Properties of the Binary Neutron Star Merger GW170817
Properties of the Binary Neutron Star Merger GW170817
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DOI：
10.1103/physrevx.9.011001
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发表时间：
2019-01-02
影响因子：
12.5
通讯作者：
Zweizig, J.
中科院分区：
文献类型：
--
作者：
Abbott, B. P.;Abbott, R.;Zweizig, J.
2017年8月17日，Advanced LIGO和Advanced Virgo引力波探测器观测到一颗低质量致密双星螺旋状。引力波信号源GW 170817的初始天空定位允许电磁观测站将NGC 4993确定为宿主星系。在这项工作中，我们改进了二进制的属性，包括组件的质量，自旋和潮汐参数的初始估计，使用已知的源位置，改进的建模，并重新校准处女座的数据。我们将引力波频率的范围扩展到23 Hz，而在最初的分析中为30 Hz。我们还比较了使用几种信号模型推断的结果，与初始分析相比，这些模型更准确，并包含额外的物理效应。我们将引力波源的定位提高到90%可信的16度区域（2）。我们发现更严格的质量，自旋和潮汐参数的限制，并继续寻找非零组件自旋没有证据。当允许大的组件自旋时，推测组件质量位于1.00和1.89 M圆点之间，当自旋限制在银河系双星中观察到的范围内时，组件质量位于1.16和1.60 M圆点之间（总质量为2.73（-0.01）（+0.04）M圆点）。使用进动模型，并允许大的组件自旋，我们约束的组件的无量纲自旋小于0.50的主要和0.61的中学。在对紧凑物体性质的最小假设下，当我们允许大分量自旋时，我们对波浪线上潮汐变形参数（Lambda）的约束是（0，630），而当我们允许大分量自旋时，我们对波浪线上潮汐变形参数（Lambda）的约束是300（-230）（+420）。（使用90%的最高后验密度间隔）当限制分量自旋的幅度时，在90%的可信度下排除了几个状态方程模型。最后，利用LIGO和GEO 600数据，我们使用贝叶斯分析对可能的合并后信号的振幅和谱能量密度设置上限。
On August 17, 2017, the Advanced LIGO and Advanced Virgo gravitational-wave detectors observed a low-mass compact binary inspiral. The initial sky localization of the source of the gravitational-wave signal, GW170817, allowed electromagnetic observatories to identify NGC 4993 as the host galaxy. In this work, we improve initial estimates of the binary's properties, including component masses, spins, and tidal parameters, using the known source location, improved modeling, and recalibrated Virgo data. We extend the range of gravitational-wave frequencies considered down to 23 Hz, compared to 30 Hz in the initial analysis. We also compare results inferred using several signal models, which are more accurate and incorporate additional physical effects as compared to the initial analysis. We improve the localization of the gravitational-wave source to a 90% credible region of 16 deg(2). We find tighter constraints on the masses, spins, and tidal parameters, and continue to find no evidence for nonzero component spins. The component masses are inferred to lie between 1.00 and 1.89 M-circle dot when allowing for large component spins, and to lie between 1.16 and 1.60 M-circle dot (with a total mass 2.73(-0.01)(+0.04) M-circle dot) when the spins are restricted to be within the range observed in Galactic binary neutron stars. Using a precessing model and allowing for large component spins, we constrain the dimensionless spins of the components to be less than 0.50 for the primary and 0.61 for the secondary. Under minimal assumptions about the nature of the compact objects, our constraints for the tidal deformability parameter (Lambda) over tilde are (0,630) when we allow for large component spins, and 300(-230)(+420) (using a 90% highest posterior density interval) when restricting the magnitude of the component spins, ruling out several equation-of-state models at the 90% credible level. Finally, with LIGO and GEO600 data, we use a Bayesian analysis to place upper limits on the amplitude and spectral energy density of a possible postmerger signal.