Measurements of electronic properties of the Miyun 50 m Radio Telescope

Zhang, Xizhen; Zhu, Xinying; Kong, Deqing; Zheng, Li; Yao, Chuanhao; Zhang, Hongbo; Su, Yan; Piao, Tingyi

doi:10.1088/1674-4527/9/3/011

Cited by 11 publications

(10 citation statements)

References 10 publications

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“…迄今为止, 诺贝尔物理学奖中有 6 项是射电天文学的成就, 如 1962 年的 Ryle [7] 建造了世界上第一台综合孔径望远镜, 获得 1974 年诺贝尔物理学奖. 这个阶段国外又陆续建成了一批大型米波和厘米波射电望远镜, 其最具代表性的是单口径大型射电望远镜, 主要包括澳大利亚 Parkes [8] (64 m)、英国 Jordrell Bank [9] (76 m)、德国 Effelsberg [10] (100 m)、美国 Green Bank [11] (100 m) 和 Arecibo [12] (305 m) 望远镜等, 国内具有代表性的包括青海德令哈 13.7 m 毫米波射电望远镜 [13] 、上海天马 65 m 射电天文望远镜 [14] 、云南昆明凤凰山 40 m 射电望远镜 [15] 、北京密云 50 m 综合孔径射电望远镜 [16] , 以及贵州正在建设的 FAST--世界最大单口径射电望远镜 [17] , 直径 500 m. 上述射电天文装置大部分都是基于单口径抛物面形式.…”

Section: 国内外射电望远镜发展趋势unclassified

世界最大综合孔径望远镜ska低频数字阵列系统研究

ManQing¹,

Cao²,

Tao³

et al. 2015

Sci. Sin.-Inf.

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关键词射电天文望远镜平方公里阵数字阵列技术低频孔径阵列子阵处理模块 100 万支天线单元的低频孔径阵列 (low frequency aperture array, LFAA)、2500 面抛物面天线 (dishes) 阵列以及中频孔径阵列 (mid-frequency aperture array, MFAA) 组成, 分布在 3000 公里基线内形成望远镜阵列, 其中 LFAA 采用稀疏布阵方式, MFAA 采用致密布阵方式 (布阵方式请参考 SKA 官网 1)). SKA 将致力于回答宇宙最基本的问题, 使人类更好地理解所生活的宇宙 [2]. SKA 的概念提出是在 1991 年, 计划于 2024 年建成投入运行, 其中 2013∼2017 年为建设准备阶段 [3] , 也是 SKA 整个生命周期中最重要阶段, 这一阶段的初步设计评审 (preliminary design review, PDR) 和关键设计评审 (critical design review, CDR) 也是项目中最重要的里程碑节点 [4]. 孔径阵列与空间探测安徽省重点实验室 (KLAASA) 的中低频孔径阵列课题组依托中国电子科技集团公司第三十

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Section: 国内外射电望远镜发展趋势unclassified

世界最大综合孔径望远镜ska低频数字阵列系统研究

ManQing¹,

Cao²,

Tao³

et al. 2015

Sci. Sin.-Inf.

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“…Since the errors are relatively small, the final pointing deviation is the algebraic sum of all these partial deviations in the linear calibration model. The widely used pointing calibration models are constructed as (Zhang et al 2009)…”

Section: A Linear Model For Pointing Calibrationmentioning

confidence: 99%

“…Quite a few engineers introduced the principle and method of acquiring a pointing calibration of a telescope (Meeks et al 1968;Yuan et al 1986;Himwich 1993). A linear calibration model is applied in the software that calculates the pointing calibration of most large radio telescopes (Zhang et al 2009;Meeks et al 1968;Yuan et al 1986). Based on pointing measurements using radio sources whose precise locations are known, the pointing errors of the whole sky area are obtained, and the model parameters are identified by using the method of least squares.…”

Section: Introductionmentioning

confidence: 99%

A new calibration model for pointing a radio telescope that considers nonlinear errors in the azimuth axis

Kong¹,

Song-gen²,

Wang³

et al. 2014

Res. Astron. Astrophys.

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A new calibration model of a radio telescope that includes pointing error is presented, which considers nonlinear errors in the azimuth axis. For a large radio telescope, in particular for a telescope with a turntable, it is difficult to correct pointing errors using a traditional linear calibration model, because errors produced by the wheel-on-rail or center bearing structures are generally nonlinear. Fourier expansion is made for the oblique error and parameters describing the inclination direction along the azimuth axis based on the linear calibration model, and a new calibration model for pointing is derived. The new pointing model is applied to the 40m radio telescope administered by Yunnan Observatories, which is a telescope that uses a turntable. The results show that this model can significantly reduce the residual systematic errors due to nonlinearity in the azimuth axis compared with the linear model.

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“…For large telescopes, pointing calibration needs to be carried out first (Meeks et al 1968;Yuan et al 1986;Himwich 1993). The linear calibration model is applied in the pointing calibration of mostly large radio telescopes (Meeks et al 1968;Yuan et al 1986;Zhang et al 2009). However, the linear model does not take the structure nonlinear errors into considerations.…”

Section: Introductionmentioning

confidence: 99%

The New Wuqing 70 m Radio Telescope and Measurements of Main Electronic Properties in the X-band

Kong¹,

Li²,

Su³

et al. 2022

Res. Astron. Astrophys.

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The new Wuqing 70 m radio telescope is firstly used for the downlink data reception in the first Mars exploration mission of China, and will be used for the other deep space communications and radio astronomical observations in the future. The main specifications and measurement results of some properties in X-band are introduced in this paper, such as pointing calibration, gain and efficiency, system noise temperature, system equivalent flux density, and variations with elevation. The 23 parameters pointing calibration model considering the atmospheric refraction correction in real time is presented in the telescope, and the pointing accuracy is reached 5.70″ in azimuth direction and 6.07″ in elevation direction respectively for different weather condi-tions. More than 62% efficiencies are achieved at full elevation range, and more than 70% in the mid-elevation. The system equivalent flux density of X-band in the mid-elevation is reached 26 Jy.

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Measurements of electronic properties of the Miyun 50 m Radio Telescope

Cited by 11 publications

References 10 publications

世界最大综合孔径望远镜ska低频数字阵列系统研究

世界最大综合孔径望远镜ska低频数字阵列系统研究

A new calibration model for pointing a radio telescope that considers nonlinear errors in the azimuth axis

The New Wuqing 70 m Radio Telescope and Measurements of Main Electronic Properties in the X-band

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