2. ECT*, October 7 2004 Tom Weiler, Vanderbilt University High-Energy Neutrino Astrophysics Tom Weiler Vanderbilt University Neutrinos and the Early Universe”, Trento ECT* Workshop, October 4-8 2004

3. ECT*, October 7 2004 Tom Weiler, Vanderbilt University Cosmic Photo- Proto-Spectra hadron wall? no wall a’tall sun SN87a Neutrino Incognito

4. ECT*, October 7 2004 Tom Weiler, Vanderbilt University 1991Fly’s Eye reports 3x10 20 eV, with proton-like profile; Akeno/AGASA Xpt begins mid-90sDUMAND taken off life-support; Baikal continues 90sSuperK neutrinos from the sun (directional astro) 1996AGASA reports event clustering within 2.5 0 ang. res’n and: F(E  10 20 eV) ~ 1/km 2 /century, with shower diameter ~ 5km, N(e  ) ~ 10 11 200020 events at and above 10 20 eV 2001HiRes withdraws 7 events; AGASA adds 6 (from  z > 45 o ); And the controversy has begun! Importantly, Auger gets first “light” 2002AMANDA pushes to 10 14 eV thru-Earth neutrinos 2005 Auger Observatory data expected 2008 Extreme Universe Space Observatory (EUSO) ?

5. ECT*, October 7 2004 Tom Weiler, Vanderbilt University CR Spectrum above a TeV from Tom Gaisser VLHC (100 TeV) 2

6. ECT*, October 7 2004 Tom Weiler, Vanderbilt University Highest Energy Event The CR record energy is 3x10 20 eV (0.3 ZeV). Found by Fly’s Eye a decade ago (they got lucky!). This is truly a macroscopic energy: 3x10 20 eV = 50 Joules equivalent to a Roger Clemens fastball, a Tiger Woods tee shot, a Pete Sampras tennis serve, Or a speeding bullet. (Also to 12 Calories, which heats a gram of water by 12 o C)

7. ECT*, October 7 2004 Tom Weiler, Vanderbilt University 3 x10 20 eV = macroscopic 50 Joules Clemens does this with 10 27 nucleons; Nature does this with one nucleon, 10 27 times more efficient !

8. ECT*, October 7 2004 Tom Weiler, Vanderbilt University Fly’s Eye 3 x 10 20 eV event (1992) 100 billion e+e- pairs at x max ~ 800 g/cm 2 This longitudinal profile is consistent with a primary proton, but not with a primary photon; Disfavors “local” top-down sources such as massive Particle DK, topo-defects, Z-bursts, etc.

9. ECT*, October 7 2004 Tom Weiler, Vanderbilt University EE Neutrinos are young Liberated at T=Mev, t= 1 sec Depends on energy (Lorentz boost) Consider a 10 20 eV neutrino. Lorentz factor = 10 21 for m = 0.1 eV. Age of Uni is 10 18 sec, But age of is 10 18 /10 21 sec = 1 millisecond ! And it doesn’t even see the stream of radiation rushing past it – untouched !

10. ECT*, October 7 2004 Tom Weiler, Vanderbilt University Size matters EUSO ~ 300 x AGASA ~ 10 x Auger EUSO (Instantaneous) ~3000 x AGASA ~ 100 x Auger

11. ECT*, October 7 2004 Tom Weiler, Vanderbilt University Extreme Universe Space Observatory 2009 EUSO onboard the ISS (Or Not!) 2012Hundredth anniversary of Hess – EUSO finishes three-year data-taking Article Images

12. ECT*, October 7 2004 Tom Weiler, Vanderbilt University “clear moonless nights” Or New York State power blackout

13. ECT*, October 7 2004 Tom Weiler, Vanderbilt University Orbiting Wide-angle Lens (OWL) 3000 events/year above 10 20 eV and UHE Neutrinos!

14. ECT*, October 7 2004 Tom Weiler, Vanderbilt University HAS event rate is small e.g. F CR at 10 20 eV implies 10 -2 events/yr;

15. ECT*, October 7 2004 Tom Weiler, Vanderbilt University AGASA Spectrum: EeV to ZeV AGASA, July 2002

16. ECT*, October 7 2004 Tom Weiler, Vanderbilt University Greisen-Zatsepin- Kuzmin and the Cosmic-Ray Wall  -resonance multi-pions Photo-pion production off CMB p+  cmb    p/n+ 

17. ECT*, October 7 2004 Tom Weiler, Vanderbilt University HiRes vs. AGASA UHE spectrum discovery opportunity GZK recovery ? Z-burst uncovery ? FlysEye event goes here EUSO reach x 10 3 better

18. ECT*, October 7 2004 Tom Weiler, Vanderbilt University AGASA hot-spots -- Data red: E > 4 10 19 eV green: E > 10 20 eV Cluster Component ~ E -1.8±0.5 Neutrinos will point better

19. ECT*, October 7 2004 Tom Weiler, Vanderbilt University AGASA hot-spots -- numbers Within 2.5 degree circles, AGASA identifies six doublet, one triplet, Out of 57 events; Opening the angle to just 2.6 degrees, AGASA identifies seven doublets, two triplets; Haverah Park contributes two more paired events in AGASA directions. NOT corroborated by HiRes. Source number ~ N 1 2 /2N 2 ~ 270 to 50%, weighting with GZK suppression,  ~ 10 -5 /Mpc 3  for source density

20. ECT*, October 7 2004 Tom Weiler, Vanderbilt University Berezinsky et al Xgal proton flux Mass-composition data (HiRes 2002) Xgal proton dominance begins at 10 18 eV, not 10 19 eV !  F ~ 50 x Waxman-Bahcall  AMANDA/RICE/EAS -sensitive !! (AGHW, to appear) Theory threshold for p  2.7K  pe + e - and data (knee) are at 10 17.6 eV.

21. ECT*, October 7 2004 Tom Weiler, Vanderbilt University AMANDA to 100 TeV

22. ECT*, October 7 2004 Tom Weiler, Vanderbilt University AMANDA/IceCube  event

23. ECT*, October 7 2004 Tom Weiler, Vanderbilt University Xgal proton fit  huge flux   is pion energy/CR energy at source (1 for WB “limit”);  z is cosmic evolution factor, 0.6 (no) to 3.0 (SFR) WB fluxes low Xgal dominance flux, with no evolution AGHW, hep-ph/04010003

24. ECT*, October 7 2004 Tom Weiler, Vanderbilt University Neutrinos versus Cosmic-Rays and Photons s come from central engines - near R s of massive BHs - even from dense “hidden” sources cf. s vs.  s from the sun s not affected by cosmic radiation (except for annihilation resonance) s not bent by magnetic fields - enables neutrino astronomy Also, besides Energy and Direction, ’s carry flavor

25. ECT*, October 7 2004 Tom Weiler, Vanderbilt University diagnostic of astro-engines: pp   vs. p    The process e +e --  W -- is resonant at 6.4 PeV; IceCube will have flavor ID, and  E/E of 25%, and so can measure On-Res/Off-Res ratio. pp make nearly equal       :  : e : e = 2:2:1:1  flavor democracy, e = 1/6 total p  via  + make  +      e = 1:1:1 (no e )  e = 1/15 total IceCube can resolve this (AGHW, ArXiv this week)

26. ECT*, October 7 2004 Tom Weiler, Vanderbilt University Flavor ratio  Topology ratio Map Beacom, Bell, Hooper, Pakvasa, TJW, 2003

27. ECT*, October 7 2004 Tom Weiler, Vanderbilt University The cosmic flavor-mixing theorem If theta 32 is maximal (it is), And if Re(U e3 ) is minimal (it is), Then  and  equilibrate; Further, if initial e flux is 1/3 (as from pion-muon decay chain), Then all three flavors equilibrate. e :  :  = 1 : 1 : 1 at Earth

28. ECT*, October 7 2004 Tom Weiler, Vanderbilt University Democracy Broken: 1. decay (15 minutes of fame) 2. Vacuum resonance (MaVaNs, LIV vector) 3. Pseudo-Dirac oscillations 4. Source dynamics (w/ Farzan)

29. ECT*, October 7 2004 Tom Weiler, Vanderbilt University Neutrino Decay -- Models, Signatures, and Reach

30. ECT*, October 7 2004 Tom Weiler, Vanderbilt University “Essentially Guaranteed” High-Energy Galactic Neutrino Flux c  n = 10 kpc (E n / EeV) and E  / E n ~ Q / m n ~ 0.8 x 10-3  E ~ PeV, for E n ~ EeV

31. ECT*, October 7 2004 Tom Weiler, Vanderbilt University “More Guaranteed” Icecube atmos background in 1 o circle is just 1.5events/yr,  3.5 events offers 95% CL detection in 1 yr; Calculated signal is 4  /yr and 16 e +  showers/yr. Conclude that in a few years, IceCube attains 5  discovery sensitivity for Fe  n  e    Providing “smoking ice” for GP neutron hypothesis. Comparing to “guaranteed” cosmogenic flux, Galactic beam (here) is higher !