Suitability of post-Newtonian/numerical-relativity hybrid waveforms for gravitational wave detectors
Suitability of post-Newtonian/numerical-relativity hybrid waveforms for gravitational wave detectors
复制标题
后牛顿/数值相对论混合波形对引力波探测器的适用性
DOI：
10.1088/0264-9381/28/13/134002
复制
发表时间：
2011
影响因子：
3.5
通讯作者：
H. Pfeiffer
中科院分区：
文献类型：
--
作者：
I. MacDonald;S. Nissanke;H. Pfeiffer
本文提出了一种研究后牛顿和数值相对论波形的最苛刻的使用情况下，足够的精度：先进的引力波探测器中的强源的参数估计。对于黑洞双星，这些检测器需要精确的波形模型，可以通过融合分析后牛顿inspiral波形与数值相对论合并振铃波形来构建。我们执行一个全面的分析，进入这样的“混合波形”的错误。我们发现后牛顿的波形必须与数值相对论的波形精确地对齐，大约是引力波周期的1/100。数值相对论模拟的螺旋相位误差必须控制在± 0.1rad以内。（这些数字适用于对GW来源数量的适度乐观估计;特别强的信号需要更小的误差。误差的主要来源来自于所研究的后牛顿泰勒近似的不准确性。使用我们的误差标准，即使在3.5后牛顿秩序，杂交必须进行显着的最长的目前可用的数值波形，涵盖30引力波周期开始之前。目前的研究仅限于等质量、零自旋的情况，没有考虑引力波探测器的校准误差。
This paper presents a study of the sufficient accuracy of post-Newtonian and numerical relativity waveforms for the most demanding usage case: parameter estimation of strong sources in advanced gravitational wave detectors. For black hole binaries, these detectors require accurate waveform models which can be constructed by fusing an analytical post-Newtonian inspiral waveform with a numerical relativity merger-ringdown waveform. We perform a comprehensive analysis of errors that enter such ‘hybrid waveforms’. We find that the post-Newtonian waveform must be aligned with the numerical relativity waveform to exquisite accuracy, about 1/100 of a gravitational wave cycle. Phase errors in the inspiral phase of the numerical relativity simulation must be controlled to ≲ 0.1 rad. (These numbers apply to moderately optimistic estimates about the number of GW sources; exceptionally strong signals require even smaller errors.) The dominant source of error arises from the inaccuracy of the investigated post-Newtonian Taylor approximants. Using our error criterion, even at 3.5th post-Newtonian order, hybridization has to be performed significantly before the start of the longest currently available numerical waveforms which cover 30 gravitational wave cycles. The current investigation is limited to the equal-mass, zero-spin case and does not take into account calibration errors of the gravitational wave detectors.