为了充分利用不同类型的时间传递链路,需要实现不同采样率下时间传递链路数据的融合应用,提出了一种基于多分辨率分析的数据融合方法.首先对原始数据进行小波分解,把数据分解到统一的分辨率,初步消除高频噪声;然后在不同分辨率下进行Kal...为了充分利用不同类型的时间传递链路,需要实现不同采样率下时间传递链路数据的融合应用,提出了一种基于多分辨率分析的数据融合方法.首先对原始数据进行小波分解,把数据分解到统一的分辨率,初步消除高频噪声;然后在不同分辨率下进行Kalman滤波;最后通过Mallat快速重构算法得到融合结果.使用该方法处理中国科学院国家授时中心(National Time Service Center,NTSC)和德国联邦物理技术研究所(PhysikalischTechnische Bundesanstalt,PTB)之间的时间传递数据,结果显示融合算法能够处理链路异常或中断造成的数据问题.由于GPS(Global Positioning System)PPP(Precise Point Positioning solutions)链路实测结果性能整体优于TWSTFT(Two-Way Satellite Time and Frequency Transfer)链路,因此用GPS PPP链路测量结果评估融合算法增益.以快速协调世界时(Rapid Realization of Coordinated Universal Time,UTCr)为参考,数据融合结果的准确性增益约1%,日频率稳定度增益优于20%.同时融合算法可以抑制TWSTFT链路的周期噪声,能够有效提高链路的稳定性和鲁棒性.展开更多
喀什13 m甚长基线干涉测量(very long baseline interferometry,VLBI)观测站是中国科学院国家授时中心宽带VLBI观测系统的重要台站,特别是对世界时UT1测量有着不可替代的作用。随着城市的快速扩张和5G移动通信普及,5G移动通信信号等强...喀什13 m甚长基线干涉测量(very long baseline interferometry,VLBI)观测站是中国科学院国家授时中心宽带VLBI观测系统的重要台站,特别是对世界时UT1测量有着不可替代的作用。随着城市的快速扩张和5G移动通信普及,5G移动通信信号等强干扰导致喀什观测站天线系统灵敏度严重下降,严重影响了世界时UT1常规观测。针对此问题,提出利用超导滤波器将接收频带从C频段调整为X频段,设计了优化调整方案并进行了改造实施。测试结果表明,优化后基线灵敏度较优化前C频段提升3.7倍,UT1测量精度提升了12%。展开更多
The Wide Field Survey Telescope(WFST)is located at 4200 m on Saishiteng Mountain in Lenghu,Qinghai Province,China.It features a primary mirror with a diameter of 2.5 m and a camera equipped with nine CCDs,providing a ...The Wide Field Survey Telescope(WFST)is located at 4200 m on Saishiteng Mountain in Lenghu,Qinghai Province,China.It features a primary mirror with a diameter of 2.5 m and a camera equipped with nine CCDs,providing a wide field of view of approximately 3×3 square degrees.Calibration parameters are essential to ensure the precision of astrometric observations with the WFST.These parameters are derived from geometric distortion(GD)and gaps through astrometric modeling and are subsequently validated via the Yao’An High Precision Telescope(YAHPT).The GD solutions show maximum distortions between 1.18 and 10.29 pixels for the WFST chips,with central chips exhibiting lower distortion.After applying the GD correction,the precision of the WFST reaches 4 mas.The interchip gaps of the WFST range from 1.922 mm to 7.765 mm,corresponding to 10μm/pixel,aligning with the design and measurements.The calibrated parameters guarantee that the WFST can perform highly accurate astrometric measurements.Furthermore,as the WFST undergoes updates,the parameter model remains consistently applicable.展开更多
文摘为了充分利用不同类型的时间传递链路,需要实现不同采样率下时间传递链路数据的融合应用,提出了一种基于多分辨率分析的数据融合方法.首先对原始数据进行小波分解,把数据分解到统一的分辨率,初步消除高频噪声;然后在不同分辨率下进行Kalman滤波;最后通过Mallat快速重构算法得到融合结果.使用该方法处理中国科学院国家授时中心(National Time Service Center,NTSC)和德国联邦物理技术研究所(PhysikalischTechnische Bundesanstalt,PTB)之间的时间传递数据,结果显示融合算法能够处理链路异常或中断造成的数据问题.由于GPS(Global Positioning System)PPP(Precise Point Positioning solutions)链路实测结果性能整体优于TWSTFT(Two-Way Satellite Time and Frequency Transfer)链路,因此用GPS PPP链路测量结果评估融合算法增益.以快速协调世界时(Rapid Realization of Coordinated Universal Time,UTCr)为参考,数据融合结果的准确性增益约1%,日频率稳定度增益优于20%.同时融合算法可以抑制TWSTFT链路的周期噪声,能够有效提高链路的稳定性和鲁棒性.
文摘喀什13 m甚长基线干涉测量(very long baseline interferometry,VLBI)观测站是中国科学院国家授时中心宽带VLBI观测系统的重要台站,特别是对世界时UT1测量有着不可替代的作用。随着城市的快速扩张和5G移动通信普及,5G移动通信信号等强干扰导致喀什观测站天线系统灵敏度严重下降,严重影响了世界时UT1常规观测。针对此问题,提出利用超导滤波器将接收频带从C频段调整为X频段,设计了优化调整方案并进行了改造实施。测试结果表明,优化后基线灵敏度较优化前C频段提升3.7倍,UT1测量精度提升了12%。
基金supported by the Strategic Priority Research Program of the Chinese Academy of Sciences(XDA0350300)the National Natural Science Foundation of China(12203105,12103091,62394351,12073008)the China Manned Space Project(CMS-CSST-2021-A12,CMS-CSST-2021-B10).
文摘The Wide Field Survey Telescope(WFST)is located at 4200 m on Saishiteng Mountain in Lenghu,Qinghai Province,China.It features a primary mirror with a diameter of 2.5 m and a camera equipped with nine CCDs,providing a wide field of view of approximately 3×3 square degrees.Calibration parameters are essential to ensure the precision of astrometric observations with the WFST.These parameters are derived from geometric distortion(GD)and gaps through astrometric modeling and are subsequently validated via the Yao’An High Precision Telescope(YAHPT).The GD solutions show maximum distortions between 1.18 and 10.29 pixels for the WFST chips,with central chips exhibiting lower distortion.After applying the GD correction,the precision of the WFST reaches 4 mas.The interchip gaps of the WFST range from 1.922 mm to 7.765 mm,corresponding to 10μm/pixel,aligning with the design and measurements.The calibrated parameters guarantee that the WFST can perform highly accurate astrometric measurements.Furthermore,as the WFST undergoes updates,the parameter model remains consistently applicable.
