On the gravitational wave background from compact binary coalescences in the band of ground-based interferometers

被引：108

作者：

Zhu, Xing-Jiang ^{[1
]}

Howell, Eric J. ^{[1
]}

Blair, David G. ^{[1
]}

Zhu, Zong-Hong ^{[2
]}

机构：

[1] Univ Western Australia, Sch Phys, Crawley, WA 6009, Australia

[2] Beijing Normal Univ, Dept Astron, Beijing 100875, Peoples R China

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2013年 / 431卷 / 01期

基金：

中国国家自然科学基金;

关键词：

gravitational waves; binaries: close; cosmology: miscellaneous; DELAY-TIME DISTRIBUTION; BLACK-HOLE; STAR-FORMATION; MASS-DISTRIBUTION; STELLAR-MASS; COSMOLOGICAL POPULATION; IA SUPERNOVAE; MERGER RATE; CYG X-1; PROSPECTS;

D O I：

10.1093/mnras/stt207

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

This paper reports a comprehensive study on the gravitational wave (GW) background from compact binary coalescences. We consider in our calculations newly available observation-based neutron star and black hole mass distributions and complete analytical waveforms that include post-Newtonian amplitude corrections. Our results show that: (i) post-Newtonian effects cause a small reduction in the GW background signal; (ii) below 100 Hz the background depends primarily on the local coalescence rate r(0) and the average chirp mass and is independent of the chirp mass distribution; (iii) the effects of cosmic star formation rates and delay times between the formation and merger of binaries are linear below 100 Hz and can be represented by a single parameter within a factor of similar to 2; (iv) a simple power-law model of the energy density parameter Omega(GW)(f) similar to f(2/3) up to 50-100 Hz is sufficient to be used as a search template for ground-based interferometers. In terms of detection prospects of this background signal, we show that: (i) detection (a signal-to-noise ratio of 3) within one year of observation by the Advanced Laser Interferometer Gravitational-wave Observatory (LIGO) detectors (H1-L1) requires a coalescence rate of r(0) = 3 (0.2) Mpc(-3) Myr(-1) for binary neutron stars (binary black holes); (ii) this limit on r(0) could be reduced threefold for two co-located and co-aligned detectors, whereas the currently proposed worldwide network of advanced instruments gives only similar to 30 per cent improvement in detectability; (iii) the improved sensitivity of the planned Einstein Telescope allows not only confident detection of the background but also the high-frequency components of the spectrum to be measured, possibly enabling rate evolutionary histories and mass distributions to be probed. Finally, we show that sub-threshold binary neutron star merger events produce a strong foreground, which could be an issue for future terrestrial stochastic searches of primordial GWs.

引用

页码：882 / 899

页数：18

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