Aartsen MG Ackermann M Adams J Aguilar JA Ahlers M Ahrens M Al Samarai I Altmann D Andeen K Anderson T Ansseau I Anton G Argüelles C Auffenberg J Axani S Backes P Bagherpour H Bai X Barbano A Barron JP Barwick SW Baum V Bay R Beatty JJ Becker Tjus J Becker KH BenZvi S Berley D Bernardini E Besson DZ Binder G Bindig D Blaufuss E Blot S Bohm C Börner M Bos F Böser S Botner O Bourbeau E Bourbeau J Bradascio F Braun J Brenzke M Bretz HP Bron S Brostean-Kaiser J Burgman A Busse RS Carver T Cheung E Chirkin D Christov A Clark K Classen L Collin GH Conrad JM Coppin P Correa P Cowen DF Cross R Dave P Day M de André JPAM De Clercq C DeLaunay JJ Dembinski H Deoskar K De Ridder S Desiati P de Vries KD de Wasseige G de With M DeYoung T Díaz-Vélez JC di Lorenzo V Dujmovic H Dumm JP Dunkman M Dvorak E Eberhardt B Ehrhardt T Eichmann B Eller P Evans PA Evenson PA Fahey S Fazely AR Felde J Filimonov K Finley C Franckowiak A Friedman E Fritz A Gaisser TK Gallagher J Ganster E Gerhardt L Ghorbani K Giang W Glauch T Glüsenkamp T Goldschmidt A Gonzalez JG Grant D Griffith Z Haack C Hallgren A Halve L Halzen F Hanson K Hebecker D Heereman D Helbing K Hellauer R Hickford S Hignight J Hill GC Hoffman KD Hoffmann R Hoinka T Hokanson-Fasig B Hoshina K Huang F Huber M Hultqvist K Hünnefeld M Hussain R In S Iovine N Ishihara A Jacobi E Japaridze GS Jeong M Jero K Jones BJP Kalaczynski P Kang W Kappes A Kappesser D Karg T Karle A Katz U Kauer M Keivani A Kelley JL Kheirandish A Kim J Kintscher T Kiryluk J Kittler T Klein SR Koirala R Kolanoski H Köpke L Kopper C Kopper S Koschinsky JP Koskinen DJ Kowalski M Krings K Kroll M Krückl G Kunwar S Kurahashi N Kyriacou A Labare M Lanfranchi JL Larson MJ Lauber F Leonard K Leuermann M Liu QR Lohfink E Lozano Mariscal CJ Lu L Lünemann J Luszczak W Madsen J Maggi G Mahn KBM Makino Y Mancina S Mariş IC Maruyama R Mase K Maunu R Meagher K Medici M Meier M Menne T Merino G Meures T Miarecki S Micallef J Momenté G Montaruli T Moore RW Moulai M Nagai R Nahnhauer R Nakarmi P Naumann U Neer G Niederhausen H Nowicki SC Nygren DR Obertacke Pollmann A Olivas A O'Murchadha A Osborne JP O'Sullivan E Palczewski T Pandya H Pankova DV Peiffer P Pepper JA Pérez de Los Heros C Pieloth D Pinat E Pizzuto A Plum M Price PB Przybylski GT Raab C Rameez M Rauch L Rawlins K Rea IC Reimann R Relethford B Renzi G Resconi E Rhode W Richman M Robertson S Rongen M Rott C Ruhe T Ryckbosch D Rysewyk D Safa I Sanchez Herrera SE Sandrock A Sandroos J Santander M Sarkar S Sarkar S Satalecka K Schaufel M Schlunder P Schmidt T Schneider A Schneider J Schöneberg S Schumacher L Sclafani S Seckel D Seunarine S Soedingrekso J Soldin D Song M Spiczak GM Spiering C Stachurska J Stamatikos M Stanev T Stasik A Stein R Stettner J Steuer A Stezelberger T Stokstad RG Stößl A Strotjohann NL Stuttard T Sullivan GW Sutherland M Taboada I Tenholt F Ter-Antonyan S Terliuk A Tilav S Toale PA Tobin MN Tönnis C Toscano S Tosi D Tselengidou M Tung CF Turcati A Turley CF Ty B Unger E Unland Elorrieta MA Usner M Vandenbroucke J Van Driessche W van Eijk D van Eijndhoven N Vanheule S van Santen J Vraeghe M Walck C Wallace A Wallraff M Wandler FD Wandkowsky N Watson TB Waza A Weaver C Weiss MJ Wendt C Werthebach J Westerhoff S Whelan BJ Whitehorn N Wiebe K Wiebusch CH Wille L Williams DR Wills L Wolf M Wood J Wood TR Woolsey E Woschnagg K Wrede G Xu DL Xu XW Xu Y Yanez JP Yodh G Yoshida S Yuan T 2019 High-energy neutrino emission has been predicted for several short-lived astrophysical transients including gamma-ray bursts (GRBs), core-collapse supernovae with choked jets, and neutron star mergers. IceCube's optical and x-ray follow-up program searches for such transient sources by looking for two or more muon neutrino candidates in directional coincidence and arriving within 100 s. The measured rate of neutrino alerts is consistent with the expected rate of chance coincidences of atmospheric background events and no likely electromagnetic counterparts have been identified in Swift follow-up observations. Here, we calculate generic bounds on the neutrino flux of short-lived transient sources. Assuming an E^{-2.5} neutrino spectrum, we find that the neutrino flux of rare sources, like long gamma-ray bursts, is constrained to <5% of the detected astrophysical flux and the energy released in neutrinos (100 GeV to 10 PeV) by a median bright GRB-like source is <10^{52.5}  erg. For a harder E^{-2.13} neutrino spectrum up to 30% of the flux could be produced by GRBs and the allowed median source energy is <10^{52}  erg. A hypothetical population of transient sources has to be more common than 10^{-5}  Mpc^{-3}  yr^{-1} (5×10^{-8}  Mpc^{-3}  yr^{-1} for the E^{-2.13} spectrum) to account for the complete astrophysical neutrino flux. application/pdf https://sonar.ch/global/documents/70123 eng info:eu-repo/semantics/altIdentifier/doi/10.1103/PhysRevLett.122.051102 info:eu-repo/semantics/altIdentifier/pmid/30822017 info:eu-repo/semantics/openAccess Physical review letters. - 2019 General Physics and Astronomy Constraints on Minute-Scale Transient Astrophysical Neutrino Sources. http://purl.org/coar/resource_type/c_6501