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High-Energy Cosmic Ray/ n Observatories, and What They Can Do for Us

High-Energy Cosmic Ray/ n Observatories, and What They Can Do for Us. Tom Weiler Vanderbilt University m. Cosmic Photon- Proton-Spectra. SN87a. sun. Neutrino Incognito. hadron wall?. no wall a’tall. The Sun thru SuperK n eyes:. No dark glasses required. Timeline.

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High-Energy Cosmic Ray/ n Observatories, and What They Can Do for Us

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  1. High-Energy Cosmic Ray/n Observatories,and What They Can Do for Us Tom Weiler Vanderbilt University m Tom Weiler, Vanderbilt University

  2. Cosmic Photon- Proton-Spectra SN87a sun Neutrino Incognito hadron wall? no wall a’tall Tom Weiler, Vanderbilt University

  3. The Sun thru SuperK n eyes: No dark glasses required Tom Weiler, Vanderbilt University

  4. Timeline 1991 Fly’s Eye reports 3x1020 eV, with proton-like profile; Akeno/AGASA Xpt begins  mid-90s DUMAND prototype ended; Baikal continues  90s SuperK neutrinos from the sun (directional astro)  1996 AGASA reports event clustering within 2.50 ang. res’n and: F(E  1020 eV) ~ 1/km2/century, withshower diameter ~ 5km, N(e) ~ 1011  2000 20 events at and above 1020 eV  2001 HiRes withdraws 7 events;AGASA adds 6 (from z > 45o); And the controversy has begun! Importantly, Auger gets first “light”  2002 AMANDA pushes to 1014 eV thru-Earth neutrinos 2005 IceCube sees first muon  2005 Auger Observatory data expected  2008 Extreme Universe Space Observatory (EUSO) ? Tom Weiler, Vanderbilt University

  5. 2012, a hundred years since Victor Hess Auger data digested IceCube data digested (neutrinos are calorie-free) Anita data on cosmogenics Nestor/Antares 100 GeV point sources EUSO extends Auger GZK are history! Neutrino sky-maps are available in textbooks; But, there is no consensus theory in sight for neutrino mass and mixing Tom Weiler, Vanderbilt University

  6. CR Spectrum above a TeV from Tom Gaisser VLHC (100 TeV)2 Tom Weiler, Vanderbilt University

  7. Highest Energy Event The CR record energy is 3x1020 eV (0.3 ZeV). Found by Fly’s Eye a decade ago (they got lucky!). This is truly a macroscopic energy: 3x1020 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 12oC) Tom Weiler, Vanderbilt University

  8. 3 x1020 eV = macroscopic 50 Joules Clemens does this with 1027 nucleons; Nature does this with one nucleon, 1027 times better pitcher ! Tom Weiler, Vanderbilt University

  9. Fly’s Eye 3x1020 eV event (1992) 100 billion e+e- pairs at xmax ~ 800 g/cm2 This longitudinal profile is consistent with a primary proton, but less so with a primary photon; Disfavors “local” top-down sources such as massive Particle DK, topo-defects, Z-bursts, etc. Tom Weiler, Vanderbilt University

  10. AGASA Spectrum: EeV to ZeV AGASA, July 2002 Tom Weiler, Vanderbilt University

  11. UHECR Mysteries -- acceleration mechanism above 10^18 eV -- bottom-up: few nearby candidates for p&A (50Mpc horizon) -- top-down gammas (5Mpc horizon) and neutrinos (no horizon) -- is there a GZK suppression? (AGASA vs HiRes) -- is there directional clustering of events? (AGASA vs HiRes) -- is the crossover to Xgal at 2nd knee (10^18eV), or ankle (~10^19eV) ? Neurtrino co-emission an important tool !! Tom Weiler, Vanderbilt University

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

  13. HiRes vs. AGASA UHE spectrum FlysEye event goes here discovery opportunity GZK recovery ? Z-burst uncovery ? Auger (EUSO) reach 70 (103) better Tom Weiler, Vanderbilt University

  14. Auger update – February05 -- 12 of 24 FD’s operational (50%) -- 650 (of 1600) tank’s operational (40%) -- 100,000 events within 60deg vertical -- data set Jan04-Mar05 to publish at ICRC Aug05, with AGASA-equivalent exposure -- site inaugural celebration Nov05 -- all 24 FDs end of 05 -- all 1600 SDs July06 Tom Weiler, Vanderbilt University

  15. Auger Rates No GZK  EUSO comparison: EUSO FOV ~ (230 km)2~ 70 (instantaneous) Auger FOV (30 km)2 x 15% EUSO duty cycle ~ 10 (averaged) But EUSO energy threshold ~ n x 1019 eV, versus Auger threshold ~ 1018 eV. Tom Weiler, Vanderbilt University

  16. AGASA hot-spots -- Data red: E > 4 1019 eV green: E > 1020 eV Cluster Component ~ E -1.8±0.5 Neutrinos will point better Tom Weiler, Vanderbilt University

  17. 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 ~ N12/2N2 ~ 270 to 50%, • weighting with GZK suppression, • ~ 10-5 /Mpc3for source density Tom Weiler, Vanderbilt University

  18. “Essentially Guaranteed” High-Energy Galactic Neutrino Flux ctn = 10 kpc (En / EeV) and En/ En ~ Q / mn ~ 0.8 x 10-3  En ~ PeV, for En ~ EeV AGHW2004 Tom Weiler, Vanderbilt University

  19. AMANDA, RICE, Anita, and IceCube:neutrinos as ice-art Tom Weiler, Vanderbilt University

  20. AMANDA/IceCube nm event and coming in the Mediterranean: Nestor,Antares Tom Weiler, Vanderbilt University

  21. “More Guaranteed” Comparing to “guaranteed” cosmogenic flux, Galactic beam (here) is higher ! Icecube atmos background in 1o circle is just 1.5events/yr,  3.5 events offers 95% CL detection in 1 yr; Calculated signal is 4 nm /yr and 16 ne+nt showers/yr. Conclude that in a few years, IceCube attains 5s discovery sensitivity for Fe  n  ne  nm, providing “smoking ice” for GP neutron hypothesis. Tom Weiler, Vanderbilt University

  22. Galactic Plane b-beam, pure anti-ne at source Tom Weiler, Vanderbilt University Serpico and kachelreiss, 2005

  23. Xgal proton flux – Berezinsky et al Mass-composition data (HiRes 2002) Theory threshold for pg2.7Kpe+e- and data (knee) are at 1017.6 eV. • Xgal proton dominance • begins at 1018 eV, not 1019 eV ! • Fn ~ 50 x Waxman-Bahcall • AMANDA/RICE/EAS-sensitive !! (AGHW, 2004) Tom Weiler, Vanderbilt University

  24. AMANDA to 100 TeV Tom Weiler, Vanderbilt University

  25. Xgal proton fit huge n flux low Xgal dominance flux, with no evolution WB fluxes AGHW, hep-ph/04010003, And in prog, w/ A. Ringwald xp is pion energy/CR energy at source (1 for WB “limit”); xz is cosmic evolution factor, 0.6 (no) to 3.0 (SFR) Tom Weiler, Vanderbilt University

  26. Auger Skies Galaxy Distribution 7-21 MpcVisible from the southern site Galaxy Distribution 7-21 Mpc Visible from the northern site Tom Weiler, Vanderbilt University

  27. Centaurus A (3.4 Mpc South) Tom Weiler, Vanderbilt University

  28. Auger neutrons form Cen-A Since ctn = 0.9 Mpc E20, Neutron survival probability from Cen-A = e –3.8/E20 = 2% at 1020 eV = 15% at 2 1020 eV = 1/e at 3.8 1020 eV Maybe 2 evts/yr at Auger, more at EUSO, with Glennys’ flux (Farrar-Piran) Anchordoqui, Goldberg, TJW; PRL2001 Tom Weiler, Vanderbilt University

  29. Size matters EUSO ~ 300 x AGASA ~ 15 x Auger EUSO (Instantaneous) ~3000 x AGASA ~ 100 x Auger Tom Weiler, Vanderbilt University

  30. Article Images Extreme Universe Space Observatory • EUSO onboard the ISS (Or Not!) • 2012 Hundredth anniversary of Hess • – EUSO finishes three-year data-taking Tom Weiler, Vanderbilt University

  31. “clear moonless nights” Or New York State power blackout Tom Weiler, Vanderbilt University

  32. Orbiting Wide-angle Lens (OWL) 3000 events/year above 1020eV and UHE Neutrinos! Tom Weiler, Vanderbilt University

  33. On to Neutrinos Tom Weiler, Vanderbilt University

  34. Neutrinos versusCosmic-Rays and Photons ns come from central engines - near Rs of massive BHs - even from dense “hidden” sources cf. ns vs. gs from the sun ns not affected by cosmic radiation (except for annihilation resonance) ns not bent by magnetic fields - enables neutrino astronomy Also, besides Energy and Direction, n’s carry flavor Tom Weiler, Vanderbilt University

  35. The “Learned Plot” – merits of cosmic L/E Oscillation phase is ( L dm2 / 4 En ) Figure parameterized by dm2 / (eV)2 Nature’s miracles: L/E, m, nmatter Tom Weiler, Vanderbilt University

  36. The cosmicnflavor-mixing theorem If theta32 is maximal (it is), And if Re(Ue3) is minimal (it is), Then nm and nt equilibrate; Further, if initial ne flux is 1/3 (as from pion-muon decay chain), Then all three flavors equilibrate. ne:nm:nt = 1 : 1 : 1 at Earth Tom Weiler, Vanderbilt University

  37. Democracy Broken: • Galactic b-beam • 2. Source dynamics • 3. n decay (15 minutes of fame) • 4. Vacuum resonance • (MaVaNs, LIV vector) • 5. Pseudo-Dirac n oscillations Tom Weiler, Vanderbilt University

  38. n-decay (via majoron emission) P(survive)= e –t/t = e –(L/E)(m/t0) Beacom, Bell, Hooper, Pakvasa, TJW, PRL2003 Tom Weiler, Vanderbilt University

  39. diagnostic of astro-engines:ppp vs. pg p The process ne+e-- W-- is resonant at 6.4 PeV; IceCube will have flavor ID, and DE/E of 25%, and so can measure On-Res/Off-Res ratio. pp make nearly equal p+p-, with Pp/Pp ~ 0.6  nm:nm:ne:ne = 2:2:1:1  flavor democracy, ne = 1/6 total pg via D+ make p+, with Pp/Pp ~ 0.25  nm:nm:ne = 1:1:1 (no ne)  ne = 1/15 total IceCube can resolve this (AGHW, hep-ph/0410003) Tom Weiler, Vanderbilt University

  40. Extreme Energy (EE) Neutrinos Sources: Bottom-Up “Zevatrons” - givens Cosmogenics ~1019 eV ·     AGNs ·     GRBs ·     Hidden vs. Transparent (the thick/thin debate) Top-Down “EE-trons” - pure speculation ·     Topological Defects ·     Wimpzillas, M ~H(post-inflation) ~1022 eV ·     Msee-saw ~ 1023 eV ·     MGUT ~ 1025 eV ·     And even MPlanck ~ 1028 eV Other: - impure thoughts   Mirror-Matter mixing Multiverse Leakage (Brane-bridges) Tom Weiler, Vanderbilt University

  41. Model n fluxes(Protheroe review 199X) atmosphere AGN pgIsm GRB GZK GeV SMPs TDs MGUT Tom Weiler, Vanderbilt University

  42. EE Neutrinos are young Liberated at T=Mev, t= 1 sec; But age depends on energy (Lorentz boost) (Peter Minkowski) Consider a 1020 eV neutrino. Lorentz factor = 1021 for mn = 0.1 eV. Age of Uni is 1018 sec, But age of n is 1018/1021 sec = 1 millisecond ! And it doesn’t even see the stream of radiation rushing past it – untouched ! Tom Weiler, Vanderbilt University

  43. Earth Absorption versus Neutrino Cross-Section Tom Weiler, Vanderbilt University

  44. Can’t Lose Thm for Space-based Whatever the weak cross-section, get robust event rate from HAS or UAS! and Get measurement of neutrino cross-section (peak angle also gives snN) A. Kusenko, TJW PRL2002 Tom Weiler, Vanderbilt University

  45. Upward and Horizontal Air-shower Rates Versus Neutrino Cross-section HAS UAS Kusenko, TJW, PRL2002 Tom Weiler, Vanderbilt University

  46. Space-based HAS/UAS with cirrus (12km) or high cumulus (4km) clouds No clouds Sergio Palomares-Ruiz, TJW Tom Weiler, Vanderbilt University

  47. n HAS event rate is small e.g. FCR at 1020 eV implies 10-2 events/yr; Tom Weiler, Vanderbilt University

  48. View (Japanese) of Earth-Moon System – Radio Cherenkov n radio Cherenkov This is literally GLUE Xpt, is related to RICE and FORTE, and eventually, to SalSa Tom Weiler, Vanderbilt University

  49. Model Neutrino Fluxes and Future Limits GLUE, RICE, Forte ,Auger, Anita, EUSO From Eberle, AR, Song, TJW; Semikoz and Sigl Tom Weiler, Vanderbilt University

  50. Z-burst integrated rate (EUSO/yr) toward Virgo Red = photons Blue = protons Green = Gal bkgd Tom Weiler, Vanderbilt University

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