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, ..
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
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
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
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 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
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
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
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
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
-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