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Published July 4, 2014 | Published + Submitted + Supplemental Material
Journal Article Open

Search for Gravitational Waves Associated with γ-ray Bursts Detected by the Interplanetary Network


We present the results of a search for gravitational waves associated with 223 γ-ray bursts (GRBs) detected by the InterPlanetary Network (IPN) in 2005–2010 during LIGO's fifth and sixth science runs and Virgo's first, second, and third science runs. The IPN satellites provide accurate times of the bursts and sky localizations that vary significantly from degree scale to hundreds of square degrees. We search for both a well-modeled binary coalescence signal, the favored progenitor model for short GRBs, and for generic, unmodeled gravitational wave bursts. Both searches use the event time and sky localization to improve the gravitational wave search sensitivity as compared to corresponding all-time, all-sky searches. We find no evidence of a gravitational wave signal associated with any of the IPN GRBs in the sample, nor do we find evidence for a population of weak gravitational wave signals associated with the GRBs. For all IPN-detected GRBs, for which a sufficient duration of quality gravitational wave data are available, we place lower bounds on the distance to the source in accordance with an optimistic assumption of gravitational wave emission energy of 10^(−2)M⊙c^2 at 150 Hz, and find a median of 13 Mpc. For the 27 short-hard GRBs we place 90% confidence exclusion distances to two source models: a binary neutron star coalescence, with a median distance of 12 Mpc, or the coalescence of a neutron star and black hole, with a median distance of 22 Mpc. Finally, we combine this search with previously published results to provide a population statement for GRB searches in first-generation LIGO and Virgo gravitational wave detectors and a resulting examination of prospects for the advanced gravitational wave detectors.

Additional Information

© 2014 American Physical Society. Received 7 April 2014; Published 30 June 2014. The authors gratefully acknowledge the support of the United States National Science Foundation for the construction and operation of the LIGO Laboratory, the Science and Technology Facilities Council of the United Kingdom, the Max Planck Society, and the State of Niedersachsen, Germany, for support of the construction and operation of the GEO600 detector and the Italian Istituto Nazionale di Fisica Nucleare and the French Centre National de la Recherche Scientifique for the construction and operation of the Virgo detector. The authors also gratefully acknowledge the support of the research by these agencies and by the Australian Research Council, the International Science Linkages program of the Commonwealth of Australia, the Council of Scientific and Industrial Research of India, the Istituto Nazionale di Fisica Nucleare of Italy, the Spanish Ministerio de Economía y Competitividad, the Conselleria d'Economia Hisenda i Innovació of the Govern de les Illes Balears, the Foundation for Fundamental Research on Matter supported by the Netherlands Organisation for Scientific Research, the Polish Ministry of Science and Higher Education, the FOCUS Programme of Foundation for Polish Science, the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, The National Aeronautics and Space Administration, the Carnegie Trust, the Leverhulme Trust, the David and Lucile Packard Foundation, the Research Corporation, and the Alfred P. Sloan Foundation. K. H. acknowledges IPN support from the following sources: NASA NNX06AI36G, NNX08AB84G, NNX08AZ85G, NNX09AV61G, and NNX10AR12G (Suzaku), NASA NNG06GI89G, NNX07AJ65G, NNX08AN23G, NNX09AO97G, NNX10AI23G (Swift), NASA NNG06GE69G, NNX07AQ22G, NNX08AC90G, NNX08AX95G, NNX09AR28G (INTEGRAL). TheKonus-Wind experiment is partially supported by a Russian Space Agency contract and RFBRGrantsNo. 12-02-00032-a and No. 13-02-12017-ofi_m. This document has been assigned LIGO Laboratory document number LIGO-P1300226-v10.

Attached Files

Submitted - 1403.6639v2.pdf

Published - PhysRevLett.113.011102.pdf

Supplemental Material - Supplementarymaterial_LR14000Aasi.pdf

Supplemental Material - Supplementarymaterial_LR14000Aasi.tex


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August 20, 2023
August 20, 2023