C. Spiering, Leeds, July 23, 2004

Entrance to the Promised Land after 40 Years !

Moisej Markov Bruno Pontecorvo

M.Markov,1960: We propose to install detectors deep in a lake or in the sea and to determine the direction of charged particles with the help of Cherenkov radiation

Pioneering

DUMANDFred Reines

John Learned

~ 1975: first meetings towards an underwater array close to Hawaii

+ Roberts, Stenger, Gorham, ..

DUMAND-II Proposal 1988 : - 216 PMTs at 9 strings - height 230 m

Alas !... terminated in 1996

1987: DUMAND test stringLater used by Amanda and Baikal

Search for diffuse excess of extra-terrestrial high energy neutrinos

bound

WB bound

log E /GeV

DUMAND

FREJUSMACRO

Neutrino Telescopes

UndergroundKGF

Baksan

FREJUS

IMB

Kamiokande Superkamiokande

MACRO ~ 1000 m²

e.g. MACRO, 1356 upgoing muons

Pioneering

BAIKAL

G. Domogatsky

Bezrukov, Domogatsky Berezinsky, Zatsepin

1981 first site explorations1984 first stationary string1993 first neutrino detector

NT-361994 first atm. neutrino

separated1998 NT-200 finished

~ 2x Super-K for 1 TeV muons

CampIce as a natural deployment platform

NT-200

3600 m

1366

m

4-string stage (1996)

Baikal Search for H.E.Cascades

Look for upward moving light fronts.

Signal: isolated cascades from neutrino interactions

Background:Bremsshowers fromh.e. downward muons

NT-200

large effective volume

cascades

140 m

36 additional PMTs 4 times better sensitivity !

Baikal Upgrade NT200+

Mediterannean approaches

NESTOR (since 1991) „Amanda-sized“ -- under construction

ANTARES (since 1996)„Amanda sized“ -- under construction

NEMO: R&D for km3 project

Since 2003: joined km3 initiative KM3NET

4100m

2400m

3400mANTARESNEMO NESTOR

Beyond the DUMAND scale:

AMANDA

Francis Halzen

+ Steve Barwick, Bob Morse, ....

first site studies at South Pole ~ 1990shallow detector in bubbly ice 1993/4

10 strings (Amanda-B10) 1997

19 strings (Amanda-II) 2000

AMANDA-II

depth AMANDA

Super-K

DUMANDAmanda-II:677 PMTsat 19 strings

(1996-2000)

Ocean Water

DrillingHot water drillingHot water drilling

AMANDA Event

Signatures:Muons

AMANDA Event

Signatures:Muons

+ N + X

CC muon neutrinointeraction track

AMANDA Event

Signatures: Cascades

AMANDA Event

Signatures: Cascades

CC electron and tau neutrino interaction:

(e,,) + N (e, ) + X

NC neutrino interaction:

x + N x + X

Cascades

PRELIMINARY

First spectrum > 3 TeV:

- up to 100 TeV

- matches lower-energy Frejus data

Skyplot Amanda-II, 2000

697 eventsbelow horizon

above horizon:mostly fake events

AMANDA average flux limit for two assumedspectral indices , compared to the average gamma flux of Markarian 501 as observed in 1997 by HEGRA.

Intrinsic source spectrum(corrected for IR absorption)

AMANDA-II has reachedthe sensitivity needed tosearch from neutrino fluxesfrom TeV gamma sourcesof similar strength to theinstrinsic gamma flux.

Measured spectrum

1997 2000 2000+2001

Source Declination Nobs / Nbgr Nobs / Nbgr

SS433 5.0o - 0.7 0 / 2.38 2.3 1 / 1.69

M87 12.4o 17.0 1.0 0 / 0.95 3.8 2 / 1.10

Crab 22.0o 4.2 2.4 2 / 1.76 4.2 3 / 1.10

Mkn 421 38.2o 11.2 3.5 3 / 1.50 1.5 0 / 0.65

Mkn 501 39.8o 9.5 1.8 1 / 1.57 1.4 0 / 0.69

Cyg. X-3 41.0o 4.9 3.5 3 / 1.69 1.5 0 / 0.67

Cas. A 58.8o 9.8 1.2 0 / 1.01 4.7 2 / 1.03

90% C.L. upper limits (in units of 10-8cm-2s-1) for selected sourcesfor an E-2 spectral shape integrated above Eν=10 GeV

limitνΦ

PRELIMINARY

limitνΦ limit

νΦ

AMANDA skyplot 2000-2003 optimized for best sensitivity to E-3 – E-2 sources

3369 eventsPreliminary

Preliminary

Crab

Mk421

SS433

Mk501

M87

Cyg

Cas A

Preliminary

Selected Source Analysis

Stacking Source Analysis

Galactic Plane

Transient Sources

Burst Search

Correlation Analysis

Multi-Pole Analysis

Lower energy threshold (optimize to steeper spectra)

Expected sensitivity

for AMANDA 97-03

4 years Super-Kamiokande

8 years MACRO

-90 0-45 9045

10-15

10-14

cm-2 s

-1

declination (degrees)

southern sky

northern sky

SS-433

Mk-501 / ~ 1

170 days AMANDA-B10

230 days AMANDA-II

Measured sensitivity 00-03

bound

WB bound

DUMAND

FREJUSMACRO

Amanda-B10 (1997)

Expectation Amanda-II, 3 years

Expectation IceCube, 3 years

Experimental Limits

Amanda-II (2000)

Amanda-II (2000) cascades

Baikal (98,99,00)

Amanda-B10 (1997), UHE

In red: only muonsIn blue: all flavorsIn red: only muonsIn blue: all flavors

bound

WB bound

bound

WB bound

e:: = 1:2:0 1:1:1e:: = 1:2:0 1:1:1

bound

WB bound

bound

WB bound

bound

WB bound

Experimental all-flavor limits

bound

WB bound

DUMANDFREJUS

MACRO

Amanda-B10 (1997)

Expectation Amanda-II, 3 years

Expectation IceCube, 3 years

Amanda-II (2000) Amanda-II (2000) cascades

Baikal (98,99,00)

Amanda-B10 (1997), UHE

Year # of GRB

Bkgd seen

events

1997 78 0.06 0

1998 99 0.20 0

1999 96 0.20 0

2000 44 0.40 0

Total 218 0.86 0t=0+1h

Waxman/Bahcall 99

- Low background (due narrow time and space coincidence)

- Large effective areas (50 000 m² @ 1 PeV)

Upper limit:

16 · Waxman/Bahcall flux

-1 hour +1 hour

Background determined on-source/off-time Background determined on-source/off-time

10 min

Blinded Window

Neutrinos fromthe Sun

Amanda

At South Pole the Sun sinks maximally 23° below horizon. Therefore only Amanda-II with its dramatically improved reconstruction capabilities for horizontial tracks (compared to Amanda-B10) can be used for solar WIMP search.

Indirect Search for WIMPs

Present upper limits and expected IceCube sensitivity on muon flux from

neutralino annihilations in center of Sun

Disfavored

by direct search

Search for relativistic magneticmonopoles

10-16

10-15

10-14

10-18

10-17

= v/c

1.000.750.50

up

per

lim

it (

cm-2 s

-1 s

r-1)

Cherenkov-Light n2·(g/e)2

n = 1.33

(g/e) = 137/ 2

8300

KGF

Soudan

MACRO

Orito

Baikal-98,99,00

Amanda-97

IceCube

electrons

Supernova-MonitorAmanda-II

Amanda-B10

IceCube0 5 10 sec

Count rates

B10: 60% of Galaxy

A-II:95% of Galaxy

IceCube:Up to LMC

The km3 scale at South Pole

IceCube- 80 Strings- 4800 PMTs - Instrumented

Volume: 1 km3

- Installation: 2005-2010

6 Amanda modules

Super- Kamiokande (Japan)

AMANDA-II

IceCube

IceCube Eff Area

cos

Ae

ff /

km2

IceCube Effective Area

IceTop + IceCube: 1/3 km2 sr ….. for coincident tracks

VETO against

all downward events E > 300 TeV with trajectories inside IceTop

CALIBRATION

of angular response and geometry with tagged muons

CHEMICAL COMPOSITION

in energy range 1015 eV – 1018 eV

Cosmic rays

Amanda/Spase

IceCube/IceTop

... investigatestransition toextra-galactic CR

-90 0-45 9045

10-15

10-14

cm-2 s-1

SS-433

Mk-501

/ ~ 1

10-17

10-16

2001

2007

2003

2012

Achieved andexpected sensitivitiesto steady point sources

GX339-4

Super-K,MACRO

AntaresNestor ?

IceCubeKM3 in Mediterr.

AMANDA

RICE AGASA

Amanda, Baikal2002

2007

AUGER

Anita

AABN

2012

km3

EUSOAugerSalsa

2004

RICE AGASA

Achieved and expected sensitivities to diffuse fluxes

„Nothing is guaranteed, but history is on our side.“

Francis Halzen

Moses HAD a guarantee forfinal success

... but saw the promised landonly from far and neverentered it by himself.

With nearly 3 orders of magnitude improvementover 10 years we have a good chance for success before OURretirement !