CIPANP 2006K. Filimonov, UC Berkeley From AMANDA to IceCube: Neutrino Astronomy at the South Pole Kirill Filimonov University of California, Berkeley

CIPANP 2006K. Filimonov, UC Berkeley USA: Bartol Research Institute University of Alabama Pennsylvania State University University of California – Berkeley University of California – Irvine Clark-Atlanta University University of Maryland Institute for Advanced Study University of Wisconsin-Madison University of Wisconsin-River Falls Lawrence Berkeley National Lab University of Kansas Southern University and A&M College Sweden: Uppsala Universitet Stockholm Universitet In March 2005, AMANDA merged into the IceCube collaboration UK: Imperial College Oxford University Netherlands: Utrecht University Belgium: Université Libre de Bruxelles Vrije Universiteit Brussel Universiteit Gent Université de Mons-Hainaut Germany: Humboldt Universität Universität Mainz DESY-Zeuthen MPIfK Heidelberg Universität Dortmund Universität Wuppertal Universität Berlin Japan: Chiba University New Zealand: University of Canterbury The IceCube Collaboration Antarctica: Amundsen Scott South Pole Station The IceCube Collaboration 250 scientists from 30 Institutions

CIPANP 2006K. Filimonov, UC Berkeley Why Neutrino Astronomy? 100 TeV photons travel ~10 Mpc 1 PeV photons travel 10’s of kpc

CIPANP 2006K. Filimonov, UC Berkeley Neutrino Detection Track length: O(1 km) Pointing Resolution: AMANDA ~ 1.5° - 2.5°, IceCube < 1° Energy Resolution: AMANDA ~ , IceCube < 0.3 in log(E) e, ,  e, ,  Z N N “Point” sources: O(10 m) Pointing Resolution: AMANDA ~ 30° - 40° Energy Resolution: AMANDA ~ in log(E)  W N e,  e,  W N Upgoing  tracks (  )Cascades ( e  CC, e  NC)

CIPANP 2006K. Filimonov, UC Berkeley AMANDA Status South Pole Dome Summer camp AMANDA Road to work 1500 m 2000 m [not to scale] IceCube Skiway Operation 2000-Present (Current Configuration) 19 strings, 677 Optical Modules Diameter of ~200m, height 500m

CIPANP 2006K. Filimonov, UC Berkeley 1. MACRO [x3] 2. AMANDA B10  (1997) [x3] 3. AMANDA-B10 UHE (1997) 4. AMANDA-II cascades (2000) 5. Baikal cascades AMANDA-II  -analysis (2000) [x3] 7. AMANDA-II UHE sensitivity 8. AMANDA  -analysis ( ) sensitivity [x3] Preliminary! Diffuse Neutrino Flux Limits No astrophysical neutrinos observed: need bigger detector 1:1:1n flavor ratio

CIPANP 2006K. Filimonov, UC Berkeley Search for Point-Like Sources AMANDA II preliminary data from (1001 live days) 4282 from northern hemisphere Significance map 24h 0h 15 o 30 o 45 o 60 o 75 o Randomized (time scrambled) data 24h 0h 15 o 30 o 45 o 60 o 75 o No significant excess found 1ES Crab Nebula Markarian 501 source nr. of n events (5 years) expected background (5 years) flux upper limit F 90% (E n >10 GeV) [10 -8 cm -2 s -1 ] Markarian ES Crab Nebula

CIPANP 2006K. Filimonov, UC Berkeley Other AMANDA Results GRB signal search (time and direction from satellites) Atmospheric neutrinos Cosmic ray muon spectrum Dark Matter search (WIMP annihilation in Earth or Sun) Supernova (galactic) monitoring

CIPANP 2006K. Filimonov, UC Berkeley AMANDA 500 m Only IceTop tank InIce string & IceTop AMANDA-II IceCube IceTop IceCube: km 3 Detector AMANDA-II: OMs on 19 strings IceCube: 2005-… InIce Array: 4800 DOMs, 80 strings – m deep – 17 m spacing – 125 m hexagonal grid Feb 2006: 9 strings deployed Surface Array: 320 IceTop DOMs - 80 pairs of surface frozen water tanks Feb 2006: 32 tanks deployed

CIPANP 2006K. Filimonov, UC Berkeley View of the Drilling Site Hose Reel Drill Tower IceTop Tanks 5MW Hot Water Generator Drilling ICECUBE 2450 m AMANDA TIME (hours) DEPTH (meters)

CIPANP 2006K. Filimonov, UC Berkeley

CIPANP 2006K. Filimonov, UC Berkeley

CIPANP 2006K. Filimonov, UC Berkeley IceTop Tanks

CIPANP 2006K. Filimonov, UC Berkeley “Standard Candle” Light Calibration Source Nitrogen (337 nm) pulsed (4ns) laser Cone reflected Pointing-up PeV n e cascade equiv.

CIPANP 2006K. Filimonov, UC Berkeley Event samples in 9 strings IceTop-InIce Event Downgoing Muon EventUpgoing Neutrino Event

CIPANP 2006K. Filimonov, UC Berkeley Summary/Conclusions 1 st km 3 neutrino detector is becoming a reality Successful drilling/deployment – 4 days/string –survival upon freeze-in: 99% 14 strings/year are projected to be deployed Completion of IceCube construction in 2011

CIPANP 2006K. Filimonov, UC Berkeley Backups

CIPANP 2006K. Filimonov, UC Berkeley 33 cm Benthosphere 25 cm PMT 75 ns delay board main board LED flasher board HV PMT base HV generator Digital Optical Module 4W

CIPANP 2006K. Filimonov, UC Berkeley Simulated Event Signatures in IceCube 10 PeV  (500 m  track) 375 TeV e 6 PeV    +N ® t +X  ®  + X 

CIPANP 2006K. Filimonov, UC Berkeley Diffuse neutrino flux limits