kilometer-scale neutrino observatories

1. kilometer-scale neutrino observatories

2. AMANDA: Proof of Concept • since 1992 we have deployed24strings with more than 750photon detectors (basically 8-inch photomultipliers). • R&D detector for proof of concept:375 times SuperK instrumented volume with 1.5% the total photocathode area. • IceCube: 45 times AMANDA II instrumented volume with 7 times the total photocathode area.

4. IceTop AMANDA South Pole Runway 1400 m 2400 m IceCube • 80 Strings • 4800 PMT • Instrumented volume: 1 km3 (1 Gton) • IceCube is designed to detect neutrinos of all flavors at energies from 107 eV (SN) to 1020 eV

5. South Pole AMANDA– 1 mile deep

6. South Pole Dark sector Skiway AMANDA Dome IceCube Planned Location 1 km east

7. South Pole Dark sector Skiway AMANDA Dome IceCube

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

9. Muon Events Eµ= 6 PeV Eµ= 10 TeV Measure energy by counting the number of fired PMT. (This is a very simple but robust method)

10. Cherenkov light from muons and cascades muon cascade: e or t • Maximum likelihood method • Use expected time profiles of photon flight times Reconstruction

11. AMANDA Event Signatures: Cascades • CC electron and tau neutrino interaction: (e,,) + N  (e, ) + X • NC neutrino interaction: x + N  x + X Cascades

12. ne + N --> e- + X Cascade event • the length of the e- cascade is small compared to the spacing of sensors. • roughly spherical density distribution of light. • 1 PeV ≈ 500 m diameter, additional 100 m per decade of energy • linear energy resolution Energy = 375 TeV

13. nt t PeVt(300m) t decays

14. Neutrino ID (solid)Energy and angle (shaded) Neutrino flavor • Filled area: particle id, direction, energy • Shaded area: energy only

15. enhanced role of tau neutrinos: • cosmic beam: ne = nm = nt because of oscillations • nt not absorbed by the Earth • (regeneration) • pile-up near 1 PeV • where ideal sensitivity

16. IceCube • start 02 • first strings 04 • completed 09

18. Drilling Amanda (3-reel) and ICECUBE (1-reel) Drill

19. Drilling ICECUBE

20. Schedule and Cost 03-04 drill equipment to Pole 04-05 first strings (proof that 16/season are feasible, prepare 10 full strings) 05-06 16 strings 06-07 16 strings 07-08 16 strings 08-09 16 strings 09-10 remaining strings Overall cost with personnel, contingency, overhead: ~ 250 M$ Detector: ~ 55 M$ Logistics, including drilling: ~ 40 M$

22. - timing - dyn. range - no x-talk - easy calibration - cost - robustness - dynamic range evolution of read-out strategy Test of ICE3 technology 01/02 - 03/04: Equipping all Amanda channels with FADCs to get full waveform information (IceCube compatibility)  better reconstruction, particularly cascades and high energy tracks

23. Assembled DOM

25. IceCube has been designed as a discovery instrument with improved: • telescope area ( > 1km2 after all cuts) • detection volume ( > 1km3 after all cuts) • energy measurement: • secondary muons ( < 0.3 in ln E) and • electromagnetic showers ( < 20% in E) • identification of neutrino flavor • Sub-degree angular resolution • (< unavoidable neutrino-muon misalignment)

26. AMANDA • AMANDA collected > 3,000 n’s • 4 more every day on-line • neutrino sensitivity has reached n = g • > 300,000 per year from IceCube • race for solving the CR puzzle is on!

27. conclusions • nu astronomy reached ~ 0.1 km2year • will reach km-scale in < 5 years • northern hemisphere detectors soon • EeV detectors over similar time scale • if history repeats, I did not tell • you about the science !!!

28. The IceCube Collaboration • Bartol Research Institute, University of Delaware • BUGH Wuppertal, Germany • Universite Libre de Bruxelles, Brussels, Belgium • CTSPS, Clark-Atlanta University, Atlanta USA • DESY-Zeuthen, Zeuthen, Germany • Institute for Advanced Study, Princeton, USA • Dept. of Technology, Kalmar University, Kalmar, Sweden • Lawrence Berkeley National Laboratory, Berkeley, USA • Department of Physics, Southern University and A\&M College, Baton Rouge, LA, USA • Dept. of Physics, UC Berkeley, USA • Institute of Physics, University of Mainz, Mainz, Germany • Dept. of Physics, University of Maryland, USA • University of Mons-Hainaut, Mons, Belgium • Dept. of Physics and Astronomy, University of Pennsylvania, Philadelphia, USA • Dept. of Astronomy, Dept. of Physics, SSEC, PSL, University of Wisconsin, Madison, USA • Physics Department, University of Wisconsin, River Falls, USA • Division of High Energy Physics, Uppsala University, Uppsala, Sweden • Fysikum, Stockholm University, Stockholm, Sweden • University of Alabama, Tusceloosa, USA • Vrije Universiteit Brussel, Brussel, Belgium • Chiba University, Japan • Imperial College London, UK • Utrecht University, Utrecht, The Netherlands • Universidad Simon Bolivar, Caracas, Venezuela • University of Canterbury, Christchurch, New Zealand

29. super-EeV detectors

30. GZK Cosmic Rays & Neutrinos • cosmogenic neutrinos are guaranteed • fluxes may be larger for some models, such as topological defects p + gCMBp + n

31. Radio Emission from neutrino-induced electromagnetic cascades • Electromagnetic cascades: electron-positron pairs and • (mostly) gammas  electrically neutral, no radio emission. • Compton scattering of photons on atomic electrons creates • negative charge excess of ~ 20% • Negative charge radiates coherently at MHz ~ GHz  • Power = Energy 2 • Askarian effect demonstrated at SLAC: consistent with • calculations

32. RICERadio Detection in South Pole Ice • Installed ~15 antennas • few hundred m depth with • AMANDA strings. • • Tests and data since 1996. • • Most events due to local • radio noise, few candidates. • • Continuing to take data, • and first limits prepared. • • Proposal to Piggyback with • ICECUBE Neutrino enters ice Neutrino interacts Antenna & Cable Two cones show 3 dB signal strength Cube is .6 km on side

33. TauWatchUsing Mountains to Convert ντ 3/02 Workshop in Taiwan, see http://hep1.phys.ntu.edu.tw/vhetnw also, HiRes, Auger….

34. ANITA : Radio from EeV n’s in Polar Ice • •Antarctic Ice at f<1GHz, T<-20C • largest homogenous, RF-transmissive solid mass in the world

35. Antarctic Impulsive Transient Antenna (ANITA) • ANITA Goal: Pathfinding mission for GZK neutrinos • NASA SR&T start expected this October, launch in 2006 Solar Panels M. Rosen, Univ. of Hawaii ANITA Gondola & Payload Antenna array Cover (partially cut away)

36. Ocean Acoustic Detection New Stanford Effort using US Navy Array US Navy acoustic tracking range in Tongue of the Ocean, Atlantic Hydrophones 1550-1600 m deep pancake beam pattern G.Gratta, atro-ph/0104033

37. Summary on Technology  Over 5 years, Amanda has evolved into a 30.000 m2 neutrino telescope  Construction and improvement hand in hand  Developed and tested IceCube technology  Detailed measurement of ice down to 2.4 km  Clear record in performance, reliability, time schedule and cost  We know that we can build a km3 telescope

38. Summary Amanda Physics Diffuse flux: Best limits. Entering interesting range.  EHE fluxes: 0.3 km2 at EeV. A-II testing EeV blazar models.  Point sources: Best limits. Testing first models.  GRB: sensitivity after 4 years close to predictions  Relativistic Magnetic Monopoles: Best limits (0.05 x Parker bound)  WIMP search: high mass limits ~ Underground limits  Monitoring Galaxy for SN bursts  Cosmic Ray Composition at knee

39. ... and IceCube Physics  Diffuse flux: sensitivity nearly factor 10 below WB limit  EHE fluxes: IceCube testing some GZK models  Point sources: sensitivity ~ 10-12 cm-2 s-1 for > 1 TeV Many models predict up to few tens of events/year  GRB: 10-100 events per year. Test WB model  Rel.Magnetic Monopoles: < 1/1000 Parker bound)  WIMPs: complementary to future direct search expts.  SN monitoring up to LMC. Triangulation ?  Cosmic ray composition at knee