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Results from IceCube

Patrick BerghausUniversity of Delaware

Patrick BerghausResults from IceCube

 USA:   Bartol Research Institute, Delaware  Univ. of Alabama  Pennsylvania State University  UC Berkeley  UC Irvine  Clark­Atlanta University  Univ. of Maryland  Georgia Tech  Ohio State University  University of Wisconsin­Madison  University of Wisconsin­River 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

Barbados: University of the 

West IndiesBelgium: Vrije Universiteit Brussel Université Libre de Bruxelles Universiteit Gent Université de Mons

Germany: Universität Mainz DESY­Zeuthen Universität Dortmund Universität Wuppertal Humboldt­Universität Berlin RWTH Aachen Universität Bonn Ruhr­Universität Bochum

Japan:Chiba University

New Zealand: University of Canterbury

Antarctica: Amundsen­Scott Station

Canada: University of Alberta

Switzerland:EPF Lausanne

IceCube Collaboration: > 250 People

Patrick BerghausResults from IceCube

IceTop (Surface Array):●2 Surface Tanks per InIce String 

●2 DOMs per Tank

●2010: 2x73 Tanks Installed

DeepCore (Low Energy):●6 Strings●DOMs have 50% higher q.e. (34%)●DOM Spacing 7 meters

InIce:●1 km3 instrumented●4800 DOMs, 17 meter spacing●80 strings●2010: 73 Strings deployed

IceCube: 3 Components

Surface:2835 m a.s.l

-1450 m

-2450 m

-2620 m

Patrick BerghausResults from IceCube

IceCubeAMANDA(until 2009)

Runway

DeepCore

South Pole

Location: South Pole

Patrick BerghausResults from IceCube

PMT:  10” HamamatsuDigitization: ATWD (custom): 300 Mhz / 400nsFADC:     40MHz / 6,400nsNoise Rate: 650Hz

12-LED 12-LED flasher flasher boardboard

Main Board

Digital Optical Module (DOM)

Waveform(CR Data)

PMT

400 ns

Patrick BerghausResults from IceCube

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EventTypes

Neutrino-Induced Muons(100 per hour)

CR Air Showers(2000 per second)

ApproximateValues for IC80(Trigger Level)

Neutrino-InducedCascades (had/em)

(<1 per day)

Patrick BerghausResults from IceCube

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All Sky Muon Flux (IC22, 2008)

arXiv:0902.0021

Neutrinos

Muons106

Patrick BerghausResults from IceCube

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7+ Decades in Energy

IceCube Neutrino Physics

Oscillations Gamma-Ray Bursts

Active Galactic Nuclei GZK Neutrinos(CMB Interactions)

Galactic Sources(Supernova Remnants?)

AtmosphericCharm Production

Dark Matter QG

Patrick BerghausResults from IceCube

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Primary Interaction (?)

Muon Track

Muon Neutrino

Size: PMT Signal

Color: Time

Angular Resolution< 1°

Energy Resolution:0.3 in log

10E

Patrick BerghausResults from IceCube

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Size: PMT Signal

Color: Time

Neutrino-Induced Cascade

Reconstructed Energy:

80 TeV

fullycontained

Energy Resolution:0.1 in log

10E

Patrick BerghausResults from IceCube

Neutrino Point Sources

X

CR Air Shower Array

direction scrambledby interstellar/-galactic

magnetic field

Cherenkov Telescope

ambiguity with purelyelectromagnetic

processes

Astrophysical Hadron Accelerator

Neutrino Telescope

“Smoking Gun”for hadronicacceleration

Patrick BerghausResults from IceCube

Sky Coverage

A. Gross, MPIK-HD

Galactic Equator

Patrick BerghausResults from IceCube

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Below Horizon:Data dominated by atmospheric NeutrinosEnergy Range 10s-100s of TeV

Above Horizon:Data dominated by atmospheric MuonsEnergy Range >PeV, increasing with angle

IC40 Point Source Search-log

10p: 5.28

prandom

: 18%

J. Dumm et al., UW

Patrick BerghausResults from IceCube

Neutrino Point Source Flux Limits

Further Analyses:

Flare Searches

Multi-Wavelength

Target-of-Opportunity

Optical Follow-Up

Source Stacking

Patrick BerghausResults from IceCube

PRELIMINARY

Based on 117 satellite-detectedGamma-Ray Bursts

Search for coincidentneutrino events

Burst parameters individually modeled

IceCube limit approaches“standard” Waxman-Bahcall neutrino emission model

Triggered GRB Search

Patrick BerghausResults from IceCube

Indirect Dark Matter Searches

Neutralino(Kaluza-Klein)

Pair Annihilation

in

Sun(Earth,

Galactic Center,Galactic Halo)

Allowed Region fromDirect Measurements

(Cryogenic)

IC80+DC6 (expected)

Patrick BerghausResults from IceCube

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Electromagnetic Particles(10s-100s of MeV)

LE Muons(1-10 GeV)

HE Muons(TeV)

Shower Axis

IceTop

InIcePrimary Energy: 1-100s PeV

InIce Muon Multiplicity: 10s-1000s

Ratio depends onPrimary Mass

CR Physics

Patrick BerghausResults from IceCube

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Electromagnetic Particles(10s-100s of MeV)

LE Muons(1-10 GeV)

HE Muons(TeV)

Shower Axis

IceTop

InIcePrimary Energy: 1-100s PeV

InIce Muon Multiplicity: 10s-1000s

CR “Knee”

astro-ph/0210453

Primary composition becomes heavier

Ratio depends onPrimary Mass

CR Physics

Patrick BerghausResults from IceCube

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Size: PMT Signal

Color: Time

IC79 CR ShowerShower core fully

containedin IceTop array

High-MultiplicityHE Muon Bundle

In InIce/DeepCore

Patrick BerghausResults from IceCube

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IceTop/InIce Energy Correlation

<QMC

(A)>

= <Q

data>

<log A> = Heat

Eprim

≈ 10PeV

PRELIMINARY

IceTop (EM)

InIce(HE muons)

Patrick BerghausResults from IceCube

PRELIMINARY

CR AnisotropyFirst measurement

in the southernhemisphere, consistent

with northern results

“Hot Spots”from nearby

Sources?

Thank youfor your

attention!

Patrick BerghausResults from IceCube

backup

Patrick BerghausResults from IceCube

CR

muons

Moon ShadowMoon Shadow seenwith >6significance

Patrick BerghausResults from IceCube

Neutrino Effective Area

Patrick BerghausResults from IceCube

Angular Resolution (Muon Neutrinos)

50%

224080 String Configuration