All-sky search for continuous gravitational waves from isolated neutron stars in the early O3 LIGO data

(LIGO Scientific Collaboration, Virgo Collaboration, and KAGRA Collaboration)

doi:10.1103/PhysRevD.104.082004

All-sky search for continuous gravitational waves from isolated neutron stars in the early O3 LIGO data

(LIGO Scientific Collaboration, Virgo Collaboration, and KAGRA Collaboration)

California Institute of Technology
Louisiana State University
The Inter-University Centre for Astronomy and Astrophysics
Salerno
Complesso Universitario di Monte Sant'Angelo
Monash University
Christopher Newport University
LIGO Livingston Observatory
Australian National University
Max Planck Institute for Gravitational Physics (Albert Einstein Institute)
Leibniz Universität Hannover
University of Cambridge
Friedrich Schiller Universität
University of Birmingham
Northwestern University
Instituto Nacional de Pesquisas Espaciais
Cardiff University
Gran Sasso Science Institute
Laboratori Nazionali del Gran Sasso
INFN
Università di Pisa
Tata Institute of Fundamental Research
National Astronomical Observatory of Japan
California State University
University of Illinois
Complesso Universitario di Monte S.Angelo
Université Claude Bernard Lyon 1
University of Wisconsin-Milwaukee
University of Tokyo
University of Strathclyde
Università di Udine
Sezione di Trieste
Embry-Riddle Aeronautical University
Université de Paris
High Energy Accelerator Research Organization (KEK)
Université Paris-Saclay
European Gravitational Observatory (EGO)
University of Florida
Hirosaki University
Columbia University in the City of New York
The Graduate University for Advanced Studies
Gran Sasso Science Institute
CNRS/IN2P3
Science Park
Korea Institute of Science and Technology Information
National Institute for Mathematical Sciences
INFN Sezione di Torino
Osaka University
University of Oregon
Syracuse University
University of Liege
University of Minnesota Twin Cities
Università Degli Studi di Milano-Bicocca
Sezione di Milano-Bicocca
INAF-Osservatorio Astronomico di Brera
LIGO Hanford Observatory
University of Barcelona
Dipartimento di Medicina, Chirurgia e Odontoiatria “Scuola Medica Salernitana"
University of Glasgow
LIGO, Massachusetts Institute of Technology
Institute for Particle and Nuclear Physics
Stanford University
INFN
Università di Perugia
University of Padua
Montana State University
Institute for Plasma Research India
Nicolaus Copernicus Astronomical Center of the Polish Academy of Sciences
University of Sannio at Benevento
University of Adelaide
RRCAT
Missouri University of Science and Technology
Lomonosov Moscow State University
University of the West of Scotland
Bar-Ilan University
Università degli Studi di Urbino Carlo Bo
Sezione di Firenze
Observatoire de la Côte d'Azur
University of Western Australia
Università di Roma la Sapienza
Centre National de la Recherche Scientifique
Indian Institute of Technology Bombay
Université Pierre et Marie Curie
University of Louvain
Astronomical Observatory Warsaw University
Vrije University Amsterdam
University of Maryland
Georgia Institute of Technology
Villanova University
Chinese University of Hong Kong
Stony Brook University
Flatiron Institute
NASA/Goddard Space Flight Center
Università degli Studi di Genova
Tsinghua University
Beijing Normal University
University of Melbourne
Università degli Studi di Sassari
Laboratori Nazionali Del Sud (LNS)
Università di Roma Tor Vergata
Sezione di Roma Tor Vergata
Utrecht University
University of Valencia
Rochester Institute of Technology
National Tsing Hua University
Fukuoka University
Tamkang University
University of Chicago
National Central University Taiwan
Academia Sinica, Institute Of Physics
Seoul National University
Pusan National University

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Abstract

We report on an all-sky search for continuous gravitational waves in the frequency band 20-2000 Hz and with a frequency time derivative in the range of [-1.0,+0.1]×10-8 Hz/s. Such a signal could be produced by a nearby, spinning and slightly nonaxisymmetric isolated neutron star in our Galaxy. This search uses the LIGO data from the first six months of Advanced LIGO's and Advanced Virgo's third observational run, O3. No periodic gravitational wave signals are observed, and 95% confidence-level (C.L.) frequentist upper limits are placed on their strengths. The lowest upper limits on worst-case (linearly polarized) strain amplitude h0 are ∼1.7×10-25 near 200 Hz. For a circularly polarized source (most favorable orientation), the lowest upper limits are ∼6.3×10-26. These strict frequentist upper limits refer to all sky locations and the entire range of frequency derivative values. For a population-averaged ensemble of sky locations and stellar orientations, the lowest 95% C.L. upper limits on the strain amplitude are ∼1.4×10-25. These upper limits improve upon our previously published all-sky results, with the greatest improvement (factor of ∼2) seen at higher frequencies, in part because quantum squeezing has dramatically improved the detector noise level relative to the second observational run, O2. These limits are the most constraining to date over most of the parameter space searched.

Original language	English
Article number	A2
Pages (from-to)	1-28
Number of pages	28
Journal	Physical Review D
Volume	104
Issue number	8
DOIs	https://doi.org/10.1103/PhysRevD.104.082004
Publication status	Published - 15 Oct 2021

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10.1103/PhysRevD.104.082004

173854987 published articleFinal published version, 2.41 MB

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@article{3290f2f5b92c40649c3dd22caea89255,

title = "All-sky search for continuous gravitational waves from isolated neutron stars in the early O3 LIGO data",

abstract = "We report on an all-sky search for continuous gravitational waves in the frequency band 20-2000 Hz and with a frequency time derivative in the range of [-1.0,+0.1]{\texttimes}10-8 Hz/s. Such a signal could be produced by a nearby, spinning and slightly nonaxisymmetric isolated neutron star in our Galaxy. This search uses the LIGO data from the first six months of Advanced LIGO's and Advanced Virgo's third observational run, O3. No periodic gravitational wave signals are observed, and 95\% confidence-level (C.L.) frequentist upper limits are placed on their strengths. The lowest upper limits on worst-case (linearly polarized) strain amplitude h0 are ∼1.7{\texttimes}10-25 near 200 Hz. For a circularly polarized source (most favorable orientation), the lowest upper limits are ∼6.3{\texttimes}10-26. These strict frequentist upper limits refer to all sky locations and the entire range of frequency derivative values. For a population-averaged ensemble of sky locations and stellar orientations, the lowest 95\% C.L. upper limits on the strain amplitude are ∼1.4{\texttimes}10-25. These upper limits improve upon our previously published all-sky results, with the greatest improvement (factor of ∼2) seen at higher frequencies, in part because quantum squeezing has dramatically improved the detector noise level relative to the second observational run, O2. These limits are the most constraining to date over most of the parameter space searched.",

author = "\{(LIGO Scientific Collaboration, Virgo Collaboration, and KAGRA Collaboration)\} and R. Abbott and Abbott, \{T. D.\} and S. Abraham and F. Acernese and K. Ackley and A. Adams and C. Adams and Adhikari, \{R. X.\} and Adya, \{V. B.\} and C. Affeldt and D. Agarwal and M. Agathos and K. Agatsuma and N. Aggarwal and Aguiar, \{O. D.\} and L. Aiello and A. Ain and P. Ajith and T. Akutsu and Aleman, \{K. M.\} and G. Allen and A. Allocca and Altin, \{P. A.\} and A. Amato and S. Anand and A. Ananyeva and Anderson, \{S. B.\} and Anderson, \{W. G.\} and M. Ando and Angelova, \{S. V.\} and S. Ansoldi and Antelis, \{J. M.\} and S. Antier and S. Appert and Koya Arai and Koji Arai and Y. Arai and S. Araki and A. Araya and Araya, \{M. C.\} and Areeda, \{J. S.\} and M. Ar{\`e}ne and N. Aritomi and N. Arnaud and Aronson, \{S. M.\} and H. Asada and Y. Asali and G. Ashton and Y. Aso and Aston, \{S. M.\} and P. Astone and F. Aubin and P. Aufmuth and K. Aultoneal and C. Austin and S. Babak and F. Badaracco and Bader, \{M. K.M.\} and S. Bae and Y. Bae and Baer, \{A. M.\} and S. Bagnasco and Y. Bai and L. Baiotti and J. Baird and R. Bajpai and M. Ball and G. Ballardin and Ballmer, \{S. W.\} and M. Bals and A. Balsamo and G. Baltus and S. Banagiri and D. Bankar and Bankar, \{R. S.\} and Barayoga, \{J. C.\} and C. Barbieri and Barish, \{B. C.\} and D. Barker and P. Barneo and F. Barone and B. Barr and L. Barsotti and M. Barsuglia and D. Barta and J. Bartlett and Barton, \{M. A.\} and I. Bartos and R. Bassiri and A. Basti and M. Bawaj and Bayley, \{J. C.\} and Baylor, \{A. C.\} and M. Bazzan and B. B{\'e}csy and Bedakihale, \{V. M.\} and M. Bejger and I. Belahcene and V. Benedetto and D. Beniwal and Benjamin, \{M. G.\} and Bennett, \{T. F.\} and Bentley, \{J. D.\} and M. Benyaala and F. Bergamin and Berger, \{B. K.\} and S. Bernuzzi and D. Bersanetti and A. Bertolini and J. Betzwieser and R. Bhandare and Bhandari, \{A. V.\} and D. Bhattacharjee and S. Bhaumik and J. Bidler and Bilenko, \{I. A.\} and G. Billingsley and R. Birney and O. Birnholtz and S. Biscans and M. Bischi and S. Biscoveanu and A. Bisht and B. Biswas and M. Bitossi and Bizouard, \{M. A.\} and Blackburn, \{J. K.\} and J. Blackman and Blair, \{C. D.\} and Blair, \{D. G.\} and Blair, \{R. M.\} and F. Bobba and N. Bode and M. Boer and G. Bogaert and M. Boldrini and F. Bondu and E. Bonilla and R. Bonnand and P. Booker and Boom, \{B. A.\} and R. Bork and V. Boschi and N. Bose and S. Bose and V. Bossilkov and V. Boudart and Y. Bouffanais and A. Bozzi and C. Bradaschia and Brady, \{P. R.\} and A. Bramley and A. Branch and M. Branchesi and Brau, \{J. E.\} and M. Breschi and T. Briant and Briggs, \{J. H.\} and A. Brillet and M. Brinkmann and P. Brockill and Brooks, \{A. F.\} and J. Brooks and Brown, \{D. D.\} and S. Brunett and G. Bruno and R. Bruntz and J. Bryant and A. Buikema and T. Bulik and Bulten, \{H. J.\} and A. Buonanno and R. Buscicchio and D. Buskulic and Byer, \{R. L.\} and L. Cadonati and M. Caesar and G. Cagnoli and C. Cahillane and Cain, \{H. W.\} and \{Calder{\'o}n Bustillo\}, J. and Callaghan, \{J. D.\} and Callister, \{T. A.\} and E. Calloni and Camp, \{J. B.\} and M. Canepa and M. Cannavacciuolo and Cannon, \{K. C.\} and H. Cao and J. Cao and Z. Cao and E. Capocasa and E. Capote and G. Carapella and F. Carbognani and Carlin, \{J. B.\} and Carney, \{M. F.\} and M. Carpinelli and G. Carullo and Carver, \{T. L.\} and \{Casanueva Diaz\}, J. and C. Casentini and G. Castaldi and S. Caudill and M. Cavagli{\`a} and F. Cavalier and R. Cavalieri and G. Cella and P. Cerd{\'a}-Dur{\'a}n and E. Cesarini and W. Chaibi and K. Chakravarti and B. Champion and Chan, \{C. H.\} and Chan, \{C. L.\} and Chan, \{C. L.\} and M. Chan and K. Chandra and P. Chanial and S. Chao and P. Charlton and Chase, \{E. A.\} and E. Chassande-Mottin and D. Chatterjee and M. Chaturvedi and A. Chen and C. Chen and Chen, \{H. Y.\} and J. Chen and K. Chen and X. Chen and Chen, \{Y. B.\} and Chen, \{Y. R.\} and Z. Chen and H. Cheng and Cheong, \{C. K.\} and Cheung, \{H. Y.\} and Chia, \{H. Y.\} and F. Chiadini and Chiang, \{C. Y.\} and R. Chierici and A. Chincarini and Chiofalo, \{M. L.\} and A. Chiummo and G. Cho and Cho, \{H. S.\} and S. Choate and Choudhary, \{R. K.\} and S. Choudhary and N. Christensen",

note = "Publisher Copyright: {\textcopyright} 2021 us. ",

year = "2021",

month = oct,

day = "15",

doi = "10.1103/PhysRevD.104.082004",

language = "English",

volume = "104",

pages = "1--28",

journal = "Physical Review D",

issn = "2470-0010",

publisher = "American Physical Society",

number = "8",

}

TY - JOUR

T1 - All-sky search for continuous gravitational waves from isolated neutron stars in the early O3 LIGO data

AU - (LIGO Scientific Collaboration, Virgo Collaboration, and KAGRA Collaboration)

AU - Abbott, R.

AU - Abbott, T. D.

AU - Abraham, S.

AU - Acernese, F.

AU - Ackley, K.

AU - Adams, A.

AU - Adams, C.

AU - Adhikari, R. X.

AU - Adya, V. B.

AU - Affeldt, C.

AU - Agarwal, D.

AU - Agathos, M.

AU - Agatsuma, K.

AU - Aggarwal, N.

AU - Aguiar, O. D.

AU - Aiello, L.

AU - Ain, A.

AU - Ajith, P.

AU - Akutsu, T.

AU - Aleman, K. M.

AU - Allen, G.

AU - Allocca, A.

AU - Altin, P. A.

AU - Amato, A.

AU - Anand, S.

AU - Ananyeva, A.

AU - Anderson, S. B.

AU - Anderson, W. G.

AU - Ando, M.

AU - Angelova, S. V.

AU - Ansoldi, S.

AU - Antelis, J. M.

AU - Antier, S.

AU - Appert, S.

AU - Arai, Koya

AU - Arai, Koji

AU - Arai, Y.

AU - Araki, S.

AU - Araya, A.

AU - Araya, M. C.

AU - Areeda, J. S.

AU - Arène, M.

AU - Aritomi, N.

AU - Arnaud, N.

AU - Aronson, S. M.

AU - Asada, H.

AU - Asali, Y.

AU - Ashton, G.

AU - Aso, Y.

AU - Aston, S. M.

AU - Astone, P.

AU - Aubin, F.

AU - Aufmuth, P.

AU - Aultoneal, K.

AU - Austin, C.

AU - Babak, S.

AU - Badaracco, F.

AU - Bader, M. K.M.

AU - Bae, S.

AU - Bae, Y.

AU - Baer, A. M.

AU - Bagnasco, S.

AU - Bai, Y.

AU - Baiotti, L.

AU - Baird, J.

AU - Bajpai, R.

AU - Ball, M.

AU - Ballardin, G.

AU - Ballmer, S. W.

AU - Bals, M.

AU - Balsamo, A.

AU - Baltus, G.

AU - Banagiri, S.

AU - Bankar, D.

AU - Bankar, R. S.

AU - Barayoga, J. C.

AU - Barbieri, C.

AU - Barish, B. C.

AU - Barker, D.

AU - Barneo, P.

AU - Barone, F.

AU - Barr, B.

AU - Barsotti, L.

AU - Barsuglia, M.

AU - Barta, D.

AU - Bartlett, J.

AU - Barton, M. A.

AU - Bartos, I.

AU - Bassiri, R.

AU - Basti, A.

AU - Bawaj, M.

AU - Bayley, J. C.

AU - Baylor, A. C.

AU - Bazzan, M.

AU - Bécsy, B.

AU - Bedakihale, V. M.

AU - Bejger, M.

AU - Belahcene, I.

AU - Benedetto, V.

AU - Beniwal, D.

AU - Benjamin, M. G.

AU - Bennett, T. F.

AU - Bentley, J. D.

AU - Benyaala, M.

AU - Bergamin, F.

AU - Berger, B. K.

AU - Bernuzzi, S.

AU - Bersanetti, D.

AU - Bertolini, A.

AU - Betzwieser, J.

AU - Bhandare, R.

AU - Bhandari, A. V.

AU - Bhattacharjee, D.

AU - Bhaumik, S.

AU - Bidler, J.

AU - Bilenko, I. A.

AU - Billingsley, G.

AU - Birney, R.

AU - Birnholtz, O.

AU - Biscans, S.

AU - Bischi, M.

AU - Biscoveanu, S.

AU - Bisht, A.

AU - Biswas, B.

AU - Bitossi, M.

AU - Bizouard, M. A.

AU - Blackburn, J. K.

AU - Blackman, J.

AU - Blair, C. D.

AU - Blair, D. G.

AU - Blair, R. M.

AU - Bobba, F.

AU - Bode, N.

AU - Boer, M.

AU - Bogaert, G.

AU - Boldrini, M.

AU - Bondu, F.

AU - Bonilla, E.

AU - Bonnand, R.

AU - Booker, P.

AU - Boom, B. A.

AU - Bork, R.

AU - Boschi, V.

AU - Bose, N.

AU - Bose, S.

AU - Bossilkov, V.

AU - Boudart, V.

AU - Bouffanais, Y.

AU - Bozzi, A.

AU - Bradaschia, C.

AU - Brady, P. R.

AU - Bramley, A.

AU - Branch, A.

AU - Branchesi, M.

AU - Brau, J. E.

AU - Breschi, M.

AU - Briant, T.

AU - Briggs, J. H.

AU - Brillet, A.

AU - Brinkmann, M.

AU - Brockill, P.

AU - Brooks, A. F.

AU - Brooks, J.

AU - Brown, D. D.

AU - Brunett, S.

AU - Bruno, G.

AU - Bruntz, R.

AU - Bryant, J.

AU - Buikema, A.

AU - Bulik, T.

AU - Bulten, H. J.

AU - Buonanno, A.

AU - Buscicchio, R.

AU - Buskulic, D.

AU - Byer, R. L.

AU - Cadonati, L.

AU - Caesar, M.

AU - Cagnoli, G.

AU - Cahillane, C.

AU - Cain, H. W.

AU - Calderón Bustillo, J.

AU - Callaghan, J. D.

AU - Callister, T. A.

AU - Calloni, E.

AU - Camp, J. B.

AU - Canepa, M.

AU - Cannavacciuolo, M.

AU - Cannon, K. C.

AU - Cao, H.

AU - Cao, J.

AU - Cao, Z.

AU - Capocasa, E.

AU - Capote, E.

AU - Carapella, G.

AU - Carbognani, F.

AU - Carlin, J. B.

AU - Carney, M. F.

AU - Carpinelli, M.

AU - Carullo, G.

AU - Carver, T. L.

AU - Casanueva Diaz, J.

AU - Casentini, C.

AU - Castaldi, G.

AU - Caudill, S.

AU - Cavaglià, M.

AU - Cavalier, F.

AU - Cavalieri, R.

AU - Cella, G.

AU - Cerdá-Durán, P.

AU - Cesarini, E.

AU - Chaibi, W.

AU - Chakravarti, K.

AU - Champion, B.

AU - Chan, C. H.

AU - Chan, C. L.

AU - Chan, M.

AU - Chandra, K.

AU - Chanial, P.

AU - Chao, S.

AU - Charlton, P.

AU - Chase, E. A.

AU - Chassande-Mottin, E.

AU - Chatterjee, D.

AU - Chaturvedi, M.

AU - Chen, A.

AU - Chen, C.

AU - Chen, H. Y.

AU - Chen, J.

AU - Chen, K.

AU - Chen, X.

AU - Chen, Y. B.

AU - Chen, Y. R.

AU - Chen, Z.

AU - Cheng, H.

AU - Cheong, C. K.

AU - Cheung, H. Y.

AU - Chia, H. Y.

AU - Chiadini, F.

AU - Chiang, C. Y.

AU - Chierici, R.

AU - Chincarini, A.

AU - Chiofalo, M. L.

AU - Chiummo, A.

AU - Cho, G.

AU - Cho, H. S.

AU - Choate, S.

AU - Choudhary, R. K.

AU - Choudhary, S.

AU - Christensen, N.

PY - 2021/10/15

Y1 - 2021/10/15

N2 - We report on an all-sky search for continuous gravitational waves in the frequency band 20-2000 Hz and with a frequency time derivative in the range of [-1.0,+0.1]×10-8 Hz/s. Such a signal could be produced by a nearby, spinning and slightly nonaxisymmetric isolated neutron star in our Galaxy. This search uses the LIGO data from the first six months of Advanced LIGO's and Advanced Virgo's third observational run, O3. No periodic gravitational wave signals are observed, and 95% confidence-level (C.L.) frequentist upper limits are placed on their strengths. The lowest upper limits on worst-case (linearly polarized) strain amplitude h0 are ∼1.7×10-25 near 200 Hz. For a circularly polarized source (most favorable orientation), the lowest upper limits are ∼6.3×10-26. These strict frequentist upper limits refer to all sky locations and the entire range of frequency derivative values. For a population-averaged ensemble of sky locations and stellar orientations, the lowest 95% C.L. upper limits on the strain amplitude are ∼1.4×10-25. These upper limits improve upon our previously published all-sky results, with the greatest improvement (factor of ∼2) seen at higher frequencies, in part because quantum squeezing has dramatically improved the detector noise level relative to the second observational run, O2. These limits are the most constraining to date over most of the parameter space searched.

AB - We report on an all-sky search for continuous gravitational waves in the frequency band 20-2000 Hz and with a frequency time derivative in the range of [-1.0,+0.1]×10-8 Hz/s. Such a signal could be produced by a nearby, spinning and slightly nonaxisymmetric isolated neutron star in our Galaxy. This search uses the LIGO data from the first six months of Advanced LIGO's and Advanced Virgo's third observational run, O3. No periodic gravitational wave signals are observed, and 95% confidence-level (C.L.) frequentist upper limits are placed on their strengths. The lowest upper limits on worst-case (linearly polarized) strain amplitude h0 are ∼1.7×10-25 near 200 Hz. For a circularly polarized source (most favorable orientation), the lowest upper limits are ∼6.3×10-26. These strict frequentist upper limits refer to all sky locations and the entire range of frequency derivative values. For a population-averaged ensemble of sky locations and stellar orientations, the lowest 95% C.L. upper limits on the strain amplitude are ∼1.4×10-25. These upper limits improve upon our previously published all-sky results, with the greatest improvement (factor of ∼2) seen at higher frequencies, in part because quantum squeezing has dramatically improved the detector noise level relative to the second observational run, O2. These limits are the most constraining to date over most of the parameter space searched.

UR - https://www.scopus.com/pages/publications/85117203483

UR - https://www.scopus.com/pages/publications/85117203483#tab=citedBy

U2 - 10.1103/PhysRevD.104.082004

DO - 10.1103/PhysRevD.104.082004

M3 - Article

AN - SCOPUS:85117203483

SN - 2470-0010

VL - 104

SP - 1

EP - 28

JO - Physical Review D

JF - Physical Review D

IS - 8

M1 - A2

ER -

All-sky search for continuous gravitational waves from isolated neutron stars in the early O3 LIGO data

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