Constraints from LIGO O3 Data on Gravitational-wave Emission Due to R-modes in the Glitching Pulsar PSR J0537–6910
- Creators
- Abbott, R.
- Abbott, T. D.
- Abraham, S.
- Acernese, F.
- Ackley, K.
- Adams, A.
- Adams, C.
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Adhikari, R. X.
- Adya, V. B.
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- Agatsuma, K.
- Aggarwal, N.
- Aguiar, O. D.
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Ajith, P.
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Akutsu, T.
- Aleman, K. M.
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Allocca, A.
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Amato, A.
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Anand, S.
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Anderson, S. B.
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Ansoldi, S.
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Arai, Koji
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Araya, A.
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Araya, M. C.
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Areeda, J. S.
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Arnaud, N.
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Ashton, G.
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Aso, Y.
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Austin, C.
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Bae, Y.
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- Baiotti, L.
- Baird, J.
- Bajpai, R.
- Ball, M.
- Ballardin, G.
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Ballmer, S. W.
- Bals, M.
- Balsamo, A.
- Baltus, G.
- Banagiri, S.
- Bankar, D.
- Bankar, R. S.
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Barsotti, L.
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Barton, M. A.
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Bartos, I.
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Bassiri, R.
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Bernuzzi, S.
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Bizouard, M.-A.
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Blackburn, J. K.
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Blackman, J.
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- Yang, Yi
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- Ying, M.
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Yu, Hang
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Yu, Haocun
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- Zhao, Yue
-
Zhao, Yuhang
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Zucker, M. E.
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Zweizig, J.
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Enoto, T.
- Espinoza, C. M.
-
Guillot, S.
- LIGO Scientific Collaboration
- Virgo Collaboration
- KAGRA Collaboration
Abstract
We present a search for continuous gravitational-wave emission due to r-modes in the pulsar PSR J0537–6910 using data from the LIGO–Virgo Collaboration observing run O3. PSR J0537–6910 is a young energetic X-ray pulsar and is the most frequent glitcher known. The inter-glitch braking index of the pulsar suggests that gravitational-wave emission due to r-mode oscillations may play an important role in the spin evolution of this pulsar. Theoretical models confirm this possibility and predict emission at a level that can be probed by ground-based detectors. In order to explore this scenario, we search for r-mode emission in the epochs between glitches by using a contemporaneous timing ephemeris obtained from NICER data. We do not detect any signals in the theoretically expected band of 86–97 Hz, and report upper limits on the amplitude of the gravitational waves. Our results improve on previous amplitude upper limits from r-modes in J0537-6910 by a factor of up to 3 and place stringent constraints on theoretical models for r-mode-driven spin-down in PSR J0537–6910, especially for higher frequencies at which our results reach below the spin-down limit defined by energy conservation.
Additional Information
© 2021. The American Astronomical Society. Received 2021 April 29; revised 2021 June 15; accepted 2021 June 15; published 2021 November 23. 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 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: 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. We would like to thank all of the essential workers who put their health at risk during the COVID-19 pandemic, without whom we would not have been able to complete this work. D.An. acknowledges support from an EPSRC fellowship (EP/T017325/1) and NCN grant 2015/18/E/ST9/00577. T.En. is supported by JSPS/MEXT KAKENHI grant numbers 15H00845, 17K18776, and 18H04584. C.M.E. acknowledges support from ANID FONDECYT/Regular 1171421. W.C.G.H. acknowledges support through grant 80NSSC21K0091 from NASA.Attached Files
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Additional details
- Eprint ID
- 110562
- Resolver ID
- CaltechAUTHORS:20210825-184643051
- NSF
- Science and Technology Facilities Council (STFC)
- Max-Planck-Society
- State of Niedersachsen/Germany
- Australian Research Council
- Istituto Nazionale di Fisica Nucleare (INFN)
- Centre National de la Recherche Scientifique (CNRS)
- Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)
- Council of Scientific and Industrial Research (India)
- Department of Science and Technology (India)
- Science and Engineering Research Board (SERB)
- Ministry of Human Resource Development (India)
- Agencia Estatal de Investigación
- Vicepresidència i Conselleria d'Innovació, Recerca i Turisme
- Conselleria d'Educacío i Universitat del Govern de les Illes Balears
- Conselleria d'Innovació, Universitats, Ciència i Societat Digital de la Generalitat Valenciana
- Generalitat de Catalunya
- Foundation for Polish Science
- Swiss National Science Foundation (SNSF)
- Russian Foundation for Basic Research
- Russian Science Foundation
- European Commission
- European Regional Development Funds (ERDF)
- Royal Society
- Scottish Funding Council
- Scottish Universities Physics Alliance
- Hungarian Scientific Research Fund (OTKA)
- Lyon Institute of Origins (LIO)
- Fonds de la Recherche Scientifique (FNRS)
- Actions de Recherche Concertees (Communauté Française de Belgique)
- Fonds Wetenschappelijk Onderzoek (FWO)
- Île-de-France Region
- National Research, Development and Innovation Office (Hungary)
- National Research Foundation of Korea
- Natural Science and Engineering Research Council of Canada (NSERC)
- Canada Foundation for Innovation
- Ministério da Ciência, Tecnologia, Inovações e Comunicações (MCTIC)
- International Center for Theoretical Physics South American Institute for Fundamental Research (ICTP-SAIFR)
- Research Grants Council of Hong Kong
- National Natural Science Foundation of China
- Leverhulme Trust
- Research Corporation
- Department of Energy (DOE)
- Kavli Foundation
- Ministry of Education, Culture, Sports, Science and Technology (MEXT)
- Japan Society for the Promotion of Science (JSPS)
- 26000005
- Japan Society for the Promotion of Science (JSPS)
- JP17H06358
- Japan Society for the Promotion of Science (JSPS)
- JP17H06361
- Japan Society for the Promotion of Science (JSPS)
- JP17H06364
- Japan Society for the Promotion of Science (JSPS)
- 17H06133
- Institute for Cosmic Ray Research
- University of Tokyo
- Korea Institute of Science and Technology Information (KISTI)
- Academia Sinica
- Ministry of Science and Technology (Taipei)
- AS-CDA-105-M06
- National Astronomical Observatory of Japan
- High Energy Accelerator Research Organization (KEK)
- Engineering and Physical Sciences Research Council (EPSRC)
- EP/T017325/1
- National Science Centre (Poland)
- 2015/18/E/ST9/00577
- Japan Society for the Promotion of Science (JSPS)
- 15H00845
- Japan Society for the Promotion of Science (JSPS)
- 17K18776
- Japan Society for the Promotion of Science (JSPS)
- 18H04584
- Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT)
- 1171421
- NASA
- 80NSSC21K0091
- Created
-
2021-08-30Created from EPrint's datestamp field
- Updated
-
2022-10-28Created from EPrint's last_modified field
- Caltech groups
- LIGO, Astronomy Department, TAPIR
- Other Numbering System Name
- LIGO Document
- Other Numbering System Identifier
- P2100069