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1、Observation of GravitationalWaves from a Binary Black Hole MergerThe LIGO Scientific Collaboration and The Virgo CollaborationOn September 14, 2015 at 09:50:45 UTC the two detectors of the Laser Interferometer GravitationalwaveObservatory (LIGO) simultaneously observed a transient gravitational-wave
2、 signal. The signalsweeps upwards in frequency from 35 Hz to 250 Hz with a peak gravitational-wave strain of 1:0 _ 1021.It matches the waveform predicted by general relativity for the inspiral and merger of a pair of black holesand the ringdown of the resulting single black hole. The signal was obse
3、rved with a matched filter signalto-noise ratio of 24 and a false alarm rate estimated to be less than 1 event per 203 000 years, equivalent toa significance greater than 5:1 _. The source lies at a luminosity distance of 410+160180 Mpc correspondingto a redshift z = 0:09+0:030:04. In the source fra
4、me, the initial black hole masses are 36+54M_ and 29+44M_,and the final black hole mass is 62+44M_, with 3:0+0:50:5M_c2 radiated in gravitational waves. All uncertaintiesdefine 90% credible intervals. These observations demonstrate the existence of binary stellar-massblack hole systems. This is the
5、first direct detection of gravitational waves and the first observation of abinary black hole merger.PACS numbers: 04.80.Nn, 04.25.dg, 95.85.Sz, 97.80.-dIntroduction In 1916, the year after the final formulationof the field equations of general relativity, Albert Einsteinpredicted the existence of g
6、ravitational waves. Hefound that the linearized weak-field equations had wavesolutions: transverse waves of spatial strain that travel atthe speed of light, generated by time variations of the massquadrupole moment of the source 1, 2. Einstein understood从一个黑洞的合并 gravitationalwaves 观察LIGO 科学合作和处女座的合作
7、在 09:50:45 UTC 两探测器的激光干涉引力波 2015 年 9 月 14 日天文台（LIGO）同时观察到一个短暂的引力波信号。信号把以上的频率从 35 赫兹到 250 赫兹以 1:0 _ 1021 峰引力波应变。它与波形的灵感和一对广义相对论所预言的黑洞合并和由此产生的单一黑洞的响铃。一个匹配滤波器的信号，观察信号噪音之比为 24 和假警报率估计为小于 1 事件每 000 203 年，相当于一个意义大于 5:1 _。源位于 160 + 410 的亮度距离180 MPC 相应一个红移 z = + 0:03 0:090:04 。在源框架，初始黑洞群众 36 + 54m_ 和 29 + 4
8、4m_ ，而最终黑洞质量为 6244m_ ，以 3:0 + 0:50:5m_c2 辐射引力波。所有不确定因素定义 90%可信区间。这些观察表明存在的二进制恒星质量黑洞系统。这是第一个直接探测引力波和第一个观察的二元黑洞合并。PACS 编号：04.80.nn，04.25.dg，95.85.sz，D 97.80。介绍-在 1916，年后的最后制定广义相对论的场方程，爱因斯坦艾伯特预测引力波的存在。他发现线性化的弱场方程有波解决方案：横向波的空间应变，旅行光的速度，所产生的时间变化的质量四极矩的来源 1，2 。爱因斯坦明白that gravitational-wave amplitudes woul
9、d be remarkablysmall; moreover, until the Chapel Hill conference in1957 there was significant debate about the physical realityof gravitational waves 3.Also in 1916, Schwarzschild published a solution for thefield equations 4 that was later understood to describe ablack hole 5, 6, and in 1963 Kerr g
10、eneralized the solutionto rotating black holes 7. Starting in the 1970s theoreticalwork led to the understanding of black hole quasinormalmodes 810, and in the 1990s higher-order post-Newtonian calculations 11 preceded extensive analyticalstudies of relativistic two-body dynamics 12, 13. In thepast
11、decade these analytical advances, together with breakthroughsin numerical relativity 1416, have enabled accuratesimulations of binary black hole mergers. Whilenumerous black hole candidates have now been identifiedthrough electromagnetic observations 1719, black holemergers have not previously been
12、observed.The discovery of the binary pulsar systemPSR B1913+16 by Hulse and Taylor 20 and subsequentobservations of its energy loss by Taylor andWeisberg 21 demonstrated the existence of gravitationalwaves. This discovery, along with emerging astrophysicalunderstanding 22, led to the recognition tha
13、t direct observationsof the amplitude and phase of gravitational waveswould enable studies of additional relativistic systems andprovide new tests of general relativity, especially in thedynamic strong-field regime.Experiments to detect gravitational waves began withWeber and his resonant mass detec
14、tors in the 1960s 23,followed by an international network of cryogenic resonantdetectors 24. Interferometric detectors were firstsuggested in the early 1960s 25 and the 1970s 26. Astudy of the noise and performance of such detectors 27,这种引力波的振幅将非常明显小；而且，直到教堂山会议在1957 关于物理现实的重大辩论引力波 3 。在 1916 出版的，史瓦西解
15、场方程 4 ，后来被理解为描述黑洞 5，6 ，并在 1963 克尔广义的解决方案旋转黑洞 7 。从 20 世纪 70 年代开始的理论工作导致黑洞似的理解模式 8，10 ，并在 20 世纪 90 年代高阶牛顿计算 11 之前广泛的分析相对论双体动力学研究 12，13 。在过去的十年中，这些分析的进步，与突破在数值相对论 14，16 ，使精确二元黑洞合并的模拟。而现在已经确定了许多黑洞候选通过电磁观测 17，19 ，黑洞合并以前没有被观察到。双星系统的发现PSR b1913 + 16 哈尔斯和泰勒 20 和随后的泰勒对其能量损失的观测韦斯伯格 21 证明引力的存在波。这一发现，随着新兴天体物理学理
16、解 22 ，导致认识到直接观察引力波的振幅和相位将使额外的相对论系统的研究和提供新的广义相对论，特别是在动力强场。探测引力波的实验开始了在 20 世纪 60 年代，韦伯和他的共振质谱检测器 23 ，其次是一个国际低温共振网络探测器 24 。干涉探测器建议在 20 世纪 60 年代初 25 和 20 世纪 70 年代 26 。一这种探测器的噪声和性能的研究 27 ，and further concepts to improve them 28, led to proposalsfor long-baseline broadband laser interferometers withthe potential for significantly increased sensitivity 2932.By the early 2000s, a set of initial
