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Neutrino Astronomy

Neutrino Astronomy. @ South Pole. AMANDA & IceCube. Why Neutrino ?. High energy photons are absorbed beyond ~ 150Mpc g HE g LE  e - e + HE n s are unique to probe HE processes in the vicinity of cosmic accelerators HE Cosmic Rays and n s may have the same origin.

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Neutrino Astronomy

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  1. Neutrino Astronomy @ South Pole AMANDA & IceCube

  2. Why Neutrino ? • High energy photons are absorbed beyond ~ 150Mpc • gHE gLEe-e+ • HE ns are unique to probe HE processes in the vicinity • of cosmic accelerators • HE Cosmic Rays and ns may have the same origin

  3. Cosmic Neutrino Factories Most models assume a central black-hole and accretion disk. Particle acceleration occurs either near the black hole or in the jet p + p() p0 + p + ...  ggnmm  nm ne e

  4. nm + N m+ X Detection Principle neutrino Astrophysical Sources muon Neutrino interacts in ice surrounding the detector Muon track is reconstructed by mapping the Cherenkov photon times recorded by the Optical Modules

  5. AMANDA Detector @ South Pole Antarctica • 677 OMs • on 19 strings • since Jan 2000

  6. Building AMANDA

  7. AMANDA Event Signatures:Muons CC muon neutrino Interaction  track nm + N  m +X

  8. 1 km 0.02 0.1 0.5 Scattering coefficient (1/m) vs. depth 2 km 1 km deep and shallow ice for future IceCube IceCube

  9. Source\Sensitivity muon (10-15 cm-2 s-1) n(10-8 cm-2 s-1) Markarian 421 1.8 1.1 Markarian 501 1.8 1.1 Crab 2.7 1.3 Cass. A 1.6 1.2 SS433 5.9 2.4 Cyg. X-3 1.7 1.1 Point Sources Amanda II (2000) 1129 events • Improved coverage near horizon • Sensitivities calculated using background levels predicted from data • close to “/~ 1 sensitivity” for some sources Event times scrambled for blind analysis purposes. PRELIMINARY

  10. IceTop AMANDA • 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 1014 eV to 1018 eV South Pole Skiway • 4800 PMT • Instrumented volume: 1 km3 (1Gt) • 80 Strings • IceCube is designed to detect neutrinos of all flavors at energies from 107 eV to 1020 eV 1400 m IceCube 2400 m

  11. Construction: 11/2004-01/2010 Grid North 100 m AMANDA South Pole SPASE-2 Dome IceCube Skiway

  12. 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 Digital Optical Module - (DOM) DOM 33 cm

  13. IceCube String Main Cable 60 optical sensors DOM Base with HV 1400 m generator Electrical feedthrough for power + data OM Spacing: 17 m Photomultiplier DOM Board Gel Glass pressure String sphere. Rated to 10000 psi. Outer diameter: 13" 2400 m

  14. Two functions veto and calibration cosmic-ray physics Energy range: ~3 x 1014 -- 1018 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 Coincident events

  15. µ-event in IceCube300 atmospheric neutrinos per day AMANDAII IceCube: -> Larger telescope -> Superior detector 1 km

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