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Theoretical Bounds and Current Experimental Limits on the Diffuse Neutrino Flux

Theoretical Bounds and Current Experimental Limits on the Diffuse Neutrino Flux. Rezo Shanidze 17/06/2004 Seminar zu aktuellen Fragen der Astroteilchenphysik. Layout. The sources of high energy n: - Bottom-up models: pp( g ) g p + X g mn m g e n m n e

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Theoretical Bounds and Current Experimental Limits on the Diffuse Neutrino Flux

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  1. Theoretical Bounds and Current Experimental Limits on the Diffuse Neutrino Flux Rezo Shanidze 17/06/2004 Seminar zu aktuellen Fragen der Astroteilchenphysik Reso Shanidze

  2. Layout • The sources of high energy n: - Bottom-up models: pp(g) g p + Xgmnm genm ne - Top-down models: Decays of WIMPs (Dark matter, SUSY, Topolocical defects) • Models and bounds: - Atmospheric n, WB-bound, HE-n from the Sun - Fluxes from AGN, GRB, … • Current experimental limits • Future prospects • Summary Reso Shanidze

  3. The Sources of High Energyn • Weak decays: p, K, …, charm hadrons: p g m nm (99.99 %) Kg m nm (63.4 %) p e n (4.9 %, 38.8%) - Ke3 decay (K, Ko) pmnm (4.9 %, 27.2%) - Km3 decay c gl nl + X , l =e, m ( 10 %) m ge nmne • ct (p,K, Ko)= 7.8 , 3.7 , 15.5 m, L=gct, g=E/m • ct( charm ) ~ 100 mm Reso Shanidze

  4. Neutrino Flux from pp and pg • Learned, Mannheim, Annu.Rev.Nucl.Part.Sci. 50(2000), 679-749 • The volume emissivity of produced p: • Qp(pp) =∫nt c Np (dspp(Ep,E)/dEp)(dN/dE) dE • dspp(EpE) /dEp - diff. Inclusive cross-section • dN/dE = N 0E–sdE - diff. energy spectra of p(CR) • Qp(pp)(E) – practically same energy spectra • Qn(pp) ~ 1Qp(pp) (4En) ~ En-s • dFn/dEn= ∫Q n drover spatial extent of the source Reso Shanidze

  5. Atmospheric n flux • CR spectra: dN/dE = a E-a • a=2.7 (knee ~1015-1016eV) • Hydrogen(0,9) He(0.08), … • p(He) + A g p,(K) +X • r = r0exp(-h/h0) , h0=8.4km • Earth atmosphere: 1030 g/cm-2 • LpA(LKA)=116 (138) gm/cm-2 • Int./decay(GeV): 115(850) • change of a: 2.7 g 3.7 • Secant theta effect Reso Shanidze

  6. Atmospheric n/m flux • CR interaction and propagation: • MC codes: AIRES, COSMOS, MOCCA, HEMAS, CORSIKA • CORSICA physics models: VENUS, QGSJET, DPMJET, SYBILL, HDPM. • Experimental Data: - Underground experiments: MACRO, Frejus, L3C, … - NT data: Baikal, AMANDA Reso Shanidze

  7. E.Waxman,J.Bahcall PRD, v59(1998), 023003 Based on observations of Fly‘s Eye and AGASA Cosmological origin of CR above 1019 GeV (E.Waxman, astro-ph/9508037) Cosmological distribution of CR sources: dN/dE ~ E-a, a=2 Energy production rate ~ 5x10 44 erg Mpc-3yr -1 E2Fn< 2 x 10-8 GeV/cm2 s sr Waxman-Bahcal Bound:High energy n from astrophysical sources Reso Shanidze

  8. Cosmogenic (GZK) n Flux • Photopion production by UHECR (E>1019 GeV) : • g + p g D g N p ( np :2/3 ) • CMB : 2.7K , ~400 g /cm3, E ~ meV. • IR: 1-2 g cm3, E ~ eV. (T.Stanev, astro-ph/0404535) Reso Shanidze

  9. High Energy n from the SunSun as a standard n - candle ? • G. Ingelman, M. Thunman Phys. Rev. D 54(1996), 4385 • Calculations with LUND MC: PYTHIA(v5.7) /JETSET(7.4) CR flux: (aE-a), interaction With the Sun atmosphere • Rate of nm events integrated over the Sun solid angle. for NT (En > 100 GeV): 1 event /yr ~6x104m2 Reso Shanidze

  10. High Energy n Detectors Reso Shanidze

  11. NT-200 140 m The Baikal NT • First n telescope • 1.1 km depth • NT-36, 96, 192 Reso Shanidze

  12. Results from BAIKAL • 34 events of upward m • astro-ph/0404096 • Search for bright cascades • E-2, ne:nm:nt=1:1:1 • 90% C.L. limit FnE2: 1.3x10-6 cm-2s-1sr-1GeV Reso Shanidze

  13. AMANDA n Detector AntarcticMuonAndNeutrinoDetectorArray AMANDA (ice): 1150-2350m B10 (97-99): 10 strings, 302 OM II (2000): 19 strings 677 OM Reso Shanidze

  14. AMANDA Results( nm flux) • AMANDA B10: 1977 • m -measurement: • Coverage - 2p • ang. ~ 2o -2.5o • logE ~ 0.3-0.4 • 6 < E < 1000 TeV • PRL 90(2003) 2151101-1 • E-2, ne:nm:nt=1:1:1 • E2F(E) < 8.4x10-7GeV /cm2 s sr Reso Shanidze

  15. AMANDA Results(cascades) • cascades: • Coverage - 4p • ang. ~ 30o -40o • logE ~ 0.1-0.2 • Astro-ph/0405218 • 197 d, MC: 920 d • 50 TeV<E<5 PeV • E-2, ne:nm:nt=1:1:1 • E2F(E) < 8.6x10-7GeV /cm2 s sr Reso Shanidze

  16. Acoustic Detection of UHE n • Astro-ph/0406105 • SAUND detector: ~ 250 km2 (US Navy array) - only 7 used. • ~1600 m undersea • 147 days of running (2002) • Calibration, analysis -Energy, position - Rates, reconstraction Reso Shanidze

  17. IceTop AMANDA South Pole 1400 m 2400 m IceCube - 80 Strings - 4800 PMT • Instrumented volume: 1 km3 • Installation: 2004-2010 ~ 80.000 atm. per year Reso Shanidze

  18. DUMAND FREJUS  bound MACRO Muons in Amanda-B10 (1997) WB bound Expectation Amanda-II, 3 years Expectation IceCube, 3 years Search for diffuse excess of extra-terrestrial high energy muon neutrinos C.Spiering, VLVNT Workshop log E /GeV

  19. RICE AGASA Amanda, Baikal 2002 Anita 2004 AUGER nt AABN 2007 EUSO 2012 Auger Salsa km3 GLUE Reso Shanidze

  20. Sumary and Outlook • High energy n astronomy: Data from Baika(lake), AMANDA(ice) • New undersea NT: ANTARES, NESTOR • Sensitivity to the cosmic n diffuse flux NT on km3 scale: IceCube, KM3NeT • Acoustic and other technique (RICE, ANITA, EUSO, GLUE) for UHE n. Reso Shanidze

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