All-sky search for long-duration gravitational-wave bursts in the third Advanced LIGO and Advanced Virgo run

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

doi:10.1103/PhysRevD.104.102001

All-sky search for long-duration gravitational-wave bursts in the third Advanced LIGO and Advanced Virgo run

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

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

2 Citations (Scopus)

Abstract

After the detection of gravitational waves from compact binary coalescences, the search for transient gravitational-wave signals with less well-defined waveforms for which matched filtering is not well suited is one of the frontiers for gravitational-wave astronomy. Broadly classified into "short"1 s and "long"1 s duration signals, these signals are expected from a variety of astrophysical processes, including non-axisymmetric deformations in magnetars or eccentric binary black hole coalescences. In this work, we present a search for long-duration gravitational-wave transients from Advanced LIGO and Advanced Virgo's third observing run from April 2019 to March 2020. For this search, we use minimal assumptions for the sky location, event time, waveform morphology, and duration of the source. The search covers the range of 2-500 s in duration and a frequency band of 24-2048 Hz. We find no significant triggers within this parameter space; we report sensitivity limits on the signal strength of gravitational waves characterized by the root-sum-square amplitude hrss as a function of waveform morphology. These hrss limits improve upon the results from the second observing run by an average factor of 1.8.

Original language	English
Article number	102001
Pages (from-to)	1-17
Number of pages	17
Journal	Physical Review D
Volume	104
Issue number	10
DOIs	https://doi.org/10.1103/PhysRevD.104.102001
Publication status	Published - 11 Nov 2021

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10.1103/PhysRevD.104.102001

Cite this

@article{74c838fd2b9e46e9af3cd28ed9741bba,

title = "All-sky search for long-duration gravitational-wave bursts in the third Advanced LIGO and Advanced Virgo run",

abstract = "After the detection of gravitational waves from compact binary coalescences, the search for transient gravitational-wave signals with less well-defined waveforms for which matched filtering is not well suited is one of the frontiers for gravitational-wave astronomy. Broadly classified into {"}short{"}1 s and {"}long{"}1 s duration signals, these signals are expected from a variety of astrophysical processes, including non-axisymmetric deformations in magnetars or eccentric binary black hole coalescences. In this work, we present a search for long-duration gravitational-wave transients from Advanced LIGO and Advanced Virgo's third observing run from April 2019 to March 2020. For this search, we use minimal assumptions for the sky location, event time, waveform morphology, and duration of the source. The search covers the range of 2-500 s in duration and a frequency band of 24-2048 Hz. We find no significant triggers within this parameter space; we report sensitivity limits on the signal strength of gravitational waves characterized by the root-sum-square amplitude hrss as a function of waveform morphology. These hrss limits improve upon the results from the second observing run by an average factor of 1.8.",

author = "{(LIGO Scientific Collaboration, Virgo Collaboration, and KAGRA Collaboration)} and R. Abbott and Abbott, {T. D.} and F. Acernese and K. Ackley and C. Adams and N. Adhikari 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 S. Albanesi and A. Allocca and Altin, {P. A.} and A. Amato and C. Anand and S. Anand and A. Ananyeva and Anderson, {S. B.} and Anderson, {W. G.} and M. Ando and T. Andrade and N. Andres and T. Andri{\'c} and Angelova, {S. V.} and S. Ansoldi and Antelis, {J. M.} and S. Antier and S. Appert and Koji Arai and Koya 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 Arun, {K. G.} and H. Asada and Y. Asali and G. Ashton and Y. Aso and M. Assiduo and Aston, {S. M.} and P. Astone and F. Aubin and C. Austin and S. Babak and F. Badaracco and Bader, {M. K.M.} and C. Badger 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 A. Balsamo and G. Baltus and S. Banagiri and D. Bankar 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 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 D. Beveridge and R. Bhandare and U. Bhardwaj and D. Bhattacharjee and S. Bhaumik and Bilenko, {I. A.} and G. Billingsley and S. Bini 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 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 Bonavena, {L. D.} 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 T. Bulik and Bulten, {H. J.} and A. Buonanno and R. Buscicchio and D. Buskulic and C. Buy and Byer, {R. L.} and L. Cadonati and G. Cagnoli and C. Cahillane and Bustillo, {J. Calder{\'o}n} and Callaghan, {J. D.} and Callister, {T. A.} and E. Calloni and J. Cameron and Camp, {J. B.} and M. Canepa and S. Canevarolo and M. Cannavacciuolo and Cannon, {K. C.} and H. 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. Carrillo and G. Carullo and Carver, {T. L.} and Diaz, {J. Casanueva} and C. Casentini and G. Castaldi and S. Caudill and M. Cavagli{\`a} and F. Cavalier and R. Cavalieri and M. Ceasar and G. Cella and P. Cerd{\'a}-Dur{\'a}n and E. Cesarini and W. Chaibi and K. Chakravarti and Subrahmanya, {S. Chalathadka} and E. Champion and Chan, {C. H.} and Chan, {C. L.} and Chan, {C. L.} and K. Chan and M. Chan and K. Chandra and P. Chanial and S. Chao and Philip Charlton and Chase, {E. A.} and E. Chassande-Mottin and C. Chatterjee and Debarati Chatterjee and Deep Chatterjee and M. Chaturvedi and S. Chaty 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 G. Chiarini and R. Chierici and A. Chincarini and Chiofalo, {M. L.}",

note = "Funding Information: This material is based upon work supported by NSF{\textquoteright}s 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 Investigaci{\'o}n, the Vicepresid{\`e}ncia i Conselleria d{\textquoteright}Innovaci{\'o}, Recerca i Turisme and the Conselleria d{\textquoteright}Educaci{\'o} i Universitat del Govern de les Illes Balears, the Conselleria d{\textquoteright}Innovaci{\'o}, Universitats, Ci{\`e}ncia 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 Concert{\'e}es (ARC) and Fonds Wetenschappelijk Onderzoek—Vlaanderen (FWO), Belgium, the Paris {\^I}le-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: Grants No. JP17H06358, No. JP17H06361, and No. JP17H06364, JSPS Core-to-Core Program A. Advanced Research Networks, JSPS Grant-in-Aid for Scientific Research (S) Grants No. 17H06133 and No. 20H05639, JSPS Grant-in-Aid for Transformative Research Areas (A) 20A203: Grant No. JP20H05854, 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 Grant No. AS-CDA-105-M06, Advanced Technology Center (ATC) of NAOJ, Mechanical Engineering Center of KEK. Publisher Copyright: {\textcopyright} 2021 us.",

year = "2021",

month = nov,

day = "11",

doi = "10.1103/PhysRevD.104.102001",

language = "English",

volume = "104",

pages = "1--17",

journal = "Physical Review D: covering particles, fields, gravitation, and cosmology",

issn = "1550-2368",

publisher = "AMER PHYSICAL SOC",

number = "10",

}

TY - JOUR

T1 - All-sky search for long-duration gravitational-wave bursts in the third Advanced LIGO and Advanced Virgo run

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

AU - Abbott, R.

AU - Abbott, T. D.

AU - Acernese, F.

AU - Ackley, K.

AU - Adams, C.

AU - Adhikari, N.

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 - Albanesi, S.

AU - Allocca, A.

AU - Altin, P. A.

AU - Amato, A.

AU - Anand, C.

AU - Anand, S.

AU - Ananyeva, A.

AU - Anderson, S. B.

AU - Anderson, W. G.

AU - Ando, M.

AU - Andrade, T.

AU - Andres, N.

AU - Andrić, T.

AU - Angelova, S. V.

AU - Ansoldi, S.

AU - Antelis, J. M.

AU - Antier, S.

AU - Appert, S.

AU - Arai, Koji

AU - Arai, Koya

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 - Arun, K. G.

AU - Asada, H.

AU - Asali, Y.

AU - Ashton, G.

AU - Aso, Y.

AU - Assiduo, M.

AU - Aston, S. M.

AU - Astone, P.

AU - Aubin, F.

AU - Austin, C.

AU - Babak, S.

AU - Badaracco, F.

AU - Bader, M. K.M.

AU - Badger, C.

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 - Balsamo, A.

AU - Baltus, G.

AU - Banagiri, S.

AU - Bankar, D.

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 - 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 - Beveridge, D.

AU - Bhandare, R.

AU - Bhardwaj, U.

AU - Bhattacharjee, D.

AU - Bhaumik, S.

AU - Bilenko, I. A.

AU - Billingsley, G.

AU - Bini, S.

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 - 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 - Bonavena, L. D.

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 - Bulik, T.

AU - Bulten, H. J.

AU - Buonanno, A.

AU - Buscicchio, R.

AU - Buskulic, D.

AU - Buy, C.

AU - Byer, R. L.

AU - Cadonati, L.

AU - Cagnoli, G.

AU - Cahillane, C.

AU - Bustillo, J. Calderón

AU - Callaghan, J. D.

AU - Callister, T. A.

AU - Calloni, E.

AU - Cameron, J.

AU - Camp, J. B.

AU - Canepa, M.

AU - Canevarolo, S.

AU - Cannavacciuolo, M.

AU - Cannon, K. C.

AU - Cao, H.

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 - Carrillo, G.

AU - Carullo, G.

AU - Carver, T. L.

AU - Diaz, J. Casanueva

AU - Casentini, C.

AU - Castaldi, G.

AU - Caudill, S.

AU - Cavaglià, M.

AU - Cavalier, F.

AU - Cavalieri, R.

AU - Ceasar, M.

AU - Cella, G.

AU - Cerdá-Durán, P.

AU - Cesarini, E.

AU - Chaibi, W.

AU - Chakravarti, K.

AU - Subrahmanya, S. Chalathadka

AU - Champion, E.

AU - Chan, C. H.

AU - Chan, C. L.

AU - Chan, K.

AU - Chan, M.

AU - Chandra, K.

AU - Chanial, P.

AU - Chao, S.

AU - Charlton, Philip

AU - Chase, E. A.

AU - Chassande-Mottin, E.

AU - Chatterjee, C.

AU - Chatterjee, Debarati

AU - Chatterjee, Deep

AU - Chaturvedi, M.

AU - Chaty, S.

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 - Chiarini, G.

AU - Chierici, R.

AU - Chincarini, A.

AU - Chiofalo, M. L.

N1 - Funding Information: This material is based upon work supported by NSF’s 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 Concertées (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: Grants No. JP17H06358, No. JP17H06361, and No. JP17H06364, JSPS Core-to-Core Program A. Advanced Research Networks, JSPS Grant-in-Aid for Scientific Research (S) Grants No. 17H06133 and No. 20H05639, JSPS Grant-in-Aid for Transformative Research Areas (A) 20A203: Grant No. JP20H05854, 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 Grant No. AS-CDA-105-M06, Advanced Technology Center (ATC) of NAOJ, Mechanical Engineering Center of KEK. Publisher Copyright: © 2021 us.

PY - 2021/11/11

Y1 - 2021/11/11

N2 - After the detection of gravitational waves from compact binary coalescences, the search for transient gravitational-wave signals with less well-defined waveforms for which matched filtering is not well suited is one of the frontiers for gravitational-wave astronomy. Broadly classified into "short"1 s and "long"1 s duration signals, these signals are expected from a variety of astrophysical processes, including non-axisymmetric deformations in magnetars or eccentric binary black hole coalescences. In this work, we present a search for long-duration gravitational-wave transients from Advanced LIGO and Advanced Virgo's third observing run from April 2019 to March 2020. For this search, we use minimal assumptions for the sky location, event time, waveform morphology, and duration of the source. The search covers the range of 2-500 s in duration and a frequency band of 24-2048 Hz. We find no significant triggers within this parameter space; we report sensitivity limits on the signal strength of gravitational waves characterized by the root-sum-square amplitude hrss as a function of waveform morphology. These hrss limits improve upon the results from the second observing run by an average factor of 1.8.

AB - After the detection of gravitational waves from compact binary coalescences, the search for transient gravitational-wave signals with less well-defined waveforms for which matched filtering is not well suited is one of the frontiers for gravitational-wave astronomy. Broadly classified into "short"1 s and "long"1 s duration signals, these signals are expected from a variety of astrophysical processes, including non-axisymmetric deformations in magnetars or eccentric binary black hole coalescences. In this work, we present a search for long-duration gravitational-wave transients from Advanced LIGO and Advanced Virgo's third observing run from April 2019 to March 2020. For this search, we use minimal assumptions for the sky location, event time, waveform morphology, and duration of the source. The search covers the range of 2-500 s in duration and a frequency band of 24-2048 Hz. We find no significant triggers within this parameter space; we report sensitivity limits on the signal strength of gravitational waves characterized by the root-sum-square amplitude hrss as a function of waveform morphology. These hrss limits improve upon the results from the second observing run by an average factor of 1.8.

UR - http://www.scopus.com/inward/record.url?scp=85120443427&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=85120443427&partnerID=8YFLogxK

U2 - 10.1103/PhysRevD.104.102001

DO - 10.1103/PhysRevD.104.102001

M3 - Article

AN - SCOPUS:85120443427

VL - 104

SP - 1

EP - 17

JO - Physical Review D: covering particles, fields, gravitation, and cosmology

JF - Physical Review D: covering particles, fields, gravitation, and cosmology

SN - 1550-2368

IS - 10

M1 - 102001

ER -

All-sky search for long-duration gravitational-wave bursts in the third Advanced LIGO and Advanced Virgo run

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