RT Journal Article
T1 Very high-energy gamma-ray follow-up program using neutrino triggers from IceCube
A1 Barrio Uña, Juan Abel
A1 Bonnefoy, Simon Francois Albert
A1 Contreras González, José Luis
A1 Domínguez, A.
A1 Fidalgo, D.
A1 Fonseca González, María Victoria
A1 López, M.
A1 Nievas Rosillo, Mireia
AB We describe and report the status of a neutrino-triggered program in IceCube that generates real-time alerts for gamma-ray follow-up observations by atmospheric-Cherenkov telescopes (MAGIC and VERITAS). While IceCube is capable of monitoring the whole sky continuously, high-energy gamma-ray telescopes have restricted fields of view and in general are unlikely to be observing a potential neutrino-flaring source at the time such neutrinos are recorded. The use of neutrino-triggered alerts thus aims at increasing the availability of simultaneous multi-messenger data during potential neutrino flaring activity, which can increase the discovery potential and constrain the phenomenological interpretation of the high-energy emission of selected source classes (e. g. blazars). The requirements of a fast and stable online analysis of potential neutrino signals and its operation are presented, along with first results of the program operating between 14 March 2012 and 31 December 2015.
PB IOP Publishing LTD
SN 1748-0221
YR 2016
FD 2016-11
LK https://hdl.handle.net/20.500.14352/17915
UL https://hdl.handle.net/20.500.14352/17915
LA eng
NO © 2016 IOP Publishing Ltd and Sissa Medialab srl Artículo firmado por más de 10 autoresWe acknowledge the support from the following agencies: U.S. National Science Foundation-Office of Polar Programs, U.S. National Science Foundation-Physics Division, University of Wisconsin Alumni Research Foundation, the Grid Laboratory Of Wisconsin (GLOW) grid infrastructure at the University of Wisconsin - Madison, the Open Science Grid (OSG) grid infrastructure; U.S. Department of Energy, and National Energy Research Scientific Computing Center, the Louisiana Optical Network Initiative (LONI) grid computing resources; Natural Sciences and Engineering Research Council of Canada, WestGrid and Compute/Calcul Canada; Swedish Research Council, Swedish Polar Research Secretariat, Swedish National Infrastructure for Computing (SNIC), and Knut and Alice Wallenberg Foundation, Sweden; German Ministry for Education and Research (BMBF), Deutsche Forschungsgemeinschaft (DFG), Helmholtz Alliance for Astroparticle Physics (HAP), Research Department of Plasmas with Complex Interactions (Bochum), Germany; Fund for Scientific Research (FNRS-FWO), FWO Odysseus programme, Flanders Institute to encourage scientific and technological research in industry (IWT), Belgian Federal Science Policy Office (Belspo); University of Oxford, United Kingdom; Marsden Fund, NewZealand; Australian Research Council; Japan Society for Promotion of Science (JSPS); the Swiss National Science Foundation (SNSF), Switzerland; National Research Foundation of Korea (NRF); Villum Fonden, Danish National Research Foundation (DNRF), Denmark.; The VERITAS Collaboration acknowledges the support of the U.S. Department of Energy Office of Science, the U.S. National Science Foundation and the Smithsonian Institution, and NSERC in Canada. We also acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instrument.; The MAGIC collaboration would like to thank the Instituto de Astrofisica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The financial support of the German BMBF and MPG, the Italian INFN and INAF, the Swiss National Fund SNF, the he ERDF under the Spanish MINECO (FPA2015-69818-P, FPA2012-36668, FPA2015-68278-P, FPA2015-69210-C6-2-R, FPA2015-69210-C6-4-R, FPA2015-69210-C6-6-R, AYA2013-47447-C3-1-P, AYA2015-71042-P, ESP2015-71662-C2-2-P, CSD2009-00064), and the Japanese JSPS and MEXT is gratefully acknowledged. This work was also supported by the Spanish Centro de Excelencia "Severo Ochoa" SEV-2012-0234 and SEV-2015-0548, and Unidad de Excelencia "Maria de Maeztu" MDM-2014-0369, by grant 268740 of the Academy of Finland, by the Croatian Science Foundation (HrZZ) Project 09/176 and the University of Rijeka Project 13.12.1.3.02, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, and by the Polish MNiSzW grant 745/N-HESS-MAGIC/2010/0.
NO Ministerio de Economía y Competitividad (MINECO)
NO Swedish Research Council
NO Swedish Polar Research Secretariat
NO Swedish National Infrastructure for Computing (SNIC)
NO Knut and Alice Wallenberg Foundation, Sweden
NO German Ministry for Education and Research (BMBF)
NO Deutsche Forschungsgemeinschaft (DFG)
NO Helmholtz Alliance for Astroparticle Physics (HAP)
NO Research Department of Plasmas with Complex Interactions (Bochum), Germany
NO Fund for Scientific Research (FNRS-FWO)
NO FWO Odysseus programme
NO Flanders Institute to encourage scientific and technological research in industry (IWT)
NO Belgian Federal Science Policy Office (Belspo)
NO University of Oxford, United Kingdom
NO Swiss National Science Foundation (SNSF), Switzerland
NO Villum Fonden, Danish National Research Foundation (DNRF), Denmark
NO German BMBF and MPG
NO Italian INFN and INAF
NO Spanish Centro de Excelencia "Severo Ochoa"
NO Unidad de Excelencia "Maria de Maeztu"
NO Academy of Finland
NO Croatian Science Foundation (HrZZ) Project
NO University of Rijeka Project
NO DFG Collaborative Research Centers
NO Polish MNiSzW
DS Docta Complutense
RD 29 abr 2025