2. 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

3. 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

4. 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

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

6. Building AMANDA

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

8. 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

9. 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

10. 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

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

12. 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

13. 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

14. 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

15. 1 km AMANDA II µ-event in IceCube 300 atmospheric neutrinos per day IceCube : -> Larger telescope -> Larger telescope -> Superior detector -> Superior detector