GW150914: Implications for the stochastic gravitational-wave background from binary black holes

LIGO Scientific Collaboration and Virgo Collaborations

doi:10.1103/PhysRevLett.116.131102

GW150914: Implications for the stochastic gravitational-wave background from binary black holes

LIGO Scientific Collaboration and Virgo Collaborations

Physics

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Abstract

The LIGO detection of the gravitational wave transient GW150914, from the inspiral and merger of two black holes with masses 30M, suggests a population of binary black holes with relatively high mass. This observation implies that the stochastic gravitational-wave background from binary black holes, created from the incoherent superposition of all the merging binaries in the Universe, could be higher than previously expected. Using the properties of GW150914, we estimate the energy density of such a background from binary black holes. In the most sensitive part of the Advanced LIGO and Advanced Virgo band for stochastic backgrounds (near 25 Hz), we predict ΩGW(f=25 Hz)=1.1-0.9+2.7×10-9 with 90% confidence. This prediction is robustly demonstrated for a variety of formation scenarios with different parameters. The differences between models are small compared to the statistical uncertainty arising from the currently poorly constrained local coalescence rate. We conclude that this background is potentially measurable by the Advanced LIGO and Advanced Virgo detectors operating at their projected final sensitivity.

Original language	English
Article number	131102
Journal	Physical Review Letters
Volume	116
Issue number	13
DOIs	https://doi.org/10.1103/PhysRevLett.116.131102
Publication status	Published - 31 Mar 2016

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10.1103/PhysRevLett.116.131102

Abbott et al., 2016 GW150914_ Implications
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@article{d1597653224e4c7ba825d16664b3c560,

title = "GW150914: Implications for the stochastic gravitational-wave background from binary black holes",

abstract = "The LIGO detection of the gravitational wave transient GW150914, from the inspiral and merger of two black holes with masses 30M, suggests a population of binary black holes with relatively high mass. This observation implies that the stochastic gravitational-wave background from binary black holes, created from the incoherent superposition of all the merging binaries in the Universe, could be higher than previously expected. Using the properties of GW150914, we estimate the energy density of such a background from binary black holes. In the most sensitive part of the Advanced LIGO and Advanced Virgo band for stochastic backgrounds (near 25 Hz), we predict ΩGW(f=25 Hz)=1.1-0.9+2.7{\texttimes}10-9 with 90\% confidence. This prediction is robustly demonstrated for a variety of formation scenarios with different parameters. The differences between models are small compared to the statistical uncertainty arising from the currently poorly constrained local coalescence rate. We conclude that this background is potentially measurable by the Advanced LIGO and Advanced Virgo detectors operating at their projected final sensitivity.",

author = "\{LIGO Scientific Collaboration and Virgo Collaborations\} and Abbott, \{B. P.\} and R. Abbott and Abbott, \{T. D.\} and Abernathy, \{M. R.\} and F. Acernese and K. Ackley and C. Adams and T. Adams and P. Addesso and Adhikari, \{R. X.\} and Adya, \{V. B.\} and C. Affeldt and M. Agathos and K. Agatsuma and N. Aggarwal and Aguiar, \{O. D.\} and L. Aiello and A. Ain and P. Ajith and B. Allen and A. Allocca and Altin, \{P. A.\} and Anderson, \{S. B.\} and Anderson, \{W. G.\} and K. Arai and Araya, \{M. C.\} and Arceneaux, \{C. C.\} and Areeda, \{J. S.\} and N. Arnaud and Arun, \{K. G.\} and S. Ascenzi and G. Ashton and M. Ast and Aston, \{S. M.\} and P. Astone and P. Aufmuth and C. Aulbert and S. Babak and P. Bacon and Bader, \{M. K.M.\} and Baker, \{P. T.\} and F. Baldaccini and G. Ballardin and Ballmer, \{S. W.\} and Barayoga, \{J. C.\} and Barclay, \{S. E.\} and Barish, \{B. C.\} and D. Barker and F. Barone and B. Barr and L. Barsotti and M. Barsuglia and D. Barta and J. Bartlett and I. Bartos and R. Bassiri and A. Basti and Batch, \{J. C.\} and C. Baune and V. Bavigadda and M. Bazzan and B. Behnke and M. Bejger and Bell, \{A. S.\} and Bell, \{C. J.\} and Berger, \{B. K.\} and J. Bergman and G. Bergmann and Berry, \{C. P.L.\} and D. Bersanetti and A. Bertolini and J. Betzwieser and S. Bhagwat and R. Bhandare and Bilenko, \{I. A.\} and G. Billingsley and J. Birch and R. Birney and S. Biscans and A. Bisht and M. Bitossi and C. Biwer and Bizouard, \{M. A.\} and Blackburn, \{J. K.\} and Blair, \{C. D.\} and Blair, \{D. G.\} and Blair, \{R. M.\} and S. Bloemen and O. Bock and Bodiya, \{T. P.\} and M. Boer and G. Bogaert and C. Bogan and A. Bohe and P. Bojtos and C. Bond and F. Bondu and R. Bonnand and Boom, \{B. A.\} and R. Bork and V. Boschi and S. Bose and Y. Bouffanais and A. Bozzi and C. Bradaschia and Brady, \{P. R.\} and Braginsky, \{V. B.\} and M. Branchesi and Brau, \{J. E.\} and T. Briant and A. Brillet and M. Brinkmann and V. Brisson and P. Brockill and Brooks, \{A. F.\} and Brown, \{D. D.\} and Brown, \{N. M.\} and Buchanan, \{C. C.\} and A. Buikema and T. Bulik and Bulten, \{H. J.\} and A. Buonanno and D. Buskulic and C. Buy and Byer, \{R. L.\} and L. Cadonati and G. Cagnoli and C. Cahillane and Bustillo, \{J. Calder{\'o}n\} and T. Callister and E. Calloni and Camp, \{J. B.\} and Cannon, \{K. C.\} and J. Cao and Capano, \{C. D.\} and E. Capocasa and F. Carbognani and S. Caride and Diaz, \{J. Casanueva\} and C. Casentini and S. Caudill and M. Cavagli{\`a} and F. Cavalier and R. Cavalieri and G. Cella and Cepeda, \{C. B.\} and Baiardi, \{L. Cerboni\} and G. Cerretani and E. Cesarini and R. Chakraborty and T. Chalermsongsak and Chamberlin, \{S. J.\} and M. Chan and S. Chao and P. Charlton and E. Chassande-Mottin and Chen, \{H. Y.\} and Y. Chen and C. Cheng and A. Chincarini and A. Chiummo and Cho, \{H. S.\} and M. Cho and Chow, \{J. H.\} and N. Christensen and Q. Chu and S. Chua and S. Chung and G. Ciani and F. Clara and Clark, \{J. A.\} and F. Cleva and E. Coccia and Cohadon, \{P. F.\} and A. Colla and Collette, \{C. G.\} and L. Cominsky and M. Constancio and A. Conte and L. Conti and D. Cook and Corbitt, \{T. R.\} and N. Cornish and A. Corsi and S. Cortese and Costa, \{C. A.\} and Coughlin, \{M. W.\} and Coughlin, \{S. B.\} and Coulon, \{J. P.\} and Countryman, \{S. T.\} and P. Couvares and Cowan, \{E. E.\} and Coward, \{D. M.\} and Cowart, \{M. J.\} and Coyne, \{D. C.\} and R. Coyne and K. Craig and Creighton, \{J. D.E.\} and J. Cripe and Crowder, \{S. G.\} and A. Cumming and L. Cunningham and E. Cuoco and Canton, \{T. Dal\} and Danilishin, \{S. L.\} and S. D'Antonio and K. Danzmann and Darman, \{N. S.\} and V. Dattilo and I. Dave and Daveloza, \{H. P.\} and M. Davier and Davies, \{G. S.\} and Daw, \{E. J.\} and R. Day and D. Debra and G. Debreczeni and J. Degallaix and \{De Laurentis\}, M. and S. Del{\'e}glise and \{Del Pozzo\}, W. and T. Denker and T. Dent and H. Dereli and V. Dergachev and Derosa, \{R. T.\} and \{De Rosa\}, R. and R. Desalvo and S. Dhurandhar and D{\'i}az, \{M. C.\} and \{Di Fiore\}, L. and \{Di Giovanni\}, M. and \{Di Lieto\}, A. and \{Di Pace\}, S. and \{Di Palma\}, I. and \{Di Virgilio\}, A. and G. Dojcinoski and V. Dolique and F. Donovan and Dooley, \{K. L.\} and S. Doravari and R. Douglas and Downes, \{T. P.\} and B. Gendre and Howell, \{E. J.\} and L. Ju and \{Van Heijningen\}, \{J. V.\} and L. Wen and C. Zhao and Zhu, \{X. J.\}",

year = "2016",

month = mar,

day = "31",

doi = "10.1103/PhysRevLett.116.131102",

language = "English",

volume = "116",

journal = "Physical Review Letters",

issn = "0031-9007",

publisher = "American Physical Society",

number = "13",

}

TY - JOUR

T1 - GW150914: Implications for the stochastic gravitational-wave background from binary black holes

AU - LIGO Scientific Collaboration and Virgo Collaborations

AU - Abbott, B. P.

AU - Abbott, R.

AU - Abbott, T. D.

AU - Abernathy, M. R.

AU - Acernese, F.

AU - Ackley, K.

AU - Adams, C.

AU - Adams, T.

AU - Addesso, P.

AU - Adhikari, R. X.

AU - Adya, V. B.

AU - Affeldt, C.

AU - Agathos, M.

AU - Agatsuma, K.

AU - Aggarwal, N.

AU - Aguiar, O. D.

AU - Aiello, L.

AU - Ain, A.

AU - Ajith, P.

AU - Allen, B.

AU - Allocca, A.

AU - Altin, P. A.

AU - Anderson, S. B.

AU - Anderson, W. G.

AU - Arai, K.

AU - Araya, M. C.

AU - Arceneaux, C. C.

AU - Areeda, J. S.

AU - Arnaud, N.

AU - Arun, K. G.

AU - Ascenzi, S.

AU - Ashton, G.

AU - Ast, M.

AU - Aston, S. M.

AU - Astone, P.

AU - Aufmuth, P.

AU - Aulbert, C.

AU - Babak, S.

AU - Bacon, P.

AU - Bader, M. K.M.

AU - Baker, P. T.

AU - Baldaccini, F.

AU - Ballardin, G.

AU - Ballmer, S. W.

AU - Barayoga, J. C.

AU - Barclay, S. E.

AU - Barish, B. C.

AU - Barker, D.

AU - Barone, F.

AU - Barr, B.

AU - Barsotti, L.

AU - Barsuglia, M.

AU - Barta, D.

AU - Bartlett, J.

AU - Bartos, I.

AU - Bassiri, R.

AU - Basti, A.

AU - Batch, J. C.

AU - Baune, C.

AU - Bavigadda, V.

AU - Bazzan, M.

AU - Behnke, B.

AU - Bejger, M.

AU - Bell, A. S.

AU - Bell, C. J.

AU - Berger, B. K.

AU - Bergman, J.

AU - Bergmann, G.

AU - Berry, C. P.L.

AU - Bersanetti, D.

AU - Bertolini, A.

AU - Betzwieser, J.

AU - Bhagwat, S.

AU - Bhandare, R.

AU - Bilenko, I. A.

AU - Billingsley, G.

AU - Birch, J.

AU - Birney, R.

AU - Biscans, S.

AU - Bisht, A.

AU - Bitossi, M.

AU - Biwer, C.

AU - Bizouard, M. A.

AU - Blackburn, J. K.

AU - Blair, C. D.

AU - Blair, D. G.

AU - Blair, R. M.

AU - Bloemen, S.

AU - Bock, O.

AU - Bodiya, T. P.

AU - Boer, M.

AU - Bogaert, G.

AU - Bogan, C.

AU - Bohe, A.

AU - Bojtos, P.

AU - Bond, C.

AU - Bondu, F.

AU - Bonnand, R.

AU - Boom, B. A.

AU - Bork, R.

AU - Boschi, V.

AU - Bose, S.

AU - Bouffanais, Y.

AU - Bozzi, A.

AU - Bradaschia, C.

AU - Brady, P. R.

AU - Braginsky, V. B.

AU - Branchesi, M.

AU - Brau, J. E.

AU - Briant, T.

AU - Brillet, A.

AU - Brinkmann, M.

AU - Brisson, V.

AU - Brockill, P.

AU - Brooks, A. F.

AU - Brown, D. D.

AU - Brown, N. M.

AU - Buchanan, C. C.

AU - Buikema, A.

AU - Bulik, T.

AU - Bulten, H. J.

AU - Buonanno, A.

AU - Buskulic, D.

AU - Buy, C.

AU - Byer, R. L.

AU - Cadonati, L.

AU - Cagnoli, G.

AU - Cahillane, C.

AU - Bustillo, J. Calderón

AU - Callister, T.

AU - Calloni, E.

AU - Camp, J. B.

AU - Cannon, K. C.

AU - Cao, J.

AU - Capano, C. D.

AU - Capocasa, E.

AU - Carbognani, F.

AU - Caride, S.

AU - Diaz, J. Casanueva

AU - Casentini, C.

AU - Caudill, S.

AU - Cavaglià, M.

AU - Cavalier, F.

AU - Cavalieri, R.

AU - Cella, G.

AU - Cepeda, C. B.

AU - Baiardi, L. Cerboni

AU - Cerretani, G.

AU - Cesarini, E.

AU - Chakraborty, R.

AU - Chalermsongsak, T.

AU - Chamberlin, S. J.

AU - Chan, M.

AU - Chao, S.

AU - Charlton, P.

AU - Chassande-Mottin, E.

AU - Chen, H. Y.

AU - Chen, Y.

AU - Cheng, C.

AU - Chincarini, A.

AU - Chiummo, A.

AU - Cho, H. S.

AU - Cho, M.

AU - Chow, J. H.

AU - Christensen, N.

AU - Chu, Q.

AU - Chua, S.

AU - Chung, S.

AU - Ciani, G.

AU - Clara, F.

AU - Clark, J. A.

AU - Cleva, F.

AU - Coccia, E.

AU - Cohadon, P. F.

AU - Colla, A.

AU - Collette, C. G.

AU - Cominsky, L.

AU - Constancio, M.

AU - Conte, A.

AU - Conti, L.

AU - Cook, D.

AU - Corbitt, T. R.

AU - Cornish, N.

AU - Corsi, A.

AU - Cortese, S.

AU - Costa, C. A.

AU - Coughlin, M. W.

AU - Coughlin, S. B.

AU - Coulon, J. P.

AU - Countryman, S. T.

AU - Couvares, P.

AU - Cowan, E. E.

AU - Coward, D. M.

AU - Cowart, M. J.

AU - Coyne, D. C.

AU - Coyne, R.

AU - Craig, K.

AU - Creighton, J. D.E.

AU - Cripe, J.

AU - Crowder, S. G.

AU - Cumming, A.

AU - Cunningham, L.

AU - Cuoco, E.

AU - Canton, T. Dal

AU - Danilishin, S. L.

AU - D'Antonio, S.

AU - Danzmann, K.

AU - Darman, N. S.

AU - Dattilo, V.

AU - Dave, I.

AU - Daveloza, H. P.

AU - Davier, M.

AU - Davies, G. S.

AU - Daw, E. J.

AU - Day, R.

AU - Debra, D.

AU - Debreczeni, G.

AU - Degallaix, J.

AU - De Laurentis, M.

AU - Deléglise, S.

AU - Del Pozzo, W.

AU - Denker, T.

AU - Dent, T.

AU - Dereli, H.

AU - Dergachev, V.

AU - Derosa, R. T.

AU - De Rosa, R.

AU - Desalvo, R.

AU - Dhurandhar, S.

AU - Díaz, M. C.

AU - Di Fiore, L.

AU - Di Giovanni, M.

AU - Di Lieto, A.

AU - Di Pace, S.

AU - Di Palma, I.

AU - Di Virgilio, A.

AU - Dojcinoski, G.

AU - Dolique, V.

AU - Donovan, F.

AU - Dooley, K. L.

AU - Doravari, S.

AU - Douglas, R.

AU - Downes, T. P.

AU - Gendre, B.

AU - Howell, E. J.

AU - Ju, L.

AU - Van Heijningen, J. V.

AU - Wen, L.

AU - Zhao, C.

AU - Zhu, X. J.

PY - 2016/3/31

Y1 - 2016/3/31

N2 - The LIGO detection of the gravitational wave transient GW150914, from the inspiral and merger of two black holes with masses 30M, suggests a population of binary black holes with relatively high mass. This observation implies that the stochastic gravitational-wave background from binary black holes, created from the incoherent superposition of all the merging binaries in the Universe, could be higher than previously expected. Using the properties of GW150914, we estimate the energy density of such a background from binary black holes. In the most sensitive part of the Advanced LIGO and Advanced Virgo band for stochastic backgrounds (near 25 Hz), we predict ΩGW(f=25 Hz)=1.1-0.9+2.7×10-9 with 90% confidence. This prediction is robustly demonstrated for a variety of formation scenarios with different parameters. The differences between models are small compared to the statistical uncertainty arising from the currently poorly constrained local coalescence rate. We conclude that this background is potentially measurable by the Advanced LIGO and Advanced Virgo detectors operating at their projected final sensitivity.

AB - The LIGO detection of the gravitational wave transient GW150914, from the inspiral and merger of two black holes with masses 30M, suggests a population of binary black holes with relatively high mass. This observation implies that the stochastic gravitational-wave background from binary black holes, created from the incoherent superposition of all the merging binaries in the Universe, could be higher than previously expected. Using the properties of GW150914, we estimate the energy density of such a background from binary black holes. In the most sensitive part of the Advanced LIGO and Advanced Virgo band for stochastic backgrounds (near 25 Hz), we predict ΩGW(f=25 Hz)=1.1-0.9+2.7×10-9 with 90% confidence. This prediction is robustly demonstrated for a variety of formation scenarios with different parameters. The differences between models are small compared to the statistical uncertainty arising from the currently poorly constrained local coalescence rate. We conclude that this background is potentially measurable by the Advanced LIGO and Advanced Virgo detectors operating at their projected final sensitivity.

UR - https://www.scopus.com/pages/publications/84962867362

U2 - 10.1103/PhysRevLett.116.131102

DO - 10.1103/PhysRevLett.116.131102

M3 - Article

C2 - 27081965

SN - 0031-9007

VL - 116

JO - Physical Review Letters

JF - Physical Review Letters

IS - 13

M1 - 131102

ER -

GW150914: Implications for the stochastic gravitational-wave background from binary black holes

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The Astrophysical Stochastic Background of Gravitational Waves and Detection by Advanced High Optical Power Interferometers: An Australia-US Collaboration

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GW150914: Implications for the stochastic gravitational-wave background from binary black holes

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The Astrophysical Stochastic Background of Gravitational Waves and Detection by Advanced High Optical Power Interferometers: An Australia-US Collaboration

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