Search for astrophysical tau neutrinos in three years of IceCube data. Calibration and characterization of the IceCube photomultiplier tube. The IceCube data acquisition system: signal capture, digitization, and timestamping. Energy reconstruction methods in the IceCube neutrino telescope. Event reconstruction in IceCube based on direct event re-simulation. The IceCube Neutrino Observatory: instrumentation and online systems. High-energy neutrinos from astrophysical sources: an upper bound. The acceleration of cosmic rays in shock fronts. Flavoring astrophysical neutrinos: flavor ratios depend on energy. Glashow resonance as a window into cosmic neutrino sources.
#ANTIMATTER PEPE UPDATE#
Update of a combined analysis of the high-energy cosmic neutrino flux at the IceCube detector. As such, knowledge of both the flavour (that is, electron, muon or tau neutrinos) and charge (neutrino or antineutrino) will facilitate the advancement of neutrino astronomy. Its unique signature indicates a method of distinguishing neutrinos from antineutrinos, thus providing a way to identify astronomical accelerators that produce neutrinos via hadronuclear or photohadronic interactions, with or without strong magnetic fields.
The evidence of the Glashow resonance suggests the presence of electron antineutrinos in the astrophysical flux, while also providing further validation of the standard model of particle physics. Features consistent with the production of secondary muons in the particle shower indicate the hadronic decay of a resonant W − boson, confirm that the source is astrophysical and provide improved directional localization. A shower with an energy of 6.05 ± 0.72 PeV (determined from Cherenkov radiation in the Antarctic Ice Sheet) was measured. Here we report the detection by the IceCube neutrino observatory of a cascade of high-energy particles (a particle shower) consistent with being created at the Glashow resonance. Whereas this energy scale is out of reach for currently operating and future planned particle accelerators, natural astrophysical phenomena are expected to produce antineutrinos with energies beyond the PeV scale. The Glashow resonance describes the resonant formation of a W − boson during the interaction of a high-energy electron antineutrino with an electron 1, peaking at an antineutrino energy of 6.3 petaelectronvolts (PeV) in the rest frame of the electron.