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dc.contributor.authorAbbott, BPen_US
dc.contributor.authorAbbott, Ren_US
dc.contributor.authorAbbott, TDen_US
dc.contributor.authorAbernathy, MRen_US
dc.contributor.authorAcernese, Fen_US
dc.contributor.authorAckley, Ken_US
dc.contributor.authorAdams, Cen_US
dc.contributor.authorAdams, Ten_US
dc.contributor.authorAddesso, Pen_US
dc.contributor.authorAdhikari, RXen_US
dc.contributor.authorAdya, VBen_US
dc.contributor.authorAffeldt, Cen_US
dc.contributor.authorAgathos, Men_US
dc.contributor.authorAgatsuma, Ken_US
dc.contributor.authorAggarwal, Nen_US
dc.contributor.authorAguiar, ODen_US
dc.contributor.authorAiello, Len_US
dc.contributor.authorAin, Aen_US
dc.contributor.authorAjith, Pen_US
dc.contributor.authorAllen, Ben_US
dc.contributor.authorAllocca, Aen_US
dc.contributor.authorAltin, PAen_US
dc.contributor.authorAnderson, SBen_US
dc.contributor.authorAnderson, WGen_US
dc.contributor.authorArai, Ken_US
dc.contributor.authorAraya, MCen_US
dc.contributor.authorArceneaux, CCen_US
dc.contributor.authorAreeda, JSen_US
dc.contributor.authorArnaud, Nen_US
dc.contributor.authorArun, KGen_US
dc.contributor.authorAscenzi, Sen_US
dc.contributor.authorAshton, Gen_US
dc.contributor.authorAst, Men_US
dc.contributor.authorAston, SMen_US
dc.contributor.authorAstone, Pen_US
dc.contributor.authorAufmuth, Pen_US
dc.contributor.authorAulbert, Cen_US
dc.contributor.authorBabak, Sen_US
dc.contributor.authorBacon, Pen_US
dc.contributor.authorBader, MKMen_US
dc.contributor.authorBaker, PTen_US
dc.contributor.authorBaldaccini, Fen_US
dc.contributor.authorBallardin, Gen_US
dc.contributor.authorBallmer, SWen_US
dc.contributor.authorBarayoga, JCen_US
dc.contributor.authorBarclay, SEen_US
dc.contributor.authorBarish, BCen_US
dc.contributor.authorBarker, Den_US
dc.contributor.authorBarone, Fen_US
dc.contributor.authorBarr, Ben_US
dc.contributor.authorBarsotti, Len_US
dc.contributor.authorBarsuglia, Men_US
dc.contributor.authorBarta, Den_US
dc.contributor.authorBartlett, Jen_US
dc.contributor.authorBartos, Ien_US
dc.contributor.authorBassiri, Ren_US
dc.contributor.authorBasti, Aen_US
dc.contributor.authorBatch, JCen_US
dc.contributor.authorBaune, Cen_US
dc.contributor.authorBavigadda, Ven_US
dc.contributor.authorBazzan, Men_US
dc.contributor.authorBejger, Men_US
dc.contributor.authorBell, ASen_US
dc.contributor.authorBerger, BKen_US
dc.contributor.authorBergmann, Gen_US
dc.contributor.authorBerry, CPLen_US
dc.contributor.authorBersanetti, Den_US
dc.contributor.authorBertolini, Aen_US
dc.contributor.authorBetzwieser, Jen_US
dc.contributor.authorBhagwat, Sen_US
dc.contributor.authorBhandare, Ren_US
dc.contributor.authorBilenko, IAen_US
dc.contributor.authorBillingsley, Gen_US
dc.contributor.authorBirch, Jen_US
dc.contributor.authorBirney, Ren_US
dc.contributor.authorBiscans, Sen_US
dc.contributor.authorBisht, Aen_US
dc.contributor.authorBitossi, Men_US
dc.contributor.authorBiwer, Cen_US
dc.contributor.authorBizouard, MAen_US
dc.contributor.authorBlackburn, JKen_US
dc.contributor.authorBlair, CDen_US
dc.contributor.authorBlair, DGen_US
dc.contributor.authorBlair, RMen_US
dc.contributor.authorBloemen, Sen_US
dc.contributor.authorBock, Oen_US
dc.contributor.authorBoer, Men_US
dc.date.accessioned2017-05-19T10:03:38Z
dc.date.available2016-06-10en_US
dc.date.issued2016-09-14en_US
dc.date.submitted2017-05-16T13:34:30.524Z
dc.identifier.issn1550-7998en_US
dc.identifier.urihttp://qmro.qmul.ac.uk/xmlui/handle/123456789/23181
dc.description.abstract© 2016 American Physical Society.We compare GW150914 directly to simulations of coalescing binary black holes in full general relativity, including several performed specifically to reproduce this event. Our calculations go beyond existing semianalytic models, because for all simulations - including sources with two independent, precessing spins - we perform comparisons which account for all the spin-weighted quadrupolar modes, and separately which account for all the quadrupolar and octopolar modes. Consistent with the posterior distributions reported by Abbott et al. [Phys. Rev. Lett. 116, 241102 (2016)] (at the 90% credible level), we find the data are compatible with a wide range of nonprecessing and precessing simulations. Follow-up simulations performed using previously estimated binary parameters most resemble the data, even when all quadrupolar and octopolar modes are included. Comparisons including only the quadrupolar modes constrain the total redshifted mass Mz [64 M-82 M], mass ratio 1/q=m2/m1 [0.6,1], and effective aligned spin χeff [-0.3,0.2], where χeff=(S1/m1+S2/m2)·L/M. Including both quadrupolar and octopolar modes, we find the mass ratio is even more tightly constrained. Even accounting for precession, simulations with extreme mass ratios and effective spins are highly inconsistent with the data, at any mass. Several nonprecessing and precessing simulations with similar mass ratio and χeff are consistent with the data. Though correlated, the components' spins (both in magnitude and directions) are not significantly constrained by the data: the data is consistent with simulations with component spin magnitudes a1,2 up to at least 0.8, with random orientations. Further detailed follow-up calculations are needed to determine if the data contain a weak imprint from transverse (precessing) spins. For nonprecessing binaries, interpolating between simulations, we reconstruct a posterior distribution consistent with previous results. The final black hole's redshifted mass is consistent with Mf,z in the range 64.0 M-73.5 M and the final black hole's dimensionless spin parameter is consistent with af=0.62-0.73. As our approach invokes no intermediate approximations to general relativity and can strongly reject binaries whose radiation is inconsistent with the data, our analysis provides a valuable complement to Abbott et al. [Phys. Rev. Lett. 116, 241102 (2016)].en_US
dc.relation.ispartofPhysical Review D - Particles, Fields, Gravitation and Cosmologyen_US
dc.titleDirectly comparing GW150914 with numerical solutions of Einstein's equations for binary black hole coalescenceen_US
dc.typeArticle
dc.rights.holder© 2016 American Physical Society
dc.identifier.doi10.1103/PhysRevD.94.064035en_US
pubs.declined2017-05-16T13:34:30.49+0100
pubs.issue6en_US
pubs.notesNot knownen_US
pubs.publication-statusPublisheden_US
pubs.volume94en_US
dcterms.dateAccepted2016-06-10en_US


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