Details
| Original language | English |
|---|---|
| Article number | 084002 |
| Number of pages | 24 |
| Journal | Physical Review D |
| Volume | 101 |
| Issue number | 8 |
| Publication status | Published - 2 Apr 2020 |
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.
ASJC Scopus subject areas
- Physics and Astronomy(all)
- Physics and Astronomy (miscellaneous)
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In: Physical Review D, Vol. 101, No. 8, 084002, 02.04.2020.
Research output: Contribution to journal › Article › Research › peer review
}
TY - JOUR
T1 - Optically targeted search for gravitational waves emitted by core-collapse supernovae during the first and second observing runs of advanced LIGO and advanced Virgo
AU - The LIGO Scientific Collaboration
AU - The Virgo Collaboration
AU - Abbott, B. P.
AU - Abbott, R.
AU - Abbott, T. D.
AU - Abraham, S.
AU - Acernese, F.
AU - Ackley, K.
AU - Adams, C.
AU - Adya, V. B.
AU - Affeldt, C.
AU - Agathos, M.
AU - Agatsuma, K.
AU - Aggarwal, N.
AU - Aguiar, O. D.
AU - Aiello, L.
AU - Ain, A.
AU - Ajith, P.
AU - Allen, G.
AU - Allocca, A.
AU - Aloy, M. A.
AU - Altin, P. A.
AU - Amato, A.
AU - Anand, S.
AU - Ananyeva, A.
AU - Anderson, S. B.
AU - Anderson, W. G.
AU - Angelova, S. V.
AU - Antier, S.
AU - Appert, S.
AU - Arai, K.
AU - Araya, M. C.
AU - Areeda, J. S.
AU - Arène, M.
AU - Arnaud, N.
AU - Aronson, S. M.
AU - Ascenzi, S.
AU - Ashton, G.
AU - Aston, S. M.
AU - Astone, P.
AU - Aubin, F.
AU - Aufmuth, P.
AU - Danilishin, S. L.
AU - Danzmann, K.
AU - Heurs, M.
AU - Lück, H.
AU - Steinmeyer, D.
AU - Vahlbruch, H.
AU - Wei, L.-w.
AU - Wilken, D. M.
AU - Willke, B.
AU - Wittel, H.
AU - Bose, Sukanta
AU - Brown, D. D.
AU - Chen, Y. B.
AU - Cheng, Hai-Ping
AU - Gniesmer, J.
AU - Hanke, Manuela
AU - Hennig, J.
AU - Hübner, M. T.
AU - Lang, R. N.
AU - Lee, C. H.
AU - Lee, H. K.
AU - Lee, H. W.
AU - Lee, J.
AU - Lee, K.
AU - Li, X.
AU - Rose, C. A.
AU - Rose, D.
AU - Sanders, J. R.
AU - Schmidt, Patricia
AU - Sun, L.
AU - Wang, Y. F.
AU - Wu, D. S.
AU - Zhang, L.
AU - Zhou, Minchuan
AU - Zhu, X. J.
AU - Bergmann, G.
AU - Bisht, Aparna
AU - Bode, Nina
AU - Booker, P.
AU - Brinkmann, Marc
AU - Cabero, M.
AU - de Varona, O.
AU - Hochheim, S.
AU - Junker, J.
AU - Kaufer, Stefan
AU - Khan, S.
AU - Kirchhoff, R.
AU - Koch, Patrick
AU - Koper, N.
AU - Köhlenbeck, S. M.
AU - Kringel, Volker
AU - Krämer, C.
AU - Kuehn, G.
AU - Leavey, S.
AU - Lehmann, J.
AU - Lough, James
AU - Mehmet, Moritz
AU - Meylahn, Fabian
AU - Mukund, Nikhil
AU - Rüdiger, A.
AU - Phelps, M.
AU - Ohme, F.
AU - Oppermann, P.
AU - Schulte, B. W.
AU - Schreiber, Emil
AU - Nery, M.
AU - Setyawati, Y.
AU - Standke, M.
AU - Steinke, M.
AU - Weinert, Michael
AU - Wellmann, F.
AU - Weßels, Peter
AU - Winkler, W.
AU - Woehler, J.
AU - Arunava Mukherjee, Mukherjee
N1 - Funding Information: 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.
PY - 2020/4/2
Y1 - 2020/4/2
N2 - 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.
AB - 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.
UR - http://www.scopus.com/inward/record.url?scp=85084593840&partnerID=8YFLogxK
U2 - 10.1103/PhysRevD.101.084002
DO - 10.1103/PhysRevD.101.084002
M3 - Article
VL - 101
JO - Physical Review D
JF - Physical Review D
SN - 2470-0010
IS - 8
M1 - 084002
ER -