Constraining the Properties of the Proposed Super-Massive Black Hole System in 3C66B: Limits from Pulsar Timing
Constraining the Properties of the Proposed Super-Massive Black Hole System in 3C66B: Limits from Pulsar Timing
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DOI：
10.1086/383020
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发表时间：
2003-10
期刊：
影响因子：
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通讯作者：
F. Jenet;A. Lommen;S. Larson;L. Wen
中科院分区：
文献类型：
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作者：
F. Jenet;A. Lommen;S. Larson;L. Wen
本文首次导出了一个缓慢演化的偏心双黑洞系统的引力波（G波）辐射所引起的期望时间残差的一般表达式。这些表达式被用来搜索的G-波的签名所提出的超大质量双黑洞系统在3C 66 B。我们使用的数据来自射电脉冲星PSR B1855+09的长期定时观测。对于圆形轨道的情况，发射的G波应该在PSR B1855+09的脉冲到达时间中产生明显可检测的波动。由于没有检测到G波，因此将波形用于蒙特卡罗分析，以便对所提出的黑洞系统的质量和偏心率进行限制。这里给出的分析以95%的置信度排除了所采用的系统。报告的分析还展示了几个有趣的功能的G波探测器的脉冲星定时的基础上。
General expressions for the expected timing residuals induced by gravitational wave (G-wave) emission from a slowly evolving, eccentric, binary black hole system are derived here for the first time. These expressions are used to search for the signature of G-waves emitted by the proposed supermassive binary black hole system in 3C 66B. We use data from long-term timing observations of the radio pulsar PSR B1855+09. For the case of a circular orbit, the emitted G-waves should generate clearly detectable fluctuations in the pulse-arrival times of PSR B1855+09. Since no G-waves are detected, the waveforms are used in a Monte Carlo analysis in order to place limits on the mass and eccentricity of the proposed black hole system. The analysis presented here rules out the adopted system with 95% confidence. The reported analysis also demonstrates several interesting features of a G-wave detector based on pulsar timing.