1. Neutrino astronomy with AMANDA and IceCube Per Olof Hulth Stockholm University hulth@physto.se

2. 02-10-31 Per Olof Hulth Stockholm university Content Introduction Introduction AMANDA results AMANDA results IceCube expectations IceCube expectations Summary Summary

3. 02-10-31 Per Olof Hulth Stockholm university Short summary of neutrinos for pedestrians There are three different “families” of leptons There are three different “families” of leptons Electron neutrino ( e ) and the electron (e - ) Electron neutrino ( e ) and the electron (e - ) Muon neutrino (  ) and the muon    Muon neutrino (  ) and the muon    Tau neutrino (  ) and the tau    Tau neutrino (  ) and the tau    The neutrinos penetrates huge amount of matter without being absorbed The neutrinos penetrates huge amount of matter without being absorbed E.g. a 1 MeV neutrino from the sun has an absorption length of 20 light years in lead!! E.g. a 1 MeV neutrino from the sun has an absorption length of 20 light years in lead!!

4. 02-10-31 Per Olof Hulth Stockholm university Some neutrino numbers The Sun sends every second out 200.000.000.000.000.000.000.000.000.000.000.000.000 (2*10 38 ) neutrinos The Sun sends every second out 200.000.000.000.000.000.000.000.000.000.000.000.000 (2*10 38 ) neutrinos At Earth we receive about 40.000.000.000 neutrinos/cm 2 /second At Earth we receive about 40.000.000.000 neutrinos/cm 2 /second From Big Bang we have 330 000 000 neutrinos/m 3 (Energi 0.0004 eV) but only half a proton From Big Bang we have 330 000 000 neutrinos/m 3 (Energi 0.0004 eV) but only half a proton 340 000 000 neutrinos are creataed in our body every day ( 40 K) 340 000 000 neutrinos are creataed in our body every day ( 40 K)

5. 02-10-31 Per Olof Hulth Stockholm university Neutrinos from Supernova When a star explodes 99% of the energy is emitted in neutrinos When a star explodes 99% of the energy is emitted in neutrinos A star exploded 1054. Today the Crab nebula A star exploded 1054. Today the Crab nebula

6. 02-10-31 Per Olof Hulth Stockholm university R. Svensson Zdziarski AA.Ap.J.349:415-28(1990) Kneiski TM, Mannerheim K, Hartmann D.Ap.J. Submitted 2000) Gamma astronomy Space is not transparent for High Energy Photons!

7. 02-10-31 Per Olof Hulth Stockholm university Three open questions in Astrophysics What is the missing dark matter in the Universe? What is the missing dark matter in the Universe? What is the origin of the Highest Energy Cosmic rays? What is the origin of the Highest Energy Cosmic rays? What is powering the Gamma Ray Bursts (GRB)? What is powering the Gamma Ray Bursts (GRB)?

8. 02-10-31 Per Olof Hulth Stockholm university You need 20 times more matter to keep the system together than what is observed DARK MATTER !!!!

9. 02-10-31 Per Olof Hulth Stockholm university Most popular model New type of matter (WIMPs) New type of matter (WIMPs) Supersymmetric particles from Big Bang Supersymmetric particles from Big Bang Neutralinos. Neutralinos.

10. 02-10-31 Per Olof Hulth Stockholm university WIMPs from Sun/Earth Look for excess of neutrinos from centre of the Earth and the Sun!! Dark Matter search

11. 02-10-31 Per Olof Hulth Stockholm university Cosmic rays About 100 muons/m 2 sek proton muons mesoner

12. 02-10-31 Per Olof Hulth Stockholm university Cosmic rays Energies up to 50 Joules! What is the process creating these particles???

13. 02-10-31 Per Olof Hulth Stockholm university A possible candidate for a source for cosmic rays

14. 02-10-31 Per Olof Hulth Stockholm university Gamma Ray Bursts The sources of GRBs on cosmologic distances! The most “violent” objects in the Universe Source 9 Billion light years away!

15. 02-10-31 Per Olof Hulth Stockholm university Gamma Ray Bursts Could be danger to be too close… Could be danger to be too close…

16. 02-10-31 Per Olof Hulth Stockholm university Messengers of Astronomy Only neutrinos cover the whole energy range

17. 02-10-31 Per Olof Hulth Stockholm university Neutrino production If protons are accelerated we expect about equal amount of gammas and neutrino!!

18. 02-10-31 Per Olof Hulth Stockholm university log(E 2  Flux) log(E/GeV) TeV PeV EeV 3 6 9 pp core AGN p  blazar jet Top-Bottom model GRB (W&B) Various recent models for transient sources Classes of Models

19. 02-10-31 Per Olof Hulth Stockholm university Neutrino astronomy so far Only two neutrino sources in space has been observed. Only two neutrino sources in space has been observed. The solar neutrinos (Nobel price 2002) The solar neutrinos (Nobel price 2002) Neutrinos from SN1987 in the Large Magellanic Cloud (180 000 light years) Neutrinos from SN1987 in the Large Magellanic Cloud (180 000 light years) Energy of neutrinos only 1-30 MeV Energy of neutrinos only 1-30 MeV

20. 02-10-31 Per Olof Hulth Stockholm university Neutrino physics (again) We have three types of neutrinos: Electron neutrino  e Muon neutrino  Tau neutrinon  E.g. Neutron decay : neutron -> proton + e - + e

21. 02-10-31 Per Olof Hulth Stockholm university Neutrino interaction   The muon can travel several km in e.g. ice < 1 degree

22. 02-10-31 Per Olof Hulth Stockholm university Cherenkov radiation cos  n   v/c, n= refraction index  A charged particle moving with the speed of light in the medium will generate a shock wave of light

23. 02-10-31 Per Olof Hulth Stockholm university The AMANDA telescope at the South Pole Why the South Pole? A 3000 meter thick glaciar A scientific base with all infra structure No fishes and no 40 K

24. 02-10-31 Per Olof Hulth Stockholm university AMANDA

25. 02-10-31 Per Olof Hulth Stockholm university South Pole

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27. 02-10-31 Per Olof Hulth Stockholm university Joakim Edsjö SU

28. 02-10-31 Per Olof Hulth Stockholm university Joakim Edsjö SU

29. 02-10-31 Per Olof Hulth Stockholm university neutrino myon

30. 02-10-31 Per Olof Hulth Stockholm university neutrino myon 10 6 muons from cosmic rays/muon from neutrinos !!!! Select only muons from below!!!! Select only muons from below!!!!

31. 02-10-31 Per Olof Hulth Stockholm university Hot water heaters -55 C -25 C -2400 m -50 m

32. 02-10-31 Per Olof Hulth Stockholm university Joakim Edsjö SU

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34. 02-10-31 Per Olof Hulth Stockholm university -840 m

35. 02-10-31 Per Olof Hulth Stockholm university AMANDA

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37. 02-10-31 Per Olof Hulth Stockholm university AMANDA Event Signatures: Muons CC muon neutrino interactions  Muon tracks  + N   + X DATA

38. 02-10-31 Per Olof Hulth Stockholm university Equatorial coordinates: declination vs. right ascension. Point Sources Amanda II (2000) Skyplot is scrambled in event time for blind analysis, Plot has been released, and results will be available soon. Examples for a few candidates will be given.

39. 02-10-31 Per Olof Hulth Stockholm university Point Sources Amanda II (2000) Source candidate looked at Mrk421Mrk501SS433Declination38.239.85.0 Right ascension 11.116.919.2   (E>10GeV,90% c.l.)/10 -15 cm -2 s -1 2.051.7110.52  (E>10GeV,90% c.l.)/10 -8 cm -2 s -1 1.281.063.49 Number of events (observed) 217 Number of events (background) 1.51.14.1 Muon sensitivity (as    1.721.806.05 Neutrino sensitivity (as   1.071.122.01    Limit on integrated E -2 muon flux above 10 GeV [10 -15 cm -2 s -1 ]    Limit on integrated E -2 neutrino flux [10 -8 cm -2 s -1 ] Results for three examples of possible sources:

40. 02-10-31 Per Olof Hulth Stockholm university Super-Kamiokande MACRO -90 0-45 9045 10 -15 10 -13 10 -14   cm -2 s -1 Declination (deg) AMANDA B10 and A-II : some limits and projected sensitivity SS433* Mrk501 (HEGRA 97,  ) A-II, sensitivity on SS433 A-II, limit on SS433 A-II, limit on Mrk 501 AMANDA B10 average Sensitivity for sel. soruces A-II projected sensitivity Combined 97-02 To appear in ApJ: astro-ph/0208006

41. 02-10-31 Per Olof Hulth Stockholm university AMANDA-II “Online analysis” 4.5 atmospheric  candidates / day The Stockholm model

42. 02-10-31 Per Olof Hulth Stockholm university Amanda Analysis activities AMANDA-B10 1997 analysis at the end AMANDA-B10 1999 analysis started AMANDA-II 2000 filtering done, first analyses started AMANDA-II 2001 online filtering continuously done In order to do a “blind analysis” only 20% of the data is used for tuning cuts

43. 02-10-31 Per Olof Hulth Stockholm university IceCube has been designed as a discovery instrument with improved : telescope area detection volume energy measurement of secondary muons and electromagnetic showers identification of neutrino flavor angular resolution IceCube!!

44. 02-10-31 Per Olof Hulth Stockholm university The IceCube Collaboration Institutions: 11 US and 8 European institutions Bartol Research Institute, University of Delaware BUGH Wuppertal, Germany Universite Libre de Bruxelles, Brussels, Belgium CTSPS, Clark-Atlanta University, Atlanta USA DESY-Zeuthen, Zeuthen, Germany Institute for Advanced Study, Princeton, USA Lawrence Berkeley National Laboratory, Berkeley, USA Department of Physics, Southern University and A\&M College, Baton Rouge, LA, USA Dept. of Physics, UC Berkeley, USA Institute of Physics, University of Mainz, Mainz, Germany Dept. of Physics, University of Maryland, USA University of Mons-Hainaut, Mons, Belgium Dept. of Physics and Astronomy, University of Pennsylvania, Philadelphia, USA Dept. of Astronomy, Dept. of Physics, SSEC, University of Wisconsin, Madison, USA Physics Department, University of Wisconsin, River Falls, USA Division of High Energy Physics, Uppsala University, Uppsala, Sweden Dept. of Physics, SCFAB, Stockholm University, Stockholm, Sweden University of Alabama Vrije Universiteit Brussel, Brussel, Belgium Also AMANDA only IceCube Spokesperson: P.O.Hulth Stockholm University Co-spokesperson: F.Halzen University of Wisconsin

45. 02-10-31 Per Olof Hulth Stockholm university The IceCube Collaboration 11 European, 1 Japanese, 1 South American and 11 US Institutions (many of them are also AMANDA member institutions) 1. Bartol Research Institute, University of Delaware, Newark, USA 2. BUGH Wuppertal, Germany 3. Universite Libre de Bruxelles, Brussels, Belgium 4. Dept. of Physics, Chiba University, Japan 5. CTSPS, Clark-Atlanta University, Atlanta USA 6. DESY-Zeuthen, Zeuthen, Germany 7. Imperial College, London, UK 8. Institute for Advanced Study, Princeton, USA 9. Dept. of Technology, Kalmar University, Kalmar, Sweden 10. Lawrence Berkeley National Laboratory, Berkeley, USA 11. Dept. of Physics, Southern University and A\&M College, Baton Rouge, LA, USA 12. Dept. of Physics, UC Berkeley, USA 13. Institute of Physics, University of Mainz, Mainz, Germany 14. Dept. of Physics, University of Maryland, USA 15. University of Mons-Hainaut, Mons, Belgium 16. Dept. of Physics, Pennsylvania State University, University Park, PA, USA 17. Dept. of Physics, Simon Bolivar University, Caracas, Venezuela 18. Dept. of Astronomy, Dept. of Physics, SSEC, University of Wisconsin, Madison, USA 19. Physics Dept., University of Wisconsin, River Falls, USA 20. Division of High Energy Physics, Uppsala University, Uppsala, Sweden 21. Fysikum, Stockholm University, Stockholm, Sweden 22. Dept. of Physics, University of Alabama, Tuscaloosa, USA 23. Vrije Universiteit Brussel, Brussel, Belgium 24.Utrecht, Holland (since 29th of October 2002)

46. 02-10-31 Per Olof Hulth Stockholm university IceCube:Top View AMANDA SPASE-2 South Pole Dome Skiway 100 m Grid North Counting House 80 strings 60 modules/string Volume 1 km 3 Depth 1400-2400 m

47. 02-10-31 Per Olof Hulth Stockholm university IceCube 80 Strings 4800 PMT 1400 m 2400 m AMANDA South Pole IceTop Skiway

48. 02-10-31 Per Olof Hulth Stockholm university - flavors and energy ranges Filled area: particle id, angle, energy Shaded area: energy and angle.

49. 02-10-31 Per Olof Hulth Stockholm university µ-events in IceCube 1 km E µ =10 TeV E µ =6 PeV AMANDA-II Measure energy by counting the number of fired PMT. (This is a very simple but robust method)

50. 02-10-31 Per Olof Hulth Stockholm university Sensitivity to diffuse  -fluxes Atmospheric neutrino flux (after quality cuts): 130.000 / year Signal: hard spectrum (E -2 ) Apply energy cut: ≥ 200 PMT signals (5 background events left) Sensitivity (3 yr): dN/dE ≤ 4.8 x 10 -9 * E -2 /(cm 2 sec GeV) Atmospheric E-2 flux True neutrino energyNumber fired PMT

51. 02-10-31 Per Olof Hulth Stockholm university 1 pp core AGN (Nellen) 2 p  core AGN Stecker & Salomon) 3 p  „maximum model“ (Mannheim et al.) 4 p  blazar jets (Mannh) 5 p  AGN (Rachen & Biermann) 6 pp AGN (Mannheim) 7 GRB (Waxman & Bahcall) 8 TD (Sigl) Mannheim & Learned, 2000 Macro Baikal IceCube Amanda Diffuse Fluxes: Predictions and Limits

52. 02-10-31 Per Olof Hulth Stockholm university Point source sensitivity

53. 02-10-31 Per Olof Hulth Stockholm university Compare to Mrk 501 gamma rays Sensitivity of 3 years of IceCube Field of view: Continuous 2  sr (northern sky) AMANDA B10 prelim. limit

54. 02-10-31 Per Olof Hulth Stockholm university Only 200 GRB needed to detect/rule out WB99 flux Test signal: 1000 GRB a la Waxman/Bahcall 1999 Expected no. of events: 11 upgoing muon events Expected background: 0.05 events Sensitivity (1000 bursts): 0.2  dN/dE (Waxman/Bahcall 99) Neutrinos from Gamma Ray Bursts

55. 02-10-31 Per Olof Hulth Stockholm university Cascade event E = 375 TeV The length of the actual cascade, ≈ 10 m, is small compared to the spacing of sensors 1 PeV ≈ 500 m diameter Fully active calorimeter with linear energy resolution e + N --> e - + X Sensitivity for diffused flux about the same as for muons

56. 02-10-31 Per Olof Hulth Stockholm university  + N -->  - + X  + X E << 1 PeV: Single cascade (2 cascades coincide) E ≈ 1 PeV: Double bang E >> 1 PeV: Second cascade + tau track “Double Bang”

57. 02-10-31 Per Olof Hulth Stockholm university Cosmic beam: e = µ =  because of oscillations  not absorbed by the Earth (regeneration) Pile-Up near 1 PeV where ideal sensitivity IceCube sensitive to  m 2 >10 -17 eV 2 Enhanced role of tau neutrinos because of neutrino oscillation!? Tau neutrinos and oscillations

58. 02-10-31 Per Olof Hulth Stockholm university Dark matter detection with IceCube Ice 3 will significantly improve the sensitivity! WIMPS from EarthWIMPS from Sun

59. 02-10-31 Per Olof Hulth Stockholm university Supernova detection e + p n + e + (10-40 MeV) PMT noise increase due to the positrons AMANDA/IceCube records the noise of the PMTs over 0.5 sec and summing up total rate over 10 sec intervals. Detectors to be connected to Supernova Early Warning System In addition to the MeV e neutrinos, 10-100 muon neutrinos are expected after a few hours in the TeV energy range. AMANDA IceCube

60. 02-10-31 Per Olof Hulth Stockholm university IceCube deployment schedule

61. 02-10-31 Per Olof Hulth Stockholm university Summary IceCube will open a significant new window on the Universe. IceCube will open a significant new window on the Universe. Hopefully we will observe something which has not been discussed in this presentation. Hopefully we will observe something which has not been discussed in this presentation.

62. 02-10-31 Per Olof Hulth Stockholm university Hotwater Drilling Experience with AMANDA: 19 holes Upgrade:from 2 to  5 MW Projected time to 2450 m depth: 40 h Diameter: 50 cm Drill 2 holes per week; 16 holes per season

63. 02-10-31 Per Olof Hulth Stockholm university Optical sensor Installation of one sensor: ≈10 min

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65. 02-10-31 Per Olof Hulth Stockholm university Mats Pettersson Gymnasielärare från Angereds gymnasium Göteborg vid sydpolen 14 november 2001

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67. 02-10-31 Per Olof Hulth Stockholm university Joakim Edsjö SU

68. 02-10-31 Per Olof Hulth Stockholm university Joakim Edsjö SU

69. 02-10-31 Per Olof Hulth Stockholm university Joakim Edsjö SU

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