DOUBLE COMPACT OBJECTS. III. GRAVITATIONAL-WAVE DETECTION RATES

被引：360

作者：

Dominik, Michal ^{[1
]}

Berti, Emanuele ^{[2
]}

O'Shaughnessy, Richard ^{[3
]}

Mandel, Ilya ^{[4
]}

Belczynski, Krzysztof ^{[1
,5
]}

Fryer, Christopher ^{[6
]}

Holz, Daniel E. ^{[7
,8
]}

Bulik, Tomasz ^{[1
]}

Pannarale, Francesco ^{[9
]}

机构：

[1] Univ Warsaw, Astron Observ, PL-00478 Warsaw, Poland

[2] Univ Mississippi, Dept Phys & Astron, University, MS 38677 USA

[3] Univ Wisconsin, Ctr Gravitat Cosmol & Astrophys, Milwaukee, WI 53201 USA

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

[5] Univ Texas Brownsville, Ctr Gravitat Wave Astron, Brownsville, TX 78520 USA

[6] Los Alamos Natl Lab, Los Alamos, NM 87545 USA

[7] Univ Chicago, Enrico Fermi Inst, Dept Phys, Chicago, IL 60637 USA

[8] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA

[9] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales

来源：

ASTROPHYSICAL JOURNAL | 2015年 / 806卷 / 02期

基金：

美国国家科学基金会;

关键词：

binaries: close; gravitational waves; stars: black holes; stars: neutron; MASS BLACK-HOLES; GAMMA-RAY BURSTS; NEUTRON-STAR BINARIES; ATMOSPHERIC STRUCTURE; RELATIVISTIC GRAVITY; GLOBULAR-CLUSTERS; COMMON ENVELOPE; EVOLUTION; MERGERS; METALLICITY;

D O I：

10.1088/0004-637X/806/2/263

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The unprecedented range of second-generation gravitational-wave (GW) observatories calls for refining the predictions of potential sources and detection rates. The coalescence of double compact objects (DCOs)-i.e., neutron star-neutron star (NS-NS), black hole-neutron star (BH-NS), and black hole-black hole (BH-BH) binary systems-is the most promising source of GWs for these detectors. We compute detection rates of coalescing DCOs in second-generation GW detectors using the latest models for their cosmological evolution, and implementing inspiral-merger-ringdown gravitational waveform models in our signal-to-noise ratio calculations. We find that (1) the inclusion of the merger/ringdown portion of the signal does not significantly affect rates for NS-NS and BH-NS systems, but it boosts rates by a factor of similar to 1.5 for BH-BH systems; (2) in almost all of our models BH-BH systems yield by far the largest rates, followed by NS-NS and BH-NS systems, respectively; and (3) a majority of the detectable BH-BH systems were formed in the early universe in low-metallicity environments. We make predictions for the distributions of detected binaries and discuss what the first GW detections will teach us about the astrophysics underlying binary formation and evolution.

引用

页数：18

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