1. Gary C. Hill, CCAPP Symposium 2009, Ohio State University, October 12th, 2009 Photograph: Forest Banks Gary C. Hill University of Wisconsin, Madison for the IceCube collaboration

2. Gary C. Hill, CCAPP Symposium 2009, Ohio State University, October 12th, 2009 It’s a mysterious universe!

3. Gary C. Hill, CCAPP Symposium 2009, Ohio State University, October 12th, 2009 Neutrino and gamma production in cosmic ray accelerators? Hadronic accelerator? – cosmic ray origin? The TeV gammas? Let’s look for these neutrinos! -rays from fromsynchrotron

4. Gary C. Hill, CCAPP Symposium 2009, Ohio State University, October 12th, 2009 Cosmic ray induced “guaranteed sources” Cosmic rays on Cosmic Microwave Background: GZK neutrinos GZK neutrinos EHE: 10 9-10 GeV EHE: 10 9-10 GeV Cosmic rays on the earth’s atmosphere: Atmospheric neutrinos Cosmic rays on galactic plane: galactic plane neutrinos

5. Gary C. Hill, CCAPP Symposium 2009, Ohio State University, October 12th, 2009 The high-energy neutrino sky

6. Gary C. Hill, CCAPP Symposium 2009, Ohio State University, October 12th, 2009 Atmospheric Neutrinos Cosmic Ray ≈15 Km π+π+  + e+e+ e  

7. Gary C. Hill, CCAPP Symposium 2009, Ohio State University, October 12th, 2009

9. backgroundatmosphericmuon Direction: Reconstruction of Cerenkov cone Energy: Counting of modules that see photons

10. Gary C. Hill, CCAPP Symposium 2009, Ohio State University, October 12th, 2009

11. Event Signatures in IceCube  signature  signature 10 13 eV (10 TeV) ~90 hits 6x10 15 eV (6 PeV) ~1000 hits Multi-PeV   +N  +...  ± (300 m!)   +hadrons AMANDA Expect about 100,000 events/yr

12. Gary C. Hill, CCAPP Symposium 2009, Ohio State University, October 12th, 2009 Where are we pointing?

13. Gary C. Hill, CCAPP Symposium 2009, Ohio State University, October 12th, 2009 Moon declination during first 15 years

14. Gary C. Hill, CCAPP Symposium 2009, Ohio State University, October 12th, 2009 RA distribution relative to moon

15. Gary C. Hill, CCAPP Symposium 2009, Ohio State University, October 12th, 2009 Li and Ma significance distribution

16. Gary C. Hill, CCAPP Symposium 2009, Ohio State University, October 12th, 2009 Point source searches

17. Gary C. Hill, CCAPP Symposium 2009, Ohio State University, October 12th, 2009 IC40 6 month all-sky point source search

18. Gary C. Hill, CCAPP Symposium 2009, Ohio State University, October 12th, 2009 pre-trial significance 10 -4.4 expected in 61% of random skies IC40 6 month all-sky point source search

19. Gary C. Hill, CCAPP Symposium 2009, Ohio State University, October 12th, 2009 Search for a diffuse  signal with IC40 Diffuse models all harder (~E -2 ) than atmospheric (~E -3.7 ): energy separation Nch variable Range of spectral slopes: start with E -2

20. Gary C. Hill, CCAPP Symposium 2009, Ohio State University, October 12th, 2009 Blind region Energy separation: Nch variable Blind analysis: Best limit setting power (model rejection potential) Nch>100 E -2 test flux Atmospheric neutrinos

21. Gary C. Hill, CCAPP Symposium 2009, Ohio State University, October 12th, 2009 Sensitivity: for bg=6.1 events median event limit 5.84 Flux limit : 5.84/66.7x10 -6 = 8.8 x 10 -8 = 8.8 x 10 -8

22. Gary C. Hill, CCAPP Symposium 2009, Ohio State University, October 12th, 2009 Unblind the data: 6 events observed event limit 5.84 Flux limit : 5.84/66.1x10 -6 = 8.8 x 10 -8 = 8.8 x 10 -8

23. Gary C. Hill, CCAPP Symposium 2009, Ohio State University, October 12th, 2009 Reconstructing The Muon energy loss Reconstructing The Muon energy loss Approximate as: dusty clean deep shallow Incorporate Ice Properties: Formulate LLH: e+e-e+e-    pair-creation bremsstrahlung photo-nuclear

24. Gary C. Hill, CCAPP Symposium 2009, Ohio State University, October 12th, 2009 Energy estimator comparison Reconstructed dE/dX Number of Channels

25. Gary C. Hill, CCAPP Symposium 2009, Ohio State University, October 12th, 2009 Atmospheric neutrinos E -2 test flux

26. Gary C. Hill, CCAPP Symposium 2009, Ohio State University, October 12th, 2009 Likelihood shape analysis - probability of observable shape distribution {n i } given theory {μ i } ? Product of Poisson probabilities over bins: m parameters of interest; k-m nuisance parameters

27. Gary C. Hill, CCAPP Symposium 2009, Ohio State University, October 12th, 2009 Atmospheric neutrinos only

28. Gary C. Hill, CCAPP Symposium 2009, Ohio State University, October 12th, 2009 Allowed E -2 and prompt contributions Number of E -2 Number of prompt

29. Gary C. Hill, CCAPP Symposium 2009, Ohio State University, October 12th, 2009 Atmospheric and E -2 neutrinos

30. Gary C. Hill, CCAPP Symposium 2009, Ohio State University, October 12th, 2009 Allowed E -2 and prompt contributions Number of E -2 Number of prompt

31. Gary C. Hill, CCAPP Symposium 2009, Ohio State University, October 12th, 2009 Atmospheric, E -2 and prompt neutrinos

32. Gary C. Hill, CCAPP Symposium 2009, Ohio State University, October 12th, 2009 Allowed E -2 and prompt contributions Number of E -2 Number of prompt

33. Gary C. Hill, CCAPP Symposium 2009, Ohio State University, October 12th, 2009 IC40 diffuse sensitivity