Modeling the Uncertainties of Solar System Ephemerides for Robust Gravitational-wave Searches with Pulsar-timing Arrays
Modeling the Uncertainties of Solar System Ephemerides for Robust Gravitational-wave Searches with Pulsar-timing Arrays
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DOI：
10.3847/1538-4357/ab7b67
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发表时间：
2020-01
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通讯作者：
M. Vallisneri;Stephen R. Taylor;Stephen R. Taylor;J. Simon;W. Folkner;Ryan S. Park;Curt Cutler;Justin A. Ellis;T. Lazio;S. Vigeland;K. Aggarwal;Z. Arzoumanian;P. T. Baker;P. T. Baker;A. Brazier;P. Brook;S. Burke-Spolaor;S. Chatterjee;J. Cordes;N. Cornish;F. Crawford;H. Cromartie;K. Crowter;M. DeCesar;P. Demorest;T. Dolch;R. Ferdman;E. Ferrara;E. Fonseca;N. Garver-Daniels;P. Gentile;D. Good;J. Hazboun;A. M. Holgado;E. Huerta;K. Islo;R. Jennings;G. Jones;Megan L. Jones;D. Kaplan;L. Z. Kelley;J. Key;M. Lam;L. Levin;D. Lorimer;Jing Luo;R. Lynch;D. Madison;M. McLaughlin;S. McWilliams;C. Mingarelli;C. Ng;D. Nice;T. Pennucci;N. Pol;S. Ransom;S. Ransom;P. Ray;X. Siemens;X. Siemens;R. Spiewak;R. Spiewak;I. Stairs;D. Stinebring;K. Stovall;J. Swiggum;R. V. Haasteren;C. Witt;Weiwei Zhu
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作者：
M. Vallisneri;Stephen R. Taylor;Stephen R. Taylor;J. Simon;W. Folkner;Ryan S. Park;Curt Cutler;Justin A. Ellis;T. Lazio;S. Vigeland;K. Aggarwal;Z. Arzoumanian;P. T. Baker;P. T. Baker;A. Brazier;P. Brook;S. Burke-Spolaor;S. Chatterjee;J. Cordes;N. Cornish;F. Crawford;H. Cromartie;K. Crowter;M. DeCesar;P. Demorest;T. Dolch;R. Ferdman;E. Ferrara;E. Fonseca;N. Garver-Daniels;P. Gentile;D. Good;J. Hazboun;A. M. Holgado;E. Huerta;K. Islo;R. Jennings;G. Jones;Megan L. Jones;D. Kaplan;L. Z. Kelley;J. Key;M. Lam;L. Levin;D. Lorimer;Jing Luo;R. Lynch;D. Madison;M. McLaughlin;S. McWilliams;C. Mingarelli;C. Ng;D. Nice;T. Pennucci;N. Pol;S. Ransom;S. Ransom;P. Ray;X. Siemens;X. Siemens;R. Spiewak;R. Spiewak;I. Stairs;D. Stinebring;K. Stovall;J. Swiggum;R. V. Haasteren;C. Witt;Weiwei Zhu
一旦我们把脉冲到达的时间与太阳系的惯性静止坐标系联系起来，脉冲星发射的规律性就变得明显了。由此可见，在确定地球相对于太阳系质心的位置时，误差可以在脉冲星计时残余时间序列中表现为时间相关偏差，从而影响使用脉冲星计时阵列进行低频引力波的搜索。事实上，当用不同的太阳系星历表分析时，最近的阵列数据集产生了不同的引力波背景上限和探测统计数据。关键是，星历表通常不能提供可用的误差表示。在本文中，我们描述了太阳系星历不确定性物理模型的动机、构建和应用，该模型主要关注与脉冲星定时阵列引力波搜索最相关的自由度（木星的轨道元素）。该模型BayesEphem在NANOGrav 11年的随机背景搜索中得到了星历稳健的结果，并为NANOGrav和其他联盟的未来搜索提供了基础。这里报告的分析和模拟表明，星历表模型降低了11年数据集的引力波灵敏度，并且随着星历表的改进和脉冲星计时数据集的扩展远远超过单个木星轨道周期，这种简并性将消失。
The regularity of pulsar emissions becomes apparent once we reference the pulses’ times of arrivals to the inertial rest frame of the solar system. It follows that errors in the determination of Earth's position with respect to the solar system barycenter can appear as a time-correlated bias in pulsar-timing residual time series, affecting the searches for low-frequency gravitational waves performed with pulsar-timing arrays. Indeed, recent array data sets yield different gravitational-wave background upper limits and detection statistics when analyzed with different solar system ephemerides. Crucially, the ephemerides do not generally provide usable error representations. In this article, we describe the motivation, construction, and application of a physical model of solar system ephemeris uncertainties, which focuses on the degrees of freedom (Jupiter's orbital elements) most relevant to gravitational-wave searches with pulsar-timing arrays. This model, BayesEphem, was used to derive ephemeris-robust results in NANOGrav's 11 yr stochastic-background search, and it provides a foundation for future searches by NANOGrav and other consortia. The analysis and simulations reported here suggest that ephemeris modeling reduces the gravitational-wave sensitivity of the 11 yr data set and that this degeneracy will vanish with improved ephemerides and with pulsar-timing data sets that extend well beyond a single Jovian orbital period.