Search for Gravitational Waves from a Long-lived Remnant of the Binary Neutron Star Merger GW170817
- Creators
- Abbott, B. P.
- Abbott, R.
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Adhikari, R. X.
- Ananyeva, A.
- Anderson, S. B.
- Appert, S.
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Arai, K.
- Araya, M. C.
- Barayoga, J. C.
- Barish, B. C.
- Berger, B. K.
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Billingsley, G.
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Biscans, S
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Blackburn, J. K.
- Bork, R.
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Brooks, A. F.
- Brunett, S.
- Cahillane, C.
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Callister, T. A.
- Cepeda, C. B.
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Coughlin, M. W.
- Couvares, P.
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Coyne, D. C.
- Ehrens, P.
- Eichholz, J.
- Etzel, T.
- Feicht, J.
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Gossan, S. E.
- Gushwa, K. E.
- Gustafson, E. K.
- Heptonstall, A. W.
- Hulko, M.
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Isi, M.
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Kamai, B.
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Kanner, J. B.
- Kondrashov, V.
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Korth, W. Z.
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Kozak, D. B.
- Lazzarini, A.
- Markowitz, A.
- Maros, E.
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Massinger, T. J.
- Matichard, F.
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McIver, J.
- Meshkov, S.
- Nevin, L.
- Pedraza, M.
- Quintero, E. A.
- Reitze, D. H.
- Robertson, N. A.
- Rollins, J. G.
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Sachdev, S.
- Sanchez, E. J.
- Sanchez, L. E.
- Taylor, R.
- Torrie, C. I.
- Urban, A. L.
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Vajente, G.
- Vass, S.
- Venugopalan, G.
- Wade, A. R.
- Wallace, L.
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Weinstein, A. J.
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Williams, R. D.
- Willis, J. L.
- Wipf, C. C.
- Xiao, S.
- Yamamoto, H.
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Zhang, L.
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Zucker, M. E.
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Zweizig, J.
- Barkett, K.
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Blackman, J.
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Chen, Y.
- Chua, A. J. K.
- Li, X.
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Ma, Y.
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Pang, B.
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Scheel, M.
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Tso, R.
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Varma, V.
- LIGO Scientific Collaboration
- Virgo Collaboration
Abstract
One unanswered question about the binary neutron star coalescence GW170817 is the nature of its post-merger remnant. A previous search for post-merger gravitational waves targeted high-frequency signals from a possible neutron star remnant with a maximum signal duration of 500 s. Here, we revisit the neutron star remnant scenario and focus on longer signal durations, up until the end of the second Advanced LIGO-Virgo observing run, which was 8.5 days after the coalescence of GW170817. The main physical scenario for this emission is the power-law spindown of a massive magnetar-like remnant. We use four independent search algorithms with varying degrees of restrictiveness on the signal waveform and different ways of dealing with noise artefacts. In agreement with theoretical estimates, we find no significant signal candidates. Through simulated signals, we quantify that with the current detector sensitivity, nowhere in the studied parameter space are we sensitive to a signal from more than 1 Mpc away, compared to the actual distance of 40 Mpc. However, this study serves as a prototype for post-merger analyses in future observing runs with expected higher sensitivity.
Additional Information
© 2019 The American Astronomical Society. Received 2018 October 5; revised 2019 March 4; accepted 2019 March 8; published 2019 April 25. 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 and also 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 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'Educació Investigació Cultura i Esport de la Generalitat Valenciana, the National Science Centre of Poland, 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 Lyon Institute of Origins (LIO), the Paris Île-de-France Region, the National Research, Development and Innovation Office Hungary (NKFI), 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 (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 and the Kavli Foundation. The authors gratefully acknowledge the support of the NSF, STFC, MPS, INFN, CNRS and the State of Niedersachsen/Germany for provision of computational resources. This article has been assigned document number LIGO-P1800195.Attached Files
Published - Abbott_2019_ApJ_875_160.pdf
Submitted - 1810.02581.pdf
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Additional details
- Eprint ID
- 95004
- Resolver ID
- CaltechAUTHORS:20190426-072359239
- 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)
- Stichting voor Fundamenteel Onderzoek der Materie (FOM)
- 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'Educació i Universitat del Govern de les Illes Balears
- Conselleria d'Educació Investigació Cultura i Esport de la Generalitat Valenciana
- National Science Centre (Poland)
- 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)
- Paris Île-de-France Region
- National Research, Development and Innovation Fund (NKFIA)
- National Research Foundation of Korea
- Industry Canada
- Province of Ontario Ministry of Economic Development and Innovation
- Natural Science and Engineering Research Council of Canada (NSERC)
- Canadian Institute for Advanced Research (CIFAR)
- 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
- Ministry of Science and Technology (Taipei)
- Kavli Foundation
- Created
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2019-04-26Created from EPrint's datestamp field
- Updated
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2021-11-16Created from EPrint's last_modified field
- Caltech groups
- LIGO, Astronomy Department
- Other Numbering System Name
- LIGO Document
- Other Numbering System Identifier
- P1800195