Sensitivity of the Advanced LIGO detectors at the beginning of gravitational wave astronomy

D.V. Martynov; E.D. Hall; B.P. Abbott; R. Abbott; T.D. Abbott; C. Adams; R.X. Adhikari; R.A. Anderson; S.B. Anderson; K. Arai; M.A. Arain; S.M. Aston; L. Austin; S.W. Ballmer; M. Barbet; D. Barker; B. Barr; L. Barsotti; J. Bartlett; M.A. Barton; I. Bartos; J.C. Batch; A.S. Bell; I. Belopolski; J. Bergman; J. Betzwieser; G. Billingsley; J. Birch; S. Biscans; C. Biwer; E. Black; Carl Blair; C. Bogan; R. Bork; D.O. Bridges; A.F. Brooks; C. Celerier; G. Ciani; F. Clara; D. Cook; S.T. Countryman; M.J. Cowart; D.C. Coyne; A. Cumming; L. Cunningham; M. Damjanic; R. Dannenberg; K. Danzmann; C.F.D.S. Costa; E.J. Daw; D. Debra; R.T. Derosa; R. Desalvo; K.L. Dooley; S. Doravari; J.C. Driggers; S.E. Dwyer; A. Effler; T. Etzel; M. Evans; T.M. Evans; M. Factourovich; H. Fair; D. Feldbaum; R.P. Fisher; S. Foley; M. Frede; P. Fritschel; V.V. Frolov; P. Fulda; M. Fyffe; V. Galdi; J.A. Giaime; K.D. Giardina; J.R. Gleason; R. Goetz; S. Gras; C. Gray; R.J.S. Greenhalgh; H. Grote; C.J. Guido; K.E. Gushwa; E.K. Gustafson; R. Gustafson; G. Hammond; J. Hanks; J. Hanson; T. Hardwick; G.M. Harry; J. Heefner; M.C. Heintze; A.W. Heptonstall; D. Hoak; J. Hough; A. Ivanov

doi:10.1103/PhysRevD.93.112004

Sensitivity of the Advanced LIGO detectors at the beginning of gravitational wave astronomy

D.V. Martynov, E.D. Hall, B.P. Abbott, R. Abbott, T.D. Abbott, C. Adams, R.X. Adhikari, R.A. Anderson, S.B. Anderson, K. Arai, M.A. Arain, S.M. Aston, L. Austin, S.W. Ballmer, M. Barbet, D. Barker, B. Barr, L. Barsotti, J. Bartlett, M.A. BartonI. Bartos, J.C. Batch, A.S. Bell, I. Belopolski, J. Bergman, J. Betzwieser, G. Billingsley, J. Birch, S. Biscans, C. Biwer, E. Black, Carl Blair, C. Bogan, R. Bork, D.O. Bridges, A.F. Brooks, C. Celerier, G. Ciani, F. Clara, D. Cook, S.T. Countryman, M.J. Cowart, D.C. Coyne, A. Cumming, L. Cunningham, M. Damjanic, R. Dannenberg, K. Danzmann, C.F.D.S. Costa, E.J. Daw, D. Debra, R.T. Derosa, R. Desalvo, K.L. Dooley, S. Doravari, J.C. Driggers, S.E. Dwyer, A. Effler, T. Etzel, M. Evans, T.M. Evans, M. Factourovich, H. Fair, D. Feldbaum, R.P. Fisher, S. Foley, M. Frede, P. Fritschel, V.V. Frolov, P. Fulda, M. Fyffe, V. Galdi, J.A. Giaime, K.D. Giardina, J.R. Gleason, R. Goetz, S. Gras, C. Gray, R.J.S. Greenhalgh, H. Grote, C.J. Guido, K.E. Gushwa, E.K. Gustafson, R. Gustafson, G. Hammond, J. Hanks, J. Hanson, T. Hardwick, G.M. Harry, J. Heefner, M.C. Heintze, A.W. Heptonstall, D. Hoak, J. Hough, A. Ivanov

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Abstract

© 2016 American Physical Society. The Laser Interferometer Gravitational Wave Observatory (LIGO) consists of two widely separated 4 km laser interferometers designed to detect gravitational waves from distant astrophysical sources in the frequency range from 10 Hz to 10 kHz. The first observation run of the Advanced LIGO detectors started in September 2015 and ended in January 2016. A strain sensitivity of better than 10-23/Hz was achieved around 100 Hz. Understanding both the fundamental and the technical noise sources was critical for increasing the astrophysical strain sensitivity. The average distance at which coalescing binary black hole systems with individual masses of 30 M could be detected above a signal-to-noise ratio (SNR) of 8 was 1.3 Gpc, and the range for binary neutron star inspirals was about 75 Mpc. With respect to the initial detectors, the observable volume of the Universe increased by a factor 69 and 43, respectively. These improvements helped Advanced LIGO to detect the gravitational wave signal from the binary black hole coalescence, known as GW150914.

Original language	English
Article number	112004
Journal	Physical Review D - Particles, Fields, Gravitation and Cosmology
Volume	93
Issue number	11
DOIs	https://doi.org/10.1103/PhysRevD.93.112004
Publication status	Published - 2 Jun 2016

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Martynov, D. V., Hall, E. D., Abbott, B. P., Abbott, R., Abbott, T. D., Adams, C., Adhikari, R. X., Anderson, R. A., Anderson, S. B., Arai, K., Arain, M. A., Aston, S. M., Austin, L., Ballmer, S. W., Barbet, M., Barker, D., Barr, B., Barsotti, L., Bartlett, J., ... Ivanov, A. (2016). Sensitivity of the Advanced LIGO detectors at the beginning of gravitational wave astronomy. Physical Review D - Particles, Fields, Gravitation and Cosmology, 93(11), Article 112004. https://doi.org/10.1103/PhysRevD.93.112004

@article{856495b5c1da429191cec28b673a51a2,

title = "Sensitivity of the Advanced LIGO detectors at the beginning of gravitational wave astronomy",

abstract = "{\textcopyright} 2016 American Physical Society. The Laser Interferometer Gravitational Wave Observatory (LIGO) consists of two widely separated 4 km laser interferometers designed to detect gravitational waves from distant astrophysical sources in the frequency range from 10 Hz to 10 kHz. The first observation run of the Advanced LIGO detectors started in September 2015 and ended in January 2016. A strain sensitivity of better than 10-23/Hz was achieved around 100 Hz. Understanding both the fundamental and the technical noise sources was critical for increasing the astrophysical strain sensitivity. The average distance at which coalescing binary black hole systems with individual masses of 30 M could be detected above a signal-to-noise ratio (SNR) of 8 was 1.3 Gpc, and the range for binary neutron star inspirals was about 75 Mpc. With respect to the initial detectors, the observable volume of the Universe increased by a factor 69 and 43, respectively. These improvements helped Advanced LIGO to detect the gravitational wave signal from the binary black hole coalescence, known as GW150914.",

author = "D.V. Martynov and E.D. Hall and B.P. Abbott and R. Abbott and T.D. Abbott and C. Adams and R.X. Adhikari and R.A. Anderson and S.B. Anderson and K. Arai and M.A. Arain and S.M. Aston and L. Austin and S.W. Ballmer and M. Barbet and D. Barker and B. Barr and L. Barsotti and J. Bartlett and M.A. Barton and I. Bartos and J.C. Batch and A.S. Bell and I. Belopolski and J. Bergman and J. Betzwieser and G. Billingsley and J. Birch and S. Biscans and C. Biwer and E. Black and Carl Blair and C. Bogan and R. Bork and D.O. Bridges and A.F. Brooks and C. Celerier and G. Ciani and F. Clara and D. Cook and S.T. Countryman and M.J. Cowart and D.C. Coyne and A. Cumming and L. Cunningham and M. Damjanic and R. Dannenberg and K. Danzmann and C.F.D.S. Costa and E.J. Daw and D. Debra and R.T. Derosa and R. Desalvo and K.L. Dooley and S. Doravari and J.C. Driggers and S.E. Dwyer and A. Effler and T. Etzel and M. Evans and T.M. Evans and M. Factourovich and H. Fair and D. Feldbaum and R.P. Fisher and S. Foley and M. Frede and P. Fritschel and V.V. Frolov and P. Fulda and M. Fyffe and V. Galdi and J.A. Giaime and K.D. Giardina and J.R. Gleason and R. Goetz and S. Gras and C. Gray and R.J.S. Greenhalgh and H. Grote and C.J. Guido and K.E. Gushwa and E.K. Gustafson and R. Gustafson and G. Hammond and J. Hanks and J. Hanson and T. Hardwick and G.M. Harry and J. Heefner and M.C. Heintze and A.W. Heptonstall and D. Hoak and J. Hough and A. Ivanov",

year = "2016",

month = jun,

day = "2",

doi = "10.1103/PhysRevD.93.112004",

language = "English",

volume = "93",

journal = "Physical Review D - Particles, Fields, Gravitation and Cosmology",

issn = "1550-7998",

publisher = "American Physical Society",

number = "11",

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Martynov, DV, Hall, ED, Abbott, BP, Abbott, R, Abbott, TD, Adams, C, Adhikari, RX, Anderson, RA, Anderson, SB, Arai, K, Arain, MA, Aston, SM, Austin, L, Ballmer, SW, Barbet, M, Barker, D, Barr, B, Barsotti, L, Bartlett, J, Barton, MA, Bartos, I, Batch, JC, Bell, AS, Belopolski, I, Bergman, J, Betzwieser, J, Billingsley, G, Birch, J, Biscans, S, Biwer, C, Black, E, Blair, C, Bogan, C, Bork, R, Bridges, DO, Brooks, AF, Celerier, C, Ciani, G, Clara, F, Cook, D, Countryman, ST, Cowart, MJ, Coyne, DC, Cumming, A, Cunningham, L, Damjanic, M, Dannenberg, R, Danzmann, K, Costa, CFDS, Daw, EJ, Debra, D, Derosa, RT, Desalvo, R, Dooley, KL, Doravari, S, Driggers, JC, Dwyer, SE, Effler, A, Etzel, T, Evans, M, Evans, TM, Factourovich, M, Fair, H, Feldbaum, D, Fisher, RP, Foley, S, Frede, M, Fritschel, P, Frolov, VV, Fulda, P, Fyffe, M, Galdi, V, Giaime, JA, Giardina, KD, Gleason, JR, Goetz, R, Gras, S, Gray, C, Greenhalgh, RJS, Grote, H, Guido, CJ, Gushwa, KE, Gustafson, EK, Gustafson, R, Hammond, G, Hanks, J, Hanson, J, Hardwick, T, Harry, GM, Heefner, J, Heintze, MC, Heptonstall, AW, Hoak, D, Hough, J & Ivanov, A 2016, 'Sensitivity of the Advanced LIGO detectors at the beginning of gravitational wave astronomy', Physical Review D - Particles, Fields, Gravitation and Cosmology, vol. 93, no. 11, 112004. https://doi.org/10.1103/PhysRevD.93.112004

TY - JOUR

T1 - Sensitivity of the Advanced LIGO detectors at the beginning of gravitational wave astronomy

AU - Martynov, D.V.

AU - Hall, E.D.

AU - Abbott, B.P.

AU - Abbott, R.

AU - Abbott, T.D.

AU - Adams, C.

AU - Adhikari, R.X.

AU - Anderson, R.A.

AU - Anderson, S.B.

AU - Arai, K.

AU - Arain, M.A.

AU - Aston, S.M.

AU - Austin, L.

AU - Ballmer, S.W.

AU - Barbet, M.

AU - Barker, D.

AU - Barr, B.

AU - Barsotti, L.

AU - Bartlett, J.

AU - Barton, M.A.

AU - Bartos, I.

AU - Batch, J.C.

AU - Bell, A.S.

AU - Belopolski, I.

AU - Bergman, J.

AU - Betzwieser, J.

AU - Billingsley, G.

AU - Birch, J.

AU - Biscans, S.

AU - Biwer, C.

AU - Black, E.

AU - Blair, Carl

AU - Bogan, C.

AU - Bork, R.

AU - Bridges, D.O.

AU - Brooks, A.F.

AU - Celerier, C.

AU - Ciani, G.

AU - Clara, F.

AU - Cook, D.

AU - Countryman, S.T.

AU - Cowart, M.J.

AU - Coyne, D.C.

AU - Cumming, A.

AU - Cunningham, L.

AU - Damjanic, M.

AU - Dannenberg, R.

AU - Danzmann, K.

AU - Costa, C.F.D.S.

AU - Daw, E.J.

AU - Debra, D.

AU - Derosa, R.T.

AU - Desalvo, R.

AU - Dooley, K.L.

AU - Doravari, S.

AU - Driggers, J.C.

AU - Dwyer, S.E.

AU - Effler, A.

AU - Etzel, T.

AU - Evans, M.

AU - Evans, T.M.

AU - Factourovich, M.

AU - Fair, H.

AU - Feldbaum, D.

AU - Fisher, R.P.

AU - Foley, S.

AU - Frede, M.

AU - Fritschel, P.

AU - Frolov, V.V.

AU - Fulda, P.

AU - Fyffe, M.

AU - Galdi, V.

AU - Giaime, J.A.

AU - Giardina, K.D.

AU - Gleason, J.R.

AU - Goetz, R.

AU - Gras, S.

AU - Gray, C.

AU - Greenhalgh, R.J.S.

AU - Grote, H.

AU - Guido, C.J.

AU - Gushwa, K.E.

AU - Gustafson, E.K.

AU - Gustafson, R.

AU - Hammond, G.

AU - Hanks, J.

AU - Hanson, J.

AU - Hardwick, T.

AU - Harry, G.M.

AU - Heefner, J.

AU - Heintze, M.C.

AU - Heptonstall, A.W.

AU - Hoak, D.

AU - Hough, J.

AU - Ivanov, A.

PY - 2016/6/2

Y1 - 2016/6/2

N2 - © 2016 American Physical Society. The Laser Interferometer Gravitational Wave Observatory (LIGO) consists of two widely separated 4 km laser interferometers designed to detect gravitational waves from distant astrophysical sources in the frequency range from 10 Hz to 10 kHz. The first observation run of the Advanced LIGO detectors started in September 2015 and ended in January 2016. A strain sensitivity of better than 10-23/Hz was achieved around 100 Hz. Understanding both the fundamental and the technical noise sources was critical for increasing the astrophysical strain sensitivity. The average distance at which coalescing binary black hole systems with individual masses of 30 M could be detected above a signal-to-noise ratio (SNR) of 8 was 1.3 Gpc, and the range for binary neutron star inspirals was about 75 Mpc. With respect to the initial detectors, the observable volume of the Universe increased by a factor 69 and 43, respectively. These improvements helped Advanced LIGO to detect the gravitational wave signal from the binary black hole coalescence, known as GW150914.

AB - © 2016 American Physical Society. The Laser Interferometer Gravitational Wave Observatory (LIGO) consists of two widely separated 4 km laser interferometers designed to detect gravitational waves from distant astrophysical sources in the frequency range from 10 Hz to 10 kHz. The first observation run of the Advanced LIGO detectors started in September 2015 and ended in January 2016. A strain sensitivity of better than 10-23/Hz was achieved around 100 Hz. Understanding both the fundamental and the technical noise sources was critical for increasing the astrophysical strain sensitivity. The average distance at which coalescing binary black hole systems with individual masses of 30 M could be detected above a signal-to-noise ratio (SNR) of 8 was 1.3 Gpc, and the range for binary neutron star inspirals was about 75 Mpc. With respect to the initial detectors, the observable volume of the Universe increased by a factor 69 and 43, respectively. These improvements helped Advanced LIGO to detect the gravitational wave signal from the binary black hole coalescence, known as GW150914.

UR - https://www.scopus.com/pages/publications/84974849312

U2 - 10.1103/PhysRevD.93.112004

DO - 10.1103/PhysRevD.93.112004

M3 - Article

SN - 1550-7998

VL - 93

JO - Physical Review D - Particles, Fields, Gravitation and Cosmology

JF - Physical Review D - Particles, Fields, Gravitation and Cosmology

IS - 11

M1 - 112004

ER -

Sensitivity of the Advanced LIGO detectors at the beginning of gravitational wave astronomy

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