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The rate of binary black hole mergers inferred from advanced LIGO observations surrounding GW150914

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dc.contributor.authorAbbott, B.P.
dc.contributor.authorAbbott, R.
dc.contributor.authorAbbott, T.D.
dc.contributor.authorAbernathy, M.R.
dc.contributor.authorAcernese, F.
dc.contributor.authorAckley, K.
dc.contributor.authorAdams, C.
dc.contributor.authorAdams, T.
dc.contributor.authorAddesso, P.
dc.contributor.authorAdhikari, R.X.
dc.contributor.authorAdya, V.B.
dc.contributor.authorAffeldt, C.
dc.contributor.authorAgathos, M.
dc.contributor.authorAgatsuma, K.
dc.contributor.authorAggarwal, N.
dc.contributor.authorAguiar, O.D.
dc.contributor.authorAiello, L.
dc.contributor.authorAin, A.
dc.contributor.authorAjith, P.
dc.contributor.authorAllen, B.
dc.contributor.authoret al.
dc.date.issued2016
dc.description.abstractA 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 identi fies its source as a binary black hole ( BBH ) merger with component masses (m₁m₂)= (36⁺⁵−₄,29⁺⁴−₄) Μₒ at redshift z = 0.09 ⁺0.03 −0.04 (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 range2-600 Gpc⁻3 yr⁻1
dc.description.statementofresponsibilityAbbott, BP ... Hollitt, SE ... Ottaway, DJ, LIGO Scientific Collaboration and Virgo Collaboration
dc.identifier.citationAstrophysical Journal Letters, 2016; 833(1):1-8
dc.identifier.doi10.3847/2041-8205/833/1/L1
dc.identifier.issn2041-8205
dc.identifier.issn2041-8213
dc.identifier.orcidBrown, D.D. [0000-0001-7851-3939]
dc.identifier.orcidHollitt, S.E. [0000-0002-4962-3546]
dc.identifier.orcidKijbunchoo, N. [0000-0002-2874-1228]
dc.identifier.orcidOttaway, D.J. [0000-0001-6794-1591]
dc.identifier.orcidVeitch, P.J. [0000-0002-2597-435X]
dc.identifier.urihttp://hdl.handle.net/2440/103644
dc.language.isoen
dc.publisherAmerican Astronomical Society
dc.rights© 2016. The American Astronomical Society. All rights reserved.
dc.source.urihttps://doi.org/10.3847/2041-8205/833/1/l1
dc.subjectblack holes; gravitational waves; stars: massive
dc.titleThe rate of binary black hole mergers inferred from advanced LIGO observations surrounding GW150914
dc.typeJournal article
pubs.publication-statusPublished

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