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University of Wisconsin, Madison

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Presentation on theme: "University of Wisconsin, Madison"— Presentation transcript:

1 University of Wisconsin, Madison
AMANDA and IceCube Patrick Berghaus University of Wisconsin, Madison

2 IceCube: People Germany: Sweden: USA: UK: Netherlands: Belgium: Japan:
Bartol Research Institute, Delaware Univ. of Alabama Pennsylvania State University UC Berkeley UC Irvine Clark-Atlanta University Univ. of Maryland IAS, Princeton University of Wisconsin-Madison University of Wisconsin-River Falls LBNL, Berkeley University of Alaska, Anchorage University of Kansas Southern University and A&M College, Baton Rouge, Louisiana Sweden: Uppsala Universitet Stockholm Universitet UK: Oxford University Netherlands: Universiteit Utrecht Belgium: Vrije Universiteit Brussel Université Libre de Bruxelles Universiteit Gent Université de Mons-Hainaut Germany: Universität Mainz DESY-Zeuthen Universität Dortmund Universität Wuppertal Humboldt-Universität Berlin RWTH Aachen Japan: Chiba University New Zealand: University of Canterbury Antarctica: Amundsen-Scott Station

3 IceCube: Hardware IceTop(Air Showers): Amanda: InIce:
2 Surface Tanks per InIce String, 2 DOMs per Tank 2008: 80 Tanks Installed Amanda: Ø=200m, h=500m (0.02 km³) 677 OMs on 19 Strings (from 2000) InIce: 1 km3 instrumented 4800 Digital Optical Modules (DOMs) on 80 strings 2008: 40 Strings deployed (“IC40”)

4 DeepCore (2008/09-) 2008/09 2009/10 South Pole AMANDA IceCube
6+ Strings High-Energy Extension (10 strings) Runway 2008/09 2009/10 South Pole AMANDA (until 2009) IceCube

5 String Deployment 2 Days 2.5km Cable 5 MW Power

6 (Very Basic) Detection Principle Muon Interaction Neutrino
Cherenkov Cone

7 Neutrino Physics atmospheric neutrinos AGN WIMPs galactic sources GRB
C. Finley/J. Dumm, UW atmospheric neutrinos WIMPs oscillation galactic sources AGN GRB UHE diffuse flux

8 Coincident Muons 25Hz Atmospheric Muons 500Hz Muons From Neutrinos
up to 10s of meters Muons From Neutrinos ≃20/h

9 Background

10 Event Filters 70°

11 dust peaks correspond to cold periods
Ice 60ky K. Woschnagg, LBNL dust peaks correspond to cold periods during last Ice Age 40-60ky regular ice dust layer clear ice Depth of Track (Muons near Horizon) FLUX Average Ice Parameters (l=400nm): Absorption: ~110m Scattering: ~20m

12 Analyses

13 Atmospheric Neutrinos
K. Muenich, Uni Dortmund diffuse analysis MPR: Mannheim/Protheroe/Rachen AGN Model Unfolded Energy Spectrum Consistent with Theory Only proven AMANDA/IceCube neutrino source

14 WIMPs Neutralino Pair Annihilation IceCube (hoped for)

15 GRBs 080319B IC9 only expected signal: ≈0.1 events L. Gerhardt, LBNL
R03a: Choked Burst Model R03b: Supranova Model WB03: Waxman-Bahcall MN06: Murase-Nagataki L. Gerhardt, LBNL 080319B IC9 only expected signal: ≈0.1 events

16 Diffuse Neutrino Flux Charm, Composition... Latest Result
(4-year AMANDA) astro-ph/ Charm, Composition... WB Flux 1 Year IC80 (estimated) J. Hodges, UW (PhD Thesis)

17 Point Sources

18 Sources: Sky Map A. Gross, MPIK-HD

19 Final AMANDA Result 2000-2006, 3.8y livetime
95% of randomized skies have a higher maximum significance! Maximum Significance DEC=54o, RA=11.4h “3.38” Significance J. Braun, UW

20 Flux upper limit for  = 0 E-2
26 sources selected to reduce trial factor No indication for neutrino point sources (consistent with random sky) Source Excess parameter -log10 P Flux upper limit for  = 0 E-2 90% CL [10-11 TeV cm-2s-1] Markarian 421 0.82 1.26 Markarian 501 0.22 3.56 1ES 0.44 3.38 M87 0.43 2.18 AGN 3C273 0.086 4.17 SS433 0.64 1.57 LSI 0.033 7.21 Cygnus X-1 0.57 2.00 Cygnus X-3 0.29 3.28 Cassiopeia A 0.67 1.93 Crab Nebula 0.10 4.47 m-QSO Geminga 0.0086 6.07 SNR Probability: 20%

21 60% of random skies have higher significance
IC9 Point Source Search Flux limit: IC9 ≃ AMANDA 60% of random skies have higher significance Source: C. Finley, UW

22 IC22 Point Source Search Sensitivity Discovery Binned (DESY-Zeuthen)
C.Finley/ J.Dumm, UW Discovery C.Finley/J. Dumm, UW Unbinned (UW Madison) Binned (DESY-Zeuthen) Sensitivity

23 AMANDA/IceCube Evolution PSF[°] 4 2 2.5 1.5 0.8 (approx.) AMANDA B-10
A. Gross, MPIK-HD AMANDA B-10 IC9 AMANDA II IC22 IC80 (pred.)

24 CR Connection

25 Auger vs. IceCube Low Muon Multiplicity High Muon Multiplicity
High E-Threshold High Muon Multiplicity Low E-Threshold

26 Macro vs. IceCube Small Big High Multiplicity Rock Ice Large Area
No Shielding

27 Cosmic Rays IceCube Range 106 eV to ~1020 eV ~E-2.7 [GeV] ~E-3.1
T. Gaisser, ICHEP02 106 eV to ~1020 eV S. Lafèbre, PSU IceCube Range [GeV]

28 Muon Spectrum 70TeV

29 AMANDA Muons Fm(depth) Das Energieünföldingen 20TeV
J. Luenemann, Uni Dortmund 20TeV Das Energieünföldingen Fm(depth)

30 IceCube Muons ≃300 days IC22 atmospheric muons
° Zenith Angle Resolution atmospheric muons neutrino-induced muons K. Rosenau, P. Berghaus (UW)

31 IceCube uses SIBYLL SIBYLL ≈ Bartol Honda '06 Pions Kaons

32 Threshold Energy Vertical ≃400GeV top (70°) top (85°) Bottom (85°)
≃1PeV D. Chirkin, W. Rhode hep-ph/

33 IceCube Muon Rates Not Available Offline 1event/hour
Muons in IC22 above 1PeV

34 Energy Resolution m tracks, IC22 minimum ionizing
Source: D. Chirkin, UW

35 Essential Observables for Muon Spectrum:
Bundle Size Bundle Size: reject high-multiplicity showers Essential Observables for Muon Spectrum: dE/dx dE/dx: shower energy Slant Depth Slant Depth: mwe traversed

36 Physics Potential

37 Fm Not To Scale logEm Reference Flux p,K Production Atmosphere CR Flux
CR Composition Charm Fm logEm PeV TeV GeV Not To Scale

38 CR Composition ! Eprim,nucleon/Em≤10 median primary energy
(T.K.Gaisser, “CR&Part.Phys.”) ! median primary energy muon energy Composition Change at ≥few PeV

39 “Poly-Gonato” Model Steepening of Muon/Neutrino Spectrum above 100TeV
few PeV J.R. Hoerandel, astro-ph/

40 Prompt Flux Atmospheric n Diffuse n J. Hodges, UW Madison

41 Prompt Neutrinos CR Composition nm nm

42 Prompt Muons Conventional Muons (near horizon) <1PeV

43 Summary IceCube can detect Muons from all zenith angles
Muon and Neutrino spectrum up to PeV region measurable Sensitive to CR Composition around Knee And perhaps Charm Production in Atmospheric Showers

44 Backup Slides

45 hep-ph/

46 Digital Optical Module
PMT: 10” Hamamatsu Power: 3W Digitization: ATWD (custom): 300 Mhz / 400ns fADC: MHz / 6,400ns Dynamic Range: 200pe / 15ns Noise Rate: 650Hz 12-LED flasher board waveform Main Board

47 Integrated Exposure now 40 Strings! 1 km3 year by early 2009

48 Effective Area Factor 10 still to come! Earth Transparency CC NC W-res
C. Finley/J. Dumm, UW

49 Muons in CORSIKA MINOS Data 0705.3815 R. Birdsall, UW Madison

50 Unbinned Search J. Braun, UW Madison

51 Moon Shadow CR muons D. Boersma, L. Gladstone, UW PRELIMINARY

52 KASCADE Composition model-dependent astro-ph/

53 Prompt Neutrino Models
S. Klein, LBNL

54 High-pt Muons CR Composition pt≥3GeV/c ≥100m Separation
S. Klein, D. Chirkin ICRC 2007 High-pt Muons pt≥3GeV/c ≥100m Separation 1000+ year-1 in IC80 S. Klein,LBNL astro-ph/ A=1 A=10 CR Composition

55 2.5km 1.5km 4.4km (70°) 7.4km (70°) 17km (85°) 28km (85°)
King Haakon VII Plateau 4.4km (70°) 17km (85°) 2.5km 1.5km

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