Journal
ASTROPHYSICAL JOURNAL LETTERS
Volume 833, Issue 1, Pages -Publisher
IOP Publishing Ltd
DOI: 10.3847/2041-8205/833/1/L1
Keywords
black holes; gravitational waves; stars: massive
Categories
Funding
- Council of Scientific and Industrial Research of India
- Department of Science and Technology, India
- Science & Engineering Research Board (SERB), India
- Ministry of Human Resource Development, India
- Spanish Ministerio de Economia y Competitividad
- Conselleria d'Economia i Competitivitat
- Conselleria d'Educacio Cultura i Universitats of the Govern de les Illes Balears
- National Science Centre of Poland
- European Commission
- Royal Society
- Scottish Funding Council
- Scottish Universities Physics Alliance
- Hungarian Scientific Research Fund (OTKA)
- Lyon Institute of Origins (LIO)
- National Research Foundation of Korea
- Industry Canada
- Province of Ontario through the Ministry of Economic Development and Innovation
- Natural Science and Engineering Research Council Canada
- Canadian Institute for Advanced Research
- Brazilian Ministry of Science, Technology, and Innovation
- Russian Foundation for Basic Research
- Leverhulme Trust
- Ministry of Science and Technology (MOST), Taiwan
- Kavli Foundation
- Direct For Education and Human Resources
- Division Of Graduate Education [1450006] Funding Source: National Science Foundation
- Direct For Mathematical & Physical Scien
- Division Of Physics [1104371, 1505373, 1404139, 1607585, 1607709, 1151836] Funding Source: National Science Foundation
- Direct For Mathematical & Physical Scien
- Division Of Physics [1505629, 1307401, 1506360, 1205882, 1125897, 1505779] Funding Source: National Science Foundation
- Office of Advanced Cyberinfrastructure (OAC)
- Direct For Computer & Info Scie & Enginr [1443047] Funding Source: National Science Foundation
- Science and Technology Facilities Council [ST/J000345/1, ST/I000887/1 Gravitational Waves, ST/I006269/1 Gravitational Waves, ST/N000633/1, ST/L000962/1, ST/K005014/1, PPA/G/S/2002/00652, ST/N000064/1, ST/L000954/1, ST/I006269/1, ST/N005716/1, ST/H002006/1, ST/J00166X/1, ST/N000080/1, ST/M004090/1, ST/K000845/1, ST/J000345/1 Gravitational Waves, ST/I006242/1, ST/N000072/1, ST/I006285/1, ST/I000887/1, ST/N005430/1, ST/L000962/1 Gravitational Waves, ST/I006285/1 Gravitational Waves] Funding Source: researchfish
- STFC [ST/H002006/1, ST/K000845/1, ST/N005430/1, ST/I006269/1, ST/I000887/1, ST/N000633/1, ST/I006285/1, ST/L000962/1, PPA/G/S/2002/00652, ST/K005014/1, PP/C505791/1, ST/N000064/1, ST/N000072/1, ST/N005716/1, ST/J00166X/1, ST/J000345/1, ST/L000954/1, ST/I006242/1, ST/M004090/1, ST/N000080/1] Funding Source: UKRI
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A transient gravitational-wave signal, GW150914, was identified in the twin Advanced LIGO detectors on 2015 September 2015 at 09: 50: 45 UTC. To assess the implications of this discovery, the detectors remained in operation with unchanged configurations over a period of 39 days around the time of the signal. At the detection statistic threshold corresponding to that observed for GW150914, our search of the 16 days of simultaneous two-detector observational data is estimated to have a false-alarm rate (FAR) of <4.9 x 10(-6) yr(-1), yielding a p-value for GW150914 of <2 x 10(-7). Parameter estimation follow-up on this trigger identifies its source as a binary black hole (BBH) merger with component masses (m(1), m(2)) = (36(-4)(+5), 29(-4)(+4))M-circle dot at redshift z = 0.09(-0.04)(+0.03) (median and 90% credible range). Here, we report on the constraints these observations place on the rate of BBH coalescences. Considering only GW150914, assuming that all BBHs in the universe have the same masses and spins as this event, imposing a search FAR threshold of 1 per 100 years, and assuming that the BBH merger rate is constant in the comoving frame, we infer a 90% credible range of merger rates between 2-53 Gpc(-3) yr(-1)(comoving frame). Incorporating all search triggers that pass a much lower threshold while accounting for the uncertainty in the astrophysical origin of each trigger, we estimate a higher rate, ranging from 13-600 Gpc(-3) yr(-1) depending on assumptions about the BBH mass distribution. All together, our various rate estimates fall in the conservative range 2-600 Gpc(-3) yr(-1).
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