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

B.P. Abbott; R. Abbott; T.D. Abbott; F. Acernese; K. Ackley; C. Adams; T. Adams; P. Addesso; R.X. Adhikari; V.B. Adya; C. Affeldt; M. Afrough; B. Agarwal; M. Agathos; K. Agatsuma; N. Aggarwal; O.D. Aguiar; L. Aiello; A. Ain; P. Ajith; B. Allen; G. Allen; A. Allocca; P.A. Altin; A. Amato; A. Ananyeva; S.B. Anderson; W.G. Anderson; S.V. Angelova; S. Antier; S. Appert; K. Arai; M.C. Araya; J.S. Areeda; N. Arnaud; K.G. Arun; S. Ascenzi; G. Ashton; M. Ast; S.M. Aston; P. Astone; D.V. Atallah; P. Aufmuth; C. Aulbert; K. AultONeal; C. Austin; A. Avila-Alvarez; S. Babak; P. Bacon; M.K.M. Bader; S.L. Danilishin; J. Hennig; S. Hild; J. Steinlechner; S. Steinlechner; J.F.J. van den Brand

doi:10.1103/PhysRevLett.120.091101

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

B.P. Abbott, R. Abbott, T.D. Abbott, F. Acernese, K. Ackley, C. Adams, T. Adams, P. Addesso, R.X. Adhikari, V.B. Adya, C. Affeldt, M. Afrough, B. Agarwal, M. Agathos, K. Agatsuma, N. Aggarwal, O.D. Aguiar, L. Aiello, A. Ain, P. AjithB. Allen, G. Allen, A. Allocca, P.A. Altin, A. Amato, A. Ananyeva, S.B. Anderson, W.G. Anderson, S.V. Angelova, S. Antier, S. Appert, K. Arai, M.C. Araya, J.S. Areeda, N. Arnaud, K.G. Arun, S. Ascenzi, G. Ashton, M. Ast, S.M. Aston, P. Astone, D.V. Atallah, P. Aufmuth, C. Aulbert, K. AultONeal, C. Austin, A. Avila-Alvarez, S. Babak, P. Bacon, M.K.M. Bader, S.L. Danilishin, J. Hennig, S. Hild, J. Steinlechner, S. Steinlechner, J.F.J. van den Brand

Research output: Contribution to journal › Article › Academic › peer-review

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.

Original language	English
Article number	091101
Number of pages	12
Journal	Physical Review Letters
Volume	120
Issue number	9
DOIs	https://doi.org/10.1103/PhysRevLett.120.091101
Publication status	Published - 28 Feb 2018
Externally published	Yes

Keywords

STAR-FORMATION
HIGH-REDSHIFT
RATES
MERGERS
EVOLUTION

Access to Document

10.1103/PhysRevLett.120.091101Licence: Free access - publisher

Cite this

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., ... van den Brand, J. F. J. (2018). GW170817: Implications for the Stochastic Gravitational-Wave Background from Compact Binary Coalescences. Physical Review Letters, 120(9), Article 091101. https://doi.org/10.1103/PhysRevLett.120.091101

@article{1c1e9b757e5c43da8bf9cba930652dc8,

title = "GW170817: Implications for the Stochastic Gravitational-Wave Background from Compact Binary Coalescences",

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.",

keywords = "STAR-FORMATION, HIGH-REDSHIFT, RATES, MERGERS, EVOLUTION",

author = "B.P. Abbott and R. Abbott and T.D. Abbott and F. Acernese and K. Ackley and C. Adams and T. Adams and P. Addesso and R.X. Adhikari and V.B. Adya and C. Affeldt and M. Afrough and B. Agarwal and M. Agathos and K. Agatsuma and N. Aggarwal and O.D. Aguiar and L. Aiello and A. Ain and P. Ajith and B. Allen and G. Allen and A. Allocca and P.A. Altin and A. Amato and A. Ananyeva and S.B. Anderson and W.G. Anderson and S.V. Angelova and S. Antier and S. Appert and K. Arai and M.C. Araya and J.S. Areeda and N. Arnaud and K.G. Arun and S. Ascenzi and G. Ashton and M. Ast and S.M. Aston and P. Astone and D.V. Atallah and P. Aufmuth and C. Aulbert and K. AultONeal and C. Austin and A. Avila-Alvarez and S. Babak and P. Bacon and M.K.M. Bader and S.L. Danilishin and J. Hennig and S. Hild and J. Steinlechner and S. Steinlechner and {van den Brand}, J.F.J.",

year = "2018",

month = feb,

day = "28",

doi = "10.1103/PhysRevLett.120.091101",

language = "English",

volume = "120",

journal = "Physical Review Letters",

issn = "0031-9007",

publisher = "American Physical Society",

number = "9",

}

Abbott, BP, Abbott, R, Abbott, TD, Acernese, F, Ackley, K, Adams, C, Adams, T, Addesso, P, Adhikari, RX, Adya, VB, Affeldt, C, Afrough, M, Agarwal, B, Agathos, M, Agatsuma, K, Aggarwal, N, Aguiar, OD, Aiello, L, Ain, A, Ajith, P, Allen, B, Allen, G, Allocca, A, Altin, PA, Amato, A, Ananyeva, A, Anderson, SB, Anderson, WG, Angelova, SV, Antier, S, Appert, S, Arai, K, Araya, MC, Areeda, JS, Arnaud, N, Arun, KG, Ascenzi, S, Ashton, G, Ast, M, Aston, SM, Astone, P, Atallah, DV, Aufmuth, P, Aulbert, C, AultONeal, K, Austin, C, Avila-Alvarez, A, Babak, S, Bacon, P, Bader, MKM, Danilishin, SL , Hennig, J , Hild, S , Steinlechner, J , Steinlechner, S & van den Brand, JFJ 2018, 'GW170817: Implications for the Stochastic Gravitational-Wave Background from Compact Binary Coalescences', Physical Review Letters, vol. 120, no. 9, 091101. https://doi.org/10.1103/PhysRevLett.120.091101

TY - JOUR

T1 - GW170817: Implications for the Stochastic Gravitational-Wave Background from Compact Binary Coalescences

AU - Abbott, B.P.

AU - Abbott, R.

AU - Abbott, T.D.

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 - Afrough, M.

AU - Agarwal, B.

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 - Allen, G.

AU - Allocca, A.

AU - Altin, P.A.

AU - Amato, A.

AU - Ananyeva, A.

AU - Anderson, S.B.

AU - Anderson, W.G.

AU - Angelova, S.V.

AU - Antier, S.

AU - Appert, S.

AU - Arai, K.

AU - Araya, M.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 - Atallah, D.V.

AU - Aufmuth, P.

AU - Aulbert, C.

AU - AultONeal, K.

AU - Austin, C.

AU - Avila-Alvarez, A.

AU - Babak, S.

AU - Bacon, P.

AU - Bader, M.K.M.

AU - Danilishin, S.L.

AU - Hennig, J.

AU - Hild, S.

AU - Steinlechner, J.

AU - Steinlechner, S.

AU - van den Brand, J.F.J.

PY - 2018/2/28

Y1 - 2018/2/28

N2 - 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.

AB - 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.

KW - STAR-FORMATION

KW - HIGH-REDSHIFT

KW - RATES

KW - MERGERS

KW - EVOLUTION

U2 - 10.1103/PhysRevLett.120.091101

DO - 10.1103/PhysRevLett.120.091101

M3 - Article

SN - 0031-9007

VL - 120

JO - Physical Review Letters

JF - Physical Review Letters

IS - 9

M1 - 091101

ER -