THE NANOGRAV 11-YEAR DATA SET: LIMITS ON GRAVITATIONAL WAVES FROM INDIVIDUAL SUPERMASSIVE BLACK HOLE BINARIES
THE NANOGRAV 11-YEAR DATA SET: LIMITS ON GRAVITATIONAL WAVES FROM INDIVIDUAL SUPERMASSIVE BLACK HOLE BINARIES
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NANOGRAV 11 年数据集：来自单个超大质量黑洞双星的引力波的限制
DOI：
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发表时间：
2019
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通讯作者：
HU W.W.Z
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作者：
Z. A. Rzoumanian;P. T. B. Aker;A. B. Razier;M. R. B. Rinson;P. Rook;S. B. U. Polaor;S. Hatterjee;J. M. C. Ordes;N. Ornish;F. C. Rawford;K. C. Rowter;H. T. C. Romartie;M. C. Esar;P. D. Emorest;T. D. Olch;J. A. E. Llis;R. Erdman;E. F. Errara;E. F. Onseca;N. G. A. Aniels;P. G. Entile;J. S. H. Azboun;A. M. H. Olgado;E. A. H. Uerta;R. J. Ennings;A. R. K. Aiser;D. Aplan;L. Elley;AM M.T.L;T. J. L. Azio;L. Evin;D. R. L. Orimer;UO J.L;R. L. Ynch;D. R. M. Adison;M. A. M. C. L. Aughlin;S. W. Illiams;C. M. F. M. Ingarelli;D. Ice;T. T. P. Ennucci;S. R. Ansom;X. S. Iemens;J. Imon;R. S. Piewak;I. H. S. Tairs;D. R. S. Tinebring;K. S. Tovall;J. S. Wiggum;S. Aylor;J. Urner;M. V. Allisneri;R. V. H. Aasteren;S. J. V. Igeland;C. Itt;HU W.W.Z
观测表明，几乎所有星系的中心都含有超大质量黑洞（SMBH）。当星系合并时，它们的黑洞组成了SMBH双星（SMBHB），它们发射低频引力波（GW），可以被脉冲星定时阵列（PTA）探测到。我们搜索了北美纳赫兹引力波天文台 (NANOGrav) 11 年的数据集，以查找圆形轨道上单个 SMBHB 的引力波。由于我们在数据中没有找到 GW 的有力证据，因此我们对此类来源的 GW 强度设定了 95% 的上限。在 fgw = 8nHz 时，我们设置天空平均上限为 h0 < 7.3(3)× 10−15。我们还开发了一种技术，使用“丢失”参数作为识别杂散信号的方式来确定每个脉冲星中特定信号的重要性。根据这些上限，我们排除了在我们最敏感的天空位置，M = 109 M 时 120 Mpc 内的 SMBHB 发射的 GW，以及 M = 1010 M 时 5.5 Gpc 内的 fgw = 8nHz 的 GW。我们还确定，处女座星团中不存在 M > 1.6× 109 M 发射 fgw = 2.8 − 317.8nHz 的 GW 的 SMBHB。最后，我们根据两微米全天巡天 (2MASS) 中的星系和 Illustris 宇宙学模拟项目的合并率，将我们的应变上限与 SMBHB 的模拟种群进行了比较，发现 ar X iv 中只有 34 个：1 81 2. 11 58 5v 3 [ as troph .GA ] 2 1 May 2 01 9 2 THE NANOGRAV 合作 75,000 个本地宇宙的实现包含可检测的源。
Observations indicate that nearly all galaxies contain supermassive black holes (SMBHs) at their centers. When galaxies merge, their component black holes form SMBH binaries (SMBHBs), which emit low-frequency gravitational waves (GWs) that can be detected by pulsar timing arrays (PTAs). We have searched the North American Nanohertz Observatory for Gravitational Waves (NANOGrav) 11-year data set for GWs from individual SMBHBs in circular orbits. As we did not find strong evidence for GWs in our data, we placed 95% upper limits on the strength of GWs from such sources. At fgw = 8nHz, we placed a sky-averaged upper limit of h0 < 7.3(3)× 10−15. We also developed a technique to determine the significance of a particular signal in each pulsar using “dropout” parameters as a way of identifying spurious signals. From these upper limits, we ruled out SMBHBs emitting GWs with fgw = 8nHz within 120 Mpc for M = 109 M , and within 5.5 Gpc for M = 1010 M at our most-sensitive sky location. We also determined that there are no SMBHBs with M > 1.6× 109 M emitting GWs with fgw = 2.8 − 317.8nHz in the Virgo Cluster. Finally, we compared our strain upper limits to simulated populations of SMBHBs, based on galaxies in Two Micron All-Sky Survey (2MASS) and merger rates from the Illustris cosmological simulation project, and found that only 34 out of ar X iv :1 81 2. 11 58 5v 3 [ as tr oph .G A ] 2 1 M ay 2 01 9 2 THE NANOGRAV COLLABORATION 75,000 realizations of the local Universe contained a detectable source.