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1 Jan Conrad (CERN) GLAST Lunch, 09. Mar. 2006, Jan Conrad (KTH) The AMANDA neutrino telescope: Results from GRB and dark matter searches Jan Conrad (KTH,

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Presentation on theme: "1 Jan Conrad (CERN) GLAST Lunch, 09. Mar. 2006, Jan Conrad (KTH) The AMANDA neutrino telescope: Results from GRB and dark matter searches Jan Conrad (KTH,"— Presentation transcript:

1 1 Jan Conrad (CERN) GLAST Lunch, 09. Mar. 2006, Jan Conrad (KTH) The AMANDA neutrino telescope: Results from GRB and dark matter searches Jan Conrad (KTH, Stockholm)

2 2 Jan Conrad (CERN) GLAST Lunch, 09. Mar. 2006, Jan Conrad (KTH) Content AMANDA/IceCube. AMANDA results on neutrinos from Dark Matter candidates AMANDA results on neutrinos from GRBs I’ll keep it really simple …..

3 3 Jan Conrad (CERN) GLAST Lunch, 09. Mar. 2006, Jan Conrad (KTH) USA (14) Europe (15) Japan New Zealand Alabama University, USA Bartol Research Institute, Delaware, USA Pennsylvania State University, USA UC Berkeley, USA UC Irvine, USA Clark-Atlanta University, USA University of Alaska, Anchorage, USA Univ. of Maryland, USA Alabama University, USA Bartol Research Institute, Delaware, USA Pennsylvania State University, USA UC Berkeley, USA UC Irvine, USA Clark-Atlanta University, USA University of Alaska, Anchorage, USA Univ. of Maryland, USA IAS, Princeton, USA University of Wisconsin-Madison, USA University of Wisconsin-River Falls, USA LBNL, Berkeley, USA University of Kansas, USA Southern University and A&M College, Baton Rouge, USA IAS, Princeton, USA University of Wisconsin-Madison, USA University of Wisconsin-River Falls, USA LBNL, Berkeley, USA University of Kansas, USA Southern University and A&M College, Baton Rouge, USA Universite Libre de Bruxelles, Belgium Vrije Universiteit Brussel, Belgium Université de Mons-Hainaut, Belgium Universiteit Gent, Belgium Humboldt Universität, Germany Universität Mainz, Germany DESY Zeuthen, Germany Universität Dortmund, Germany Universite Libre de Bruxelles, Belgium Vrije Universiteit Brussel, Belgium Université de Mons-Hainaut, Belgium Universiteit Gent, Belgium Humboldt Universität, Germany Universität Mainz, Germany DESY Zeuthen, Germany Universität Dortmund, Germany Universität Wuppertal, Germany MPI Heidelberg, Germany Uppsala University, Sweden Stockholm University, Sweden Imperial College, London, UK Oxford University, UK Utrecht University, Netherlands Universität Wuppertal, Germany MPI Heidelberg, Germany Uppsala University, Sweden Stockholm University, Sweden Imperial College, London, UK Oxford University, UK Utrecht University, Netherlands Chiba University, Japan University of Canterbury, Christchurch, NZ Chiba University, Japan University of Canterbury, Christchurch, NZ ANTARCTICA The IceCube Collaboration (formerly known as AMANDA)

4 4 Jan Conrad (CERN) GLAST Lunch, 09. Mar. 2006, Jan Conrad (KTH) South Pole AMANDA B-10: 10 strings, 302 Optical Modules (1997-1999) AMANDA-II: 19 Strings, 677 Optical Modules (2000-2004) Trigger rate: ~60 Hz (mostly downgoing muons) Angular resolution: δθ ~ 3° (most probable for GRB search) South Pole

5 5 Jan Conrad (CERN) GLAST Lunch, 09. Mar. 2006, Jan Conrad (KTH) Detection principle O(10m) Cascades, e,  and Neutral Current O(km) muons from  ~10-20 m Optical module

6 6 Jan Conrad (CERN) GLAST Lunch, 09. Mar. 2006, Jan Conrad (KTH) IceCube Neutrino Observatory IceTop air shower array 80 pair of ice Cherenkov tanks IceCube 80 strings with 60 optical modules 17 m between optical modules 125 m between strings 1 Gton detector! Present status: 9 strings deployed !

7 7 Jan Conrad (CERN) GLAST Lunch, 09. Mar. 2006, Jan Conrad (KTH) Physics Motivations and Goals AMANDA IceCube Attractive astronomical messengers: Transparent Universe (≠γ) Travel in straight line (≠p) Produced in hadronic accelerators ? Study of: Sources: AGNs, SNRs, GRBs... neutrino-physics: oscillations, cross-sections.. “new” physics: WIMPS, monopoles...

8 8 Jan Conrad (CERN) GLAST Lunch, 09. Mar. 2006, Jan Conrad (KTH) optimized for E -2, (*) E -2, 3 signal *  lim  0.68·10 -8 cm -2 s -1 average flux upper limit [cm -2 s -1 ] sin  AMANDA-B10 AMANDA-II IceCube 1/2 year * Preliminary Steady point source: progress in sensitivity (ego slide) time >10 GeV 1999b: Jan’s analysis Jan’s model, still not excluded

9 9 Jan Conrad (CERN) GLAST Lunch, 09. Mar. 2006, Jan Conrad (KTH) Since I am among friends..some words on 1ES 1955+650 AMANDA II sees 5 neutrinos during a period of 4 years The expected background is 3.7 It turns out 3 out of the 5 events are detected within a period of 66 days (which happens to be while 1ES1955 is in a flaring state) I calculate significance of: 3.2 σ (no trial factors) 66 days ? Would I bet on it ? Well, yes.....

10 10 Jan Conrad (CERN) GLAST Lunch, 09. Mar. 2006, Jan Conrad (KTH) Neutralino as dark matter candidate (in one minute) Cosmological observations  m ~ 0.30  b ~ 0.05 Minimal Supersymmetric Standard Model R- parity conserved  LSP stable = neutralino  interacts weakly  = GeV-TeV mass = dark matter??? stable   dark, non-baryonic matter What is it ?

11 11 Jan Conrad (CERN) GLAST Lunch, 09. Mar. 2006, Jan Conrad (KTH) MSSM: presentation Bosons  Fermions ( ~double the particle content, and introduce many new couplings)  106 free parameters Measured quantity (flux, cross section) Some parameter of the thoery (often the LSP mass) Parameter 1 Of theory Parameter 2 of theory Each star represents a particular model All other parameters fixed Exclusion/Inclusion limit

12 12 Jan Conrad (CERN) GLAST Lunch, 09. Mar. 2006, Jan Conrad (KTH) Neutralino capture Higher density  appreciable rates

13 13 Jan Conrad (CERN) GLAST Lunch, 09. Mar. 2006, Jan Conrad (KTH) Neutralino-induced neutrinos qq  l + l -   W, Z, H Atmospheric background atm.  :absorbed by the Earth atm. :compare on/off source angular regions “down” “up” Neutralino signals

14 14 Jan Conrad (CERN) GLAST Lunch, 09. Mar. 2006, Jan Conrad (KTH) Earth 1997-1999 (paper in preparation) Sun 2001 (submitted to Astrop. Phys.) Analysis Cuts, ANN

15 15 Jan Conrad (CERN) GLAST Lunch, 09. Mar. 2006, Jan Conrad (KTH) signal region Earth 1997-1999 (paper in preparation) Sun 2001 ( Astropart.Phys.24:459-466,2006 ) Results Cos Θ

16 16 Jan Conrad (CERN) GLAST Lunch, 09. Mar. 2006, Jan Conrad (KTH) Limits on muon flux from Earth center Limits on muon flux from Sun Results cont’d Submitted for publicationPublished in Astrpart. Phys. Low mass  high BR into tautau  nu can play role Disfavored by direct search (CDMS II)

17 17 Jan Conrad (CERN) GLAST Lunch, 09. Mar. 2006, Jan Conrad (KTH) And now to something else....

18 18 Jan Conrad (CERN) GLAST Lunch, 09. Mar. 2006, Jan Conrad (KTH) Observations indicate: synchrotron radiation or inverse compton as source of prompt emission GRBs are unique, varying from burst to burst and class to class (short, long, X-ray strong). Durations:.1-100s, 0.1-1Mev gammas relativistic expansion from a compact object R ≤ 2Γ2cDt (compact explains rapid variability, relativistic expansions lets high energy gammas escape) (Isotropic) GRBs in a minute

19 19 Jan Conrad (CERN) GLAST Lunch, 09. Mar. 2006, Jan Conrad (KTH) Neutrinos from GRBS Self-Compton Scattering Magnetic Field Electron ---  -ray Synchrotron Radiation Electro n  -ray Low-Energy Photon Prompt  -ray emission of GRB is due to non-thermal processes such as electron synchrotron radiation or self-Compton scattering. e-p+e-p+e-p+e-p+ Internal Shocks Prompt GRB Emission Afterglow Radio Optical X-ray  -ray Hadron Acceleration ?! -  COSMIC RAYS ?

20 Jan Conrad (CERN) A Distant GRB CGRO IceCube AMANDA γ, ν ν IPN Satellites (HETE, Swift, etc.) GRB timing/localization information from correlations among satellites

21 21 Jan Conrad (CERN) GLAST Lunch, 09. Mar. 2006, Jan Conrad (KTH) Blinded 10 minute window - 5 minutes + 5 minutes ~110 (120-10) minute background used to set cuts and check for data quality & stability - 60 minutes + 60 minutes Background region is approximately ±60 minutes surrounding each GRB (determined by BATSE/IPN) Omit ±5 minutes surrounding GRB trigger time Analyse large number of BATSE GRBs assuming average neutrino spectrum (“mass search”) OR look at individual GRB: model neutrino spectrum from e.-m. observations (“individual search”) Analysis strategies

22 22 Jan Conrad (CERN) GLAST Lunch, 09. Mar. 2006, Jan Conrad (KTH) Cuts based on : event time relative to BATSE trigger reconstructed track direction relative to burst position uniformity of hits along reconstructed track event-wise angular resolution of reconstructed track  Optimize with respect to figure of merit Event quality selection

23 23 Jan Conrad (CERN) GLAST Lunch, 09. Mar. 2006, Jan Conrad (KTH) Assuming prediction from Waxman&Bahcall Phys.Rev.D59:023002,1999 E ν 2 Φ ν < 4x10 -8 GeV cm -2 s -1 sr -1 Results: Mass search YearN Bursts B Exp N Obs U.L. 2000881.0202.05 2001150.0502.19 2002170.0802.01 2003190.1001.61 00-03139 (All)1.2501.47 Note: O(10) times the WB bound

24 24 Jan Conrad (CERN) GLAST Lunch, 09. Mar. 2006, Jan Conrad (KTH) Close: z ~ 0.17 Among top 0.2 % of the 2700 BATSE GRBS (Fluence) Peak flux 100 x Crab [Razzaque et al., PRD 69 023001 (2004)] Results: individual search, example: GRB030329

25 25 Jan Conrad (CERN) GLAST Lunch, 09. Mar. 2006, Jan Conrad (KTH) General strategy Fit photon-spectrum with empirical ”Band function” get redshift from observations of optical afterglow calculate expected neutrino spectrum from photon spectrum under certain assumptions For example: Photon meson production (protons accelerated in the shock, photons are synchrotron photons in the jet) See Guetta et a,l Astropart.Phys.20:429-455,2004

26 26 Jan Conrad (CERN) GLAST Lunch, 09. Mar. 2006, Jan Conrad (KTH) Band spectrum A ,   b,   P Spectral Fit Parameters

27 27 Jan Conrad (CERN) GLAST Lunch, 09. Mar. 2006, Jan Conrad (KTH) Neutrino spectrum is expected to trace the photon spectrum. Is function of : fluence, T90, redshift, gamma luminosity Traces gammas (low) Traces gamma (high) Pions loose energy in sync radiation Neutrino spectrum

28 28 Jan Conrad (CERN) GLAST Lunch, 09. Mar. 2006, Jan Conrad (KTH) Individual vs. Average (GRB 030329) Flux modelSearch bin Size (deg) Expected background Expected number of signal events Observed number of events Isotropic individual 11.30.230.020 Isotropic average 11.30.170.0010

29 29 Jan Conrad (CERN) GLAST Lunch, 09. Mar. 2006, Jan Conrad (KTH) Conclusions Dark matter search: no dark matter found, ICECUBE might be sensitive to class of models which are not allerady excluded by CDMS, looking at the sun GRBs: no neutrinos from GRBs found IceCube will have order of magnitude larger effective area Detection likely to come from one exceptional (high fluence) burst, rather than average burst

30 30 Jan Conrad (CERN) GLAST Lunch, 09. Mar. 2006, Jan Conrad (KTH) References http://icecube.wisc.edu/ Wimps in AMANDA: D. Hubert, talk given at DM 2006 (Marina del Rey) AMANDA collab: Astropart.Phys.24:459-466,2006 (solar) AMANDA collab: Phys.Rev.D66:032006,2002 (terrestrial) GRBs in AMANDA: M.Stamatikos : to appear in SWIFT symposium IceCube collab: M. Stamatikos: ICRC 2005, Puna, India Guetta et. al: Astropart.Phys.20:429-455,2004 E. Waxman & J. Bahcall: Phys.Rev.D59:023002,1999 IceCube collab: K. Kuehn: ICRC 2005, Puna, India

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