for the IceCube Collaboration

Transcription

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

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

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

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

5 The ANDA Detector DA 7 OMs on 19 strings amamatsu 8 PMT in glass pressure vessel everal readout systems (electrical, fiber-optic) AQ electronics on surface top view 200 m Deployed in stages: ANDA-II complete in 2000 Optical Modu

6 ANDA-II Data Set ANDA-B operations results from 4 string, 10 string and 13 string phases ANDA-II complete Phys.Rev.Lett.92: Phys.Rev.D71: Phys.Rev.D75: Year Livetime d d d d d d d Total 3.8 yr

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

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

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

10 Event Parameters Preliminar Preliminary Ratio of likelihood to best downgoing likelihood Estimated angular error Preliminary

11 Full Sky Source Search x significance 3σ 1.5σ Preliminary δ=90º Max Significance δ=54º, α=11.4h 3.38σ h 0h Significance All significances pre-trials 5 yr max significance 3.74σ 2.8σ 95 of 100 background maps (data randomized in RA) have a

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

13 Source Catalog Search probability of p for at least one of 26 sources is 20% List of 26 sources selected a priori Preliminary Source μ 90 P-value Crab Nebula MGRO J Mrk Mrk LS I Geminga ES M Cyg X % C.L. limits of E 2 Φ < μ90 x TeV cm -2 s -1 Upward fluctuations: LS I Geminga MGRO J Downward fluctuations: Mrk 421

14 GRB Search earch: er 400 Northern misphere GRBs cade search ggered search with 73 GRBs lling search for Cascade (rolling) Cascade (trig d d & rolling) R03a: Razzaque et al. choked burst model R03b: Razzaque et al. supranova model WB03: Waxman-Bahcall model MN06: Murase-Nagataki internal shock model νμ R03a search WB03 R03b MN06

15 Diffuse Neutrino Limits limits assume 1:1:1 flavor ra νμ + νμ flux UHE (prelim) Diffuse νμ unfolded νμ Waxman-Bahcall UHE Full IceCube 1 yr

16 Use large atmospheric neutrino sample, look for νμ disappearance SM Violation of Lorentz invariance Quantum decoherence VLI Sensitivity (preliminary) 99% C.L. excl. 90% C.L. allowed Muon neutrino survival probability VLI oscillations, δc/c = QD Sensi (prelimina Conventional

17 olar WIMP Search χ velocity distribution ρ χ ν interactions σ scatt capture Γ annihilation Sun annihilation channels ν μ μ

18 Solar WIMP Search 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

19 IceCube + ANDA Region with dense instrumentation, lower energy threshold Outer IceCube strings form veto volume Improved DAQ (Transient Waveform Digitizers) Analysis underway (2007 data to present) Significant improvement at GeV Muon neutrino events, Eν < 10 TeV AN v

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

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

22 Summary Final seven year ANDA-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 ANDA now operating as a component of IceCube Extended low energy sensitivity Deep Core will be deployed in two coming seasons Significant improvement on ANDA+IceCube