Inference on gravitational waves from coalescences of stellar-mass compact objects and intermediate-mass black holes

被引：40

作者：

Haster, Carl-Johan ^{[1
]}

Wang, Zhilu ^{[1
,2
]}

Berry, Christopher P. L. ^{[1
]}

Stevenson, Simon ^{[1
]}

Veitch, John ^{[1
]}

Mandel, Ilya ^{[1
]}

机构：

[1] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England

[2] Univ Sci & Technol China, Dept Modern Phys, 96 JinZhai Rd, Hefei 230026, Anhui, Peoples R China

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2016年 / 457卷 / 04期

基金：

美国国家科学基金会; 英国科学技术设施理事会;

关键词：

black hole physics; gravitational waves; methods: data analysis; RATIO INSPIRALS; ADVANCED LIGO; BINARIES;

D O I：

10.1093/mnras/stw233

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Gravitational waves from coalescences of neutron stars or stellar-mass black holes into intermediate-mass black holes (IMBHs) of greater than or similar to 100 solar masses represent one of the exciting possible sources for advanced gravitational-wave detectors. These sources can provide definitive evidence for the existence of IMBHs, probe globular-cluster dynamics, and potentially serve as tests of general relativity. We analyse the accuracy with which we can measure the masses and spins of the IMBH and its companion in intermediate-mass-ratio coalescences. We find that we can identify an IMBH with a mass above 100 M-circle dot with 95 per cent confidence provided the massive body exceeds 130 M-circle dot. For source masses above similar to 200 M-circle dot, the best measured parameter is the frequency of the quasi-normal ringdown. Consequently, the total mass is measured better than the chirp mass for massive binaries, but the total mass is still partly degenerate with spin, which cannot be accurately measured. Low-frequency detector sensitivity is particularly important for massive sources, since sensitivity to the inspiral phase is critical for measuring the mass of the stellar-mass companion. We show that we can accurately infer source parameters for cosmologically redshifted signals by applying appropriate corrections. We investigate the impact of uncertainty in the model gravitational waveforms and conclude that our main results are likely robust to systematics.

引用

页码：4499 / 4506

页数：8

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