0000000000523067

AUTHOR

Timothy W. Schmidt

showing 3 related works from this author

Physics results from the Amanda neutrino detector

2001

In the winter season of 2000, the AMANDA (Antarctic Muon And Neutrino Detector Array) detector was completed to its final state. We report on major physics results obtained from the AMANDA-B10 detector, as well as initial results of the full AMANDA-II detector.

Astroparticle physicsPhysicsParticle physicsMuonPhysics::Instrumentation and DetectorsAstrophysics::High Energy Astrophysical PhenomenaDetectorSolar neutrino problemNuclear physicsNeutrino detectorHigh Energy Physics::ExperimentNeutrinoNeutrino astronomyNeutrino oscillationPhysics::Atmospheric and Oceanic PhysicsParticle Physics - Phenomenology
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Search for sterile neutrino mixing using three years of IceCube DeepCore data

2017

Physical review / D 95(11), 112002(2017). doi:10.1103/PhysRevD.95.112002

FLUXSterile neutrinoParticle physicsPhysics and Astronomy (miscellaneous)Physics::Instrumentation and DetectorsSolar neutrinoAstrophysics::High Energy Astrophysical PhenomenaFOS: Physical sciences01 natural sciences530High Energy Physics - ExperimentOSCILLATION EXPERIMENTSHigh Energy Physics - Experiment (hep-ex)High Energy Physics - Phenomenology (hep-ph)0103 physical sciencesTRACK RECONSTRUCTIONddc:530010306 general physicsNeutrino oscillationPhysics010308 nuclear & particles physicsHigh Energy Physics::PhenomenologyAstronomySolar neutrino problemLINE-EXPERIMENT-SIMULATORMODELHigh Energy Physics - PhenomenologyNeutrino detectorPhysics and AstronomyMeasurements of neutrino speedHigh Energy Physics::ExperimentNeutrino astronomyNeutrino
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Status of the neutrino telescope AMANDA: Monopoles and WIMPs

2001

The neutrino telescope AMANDA has been set up at the geographical South Pole as first step to a neutrino telescope of the scale of one cubic kilometer, which is the canonical size for a detector sensitive to neutrinos from Active Galactic Nuclei (AGN), Gamma Ray Bursts (GRB) and Topological Defects (TD). The location and depth in which the detector is installed is given by the requirement to detect neutrinos by the Cherenkov light produced by their reaction products and to keep the background due to atmospheric muons as small as possible. However, a detector optimized for this purpose is also capable to detect the bright Cherenkov light from relativistic Monopoles and neutrino signals from …

PhysicsPhysics::Instrumentation and DetectorsAstrophysics::High Energy Astrophysical PhenomenaSolar neutrinoDark matterAstrophysics::Instrumentation and Methods for AstrophysicsAstronomyAstrophysics::Cosmology and Extragalactic AstrophysicsAstrophysicsSolar neutrino problemNeutrino detectorMeasurements of neutrino speedHigh Energy Physics::ExperimentNeutrinoNeutrino astronomyCherenkov radiation
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