AHigh Energy Neutrino

Astronomyfrom infancy to maturity

LAUNCH MeetingHeidelberg

Christian SpieringDESY

A

AHigh Energy Neutrino

Astronomyfrom infancy to

maturity

A

technological

A The ideaAMoisej 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

A The detection principle

muon tracks cascades

A Why neutrinos ?

0

....

pnp

e

pp

e

or

e : : ~ 1:2:0 changes to (typically) 1:1:1 at Earth

Travel straight (in contrast to CR)

Are not absorbed by IR or CMB (in contrast to gammas and CR)

Clear signature of hadronic nature

A Challenges

Low interaction cross section Need huge detection volumes Actual neutrino flux depends on target

thickness Predictions 25 years ago have been up to two

orders of magnitude higher than today 1990s: recognize need of cubic kilometer

detectors Now: cubic kilometer detectors will possibly

just scratch the interesting range

Martin Harwitt: „Would one have believed the tim

id

predictions of theoreticians, X-ray astronomy would

likely have started only a decade later.“

A Pioneering DUMAND

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

Test string 1987

Proposal 1988:The „Octagon“ (~ 1/3 AMANDA)

Termination 1996

A Pioneering Baikal

NT-200

3600 m

1366

m

1981 first site explorations 1984 first stationary string 1993 first neutrino detector NT-36 1994 first atm. Neutrino separated 1998 NT-200 finished

Ice as natural deployment platform

A

A Pioneering Baikal

A textbook neutrino4-string stage (1996)

cascades

140 m

Detection ofhigh energy

cascadesoutside the

instrumentedvolume

Fence theobservationvolume witha few PMTs

4 timesbetter sensitivityat high energies

NT200+

NT200+ running since 2006

A AMANDA

1990: first site studies at South Pole

1993/94 shallow detectors in bubbly ice

1997: 10 strings (AMANDA-B10)

2000: AMANDA-II

A AMANDA

Hot water drilling

A AMANDA

AMANDA-II

depth

Scattering

bubbles

dust

A AMANDA

+ N + X

AMANDA sykplot 2000-20033329 events below horizon

more on point sourcesin the following talk

A South and North

AMANDA & Baikal skyplot,galactic coordinates

A Parameters of neutrino telescopes

Effective area: ~ 0.1 m² @ 10 TeV ~ 1 m² @ 100 TeV ~ 100 m² @ 100 TeV

Point source sensitivity: AMANDA, ANTARES: ~ 10-10 / (cm² s) above 1 TeV IceCube: ~ 10-12 / (cm² s) above 1

TeV

AMANDA, ANTARES

IceCube

A IceCube

Dark sector

AMANDA

IceCube

Skiway

South Pole Station

GeographicSouth Pole

A IceCube

4800 Digital Optical Modules on 80 strings

160 Ice-Cherenkov tank surface array (IceTop)

1 km3 of instrumented Ice

Surrounding existing AMANDA detector

AHose reel Drill tower

Hot water

supply IceTop

Station

(2 tanks)Less energy and more than

twice as fast as old AMANDA

drill

A

A … not always easy

A IceCube Drilling & Deployment

A Status 2007

A Cumulative Instrumented Volume

0

0.5

1

1.5

2

2.5

3

3.5

4

4.5

5

2005 2006 2007 2008 2009 2010 2011 2012

Date

km3·

yr

0

10

20

30

40

50

60

70

80

# D

eplo

yed

Stri

ngs

km3·yr Strings Graph shows cumulative km3·yr of exposure × volume

1 km3·yr reached 2 years before detector is completed

Close to 4 km3·yr at the beginning of 2nd year of full array operation.

A

4100m

2400m

3400mANTARESNEMO NESTOR

The Mediterraneanapproach

A ANTARES

Neutrinocandidate

from5-stringdetector

A Physics from Baikal & AMANDA

Atmospheric neutrinos Diffuse fluxes Point sources see talk of Elisa Resconi

Coincidences with GRB Supernova Bursts & SNEWS WIMP indirect detection Magnetic monopoles …. ….

A Atmospheric neutrinos

Spectrum measured up to ~ 100 TeV

A Limit on diffuse extraterrestrial fluxes

Spectrum measured up to ~ 100 TeV

From this method and one year data we exclude E-2 fluxes with E2 > 2.710-7 GeV sr-1 s-1 cm-2

A Limit on diffuse extraterrestrial fluxes

Spectrum measured up to ~ 100 TeV

From this method and one year data we exclude E-2 fluxes with E2 > 2.710-7 GeV sr-1 s-1 cm-2

With 4 years and improved methods we are now at

E2 > 8.810-8 GeV sr-1 s-1 cm-2

A

MPR bound, no neutron escape (gamma bound)

Factor 11 below MPR bound for sources opaque to neutrons

Experimental limits & theoretical bounds

A

MPR bound, neutrons escape (CR bound)

Factor 4 below MPR bound for sources transparent to neutrons

Experimental limits & theoretical bounds

A

AGN core (SS)

AGN Jet (MPR)

GRB (WB)GZK

Experimental limits & theoretical bounds

A

AGN core (SS)

„old“ Stecker model excluded

old version

Experimental limits & theoretical bounds

AAGN core (SS, new version)

„new“ Stecker model not excluded

(MRF = 1.9)

Experimental limits & theoretical bounds

A

AGN Jet (MPR)

GRB (WB)

still aboveAGN jet (MPR)

(MRF ~ 2.3)

Experimental limits & theoretical bounds

A Limit on diffuse extraterrestrial fluxes

AMANDA HE analysis

Baikal

IceCube muons, 1 year

Icecube, muons & cascades4 years

GRB (WB)

A Coincidences with GRB

73 bursts

Check for coincidences with- BATSE - IPN - SWIFT

408 bursts

With IceCube:test WB withina few months

A Detection of Supernova Bursts

ice uniformly illuminated detect correlated rate increase on top of PMT noise

SN neutrino signal simulation

center of galaxy, normalized to SN1987A

Dark noise inAMANDA only

~ 500 Hz !

A Participation in SNEWS

coincidenceserver @ BNL

Super-K

alertSNO

LVD

AMANDA(IceCube)

http://snews.bnl.gov and astro-ph/0406214

IceCube will follow this year

…several hours advanced notice toastronomers

A Supernova in IceCube

5 signal for SN of 1987A strength

Dark noise inIceCube

Optical Modulesis only ~ 250

Hz !

A Summary tremendous technological progress

over last decade (Baikal, South Pole, now also Mediterrannean)

no positive detection yet, but already testing realistic models/bounds

IceCube reaches 1 km3 year by the end of 2008

entering region with realistic discovery potential

IceCube discoveries/non-discoveries will influence design of KM3NeT

A Events from IC9

Left: upward muon

Right: IceTop/IceCube event

A Back-ups

A WIMPs: neutrinos from center of Earth

Assumptions:

Dark matter in Galaxy due to neutralinos

Density

~ 0.3 GeV/cm3

+ b + b

C + +

A WIMPs: neutrinos from center of Earth

A WIMPs: neutrinos from Sun

Amanda

A WIMPs: neutrinos from Sun

A Relativistic Magnetic Monopoles

Cherenkov-Light n2·(g/e)2

n = 1.33

(g/e) = 137/ 2

8300

10-16

10-15

10-14

10-18

10-17

= v/c1.000.750.50

up

per

lim

it (

cm-2 s

-1 s

r-1)

KGF

Soudan

MACRO

Orito

Baikal

Amanda

IceCube

electrons

A Icecube Performance: muons

Effective Area for Muons

Galactic center

*Studies based on simpler reconstructionswaveform information will improve

Muon neutrino

Angular resolution

A Sensitivities

AMANDA (neutrinos)

IceCube (neutrinos)

Sensitivity (2π sr, 100% ontime):

0.01 0.1 1 10 100 1000 TeV

3 years exposure, 5 sigma 90% U.L.

AMANDA, ANTARES: ~ 10-10 / (cm² s) above 1 TeV IceCube: ~ 10-12 / (cm² s) above 1 TeV

A The big picture

1980 1985 1990 1995 2000 2005 2010 2015

10-4

10-10

10-8

10-6

10-1000 TeV

1 EeV

Dumand

Frejus Macro

Baikal/Amanda

IceCube/ KM3NeT

Rice AGASA

Rice GLUE

Anita, Auger

Flu

x *

E²

(G

eV

/ cm

² se

c sr

)

Sensitivity to HE diffuse neutrino fluxes

Waxman-Bahcall limit

A Methods for > 100 PeV

Radio detection of showers at the moon GLUE, Kalyazhin in future: LOFAR, SKA

Radio detection of neutrinos in ice or salt RICE, ANITA, Test array AURA (IceCube) future: ARIANNA, SALSA

Acoustic detection of neutrinos in water and ice test arrays SPATS (IceCube) and AMADEUS (ANTARES)

Detection of fluorescence signals in air from ground: AGASA, Auger from space: FORTE, in future – EUSO, OWL

A Detectors underground

KGF BAKSAN * FREJUS IMB KAMIOKANDE

MACRO Super-

KAMIOKANDE *

e.g. MACRO, 1356 upgoing muons

~1000 m²

*) still data taking

A All flavor limitsNormalized toone flavor and

assuming

e= 1:1:1

full IceCube, 4 years, combiningmuon and cascade data

A Coincidences with GRB

73 bursts

408 bursts