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Baikal and Amanda: Neutrino-Astrophysics Collaboration

Learn about the Baikal and Amanda detectors and their contributions to neutrino astrophysics. Explore their history, current projects, and selected physics results. This collaboration aims to search for extraterrestrial point sources, study atmospheric neutrinos, and search for dark matter.

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Baikal and Amanda: Neutrino-Astrophysics Collaboration

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  1. Lake Baikal South Pole Neutrino-Astrophysics Baikal, Amanda, IceCube Christian Spiering, ESC DESY, Sept.2003

  2. 1.The present detectors Baikal and Amanda Christian Spiering

  3. The Baikal Collaboration Institute of Nuclear Research, Moscow Irkutsk State University, Irkutsk DESY Zeuthen, Zeuthen Moscow State University, Moscow Nishni Novgorod State Technical University State Marine Technical University, St.Petersburg Kurchatov Institute, Moscow JINR, Dubna since 1988 Christian Spiering

  4. Baikal History 93 94 95 96 97 98 99 00 01 02 03 04 > ----------------------------------------------------------------------- #OM 36 36 72 96 144 192 192 192 192 192 228 first 2 neutrino candidates NT-200+ NT-200 upgrade Baikal will likely stay largest H.E. neutrino telescope on northern hemisphere for another 2-3 years and nicely complement Amanda. One of the first neutrino events recorded with the 1996 four-string version of the Baikal Telescope

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

  6. The AMANDA Collaboration Bartol Research Institute UC Berkeley UC Iivine Pennsylvania State UW Madison UW River Falls LBL Berkeley U. Simón Bolivar, Caracas VUB, Brussel ULB-IHEE, Bruxelles U. de Mons-Hainaut Imperial College, London DESY, Zeuthen Mainz Universität Wuppertal Universität Stockholm Universitet Uppsala Universitet Kalmar Universitet South Pole Station Antarctica New Zealand Venezuela (1) Japan USA (7+3) Europe (10+1) + associated IceCube institutes in USA, Europe, Japan, New Zealand Christian Spiering

  7. AMANDA-II and SPASE South Pole Air Shower Experiment inner 10 strings: Amanda-B10 19 strings 677 PMTs optical module construction 1996-2000 AMANDA II Christian Spiering

  8. 2. Selected Physics Results • Search for point sources (AMANDA) • Search for a diffuse extraterrestrial flux (Amanda & Baikal) • Indirect Search for Dark Matter (Amanda & Baikal) • Search for neutrinos coincident with Gamma Ray Bursts • (Amanda & Baikal) • 5. Measurement of the spectrum of atmospheric neutrinos • (Amanda) • 6. Measurement of the spectral composition of primary cosmic • rays (Spase/Amanda) Christian Spiering

  9. Search for extraterrestrial point sources 697 events below horizon below horizon: mostly atmospheric ‘s above horizon:mostly fake events AMANDA-II 2000 data Submitted to PRL Christian Spiering

  10. Now analyzed: 1997, 1999, 2000 Started: 2001, 2002 AMANDA-II 20% of 2001 data • Planned until • Summer 2004: • combined • analysis 97-99 • combined • analysis 00-03 Christian Spiering

  11. SS-433 Christian Spiering

  12. Amanda-II, 2000 data: Neutrino flux upper limit (90% C.L.) in units of 10-7 cm-2 s-1 for an assumed E-2 spectrum, integrated above E = 10 GeV. Christian Spiering

  13. Selected point source flux limits sensitivity  flat above horizon - 4 times better than B10¶ ! declination averaged sensitivity: lim  0.23•10-7 cm-2s-1 @90% upper limits @ 90% CL in units of 10-8cm-2s-1 ¶published Ap. J, 582 (2003) Christian Spiering

  14. 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. Christian Spiering

  15. DUMAND FREJUS  bound MACRO Muons in Amanda-B10 (1997) WB bound Expectation Amanda-II, 3 years Expectation IceCube, 3 years Search for an diffuse excess of extra-terrestrial high energy neutrinos log E /GeV

  16. ... look also to cascades from electronand tau neutrino interactions Assuming e:: =1:2:0 at source e::=1:1:1 at Earth factor 3 applied to  channel AMANDA-II cascades 2000  analysis will yield an all-flavour limit close to the cascade limit Christian Spiering

  17. Indirect Search for WIMPs  (a) Neutrinos from the Center of Earth  +   b + b „soft spectrum“   W + + W - „hard spectrum“ Christian Spiering

  18. Upper limits on muon flux from neutralino annihilations in center of Earth Green dots: Excluded by present direct searches Blue crosses: can be excluded by 10 times more sensitive direct searches Baikal 98/99 data Christian Spiering

  19. Indirect Search for WIMPs (b) 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. Christian Spiering

  20. Upper limits on muon flux from neutralino annihilations in center of Sun AMANDA-II results: • based on 193 days of live time • Exclusion sensitivity from analyzing the off-source bins Will un-blind data soon and look to the Sun. preliminary ANTARES and ICECUBE: MC-calculated sensitivities

  21. 3. IceCube Christian Spiering

  22. IceCube Collaboration Institutions: 11 US, 10 European, 1 Japanese and 1 Venezuelan 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 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, Stockholm University, Stockholm, Sweden Dept. of Physics, University of Alabama, USA Vrije Universiteit Brussel, Brussel, Belgium Chiba University, Japan Dept. of Astrophysics, Imperial College, UK Dept. of Physics, University of Maryland, USA Universidad Simon Bolivar, Caracas, Venezuela University Utrecht, Netherlands Christian Spiering

  23. IceTop AMANDA South Pole 1400 m 2400 m IceCube - 80 Strings - 4800 PMT • Instrumented volume: 1 km3 • Installation: 2004-2010 ~ 80.000 atm. per year Christian Spiering

  24. Schedule 03-04 drill equipment to Pole 04-05 first 5 strings (proof that 16/season are feasible) 05-06 12 strings 06-07 16 strings 07-08 16 strings 08-09 16 strings 09-10 remaining strings Christian Spiering

  25. 4. DESY Tasks in IceCube Simulation & optimization IceCube accepted by Astropart.Phys. Design of Front-End-Electronics (Communication to Optical Module) German production site for 1300 optical modules (1/4 of all 5200 modules) IceCube lead for Amanda-IceCube integration IceCube lead for reconstruction German/European data processing center R&D wavelength shifter for optical modules R&D acoustic detection analysis: search for extraterrestrial diffuse and point-like sources, relativistic magnetic monopoles, slowly moving exotic particles

  26. 96V DOM Power DOR: DOMReadout card Quad Cable Con. Power Switch Comm. DAC Clock & Time String port Comm. ADC PLD Comm. Rec. FPGA FLASH SRAM JTAG Christian Spiering 12/19/2019 Christian Spiering

  27. DOR • Traffic over 2 km • twisted pair cable: • supply voltage • slow control • FADC output (up to 1 Mbit/sec) • synchro-signals • ( require 5 nsec accuracy) DOM Christian Spiering

  28. Production of 1300 Optical Modules Includes 10 weeks test in Dark Freezer at -45 ºC Christian Spiering

  29. Dark Freezer Lab - 45 °C Up to 120 Optical Modules Christian Spiering

  30. Enhancing the Sensitivity of IceCube Optical Modules by Application of Wave Length Shifters • Elisa Resconi • EU post-doc in DESY • guest at MPIK-Heidelberg

  31. Deep Sea Water Christian Spiering

  32. INTENSITY (a.u) Cherenkov spectrum (a.u.) OM glass, 11.5 mm Gel 10 mm PMT glass, 2.6mm Ice, in contrast to water, is UV trans- parent down to 230 nm. The glass of the pressure sphere absorbs most light below 350 nm. Light lost Light detected Cherenkov Spectrum Christian Spiering

  33. 100 100 80 Transmittance (%) Transmittance (%) Nauthilus glass (15 mm) 75 Benthos glass (11.5mm) 60 BPO 50 PPO 40 Butyl-PBD 25 20 Application of Wavelength Shifters (WLS) Earlier attempts indicated that an overall gain of 40% can be achieved. However, WLS layers deteriorated in water and where mechanically unstable. Now, a water-proof and mechanically stable WLS foil exists. Christian Spiering

  34. 10 cm THV granulate doped with PPO Extrusion of transparent foil Thermo-forming of cap Will be optically coupled with a very thin layer of gel (less then 1mm) and fixed at optical module support. Effect: ~ 40% more light  lower threshold, better reconstruction  next: Tests in Dark Freezer Room  if success: Test at 04/05 at Pole Christian Spiering

  35. 50s P t R&D on acoustic detection: 10-100 cubic kilometer volume for extremely high energies ? Particle cascade  ionization  heat  pressure wave Maximum of emission at ~ 20 kHz Attenuation length of cold ice at 15-30 kHz: ~ 2 km (light: ~ 100 meters) → given a large initial signal, huge detection volumes can be achieved. Christian Spiering

  36. Development and test of a variety of acoustic sensors in Zeuthen Rolf Nahnhauer et al. Christian Spiering

  37. tests with laser light dumped to ice and water • tests with protons dumped into ice and water • tests in open water • development of hardware and software filters Hearing 180 MeV protons dumped into ice Threshold with present sensors: ~ EeV Expected improved threshold: ~ 100 PeV Christian Spiering

  38. Request for a test at South Pole in 2004/05  Study ambient noise  Measure absorption length See also talk in closed session Christian Spiering

  39. 5. Summary • Amanda-II produces new limits on point sources, diffuse fluxes, GRB, WIMPs, and measures atmospheric neutrino spectrum up to 100 TeV. • AMANDA-II has reached the sensitivity needed to search from neutrino fluxes from TeV gamma sources of similar strength to the instrinsic gamma flux. • Next: 2000-2003 data coherently processed • Baikal produces new limits on diffuse flux, WIMPs, and GRB and will stay largest neutrino telescope on northern hemisphere for 2-3 years. • IceCube is established as MRE, 6 strings to be produced in 2004. • DESY-Zeuthen ready for OM production • New methods - WLS and acoustic – may enhance IceCube performance considerably. R&D in Zeuthen. Christian Spiering

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