Journal
ASTROPHYSICAL JOURNAL
Volume 806, Issue 2, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/806/2/263
Keywords
binaries: close; gravitational waves; stars: black holes; stars: neutron
Categories
Funding
- Polish Science Foundation
- Polish NCN grant SONATA BIS 2
- NASA [NNX09AV06A]
- NSF [HRD 1242090, PHY-0970074]
- National Science Center [DEC-2011/01/N/ST9/00383]
- National Science Foundation CAREER Grant [PHY-1055103, PHY-1151836]
- UWM Research Growth Initiative
- Kavli Institute for Cosmological Physics at the University of Chicago through NSF [PHY-1125897]
- National Science Center, Poland [DPN/N176/VIRGO/2009, DEC-2013/01/ASPERA/ST9/00001]
- STFC [ST/L000342/1]
- National Science Foundation [PHYS-1066293]
- National Science Center grant Sonata Bis 2 [DEC-2012/07/E/ST9/01360]
- STFC [Gravitational Waves, ST/K000845/1, ST/I006269/1, ST/L000342/1] Funding Source: UKRI
- Science and Technology Facilities Council [ST/L000342/1, ST/K000845/1, Gravitational Waves] Funding Source: researchfish
- Division Of Physics
- Direct For Mathematical & Physical Scien [1055103] Funding Source: National Science Foundation
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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 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.
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