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

CIPANP 2006 K. Filimonov, UC Berkeley

From AMANDA to IceCube: Neutrino Astronomy at the

South Pole

Kirill Filimonov University of California, 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 Collaboration250 scientists from 30 Institutions


Why Neutrino Astronomy?

100 TeV photons travel ~10 Mpc 1 PeV photons travel 10’s of kpc


Neutrino Detection

• Track length: O(1 km)• Pointing Resolution: AMANDA ~ 1.5° - 2.5°, IceCube < 1°

• Energy Resolution: AMANDA ~ 0.3 - 0.4, IceCube < 0.3 in log(E)

e,, e,,

Z N N

• “Point” sources: O(10 m) • Pointing Resolution:

AMANDA ~ 30° - 40°• Energy Resolution:

AMANDA ~ 0.1 - 0.2 in log(E)

WN N

e, e, WN N

Upgoing tracks () Cascades (e CC, e NC)


AMANDA Status

South South PolePole DomeDome

Summer campSummer campAMANDAAMANDA

Road to Road to workwork

1500 1500 mm

2000 m2000 m

[not to scale][not to scale]

IceCube

IceCube

SkiwaySkiway

Operation 2000-Present (Current Configuration)Operation 2000-Present (Current Configuration)

19 strings, 677 Optical ModulesDiameter of ~200m, height 500m


1. [ 3]MACRO x

2. 10 AMANDA B (1997) [ 3]x

3. - 10 AMANDA B UHE(1997)

4. - AMANDA II cascades(2000)

5. 1998-Baikal cascades2002

6. - AMANDA II - analysis(2000) [ 3]x

7. - AMANDA II UHE sensitivity

8. AMANDA - analysis(2000-2003) sensitivity[ 3]x

!Preliminary

Diffuse Neutrino Flux Limits

No astrophysical neutrinos observed: need bigger detector

1:1:1n flavor ratio


Search for Point-Like Sources

AMANDA II preliminary data from 2000-2004 (1001 live

days)4282 from northern hemisphereSignificance map

24h 0h

15o

30o

45o

60o75o

-3

-2

-1

0

12

3

Randomized (time scrambled) data

24h 0h

15o

30o

45o

60o75o

-3

-2

-1

0

12

3

No significant excess found

1ES 1959+650

Crab NebulaMarkarian 501

sourcenr. of n events

(5 years)

expectedbackground

(5 years)

flux upper limit F90%(En>10 GeV)

[10-8cm-2s-1]

Markarian 501 8 6.39 0.85

1ES1959+650 5 4.77 0.78

Crab Nebula 10 6.74 1.01


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


AMANDA500 m

Only IceToptank

InIce string& IceTop

AMANDA-IIIceCube

IceTop

IceCube: km3 Detector

AMANDA-II: 2000-...• 677 OMs on 19 strings

IceCube: 2005-…• InIce Array: 4800 DOMs, 80 strings

– 1450-2450 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


View of the Drilling Site

Hose Reel

Drill Tower

IceTop Tanks

5MW Hot Water Generator

Drilling

ICECUBE2450 m

AMANDA

TIME (hours) 0 24 48 72 96 120 144

DE

PT

H (

met

ers)




IceTop Tanks


“Standard Candle”Light Calibration Source

• Nitrogen (337 nm) pulsed (4ns) laser

• Cone reflected• Pointing-up• 0.5-50 PeV ne

cascade equiv.


Event samples in 9 strings

IceTop-InIce Event Downgoing Muon Event Upgoing Neutrino Event


Summary/Conclusions

• 1st km3 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


Backups

CIPANP 2006 K. Filimonov, UC Berkeley33 cm Benthosphere

25 cm PMT

75 ns delay board

main board

LED flasher board

HV PMT base

HV generator

Digital Optical Module

4W


Simulated Event Signatures in IceCube

10 PeV

(500 m track)375 TeV e6 PeV

+N ® t+X

®+ X


Diffuse neutrino flux limits

Documents

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