确定何时可以用重力波形测量进动

R. Green, C. Hoy, S. Fairhurst, M. Hannam, F. Pannarale, Cory M. Thomas
{"title":"确定何时可以用重力波形测量进动","authors":"R. Green, C. Hoy, S. Fairhurst, M. Hannam, F. Pannarale, Cory M. Thomas","doi":"10.1103/PhysRevD.103.124023","DOIUrl":null,"url":null,"abstract":"In binary-black-hole systems where the black-hole spins are misaligned with the orbital angular momentum, precession effects leave characteristic modulations in the emitted gravitational waveform. Here, we investigate where in the parameter space we will be able to accurately identify precession, for likely observations over coming LIGO-Virgo-KAGRA observing runs. Despite the large number of parameters that characterise a precessing binary, we perform a large scale systematic study to identify the impact of each source parameter on the measurement of precession. We simulate a fiducial binary at moderate mass-ratio, signal-to-noise ratio (SNR), and spins, such that precession will be clearly identifiable, then successively vary each parameter while holding the remaining parameters fixed. As expected, evidence for precession increases with signal-to noise-ratio (SNR), higher in-plane spins, more unequal component masses, and higher inclination, but our study provides a quantitative illustration of each of these effects, and informs our intuition on parameter dependencies that have not yet been studied in detail, for example, the effect of varying the relative strength of the two polarisations, the total mass, and the aligned-spin components. We also measure the \"precession SNR\" $\\rho_p$, which was introduced in Refs[1,2] to quantify the signal power associated with precession. By comparing $\\rho_p$ with both Bayes factors and the recovered posterior distributions, we find it is a reliable metric for measurability that accurately predicts when the detected signal contains evidence for precession.","PeriodicalId":8455,"journal":{"name":"arXiv: General Relativity and Quantum Cosmology","volume":null,"pages":null},"PeriodicalIF":0.0000,"publicationDate":"2020-10-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"13","resultStr":"{\"title\":\"Identifying when precession can be measured in gravitational waveforms\",\"authors\":\"R. Green, C. Hoy, S. Fairhurst, M. Hannam, F. Pannarale, Cory M. Thomas\",\"doi\":\"10.1103/PhysRevD.103.124023\",\"DOIUrl\":null,\"url\":null,\"abstract\":\"In binary-black-hole systems where the black-hole spins are misaligned with the orbital angular momentum, precession effects leave characteristic modulations in the emitted gravitational waveform. Here, we investigate where in the parameter space we will be able to accurately identify precession, for likely observations over coming LIGO-Virgo-KAGRA observing runs. Despite the large number of parameters that characterise a precessing binary, we perform a large scale systematic study to identify the impact of each source parameter on the measurement of precession. We simulate a fiducial binary at moderate mass-ratio, signal-to-noise ratio (SNR), and spins, such that precession will be clearly identifiable, then successively vary each parameter while holding the remaining parameters fixed. As expected, evidence for precession increases with signal-to noise-ratio (SNR), higher in-plane spins, more unequal component masses, and higher inclination, but our study provides a quantitative illustration of each of these effects, and informs our intuition on parameter dependencies that have not yet been studied in detail, for example, the effect of varying the relative strength of the two polarisations, the total mass, and the aligned-spin components. We also measure the \\\"precession SNR\\\" $\\\\rho_p$, which was introduced in Refs[1,2] to quantify the signal power associated with precession. By comparing $\\\\rho_p$ with both Bayes factors and the recovered posterior distributions, we find it is a reliable metric for measurability that accurately predicts when the detected signal contains evidence for precession.\",\"PeriodicalId\":8455,\"journal\":{\"name\":\"arXiv: General Relativity and Quantum Cosmology\",\"volume\":null,\"pages\":null},\"PeriodicalIF\":0.0000,\"publicationDate\":\"2020-10-08\",\"publicationTypes\":\"Journal Article\",\"fieldsOfStudy\":null,\"isOpenAccess\":false,\"openAccessPdf\":\"\",\"citationCount\":\"13\",\"resultStr\":null,\"platform\":\"Semanticscholar\",\"paperid\":null,\"PeriodicalName\":\"arXiv: General Relativity and Quantum Cosmology\",\"FirstCategoryId\":\"1085\",\"ListUrlMain\":\"https://doi.org/10.1103/PhysRevD.103.124023\",\"RegionNum\":0,\"RegionCategory\":null,\"ArticlePicture\":[],\"TitleCN\":null,\"AbstractTextCN\":null,\"PMCID\":null,\"EPubDate\":\"\",\"PubModel\":\"\",\"JCR\":\"\",\"JCRName\":\"\",\"Score\":null,\"Total\":0}","platform":"Semanticscholar","paperid":null,"PeriodicalName":"arXiv: General Relativity and Quantum Cosmology","FirstCategoryId":"1085","ListUrlMain":"https://doi.org/10.1103/PhysRevD.103.124023","RegionNum":0,"RegionCategory":null,"ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"","JCRName":"","Score":null,"Total":0}
引用次数: 13

摘要

在双黑洞系统中,黑洞自旋与轨道角动量不一致,进动效应会在发射的引力波形中留下特征调制。在这里,我们研究在参数空间中我们将能够准确地识别进动,以便在即将到来的LIGO-Virgo-KAGRA观测运行中进行可能的观测。尽管表征进动二进制的参数很多,但我们进行了大规模的系统研究,以确定每个源参数对进动测量的影响。我们模拟了一个中等质量比、信噪比(SNR)和自旋的基准双星,这样就可以清楚地识别进动,然后依次改变每个参数,同时保持其余参数固定。正如预期的那样,进动的证据随着信噪比(SNR)、更高的面内自旋、更不均匀的分量质量和更高的倾角而增加,但我们的研究提供了这些影响的定量说明,并告知我们对尚未详细研究的参数依赖性的直觉,例如,改变两种极化的相对强度、总质量和排列自旋分量的影响。我们还测量了参考文献[1,2]中引入的“进动信噪比”$\rho_p$,以量化与进动相关的信号功率。通过将$\rho_p$与贝叶斯因子和恢复后验分布进行比较,我们发现它是一个可靠的可测量性度量,可以准确地预测检测到的信号何时包含进动证据。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
Identifying when precession can be measured in gravitational waveforms
In binary-black-hole systems where the black-hole spins are misaligned with the orbital angular momentum, precession effects leave characteristic modulations in the emitted gravitational waveform. Here, we investigate where in the parameter space we will be able to accurately identify precession, for likely observations over coming LIGO-Virgo-KAGRA observing runs. Despite the large number of parameters that characterise a precessing binary, we perform a large scale systematic study to identify the impact of each source parameter on the measurement of precession. We simulate a fiducial binary at moderate mass-ratio, signal-to-noise ratio (SNR), and spins, such that precession will be clearly identifiable, then successively vary each parameter while holding the remaining parameters fixed. As expected, evidence for precession increases with signal-to noise-ratio (SNR), higher in-plane spins, more unequal component masses, and higher inclination, but our study provides a quantitative illustration of each of these effects, and informs our intuition on parameter dependencies that have not yet been studied in detail, for example, the effect of varying the relative strength of the two polarisations, the total mass, and the aligned-spin components. We also measure the "precession SNR" $\rho_p$, which was introduced in Refs[1,2] to quantify the signal power associated with precession. By comparing $\rho_p$ with both Bayes factors and the recovered posterior distributions, we find it is a reliable metric for measurability that accurately predicts when the detected signal contains evidence for precession.
求助全文
通过发布文献求助,成功后即可免费获取论文全文。 去求助
来源期刊
自引率
0.00%
发文量
0
×
引用
GB/T 7714-2015
复制
MLA
复制
APA
复制
导出至
BibTeX EndNote RefMan NoteFirst NoteExpress
×
提示
您的信息不完整,为了账户安全,请先补充。
现在去补充
×
提示
您因"违规操作"
具体请查看互助需知
我知道了
×
提示
确定
请完成安全验证×
copy
已复制链接
快去分享给好友吧!
我知道了
右上角分享
点击右上角分享
0
联系我们:info@booksci.cn Book学术提供免费学术资源搜索服务,方便国内外学者检索中英文文献。致力于提供最便捷和优质的服务体验。 Copyright © 2023 布克学术 All rights reserved.
京ICP备2023020795号-1
ghs 京公网安备 11010802042870号
Book学术文献互助
Book学术文献互助群
群 号:481959085
Book学术官方微信