Years of AMANDA-II Tyce DeYoung Department of Physics and Center - PowerPoint PPT Presentation

Years of AMANDA-II Tyce DeYoung Department of Physics and Center for Particle Astrophysics Penn State University for the IceCube Collaboration Neutrino ‘08 Christchurch, New Zealand

The IceCube Collaboration The IceCube Collaboration AM University of Alaska, Anchorage Stockholms Universitet University of California, Berkeley Uppsala Universitet University of California, Irvine Vrije Universiteit Brusse Clark-Atlanta University Université Libre de Brux University of Delaware / Bartol Universiteit Gent Research Institute Université de Mons-Hai University of Kansas Lawrence Berkeley Natl. Laboratory Chiba University University of Maryland Pennsylvania State University Southern University and A&M College University of Canterbury University of Wisconsin, Madison Christchurch University of Wisconsin, River Falls Universiteit Utrecht RWTH Aachen DESY, Zeuthen Universität Dortmund EPF Lausanne MPIfK Heidelberg Humboldt Universität zu Berlin Universität Mainz Oxford University

Neutrino Sources Neutrino Sources AM HESS, Astron. Astrophys. 2007 P. Mészáros, Science 2001 Gamma Ray Bursts Supernova Remnants M87, HST 1994 NASA/STScI Artist’s conception of binary merger (NASA/Swift)

Optica target nucleon modul • In the collision a relativistic lepton is produced • The lepton emits Cherenkov light • Optical sensors capture and map the light Cherenkov Muon light cone

The AMANDA Detector The AMANDA Detector NDA 77 OMs on 19 strings 77 OMs on 19 strings Hamamatsu 8” PMT in Hamamatsu 8” PMT in top view glass pressure vessel glass pressure vessel 200 m Several readout systems Several readout systems (electrical, fiber-optic) (electrical, fiber-optic) DAQ electronics on surface DAQ electronics on surface Deployed in stages: Deployed in stages: AMANDA-II AMANDA-II complete in 2000 complete in 2000 Optical Modu

AMANDA- -II Data Set II Data Set AMANDA AM 1996 1997 AMANDA-B operations results from 4 string, 10 string and 13 string phases 1998 1999 AMANDA-II complete Phys.Rev.Lett.92:071102 2004 2000 Year Livetime 2000 197 d Phys.Rev.D71:077102 2005 2001 2001 193 d Phys.Rev.D75:102001 2007 2002 2002 204 d 2003 213 d 2003 2004 194 d 2004 2005 199.3 d 2005 2006 187 d Total 3.8 yr 2006

Atmospheric Neutrinos Atmospheric Neutrinos AM Statistical unfolding of atmospheric muon neutrino spectrum Preliminary – Based on observed muon energies at detector Consistent with theoretical models Limit placed on possible high energy component – Would appear as excess above expected atmospheric flux

Atmospheric Neutrinos Atmospheric Neutrinos AM Analysis of full 7-year data set underway Preliminary sensitivity Prelimina simulated best fit 99% C.L. excluded 90% C.L. allowed

Point Source Search Point Source Search AM Raw skymap, 6595 events Preliminary Final results based on unbinned max likelihood method – Reconstruction uncertainty from eventwise shape of likelihood

Event Parameters Event Parameters AM Preliminary Preliminary Ratio of likelihood to best downgoing likelihood Estimated angular error Prelim- inary Preliminary

Full Sky Source Search Full Sky Source Search AM Preliminary δ =90º Max Significance δ =54º, α =11.4h ax significance .73 σ → 1.5 σ 3.38 σ 24h 0h 0 1 2 3 4 5 Significance 5 yr max significance 3.74 σ → 2.8 σ – All significances pre-trials – 95 of 100 background maps (data randomized in RA) have a point with significance ≥ 3.38 σ

Sensitivity Sensitivity AM Preliminary Preliminary Energy Range (90%): 1 TeV – 3 PeV

Source Catalog Search Source Catalog Search AM List of 26 sources selected a priori Preliminary Source P-value μ 90 90% C.L. limits of Crab Nebula 4.47 0.10 E 2 Φ < μ 90 x 10 -11 TeV cm -2 s -1 MGRO J2019+37 4.75 0.077 Mrk 421 1.26 0.82 Mrk 501 3.56 0.22 Upward fluctuations: LS I +61 303 7.21 0.033 LS I +61 303 Geminga 6.07 0.0086 Geminga MGRO J2019+37 1ES 1959+650 3.38 0.44 M87 2.18 0.43 Downward fluctuations: Cyg X-1 2.00 0.57 Mrk 421 probability of p ≤ 0.0086 for at least one of 26 sources is 20%

GRB Search GRB Search AM search: ver 400 Northern Cascade Cascade Hemisphere GRBs Cascade Cascade (rolling) (rolling) (trig’ ’d & rolling) d & rolling) (trig ascade search riggered search with 73 GRBs Rolling search for 2001-2003 R03b R03a: Razzaque et al. choked burst model MN06 WB03 search μ search ν μ ν R03b: Razzaque et al. supranova model WB03: R03a Waxman-Bahcall model MN06: Murase-Nagataki internal shock model

Diffuse Neutrino Limits Diffuse Neutrino Limits AM ν μ + ν μ flux UHE 2003-04 (prelim) Diffuse ν μ UHE 2000-02 2000-03 unfolded ν μ Waxman-Bahcall 2000-03 Full IceCube 1 yr limits assume 1:1:1 flavor rat

SM SM AM VLI Sensitivity (preliminary) Use large atmospheric 99% C.L. neutrino sample, look excl. for ν μ disappearance 90% C.L. allowed – Violation of Lorentz invariance – Quantum decoherence Muon neutrino survival probability QD Sensi VLI oscillations, (prelimina δ c/c = 10 -27 Conventional oscillations 90% C.L. 99% C.L

Solar WIMP Search Solar WIMP Search Solar WIMP Search χ velocity distribution ρ χ ν interactions σ scatt ν μ Γ capture Sun annihilation Γ annihilation channels μ μ live and Srednicki, ’85

Solar WIMP Search Solar WIMP Search AM Based on 2003 data set – WIMP decay mode affects expected muon spectrum – Hard: χχ → bb – Soft: χχ → W + W – (or χχ → τ + τ – ) Also searching for WIMP annihilation in center of Earth

IceCube + AMANDA IceCube + AMANDA AM Region with dense instrumentation, AMAN lower energy threshold Outer IceCube strings form veto volume Improved DAQ Significant improvement (Transient v at 30-100 GeV Waveform Digitizers) Muon neutrino events, E ν < 10 TeV Analysis underway (2007 data to present)

IceCube Deep Core IceCube Deep Core AM Extend IceCube sensitivity to Effective area neutrinos with (trigger level) energies below a few hundred GeV IceCube – Replacement for with Deep AMANDA Core – Six strings with 60 IceCube high-QE PMTs each – Use very clear ice at bottom of IceCube See poster by D.

Deep Core WIMPs Deep Core WIMPs AM Example: solar WIMPs with Deep Core – 5 year sensitivity – Significantly increased sensitivity IceCube to WIMPs with + Deep masses below Core 200 GeV – Probe SUSY models inaccessible to current direct searches (e.g.

Summary Summary AM Final seven year AMANDA-II analysis nearly complet Point source search results to be published soon – 3.8 yr total exposure Results for other analyses available, final results coming – Diffuse fluxes, GRBs, WIMPs, physics beyond Std Model AMANDA now operating as a component of IceCube – Extended low energy sensitivity Deep Core will be deployed in two coming seasons – Significant improvement on AMANDA+IceCube – AMANDA will be decommissioned