TeV Particle Astrophysics II 1 Are there EHE signals? Shigeru Yoshida

TeV Particle Astrophysics II 2 Outline EHE CR fluxes – What’s going on? Revisit EHE particles models A different approach – Neutrinos! GZK GeV  ?

TeV Particle Astrophysics II 3 EHE CR fluxes Compiled by S.Yoshida for ICRC 2005 Taken from B.M.Connolly et al 2006

TeV Particle Astrophysics II 4

5 Energy estimation AGASA(SD) R core 600~1000m HiRes(FD) R core < R moliere ~70m Even if detector calibration is perfect… FD SD

TeV Particle Astrophysics II 6 Hybrid – SD+FD P.Sommers for Auger collab. (ICRC 2005) FD-SD Correlation exists! ABSOLUTE value of Energy ?? Fluctuation plays a visible role in the end

TeV Particle Astrophysics II 7 Really discrepancy? B.M. Connolly et al PRD 2006 Poor Stats --- N(>100EeV) ~ only 11 events Energy Uncertainty ---  E scale ~ 30% Bayes Factor Test BF using AGASA and Auger Spectrum BF using AGASA and HiRes1 Spectrum data MC from a single hypothesis

TeV Particle Astrophysics II 8 Physics may be responsible EGMF complicates particle trajectories Source distribution may not be isotropic Fluctuation in the spectra and intensities of the source - “cosmic variance”

TeV Particle Astrophysics II 9 Propagation in EGMF Sigl, Lemoine, Biermann, Astropart.Phys Delay time [yr] Energy [EeV] 0.3  G pancake E -1/3 E -1 (bohm diffusion) E -2 (rectilinear)

TeV Particle Astrophysics II 10 Propagation in EGMF Delay time [yr] Energy [EeV] More detailed EGMF model following Large Scale Structure Sigl, Miniati, En  elin, PRD 2004

TeV Particle Astrophysics II 11 Spectrum fluctuated! B 100 nG Sigl, Lemoine, Biermann, Astropart.Phys. 1999

TeV Particle Astrophysics II 12 Spectrum fluctuated! B 300 nG! More pronounced GZK feature Sigl, Lemoine, Biermann, Astropart.Phys. 1999

TeV Particle Astrophysics II 13 Astrophysical sources in Large Scale Structures Sigl, Miniati, En  elin, PRD 2004 EGMF Baryon Density = Source Density uG nG Observer 20Mpc

TeV Particle Astrophysics II 14 Astrophysical sources in Large Scale Structures Sigl, Miniati, En  elin, PRD 2004 EHE Sky map

TeV Particle Astrophysics II 15 Astrophysical sources in Large Scale Structures With EGMF ~ uG Without EGMF Armengaud, Sigl, Miniati,PRD 2005 Intrinsic fluctuation due to source intensities primary spectrum source density observer’s location in LSS

TeV Particle Astrophysics II 16 “Favored” Scenario Source density 2.4x10 -5 Mpc -3 Need LSS? Yes Observer’s location Void Mean spectral index -2.4 B at the observer 8.2 pG So Many Unknown Parameters to fit poor data…. But allows many OTHER possibilities…. 

TeV Particle Astrophysics II 17 Top Down model never dies Beyond the Standard Model Top-Down neutrinos decays/interaction of massive particles (topological defects, SUSY, micro black hole, …) The main energy range: E ~ GeV X

TeV Particle Astrophysics II 18 Top Down model never dies  suppressed by (unknown) URB Cut-off feature Sigl, Lee, Bhattacharjee, Yoshida, PRD 1999

TeV Particle Astrophysics II 19 Top Down model never dies Sigl, Lee, Bhattacharjee, Yoshida, PRD 1999 A bunch of Recycling  in 100 GeV region

TeV Particle Astrophysics II 20 (EHE) Photons in EBL EM cascades lead to the diffuse  -ray BG in the GeV range URB CMB IR/O Transparent Energy Conservation

TeV Particle Astrophysics II 21 EHE astrophysics “Everything is transient” “Nothing is certain”  Unknown EGMF strength  Unknown EGMF configuration  Unknown location of us relative to EGMF halo  Unknown source spectra  Unknown source distribution  Unknown source intensity  Large energy scale uncertainty  Extremely low flux  May or may not have a GZK cutoff

TeV Particle Astrophysics II 22 Neutrinos – The Last Crusader Forget about EGMF stuff Propagate cosmological distances – no local effects EHE  -rays ? - It depends on unknown URB!

TeV Particle Astrophysics II 23 GZK The standard scenario The standard scenario EHE cosmic-ray induced neutrinos The main energy range: E ~ GeV EHE-CR  e   

TeV Particle Astrophysics II 24 GZK Yoshida, Teshima, Prog.Theo.Phys. 1993

TeV Particle Astrophysics II 25 GZK – it’s robust Compiled by A. Ishihara Yoshida, Teshima Engel, Seckel, Stanev 2001

TeV Particle Astrophysics II 26 GZK – parameter dependences Yoshida, Teshima, Prog.Theo.Phys Kalashev et al PRD 2002 E max, E -   J(E>10 EeV) m, Zmax  J(E<1EeV)

TeV Particle Astrophysics II 27 GZK – Strong Evolution case Yoshida, Dai, Jui, Sommers ApJ 1997 Hard primary proton spectrum + strong evolution of sources Unlikely case, but Flux >> Waxman.Bahcall GeV diffuse  OK with EGRAT Reachable even by present detectors.

TeV Particle Astrophysics II 28 UHE/EHE fluxes GZK (hard, high Emax) - Kalashev et al 2002 GZK (strong evolution) - ibid GZK (standard) - Yoshida Teshima 1993 TD - Sigl et al 1999 Zburst – Yoshida et al 1998

TeV Particle Astrophysics II 29 ANITA constraints Barwick et al PRL 2006 (projected) Bound from the 2003 flight. Ruled out Z-burst

TeV Particle Astrophysics II 30 IceCube constraints Yoshida, Ishibashi, Miyamoto, PRD 2004 ~5 yr constraints Look for downgoing or horizontal events.

TeV Particle Astrophysics II 31 IceCube EHE 100 TeV 9 EeV

TeV Particle Astrophysics II 32 IceCube EHE IceCube Preliminary GZK  0.35 events/year GZK  0.31 events/year Atmospheric  events/year GZK  GZK  Atmospheric  GZK  GZK  Atmospheric  A.Ishihara, S.Yoshida for the IceCube collaboration

TeV Particle Astrophysics II 33 EHE Neutrinos + 100GeV  -ray channel have its own drawback low statistics, poor pointing resolutions…  channel compensates Arrival direction Local UHECR source  VHE  (Ferrigno,Blasi,Marco, Astro.Phys.2005) (Gabici, Aharonian, PRL 2006)

TeV Particle Astrophysics II 34 (EHE) Photons in EBL URB CMB IR/O Transparent Energy Conservation Cooling down to 100 GeV

TeV Particle Astrophysics II 35 A “point” source contribution to the diffuse flux Diffuse FluxFlux from A source Source density Zmax ~4 m~4 Z~2 (cosmological distances) “R -2 ”

TeV Particle Astrophysics II 36 ICTs for point sources? Taken from W. Hofman 2006  = 2x10 -7 Mpc -3  = 2x10 -9 Mpc -3 Note: AGASA clusters   local ~10 -4 ~10 -5 Too few as UHRCR sources

TeV Particle Astrophysics II 37 A “multi-particle” campaign I would like a Munich beer.. Helles ? What are the right ascension/ declination?

TeV Particle Astrophysics II 38 Summary  EHE signals are Extremely High Epicurean money/time (your career) consuming to explore  Hard to interpret data. Large Scale Structure?  ~ Mpc -3 ?  Neutrino may be a rescue Top Down model produces easily-reachable signals. GZK detection is a probe to cosmological sources. -- Anita, Auger (>10EeV) IceCube (100 PeV-EeV)  Search for 100 GeV  ’s with ICTs is worth to try