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)

Department of Physics - at Bar-Ilan University

California Institute of Technology
Louisiana State University
Inter-University Centre for Astronomy and Astrophysics India
University of Salerno
National Institute for Nuclear Physics
Monash University
Christopher Newport University
National Science Foundation
Australian National University
Max Planck Institute for Gravitational Physics (Albert Einstein Institute)
Leibniz University Hannover
University of Cambridge
Friedrich Schiller University Jena
University of Birmingham
Northwestern University
Instituto Nacional de Pesquisas Espaciais
Cardiff University
Gran Sasso Science Institute
University of Pisa
Tata Institute of Fundamental Research
National Institutes of Natural Sciences - National Astronomical Observatory of Japan
California State University Fullerton
University of Illinois at Urbana-Champaign
University of Naples Federico II
Universite Claude Bernard Lyon 1
University of Wisconsin-Milwaukee
The University of Tokyo
University of Strathclyde
University of Udine
Embry-Riddle Aeronautical University
APC - AstroParticule et Cosmologie
High Energy Accelerator Research Organization, Accelerator Laboratory
Université Paris-Saclay
European Gravitational Observatory
University of Florida
Hirosaki University
Columbia University
The Graduate University for Advanced Studies
Université Grenoble Alpes
National Institute for Subatomic Physics
Korea Institute of Science and Technology Information
National Institute for Mathematical Sciences
The University of Osaka
University of Oregon
Syracuse University
University of Liege
University of Minnesota Twin Cities
University of Milan - Bicocca
Osservatorio Astronomico di Brera
University of Barcelona
University of Glasgow
Massachusetts Institute of Technology
Wigner Research Centre for Physics
Stanford University
University of Perugia
University of Padua
Montana State University
Institute for Plasma Research
Polish Academy of Sciences
University of Sannio
Adelaide University
California State University Los Angeles
Raja Ramanna Centre for Advanced Technology
Missouri University of Science and Technology
Lomonosov Moscow State University
University of the West of Scotland
University of Urbino
boulevard de l'Observatoire
University of Western Australia
University of Rome La Sapienza
Université de Rennes 1
Indian Institute of Technology Bombay
Sorbonne Université
Université catholique de Louvain
University of Warsaw
Vrije Universiteit Amsterdam
University of Maryland, College Park
Georgia Institute of Technology
Villanova University
Chinese University of Hong Kong
Stony Brook University
Simons Foundation
NASA Goddard Space Flight Center
University of Genoa
Tsinghua University
Beijing Normal University
University of Melbourne
University of Sassari
University of Rome Tor Vergata
Utrecht University
University of Valencia
Rochester Institute of Technology
National Tsing Hua University
Fukuoka University
Charles Sturt University
Tamkang University
The University of Chicago
National Central University
Academia Sinica - Institute of Physics
Seoul National University
Pusan National University
King's College London
Astronomical Observatory of Padua
University of Arizona
Rutherford Appleton Laboratory
Université libre de Bruxelles
University of the Balearic Islands
Texas Tech University
Pennsylvania State University
University of Rhode Island
University of Texas Rio Grande Valley
Bellevue College
Scuola Normale Superiore di Pisa
Eötvös Loránd University
Maastricht University
University of Hamburg
University of Santiago de Compostela
University of Portsmouth
University of Sheffield
University of Parma
University of Zurich
Institut Pluridisciplinaire Hubert Curien
West Virginia University
Montclair State University
Colorado State University
Hungarian Academy of Sciences
University of Basilicata
University of Utah
Kenyon College
Niigata University
CAS - Innovation Academy for Precision Measurement Science and Technology
University of Szeged
Ghent University
University of British Columbia
Osservatorio Astronomico di Capodimonte
University of Trento
University of Mississippi
University of Michigan, Ann Arbor
Ulsan National Institute of Science and Technology
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University of Trieste
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American University Washington DC
University of Toyama
Carleton College
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Nihon University
National Taiwan Normal University
Chungnam National University
Aoyama Gakuin University
Peking University
Kyoto University
Osaka Metropolitan University
JAXA Institute of Space and Astronautical Science
Directorate of Construction
University of Antwerp
University of Białystok
Ewha Womans University
CAS - National Astronomical Observatories
University of Chinese Academy of Sciences
University of Southampton
ICREA
Institute of Science Tokyo
University of Washington
RAS - Institute of Applied Physics
Inje University
Myongji University
Korea Astronomy and Space Science Institute
Hiroshima University
Bard College
Institute of Mathematics of the Polish Academy of Sciences
National Centre for Nuclear Research
Cornell University
Nagoya University
University of Montreal
Université Côte d'Azur
University of Texas at Austin
Hanyang University
CNRS
National Applied Research Laboratories Taiwan
University of Amsterdam
NASA Marshall Space Flight Center
Roma Tre University
CNRS
Concordia University Wisconsin
University of Camerino
Southern University and A&M College
Center Scientific De Monaco
Indian Institute of Technology Madras
Saha Institute of Nuclear Physics
Japan National Institute of Information and Communications Technology
IHES
Ryukoku University
Indian Institute of Science Education and Research, Kolkata
Radboud University Nijmegen
University of Notre Dame
National Research Council of Italy
Hobart and William Smith Colleges
Universidade Federal do Rio Grande do Norte
Enrico Fermi Center
Lancaster University
Swinburne University of Technology
Indian Institute of Science Education and Research Pune
University of Turin
Indian Institute of Technology Gandhinagar
National Institute of Technology, Nagaoka College
SPIC Science Foundation
University of Lisbon
Marquette University
Hosei University
Toho University
Osaka Institute of Technology
Indian Institute of Technology Hyderabad
RIKEN
Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna
Andrews University
Tokyo City University
National Institute of Advanced Industrial Science and Technology
University of Groningen
National Defense Academy of Japan
Nagaoka University of Technology
Trinity University
Sejong University
National Yang Ming Chiao Tung University
Rikkyo University

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

59 Scopus citations

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
Journal	Physical Review D
Volume	104
Issue number	8
DOIs	https://doi.org/10.1103/PhysRevD.104.082004
State	Published - 15 Oct 2021

Bibliographical note

Publisher Copyright:
© 2021 us.

Funding

This material is based upon work supported by NSFs LIGO Laboratory which is a major facility fully funded by the National Science Foundation. The authors also gratefully acknowledge the support of 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 Netherlands Organization for Scientific Research, for the construction and operation of the Virgo detector and the creation and support of the 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 (SERB), 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’Innovació, Universitats, Ciència i Societat Digital de la Generalitat Valenciana and the CERCA Programme Generalitat de Catalunya, Spain, the National Science Centre of Poland and the Foundation for Polish Science (FNP), the Swiss National Science Foundation (SNSF), the Russian Foundation for Basic Research, the Russian Science Foundation, the European Commission, the European Regional Development Funds (ERDF), the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, the Hungarian Scientific Research Fund (OTKA), the French Lyon Institute of Origins (LIO), the Belgian Fonds de la Recherche Scientifique (FRS-FNRS), Actions de Recherche Concertes (ARC) and Fonds Wetenschappelijk Onderzoek Vlaanderen (FWO), Belgium, the Paris Île-de-France Region, the National Research, Development and Innovation Office Hungary (NKFIH), the National Research Foundation of Korea, the Natural Science and Engineering Research Council Canada, Canadian Foundation for Innovation (CFI), the Brazilian Ministry of Science, Technology, and Innovations, the International Center for Theoretical Physics South American Institute for Fundamental Research (ICTP-SAIFR), the Research Grants Council of Hong Kong, the National Natural Science Foundation of China (NSFC), the Leverhulme Trust, the Research Corporation, the Ministry of Science and Technology (MOST), Taiwan, the United States Department of Energy, and the Kavli Foundation. The authors gratefully acknowledge the support of the NSF, STFC, INFN and CNRS for provision of computational resources. This work was supported by MEXT, JSPS Leading-edge Research Infrastructure Program, JSPS Grant-in-Aid for Specially Promoted Research 26000005, JSPS Grant-in-Aid for Scientific Research on Innovative Areas 2905: JP17H06358, JP17H06361 and JP17H06364, JSPS Core-to-Core Program A. Advanced Research Networks, JSPS Grant-in-Aid for Scientific Research (S) 17H06133, the joint research program of the Institute for Cosmic Ray Research, University of Tokyo, National Research Foundation (NRF) and Computing Infrastructure Project of KISTI-GSDC in Korea, Academia Sinica (AS), AS Grid Center (ASGC) and the Ministry of Science and Technology (MoST) in Taiwan under grants including AS-CDA-105-M06, Advanced Technology Center (ATC) of NAOJ, and Mechanical Engineering Center of KEK. This document has been assigned LIGO Laboratory document number LIGO-P2000334-v7 .

Funders	Funder number
Actions de Recherche Concertes
Advanced Technology Center
Brazilian Ministry of Science, Technology, and Innovations
Conselleria d’Innovació, Universitats, Ciència i Societat Digital de la Generalitat Valenciana
Fonds Wetenschappelijk Onderzoek Vlaanderen
French Lyon Institute of Origins
KISTI-GSDC
NSFs
National Science Foundation
U.S. Department of Energy
Kavli Foundation
Natural Sciences and Engineering Research Council of Canada
Canada Foundation for Innovation
Science and Technology Facilities Council
Leverhulme Trust
Royal Society
Scottish Funding Council
Scottish Universities Physics Alliance
European Commission
Australian Research Council
Department of Science and Technology, Ministry of Science and Technology, India
Council of Scientific and Industrial Research, India
Japan Society for the Promotion of Science	17H06133, JP17H06361, JP17H06364, JP17H06358
Ministry of Education, Culture, Sports, Science and Technology
Schweizerischer Nationalfonds zur Förderung der Wissenschaftlichen Forschung
National Natural Science Foundation of China
Science and Engineering Research Board
Academia Sinica	AS-CDA-105-M06
Fundacja na rzecz Nauki Polskiej
Russian Foundation for Basic Research
Fonds De La Recherche Scientifique - FNRS
Generalitat de Catalunya
Research Grants Council, University Grants Committee
Nederlandse Organisatie voor Wetenschappelijk Onderzoek
Hungarian Scientific Research Fund
National Research Foundation of Korea
Instituto Nazionale di Fisica Nucleare
Narodowe Centrum Nauki
Ministry of Education, India
Ministry of Science and Technology, Taiwan
University of Tokyo
Centre National de la Recherche Scientifique
Russian Science Foundation
European Regional Development Fund
Universitat de les Illes Balears
Nemzeti Kutatási Fejlesztési és Innovációs Hivatal
Agencia Estatal de Investigación
Istituto Nazionale di Fisica Nucleare
ICTP South American Institute for Fundamental Research

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10.1103/PhysRevD.104.082004

Cite this

@article{99b538ac9849457ba56fec4323a55c6b,

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]×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.",

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 O. Birnholtz",

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

year = "2021",

month = oct,

day = "15",

doi = "10.1103/PhysRevD.104.082004",

language = "אנגלית",

volume = "104",

journal = "Physical Review D",

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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 - Birnholtz, O.

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

U2 - 10.1103/PhysRevD.104.082004

DO - 10.1103/PhysRevD.104.082004

M3 - ???researchoutput.researchoutputtypes.contributiontojournal.article???

AN - SCOPUS:85117203483

SN - 2470-0010

VL - 104

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

Abstract

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