![Page 1: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/1.jpg)
C. Spiering, Leeds, July 23, 2004
![Page 2: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/2.jpg)
![Page 3: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/3.jpg)
![Page 4: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/4.jpg)
![Page 5: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/5.jpg)
Entrance to the Promised Land after 40 Years !
![Page 6: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/6.jpg)
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
![Page 7: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/7.jpg)
![Page 8: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/8.jpg)
Pioneering
DUMANDFred Reines
John Learned
~ 1975: first meetings towards an underwater array close to Hawaii
+ Roberts, Stenger, Gorham, ..
![Page 9: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/9.jpg)
DUMAND-II Proposal 1988 : - 216 PMTs at 9 strings - height 230 m
Alas !... terminated in 1996
![Page 10: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/10.jpg)
1987: DUMAND test stringLater used by Amanda and Baikal
![Page 11: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/11.jpg)
Search for diffuse excess of extra-terrestrial high energy neutrinos
bound
WB bound
log E /GeV
DUMAND
FREJUSMACRO
![Page 12: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/12.jpg)
Neutrino Telescopes
UndergroundKGF
Baksan
FREJUS
IMB
Kamiokande Superkamiokande
MACRO ~ 1000 m²
e.g. MACRO, 1356 upgoing muons
![Page 13: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/13.jpg)
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
![Page 14: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/14.jpg)
CampIce as a natural deployment platform
![Page 15: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/15.jpg)
NT-200
3600 m
1366
m
4-string stage (1996)
![Page 16: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/16.jpg)
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
![Page 17: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/17.jpg)
cascades
140 m
36 additional PMTs 4 times better sensitivity !
Baikal Upgrade NT200+
![Page 18: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/18.jpg)
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
![Page 19: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/19.jpg)
4100m
2400m
3400mANTARESNEMO NESTOR
![Page 20: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/20.jpg)
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
![Page 21: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/21.jpg)
AMANDA-II
depth AMANDA
Super-K
DUMANDAmanda-II:677 PMTsat 19 strings
(1996-2000)
![Page 22: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/22.jpg)
Ocean Water
![Page 23: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/23.jpg)
DrillingHot water drillingHot water drilling
![Page 24: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/24.jpg)
![Page 25: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/25.jpg)
AMANDA Event
Signatures:Muons
AMANDA Event
Signatures:Muons
+ N + X
CC muon neutrinointeraction track
![Page 26: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/26.jpg)
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
![Page 27: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/27.jpg)
![Page 28: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/28.jpg)
PRELIMINARY
First spectrum > 3 TeV:
- up to 100 TeV
- matches lower-energy Frejus data
![Page 29: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/29.jpg)
![Page 30: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/30.jpg)
Skyplot Amanda-II, 2000
697 eventsbelow horizon
above horizon:mostly fake events
![Page 31: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/31.jpg)
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
![Page 32: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/32.jpg)
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
![Page 33: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/33.jpg)
AMANDA skyplot 2000-2003 optimized for best sensitivity to E-3 – E-2 sources
3369 eventsPreliminary
![Page 34: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/34.jpg)
Preliminary
![Page 35: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/35.jpg)
![Page 36: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/36.jpg)
Crab
Mk421
SS433
Mk501
M87
Cyg
Cas A
Preliminary
![Page 37: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/37.jpg)
Selected Source Analysis
Stacking Source Analysis
Galactic Plane
Transient Sources
Burst Search
Correlation Analysis
Multi-Pole Analysis
Lower energy threshold (optimize to steeper spectra)
![Page 38: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/38.jpg)
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
![Page 39: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/39.jpg)
![Page 40: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/40.jpg)
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
![Page 41: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/41.jpg)
bound
WB bound
bound
WB bound
e:: = 1:2:0 1:1:1e:: = 1:2:0 1:1:1
![Page 42: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/42.jpg)
bound
WB bound
bound
WB bound
![Page 43: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/43.jpg)
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
![Page 44: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/44.jpg)
![Page 45: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/45.jpg)
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
![Page 46: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/46.jpg)
![Page 47: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/47.jpg)
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
![Page 48: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/48.jpg)
Present upper limits and expected IceCube sensitivity on muon flux from
neutralino annihilations in center of Sun
Disfavored
by direct search
![Page 49: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/49.jpg)
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
![Page 50: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/50.jpg)
![Page 51: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/51.jpg)
Supernova-MonitorAmanda-II
Amanda-B10
IceCube0 5 10 sec
Count rates
B10: 60% of Galaxy
A-II:95% of Galaxy
IceCube:Up to LMC
![Page 52: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/52.jpg)
The km3 scale at South Pole
IceCube- 80 Strings- 4800 PMTs - Instrumented
Volume: 1 km3
- Installation: 2005-2010
![Page 53: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/53.jpg)
6 Amanda modules
Super- Kamiokande (Japan)
AMANDA-II
IceCube
![Page 54: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/54.jpg)
IceCube Eff Area
cos
Ae
ff /
km2
IceCube Effective Area
![Page 55: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/55.jpg)
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
![Page 56: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/56.jpg)
Cosmic rays
Amanda/Spase
IceCube/IceTop
... investigatestransition toextra-galactic CR
![Page 57: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/57.jpg)
-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
![Page 58: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/58.jpg)
RICE AGASA
Amanda, Baikal2002
2007
AUGER
Anita
AABN
2012
km3
EUSOAugerSalsa
2004
RICE AGASA
Achieved and expected sensitivities to diffuse fluxes
![Page 59: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/59.jpg)
„Nothing is guaranteed, but history is on our side.“
Francis Halzen
![Page 60: The Long March Towards High Energy Neutrino Astronomy](https://reader035.vdocuments.mx/reader035/viewer/2022062810/56815a6f550346895dc7cf74/html5/thumbnails/60.jpg)
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 !