Properties of the Binary Black Hole Merger GW150914.
B P Abbott,R Abbott, T D Abbott,M R Abernathy,F Acernese,K Ackley,C Adams,T Adams,P Addesso,R X Adhikari,V B Adya, C Affeldt,M Agathos,K Agatsuma,N Aggarwal,O D Aguiar,L Aiello,A Ain,P Ajith,B Allen,A Allocca,P A Altin,S B Anderson,W G Anderson,K Arai,M C Araya, C C Arceneaux, J S Areeda,N Arnaud,K G Arun,S Ascenzi,G Ashton,M Ast,S M Aston, P Astone,P Aufmuth, C Aulbert, S Babak, P Bacon, M K M Bader,P T Baker, F Baldaccini,G Ballardin, S W Ballmer, J C Barayoga, S E Barclay, B C Barish,D Barker,F Barone,B Barr,L Barsotti, M Barsuglia,D Barta,J Bartlett,I Bartos,R Bassiri, A Basti, J C Batch,C Baune,V Bavigadda,M Bazzan,B Behnke,M Bejger, A S Bell, C J Bell,B K Berger,J Bergman,G Bergmann,C P L Berry,D Bersanetti,A Bertolini, J Betzwieser,S Bhagwat, R Bhandare, I A Bilenko, G Billingsley, J Birch,R Birney,O Birnholtz,S Biscans,A Bisht,M Bitossi, C Biwer,M A Bizouard, J K Blackburn,C D Blair, D G Blair, R M Blair,S Bloemen,O Bock, T P Bodiya,M Boer, G Bogaert, C Bogan, A Bohe, P 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PHYSICAL REVIEW LETTERS（2016）
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摘要
On September 14, 2015, the Laser Interferometer Gravitational-Wave Observatory (LIGO) detected a gravitational-wave transient (GW150914); we characterize the properties of the source and its parameters. The data around the time of the event were analyzed coherently across the LIGO network using a suite of accurate waveform models that describe gravitational waves from a compact binary system in general relativity. GW150914 was produced by a nearly equal mass binary black hole of masses 36_{-4}^{+5}M_{⊙} and 29_{-4}^{+4}M_{⊙}; for each parameter we report the median value and the range of the 90% credible interval. The dimensionless spin magnitude of the more massive black hole is bound to be <0.7 (at 90% probability). The luminosity distance to the source is 410_{-180}^{+160} Mpc, corresponding to a redshift 0.09_{-0.04}^{+0.03} assuming standard cosmology. The source location is constrained to an annulus section of 610 deg^{2}, primarily in the southern hemisphere. The binary merges into a black hole of mass 62_{-4}^{+4}M_{⊙} and spin 0.67_{-0.07}^{+0.05}. This black hole is significantly more massive than any other inferred from electromagnetic observations in the stellar-mass regime.
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