Search for the isotropic stochastic background using data from Advanced LIGO's second observing run

(LIGO Scientific and Virgo Collaboration)

doi:10.1103/PhysRevD.100.061101

Search for the isotropic stochastic background using data from Advanced LIGO's second observing run

(LIGO Scientific and Virgo Collaboration)

(Astro)-Particles Physics

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

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Abstract

The stochastic gravitational-wave background is a superposition of sources that are either too weak or too numerous to detect individually. In this study, we present the results from a cross-correlation analysis on data from Advanced LIGO's second observing run (O2), which we combine with the results of the first observing run (O1). We do not find evidence for a stochastic background, so we place upper limits on the normalized energy density in gravitational waves at the 95% credible level of ωGW<6.0×10-8 for a frequency-independent (flat) background and ωGW<4.8×10-8 at 25 Hz for a background of compact binary coalescences. The upper limit improves over the O1 result by a factor of 2.8. Additionally, we place upper limits on the energy density in an isotropic background of scalar- and vector-polarized gravitational waves, and we discuss the implication of these results for models of compact binaries and cosmic string backgrounds. Finally, we present a conservative estimate of the correlated broadband noise due to the magnetic Schumann resonances in O2, based on magnetometer measurements at both the LIGO Hanford and LIGO Livingston observatories. We find that correlated noise is well below the O2 sensitivity.

Original language	English
Article number	061101
Pages (from-to)	1-16
Number of pages	16
Journal	Physical Review D
Volume	100
Issue number	6
Early online date	4 Sept 2019
DOIs	https://doi.org/10.1103/PhysRevD.100.061101
Publication status	Published - 15 Sept 2019

Funding

The authors gratefully acknowledge the support of the United States National Science Foundation (NSF) for the construction and operation of the LIGO Laboratory and Advanced LIGO as well as the Science and Technology Facilities Council (STFC) of the United Kingdom, the Max-Planck-Society (MPS), and the State of Niedersachsen/Germany for support of the construction of Advanced LIGO and construction and operation of the GEO600 detector. Additional support for Advanced LIGO was provided by the Australian Research Council. The authors gratefully acknowledge the Italian Istituto Nazionale di Fisica Nucleare (INFN), the French Centre National de la Recherche Scientifique (CNRS), and the Foundation for Fundamental Research on Matter supported by the Netherlands Organisation for Scientific Research for the construction and operation of the Virgo detector and the creation and support of the European Gravitational Observatory (EGO) consortium. The authors also gratefully acknowledge research support from these agencies as well as by the Council of Scientific and Industrial Research of India, the Department of Science and Technology, India; the Science & Engineering Research Board, India; the Ministry of Human Resource Development, India; the Spanish Agencia Estatal de Investigación; the Vicepresidència i Conselleria d’Innovació; Recerca i Turisme and the Conselleria d’Educació i Universitat del Govern de les Illes Balears; the Conselleria d’Educació, Investigació, Cultura i Esport de la Generalitat Valenciana; the National Science Centre of Poland; the Swiss National Science Foundation; the Russian Foundation for Basic Research; the Russian Science Foundation; the European Commission; the European Regional Development Funds; the Royal Society; the Scottish Funding Council; the Scottish Universities Physics Alliance; the Hungarian Scientific Research Fund; the Lyon Institute of Origins; the Paris Île-de-France Region; the National Research, Development and Innovation Office, Hungary; the National Research Foundation of Korea; Industry Canada and the Province of Ontario through the Ministry of Economic Development and Innovation; the Natural Science and Engineering Research Council Canada; the Canadian Institute for Advanced Research; the Brazilian Ministry of Science, Technology, Innovations, and Communications; the International Center for Theoretical Physics South American Institute for Fundamental Research; the Research Grants Council of Hong Kong; the National Natural Science Foundation of China; the Leverhulme Trust, the Research Corporation; the Ministry of Science and Technology, Taiwan; and the Kavli Foundation. 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Funders	Funder number
Council of Scientific and Industrial Research, India
Ministry of Human Resource Development
Australian Research Council
ICTP South American Institute for Fundamental Research
Ministério da Ciência, Tecnologia, Inovações e Comunicações
National Research Foundation of Korea
Narodowe Centrum Nauki
Scottish Universities Physics Alliance
Scottish Funding Council
Ministry of Science and Technology, Taiwan
Leverhulme Trust
Science and Engineering Research Board
Paris Île-de-France Region
Instituto Nazionale di Fisica Nucleare
Ontario Ministry of Economic Development and Innovation
Department of Science and Technology, Ministry of Science and Technology, India
Centre National de la Recherche Scientifique
Kavli Foundation
European Commission
Russian Foundation for Basic Research
Directorate for Mathematical and Physical Sciences
Agencia Estatal de Investigación
Netherlands Organisation for Scientific Research for the construction and operation of the Virgo detector
Natural Sciences and Engineering Research Council of Canada
Research Grants Council, University Grants Committee
Russian Science Foundation
Industry Canada
Hungarian Scientific Research Fund
Schweizerischer Nationalfonds zur Förderung der Wissenschaftlichen Forschung
Institut des Origines de Lyon
Royal Society
Canadian Institute for Advanced Research
Universitat de les Illes Balears
European Regional Development Fund
Generalitat Valenciana
National Research, Development and Innovation Office
Istituto Nazionale di Fisica Nucleare
National Natural Science Foundation of China
Not added	ST/N005422/1, ST/N00003X/1, ST/N005406/2, ST/J000019/1, ST/S000550/1, ST/I006269/1, ST/K000845/1, ST/N000633/1, ST/N000072/1, ST/N005430/1, ST/H002006/1, ST/J00166X/1
National Science Foundation	1708081, 1707965, 1921006, 1806824, 1912632, 1707835, 1726215, 1806990, 1806165, 1912648

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Search for the isotropic stochastic background using data from Advanced LIGO's second observing runFinal published version, 812 KBLicence: Article 25fa Dutch Copyright Act

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@article{98814c4fd84d4e188153ca071debf7bf,

title = "Search for the isotropic stochastic background using data from Advanced LIGO's second observing run",

abstract = "The stochastic gravitational-wave background is a superposition of sources that are either too weak or too numerous to detect individually. In this study, we present the results from a cross-correlation analysis on data from Advanced LIGO's second observing run (O2), which we combine with the results of the first observing run (O1). We do not find evidence for a stochastic background, so we place upper limits on the normalized energy density in gravitational waves at the 95\% credible level of ωGW<6.0×10-8 for a frequency-independent (flat) background and ωGW<4.8×10-8 at 25 Hz for a background of compact binary coalescences. The upper limit improves over the O1 result by a factor of 2.8. Additionally, we place upper limits on the energy density in an isotropic background of scalar- and vector-polarized gravitational waves, and we discuss the implication of these results for models of compact binaries and cosmic string backgrounds. Finally, we present a conservative estimate of the correlated broadband noise due to the magnetic Schumann resonances in O2, based on magnetometer measurements at both the LIGO Hanford and LIGO Livingston observatories. We find that correlated noise is well below the O2 sensitivity.",

author = "Abbott, \{B. P.\} and R. Abbott and Abbott, \{T. D.\} and S. Abraham and F. Acernese and K. Ackley and C. Adams 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 G. Allen and A. Allocca and Aloy, \{M. A.\} and Altin, \{P. A.\} and A. Amato and A. Ananyeva and Anderson, \{S. B.\} and Anderson, \{W. G.\} and Angelova, \{S. V.\} and S. Antier and S. Appert and K. Arai and Araya, \{M. C.\} and Areeda, \{J. S.\} and M. Ar{\`e}ne and N. Arnaud and Arun, \{K. G.\} and S. Ascenzi and G. Ashton and Aston, \{S. M.\} and P. Astone and F. Aubin and P. Aufmuth and K. Aultoneal and C. Austin and V. Avendano and A. Avila-Alvarez and S. Babak and P. Bacon and F. Badaracco and Bader, \{M. K.M.\} and S. Bae and Baker, \{P. T.\} and F. Baldaccini and G. Ballardin and Ballmer, \{S. W.\} and S. Banagiri and Barayoga, \{J. C.\} and Barclay, \{S. E.\} and Barish, \{B. C.\} and D. Barker and K. Barkett and S. Barnum 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 M. Bawaj and Bayley, \{J. C.\} and M. Bazzan and B. B{\'e}csy and M. Bejger and I. Belahcene and Bell, \{A. S.\} and D. Beniwal and Berger, \{B. K.\} and G. Bergmann and S. Bernuzzi and Bero, \{J. J.\} and Berry, \{C. P.L.\} and D. Bersanetti and A. Bertolini and J. Betzwieser and R. Bhandare and J. Bidler and Bilenko, \{I. A.\} and Bilgili, \{S. A.\} and G. Billingsley and J. Birch and R. Birney and O. Birnholtz and S. Biscans and S. Biscoveanu and A. Bisht and M. Bitossi and Bizouard, \{M. A.\} and Blackburn, \{J. K.\} and Blair, \{C. D.\} and Blair, \{D. G.\} and Blair, \{R. M.\} and S. Bloemen and N. Bode and M. Boer and Y. Boetzel and G. Bogaert and F. Bondu and E. Bonilla and R. Bonnand and P. Booker and Boom, \{B. A.\} and Booth, \{C. D.\} and R. Bork and V. Boschi and S. Bose and K. Bossie and V. Bossilkov and J. Bosveld and Y. Bouffanais and A. Bozzi and C. Bradaschia and Brady, \{P. R.\} and A. Bramley and M. Branchesi and Brau, \{J. E.\} and T. Briant and Briggs, \{J. H.\} and F. Brighenti and A. Brillet and M. Brinkmann and V. Brisson and P. Brockill and Brooks, \{A. F.\} and Brown, \{D. D.\} and S. Brunett and A. Buikema and T. Bulik and Bulten, \{H. J.\} and A. Buonanno and D. Buskulic and C. Buy and Byer, \{R. L.\} and M. Cabero and L. Cadonati and G. Cagnoli and C. Cahillane and \{Calder{\'o}n Bustillo\}, J. and Callister, \{T. A.\} and E. Calloni and Camp, \{J. B.\} and Campbell, \{W. A.\} and M. Canepa and Cannon, \{K. C.\} and H. Cao and J. Cao and E. Capocasa and F. Carbognani and S. Caride and Carney, \{M. F.\} and G. Carullo and \{Casanueva Diaz\}, J. and C. Casentini and S. Caudill and M. Cavagli{\`a} and F. Cavalier and R. Cavalieri and G. Cella and P. Cerd{\'a}-Dur{\'a}n and G. Cerretani and E. Cesarini and O. Chaibi and K. Chakravarti and Chamberlin, \{S. J.\} and M. 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P.\} and Countryman, \{S. T.\} and P. Couvares and Covas, \{P. B.\} and Cowan, \{E. E.\} and Coward, \{D. M.\} and Cowart, \{M. J.\} and Coyne, \{D. C.\} and R. Coyne and Creighton, \{J. D.E.\} and Creighton, \{T. D.\} and J. Cripe and M. Croquette and Crowder, \{S. G.\} and Cullen, \{T. J.\} and A. Cumming and L. Cunningham and E. Cuoco and Canton, \{T. Dal\} and G. D{\'a}lya and Danilishin, \{S. L.\} and S. D'antonio and K. Danzmann and A. Dasgupta and \{Da Silva Costa\}, \{C. F.\} and Datrier, \{L. E.H.\} and V. Dattilo and I. Dave and M. Davier and D. Davis and Daw, \{E. J.\} and D. Debra and M. Deenadayalan and J. Degallaix and \{De Laurentis\}, M. and S. Del{\'e}glise and \{Del Pozzo\}, W. and Demarchi, \{L. M.\} and N. Demos and T. Dent and \{De Pietri\}, R. and J. Derby and \{De Rosa\}, R. and \{De Rossi\}, C. and R. Desalvo and \{De Varona\}, O. and S. Dhurandhar and D{\'i}az, \{M. C.\} and T. Dietrich and \{Di Fiore\}, L. and \{Di Giovanni\}, M. and \{Di Girolamo\}, T. and \{Di Lieto\}, A. and B. Ding and \{Di Pace\}, S. and \{Di Palma\}, I. and \{Di Renzo\}, F. and A. Dmitriev and Z. Doctor and F. Donovan and Dooley, \{K. L.\} and S. Doravari and I. Dorrington and Downes, \{T. P.\} and M. Drago and Driggers, \{J. C.\} and Z. Du and Ducoin, \{J. G.\} and P. Dupej and I. Dvorkin and Dwyer, \{S. E.\} and Easter, \{P. J.\} and Edo, \{T. B.\} and Edwards, \{M. C.\} and A. Effler and P. Ehrens and J. Eichholz and Eikenberry, \{S. S.\} and M. Eisenmann and Eisenstein, \{R. A.\} and Essick, \{R. C.\} and H. Estelles and D. Estevez and Etienne, \{Z. B.\} and T. Etzel and M. Evans and Evans, \{T. M.\} and V. Fafone and H. Fair and S. Fairhurst and X. Fan and S. Farinon and B. Farr and Farr, \{W. M.\} and Fauchon-Jones, \{E. J.\} and M. Favata and M. Fays and M. Fazio and C. Fee and J. Feicht and Fejer, \{M. M.\} and F. Feng and A. Fernandez-Galiana and I. 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Zhou and Z. Zhou and Zhu, \{X. J.\} and Zucker, \{M. E.\} and J. Zweizig and \{(LIGO Scientific and Virgo Collaboration)\}",

year = "2019",

month = sep,

day = "15",

doi = "10.1103/PhysRevD.100.061101",

language = "English",

volume = "100",

pages = "1--16",

journal = "Physical Review D",

issn = "2470-0010",

publisher = "American Physical Society",

number = "6",

}

TY - JOUR

T1 - Search for the isotropic stochastic background using data from Advanced LIGO's second observing run

AU - Abbott, B. P.

AU - Abbott, R.

AU - Abbott, T. D.

AU - Abraham, S.

AU - Acernese, F.

AU - Ackley, K.

AU - Adams, C.

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, G.

AU - Allocca, A.

AU - Aloy, M. 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 - Arène, M.

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AU - Zweizig, J.

AU - (LIGO Scientific and Virgo Collaboration)

PY - 2019/9/15

Y1 - 2019/9/15

N2 - The stochastic gravitational-wave background is a superposition of sources that are either too weak or too numerous to detect individually. In this study, we present the results from a cross-correlation analysis on data from Advanced LIGO's second observing run (O2), which we combine with the results of the first observing run (O1). We do not find evidence for a stochastic background, so we place upper limits on the normalized energy density in gravitational waves at the 95% credible level of ωGW<6.0×10-8 for a frequency-independent (flat) background and ωGW<4.8×10-8 at 25 Hz for a background of compact binary coalescences. The upper limit improves over the O1 result by a factor of 2.8. Additionally, we place upper limits on the energy density in an isotropic background of scalar- and vector-polarized gravitational waves, and we discuss the implication of these results for models of compact binaries and cosmic string backgrounds. Finally, we present a conservative estimate of the correlated broadband noise due to the magnetic Schumann resonances in O2, based on magnetometer measurements at both the LIGO Hanford and LIGO Livingston observatories. We find that correlated noise is well below the O2 sensitivity.

AB - The stochastic gravitational-wave background is a superposition of sources that are either too weak or too numerous to detect individually. In this study, we present the results from a cross-correlation analysis on data from Advanced LIGO's second observing run (O2), which we combine with the results of the first observing run (O1). We do not find evidence for a stochastic background, so we place upper limits on the normalized energy density in gravitational waves at the 95% credible level of ωGW<6.0×10-8 for a frequency-independent (flat) background and ωGW<4.8×10-8 at 25 Hz for a background of compact binary coalescences. The upper limit improves over the O1 result by a factor of 2.8. Additionally, we place upper limits on the energy density in an isotropic background of scalar- and vector-polarized gravitational waves, and we discuss the implication of these results for models of compact binaries and cosmic string backgrounds. Finally, we present a conservative estimate of the correlated broadband noise due to the magnetic Schumann resonances in O2, based on magnetometer measurements at both the LIGO Hanford and LIGO Livingston observatories. We find that correlated noise is well below the O2 sensitivity.

UR - https://www.scopus.com/pages/publications/85072995802

UR - https://www.scopus.com/inward/citedby.url?scp=85072995802&partnerID=8YFLogxK

U2 - 10.1103/PhysRevD.100.061101

DO - 10.1103/PhysRevD.100.061101

M3 - Article

AN - SCOPUS:85072995802

SN - 2470-0010

VL - 100

SP - 1

EP - 16

JO - Physical Review D

JF - Physical Review D

IS - 6

M1 - 061101

ER -

Search for the isotropic stochastic background using data from Advanced LIGO's second observing run

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