大射电望远镜馈源系统精调平台位置基准标定

Stewart并联机构作为大射电望远镜馈源系统的二次精调平台,由于馈源舱体的运动特性,精调平台的位置基准在测量坐标系下不断变化.针对大射电望远镜馈源系统精调平台位置基准的实时确定,给出了实用的测量方案及解算模型.在大射电望远镜馈源索支撑系统50 m缩比模型实验中得以应用.     

FAST射电望远镜天文轨迹规划

针对我国500 m球面射电望远镜天线(FAST),提出了一体化天文轨迹规划;给出了详细的数学模型及推导分析。相对于当前采用的FAST轨迹规划,该方法使得馈源位置和反射面位置的控制误差可以相互补偿。指出当馈源系统和反射面系统具有相同的测控延迟误差时,并不影响FAST天线的性能。     

FAST射电望远镜天文轨迹规划

针对我国500 m球面射电望远镜天线(FAST),提出了一体化天文轨迹规划;给出了详细的数学模型及推导分析.相对于当前采用的FAST轨迹规划,该方法使得馈源位置和反射面位置的控制误差可以相互补偿.指出当馈源系统和反射面系统具有相同的测控延迟误差时,并不影响FAST天线的性能.     

FAST高精度基准控制网测量方案优化

500m口径球面射电望远镜(FAST)台址中的23个基准墩是工程的重要组成部分,它主要为FAST建设、运行过程中馈源及反射面的精密、动态位姿测量提供精密的点位坐标基准。文中主要对基准墩所构成的大地基准控制网(平面网)进行测量方案设计,并进行了相应的精度估算。按照本设计方案,可以达到FAST工程所制定标校基准控制网中误差优于0.3mm,整体基准控制网中误差优于1.0mm的设计要求,同时文中方案在具体实施过程中经验证是可行的。     

FAST与近代大型射电望远镜介绍

主要介绍射电望远镜的起源，当代射电望远镜的理论及建造技术如主反射面和馈源支撑技术的发展，以及在不同领域的应用情况，并对我国正在酝酿的FAST项目所采用的主反射面及馈源支撑技术作为详细的介绍。     

FAST馈源舱精调机构位姿测量系统性能分析

FAST对馈源舱精调机构的位姿测量提出了极高的精度要求。本文介绍了由全站仪组成的精调机构测量系统,计算了全站仪跟踪观测棱镜时的主要观测条件,包括棱镜入射角、观测距离和观测高度角,并进行了棱镜初始指向的优化配置。结果表明,棱镜入射角的最大值约为35°,平均值约为13°~18°,由此产生的测量误差可以忽略;观测距离约为140~350 m,估算全站仪动态测距精度约为2.1~2.4 mm;观测高度角约为0~40°,分布合理,且有利于全站仪的防护。仿真测量结果表明,9个测站的定位精度优于2.5 mm,定姿精度优于360";6个测站的定位精度优于3 mm,定姿精度优于430",均达到精调机构的位姿测量精度要求。     

高铁无砟轨道钢轨精调优化算法

长钢轨应力放散锁定后的轨道精调是确保客运专线无砟轨道几何形位高平顺性的必要阶段。精调作业常通过轨道几何状态测量仪采集轨道三维数据,利用配套精调软件包手动模拟得出调整方案,指导轨道精调。模拟精调中常常反复调整才能使基准轨平顺性达标,自动化程度低。基准轨平顺性满足要求后,仅依靠轨距、轨距变化率、水平和扭曲等参数控制非基准轨,会降低其平顺性。为此,提出利用L₁范数最优原则进行双轨精调的优化算法（optimization algorithm of double-rails track fine adjustment,OADTFA）,建立顾及基准弦端点偏差的平顺性约束,增加非基准轨轨向、高低约束,采用逐点移动基准弦分组调整策略,由单纯形法求解优化调整量。实测数据测试结果表明,OADTFA可实现钢轨自动化精调,确保双轨任意处几何形位高平顺性,自动给出最优左右轨调整量。     

使用参照物的射电望远镜中心坐标测量方法

为满足新建射电望远镜在单站或多站联合进行的深空探测或射电天文观测对中心坐标精确测定的要求,提出一种利用已知精确中心坐标的望远镜作为参照物,测量地平式射电望远镜中心点坐标的方法和测量数据处理方法。这一方法对场地和设备的要求较低,能够得到毫米级或亚毫米级的位置精度。尤其适合对天线阵列的中心位置进行测量。对国家天文台密云观测站的40 m射电望远镜进行了中心坐标测量,位置均方根误差为2.312 mm,满足了后续的观测工作对其位置的需求。     

FAST馈源舱Stewart机构标定

馈源舱系统是FAST工程的核心部件之一。馈源在百米尺度空间内瞬时定位精度要求达到毫米级,因此需要对馈源舱Stewart机构精确标定,以克服加工及装配误差、测量误差、刚度变形以及外界扰动耦合的影响,实现馈源精确定位。本文在分析相关文献对FAST馈源舱研究的基础上,通过对馈源舱Stewart机构标定的实际操作,从测量的角度分析Stewart结构、性能、误差及参数模型等,确定机构标定方案。标定过程包括:规划位姿、用激光跟踪仪实施测量、伺服控制及数据处理等。Stewart机构标定后定位精度显著提高,这对于确保FAST馈源舱空间定位精度有着重要的促进作用。     

佘山13m口径射电望远镜指向扫描数据解析

佘山13 m射电望远镜作为新一代天体测量与空间大地测量甚长基线干涉测量系统,配备有2～14GHz宽频接收机和X/Ka双频接收机。指向精度是射电望远镜性能的重要指标之一,一般要求好于最高配置频率波束宽度的1/10。对于佘山13 m口径射电望远镜,Ka波段32 GHz时的指向精度约为18 as。基于该望远镜的指向扫描实测数据,探讨了指向改正模型建立方法,包括测量功率曲线拟合、积分时间影响分析、指向改正模型参数设置等,实测评估了该望远镜的指向精度。所得指向改正模型可作为系统调试与改进的依据,也是望远镜系统指标测量和观测目标精确跟踪的保障,数据解析模型与分析流程可用于测量系统的日常指向精度检核,也可供类似工程测量参考。     

Automated and continual determination of radio telescope reference points with sub-mm accuracy: results from a campaign at the Onsala Space Observatory

The Global Geodetic Observing System (GGOS) requires sub-mm accuracy, automated and continual determinations of the so-called local tie vectors at co-location stations. Co-location stations host instrumentation for several space geodetic techniques and the local tie surveys involve the relative geometry of the reference points of these instruments. Thus, these reference points need to be determined in a common coordinate system, which is a particular challenge for rotating equipment like radio telescopes for geodetic Very Long Baseline Interferometry. In this work we describe a concept to achieve automated and continual determinations of radio telescope reference points with sub-mm accuracy. We developed a monitoring system, including Java-based sensor communication for automated surveys, network adjustment and further data analysis. This monitoring system was tested during a monitoring campaign performed at the Onsala Space Observatory in the summer of 2012. The results obtained in this campaign show that it is possible to perform automated determination of a radio telescope reference point during normal operations of the telescope. Accuracies on the sub-mm level can be achieved, and continual determinations can be realized by repeated determinations and recursive estimation methods.     

省级地理信息公共服务平台数据体系初步设计

数据体系是地理信息公共服务平台建设的一个重要内容。主要对公共服务平台需求、数据构成及建设等内容进行了描述,为省级地理信息公共服务平台的建设提供参考。     

天球参考系的基本理论和方法研究进展

天球参考系的研究在天体测量、大地测量等研究领域中占有重要的地位。随着配置有CCD的地面光学望远镜和空间望远镜观测精度的不断提高 ,以及其它空间大地测量技术 (VLBI、LLR、SLR和GPS等 )的发展 ,对天球参考系也提出了越来越高的要求。本文从天球参考系的基本理论和方法出发 ,详细地介绍了天球参考系目前的发展状况 ,指出乌克兰里克米亚天文台、上海天文台和IERS在计算河外射电源参考架时采用的小角旋转法公式是错误的 ,并进行了改正     

Impact of network geometry, observation schemes and telescope structure deformations on local ties: simulations applied to Sardinia Radio Telescope

The 64-m Sardinia Radio Telescope (SRT) is currently under construction in Sardinia (Italy). To ensure future surveying and monitoring operations at an utmost level of accuracy, we aim at selecting the optimal design and the most cost-effective solution for the establishment of the local ground control network (LGCN). We simulate and test 45 data sets corresponding to 5 different network configurations. We investigate the influence of 2 LGCN geometries (14 or 8 ground markers) and 3 terrestrial observation schemes (based on redundant forward intersections or side shots) on the precision and accuracy of the conventional reference point (CRP) of SRT and the simulated tie vector with a global navigation satellite system (GNSS) station. In addition, thermal and gravitational deformations of the radio telescope structure are simulated as systematic errors introduced into the observations and their effects on the CRP estimates are quantified. The state-of-the-art of CRP surveying and computation, based on terrestrial indirect methods, is applied. We show how terrestrial indirect methods can estimate the position of the radio telescope CRP to the millimeter precision level. With our simulations, we prove that limiting the LGCN to a 8-point configuration ensures the same precision on the CRP obtained with a 14-point network. Furthermore, we demonstrate that in the absence of telescope deformations, side shots, despite the lower redundancy, preserve a precision similar to that of redundant forward intersections. We show that the deformations due to gravitational flexure and thermal expansion of the radio telescope cannot be neglected in the tie vector computation, since they may bias the CRP estimate by several millimeters degrading its accuracy but not impacting on its formal precision. We highlight the dependency of the correlation matrices of the solutions on the geometry of the network and the observation schemes. Similarly, varying the extent of telescope deformations, we show that the CRP estimate again depends on the combination of the network geometry and the observation schemes.     

佘山25 m与13 m射电望远镜互掩问题分析

应实际工程需要,本文分析了有限场地内两射电望远镜的互掩问题,提出了地平式（方位俯仰座架）射电望远镜外接球面的概念,给出了球冠缺面积的数值积分计算方法,并具体分析和计算了佘山25 m与13 m射电望远镜的互掩,对于工程设计阶段的站点位置选取、塔基高度设计等具有理论参考意义。分析方法也可供类似工程实践参考。     

轻小型惯性稳定平台位置环协同通信控制方法

针对轻小型航空遥感系统对姿态大机动的快响应需求,设计了一种轻量型惯性稳定平台位置环协同通信与姿态超限快响应控制策略,将位置环反馈回路设计为两种可切换工作模式。伺服模式下,参考位置姿态系统的输出,通过设计二者协同通信,保证稳定平台对飞行姿态及扰动的实时隔离;编码器实时监测框架间相对角位置,超限位且载荷视轴与垂直方向误差较大时切换模式。超限快速回复模式下,以编码器值为位置环反馈量,使用大增益将平台由超限位置迅速调整到最大限定位置,并实时监测POS值,在载荷视轴位置误差较小时返回伺服模式。实验表明,该方法可靠、有效实现了稳定平台与位置传感器的高精度实时通信与控制。     

A complete VLBI delay model for deforming radio telescopes: the Effelsberg case

Deformations of radio telescopes used in geodetic and astrometric very long baseline interferometry (VLBI) observations belong to the class of systematic error sources which require correction in data analysis. In this paper we present a model for all path length variations in the geometrical optics of radio telescopes which are due to gravitational deformation. The Effelsberg 100 m radio telescope of the Max Planck Institute for Radio Astronomy, Bonn, Germany, has been surveyed by various terrestrial methods. Thus, all necessary information that is needed to model the path length variations is available. Additionally, a ray tracing program has been developed which uses as input the parameters of the measured deformations to produce an independent check of the theoretical model. In this program as well as in the theoretical model, the illumination function plays an important role because it serves as the weighting function for the individual path lengths depending on the distance from the optical axis. For the Effelsberg telescope, the biggest contribution to the total path length variations is the bending of the main beam located along the elevation axis which partly carries the weight of the paraboloid at its vertex. The difference in total path length is almost \(-\) 100 mm when comparing observations at 90 \(^\circ \) and at 0 \(^\circ \) elevation angle. The impact of the path length corrections is validated in a global VLBI analysis. The application of the correction model leads to a change in the vertical position of \(+120\)  mm. This is more than the maximum path length, but the effect can be explained by the shape of the correction function.