Error-analysis and comparison to analytical models of numerical waveforms produced by the NRAR Collaboration
Error-analysis and comparison to analytical models of numerical waveforms produced by the NRAR Collaboration
复制标题
DOI：
10.1088/0264-9381/31/2/025012
复制
发表时间：
2013-07
影响因子：
3.5
通讯作者：
I. Hinder;A. Buonanno;M. Boyle;Z. Etienne;J. Healy;N. Johnson-McDaniel;A. Nagar;H. Nakano;
中科院分区：
文献类型：
--
作者：
I. Hinder;A. Buonanno;M. Boyle;Z. Etienne;J. Healy;N. Johnson-McDaniel;A. Nagar;H. Nakano;
数值相对论-分析相对论（NRAR）合作是数值相对论，分析相对论和引力波数据分析社区成员之间的共同努力。NRAR合作的目标是产生紧凑双星的数值相对论模拟，并使用它们为LIGO/Virgo合作开发精确的分析模板，用于检测引力波信号并从中提取天体物理信息。我们描述了NRAR项目的第一阶段的结果，该项目的重点是从中等质量比和自旋的二元黑洞以及质量比为10的非自旋二元配置中产生一组初始的数值波形。所有的数值波形进行了分析，在一个统一的和一致的方式，与数值误差评估使用的分析代码创建的NRAR合作的成员。我们比较以前校准，非处理分析波形，特别是有效单体（EOB）和唯象模板家庭，新产生的数值波形。我们发现，当双星的总质量为100- 200 M Ω时，当前的EOB和自旋的唯象模型，非旋进双星波形与所有质量比为100 - 200 M Ω的非旋进双星数值波形在最大化双星参数时具有99%以上的重叠（对于先进的LIGO）。这意味着由于建模误差导致的事件率损失低于3%。此外，先前校准为质量比小于6的五个非自旋波形的非自旋EOB波形与质量比为10的数值波形具有99.7%以上的重叠，甚至没有最大化二元参数。
The Numerical–Relativity–Analytical–Relativity (NRAR) collaboration is a joint effort between members of the numerical relativity, analytical relativity and gravitational-wave data analysis communities. The goal of the NRAR collaboration is to produce numerical-relativity simulations of compact binaries and use them to develop accurate analytical templates for the LIGO/Virgo Collaboration to use in detecting gravitational-wave signals and extracting astrophysical information from them. We describe the results of the first stage of the NRAR project, which focused on producing an initial set of numerical waveforms from binary black holes with moderate mass ratios and spins, as well as one non-spinning binary configuration which has a mass ratio of 10. All of the numerical waveforms are analysed in a uniform and consistent manner, with numerical errors evaluated using an analysis code created by members of the NRAR collaboration. We compare previously-calibrated, non-precessing analytical waveforms, notably the effective-one-body (EOB) and phenomenological template families, to the newly-produced numerical waveforms. We find that when the binary's total mass is ∼100–200M⊙, current EOB and phenomenological models of spinning, non-precessing binary waveforms have overlaps above 99% (for advanced LIGO) with all of the non-precessing-binary numerical waveforms with mass ratios ⩽4, when maximizing over binary parameters. This implies that the loss of event rate due to modelling error is below 3%. Moreover, the non-spinning EOB waveforms previously calibrated to five non-spinning waveforms with mass ratio smaller than 6 have overlaps above 99.7% with the numerical waveform with a mass ratio of 10, without even maximizing on the binary parameters.