The NANOGrav 11 yr Data Set: Limits on Gravitational Wave Memory
The NANOGrav 11 yr Data Set: Limits on Gravitational Wave Memory
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DOI：
10.3847/1538-4357/ab6083
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发表时间：
2019-11
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通讯作者：
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;J. Ellis;J. Ellis;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;M. Jones;D. Kaplan;L. Kelley;J. Key;M. Lam;T. Lazio;L. Levin;D. Lorimer;J. 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;J. Simon;R. Spiewak;R. Spiewak;I. Stairs;D. Stinebring;K. Stovall;J. Swiggum;S. Taylor;S. Taylor;M. Vallisneri;R. V. Haasteren;S. Vigeland;C. Witt;Wenbai Zhu
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作者：
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;J. Ellis;J. Ellis;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;M. Jones;D. Kaplan;L. Kelley;J. Key;M. Lam;T. Lazio;L. Levin;D. Lorimer;J. 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;J. Simon;R. Spiewak;R. Spiewak;I. Stairs;D. Stinebring;K. Stovall;J. Swiggum;S. Taylor;S. Taylor;M. Vallisneri;R. V. Haasteren;S. Vigeland;C. Witt;Wenbai Zhu
超大质量黑洞双子星（SMBHBs）的合并有望成为令人难以置信的引力波（GWs）来源。虽然合并重力波形的振荡部分将超出脉冲星定时阵列的频率灵敏度范围，但可以检测到非振荡GW记忆效应。此外，任何GW的爆发都会产生GW存储器，使存储器成为对未建模的奇异源和新物理的有用探测。我们搜索了北美纳赫兹天文台的引力波（nanogravity） 11年的数据集，用于GW存储器。该数据集对~ 3 ~ 400nhz的极低频gw（周期为~ 11年1个月）敏感。由于没有发现GWs存在的证据，我们对观察期间GWs记忆事件的应变幅度进行了限制。然后，我们使用应变上限来限制GW内存导致事件的速率。在2.5 × 10−14的应变下，对应于源天空位置函数的中位上限，我们将GW记忆事件的速率限制在<0.4 yr−1。该应变对应于SMBHB合并，在1 Gpc的距离上，η为m ~ 2 × 1010，倾角为ι = π/3。为了检验我们的分析，我们也分析了nanogravity 9年的数据集。该分析发现了一个异常信号，这在11年的数据集中没有出现。这个信号不是GW，它的来源仍然未知。
The mergers of supermassive black hole binaries (SMBHBs) promise to be incredible sources of gravitational waves (GWs). While the oscillatory part of the merger gravitational waveform will be outside the frequency sensitivity range of pulsar timing arrays, the nonoscillatory GW memory effect is detectable. Further, any burst of GWs will produce GW memory, making memory a useful probe of unmodeled exotic sources and new physics. We searched the North American Nanohertz Observatory for Gravitational Waves (NANOGrav) 11 yr data set for GW memory. This data set is sensitive to very low-frequency GWs of ∼3 to 400 nHz (periods of ∼11 yr–1 month). Finding no evidence for GWs, we placed limits on the strain amplitude of GW memory events during the observation period. We then used the strain upper limits to place limits on the rate of GW memory causing events. At a strain of 2.5 × 10−14, corresponding to the median upper limit as a function of source sky position, we set a limit on the rate of GW memory events at <0.4 yr−1. That strain corresponds to an SMBHB merger with reduced mass of ηM ∼ 2 × 1010 and inclination of ι = π/3 at a distance of 1 Gpc. As a test of our analysis, we analyzed the NANOGrav 9 yr data set as well. This analysis found an anomolous signal, which does not appear in the 11 yr data set. This signal is not a GW, and its origin remains unknown.