Searches for Neutrinos from Gamma-Ray Bursts using the IceCube Neutrino Observatory

IceCube Collaboration

doi:10.3847/1538-4357/ac9785

Searches for Neutrinos from Gamma-Ray Bursts using the IceCube Neutrino Observatory

IceCube Collaboration

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Abstract

Gamma-ray bursts (GRBs) are considered as promising sources of ultra-high-energy cosmic rays (UHECRs) due to their large power output. Observing a neutrino flux from GRBs would offer evidence that GRBs are hadronic accelerators of UHECRs. Previous IceCube analyses, which primarily focused on neutrinos arriving in temporal coincidence with the prompt gamma-rays, found no significant neutrino excess. The four analyses presented in this paper extend the region of interest to 14 days before and after the prompt phase, including generic extended time windows and targeted precursor searches. GRBs were selected between 2011 May and 2018 October to align with the data set of candidate muon-neutrino events observed by IceCube. No evidence of correlation between neutrino events and GRBs was found in these analyses. Limits are set to constrain the contribution of the cosmic GRB population to the diffuse astrophysical neutrino flux observed by IceCube. Prompt neutrino emission from GRBs is limited to 21% of the observed diffuse neutrino flux, and emission on timescales up to 104 s is constrained to 24% of the total diffuse flux.

Original language	English
Article number	116
Number of pages	17
Journal	The Astrophysical Journal
Volume	939
Issue number	2
DOIs	https://doi.org/10.3847/1538-4357/ac9785
Publication status	Published - 14 Nov 2022

Bibliographical note

Funding Information:
The IceCube Collaboration acknowledges the significant contribution to this manuscript from Paul Coppin, Kunal Deoskar and Elizabeth Friedman. The authors thank Adam Goldstein for providing GBM maps prior to 2018 and gratefully acknowledge NASA funding for this work through contract NNM13AA43C. J.W. gratefully acknowledges NASA funding through the Fermi-GBM project. The authors gratefully acknowledge the support from the following agencies and institutions: USA—U.S. National Science Foundation-Office of Polar Programs, U.S. National Science Foundation-Physics Division, U.S. National Science Foundation-EPSCoR, Wisconsin Alumni Research Foundation, Center for High Throughput Computing (CHTC) at the University of Wisconsin—Madison, Open Science Grid (OSG), Extreme Science and Engineering Discovery Environment (XSEDE), Frontera computing project at the Texas Advanced Computing Center, U.S. Department of Energy-National Energy Research Scientific Computing Center, Particle astrophysics research computing center at the University of Maryland, Institute for Cyber-Enabled Research at Michigan State University, and Astroparticle Physics computational facility at Marquette University; Belgium—Funds for Scientific Research (FRS-FNRS and FWO), FWO Odysseus and Big Science programmes, and Belgian Federal Science Policy Office (Belspo); Germany—Bundesministerium für Bildung und Forschung (BMBF), Deutsche Forschungsgemeinschaft (DFG), Helmholtz Alliance for Astroparticle Physics (HAP), Initiative and Networking Fund of the Helmholtz Association, Deutsches Elektronen Synchrotron (DESY), and High Performance Computing cluster of the RWTH Aachen; Sweden—Swedish Research Council, Swedish Polar Research Secretariat, Swedish National Infrastructure for Computing (SNIC), and Knut and Alice Wallenberg Foundation; Australia—Australian Research Council; Canada—Natural Sciences and Engineering Research Council of Canada, Calcul Québec, Compute Ontario, Canada Foundation for Innovation, WestGrid, and Compute Canada; Denmark—Villum Fonden and Carlsberg Foundation; New Zealand—Marsden Fund; Japan—Japan Society for Promotion of Science (JSPS) and Institute for Global Prominent Research (IGPR) of Chiba University; Korea—National Research Foundation of Korea (NRF); Switzerland—Swiss National Science Foundation (SNSF); United Kingdom—Department of Physics, University of Oxford.

Publisher Copyright:
© 2022. The Author(s). Published by the American Astronomical Society.

Copyright:
Copyright 2022 Elsevier B.V., All rights reserved.

Keywords

astro-ph.HE

Access to Document

10.3847/1538-4357/ac9785Licence: CC BY

Abbasi_2022_ApJ_939_116Final published version, 1.74 MBLicence: CC BY

Cite this

@article{ba30bb2bdf8846f5aabe45124e94e616,

title = "Searches for Neutrinos from Gamma-Ray Bursts using the IceCube Neutrino Observatory",

abstract = "Gamma-ray bursts (GRBs) are considered as promising sources of ultra-high-energy cosmic rays (UHECRs) due to their large power output. Observing a neutrino flux from GRBs would offer evidence that GRBs are hadronic accelerators of UHECRs. Previous IceCube analyses, which primarily focused on neutrinos arriving in temporal coincidence with the prompt gamma-rays, found no significant neutrino excess. The four analyses presented in this paper extend the region of interest to 14 days before and after the prompt phase, including generic extended time windows and targeted precursor searches. GRBs were selected between 2011 May and 2018 October to align with the data set of candidate muon-neutrino events observed by IceCube. No evidence of correlation between neutrino events and GRBs was found in these analyses. Limits are set to constrain the contribution of the cosmic GRB population to the diffuse astrophysical neutrino flux observed by IceCube. Prompt neutrino emission from GRBs is limited to 21% of the observed diffuse neutrino flux, and emission on timescales up to 104 s is constrained to 24% of the total diffuse flux.",

keywords = "astro-ph.HE",

author = "{IceCube Collaboration} and Paul Coppin and {Correa Camiroaga}, Pablo and {De Vries}, Krijn and {De Clercq}, Catherine and Yarno Merckx and {Van Eijndhoven}, Nicolaas",

note = "Funding Information: The IceCube Collaboration acknowledges the significant contribution to this manuscript from Paul Coppin, Kunal Deoskar and Elizabeth Friedman. The authors thank Adam Goldstein for providing GBM maps prior to 2018 and gratefully acknowledge NASA funding for this work through contract NNM13AA43C. J.W. gratefully acknowledges NASA funding through the Fermi-GBM project. The authors gratefully acknowledge the support from the following agencies and institutions: USA—U.S. National Science Foundation-Office of Polar Programs, U.S. National Science Foundation-Physics Division, U.S. National Science Foundation-EPSCoR, Wisconsin Alumni Research Foundation, Center for High Throughput Computing (CHTC) at the University of Wisconsin—Madison, Open Science Grid (OSG), Extreme Science and Engineering Discovery Environment (XSEDE), Frontera computing project at the Texas Advanced Computing Center, U.S. Department of Energy-National Energy Research Scientific Computing Center, Particle astrophysics research computing center at the University of Maryland, Institute for Cyber-Enabled Research at Michigan State University, and Astroparticle Physics computational facility at Marquette University; Belgium—Funds for Scientific Research (FRS-FNRS and FWO), FWO Odysseus and Big Science programmes, and Belgian Federal Science Policy Office (Belspo); Germany—Bundesministerium f{\"u}r Bildung und Forschung (BMBF), Deutsche Forschungsgemeinschaft (DFG), Helmholtz Alliance for Astroparticle Physics (HAP), Initiative and Networking Fund of the Helmholtz Association, Deutsches Elektronen Synchrotron (DESY), and High Performance Computing cluster of the RWTH Aachen; Sweden—Swedish Research Council, Swedish Polar Research Secretariat, Swedish National Infrastructure for Computing (SNIC), and Knut and Alice Wallenberg Foundation; Australia—Australian Research Council; Canada—Natural Sciences and Engineering Research Council of Canada, Calcul Qu{\'e}bec, Compute Ontario, Canada Foundation for Innovation, WestGrid, and Compute Canada; Denmark—Villum Fonden and Carlsberg Foundation; New Zealand—Marsden Fund; Japan—Japan Society for Promotion of Science (JSPS) and Institute for Global Prominent Research (IGPR) of Chiba University; Korea—National Research Foundation of Korea (NRF); Switzerland—Swiss National Science Foundation (SNSF); United Kingdom—Department of Physics, University of Oxford. Publisher Copyright: {\textcopyright} 2022. The Author(s). Published by the American Astronomical Society. Copyright: Copyright 2022 Elsevier B.V., All rights reserved.",

year = "2022",

month = nov,

day = "14",

doi = "10.3847/1538-4357/ac9785",

language = "English",

volume = "939",

journal = "The Astrophysical Journal",

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AU - IceCube Collaboration

AU - Coppin, Paul

AU - Correa Camiroaga, Pablo

AU - De Vries, Krijn

AU - De Clercq, Catherine

AU - Merckx, Yarno

AU - Van Eijndhoven, Nicolaas

N1 - Funding Information: The IceCube Collaboration acknowledges the significant contribution to this manuscript from Paul Coppin, Kunal Deoskar and Elizabeth Friedman. The authors thank Adam Goldstein for providing GBM maps prior to 2018 and gratefully acknowledge NASA funding for this work through contract NNM13AA43C. J.W. gratefully acknowledges NASA funding through the Fermi-GBM project. The authors gratefully acknowledge the support from the following agencies and institutions: USA—U.S. National Science Foundation-Office of Polar Programs, U.S. National Science Foundation-Physics Division, U.S. National Science Foundation-EPSCoR, Wisconsin Alumni Research Foundation, Center for High Throughput Computing (CHTC) at the University of Wisconsin—Madison, Open Science Grid (OSG), Extreme Science and Engineering Discovery Environment (XSEDE), Frontera computing project at the Texas Advanced Computing Center, U.S. Department of Energy-National Energy Research Scientific Computing Center, Particle astrophysics research computing center at the University of Maryland, Institute for Cyber-Enabled Research at Michigan State University, and Astroparticle Physics computational facility at Marquette University; Belgium—Funds for Scientific Research (FRS-FNRS and FWO), FWO Odysseus and Big Science programmes, and Belgian Federal Science Policy Office (Belspo); Germany—Bundesministerium für Bildung und Forschung (BMBF), Deutsche Forschungsgemeinschaft (DFG), Helmholtz Alliance for Astroparticle Physics (HAP), Initiative and Networking Fund of the Helmholtz Association, Deutsches Elektronen Synchrotron (DESY), and High Performance Computing cluster of the RWTH Aachen; Sweden—Swedish Research Council, Swedish Polar Research Secretariat, Swedish National Infrastructure for Computing (SNIC), and Knut and Alice Wallenberg Foundation; Australia—Australian Research Council; Canada—Natural Sciences and Engineering Research Council of Canada, Calcul Québec, Compute Ontario, Canada Foundation for Innovation, WestGrid, and Compute Canada; Denmark—Villum Fonden and Carlsberg Foundation; New Zealand—Marsden Fund; Japan—Japan Society for Promotion of Science (JSPS) and Institute for Global Prominent Research (IGPR) of Chiba University; Korea—National Research Foundation of Korea (NRF); Switzerland—Swiss National Science Foundation (SNSF); United Kingdom—Department of Physics, University of Oxford. Publisher Copyright: © 2022. The Author(s). Published by the American Astronomical Society. Copyright: Copyright 2022 Elsevier B.V., All rights reserved.

PY - 2022/11/14

Y1 - 2022/11/14

N2 - Gamma-ray bursts (GRBs) are considered as promising sources of ultra-high-energy cosmic rays (UHECRs) due to their large power output. Observing a neutrino flux from GRBs would offer evidence that GRBs are hadronic accelerators of UHECRs. Previous IceCube analyses, which primarily focused on neutrinos arriving in temporal coincidence with the prompt gamma-rays, found no significant neutrino excess. The four analyses presented in this paper extend the region of interest to 14 days before and after the prompt phase, including generic extended time windows and targeted precursor searches. GRBs were selected between 2011 May and 2018 October to align with the data set of candidate muon-neutrino events observed by IceCube. No evidence of correlation between neutrino events and GRBs was found in these analyses. Limits are set to constrain the contribution of the cosmic GRB population to the diffuse astrophysical neutrino flux observed by IceCube. Prompt neutrino emission from GRBs is limited to 21% of the observed diffuse neutrino flux, and emission on timescales up to 104 s is constrained to 24% of the total diffuse flux.

AB - Gamma-ray bursts (GRBs) are considered as promising sources of ultra-high-energy cosmic rays (UHECRs) due to their large power output. Observing a neutrino flux from GRBs would offer evidence that GRBs are hadronic accelerators of UHECRs. Previous IceCube analyses, which primarily focused on neutrinos arriving in temporal coincidence with the prompt gamma-rays, found no significant neutrino excess. The four analyses presented in this paper extend the region of interest to 14 days before and after the prompt phase, including generic extended time windows and targeted precursor searches. GRBs were selected between 2011 May and 2018 October to align with the data set of candidate muon-neutrino events observed by IceCube. No evidence of correlation between neutrino events and GRBs was found in these analyses. Limits are set to constrain the contribution of the cosmic GRB population to the diffuse astrophysical neutrino flux observed by IceCube. Prompt neutrino emission from GRBs is limited to 21% of the observed diffuse neutrino flux, and emission on timescales up to 104 s is constrained to 24% of the total diffuse flux.

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DO - 10.3847/1538-4357/ac9785

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SN - 0004-637X

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ER -

Searches for Neutrinos from Gamma-Ray Bursts using the IceCube Neutrino Observatory

Abstract

Bibliographical note

Keywords

Access to Document

Other files and links

Fingerprint

FWOIRI11: Exploring the Extreme Universe with the (Extended) IceCube Neutrino and Cosmic Ray Observatory at the South Pole

SRP72: SRP-Onderzoekszwaartepunt: High-energy physics (HEP@VUB).

FWOTM1076: IceCube Search for High-Energy Neutrinos from Obscured Sources in the Great Observatories All-Sky LIRG Survey (GOALS)

Cite this

Searches for Neutrinos from Gamma-Ray Bursts using the IceCube Neutrino Observatory

Abstract

Bibliographical note

Keywords

Access to Document

Other files and links

Fingerprint

Projects

FWOIRI11: Exploring the Extreme Universe with the (Extended) IceCube Neutrino and Cosmic Ray Observatory at the South Pole

SRP72: SRP-Onderzoekszwaartepunt: High-energy physics (HEP@VUB).

FWOTM1076: IceCube Search for High-Energy Neutrinos from Obscured Sources in the Great Observatories All-Sky LIRG Survey (GOALS)

Cite this