Transcript IceCube
AstroParticle Physics PRC, May 2009 Christian Spiering 1 Overview Expenditures Astro-Particlephysics total expenditures DESY/Astroparticle 3 Neutrino 2,5 Gamma 2 Mio. € Baikal: 1988-2008 Amanda: 1995-2009 1,5 1 IceCube: since 2000 0,5 0 004 2005 2004 2005 2006 2007 2008 2009 2010 2011 2012 2014 Year 2006 2007 2008 2009 2010 2011 2012 MAGIC (YIG): Year since 2006 CTA (prototype): since 2008 IceCube 2013 construction 2014 CTA prototype construction Multi-messenger approach Astroparticle Theory starting 2009 (together with U. Potsdam) 2 2013 MAGIC: Status, AGN Monitoring CTA: status and plans IceCube Construction: Status and schedule IceCube/Amanda analysis: Selected results 3 MAGIC: Status, AGN Monitoring 4 MAGIC II: commissioning • Improved sensitivity • lower threshold Pratik Majumdar DESY Young Invest. Group DESY YIG contributed HQE PMT (Helmholtz grant) MAGIC-I 5 MAGIC-II 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 6 CTA: Status and plans 7 The Cherenkov Telescope Array Increased sensitivity 50 to 100 large, medium Extended energy range and small telescopes Improved angular resolution Observatory with flexible and robotic operation Arrays in North and South for full sky coverage 8 Sensitivity AGN pulsars GRB 9 Deep look at the TeV sky Galactic sources Japan will join CTA Close collaboration with AGIS (USA) 2006 2007 2008 2009 2010 2011 2012 2013 2014 2015 2016 2017 Startup meeting FP7 proposal Array layout Consortium Design and Prototype Phase Components Telescopes Array construction Science operation VERITAS Fermi H.E.S.S. II MAGIC II 10 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 11 IceCube Construction: Status and schedule 12 IceCube IceCube 07/08: 18 06/07: 13 05/06: 8 04/05: 1 08/09: 19 strings Remaining: 22 IceCube Strings 5 DeepCore Strings complete in January 2011 13 IceCube/Amanda analysis: Selected results 14 Shadow of the Moon • Absolute pointing 1° • Angular resolution 1° Cosmic Rays 0.5° 5 months IC40 15 Large-scale anisotropy of downgoing muons recorded in IceCube relative deviations anisotropies on the per-mille scale (skymap in equatorial coordinates) 16 significance map Compare to Northern hemisphere • Compton-Getting effect ? • Solar wind pressure ? • Nearby pulsar ? • Interstellar magnetic field ? Simulation (Lallement et al. Science 2005) • First observation on Southern hemisphere adds important piece of information. 17 Tibet air shower array MILAGRO 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 18 Atmospheric Neutrinos Spectrum measured up to >100 TeV AMANDA IceCube will provide a few 105 atm neutrinos - rich physics ! 19 Neutrino Oscillations • Use large atmospheric neutrino sample, look for νμ disappearance and appearance of Muon neutrino survival probability • DeepCore will help peering into the oscillation region Goal for DeepCore: Threshold < 20 GeV oscillations 20 Exotic Oscillations • Use large atmospheric neutrino sample, look for νμ disappearance 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 21 Muon neutrino survival probability VLI oscillations, δc/c = 10-27 Conventional oscillations Limits from 7 years AMANDA (2000-2006) QD Amanda 4 years 99% C.L. allowed 90% C.L. allowed VLI 99% C.L. excl. 99% C.L. excl. 90% C.L. allowed PRD accepted and arXiv:0902.0675 22 Indirect Dark Matter Search Sun Earth Detector 23 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 24 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 25 Neutrinos from GRB Razzaque et al., PRD 68 (2003) t ~ -10-100s 26 Waxman & Bahcall, PRL 78:2292 (1997) t ~ 0 t90 Waxman & Bahcall, ApJ 541:707 (2000) t ~ t90 ? E2flux (GeVcm-2s-1sr-1) Neutrinos from GRB 10-7 AMANDA limit from 408 bursts 1997-2003 10-8 Waxman-Bahcall GRB prediction 10-9 10-10 104 105 106 107 neutrino energy E (GeV) t ~ -10-100s 27 108 t ~ 0 t90 Waxman & Bahcall, ApJ 541:707 (2000) t ~ t90 ? Neutrinos from naked-eye GRB080319B Duration: 70 s RA: 217.9o Dec: 36.3o z=0.94 Brightest GRB (optical) ever Large number of -ray, x-ray, UV and optical, observations 28 Pi of the Sky 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 29 Steady Point Sources TeV-PeV range Wisconsin, DESY, Heidelberg PeV-EeV range DESY First skymaps, 22 strings, 2007 Ultra-High Energies New territory: ¼ IceCube/1 year ~ 2 full Amanda/7 years ! 30 looking to Southern hemisphere Separate papers on standard and HE/above horizon analysis to be submitted in Summer Point Sources: The Progress point source limits/sensitivities: Common analyses with Antares & KM3NeT in overlap regions factor 1000 in 15 years ! 31 Neutrino Target of Opportunity with MAGIC (DESY) Iridium satellites AGN Flare IceCube 32 Northern Hemisphere IceCube CPU - Selected objects - Time scale of multiplets is days-weeks MAGIC (VERITAS/Whipple also interested) Neutrino Target of Opportunity with MAGIC (DESY) Iridium satellites IceCube 33 Alert rates for bin radius of 2° and pre-trial thresholds of 3 AGN and 5 (for oneFlare source) Northern Hemisphere IceCube CPU MAGIC (VERITAS/Whipple also interested) Optical Follow-Up with ROTSE ( Humboldt/DESY ) Iridium satellites SN/GRB IceCube 34 Northern Hemisphere IceCube CPU Fast reaction to GRB alerts ROTSE III 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 (~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 35 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 36 37