1 AstroParticle Physics PRC, May 2009 Christian Spiering

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

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

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 Deep look at the TeV sky AGN pulsars GRB Galactic sources

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

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 05/06: 8 Remaining: 22 IceCube Strings 5 DeepCore Strings  complete in January 2011 IceCube

14 IceCube/Amanda analysis: Selected results

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

16 relative deviations significance map Large-scale anisotropy of downgoing muons recorded in IceCube anisotropies on the per-mille scale (skymap in equatorial coordinates)

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

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19 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 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) (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 aked-eye GRB080319B –Naked-eye GRB080319B Astrophys. Journ., accepted Next weeks: unblinding of many Analyses (IC-22, IC40 first 5 months)

20 Atmospheric Neutrinos Spectrum measured up to >100 TeV IceCube will provide a few 10 5 atm neutrinos - rich physics ! AMANDA

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

22 Exotic Oscillations Use large atmospheric neutrino sample, look for ν μ disappearance and appearance of  –Violation of Lorentz invariance –Quantum decoherence (both appear in quantum gravity theories) Muon neutrino survival probability Conventional oscillations VLI oscillations, δc/c = parameters of interest: VLI:  c/c, sin 2 , phase  QD: D 3 and D 8, D 6 and D 7 Different to standard oscillations (~ 1/E), effects of QG oscillations go ~ E

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

24 Indirect Dark Matter Search Sun Detector Earth

25 Indirect Dark Matter Search Amanda: –analysis with standard point source sample ( ) –analysis with dedicated sample ( ) –similar sensitivity & limits –to be submitted in June IceCube-22: –PRL, accepted and arXiv:

26 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

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

28 t ~ -10  -100st ~ 0  t90 t ~ t90  ? Waxman & Bahcall, ApJ 541:707 (2000) Neutrinos from GRB AMANDA limit from 408 bursts Waxman-Bahcall GRB prediction neutrino energy E (GeV) E 2  flux (GeV  cm -2  s -1  sr -1 )

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

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

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

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

33 IceCube Northern Hemisphere IceCube CPU Iridium satellites MAGIC (VERITAS/Whipple also interested) AGN Flare Neutrino Target of Opportunity with MAGIC (DESY) Commissioning (online trigger) - Selected objects - Time scale of multiplets is days-weeks

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

35 IceCube Northern Hemisphere IceCube CPU Iridium satellites ROTSE III SN/GRB Fast reaction to GRB alerts Optical Follow-Up with ROTSE ( Humboldt/ DESY ) Commissioning (online trigger)

36 Further activities/results DESY  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 (  ~ ): - 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

37 Summary  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

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39 Check for coincidences with BATSE, 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 Coincidences with GRB AMANDA limit from 408 bursts Waxman-Bahcall GRB prediction neutrino energy E (GeV) E 2  flux (GeV  cm -2  s -1  sr -1 )

40 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)