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The Long March Towards High Energy Neutrino Astronomy

The Long March Towards High Energy Neutrino Astronomy. C. Spiering, Leeds, July 23, 2004. Entrance to the Promised Land after 40 Years !. Moisej Markov. Bruno Pontecorvo. M.Markov, 1960 : We propose to install detectors deep in a lake or in the sea and to determine the direction of

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The Long March Towards High Energy Neutrino Astronomy

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  1. The Long March Towards High Energy Neutrino Astronomy C. Spiering, Leeds, July 23, 2004

  2. Entrance to the Promised Land after 40 Years !

  3. Moisej Markov Bruno Pontecorvo M.Markov,1960: We propose to install detectors deep in a lake or in the sea and to determine the direction of charged particles with the help of Cherenkov radiation

  5. Pioneering DUMAND Fred Reines John Learned + Roberts, Stenger, Gorham, .. ~ 1975: first meetings towards an underwater array close to Hawaii

  6. DUMAND-II Proposal 1988 : - 216 PMTs at 9 strings - height 230 m Alas ! ... terminated in 1996

  7. Later used by Amanda and Baikal 1987: DUMAND test string

  8. DUMAND FREJUS  bound MACRO WB bound Search for diffuse excess of extra-terrestrial high energy neutrinos log E /GeV

  9. Neutrino Telescopes Underground KGF Baksan FREJUS IMB Kamiokande Superkamiokande MACRO e.g. MACRO, 1356 upgoing muons ~ 1000 m²

  10. Pioneering BAIKAL Bezrukov, Domogatsky Berezinsky, Zatsepin • 1981 first site explorations • 1984 first stationary string • first neutrino detector NT-36 • 1994 first atm. neutrino separated • 1998 NT-200 finished G. Domogatsky ~ 2x Super-K for 1 TeV muons

  11. Camp Ice as a natural deployment platform

  12. 3600 m 1366 m NT-200 4-string stage (1996)

  13. NT-200 Look for upward moving light fronts. Signal: isolated cascades from neutrino interactions Background: Bremsshowers from h.e. downward muons   large effective volume Baikal Search for H.E.Cascades

  14. NT-200 NT-200 140 m cascades Baikal Upgrade NT200+ 36 additional PMTs  4 times better sensitivity !

  15. Mediterannean approaches NESTOR (since 1991) „Amanda-sized“ -- under construction ANTARES(since 1996) „Amanda sized“ -- under construction NEMO: R&D for km3 project Since 2003: joined km3 initiative KM3NET

  16. 2400m ANTARES 4100m 3400m NEMO NESTOR

  17. Beyond the DUMAND scale: AMANDA first site studies at South Pole ~ 1990 shallow detector in bubbly ice 1993/4 10 strings (Amanda-B10) 1997 19 strings (Amanda-II) 2000 Francis Halzen + Steve Barwick, Bob Morse, ....

  18. AMANDA Super-K DUMAND depth Amanda-II: 677 PMTs at 19 strings (1996-2000) AMANDA-II

  19. Ocean Water

  20. Drilling Hot water drilling

  21. AMANDA Event Signatures:Muons CC muon neutrino interaction  track nm + N  m + X

  22. AMANDA Event Signatures: Cascades • CC electron and tau neutrino interaction: • (e,,) + N  (e, ) + X • NC neutrino interaction: x + N  x + X Cascades

  23. Atmospheric Neutrinos

  24. First spectrum > 3 TeV: - up to 100 TeV - matches lower-energy Frejus data PRELIMINARY

  25. Search for Point Sources

  26. Skyplot Amanda-II, 2000 697 events below horizon above horizon: mostly fake events

  27. Intrinsic source spectrum (corrected for IR absorption) Measured  spectrum AMANDA average flux limit for two assumed spectral indices , compared to the average gamma flux of Markarian 501 as observed in 1997 by HEGRA. AMANDA-II has reached the sensitivity needed to search from neutrino fluxes from TeV gamma sources of similar strength to the instrinsic gamma flux.

  28. 90% C.L. upper limits (in units of 10-8cm-2s-1) for selected sources for an E-2 spectral shape integrated above Eν=10 GeV PRELIMINARY

  29. AMANDA skyplot 2000-2003 optimized for best sensitivity to E-3 – E-2 sources Preliminary 3369 events

  30. Preliminary

  31. Preliminary Cas A Mk501 Mk421 Cyg Crab M87 SS433

  32. Selected Source Analysis Stacking Source Analysis Galactic Plane Transient Sources Burst Search Correlation Analysis Multi-Pole Analysis Lower energy threshold (optimize to steeper spectra)

  33. SS-433 Mk-501 / ~ 1 -45 0 45 90 -90 Measured sensitivity 00-03 Expected sensitivity for AMANDA 97-03 m cm-2 s-1 southern sky northern sky 4 years Super-Kamiokande 170 days AMANDA-B10 10-14 230 days AMANDA-II 8 years MACRO 10-15 declination (degrees)

  34. Search for a Diffuse Extraterrestrial Flux

  35. DUMAND FREJUS  bound MACRO Amanda-II (2000) WB bound Expectation Amanda-II, 3 years Expectation IceCube, 3 years Experimental Limits Baikal (98,99,00) Amanda-B10 (1997), UHE Amanda-B10 (1997) Amanda-II (2000) cascades In red: only muons In blue: all flavors

  36.  bound  bound WB bound WB bound e:: = 1:2:0  1:1:1

  37.  bound  bound WB bound WB bound

  38. DUMAND FREJUS  bound  bound MACRO WB bound WB bound Expectation Amanda-II, 3 years Expectation IceCube, 3 years Experimental all-flavor limits Baikal (98,99,00) Amanda-B10 (1997) Amanda-B10 (1997), UHE Amanda-II (2000) Amanda-II (2000) cascades

  39. Search for neutrinos related to Gamma Ray Bursts

  40. -1 hour +1 hour 10 min Blinded Window Background determined on-source/off-time Background determined on-source/off-time t=0+1h Waxman/Bahcall 99 • Low background (due narrow time and space coincidence) • - Large effective areas (50 000 m² @ 1 PeV) Upper limit: 16 · Waxman/Bahcall flux

  41. Search for exotic particles

  42. Indirect Search for WIMPs Neutrinos from the Sun    Amanda At South Pole the Sun sinks maximally 23° below horizon. Therefore only Amanda-II with its dramatically improved reconstruction capabilities for horizontial tracks (compared to Amanda-B10) can be used for solar WIMP search.

  43. Present upper limits and expected IceCube sensitivity on muon flux from neutralino annihilations in center of Sun  Disfavored by direct search

  44. 10-14 10-15 10-16 10-17 10-18 0.50 0.75 1.00  = v/c Search for relativistic magneticmonopoles Soudan KGF Baikal-98,99,00 MACRO Orito upper limit (cm-2 s-1 sr-1) Cherenkov-Light  n2·(g/e)2 Amanda-97  electrons n = 1.33 (g/e) = 137/ 2 IceCube  8300

  45. Supernova Burst Monitor

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