共查询到20条相似文献，搜索用时 93 毫秒
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2008年3月20-22日,东亚VLBI研讨会(East Asia VLBI Workshop)在中国科学院上海天文台召开.共76位代表注册参加了会议,他们分别来自澳大利亚(1人)、韩国(10人)、日本(19人)和中国(46人). 相似文献
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将不同波段的星表、特别是巡天项目产生的大型星表进行交叉证认,一直是进行多波段天文学研究,尤其是数据挖掘、统计分析研究的瓶颈.本文开发和实现了一个不依赖于特定数据库的海量星表融合系统(简称为XMaS_VO),用户能够方便地使用此系统的服务进行星表的上传及自动入库、交叉证认等工作.此外,XMaS_VO具备可移植性,如果用户需要进行很大数量的或者大型星表的交叉证认服务,可以自己建立数据库,方便地将此工具移植到自己的服务器上,自己使用或者开放服务给他人.随着该系统的进一步发展和应用.天文学家将可以轻松自如地获得他们需要的多波段融合数据,自由地选取参数和匹配的结果.从而可以更加有效地从事海量数据处理和分析工作. 相似文献
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一种扩大FAST视场的方法 总被引：1，自引：0，他引：1
所有的大口径射电望远镜都存在这样一个问题：在其分辨率和灵敏度提高的同时，视场变小．而且口径越大，视场越小．这成为大口径望远镜不可回避的矛盾．要解决这个矛盾，可以在望远镜的焦平面上放置Ⅳ个分立馈源．让它们同时工作，这样可以看作把视场扩大了Ⅳ倍．望远镜的工作效率提高Ⅳ倍．但是这样做的缺点是——视场不连续．且馈源数目Ⅳ受到望远镜焦比(F／D)的限制．采用致密焦面阵(dense focal plane array)就可以很好地解决这个问题．致密焦面阵的单元不是喇叭口天线，而是无方向性的Vivaldi天线(Vivaldi antenna)．要把Vivaldi阵列应用到望远镜上，需要对单个Vivaldi天线和Vivaldi阵列的电性能有清楚的认识，并能根据需要来设计照明方向图．还要知道大望远镜的焦面上电磁场的分布情况，借此判断能否应用Vivaldi阵列，以及给出Vivaldi单元的分路赋权网络．主要给出了FAST的焦面场的分布情况．并说明应用Vivaldi阵列的可能性． 相似文献
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高电子迁移率晶体管(HEMT)目前被广泛应用于高灵敏度(低噪声)射电天文接收机中. 在低温制冷环境下,其低噪声性能更佳,但对偏置供电系统要求很高,只有在特定的偏置条件下才能得到最佳的低噪声、高增益、高稳定性.本文提供了一套可调试、高稳定、高可靠性、带远程监控功能的可供多级低温制冷HEMT管的偏置电源的设计思路、方法和制作,使在低温制冷状态下的HEMT管能够稳定、安全、可靠地工作在最佳状态. 相似文献
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云南天文台1m红外太阳望远镜是多功能、多波段的太阳望远镜,望远镜使用过程中主镜的热变形直接关系这系统的光学精度,建立光学系统的光机热结合的分析方法,可以直观的得到热辐射对光学系统的影响结果,使得望远镜的设计阶段就能评估热变形对系统的精度影响,确定光学元件是否满足要求. 相似文献
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Zhen-Xing Fu Chandreyee Sengupta Ramya Sethuram Bikram Pradhan Mridweeka Singh Kuntal Misra TomCScott Yin-Zhe Ma 《天文和天体物理学研究(英文版)》2021,(2):149-156
We present results from our Giant Metrewave Radio Telescope(GMRT)HⅠ,Himalayan Chandra Telescope(HCT)Hα,1 m Sampurnanand Telescope(ST)and 1.3 m Devasthal Fast Optical Telescope(DFOT)deep optical observations of the NGC 7805/6(Arp 112)system to test KUG 2359+311’s tidal dwarf galaxy(TDG)candidacy and explore the properties of the interacting system.Our GMRT HⅠmap shows no HⅠdetection associated with KUG 2359+311,nor any HⅠtail or bridge-like structure connecting KUG 2359+311 to the NGC 7805/6 system.Our HCT Hαimage,on the other hand,displays strong detections in KUG 2359+311,with net SFR0.035±0.009 M⊙yr-1.The Hαdata constrain the redshift of KUG 2359+311 to 0.00≤z≤0.043,compared to the redshift of NGC 7806 of0.015.TDGs detected to date have all been HⅠrich,and displayed HⅠ,ionised gas and stellar tidal debris trails(bridges or tails)linking them to their parent systems.However,neither our HⅠdata nor our optical imaging,while three magnitudes deeper than SDSS,reveals a tidal trail connecting KUG 2359+311 to NGC 7805/6.Lack of HⅠ,presence of an old stellar population,ongoing star formation and reasonably high SFR compared to normal dwarf galaxies suggest that KUG 2359+311 may not be an Arp 112 TDG.It is most likely a case of a regular gas-rich dwarf galaxy undergoing a morphological transformation after having lost its entire gas content to an interaction with the Arp 112 system.Redshift and metallicity from future spectroscopic observations of KUG 2359+311 would help clarify the nature of this enigmatic structure. 相似文献
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通过对新月和满月夜期间测光夜数和云量统计数的比较, 高美古的天文测光夜数和可用夜数与丽江县的气象晴日数的比较, 以及在同样的观测时间高美古和丽江县云量观测值的比较, 本文对高美古选址云量观测可靠性的有关方面进行了讨论 相似文献
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鉴于分子天文学对研究银河系结构、恒星诞生和演化、宇宙化学及宇宙生命等方面有极其重要的意义,近年来国内不仅在这个领域的理论研究有迅速发展,而且积极进行着实测手段的建设.其中,用于谱线观测的射电频谱仪先后确定采用的数种技术方案,均已进行研制并已在实验室调测.然而因种种技术上的考虑,原来并没有打算采用国外已广泛使用的全数字化自相关射电频谱仪. 相似文献
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This paper reports on an observation of the appulse of (146) Lucina with AGK3 + 17° 1309 made on April 18, 1982, at the Meudon Observatory in France. During this observation a secondary event occurred and was recorded. A Nocticon camera mounted on the 1-m telescope and video equipment was used. This equipment is well adapted to these observations primarily because astrometric and photometric reductions are possible. Furthermore no diaphragm is necessary in contrast to classical photometry, and this reduces the possibility of generating artifacts. The Meudon observation is described. Observational data from other sites have been collected, and have confirmed that the short extinction observed at Meudon was not due to the asteroid itself. A possible interpretation is the existence of a faint satellite in the neighborhood of (146) Lucina. The observation leads to a diameter of at least 5.7 km and a projected distance of 1600 km from the primary. 相似文献
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1 ＳｉｇｎｉｆｉｃａｎｃｅｏｆＳｏｌａｒＳｔｏｋｅｓＳｐｅｃｔｒｕｍＯｂｓｅｒｖａｔｉｏｎＤｕｅｔｏｔｈｅｄｅｖｅｌｏｐｍｅｎｔｉｎｏｂｓｅｒｖｉｎｇｉｎｓｔｒｕｍｅｎｔ,ｔｈｅｃｏｎｃｅｐｔｏｆｓｏｌａｒｓｐｅｃｔｒｕｍｓｈｏｕｌｄｂｅｇｅｎｅｒａｌｉｚｅｄ .Ｉｎｔｈｅｐａｓｔ,ｉｔｉｓｏｎｌｙａｓｓｉｇｎｅｄｔｏｔｈｅｏｒｄｉｎａｒｙｏｒｕｎｐｏｌａｒｉｚｅｄｓｐｅｃｔｒｕｍｒｅｃｏｒｄｉｎｇｔｈｅｗａｖｅｌｅｎｇｔｈ ｄｉｓｔｒｉｂｕｔｅｄｉｎｔｅｎｓｉｔｙｏｆｔｈｅｃｏｎｔｉｎｕｕｍａｎｄ… 相似文献
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本文从日冕观测和研究的意义出发，叙述了用外遮档及小孔减光测量日晕光度的方法以及在云南和新疆若干选点的初步观测结果。 相似文献
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The results of positional observations of near earth asteroids using the combined observation method
Ye. S. Sybiryakova Ye. S. Kozyryev A. V. Shulga 《Bulletin of the Crimean Astrophysical Observatory》2013,109(1):66-70
The high velocity of the apparent motion of near Earth asteroids (NEAs) is the main problem in their observation. This problem is solved at the Research Institute Nikolaev Astronomical Observatory (RI NAO) with a combined observation method using the time delay and integration mode of a CCD array and a camera rotator. A total of 1317 positions of 74 NEAs were obtained at RI NAO in 2008–2012. All the observations were made using the combined-observation method. The error in observations made at RI NAO is compared with the results that were obtained at other observatories in this work. 相似文献
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天马望远镜是目前亚洲最大的全方位可转动的射电望远镜。连续谱观测对于天马望远镜具有重要意义。主要介绍天马望远镜连续谱观测系统的相关信息及其实现情况,包括:天马望远镜连续谱观测的过程、天马望远镜连续谱观测系统的硬件和软件系统的组成,以及连续谱观测系统的测试观测结果。在C波段6.5 GHz的观测结果表明:连续谱观测系统可实现单点观测和成图观测。修正后指向误差的平均值为2.2″,均方根误差为4.3″。目前该系统已用于天马望远镜的连续谱观测,取得了较好的结果,验证了系统的有效性。 相似文献
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F.-X. Désert A. Benoit S. Gaertner J.-P. Bernard N. Coron J. Delabrouille P. de Marcillac M. Giard J.-M. Lamarre B. Lefloch J.-L. Puget A. Sirbi 《New Astronomy》1998,3(8):1073-669
We report on the first observation of the Sunyaev–Zel'dovich (SZ) effect, a distortion of the Cosmic Microwave Background radiation (CMB) by hot electrons in clusters of galaxies, with the Diabolo experiment at the IRAM 30 m telescope. Diabolo is a dual-channel 0.1 K bolometer photometer dedicated to the observation of CMB anisotropies at 2.1 and 1.2 mm. A significant brightness decrement in the 2.1 mm channel is detected in the direction of three clusters (Abell 665, Abell 2163 and CL0016+16). With a 30 arcsec beam and 3 arcmin beamthrow, this is the highest angular resolution observation to date of the SZ effect. Interleaving integrations on targets and on nearby blank fields have been performed in order to check and correct for systematic effects. Gas masses can be directly inferred from these observations. 相似文献