1. Neutrino Astroparticle Physics
XXV Physics in Collision
Lutz Köpke
University of Mainz, Germany
July 8, 2005

2. Physics in collisions? actually not ... fixed target physics: 1012
1015
1018
1021 eV
50 GeV TeV 40 TeV TeV
center of mass energy
neutrino energy
atmospheric
neutrinos
GZK: p+CMB n+X+ 
probe physics beyond LHC
...limits exist all the way up to 1025 eV

3. Physics motivation ... astrophysics and particle physics
 origin and acceleration of cosmic rays
 understand cosmic cataclysms
 find new kind of objects?
 neutrino properties ( , cross sections ..)
 dark matter (neutralino annihilation)
tests of relativitiy ....
search for big bang relics ...
effects of extra dimension etc. ...
pp  ± + X  e,....
p  + + X  e , ....
Beam dump:

4. Particle propagation in the Universe
Protons/nuclei: deviated by magnetic fields, reactions with radiation (CMB)
protons E>1019 eV (30 MLy)
protons E<1019 eV
neutrinos
gammas ( MLy)
Cosmic
accelerator
Katz
Photons: absorbed on dust and radiation

5. Neutrino source candidates
Microquasar
(SS433 etc.)
Active Galaxy
(optically dense, e.g. FRII)
Black hole with
108 x mass of sun
 106 Ly
extra-galactic
Supernova remnant
 1 Ly
Crab nebula
Black hole with
 mass of sun
galactic

6. Required sensitivity ... for discovering extraterrestrial neutrinos -5
many specific models for
non-resolved sources ... -5
atmospheric -6
WB bound
MPR bound
 Mannheim, Protheroe
and Rachen (2000)
 Waxman, Bahcall (1999)
derive generic limits from
 limits on extragalactic p‘s
-ray flux
log [E2 · flux(E) / GeV cm-2 s-1 sr-1] -7
GZK
AGN core (SS) -8
AGN Jet (MPR)
GRB (WB) -9
log (E /GeV) 2 3 4 5 6 7 8 9 10
TeV PeV EeV

7. Can it be done ? Reaction probability [H2O, d=1km]:
Haim-Harrari: neutrino physics is the art to learn a lot from nothing ....
Reaction probability [H2O, d=1km]:
W=NAd  4 •10-7 • E[TeV]
... sources millions to billions light years away ...
 Needs huge detectors making use of natural media
 Require high energies
 Need to detect all flavors
Extended source with e:: =1:2:0 production (e.g.  decay) :
for 23  45°, 130°:
e:: =1:1:1 on earth

8. Principle detection methods
high energies (E> 1011 eV)
radio, acoustics, particles ...
moon, ice, salt
mountain ...
detectors (earth based, balloon/satellite)
extremely high energies (E>1018 eV)
grid of light sensors for Cherenkov radiation

9. Single photon detection
... information: timing and amplitude of photons - position of PMTs
IceCube
…typically 300 MHz digitization

10. Detection of  , e , 
 O(10) x less background for e – but you don’t profit from long -range
 Regeneration of  - no absorption in earth even at very high energies !
O(km) long muon tracks
direction determination
by Cherenkov light timing
 15 m
Electromagnetic and hadronic cascades
~ 5 m

11. The neutrino telescope world map
Baikal
Antares
Nemo
Nestor
KM3Net?
Amanda/IceCube

12. Importance of complete sky coverage
Need earth as shielding agains cosmic rays for  (if E < 100 TeV)
South Pole (ice)
AMANDA, ICECUBE
Mediterranean (ocean)
Antares, Nestor, 1 km3 ...
galactic center in middle
4  coverage for e ,  !

13. Importance of large energy coverage
Neutrino flavor
Log(ENERGY/eV) 12 18 15 6 21 9 ne nm nt
supernovae
Full flavor ID
Showers vs tracks
IceCube flavor ID,
direction, energy
IceCube triggered,
partial reconstruction
TeV PeV

14. Importance of low background
Nestor
cosmic ray muons
 : x dominated
by cosmic ray muons
 need low misreconstruction
 e: background much lower
(but smaller detection volume)
 scattering helps ...
IceCube
 Detector noise:
low in inert ice (1 kHz/PMT)

15. Importance of good angular resolution
Expected  resolution for
1 km3 detectors
...can‘t compete with -telescopes
..but for many analyses not crucial
Ice
size of moon
water
atmospheric 

16. Price and ease of construction
moon
... use existing moon
…and radio antennas
Ice
water
KM3Net:
< 200 MEUR
IceCube:
M$273 (US accounting)
50 M$ detector cost

17. Northern hemisphere detectors
NESTOR
Astrop. Phys. 23, 377 (2005)
Baikal NT200
Antares
Nestor
1100 m deep
data taking since 1998
new: 3 distant strings
under construction
2400 m deep
completion: early 2007
1 of 12 floors deployed
4000 m deep
completion: 2007?

18. BAIKAL NT200+
Excellent example that smart ideas can compensate small size and budget
… concentrate on  induced showers
data taking since 1998
3 external strings in operation since April sensitivity quadrupled

19. Antares string based detector, 0.01 km3 instrumented volume
 prototype strings 2003, March 2005
 1st „final“ string mid 2005
 detector completion early 2007
submarine cable
40 km
~ 40 km m

20. Antares test string 2005
string based detector, 0.01 km3 instrumented volume
... detectors moving with currents….
 acoustic positioning < 10 cm
(2mm for fixed distance)
 1st „final“ string mid 2005
 detector completion early 2007

21. AMANDA and IceCube 0.02 km3 AMANDA 1 km3 IceCube Optical module (677)
..collaborations merged March
0.02 km3 AMANDA
1 km3 IceCube
Optical
module (677)
IceTop
0 m
1400 m
2400 m
> 70 strings
> 4200 modules
 1500 atmospheric ‘s /year
 atmospheric ‘s /year

22. the South-Pole laboratory
South Pole Station
First IceCube string
1400m
2400m
IceCube Counting House
1500 m
AMANDA
2000 m
[not to scale]

23. The new station operating at least until 2035

24. First IceCube string ... January 2005: 60 optical modules
Deepest module at 2450 m

25. IceCube coincident events ..
IceTop – IceCube
Amanda – IceCube

26. The testbeams atmospheric neutrinos cosmic ray muons Eμ  E-3.8
Energy spectrum with unfolding technique
atmospheric neutrinos
1 GeV TeV
Amanda
Frejus
Eν  E-3.8
cosmic ray muons
Eμ  E-3.8
Eprimär  E-2.7
EHadrfon  E-2.7 0.02
1 TeV TeV
... Primary energy corrected
Preliminary

27. Atmospheric neutrinos
... IceCube will be abundant source of atmospheric neutrinos:
AMANDA (5y)  , between TeV
IceCube (5y)  , between TeV
e.g. study of equivalence principle,
velocity induced oscillations:
2 orders of magnitude improvement
in sensitivity

28. Neutrinos from unresolved sources
Expect deviation at high energy (hard flux)
cascades (2000 data)
 (2000 data)
Preliminary

29. Very high energies
Special analysis for very high energies above 1000 TeV ....
 large energy deposits (bremsstrahlung)
 Earth starts absorbing 
70 TeV: interaction length = earth diameter
AMANDA reach (5y): cm-2 s-1 sr-1
90% energy range: GeV

30. Experimental bounds and future
..closing in on
Waxman-Bahcall
bound
 gain factor 30
in sensitivity with
1 km3 detectors
present AMANDA sensitivity
--- Preliminary
DUMAND test string
FREJUS
MACRO
atmospheric -5
AMANDA limits -6
BAIKAL
log [E2 · flux(E) / GeV cm-2 s-1 sr-1] -7
GZK -8
IceCube (3y) -9 2 3 4 5 6 7 8 9 10
log (E /GeV)

31. Search for localized sources (AMANDA)
Maximum significance 3.4 
compatible w. atmospheric 
Preliminary
quite expected ...
92% of experiments would yield even higher maximum
(807 days)
3329  from northern hemisphere
3438  expected from atmospheric 
 also search for neutrinos from unresolved sources

32. ... measured limits and future
10-12
Macro
Super-K
10-13
IMB
Baksan
Amanda
10-14
neutrino induced muon flux /(cm2 s)
10-15
2007
Antares+Nestor
AII+IceCube
10-16
2012
KM3Net IceCube
10-17
10-18
declination (degrees)

33. ... steady progress in sensitivity
average flux upper limit [cm-2s-1]
sin(d)
AMANDA-B10
AMANDA-II
IceCube 1/2 year *
optimized for E-2, (*) E-2, 3 signal *
>10 GeV
1997 : ApJ 583, 1040  (2003)
2000 : PRL 92, (2004)
: PRD (2005)
IceCube: Astrop Phys 20, 507 (2004)
lim  0.68·10-8 cm-2s-1
time
Preliminary

34. ... closing in on predictions
 predictions very model dependent
 ... some can be tested now .. e.g. SS-433 micro quasar:
10-5
SS-433
10-6
integrated neutrino flux /(cm2 s) [E>1 GeV]
10-7
Distefano 2002
10-8
preliminary

35. Additional studies  Search for excess in galactic plane
 Search for neutrino clusters (sliding time window)
 coincidence with enhanced EM emision x-ray, radio and -ray)
 curosity: 1 neutrino candidate close to orphan peak (no radio signal)
...no statistically significant effects
need multiwavelength campaigns!
May '02
July '02
June '02
sliding search window
Error bars: off-source background per 40 days

36. GRB n search in AMANDA Cascade channel: worse pointing but 4!
Search for  candiates correlated with GRBs - background established from data
: <20°
PRELIMINARY
Cascade channel:
worse pointing but 4!
 effective area  m2 ()
 limit assumíng WB spectrum: Eν2Φν < 3 x 10-8 GeV cm-2 s-1 sr-1 ()
< 9.5x10-8 GeV cm-2 s-1 sr-1 (cascades)
 No coincident events observed observed!

37. Green’s Function Fluence Limit (allows for comparison with SK)
Further investigations ...
 Search without temporal/spacial constr.: Eν2Φν < 6.7x 10-6 GeV cm-2 s-1 sr-1
 detailed investigations of GRB large model dependencies !!
SuperKamiokande (1454)
AMANDA sensitivity
AMANDA limit
Green’s Function Fluence Limit (allows for comparison with SK)
Future goal:
determination of limits
independent of specific model
PRELIMINARY

38. Indirect search for dark matter
 neutralino is best particle physics candidate for dark matter
 stable if R-parity conserved (for most parameters)
 can self-annihilate (Majorana particle) and produce neutrinos
 gravitationally trapped in center of earth, sun or center of galaxy 
e.g.:  +   b + b
c + - + 
; W+W- 
Nuclear Recoil and indirect searches are
complementary and not equivalent !!

39. WIMP search in AMANDA Limits on muon flux from Earth center
AMANDA results submitted for publication
Limits on muon flux from Earth center
Limits on muon flux from Sun
AMANDA 1y
Antares 3 years
1km3 (IceCube) SK
Disfavored by direct search (CDMS II)
New solar system WIMP diffusion model -> more realistic neutralino velocity distribution (Lundberg&Edsjoe)
Detection threshold (mu): ~50GeV (extrapolate to get limits for E>1 GeV)
Cuts optimized for each mass independently

40. New particles 10-14 Soudan high sensitivity to rare new particles
if signature unambigous ....
... (slowly) moving bright particles ...
KGF
MACRO
Amanda
10-15
Orito
upper limit (cm-2 s-1 sr-1)
10-16
Baikal
e.g magnetic monopoles:
Cherenkov-light  (n·g/e)2
(1.33*137/2)2
 electrons
10-17
1 km3
10-18
8300 times stronger than for !
0.50
0.75
1.00
 = v/c

41. The (near) future
 complete construction of 1 km3 IceCube detector
can already work with incomplete detector …
 complete construction of smaller mediterranean detectors ?
 decide on location/design of 1km3 mediterranean detector ?
 Complete construction of KM3Net? ?
 new ideas for detection of extremely high energy neutrinos ....
 extend the search to higher energies with even bigger detectors

42. IceCube: 11/2004 - 9/2010 Up to 18 holes per season: Nov.: preparation
Dec.: construction
Jan.: construction
Feb.: commissioning
35% of money spent ...

43. Signatures in IceCube …
1013 eV (10 TeV)
6x1015 eV (6 PeV)
Multi-PeV 
+N+...
± (300 m track!)
 +hadrons
signature of 
signature of 

44. 1 km3 array in Mediterranean
 Extensive exploration and R&D (NEMO)
 efforts of all groups (Antares, Nestor, Nemo)
being joined to form single collaboration
EU-funded design study (10 M€ requested)
on list of proposed large EU-projects (ESFRI)
problems mainly „political“ (site e.g.)
new technological develoments
design report 2008
construction ?
multianode PMTs with Winston cones)
.... but time scale tight

45. Anita - quest for GZK neutrinos
 surveys > 1 million km2
 under construction
 launch Dec 2006
refracted radio
Antarctic ice
neutrino

46. ... very rare - very high energy events
many proposals for radio and acoustic detectors in ice, water, salt, from moon ..
Preliminary!
e.g. IceCube extension:
>>km attenuation length
sparse instrumentation
100-fold volume increase
>100
> 10 GZK neutrinos/year
IceCube

47. RICE AGASA Amanda, Baikal 2002 2004 Glue AUGER nt Anita 2008
0.1 km3
2008
km3
satellites
radio
later

48. Summary ..no extraterrestrial neutrinos found yet ...but:
 plenty of results (limits)
closing in on predictions …
 1 km3 IceCube  construction started
30 times efffective area
 mediterranean detectors under construction
taskforce for 1 km3 detector
 innovative concepts for even larger detectors

49. ... Limits on selected sources
0.21
4.50 2
SS433
1.25
5.36 10
Crab Nebula
0.40
5.21 4
Cygnus X-1
0.77
5.04 6
Cygnus X-3
0.38
3.71 5
1ES
0.68
5.58
Markarian 421
Flux Upper Limit
F90%(En>10 GeV)
[10-8cm-2s-1]
Expected
backgr.
(4 years)
Nr. of n events
Source
Sensitivity /~2
for 200 days of
“high-state” (HEGRA)
Crab Nebula:
MC probability for excess 64%
… out of 33 Sources
Systematic uncertainties under investigation
selected objects → no statistically significant effect observed

50. Effective Area and Angular Resolution for Muons
IceCube
Effective Area and Angular Resolution for Muons
Galactic
center
for a E-2 nm spectrum
with quality selection and BG suppression (atm m reduction by ~106)
Median angular
reconstruction uncertainty ~ 0.8
further improvement
expected using waveform info
Energy resolution: s[log10(Em)]  20%-30%

51. neutrino induced muon flux /(cm2 s)
10-12
10-14
10-15
10-16
10-17
10-18
10-13
neutrino induced muon flux /(cm2 s)
declination (degrees)
Macro
Amanda
Super-K
Baksan
IMB
2007
2012
KM3NeT IceCube
Antares+Nestor
AII+IceCube
GX339-4
SS-433
MK501 /~1

52. Sun Crab Nebula Cassiopeia. A LMC Cygnus-X1 SMC 90 000 light years
Approximate
AMANDA horizon
light years