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Published byAlison Richards Modified over 8 years ago
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Why Neutrino ? High energy photons are absorbed beyond ~ 150Mpc HE LE e - e + HE s are unique to probe HE processes in the vicinity of cosmic accelerators HE Cosmic Rays and s may have the same origin
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Most models assume a central black-hole and accretion disk. Particle acceleration occurs either near the black hole or in the jet p + p( ) e e Cosmic Neutrino Factories
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Detection Principle neutrino muon Astrophysical Sources Neutrino interacts in ice surrounding the detector Muon track is reconstructed by mapping the Cherenkov photon times recorded by the Optical Modules N X
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AMANDA Detector @ South Pole Antarctica 677 OMs on 19 strings since Jan 2000
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Building AMANDA
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AMANDA Event Signatures: Muons + N +X + N + X CC muon neutrino Interaction track track
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1 km 2 km 1 km deep and shallow ice for future IceCube for future IceCube IceCube 0.02 0.1 0.5Scatteringcoefficient(1/m) vs. depth
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Improved coverage near horizon Sensitivities calculated using background levels predicted from data close to “ / ~ 1 sensitivity” for some sources 1.11.7Cyg. X-3 2.45.9SS433 1.21.6Cass. A 1.32.7Crab 1.11.8Markarian 501 1.11.8Markarian 421 ( 10 -8 cm -2 s -1) muon ( 10 -15 cm -2 s -1) Source\Sensitivity Point Sources Amanda II (2000) Event times scrambled for blind analysis purposes. 1129 events
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1400 m 2400 m AMANDA South Pole IceTop Skiway 4800 PMT Instrumented volume: 1 km3 (1Gt) 80 Strings IceCube is designed to detect neutrinos of all flavors at energies from 10 7 eV to 10 20 eV IceCube 1 station on top of each IceCube string 2 ice tanks per station 2 DOMs in each tank IceTop will detect Air Showers of energies 10 14 eV to 10 18 eV
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Construction: 11/2004-01/2010 AMANDA SPASE-2 South Pole Dome Skiway 100 m Grid North IceCube
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Digital Optical Module - (DOM) Self-triggers on each pulse Captures waveforms Time-stamps each pulse Digitizes waveforms Performs feature extraction Buffers data Responds to Surface DAQ Set PMT HV, threshold, etc 33 cm DOM
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IceCube String 1400 m 2400 m 60 optical sensors Main Cable DOM Base with HV generator Electrical feedthrough for power + data Glass pressure sphere. Rated to 10000 psi. Outer diameter: 13" Photomultiplier Gel String OM Spacing: 17 m DOM Board
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Coincident events Two functions –veto and calibration –cosmic-ray physics Energy range: –~3 x 10 14 -- 10 18 eV –few to thousands of muons per event Measure: –Shower size at surface –High energy muon component in ice Large solid angle –One IceTop station per hole –~ 0.5 sr for C-R physics with “contained” trajectories –Larger aperture as veto IceTop
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1 km AMANDA II µ-event in IceCube 300 atmospheric neutrinos per day IceCube : -> Larger telescope -> Larger telescope -> Superior detector -> Superior detector
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