Optically targeted search for gravitational waves emitted by core-collapse supernovae during the first and second observing runs of advanced LIGO and advanced Virgo

(LIGO Scientific Collaboration and Virgo Collaboration)

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Abstract

We present the results from a search for gravitational-wave transients associated with core-collapse supernovae observed within a source distance of approximately 20 Mpc during the first and second observing runs of Advanced LIGO and Advanced Virgo. No significant gravitational-wave candidate was detected. We report the detection efficiencies as a function of the distance for waveforms derived from multidimensional numerical simulations and phenomenological extreme emission models. The sources with neutrino-driven explosions are detectable at the distances approaching 5 kpc, and for magnetorotationally driven explosions the distances are up to 54 kpc. However, waveforms for extreme emission models are detectable up to 28 Mpc. For the first time, the gravitational-wave data enabled us to exclude part of the parameter spaces of two extreme emission models with confidence up to 83%, limited by coincident data coverage. Besides, using ad hoc harmonic signals windowed with Gaussian envelopes, we constrained the gravitational-wave energy emitted during core collapse at the levels of 4.27×10-4 M·c2 and 1.28×10-1 M·c2 for emissions at 235 and 1304 Hz, respectively. These constraints are 2 orders of magnitude more stringent than previously derived in the corresponding analysis using initial LIGO, initial Virgo, and GEO 600 data.

Original languageEnglish
Article number084002
Pages (from-to)1-24
Number of pages24
JournalPhysical Review D
Volume101
Issue number8
Early online date2 Apr 2020
DOIs
Publication statusPublished - 15 Apr 2020

Funding

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, 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 European Gravitational Observatory 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, 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; the Russian Foundation for Basic Research; the Russian Science Foundation; the European Commission; the European Regional Development Funds; the Royal Society; the Scottish Funding Council; the Scottish Universities Physics Alliance; the Hungarian Scientific Research Fund; the Lyon Institute of Origins; the Paris Île-de-France Region; the National Research, Development and Innovation Office Hungary; 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; the Research Grants Council of Hong Kong; the National Natural Science Foundation of China; the Leverhulme Trust; the Research Corporation; the Ministry of Science and Technology, Taiwan; and the Kavli Foundation. The authors gratefully acknowledge the support of the NSF, STFC, INFN and CNRS for provision of computational resources. Research by D. J. S. is supported by NSF Grants No. AST-1821987, No. AST-1821967, No. AST-1813708, and No. AST-1813466. We thank the Las Cumbres Observatory and its staff for its continuing support of the ASAS-SN project. ASAS-SN is supported by the Gordon and Betty Moore Foundation through Grant No. GBMF5490 to the Ohio State University and NSF Grant No. AST-1515927. Development of ASAS-SN has been supported by NSF Grant No. AST-0908816, the Mt. Cuba Astronomical Foundation, the Center for Cosmology and AstroParticle Physics at the Ohio State University, the Chinese Academy of Sciences South America Center for Astronomy, the Villum Foundation, and George Skestos. K. Z. S. and C. S. K. are supported by NSF Grants No. AST-1515876, No. AST-1515927, and No. AST-1814440. Support for J. L. P. is provided in part by FONDECYT through Grant No. 1191038 and by the Ministry of Economy, Development, and Tourism’s Millennium Science Initiative through Grant No. IC120009, awarded to The Millennium Institute of Astrophysics, MAS. Research by S. V. is supported by NSF Grant No. AST-1813176. We are thankful to the National Science Foundation for support under Grant No. PHY 1806165. This document has been assigned LIGO Laboratory document number LIGO-P1700177.

FundersFunder number
Chinese Academy of Sciences South America Center for Astronomy
Netherlands Organisation for Scientific Research for the construction and operation of the Virgo detector
Paris Ile-de-France Region
Paris Île-de-France Region
Vicepresidencia i Conselleria d'Innovacio
National Science Foundation1813466, 0908816, 1515876, 1821987, 1515927, 1813176, 1821967, 1813708, 1814440
Gordon and Betty Moore FoundationGBMF5490
Kavli FoundationAST-1813466, AST-1821987, AST-1821967, AST-1813708
Ohio State UniversityAST-1515927, AST-0908816
Canadian Institute for Advanced Research
Villum FondenAST-1515876, AST-1814440
College of Natural Resources and Sciences, Humboldt State University
Mt. Cuba Astronomical Foundation
Institut des Origines de Lyon
Chinese Academy of Sciences South America Center for Astronomy
Natural Sciences and Engineering Research Council of Canada
Ontario Ministry of Economic Development and 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
Schweizerischer Nationalfonds zur Förderung der Wissenschaftlichen Forschung
National Natural Science Foundation of China
Science and Engineering Research Board
Russian Foundation for Basic Research
Fondo Nacional de Desarrollo Científico y Tecnológico1191038
Research Grants Council, University Grants Committee
Industry Canada
Generalitat Valenciana
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
Centre National de la Recherche Scientifique
Ministerio de Economía, Fomento y Turismo, ChileAST-1813176, PHY 1806165, IC120009
Russian Science Foundation
European Regional Development Fund
Universitat de les Illes Balears
Agencia Estatal de Investigación
Ministério da Ciência, Tecnologia, Inovações e Comunicações
Nemzeti Kutatási, Fejlesztési és Innovaciós Alap
Istituto Nazionale di Fisica Nucleare
ICTP South American Institute for Fundamental Research
National Research, Development and Innovation Office

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