Predictions for the rates of compact binary coalescences observable by ground-based gravitational-wave detectors
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Author(s)
Barsotti, Lisa
Blackburn, Lindy L.
Bodiya, Timothy P.
Corbitt, Thomas R
Donovan, Frederick J
Evans, M
Fritschel, Peter K
Harry, G. M
Hughey, Barbara
Katsavounidis, Erotokritos
Date Issued
July 2010
Journal
Classical and Quantum Gravity
Publisher
IOP Publishing
Citation
Abadie, J. et al. “Predictions for the Rates of Compact Binary Coalescences Observable by Ground-Based Gravitational-Wave Detectors.” Classical and Quantum Gravity 27, 17 (July 2010): 173001. © 2010 IOP Publishing Ltd.
Version
Original manuscript
Abstract
We present an up-to-date, comprehensive summary of the rates for all types of compact binary coalescence sources detectable by the initial and advanced versions of the ground-based gravitational-wave detectors LIGO and Virgo. Astrophysical estimates for compact-binary coalescence rates depend on a number of assumptions and unknown model parameters and are still uncertain. Themost confident among these estimates are the rate predictions for coalescing binary neutron stars which are based on extrapolations from observed binary pulsars in our galaxy. These yield a likely coalescence rate of 100 Myr -1 per MilkyWay Equivalent Galaxy (MWEG), although the rate could plausibly range from 1 Myr -1 MWEG -1 to 1000 Myr -1 MWEG -1 (Kalogera et al 2004 Astrophys. J. 601 L179; Kalogera et al 2004 Astrophys. J. 614 L137 (erratum)). We convert coalescence rates into detection rates based on data from the LIGO S5 and Virgo VSR2 science runs and projected sensitivities for our advanced detectors. Using the detector sensitivities derived from these data, we find a likely detection rate of 0.02 per year for Initial LIGO-Virgo interferometers, with a plausible range between 2 × 10 -4 and 0.2 per year. The likely binary neutron-star detection rate for the Advanced LIGO-Virgo network increases to 40 events per year, with a range between 0.4 and 400 per year.
MIT Department
Lincoln Laboratory
MIT Kavli Institute for Astrophysics and Space Research
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DOI of Published Version
https://doi.org/10.1088/0264-9381/27/17/173001
