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Bounding the time delay between high-energy neutrinos and gravitational-wave transients from gamma-ray bursts

Baret, Bruny and Bartos, Imre and Bouhou, Boutayeb and Corsi, Alessandra and Di Palma, Irene and Donzaud, Corinne and Van Elewyck, Véronique and Finley, Chad and Jones, Gareth and Kouchner, Antoine and Márka, Szabolcs and Márka, Zsuzsa and Moscoso, Luciano and Chassande-Mottin, Eric and Papa, Maria Alessandra and Pradier, Thierry and Raffai, Peter and Rollins, Jameson and Sutton, Patrick (2011) Bounding the time delay between high-energy neutrinos and gravitational-wave transients from gamma-ray bursts. Astroparticle Physics, 35 (1). pp. 1-7. ISSN 0927-6505.

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We derive a conservative coincidence time window for joint searches of gravitational-wave (GW) transients and high-energy neutrinos (HENs, with energies ≳100 GeV), emitted by gamma-ray bursts (GRBs). The last are among the most interesting astrophysical sources for coincident detections with current and near-future detectors. We take into account a broad range of emission mechanisms. We take the upper limit of GRB durations as the 95% quantile of the T_(90’)s of GRBs observed by BATSE, obtaining a GRB duration upper limit of ∼150 s. Using published results on high-energy (>100 MeV) photon light curves for 8 GRBs detected by Fermi LAT, we verify that most high-energy photons are expected to be observed within the first ∼150 s of the GRB. Taking into account the breakout-time of the relativistic jet produced by the central engine, we allow GW and HEN emission to begin up to 100 s before the onset of observable gamma photon production. Using published precursor time differences, we calculate a time upper bound for precursor activity, obtaining that 95% of precursors occur within ∼250 s prior to the onset of the GRB. Taking the above different processes into account, we arrive at a time window of t_(HEN) − t_(GW) ∈ [−500 s, +500 s]. Considering the above processes, an upper bound can also be determined for the expected time window of GW and/or HEN signals coincident with a detected GRB, t_(GW) − t_(GRB) ≈ t_(HEN) − t_(GRB) ∈ [−350 s, +150 s]. These upper bounds can be used to limit the coincidence time window in multimessenger searches, as well as aiding the interpretation of the times of arrival of measured signals.

Item Type:Article
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URLURL TypeDescription DOIArticle
Bartos, Imre0000-0001-5607-3637
Corsi, Alessandra0000-0001-8104-3536
Additional Information:© 2011 Elsevier B.V. Received 18 January 2011. Received in revised form 23 March 2011. Accepted 8 April 2011. Available online 19 April 2011. The authors are grateful to John Cannizzo, Peter Mészáros, Christian Ott, Tsvi Piran, Richard O’Shaughnessy and Eli Waxman for the helpful discussions and valuable comments. We are grateful for the generous support of Columbia University in the City of New York and the National Science Foundation under cooperative agreements PHY-0847182. The authors are grateful for support from the Swedish Research Council (VR) through the Oskar Klein Centre. The authors acknowledge financial support from the French Agence Nationale de la Recherche (contract ANR-08-JCJC-0061-01) and from the EU FP7 (Marie Curie Reintegration Grant). The authors gratefully acknowledge the support of the United States National Science Foundation for the construction and operation of the LIGO Laboratory and 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. The authors also gratefully acknowledge the support of the research by these agencies and by the Australian Research Council, the Council of Scientific and Industrial Research of India, the Istituto Nazionale di Fisica Nucleare of Italy, the Spanish Ministerio de Educación y Ciencia, the Conselleria d’Economia, Hisenda i Innovació of the Govern de les Illes Balears, 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, and the French Centre National de la Recherche Scientifique.
Funding AgencyGrant Number
Columbia UniversityUNSPECIFIED
Swedish Research CouncilUNSPECIFIED
Agence Nationale pour la Recherche (ANR)ANR-08-JCJC-0061-01
Marie Curie FellowshipUNSPECIFIED
Science and Technology Facilities Council (STFC)UNSPECIFIED
Max Planck SocietyUNSPECIFIED
State of Niedersachsen/GermanyUNSPECIFIED
Australian Research CouncilUNSPECIFIED
Council of Scientific and Industrial Research (India)UNSPECIFIED
Istituto Nazionale di Fisica Nucleare (INFN)UNSPECIFIED
Ministerio de Educaciόn y Ciencia (MEC)UNSPECIFIED
Conselleria d'Economia Hisenda i Innovacio of the Govern de les Illes BalearsUNSPECIFIED
Scottish Funding CouncilUNSPECIFIED
Scottish Universities Physics AllianceUNSPECIFIED
Leverhulme TrustUNSPECIFIED
David and Lucile Packard FoundationUNSPECIFIED
Research CorporationUNSPECIFIED
Alfred P. Sloan FoundationUNSPECIFIED
Centre National de la Recherche Scientifique (CNRS)UNSPECIFIED
Subject Keywords:Gravitational wave; High-energy neutrino; Gamma-ray burst; Multimessenger; Time window
Issue or Number:1
Record Number:CaltechAUTHORS:20111107-080520353
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Official Citation:Bruny Baret, Imre Bartos, Boutayeb Bouhou, Alessandra Corsi, Irene Di Palma, Corinne Donzaud, Véronique Van Elewyck, Chad Finley, Gareth Jones, Antoine Kouchner, Szabolcs Márka, Zsuzsa Márka, Luciano Moscoso, Eric Chassande-Mottin, Maria Alessandra Papa, Thierry Pradier, Peter Raffai, Jameson Rollins, Patrick Sutton, Bounding the time delay between high-energy neutrinos and gravitational-wave transients from gamma-ray bursts, Astroparticle Physics, Volume 35, Issue 1, August 2011, Pages 1-7, ISSN 0927-6505, 10.1016/j.astropartphys.2011.04.001. (
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:27638
Deposited By: Ruth Sustaita
Deposited On:07 Nov 2011 16:41
Last Modified:09 Mar 2020 13:18

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