Bounding the time delay between high-energy neutrinos and gravitational-wave transients from gamma-ray bursts |
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| Authors: | Bruny Baret Imre Bartos Boutayeb Bouhou Alessandra Corsi Irene Di Palma Corinne Donzaud Vronique Van Elewyck Chad Finley Gareth Jones Antoine Kouchner Szabolcs Mrka Zsuzsa Mrka Luciano Moscoso Eric Chassande-Mottin Maria Alessandra Papa Thierry Pradier Peter Raffai Jameson Rollins Patrick Sutton |
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| Institution: | a AstroParticule et Cosmologie (APC), CNRS: UMR7164-IN2P3-Observatoire de Paris-Université Denis Diderot-Paris VII-CEA: DSM/IRFU, France;b Department of Physics, Columbia University, New York, NY 10027, USA;c LIGO Laboratory, California Institute of Technology, Pasadena, CA 91125, USA;d Albert-Einstein-Institut, Max-Planck-Institut für Gravitationsphysik, D-30167 Hannover, Germany;e Université Paris-sud, Orsay F-91405, France;f Oskar Klein Centre & Department of Physics, Stockholm University, SE-10691 Stockholm, Sweden;g Cardiff University, Cardiff CF24 3AA, UK;h University of Strasbourg & Institut Pluridisciplinaire Hubert Curien, Strasbourg, France;i Eötvös University, ELTE 1053 Budapest, Hungary |
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| Abstract: | 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 T90’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 tHEN ? tGW ∈ ?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, tGW ? tGRB ≈ tHEN ? tGRB ∈ ?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. |
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| Keywords: | Gravitational wave High-energy neutrino Gamma-ray burst Multimessenger Time window |
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