估观测站的气象条件,为合理安排观测计划提供参考. 相似文献
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《天文学进展》2017,(3)
台址信息监测系统是现代天文观测台站必备的辅助系统之一,在开展天文实测过程中发挥着重要的作用。首先介绍了丽江天文观测站的基本概况,目前己经投入运行的天文望远镜设备,以及丽江2.4 m通用光学望远镜上配备的科学终端仪器。随后论述了国内外优秀天文观测台站己配备的台址信息监测设备,重点阐述了丽江天文观测站建立的台址信息监测系统。分析了丽江站一个年度的气象数据、云量数据、可观测小时数、可观测夜数和天光背景数据,以及近几年测量的大气视宁度数据,得出丽江站全年的光学天文观测条件的基本特征。根据实际观测情况,将丽江2.4 m望远镜全年的观测时间段分为三个等级,为国内天文学家申请使用并开展科学观测提供参考。 相似文献
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天文观测站夜天空星像星等信息和天区分布信息可用于指导多设备巡天观测.建立全天相机监测系统(Monitoring all-sky system)对本地天区夜天空实时监测,获取的监测图像需要有效的方法进行处理以提取全天图像星像信息.由于全天图像视场大和高阶扭曲的影响,采用天顶等距投影与多项式函数组合的方法计算图像的底片常数.天文定位的均方根残差约为0.15个像素.通过对图像中亮星部分测光得到的星等差,改正大气消光误差.最后使用HEALPix (Hierarchical Equal Area isoLatitude Pixelation)方法实现天区划分和每个天区可观测极限星等值的存储. 相似文献
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宗伟凯 付建宁 牛家树 AshleyMichaelCB 宫雪非 LawrenceJS 刘强 Luong—VanDaniel PennypackerCR StoreyJohnWV 王灵芝 王力帆 杨惠根 袁祥岩 YorkDonaldG 朱镇熹 《云南天文台台刊》2014,(1):89-94
天光背景是天文台址的一个重要指标。利用2009年位于南极冰穹A的CSTAR望远镜两个波段的观测数据,对南极冰穹A的天光背景进行了统计和分析。结果表明约74%的g波段天光背景的ADU值小于每像素100/s;90.5%的r波段的天光背景的ADU值小于每像素100/s。在不考虑大气消光的情况下,定标后的结果为2009年冰穹A的观测数据中天光背景亮度的中值:g波段为19.9mag/arcsec^2,r波段为20.1mag/aresec^2。 相似文献
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介绍一种利用大视场测光系统对观测天气质量进行评估的统计方法.此方法可以 给出大气透明度、背景天光、视宁度和观测极限星等等多种与天文观测有关的天气质 量参数.通过检验证明,此方法可提供一个天气状况的实时监视方法,对北京天文台 施密特CCD测光系统以及制定观测计划和评估观测质量有重要意义. 相似文献
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首架南极天文望远镜CSTAR的光学系统 总被引:1,自引:0,他引:1
2008年1月中国自行研制的首台南极小望远镜阵CSTAR成功安装在南极内陆最高点DOME A,用于天文观测.正如天文学家预言,南极是个极好的天文台址,CSTAR传回的清晰图像,为我们进一步证实了在南极展开天文科考的可能性与优越性.在此重点介绍我国首台南极望远镜设备CSTAR的光学系统,以及为保证在南极低温环境下望远镜保持高质量成像所采取的措施,最后给出观测结果. 相似文献
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J.W.V.Storey 《天文学报》2006,47(4):407-409
南极洲高原的天文开发在过去的10年中有了显著的进展.大的天文设施已在南极(South Pole)的Amundsen-Scott站运行,更具威力的望远镜已在计划或正在那儿建设,然而由于一些重要的原因,高原站址冰穹A(Dome A)和冰穹C(Dome C)对多种天文学科似乎比南极更具有利条件.2005年1月中国对冰穹A的成功考察,加上2005年以整年运行为目的的法/意Concordia站在冰穹C的开启,已为南极洲天文学创造了激动人心的新机遇. 相似文献
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Pei Chong Yuan Xiang-Yan Chen Hua-Lin Zhao Jian-Lin WEN Hai-Kun Li Zheng-Yang 《Chinese Astronomy and Astrophysics》2012
The Antarctic site-testing campaigns have shown that Dome C is an excellent astronomical site on the earth, it is better than any of existing mid-latitude astronomical sites in the world, because of its cold and dry weather, low infrared background radiation, continuously observable time as long as 3–4 months, clear and highly transparent atmosphere, low wind speed, and the absence of dust and light pollution. And in the international astronomical community it is generally believed that Dome A with a higher altitude may be better than Dome C as a potential excellent astronomical site. In the past 3 years, although held by the Center for Antarctic Astronomy of Chinese Academy of Sciences, the site testing at Dome A has preliminarily con?rmed the many advantages of Dome A as an excellent astronomical site, but the data about the atmospheric seeing, which is an important parameter for assessing the site quality for optical observations, have not been obtained until now. Hence, on the basis of a commercial telescope with the diameter of 35 cm, we have made the hardware reformation and software development to have it operate as a DIMM (Differential Image Motion Monitor), which can simultaneously monitor both the seeing and isoplanatic angle at Dome A automatically. At present this instrument has been shipped to Antarctica by the “Xuelong” exploration ship, and will be installed at Dome A, and begin to work in early 2011. Before the shipment, by through the comparative measurements together with an existing seeing monitor at the Xinglong astronomical station, the software, hardware, as well as the installation and adjustment of the instrument, are further veri?ed by testing. 相似文献
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根据1994年6月—1995年12月期间在新疆天山南坡的奎先达坂进行的云量观测结果和邻近的巴仑台气象站的多年气候观测资料作统计分析,作者推断奎先达坂的天文可用小时数和天文夜数均可与目前世界上最优良的天文台址相比。 相似文献
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Michael G. Burton 《Astronomy and Astrophysics Review》2010,18(4):417-469
Antarctica provides a unique environment for astronomers to practice their trade. The cold, dry and stable air found above
the high Antarctic plateau, as well as the pure ice below, offers new opportunities for the conduct of observational astronomy
across both the photon and the particle spectrum. The summits of the Antarctic plateau provide the best seeing conditions,
the darkest skies and the most transparent atmosphere of any earth-based observing site. Astronomical activities are now underway
at four plateau sites: the Amundsen-Scott South Pole Station, Concordia Station at Dome C, Kunlun Station at Dome A and Fuji
Station at Dome F, in addition to long duration ballooning from the coastal station of McMurdo, at stations run by the USA,
France/Italy, China, Japan and the USA, respectively. The astronomy conducted from Antarctica includes optical, infrared,
terahertz and sub-millimetre astronomy, measurements of cosmic microwave background anisotropies, solar astronomy, as well
as high energy astrophysics involving the measurement of cosmic rays, gamma rays and neutrinos. Antarctica is also the richest
source of meteorites on our planet. An extensive range of site testing measurements have been made over the high plateau sites.
In this article, we summarise the facets of Antarctica that are driving developments in astronomy there, and review the results
of the site testing experiments undertaken to quantify those characteristics of the Antarctic plateau relevant for astronomical
observation. We also outline the historical development of the astronomy on the continent, and then review the principal scientific
results to have emerged over the past three decades of activity in the discipline. These range from determination of the dominant
frequencies of the 5 min solar oscillation in 1979 to the highest angular scale measurements yet made of the power spectrum
of the CMBR anisotropies in 2010. They span through infrared views of the galactic ecology in star formation complexes in
1999, the first clear demonstration that the Universe was flat in 2000, the first detection of polarization in the CMBR in
2002, the mapping of the warm molecular gas across the ~ 300 pc extent of the Central Molecular Zone of our Galaxy in 2003,
the measurement of cosmic neutrinos in 2005, and imaging of the thermal Sunyaev Zel’dovich effect in galaxy clusters in 2008.
This review also discusses how science is conducted in Antarctica, and in particular the difficulties, as well as the advantages,
faced by astronomers seeking to bring their experiments there. It also reviews some of the political issues that will be encountered,
both at national and international level. Finally, the review discusses where Antarctic astronomy may be heading in the coming
decade, in particular plans for infrared and terahertz astronomy, including the new facilities being considered for these
wavebands at the high plateau stations. 相似文献
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Xu Zhou Zhen-Yu Wu Zhao-Ji Jiang Xiang-Qun Cui Long-Long Feng Xue-Fei Gong Jing-Yao Hu Qi-Sheng Li Gen-Rong Liu Jun Ma Jia-Li Wang Li-Fan Wang Jiang-Hua Wu Li-Rong Xia Jun Yan Xiang-Yan Yuan Feng-Xiang Zhai Ru Zhang Zhen-Xi Zhu National Astronomical Observatories Chinese Academy of Sciences Beijing China Nanjing Institute of Astronomical Optics & Technology National Astronomical Observatories Nanjing China Purple Mo... 《中国天文和天体物理学报》2010,10(3)
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This article examines the use of Laser Beacons for daytime astronomical observations. There are two potential applications: the diffraction limited observation of (1) the structure in the solar corona at all wavelengths, and (2) non-solar astronomical objects in the thermal infrared part of the spectrum. We examine the brightness of the Laser Beacon required as well as the limitations imposed by the daytime sky brightness and sky/telescope thermal emission on the observable magnitude limits. For both applications the use of Laser Beacon adaptive optics in daytime results in important research opportunities. 相似文献
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Li Zhen-qiang Li Ji-bin Zhang Xu-guo Shan Wen-lei Xu Ye Zuo Ying-xi Zhang Hai-long Jin Feng-juan Sun Ji-xian Lu Deng-rong Ju Bing-gang 《Chinese Astronomy and Astrophysics》2019,43(4):590-608
In astronomical observations, the radio frequency interference (RFI) will cause pseudo spectra and reduce the reliability and validity of observational data. The RFI mitigation, which includes many technical innovations of devices and the method studies of data processing, aims at reducing the influence of RFI on the radio astronomical observation. Various efforts were made to improve the anti-RFI capability of the multi-beam receiver (Superconducting Spectroscopic Array Receiver, SSAR) of the Delingha 13.7 m telescope. The interference transmission path was analyzed. The concepts of the device RFI direct coupling coefficient and the device RFI system coupling coefficient were proposed. The proportions of interference introduced in the receiver system by the different devices were quantified, and the interference-susceptible devices in the system were located. After the anti-RFI treatment of the interference-susceptible devices, the anti-RFI capability of the receiver system is improved by 30 dB in average, and the astronomical observation efficiency of the telescope is increased by more than 10%. 相似文献