we built a km 3 neutrino detector  3 challenges: drilling optics of ice atmospheric muons

1. we built a km3 neutrino detector  3 challenges: • drilling • optics of ice • atmospheric muons • atmospheric neutrino spectrum • atmospheric muon spectrum: first surprise • search for the sources of the Galactic cosmic rays • search for the extragalactic cosmic rays • gamma ray bursts • GZK neutrinos • a multi-wavelength story • search for dark matter IceCube.wisc.edu

2. WIMP search strategies • Direct detection • Indirect detection:– neutrinos from the Earth/Sun– antiprotons from the galactic halo– positrons from the galactic halo– gamma rays from the galactic halo– gamma rays from external galaxies/halos– synchrotron radiation from the galactic center / galaxy clusters– ...

3. WIMP + nucleus WIMP + nucleus • Measure the nuclear recoil energy • Suppress backgrounds • Search for an annual modulation due to the Earth’s motion around the Sun direct detection - general principles c c c c c December June

7. present limits

8. DAMA result (> 8 sigma)

9. rc velocity distribution c n interactions sscatt n int. m int. nm Gcapture Gannihilation m neutralino capture and annihilation sun Freese, ’86; Krauss, Srednicki &Wilczek, ’86 Gaisser, Steigman & Tilav, ’86 Silk, Olive and Srednicki, ’85Gaisser, Steigman & Tilav, ’86

10. supersymmetry on the back of an envelope arXiv 9404252

11. c WIMP Capture and Annihilation n nm DETECTOR c + c W + W  n + n

12. indirect detection for cyclists e.g.n-telescope searches for 500 GeV WIMP 300 km/s > LHC limit 1.  - flux 2. solar cross section

13. Nsun = capture rate = annihilation rate 250 GeV 500 GeV mnm 3. Capture rate by the sun 4. Number of muon-neutrinos 0.1is the leptonic branching ratio

14. # events = 60 per year

15. update: focus region

20. neutrino rate versus WIMP masswhite line: 100 events km-2 yr-1

21. IC22

22. solar neutrino ratevs wimp mass0—1 TeV100 events km-2 yr-1

26. capture • equilibrium neutrino flux wimp-nucleon cross section indirect detection of dark matter

28. atmospheric neutrino events the sun

29. sensitivity to wimps withspin-independent interactions

30. <103 SI limit >103 SI limit arXiv:0906.1615

31. arXiv:0906.1615

32. neutrinos from the center of the Galaxy

33. conclusions • supersymmetry comes in 2 flavors: • spin-independent ( favors direct detection • because of A2 ) and spin-dependent • IceCube is competitive for spin-dependent • can probe most of the interesting parameter • space of the MSSM • [astrophysics is known ( no toothfairies )]

34. IceCube: multiwavelength analysis • IceCube • supernova explosions (millisecond alert) • a story from AMANDA days • TeV gamma ray observations • GRB IceCube takes data continuously and records and archives them

35. supernova burst: light from  PMT noise low (280 Hz)  detect correlated rate increase on top of PMT noise when supernova neutrinos pass through the detector

36. Simulation Data Kitaura, Janka, Hillebrandt (Astron. Astrophys. 450 (2006) 345) Garching first 20 msec deleptonization • Luminosities

37. starting points of neutrino showers • equivalent detection volume • of a 2.5 megaton SuperK-style • detector • 1 million events from 10 kpc • time of neutronization to a few • milliseconds

39. signal depends on • properties of the supernova collapse • unknown neutrino physics

41. Kamioka II 1987A

42. Super-K SNO coincidence server @ BNL alert LVD AMANDA (IceCube) Participation in SNEWS …several hours advanced notice to astronomers … IceCube will follow this year http://snews.bnl.gov astro-ph/0406214