Multimessenger Gravitational-wave Searches with Pulsar Timing Arrays: Application to 3C 66B Using the NANOGrav 11-year Data Set
Multimessenger Gravitational-wave Searches with Pulsar Timing Arrays: Application to 3C 66B Using the NANOGrav 11-year Data Set
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DOI：
10.3847/1538-4357/ababa1
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发表时间：
2020-05
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通讯作者：
Z. Arzoumanian;P. T. Baker;A. Brazier;P. Brook;S. Burke-Spolaor;B. Bécsy;M. Charisi;S. Chatterjee;J. Cordes;N. Cornish;F. Crawford;H. Cromartie;K. Crowter;M. DeCesar;P. Demorest;T. Dolch;R. D. Elliott;Justin A. Ellis;R. Ferdman;E. Ferrara;E. Fonseca;N. Garver-Daniels;P. Gentile;D. Good;J. Hazboun;K. Islo;R. Jennings;Megan L. Jones;A. Kaiser;D. Kaplan;L. Z. Kelley;J. Key;M. Lam;T. Joseph W. Lazio;L. Levin;Jing Luo;R. Lynch;D. Madison;M. McLaughlin;C. Mingarelli;C. Ng;D. Nice;T. Pennucci;N. Pol;S. Ransom;P. Ray;B. Shapiro-Albert;X. Siemens;J. Simon;R. Spiewak;I. Stairs;D. Stinebring;K. Stovall;J. Swiggum;Stephen R. Taylor;M. Vallisneri;S. Vigeland;C. Witt;Weiwei Zhu
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作者：
Z. Arzoumanian;P. T. Baker;A. Brazier;P. Brook;S. Burke-Spolaor;B. Bécsy;M. Charisi;S. Chatterjee;J. Cordes;N. Cornish;F. Crawford;H. Cromartie;K. Crowter;M. DeCesar;P. Demorest;T. Dolch;R. D. Elliott;Justin A. Ellis;R. Ferdman;E. Ferrara;E. Fonseca;N. Garver-Daniels;P. Gentile;D. Good;J. Hazboun;K. Islo;R. Jennings;Megan L. Jones;A. Kaiser;D. Kaplan;L. Z. Kelley;J. Key;M. Lam;T. Joseph W. Lazio;L. Levin;Jing Luo;R. Lynch;D. Madison;M. McLaughlin;C. Mingarelli;C. Ng;D. Nice;T. Pennucci;N. Pol;S. Ransom;P. Ray;B. Shapiro-Albert;X. Siemens;J. Simon;R. Spiewak;I. Stairs;D. Stinebring;K. Stovall;J. Swiggum;Stephen R. Taylor;M. Vallisneri;S. Vigeland;C. Witt;Weiwei Zhu
当星系合并时，中心的超大质量黑洞可能会形成双星，并在此过程中发射低频引力辐射。在本文中，我们考虑的星系3C 66 B，这是第一个多信使搜索引力波的目标。由于观测到的源的测光和天体测量数据中存在的周期性，它已经被理论上包含一个超大质量黑洞双星。它明显的1.05年轨道周期将把引力波发射直接放在脉冲星的时间带内。自从3C 66 B的第一次脉冲星定时阵列研究以来，已经公布了源的修订模型，并且定时阵列的灵敏度和技术已经显着改善。利用这些进展，我们进一步利用NANOGrav 11年数据集的数据，将3C 66 B中潜在超大质量黑洞双星的啁啾质量限制在（1.65 ± 0.02）× 109 M Ω以下.该上限提供了比先前限值提高1.6倍的因子，以及比第一次检索提高4.3倍的因子。尽管如此，最新的轨道模型的来源仍然是符合我们的限制脉冲星定时阵列数据。此外，我们能够量化的改进所取得的列入源属性收集的电磁数据超过“盲”脉冲星定时阵列搜索。利用这些方法，很明显，它是不必要的，以获得有意义的天体物理推论，以获得确切的先验知识的周期的一个双。
When galaxies merge, the supermassive black holes in their centers may form binaries and emit low-frequency gravitational radiation in the process. In this paper, we consider the galaxy 3C 66B, which was used as the target of the first multimessenger search for gravitational waves. Due to the observed periodicities present in the photometric and astrometric data of the source, it has been theorized to contain a supermassive black hole binary. Its apparent 1.05-year orbital period would place the gravitational-wave emission directly in the pulsar timing band. Since the first pulsar timing array study of 3C 66B, revised models of the source have been published, and timing array sensitivities and techniques have improved dramatically. With these advances, we further constrain the chirp mass of the potential supermassive black hole binary in 3C 66B to less than (1.65 ± 0.02) × 109 M⊙ using data from the NANOGrav 11-year data set. This upper limit provides a factor of 1.6 improvement over previous limits and a factor of 4.3 over the first search done. Nevertheless, the most recent orbital model for the source is still consistent with our limit from pulsar timing array data. In addition, we are able to quantify the improvement made by the inclusion of source properties gleaned from electromagnetic data over “blind” pulsar timing array searches. With these methods, it is apparent that it is not necessary to obtain exact a priori knowledge of the period of a binary to gain meaningful astrophysical inferences.