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
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