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累积轮廓、流量和周期是X射线脉冲星辐射信号的三个重要特征,将其应用于X射线脉冲星信号检测中,提出了一种基于Bayesian估计的X射线脉冲星周期辐射信号时域检测方法.该方法以非脉冲区噪声观测为先验知识,利用X射线脉冲星辐射信号的泊松分布模型推导了信号概率密度分布函数,以该函数的累积分布函数为判据,对X射线脉冲星微弱信号进行检测,并提取位相偏移量.利用仿真数据和RXTE卫星的实测数据进行实验验证,结果表明:本文方法性能优于同类的基于高斯分布模型的检测方法,在检测信号的同时能在一定精度下给出信号位相偏移值.
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关键词:
- 脉冲星 /
- Bayesian估计 /
- 位相测量 /
- 时域检测
Integrated profile, flux and period are three major characteristics of pulsar. Taking advantage of these characteristics, a time domain detecting method is presented based on Bayesian estimation to detect pulsar periodic radiation signals. The signal probability distribution is deduced based on the Poisson distribution model of X-ray pulsar, with noise observation of non-pulse region used as the priori knowledge. The cumulative distribution function of the signal probability is used as a criterion to detect weak signals of X-ray pulsars and extract the phase offset. The RXTE data and the simulation data are used for experimental verification, and the results show that the method outperforms a similar method which is based on the Gauss distribution model, in addition, it can give the phase offset in a certain accuracy.-
Keywords:
- pulsars /
- Bayesian estimation /
- phase measurement /
- time domain detection
[1] Pei Y J, Jun Z 2008 Chin. Phys. B 17 1
[2] Sheikh S I 2005 Ph. D. Dissertation (Maryland:University of Maryland)
[3] Seward F D, Harnden F R, Helfand D J 1984 Astrophysical Journal 287 L19
[4] Xie Z H, Xu L P, Ni G R 2007 J. Infrared Millim. Waves 26 187 (in Chinese) [谢振华、许录平、倪广仁 2008 红外与毫米波学报 26 187]
[5] Xie Z H, Xu L P, Ni G R 2007 Acta Phys. Sin. 26 187 (in Chinese)[谢振华、许录平、倪广仁 2007 物理学报 〖6] Gregory P C 1996 Astrophysical Journal 10 1
[6] Currie L A 1968 Analytical Chemistry 40 586
[7] Gregory P 2003 Bayesian Logical Data Analysis for the Physical Sciences (U.K.:Cambridge Univ) p5
[8] Sala J, Urruela A, Villares X 2004 European Space Agency Advanced Concepts Team ARIADNA Study June 4202 23
[9] Li J X, Ke X Z 2010 Acta Phys. Sin. 59 8304 (in Chinese)[李建勋、柯熙政 2010 物理学报 59 8304]
[10] Young J M K A 2009 IEEE Trans. Nucl. Sci. 56 1278
[11] Kuiper L, Hermsen W 2003 proceedings of AGILE Science Workshop Rome, Italy, Dec, 2003 p11
[12] Nicastro L, Cusumano G, Lohmer O, Kramer M, Kuiper L, Hermsen W, Mineo T, Becker W 2004 Astron.Astrophys 413 1065
[13] Rxte. FTP:legacy.gsfc.nasa.gov.
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[1] Pei Y J, Jun Z 2008 Chin. Phys. B 17 1
[2] Sheikh S I 2005 Ph. D. Dissertation (Maryland:University of Maryland)
[3] Seward F D, Harnden F R, Helfand D J 1984 Astrophysical Journal 287 L19
[4] Xie Z H, Xu L P, Ni G R 2007 J. Infrared Millim. Waves 26 187 (in Chinese) [谢振华、许录平、倪广仁 2008 红外与毫米波学报 26 187]
[5] Xie Z H, Xu L P, Ni G R 2007 Acta Phys. Sin. 26 187 (in Chinese)[谢振华、许录平、倪广仁 2007 物理学报 〖6] Gregory P C 1996 Astrophysical Journal 10 1
[6] Currie L A 1968 Analytical Chemistry 40 586
[7] Gregory P 2003 Bayesian Logical Data Analysis for the Physical Sciences (U.K.:Cambridge Univ) p5
[8] Sala J, Urruela A, Villares X 2004 European Space Agency Advanced Concepts Team ARIADNA Study June 4202 23
[9] Li J X, Ke X Z 2010 Acta Phys. Sin. 59 8304 (in Chinese)[李建勋、柯熙政 2010 物理学报 59 8304]
[10] Young J M K A 2009 IEEE Trans. Nucl. Sci. 56 1278
[11] Kuiper L, Hermsen W 2003 proceedings of AGILE Science Workshop Rome, Italy, Dec, 2003 p11
[12] Nicastro L, Cusumano G, Lohmer O, Kramer M, Kuiper L, Hermsen W, Mineo T, Becker W 2004 Astron.Astrophys 413 1065
[13] Rxte. FTP:legacy.gsfc.nasa.gov.
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