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arxiv 1405.7016 v2 pith:AEGM2SIX submitted 2014-05-27 astro-ph.HE gr-qc

Double Compact Objects III: Gravitational Wave Detection Rates

M. Dominik , E. Berti , R. O'Shaughnessy , I. Mandel , K. Belczynski , C.Fryer , D. Holz , T. Bulik
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F. Pannarale
This is my paper
classification astro-ph.HE gr-qc
keywords ratessystemsbh-bhbh-nsdetectionmodelsns-nsbinary
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved
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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 (IMR) 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 $\sim 1.5$ 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.

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