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AstroParticle Physics PRC, May 2009 Christian Spiering

AstroParticle Physics PRC, May 2009 Christian Spiering. Overview. . total expenditures DESY/Astroparticle. Baikal: 1988-2008 Amanda: 1995-2009 IceCube: since 2000 MAGIC (YIG): since 2006 CTA (prototype): since 2008

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AstroParticle Physics PRC, May 2009 Christian Spiering

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  1. AstroParticle Physics PRC, May 2009Christian Spiering

  2. Overview  total expenditures DESY/Astroparticle • Baikal: 1988-2008 • Amanda: 1995-2009 • IceCube: since 2000 • MAGIC (YIG): since 2006 • CTA (prototype): since 2008 • Astroparticle Theory starting 2009(together with U. Potsdam)  IceCube construction CTA prototype construction Multi-messenger approach

  3. MAGIC: Status, AGN Monitoring CTA: status and plans IceCube Construction: Status and schedule IceCube/Amanda analysis: Selected results

  4. MAGIC:Status, AGN Monitoring

  5. MAGIC II: commissioning Pratik Majumdar DESY Young Invest. Group • Improved sensitivity • lower threshold DESY YIG contributed HQE PMT (Helmholtz grant) MAGIC-II MAGIC-I

  6. DESY: Monitoring of bright blazars Un-biased statistics of different flux levels Long-term flux level variability studies Determination of flare probabilities Studies of spectra for different flux levels Triggers for ToO (self-trigger, other IACTs, X-ray, etc.)‏ Studies of correlations with other wavelengths and neutrino events Mkn 501 MAGIC long-term Light curve Satalecka et al, SciNEGHE'08 AIP Conf. Ser. in press

  7. CTA:Status and plans

  8. The Cherenkov Telescope Array • Increased sensitivity • Extended energy range • Improved angular resolution • Observatory with flexible and robotic operation • Arrays in North and South for full sky coverage 50 to 100 large, medium and small telescopes

  9. Sensitivity AGN pulsars GRB Galactic sources Deep look at the TeV sky

  10. Japan will join CTA Close collaboration with AGIS (USA) Startup meeting FP7 proposal Array layout Consortium Components Telescopes Array construction Science operation VERITAS Fermi H.E.S.S. II MAGIC II

  11. DESY works on • 12 m telescope prototype with large field of view • Drive and control and safety system • Fast read-out system based on domino ring sampler • HV concept for camera • Timing studies for background suppression • Trigger optimization Detailed report at next PRC

  12. IceCube Construction:Status and schedule

  13. IceCube IceCube 07/08: 18 06/07: 13 04/05: 1 08/09: 19 strings 05/06: 8 Remaining: 22 IceCube Strings 5 DeepCore Strings  complete in January 2011

  14. IceCube/Amanda analysis: Selected results

  15. Shadow of the Moon • Absolute pointing  1° • Angular resolution  1° Cosmic Rays 0.5° 5 months IC40

  16. Large-scale anisotropyof downgoing muons recordedin IceCube relative deviations anisotropies on the per-mille scale (skymap in equatorial coordinates) significance map

  17. Tibet air shower array Compare to Northern hemisphere • Compton-Getting effect ? • Solar wind pressure ? • Nearby pulsar ? • Interstellar magnetic field ? • First observation on Southern hemi- sphere adds important piece of information. MILAGRO Simulation (Lallement et al. Science 2005)

  18. Journal Publications(recently published or accepted) • Observation of solar flare with IceTop • Astrophys. Journ. 689/1 (2008) L65 • IceCube DAQ • Nucl.Instr.Meth. A601 (2009) 294 • AMANDA 7-year point source search • Phys. Rev. D79 (2009) 062001 (events available on the web) • AMANDA 7-year atmosph. neutrinos & Quantum Gravity effects • Phys. Rev. D, accepted • IceCube-22 WIMP search • Phys. Rev. Lett., accepted • Naked-eye GRB080319B • Astrophys. Journ., accepted • ICRC 2009:42 four-page contributions, 5 from DESY • 2 x point source search • 1 x cascade search • 1 x cosmic ray with IceTop • 1 x acoustic detection technique Next weeks: unblinding of many Analyses (IC-22, IC40 first 5 months)

  19. Atmospheric Neutrinos Spectrum measured up to >100 TeV AMANDA IceCube will provide a few 105 atm neutrinos - rich physics !

  20. Neutrino Oscillations • Use large atmospheric neutrino sample, look for νμdisappearance and appearance of  • DeepCore will help peering into the oscillation region Muon neutrino survival probability Goal for DeepCore: Threshold < 20 GeV oscillations

  21. Exotic Oscillations Muon neutrino survival probability VLI oscillations,δc/c = 10-27 Conventionaloscillations • Use large atmospheric neutrino sample, look for νμdisappearance and appearance of  • Violation of Lorentz invariance • Quantum decoherence (both appear in quantum gravity theories) parameters of interest: VLI:c/c, sin 2, phase  QD: D3 and D8, D6 and D7 Different to standard oscillations (~ 1/E), effects of QG oscillations go ~ E

  22. Limits from 7 years AMANDA (2000-2006) QD VLI Amanda 4 years 99% C.L.allowed 99% C.L. excl. Full IceCube (sensitivity) 90% C.L.allowed 99% C.L. excl. 90% C.L.allowed PRD accepted and arXiv:0902.0675

  23. Indirect Dark Matter Search Sun Earth Detector

  24. Indirect Dark Matter Search • Amanda: • analysis with standard point source sample (2000-2006) • analysis with dedicated sample (2001-2003) • similar sensitivity & limits • to be submitted in June • IceCube-22: • PRL, accepted and arXiv:0902.2460

  25. Indirect Dark Matter Search ….. apply to spin-dependent cross section • Models with strong spin-dependent coupling are the least constrained by direct DM searches. • W.r.t. spin-dependent coupling, Amanda & IceCube are ~100 times more sensitive than direct search experiments (Sun is mostly hydrogen) Effect of DeepCore

  26. Neutrinos from GRB Razzaque et al., PRD 68 (2003) Waxman & Bahcall, PRL 78:2292 (1997) Waxman & Bahcall, ApJ 541:707 (2000) t ~ -10-100s t ~ 0 t90 t ~ t90 ?

  27. Neutrinos from GRB 10-7 AMANDA limit from 408 bursts 1997-2003 10-8 Waxman-Bahcall GRB prediction E2flux (GeVcm-2s-1sr-1) 10-9 10-10 104 105 106 107 108 neutrino energy E(GeV) Waxman & Bahcall, ApJ 541:707 (2000) t ~ -10-100s t ~ 0 t90 t ~ t90 ?

  28. Neutrinos from naked-eye GRB080319B Duration: 70 s RA: 217.9o Dec: 36.3o z=0.94 Brightest GRB (optical) ever Large number of g-ray, x-ray, UV and optical, observations Pi of the Sky

  29. Neutrinos from naked-eye GRB080319B Detector running in maintenance mode at the time:9 out of 22 strings. Signal expectation: 0.1 events (G = 300) No events at GRB position/time after cut  Limit ~1.5 event in full IceCube arXiv:0902.01311 APJ accepted and arXiv:0902.0131

  30. Steady Point Sources TeV-PeV range PeV-EeV range Wisconsin, DESY, Heidelberg DESY First skymaps, 22 strings, 2007 New territory: ¼ IceCube/1 year ~ 2  full Amanda/7 years ! Ultra-High Energies looking to Southern hemisphere Separate papers on standard and HE/above horizon analysis to be submitted in June/July

  31. Point Sources: The Progress point source limits/sensitivities: Common analyses with Antares & KM3NeT in overlap regions factor 1000 in 15 years !

  32. Neutrino Target of Opportunity with MAGIC (DESY) Commissioning (online trigger) • - Selected objects • Time scale of • multiplets is • days-weeks Iridiumsatellites AGN Flare IceCube NorthernHemisphereIceCube CPU MAGIC (VERITAS/Whipple also interested)

  33. Neutrino Target of Opportunity with MAGIC (DESY) Commissioning (online trigger) Iridiumsatellites Alert rates for bin radius of 2°and pre-trial thresholds of 3and 5 (for one source) AGN Flare IceCube NorthernHemisphereIceCube CPU MAGIC (VERITAS/Whipple also interested)

  34. Optical Follow-Up with ROTSE ( Humboldt/DESY ) Commissioning (online trigger) Iridiumsatellites Fast reactionto GRB alerts SN/GRB IceCube NorthernHemisphereIceCube CPU ROTSE III

  35. IceCube-40: Off-line search for time flares - close to unblinding IceCube-40: reconstruction of cascades - record accuracy for energy, position & angle ! IceTop: spectrum and mass composition of cosmic rays - first spectrum derived Search for slowly moving particles (~10-5 -10-3): - GUT magnetic monopoles, SUSY Q-balls, strange quark matter, ongoing work R&D on acoustic detection - considerably improved parameters from last season, report at next PRC Further activities/results DESY

  36. IceCube Amanda analyses completed IceCube-22 results being published Lot of interesting results Unblinding of first 5 months IceCube-40 data within the next weeks  summer conferences Sensitivity gradient strongest within next 3-5 years MAGIC Soon first light with MAGIC-II. YIG: AGN monitoring, low energy sources CTA Steep start. Wide front of activities DESY well positioned Application for additional Helmholtz investment Summary

  37. Coincidences with GRB 10-7 AMANDA limit from 408 bursts 1997-2003 10-8 Waxman-Bahcall GRB prediction E2flux (GeVcm-2s-1sr-1) 10-9 10-10 104 105 106 107 108 neutrino energy E(GeV) Check for coincidences withBATSE, IPN, SWIFT, FERMI • WB model one of the most testable astrophys. Models for IceCube • Amanda came close to WB within < factor 2 • full IceCube: 95% probability to detect WB flux with 5 within 1 year • ~ 10 ongoing analyses

  38. Different alert philosophies • Optical follow-up: 2 events from the same direction within t (minute scale). Look to the full sky. • NToO:  n events within t (days-weeks) from directions of a few pre-defined sources with known flaring behaviour. n andt optimized to a given significance threshold (e.g. 3,5) Alert rates for bin radius of 2°and pre-trial thresholds of 3and 5 (for one source)

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