1. 17.05.2004 Reso Shanidze 1 Theoretical Bounds and Current Experimental Limits on the Diffuse Neutrino Flux Rezo Shanidze 17/06/2004 Seminar zu aktuellen Fragen der Astroteilchenphysik

2. 17.05.2004 Reso Shanidze 2 Layout The sources of high energy  The sources of high energy  - Bottom-up models: pp(  )   + X     e  e - Bottom-up models: pp(  )   + X     e  e  - Top-down models: Decays of WIMPs (Dark matter, SUSY, Topolocical defects) (Dark matter, SUSY, Topolocical defects) Models and bounds: Models and bounds: - Atmospheric, WB-bound, HE- from the Sun - Atmospheric, WB-bound, HE- from the Sun - Fluxes from AGN, GRB, … - Fluxes from AGN, GRB, … Current experimental limits Current experimental limits Future prospects Future prospects  Summary  Summary

3. 17.05.2004 Reso Shanidze 3 The Sources of High Energy The Sources of High Energy Weak decays: , K, …, charm hadrons: Weak decays: , K, …, charm hadrons:     (99.99 %)     (99.99 %) K    (63.4 %) K    (63.4 %)  e  4.9 %, 38.8%) - K e3 decay (K, K o )  e  4.9 %, 38.8%) - K e3 decay (K, K o )     4.9 %, 27.2%) - K  3 decay     4.9 %, 27.2%) - K  3 decay c   l l + X, l =e,  ( 10 %) c   l l + X, l =e,  ( 10 %)   e  e   e  e c ,K, K o )= 7.8, 3.7, 15.5 m, L=  c   =E/m c ,K, K o )= 7.8, 3.7, 15.5 m, L=  c   =E/m c  ( charm ) ~ 100  m c  ( charm ) ~ 100  m

4. 17.05.2004 Reso Shanidze 4 Neutrino Flux from pp and p  Neutrino Flux from pp and p  Learned, Mannheim, Annu.Rev.Nucl.Part.Sci. 50(2000), 679-749 Learned, Mannheim, Annu.Rev.Nucl.Part.Sci. 50(2000), 679-749  The volume emissivity of produced   The volume emissivity of produced   Q  (pp) = ∫ n t c N  (d  pp (E ,E)/dE  )(dN/dE) dE d  pp (E  E) /dE    diff. Inclusive cross-section d  pp (E  E) /dE    diff. Inclusive cross-section dN/dE = N 0 E –s dE - diff. energy spectra of p(CR) dN/dE = N 0 E –s dE - diff. energy spectra of p(CR) Q  (pp) (E) – practically same energy spectra Q  (pp) (E) – practically same energy spectra Q (pp) ~ 1 Q  (pp) (4E ) ~ E -s Q (pp) ~ 1 Q  (pp) (4E ) ~ E -s d  /  dE  = ∫ Q dr over spatial extent of the source d  /  dE  = ∫ Q dr over spatial extent of the source

5. 17.05.2004 Reso Shanidze 5 Atmospheric flux CR spectra: dN/dE = a E - CR spectra: dN/dE = a E - =2.7 (knee ~10 15 -10 16 eV) =2.7 (knee ~10 15 -10 16 eV) Hydrogen(0,9) He(0.08), … Hydrogen(0,9) He(0.08), … p(He) + A   +X p(He) + A   +X   exp(- h/h 0 )  h 0 =8.4km   exp(- h/h 0 )  h 0 =8.4km Earth atmosphere : 1030 g/cm -2 Earth atmosphere : 1030 g/cm -2   A (  KA  116 (138) gm/ cm -2   A (  KA  116 (138) gm/ cm -2 Int./decay(GeV): 115(850) Int./decay(GeV): 115(850) change of 2.7  3.7 change of 2.7  3.7 Secant theta effect Secant theta effect

6. 17.05.2004 Reso Shanidze 6 Atmospheric  flux CR interaction and propagation: CR interaction and propagation: MC codes: AIRES, COSMOS, MOCCA, HEMAS, CORSIKA MC codes: AIRES, COSMOS, MOCCA, HEMAS, CORSIKA CORSICA physics models: CORSICA physics models: VENUS, QGSJET, DPMJET, VENUS, QGSJET, DPMJET, SYBILL, HDPM. SYBILL, HDPM. Experimental Data: Experimental Data: - Underground experiments: - Underground experiments: MACRO, Frejus, L3C, … MACRO, Frejus, L3C, … - NT data: - NT data: Baikal, AMANDA Baikal, AMANDA

7. 17.05.2004 Reso Shanidze 7 Prompt  flux p() + N  C + X p() + N  C + X C – charmed particles C – charmed particles M.Thunman et al., Astropart. Phys. 5(1996), 309 M.Thunman et al., Astropart. Phys. 5(1996), 309 (hep-ph/9505417) (hep-ph/9505417)

8. 17.05.2004 Reso Shanidze 8 Waxman-Bahcal Bound: High energy from astrophysical sources Waxman-Bahcal Bound: High energy from astrophysical sources E.Waxman,J.Bahcall PRD, v59(1998), 023003E.Waxman,J.Bahcall PRD, v59(1998), 023003 Based on observations of Fly‘s Eye and AGASABased on observations of Fly‘s Eye and AGASA Cosmological origin of CR above 10 19 GeVCosmological origin of CR above 10 19 GeV ( E.Waxman, astro-ph/9508037 ) ( E.Waxman, astro-ph/9508037 ) Cosmological distribution of CR sources:Cosmological distribution of CR sources: dN/dE ~ E -   2 dN/dE ~ E -   2 Energy production rate ~ 5x10 44 erg Mpc -3 yr -1Energy production rate ~ 5x10 44 erg Mpc -3 yr -1 E 2  < 2 x 10 -8 GeV/cm 2 s srE 2  < 2 x 10 -8 GeV/cm 2 s sr

9. 17.05.2004 Reso Shanidze 9 Cosmogenic (GZK) Flux Photopion production by Photopion production by UHECR (E>10 19 GeV) : UHECR (E>10 19 GeV) :  + p    N  n   + p    N  n  CMB : 2.7K, ~400  /cm 3, E ~ meV. CMB : 2.7K, ~400  /cm 3, E ~ meV. IR: 1-2  cm 3, E ~ eV. IR: 1-2  cm 3, E ~ eV. (T.Stanev, astro-ph/0404535) (T.Stanev, astro-ph/0404535) 

10. 17.05.2004 Reso Shanidze 10 High Energy from the Sun Sun as a standard - candle ? High Energy from the Sun Sun as a standard - candle ? G. Ingelman, M. Thunman Phys. Rev. D 54(1996), 4385 G. Ingelman, M. Thunman Phys. Rev. D 54(1996), 4385 Calculations with LUND MC: Calculations with LUND MC: PYTHIA(v5.7) /JETSET(7.4) PYTHIA(v5.7) /JETSET(7.4) CR flux: (aE - interaction With the Sun atmosphere Rate of  events integrated over the Sun solid angle. Rate of  events integrated over the Sun solid angle. for NT (E > 100 GeV): for NT (E > 100 GeV): 1 event /yr ~6x10 4 m 2 

11. 17.05.2004 Reso Shanidze 11 High Energy Detectors High Energy Detectors

12. 17.05.2004 Reso Shanidze 12 The Baikal NT First telescope First telescope 1.1 km depth 1.1 km depth NT-36, 96, 192 NT-36, 96, 192 140 m

13. 17.05.2004 Reso Shanidze 13 Results from BAIKAL Results from BAIKAL 34 events of upward  34 events of upward  astro-ph/0404096 astro-ph/0404096 Search for bright cascades Search for bright cascades E -2, e     =1:1:1 E -2, e     =1:1:1 90% C.L. limit  E 2 : 90% C.L. limit  E 2 : 1.3x10 -6 cm -2 s -1 sr -1 GeV 1.3x10 -6 cm -2 s -1 sr -1 GeV

14. 17.05.2004 Reso Shanidze 14 AMANDA Detector Antarctic Muon And Neutrino Detector Array AMANDA Detector Antarctic Muon And Neutrino Detector Array AMANDA (ice): 1150-2350m B10 (97-99): 10 strings, 302 OM II (2000): 19 strings 677 OM

15. 17.05.2004 Reso Shanidze 15 AMANDA Results (  flux) AMANDA B10: 1977 AMANDA B10: 1977 measurement: measurement: Coverage - 2 Coverage - 2  ang. ~ 2 o -2.5 o  logE ~ 0.3-0.4 6 < E < 1000 TeV 6 < E < 1000 TeV PRL 90(2003) 2151101-1 PRL 90(2003) 2151101-1 E -2, e     =1:1:1 E -2, e     =1:1:1 E 2 (E) < E 2 (E) < 8.4x10 -7 GeV /cm 2 s sr

16. 17.05.2004 Reso Shanidze 16 AMANDA Results (cascades) cascades: cascades: Coverage - 4 Coverage - 4  ang. ~ 30 o -40 o  logE ~ 0.1-0.2 Astro-ph/0405218 Astro-ph/0405218 197 d, MC: 920 d 197 d, MC: 920 d 50 TeV<E<5 PeV 50 TeV<E<5 PeV E -2, e     =1:1:1 E -2, e     =1:1:1 E 2 (E) < E 2 (E) < 8.6x10 -7 GeV /cm 2 s sr

17. 17.05.2004 Reso Shanidze 17 Acoustic Detection of UHE Acoustic Detection of UHE Astro-ph/0406105 Astro-ph/0406105 SAUND detector: ~ 250 km2 (US Navy array) - only 7 used. SAUND detector: ~ 250 km2 (US Navy array) - only 7 used. ~1600 m undersea ~1600 m undersea 147 days of running (2002) 147 days of running (2002) Calibration, analysis Calibration, analysis -Energy, position -Energy, position - Rates, reconstraction - Rates, reconstraction

18. 17.05.2004 Reso Shanidze 18 IceCube 1400 m 2400 m AMANDA South Pole IceTop - 80 Strings - 4800 PMT - Instrumented volume: 1 km 3 - Installation: 2004-2010 2004-2010 ~ 80.000 atm. per year

19. 10/7/2003 C.Spiering, VLVNT Workshop Search for diffuse excess of extra-terrestrial high energy muon neutrinos  bound WB bound log E /GeV DUMANDFREJUSMACRO Muons in Amanda-B10 (1997)Expectation Amanda-II, 3 yearsExpectation IceCube, 3 years

20. 17.05.2004 Reso Shanidze 20 RICEAGASA Amanda, Baikal 2002 2004 2007 AUGER  Anita AABN 2012 km 3 EUSO Auger Salsa GLUE

21. 17.05.2004 Reso Shanidze 21 Sumary and Outlook High energy astronomy: High energy astronomy: Data from Baika(lake), AMANDA(ice) Data from Baika(lake), AMANDA(ice) New undersea NT: ANTARES, NESTOR New undersea NT: ANTARES, NESTOR Sensitivity to the cosmic diffuse flux Sensitivity to the cosmic diffuse flux NT on km3 scale: IceCube, KM3NeT NT on km3 scale: IceCube, KM3NeT Acoustic and other technique (RICE, ANITA, EUSO, GLUE) for UHE. Acoustic and other technique (RICE, ANITA, EUSO, GLUE) for UHE.