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High Energy Neutrino Astronomy from infancy to maturity

. A. High Energy Neutrino Astronomy from infancy to maturity. LAUNCH Meeting Heidelberg Christian Spiering DESY. . A. High Energy Neutrino Astronomy from infancy to maturity. technological. . A. The idea. Bruno Pontecorvo. Moisej Markov. M.Markov, 1960 :

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High Energy Neutrino Astronomy from infancy to maturity

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  1. A High Energy Neutrino Astronomyfrom infancy to maturity LAUNCH Meeting Heidelberg Christian Spiering DESY

  2. A High Energy Neutrino Astronomyfrom infancy to maturity technological

  3. A The idea Bruno Pontecorvo Moisej Markov 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

  4. The detection principle muon tracks cascades

  5. Why neutrinos ? • Travel straight(in contrast to CR) • Are not absorbed by IR or CMB(in contrast to gammas and CR) • Clear signature of hadronic nature or e :  :  ~ 1:2:0 changes to (typically) 1:1:1 at Earth

  6. Challenges • Low interaction cross section • Need huge detection volumes • Actual neutrino flux depends on target thickness • Predictions 25 years ago have been up to two orders of magnitude higher than today • 1990s: recognize need of cubic kilometer detectors • Now: cubic kilometer detectors will possibly just scratch the interesting range Martin Harwitt: „Would one have believed the timid predictions of theoreticians, X-ray astronomy would likely have started only a decade later.“

  7. Pioneering DUMAND ~ 1975: first meetings towards an underwater array close to Hawaii Test string 1987 Proposal 1988: The „Octagon“ (~ 1/3 AMANDA) Termination 1996

  8. 3600 m 1366 m NT-200 Pioneering Baikal • 1981 first site explorations • 1984 first stationary string • 1993 first neutrino detector NT-36 • 1994 first atm. Neutrino separated • 1998 NT-200 finished Ice as natural deployment platform

  9. NT-200 NT-200 140 m cascades Pioneering Baikal • Detection of • high energy • cascades • outside the • instrumented • volume • Fence the • observation • volume with • a few PMTs • 4 times better sensitivity at high energies NT200+ A textbook neutrino 4-string stage (1996) NT200+ running since 2006

  10. AMANDA • 1990: first site studies at South Pole • 1993/94 shallow detectors in bubbly ice • 1997: 10 strings (AMANDA-B10) • 2000: AMANDA-II

  11. AMANDA Hot water drilling

  12. AMANDA Scattering depth bubbles dust AMANDA-II

  13. AMANDA AMANDA sykplot 2000-2003 3329 events below horizon more on point sources in the following talk nm + N  m + X

  14. South and North AMANDA & Baikal skyplot, galactic coordinates

  15. Parameters of neutrino telescopes Effective  area: • ~ 0.1 m² @ 10 TeV • ~ 1 m² @ 100 TeV • ~ 100 m² @ 100 TeV AMANDA, ANTARES IceCube Point source sensitivity: • AMANDA, ANTARES:~ 10-10 / (cm² s) above 1 TeV • IceCube: ~ 10-12 / (cm² s) above 1 TeV

  16. IceCube South Pole Station AMANDA Skiway Dark sector Geographic South Pole IceCube

  17. IceCube • 4800 Digital Optical Modules on 80 strings • 160 Ice-Cherenkov tank surface array (IceTop) • 1 km3 of instrumented Ice • Surrounding existing AMANDA detector

  18. Drill tower Hose reel Hot water supply IceTop Station (2 tanks) Less energy and more than twice as fast as old AMANDA drill

  19. … not always easy

  20. IceCube Drilling & Deployment

  21. Status 2007

  22. Cumulative Instrumented Volume • Graph shows cumulative km3·yr of exposure × volume • 1 km3·yr reached 2 years before detector is completed • Close to 4 km3·yr at the beginning of 2nd year of full array operation.

  23. The Mediterranean approach 2400m ANTARES 4100m 3400m NEMO NESTOR

  24. ANTARES Neutrino candidate from 5-string detector

  25. Physics from Baikal & AMANDA • Atmospheric neutrinos • Diffuse fluxes • Point sources  see talk of Elisa Resconi • Coincidences with GRB • Supernova Bursts & SNEWS • WIMP indirect detection • Magnetic monopoles • …. • ….

  26. Atmospheric neutrinos • Spectrum measured up to ~ 100 TeV

  27. Limit on diffuse extraterrestrial fluxes • Spectrum measured up to ~ 100 TeV • From this method and one year data we exclude E-2 fluxes with E2 > 2.710-7 GeV sr-1 s-1 cm-2

  28. Limit on diffuse extraterrestrial fluxes • Spectrum measured up to ~ 100 TeV • From this method and one year data we exclude E-2 fluxes with E2 > 2.710-7 GeV sr-1 s-1 cm-2 • With 4 years and improved methods we are now at E2 > 8.810-8 GeV sr-1 s-1 cm-2

  29. Experimental limits & theoretical bounds • MPR bound, no neutron escape (gamma bound) • Factor 11 below MPR bound for sources opaque to neutrons

  30. Experimental limits & theoretical bounds • MPR bound, neutrons escape (CR bound) • Factor 4 below MPR bound for sources transparent to neutrons

  31. Experimental limits & theoretical bounds AGN core (SS) AGN Jet (MPR) GZK GRB (WB)

  32. Experimental limits & theoretical bounds old version AGN core (SS) „old“ Stecker model excluded

  33. Experimental limits & theoretical bounds AGN core (SS, new version) „new“ Stecker model not excluded (MRF = 1.9)

  34. Experimental limits & theoretical bounds AGN Jet (MPR) still above AGN jet (MPR) (MRF ~ 2.3) GRB (WB)

  35. Limit on diffuse extraterrestrial fluxes AMANDA HE analysis Baikal IceCube muons, 1 year Icecube, muons & cascades 4 years GRB (WB)

  36. Coincidences with GRB • Check for • coincidences with • BATSE • IPN • SWIFT Hughey et al., astro-ph/0611597 73 bursts 408 bursts With IceCube: test WB within a few months 407 bursts

  37. Detection of Supernova Bursts • ice uniformly illuminated • detect correlated rate increase on top of PMT noise Dark noise in AMANDA only ~ 500 Hz ! SN neutrino signal simulation center of galaxy, normalized to SN1987A

  38. Participation in SNEWS …several hours advanced notice to astronomers Super-K SNO coincidence server @ BNL alert LVD AMANDA (IceCube) IceCube will follow this year http://snews.bnl.gov and astro-ph/0406214

  39. Supernova in IceCube 5 signal for SN of 1987A strength Dark noise in IceCube Optical Modules is only ~ 250 Hz !

  40. Summary • tremendous technological progress over last decade (Baikal, South Pole, now also Mediterrannean) • no positive detection yet, but already testing realistic models/bounds • IceCube reaches 1 km3 year by the end of 2008 • entering region with realistic discovery potential • IceCube discoveries/non-discoveries will influence design of KM3NeT

  41. Events from IC9 • Left: upward muon • Right: IceTop/IceCube event

  42. Back-ups

  43. WIMPs:neutrinos from center of Earth  Assumptions:  Dark matter in Galaxy due to neutralinos  Density ~ 0.3 GeV/cm3  +   b + b C +  + 

  44. WIMPs:neutrinos from center of Earth

  45. WIMPs:neutrinos from Sun    Amanda

  46. WIMPs:neutrinos from Sun

  47. Relativistic Magnetic Monopoles 10-14 Soudan KGF Cherenkov-Light  n2·(g/e)2 Amanda 10-15 MACRO Orito upper limit (cm-2 s-1 sr-1) n = 1.33 (g/e) = 137/ 2 10-16 Baikal  electrons 10-17  8300 IceCube 10-18 0.50 0.75 1.00  = v/c

  48. Angular resolution Effective Area for Muons Galactic center *Studies based on simpler reconstructions waveform information will improve Icecube Performance: muons Muon neutrino

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