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Neutrino astronomy with AMANDA and IceCube Per Olof Hulth Stockholm University [email protected] Short summary of neutrinos for pedestrians There are three different “families” of leptons Electron neutrino (e) and the electron (e-) Muon neutrino () and the muon (-) Tau neutrino () and the tau (-) The neutrinos penetrates huge amount of matter without being absorbed 02-10-31 E.g. a 1 MeV neutrino from the sun has an absorption length of 20 light years in lead!! 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*1038) neutrinos At Earth we receive about 40.000.000.000 neutrinos/cm2/second From Big Bang we have 330 000 000 neutrinos/m3 (Energi 0.0004 eV) but only half a proton 340 000 000 neutrinos are creataed in our body every day (40K) 02-10-31 Per Olof Hulth Stockholm university Neutrinos from Supernova When a star explodes 99% of the energy is emitted in neutrinos A star exploded 1054. Today the Crab nebula 02-10-31 Per Olof Hulth Stockholm university Gamma astronomy Backgnd e e - Space is not transparent for High Energy Photons! R. Svensson Zdziarski AA.Ap.J.349:415-28(1990) 02-10-31 Per Olof Hulth Kneiski TM, Mannerheim K, Hartmann D.Ap.J. Submitted 2000) Stockholm university Three open questions in Astrophysics What is the missing dark matter in the Universe? What is the origin of the Highest Energy Cosmic rays? What is powering the Gamma Ray Bursts (GRB)? 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 !!!! 02-10-31 Per Olof Hulth Stockholm university Most popular model New type of matter (WIMPs) Supersymmetric particles from Big Bang Neutralinos. 02-10-31 Per Olof Hulth Stockholm university WIMPs from Sun/Earth Dark Matter search Look for excess of neutrinos from centre of the Earth and the Sun!! 02-10-31 Per Olof Hulth Stockholm university Cosmic rays mesoner muons About 100 muons/m2sek 02-10-31 Per Olof Hulth Stockholm university Cosmic rays Energies up to 50 Joules! What is the process creating these particles??? 02-10-31 Per Olof Hulth Stockholm university A possible candidate for a source for cosmic rays 02-10-31 Per Olof Hulth Stockholm university Gamma Ray Bursts Source 9 Billion light years away! The sources of GRBs on cosmologic distances! The most “violent” objects in the Universe 02-10-31 Per Olof Hulth Stockholm university Gamma Ray Bursts Could be danger to be too close… 02-10-31 Per Olof Hulth Stockholm university Messengers of Astronomy Only neutrinos cover the whole energy range 02-10-31 Per Olof Hulth Stockholm university Neutrino production p p 0 p 2 n n e e If protons are accelerated we expect about equal amount of gammas and neutrino!! 02-10-31 Per Olof Hulth Stockholm university Classes of Models log(E2 Flux) pp core AGN p blazar jet Top-Bottom model Various recent models for transient sources GRB (W&B) 02-10-31 3 6 9 TeV PeV EeV Per Olof Hulth Stockholm university log(E/GeV) Neutrino astronomy so far Only two neutrino sources in space has been observed. The solar neutrinos (Nobel price 2002) Neutrinos from SN1987 in the Large Magellanic Cloud (180 000 light years) Energy of neutrinos only 1-30 MeV 02-10-31 Per Olof Hulth Stockholm university Neutrino physics (again) We have three types of neutrinos: e Electron neutrino Muon neutrino Tau neutrinon E.g. Neutron decay : neutron -> proton + e- + e 02-10-31 Per Olof Hulth Stockholm university Neutrino interaction < 1 degree The muon can travel several km in e.g. ice 02-10-31 Per Olof Hulth Stockholm university Cherenkov radiation A charged particle moving with the speed of light in the medium will generate a shock wave of light q cosq=1/(nb) b=v/c, n= refraction index 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 40K 02-10-31 Per Olof Hulth Stockholm university AMANDA 02-10-31 Per Olof Hulth Stockholm university South Pole 02-10-31 Per Olof Hulth Stockholm university 02-10-31 Per Olof Hulth Stockholm university 02-10-31 Per Olof Hulth Stockholm university Joakim Edsjö SU 02-10-31 Per Olof Hulth Stockholm university Joakim Edsjö SU 02-10-31 Per Olof Hulth Stockholm university 106 muons from cosmic rays/muon from neutrinos !!!! Select only muons from below!!!! 02-10-31 Per Olof Hulth Stockholm university Hot water heaters -50 m -55 C -2400 m 02-10-31 Per Olof Hulth -25 C Stockholm university 02-10-31 Per Olof Hulth Stockholm university Joakim Edsjö SU 02-10-31 Per Olof Hulth Stockholm university -840 m 02-10-31 Per Olof Hulth Stockholm university AMANDA Year Detector 1995/1996 AMANDA-B4 Total number of OM 86 1996/1997 AMANDA-B10 302 1998/1999 AMANDA-B13 428 1999/2000 680 02-10-31 AMANDA-II Per Olof Hulth Stockholm university 02-10-31 Per Olof Hulth Stockholm university DATA AMANDA Event Signatures: Muons CC muon neutrino interactions Muon tracks 02-10-31 + N + X Per Olof Hulth Stockholm university 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. Equatorial coordinates: declination vs. right ascension. 02-10-31 Per Olof Hulth Stockholm university AMANDA B10 and A-II: cm-2 s-1 some limits and projected sensitivity 10-13 10 AMANDA B10 average Sensitivity for sel. soruces To appear in ApJ: astro-ph/0208006 -14 A-II, limit on SS433 A-II, sensitivity on SS433 MACRO 10-15 SS433* A-II projected sensitivity Combined 97-02 -90 -45 0 A-II, limit on Mrk 501 45 Declination (deg) 02-10-31 Per Olof Hulth Stockholm university 90 Mrk501 (HEGRA 97, /=1) 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 02-10-31 Per Olof Hulth Stockholm university IceCube!! 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 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 Olof Hulth 02-10-31 24. Utrecht, Holland (since 29th ofPer October 2002) Stockholm university IceCube:Top View Grid North 100 m AMANDA 80 strings 60 modules/string Volume 1 km3 Depth 1400-2400 m Counting House South Pole SPASE-2 Dome Skiway 02-10-31 Per Olof Hulth Stockholm university IceTop AMANDA South Pole Skiway IceCube 80 Strings 4800 PMT 1400 m 2400 m 02-10-31 Per Olof Hulth Stockholm university - flavors and energy ranges Neutrino flavor Filled area: particle id, angle, energy Shaded area: energy and angle. e e 6 02-10-31 Per Olof Hulth 9 12 15 18 Log(ENERGY/eV) Stockholm university 21 µ-events in IceCube Eµ=10 TeV Eµ=6 PeV AMANDA-II 1 km 02-10-31 Measure energy by counting the number of fired PMT. Olof Hulth Stockholm university (This is a veryPersimple but robust method) Diffuse Fluxes: Predictions and Limits Mannheim & Learned, 2000 Macro Baikal Amanda IceCube 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) Compare to Mrk 501 gamma rays Field of view: Continuous 2 sr AMANDA B10 (northern sky) prelim. limit Sensitivity of 3 years of IceCube 02-10-31 Per Olof Hulth Stockholm university Neutrinos from Gamma Ray Bursts 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) Only 200 GRB needed to detect/rule out WB99 flux 02-10-31 Per Olof Hulth Stockholm university Cascade event e + N --> e- + X 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 Sensitivity for diffused flux about the same as for muons Per Olof Hulth Stockholm university 02-10-31 E = 375 TeV “Double Bang” + N --> - + X + X • E << 1 PeV: Single cascade (2 cascades coincide) • E ≈ 1 PeV: Double bang • E >> 1 PeV: Second cascade + tau track 02-10-31 Per Olof Hulth Stockholm university Tau neutrinos and oscillations Enhanced role of tau neutrinos because of neutrino oscillation!? Cosmic beam: e = µ = because of oscillations not absorbed by the Earth (regeneration) Pile-Up near 1 PeV where ideal sensitivity IceCube sensitive to m2>10-17 eV2 02-10-31 Per Olof Hulth Stockholm university Dark matter detection with IceCube WIMPS from Earth WIMPS from Sun Ice3 will significantly improve the sensitivity! 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 AMANDA IceCube In addition to the MeV e neutrinos, 10-100 muon neutrinos are expected after a few hours in the TeV energy range. 02-10-31 Per Olof Hulth Stockholm university Summary IceCube will open a significant new window on the Universe. Hopefully we will observe something which has not been discussed in this presentation. 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 02-10-31 Per Olof Hulth QuickTime™ and a Photo - JPEG decompressor are needed to see this picture. Stockholm university Optical sensor Installation of one sensor: ≈10 min 02-10-31 QuickTime™ and a Photo - JPEG decompressor are needed to see this picture. Per Olof Hulth Stockholm university 02-10-31 Per Olof Hulth Stockholm university Mats Pettersson Gymnasielärare från Angereds gymnasium Göteborg vid sydpolen 14 november 2001 02-10-31 Per Olof Hulth Stockholm university 02-10-31 Per Olof Hulth Stockholm university 02-10-31 Per Olof Hulth Stockholm university Joakim Edsjö SU Joakim Edsjö SU 02-10-31 Per Olof Hulth Stockholm university 02-10-31 Per Olof Hulth Stockholm university Joakim Edsjö SU 02-10-31 Per Olof Hulth Stockholm university