共查询到18条相似文献，搜索用时 640 毫秒
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为保证BPL长波授时时号(以国家授时中心(NTSC)保持的UTC(NTSC)为基准)的准确度,必须对该时号进行定时校准(确定发射时号与发播工作钟同步时定时校准信号的相位)。阐述了定时校准的原理和方法。与传统罗兰-C系统校准方法不同,该方法选择发射天线电流取样信号基准过零点而非定时控制单元基本定时信号为定时校准点,消除了因锁相控制精度不足引起的误差,提高了时号精度。该方法可以作为罗兰-C授时系统的通用校准方法。 相似文献
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罗兰—C导航系统的精度取决于其传播信号的地波部分的高稳定性。这一系统的有效工作范围受到地波信号传播距离和远距离处天波信号干扰的限制。本文叙述了一种测定天波特性的技术,以便估计天波对导航过程的影响,从而改进或扩大罗兰—C系统的导航范围。到目前为止所取得的资料表明:有可能工作在地波脉冲较迟一些的点上,以得到较高的信噪比;并且也有可能以低一些的精度用天波本身导航。文中还提出了进一步研究的工作。 相似文献
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本文比较详细地叙述了产生一个标准罗兰—C包络信号及罗兰—C脉冲信号的方法。同时,也介绍了所采用的线路,分析了这种方法的优点及存在的问题。 相似文献
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BPL时码发播和自主授时方法 总被引：1，自引：0，他引：1
在对国际上普遍采用的3种罗兰-C数字调制方法分析比较的基础上,对我国BPL长波授时发播系统技术改造中选用的数字调制方法、时码发播和自主授时方法进行了介绍,并提出了实现BPL时码发播和自主授时后宜采用的闰秒方案. 相似文献
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应用于数字下变频中CORDIC算法的FPGA实现 总被引：3，自引：0，他引：3
正余弦信号在GNSS接收终端的数字下变频中有着重要的应用,CORDIC算法是实现正余弦信号的最重要方法。立足于DDS与CORDIC算法的基本原理,针对CORDIC算法实现主要存在的3个问题,结合变象限法、流水线技术及相幅量化数据格式,在FPGA上通过实现CORDIC算法可在一个时钟周期内计算出正余弦信号幅值。仿真结果表明：与传统CORDIC算法实现相比,本文实现的正余弦信号精度高且速度快,并能满足GNSS接收终端数字下变频对正余弦信号的需求。 相似文献
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《中国科学院上海天文台年刊》2016,(0)
VLBI观测比单天线观测拥有更高的角分辨率,在脉冲星观测,尤其是成图和定位研究中有着重要的作用。相关处理机在进行脉冲星信号处理时,首先必须知道脉冲信号到达时刻、脉冲星相位及脉冲宽度等脉冲轮廓信息。研究了利用脉冲信号自功率谱来绘制脉冲星轮廓图的算法,此算法只需对单站信号进行频谱分析就可确定脉冲位置和宽度,然后在VLBI软件相关处理机中完成脉冲信号的相关计算。实际的VLBI数据相关处理结果表明,用上述方法可准确获得脉冲星的轮廓。 相似文献
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《天文和天体物理学研究(英文版)》2015,(5)
The wavefront measuring range and recovery precision of a curvature sensor can be improved by an intensity compensation algorithm. However, in a focal system with a fast f-number, especially a telescope with a large field of view, the accuracy of this algorithm cannot meet the requirements. A theoretical analysis of the corrected intensity compensation algorithm in a focal system with a fast f-number is first introduced and afterwards the mathematical equations used in this algorithm are expressed.The corrected result is then verified through simulation. The method used by such a simulation can be described as follows. First, the curvature signal from a focal system with a fast f-number is simulated by Monte Carlo ray tracing; then the wavefront result is calculated by the inner loop of the FFT wavefront recovery algorithm and the outer loop of the intensity compensation algorithm. Upon comparing the intensity compensation algorithm of an ideal system with the corrected intensity compensation algorithm, we reveal that the recovered precision of the curvature sensor can be greatly improved by the corrected intensity compensation algorithm. 相似文献
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D Buskulic R Flaminio F Marion L Massonnet R Morand B Mours D Verkindt M Yvert 《Astroparticle Physics》2001,15(4):383-389
In this paper we report a study – based on simulated data – performed to assess the level of accuracy needed in the process of calibrating the output of the VIRGO gravitational wave detector. A simple algorithm searching for signals from coalescing binaries is applied on data containing simulated signals and noise. Two kinds of calibration errors are then assumed to affect the data. The sensitivity of the algorithm to these errors is evaluated, both in terms of the signal-to-noise ratio and the estimation of the signal arrival time. 相似文献
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D. K. Hammond Y. Wiaux P. Vandergheynst 《Monthly notices of the Royal Astronomical Society》2009,398(3):1317-1332
An algorithm is proposed for denoising the signal induced by cosmic strings in the cosmic microwave background. A Bayesian approach is taken, based on modelling the string signal in the wavelet domain with generalized Gaussian distributions. Good performance of the algorithm is demonstrated by simulated experiments at arcminute resolution under noise conditions including primary and secondary cosmic microwave background anisotropies, as well as instrumental noise. 相似文献
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H. Ebeling D. A. White F. V. N. Rangarajan 《Monthly notices of the Royal Astronomical Society》2006,368(1):65-73
An efficient algorithm for adaptive kernel smoothing (AKS) of two-dimensional imaging data has been developed and implemented using the Interactive Data Language ( idl ). The functional form of the kernel can be varied (top-hat, Gaussian, etc.) to allow different weighting of the event counts registered within the smoothing region. For each individual pixel, the algorithm increases the smoothing scale until the signal-to-noise ratio (S/N) within the kernel reaches a pre-set value. Thus, noise is suppressed very efficiently, while at the same time real structure, that is, signal that is locally significant at the selected S/N level, is preserved on all scales. In particular, extended features in noise-dominated regions are visually enhanced. The asmooth algorithm differs from other AKS routines in that it allows a quantitative assessment of the goodness of the local signal estimation by producing adaptively smoothed images in which all pixel values share the same S/N above the background .
We apply asmooth to both real observational data (an X-ray image of clusters of galaxies obtained with the Chandra X-ray Observatory) and to a simulated data set. We find the asmooth ed images to be fair representations of the input data in the sense that the residuals are consistent with pure noise, that is, they possess Poissonian variance and a near-Gaussian distribution around a mean of zero, and are spatially uncorrelated. 相似文献
We apply asmooth to both real observational data (an X-ray image of clusters of galaxies obtained with the Chandra X-ray Observatory) and to a simulated data set. We find the asmooth ed images to be fair representations of the input data in the sense that the residuals are consistent with pure noise, that is, they possess Poissonian variance and a near-Gaussian distribution around a mean of zero, and are spatially uncorrelated. 相似文献