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GW170817: Implications for the Stochastic Gravitational-Wave Background from Compact Binary Coalescences

Title
GW170817: Implications for the Stochastic Gravitational-Wave Background from Compact Binary Coalescences
Authors
Abbott, B. P.Abbott, R.Abbott, T. D.Acernese, F.Ackley, K.Adams, C.Adams, T.Addesso, P.Adhikari, R. X.Adya, V. B.Affeldt, C.Afrough, M.Agarwal, B.Agathos, M.Agatsuma, K.Aggarwal, N.Aguiar, O. D.Aiello, L.Ain, A.Ajith, P.Allen, B.Allen, G.Allocca, A.Altin, P. A.Amato, A.Ananyeva, A.Anderson, S. B.Anderson, W. G.Angelova, S. V.Antier, S.Appert, S.Arai, K.Araya, M. C.Areeda, J. S.Arnaud, N.Arun, K. G.Ascenzi, S.Ashton, G.Ast, M.Aston, S. M.Astone, P.Atallah, D. V.Aufmuth, P.Aulbert, C.AultONeal, K.Austin, C.Avila-Alvarez, A.Babak, S.Bacon, P.Bader, M. K. M.Bae, S.Baker, P. T.Baldaccini, F.Ballardin, G.Ballmer, S. W.Banagiri, S.Barayoga, J. C.Barclay, S. E.Barish, B. C.Barker, D.Barkett, K.Barone, F.Barr, B.Barsotti, L.Barsuglia, M.Barta, D.Bartlett, J.Bartos, I.Bassiri, R.Basti, A.Batch, J. C.Bawaj, M.Bayley, J. C.Bazzan, M.Becsy, B.Beer, C.Bejger, M.Belahcene, I.Bell, A. S.Berger, B. K.Bergmann, G.Bero, J. J.Berry, C. P. L.Bersanetti, D.Bertolini, A.Betzwieser, J.Bhagwat, S.Bhandare, R.Bilenko, I. A.Billingsley, G.Billman, C. R.Birch, J.Birney, R.Birnholtz, O.Biscans, S.Biscoveanu, S.Bisht, A.Bitossi, M.Biwer, C.Bizouard, M. A.Blackburn, J. K.Blackman, J.Blair, C. D.Blair, D. G.Blair, R. M.Bloemen, S.Bock, O.Bode, N.Boer, M.Bogaert, G.Bohe, A.Bondu, F.Bonilla, E.Bonnand, R.Boom, B. A.Bork, R.Boschi, V.Bose, S.Bossie, K.Bouffanais, Y.Bozzi, A.Bradaschia, C.Brady, P. R.Branchesi, M.Brau, J. E.Briant, T.Brillet, A.Brinkmann, M.Brisson, V.Brockill, P.Broida, J. E.Brooks, A. F.Brown, D. A.Brown, D. D.Brunett, S.Buchanan, C. C.Buikema, A.Bulik, T.Bulten, H. J.Buonanno, A.Buskulic, D.Buy, C.Byer, R. L.Cabero, M.Cadonati, L.Cagnoli, G.Cahillane, C.Bustillo, J. CalderonCallister, T. A.Calloni, E.Camp, J. B.Canepa, M.Canizares, P.Cannon, K. C.Cao, H.Cao, J.Capano, C. D.Capocasa, E.Carbognani, F.Caride, S.Carney, M. F.Diaz, J. CasanuevaCasentini, C.Caudill, S.Cavaglia, M.Cavalier, F.Cavalieri, R.Cella, G.Cepeda, C. B.Cerda-Duran, P.Cerretani, G.Cesarini, E.Chamberlin, S. J.Chan, M.Chao, S.Charlton, P.Chase, E.Chassande-Mottin, E.Chatterjee, D.Cheeseboro, B. D.Chen, H. Y.Chen, X.Chen, Y.Cheng, H. -P.Chia, H.Chincarini, A.Chiummo, A.Chmiel, T.Cho, H. S.Cho, M.Chow, J. H.Christensen, N.Chu, Q.Chua, A. J. K.Chua, S.Chung, A. K. W.Chung, S.Ciani, G.Ciolfi, R.Cirelli, C. E.Cirone, A.Clara, F.Clark, J. A.Clearwater, P.Cleva, F.Cocchieri, C.Coccia, E.Cohadon, P. -F.Cohen, D.Colla, A.Collette, C. G.Cominsky, L. R.Constancio, M., Jr.Conti, L.Cooper, S. J.Corban, P.Corbitt, T. R.Cordero-Carrion, I.Corley, K. R.Cornish, N.Corsi, A.Cortese, S.Costa, C. A.Coughlin, M. W.Coughlin, S. B.Coulon, J. -P.Countryman, S. T.Couvares, P.Covas, P. B.Cowan, E. E.Coward, D. M.Cowart, M. J.Coyne, D. C.Coyne, R.Creighton, J. D. E.Creighton, T. D.Cripe, J.Crowder, S. G.Cullen, T. 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J.Favata, M.Fays, M.Fee, C.Fehrmann, H.Feicht, J.Fejer, M. M.Fernandez-Galiana, A.Ferrante, I.Ferreira, E. C.Ferrini, F.Fidecaro, F.Finstad, D.Fiori, I.Fiorucci, D.Fishbach, M.Fisher, R. P.Fitz-Axen, M.Flaminio, R.Fletcher, M.Fong, H.Font, J. A.Forsyth, P. W. F.Forsyth, S. S.Fournier, J. -D.Frasca, S.Frasconi, F.Frei, Z.Freise, A.Frey, R.Frey, V.Fries, E. M.Fritschel, P.Frolov, V. V.Fulda, P.Fyffe, M.Gabbard, H.Gadre, B. U.Gaebel, S. M.Gair, J. R.Gammaitoni, L.Ganija, M. R.Gaonkar, S. G.Garcia-Quiros, C.Garufi, F.Gateley, B.Gaudio, S.Gaur, G.Gayathri, V.Gehrels, N.Gemme, G.Genin, E.Gennai, A.George, D.George, J.Gergely, L.Germain, V.Ghonge, S.Ghosh, AbhirupGhosh, ArchismanGhosh, S.Giaime, J. A.Giardina, K. D.Giazotto, A.Gill, K.Glover, L.Goetz, E.Goetz, R.Gomes, S.Goncharov, B.Gonzalez, G.Castro, J. M. GonzalezGopakumar, A.Gorodetsky, M. L.Gossan, S. E.Gosselin, M.Gouaty, R.Grado, A.Graef, C.Granata, M.Grant, A.Gras, S.Gray, C.Greco, G.Green, A. C.Gretarsson, E. 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E.Ramos-Buades, A.Rapagnani, P.Raymond, V.Razzano, M.Read, J.Regimbau, T.Rei, L.Reid, S.Reitze, D. H.Ren, W.Reyes, S. D.Ricci, F.Ricker, P. M.Rieger, S.Riles, K.Rizzo, M.Robertson, N. A.Robie, R.Robinet, F.Rocchi, A.Rolland, L.Rollins, J. G.Roma, V. J.Romano, J. D.Romano, R.Romel, C. L.Romie, J. H.Rosinska, D.Ross, M. P.Rowan, S.Ruediger, A.Ruggi, P.Rutins, G.Ryan, K.Sachdev, S.Sadecki, T.Sadeghian, L.Sakellariadou, M.Salconi, L.Saleem, M.Salemi, F.Samajdar, A.Sammut, L.Sampson, L. M.Sanchez, E. J.Sanchez, L. E.Sanchis-Gual, N.Sandberg, V.Sanders, J. R.Sassolas, B.Sathyaprakash, B. S.Saulson, P. R.Sauter, O.Savage, R. L.Sawadsky, A.Schale, P.Scheel, M.Scheuer, J.Schmidt, J.Schmidt, P.Schnabel, R.Schofield, R. M. S.Schoenbeck, A.Schreiber, E.Schuette, D.Schulte, B. W.Schutz, B. F.Schwalbe, S. G.Scott, J.Scott, S. M.Seidel, E.Sellers, D.Sengupta, A. S.Sentenac, D.Sequino, V.Sergeev, A.Shaddock, D. A.Shaffer, T. J.Shah, A. A.Shahriar, M. S.Shaner, M. 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Ewha Authors
김정리
SCOPUS Author ID
김정리scopus
Issue Date
2018
Journal Title
PHYSICAL REVIEW LETTERS
ISSN
0031-9007JCR Link

1079-7114JCR Link
Citation
PHYSICAL REVIEW LETTERS vol. 120, no. 9
Publisher
AMER PHYSICAL SOC
Indexed
SCIE; SCOPUS WOS
Document Type
Article
Abstract
The LIGO Scientific and Virgo Collaborations have announced the event GW170817, the first detection of gravitational waves from the coalescence of two neutron stars. The merger rate of binary neutron stars estimated from this event suggests that distant, unresolvable binary neutron stars create a significant astrophysical stochastic gravitational-wave background. The binary neutron star component will add to the contribution from binary black holes, increasing the amplitude of the total astrophysical background relative to previous expectations. In the Advanced LIGO-Virgo frequency band most sensitive to stochastic backgrounds (near 25 Hz), we predict a total astrophysical background with amplitude Omega(GW) (f = 25 Hz) = 1.8(-1.3)(+2.7) x 10(-9) with 90% confidence, compared with Omega(GW) (f = 25 Hz) = 1.1(-0.7)(+1.2) x 10(-9) from binary black holes alone. Assuming the most probable rate for compact binary mergers, we find that the total background may be detectable with a signal-to-noise-ratio of 3 after 40 months of total observation time, based on the expected timeline for Advanced LIGO and Virgo to reach their design sensitivity.
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DOI
10.1103/PhysRevLett.120.091101
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자연과학대학 > 물리학전공 > Journal papers
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