1. IceCube
C. Spiering
Saclay, Dec 2007

2. Congratulations to our
ANTARES friends:
10 strings connected !

3. Content
Sources and signal expectations
Neutrino telescopes under water and ice
Physics results from AMANDA and Baikal
IceCube: status, first results, prospects
Summary

4. The unified spectrum of neutrinos
under-
ground
optical:
- deep water
- deep ice
air showers
radio
acoustics

5. Prominent Source Candidates
Extra-Galactic
Galactic
AGN
Galaxy Clusters
GRB …
SNR
Microquasars
Young SN shells …

6. Prominent Source Candidates
Extra-Galactic
Galactic eV
AGN
Galaxy Clusters
GRB … eV
SNR
Microquasars
Young SN shells …

7. e :  :  ~1:2:0 turns to 1:1:1 at Earth
Neutrino Production or
e :  :  ~1:2:0 turns to 1:1:1 at Earth

8. Diffuse Fluxes (1998)
 bound
WB bound
MPR bound
p + CMB  p +

9. Signal predictions: extragalactic sources
WB bound corresponds to neutrinos per km²year
AGN predictions are highly uncertain (several orders of magnitude !)
Some of the older AGN models dramatically violate even soft upper bounds on diffuse fluxes, as derived from CR
Fluxes from individual AGN: less constrained
GRB: various models, benchmark model of Waxman-Bahcall can be easily tested with km3 detectors

10. Signal predictions: galactic sources
Predictions on firmer ground than for AGN
Shell-type SNR
Pulsar Wind Nebula
Compact Binary Systems
Many papers in the last 2 years:
Bednarek and Montaruli 2005
Vissani 2006
DiStefano 2006
Lipari 2006
Kappes, Hinton, Stegmann, Aharonian 2007
Gabici, Aharonian 2007 …
Unanimous conclusion: Cubic kilometer detectors will just scrape the detection region

11. Expected n flux from galactic point sources, example: RXJ 1713-3946
Assume p0  g and calculate related p±  n
C. Stegmann
ICRC 2007

13. PKS2105-304 (R. White, ICRC) PKS2105-304 as measured by H.E.S.S.
Correcting for  absorption
kinematics for / in source
KM3NeT with angular resolution 0.5°
S/Bg (> 1TeV) = 27/61
S/Bg(> 5TeV)
=21/10 (5)
R.J.White, ICRC

14. Conclusions for galactic sources
Desirable area km²
Threshold: for most cases 1 TeV OK
But: don‘t forget SN shells in first months after explosion
Always to the rescue: hidden sources
(but they also eventually should be visible at low photon energies !)

15. Underwater/Ice: optical telescopes
muon tracks cascades
angle water < 0.3° water 3-6° (at 10 TeV)
ice ° ice ~25° (at 10 TeV)
energy in log E % in E (at 10 TeV)

16. The Projects
Baikal
Antares
Nestor, Nemo
KM3NeT
Amanda
IceCube

17. BUT: North and South South Pole Mediterranean „blind“ „blind“
Galactic Center
„blind“
Mediterranean
„blind“
BUT:

18. North and South
At high energies: much less  BG from above  look above horizon !
At low energies: contained events in large detectors  look above horizon ! (more below)
IceCube, after 106 BG reduction
up galactic down
center

19. Baikal and AMANDA

20. AMANDA-II
ANTARES
NT200
NT200+

21. Basic parameters of present and planned neutrino telescopes
Effective  area:
~ 0.1 m² @ 10 TeV Amanda/Antares
~ 4 m² @ 100 TeV Amanda/Antares
~ 20 m² @ 100 TeV IceCube now
~100 m² @ 100 TeV IceCube complete
Point source sensitivity:
AMANDA, ANTARES: ~ 310-10  / (cm² s) above 1 TeV
IceCube, KM3NeT ~  / (cm² s) above 1 TeV
(for 5 discovery)

22. AMANDA Results

23. Atmospheric neutrinos
K. Münich
RICAP 2007
spectrum
measured
up to 100 TeV

24. Search for steady point source-3 -2 -1 1 2 3
AMANDA-II: (1001 live days) n from Northern hemisphere
No significant excess found

25. Results for 2005

26. 2005 data unbinned search
90% confidence level sensitivity to E-2 spectra

27. 2005 Results
69 out of 100 sky maps randomized in RA contain an excess of at least 3.6s
Largest Excess: 3.6s
d=48o , a=2.75h
Log10(p-value)
Need to mention how significances are evaluated again

28. ES
WHIPPLE
Flux of
TeV photons
(arb. units)
Arrival time of neutrinos from the direction of the AGN ES 3   2 1
May
June
July
2000
2001
2002
2003
Year

29. Diffuse fluxes Atmospheric neutrinos behave like E-3.7
Typical extraterrestrial fluxes behave like E-2

30. Limit on diffuse extraterrestrial fluxes
Atmospheric neutrinos behave like E-3.7
Typical extraterrestrial fluxes behave like E-2
From this method and one year data we exclude E-2 fluxes with E2 > 2.7 GeV sr-1 s-1 cm-2

31. Limit on diffuse extraterrestrial fluxes
From this method and one year data we exclude E-2 fluxes with E2 > 2.7 GeV sr-1 s-1 cm-2
With 4 years and improved methods we are now at
E2 > 8.8 GeV sr-1 s-1 cm-2

32. Experimental limits & theoretical bounds
MPR bound, no neutron escape (gamma bound)
Factor 11 below MPR bound for sources opaque to neutrons

33. Experimental limits & theoretical bounds
MPR bound, neutrons escape (CR bound)
Factor 4 below MPR bound for sources transparent to neutrons

34. Experimental limits & theoretical bounds
AGN core (SS)
AGN Jet (MPR)
GZK
GRB (WB)

35. Experimental limits & theoretical bounds
old version
AGN core (SS)
„old“
Stecker model
excluded

36. Experimental limits & theoretical bounds
AGN core
(SS, new version)
„new“
Stecker model
not excluded
(MRF = 1.9)

37. Experimental limits & theoretical bounds
AGN Jet (MPR)
still above
AGN jet (MPR)
(MRF ~ 2.3)
GRB (WB)

39. Prompt Neutrinos from Charm Decay
Muon neutrinos
Electron neutrinos

40. Limit on diffuse extraterrestrial fluxes
AMANDA HE analysis
Baikal
IceCube muons,
1 year
Icecube,
muons & cascades
4 years
2003
2006
2009
2013
GRB (WB)

41. Gamma Ray Bursts
Vela Satellite 1969
Jet with G ~

42. Coincidences with GRB close to WB within < factor 2 with IceCube:
Check for coincidences with BATSE, IPN, SWIFT
10-7
AMANDA limit from 408 bursts
close to WB
within < factor 2
with IceCube:
test WB within
a few months
10-8
Waxman-Bahcall
GRB prediction
E2flux (GeVcm-2s-1sr-1)
10-9
10-10
104
105
106
107
108
neutrino energy E (GeV)

43. Relativistic Magnetic Monopoles b
105
103
101
107
photons/cm
monopole d
bare
muon
Cherenkov Light 
n2·(g/e)2
n = 1.33
(g/e) = 137/2
 8300

44. Relativistic Magnetic Monopoles
Baikal years
AMANDA-II 1 year

45. Relativistic Magnetic Monopoles
IceCube-9 preliminary

46. Neutralino Capture in the Sun
Detector
Earth

47. Neutralino Capture in the Earth 
Look for neutrinos
from the center of
the Earth.
 +   b + b
C +  + 

48. Sun Earth

49. IceCube

50. IceCube IceTop InIce Completion by 2011. AMANDA now operating as part:
13 strings deployed
: 8 strings
: 1 string
IceTop
Current configuration
- 22 strings
- 52 surface tanks
Air shower detector
80 pairs of ice Cherenkov tanks
Threshold ~ 300 TeV
1450m
InIce
AMANDA-II
19 strings
677 modules
Goal of 80 strings of 60
optical modules each
17 m between modules
125 m string separation
AMANDA now
operating as part
of IceCube
AMANDA now
operating as part
of IceCube
2450m
Completion by 2011.
2007/08: add 14 to 18 strings and tank stations

51. IceCube IceTop IceTop InIce Current configuration - 22 strings
- 52 surface tanks
Air shower detector
80 pairs of ice Cherenkov tanks
Threshold ~ 300 TeV
IceTop
Angular calibration
of IceCube
chemical composition
(with IceCube)
veto for IceCube
1450m
InIce
Goal of 80 strings of 60
optical modules each
17 m between modules
125 m string separation
2450m

52. IceCube IceTop InIce AMANDA now operating as part AMANDA now:
13 strings deployed
IceTop
Current configuration
- 22 strings
- 52 surface tanks
Air shower detector
80 pairs of ice Cherenkov tanks
Threshold ~ 300 TeV
: 8 strings
1450m
InIce
AMANDA-II
19 strings
677 modules
Goal of 80 strings of 60
optical modules each
17 m between modules
125 m string separation
AMANDA now
operating as part
of IceCube
AMANDA now
operating as part
of IceCube
2450m

53. Measured Effective Scattering Coefficient
IceCube Coll, J. Geophys. Res. 111 (2006) D13203

54. IceCube deployment 2005-2011 2004 / 05 2005 / 06 2006 / 07 2007 / 08
AMANDA 78
Planned for 07 / 08 77
IceCube string and IceTop station deployed 01/05 75 76 70 69 68 63 62 61 60 53 54 52 74 73 71 72
2004 / 05
IceCube string and IceTop station deployed 12/05 – 01/06 67 66 65 64
2005 / 06 58 59 57 55 56
IceTop station only 2006 50
2006 / 07 49 48 47
IceCube string and IceTop station deployed 12/06 – 01/07 44 45 46 39 40 38
2007 / 08
IceTop station only in 06 / 07 30 29 21
1424 DOMs deployed to date
Next year looking for ≥ 14 strings and 14 IceTop stations.
Want to achieve steady state of ≥ 14 strings / season.

55. IceCube

56. Drilling: First 30 m
Firn Drill

57. Hot Water Drilling
- 5 MW power
- 16 m³ fuel
per hole

58. Hot Water Drilling

59. Drilling: time reproducable
36 h

60. Deployment

61. Deployment
10 h

62. IceTop

63. IceTop
Tom Gaisser

64. IceCube Laboratory and Data Center
Commissioned for operation
in January 2007

66. IceCube Laboratory and Data Center

67. IceCube Laboratory and Data Center

68. Growth of IceCube Full IceCube | +IC36-40 +IC22 +IC9 KM3NeT
AMANDA ANTARES

69. Growth of IceCube

70. First DOMs stops communication Second DOM stops communication
Assumed constant
Failure rate (exponential)
76 DOMs
589 DOMs
1390 DOMs
First DOMs stops communication
Second DOM stops communication

71. AMANDA as low energy subdetector of IceCube
threshold GeV
IceCube with
Amanda GeV
Amanda without
IceCube GeV

72. Effect on 22-string detector
Preliminary
8200
incl.
AMANDA
Atmos. 
per 200 days
(trigger level,
IC22+AMANDA)
30 GeV!
5400
IceCube
only
Gross, Tluczykont, Ha, Rott, DeYoung,
Resconi, & Wikström, ICRC 2007

73. DeepCore AMANDA DeepCore? 6 strings each with 40 PM, spaced by 10 m
better veto from top
Can look South
located in best ice
uses IceCube technology
considerably better performance at low energy
AMANDA
DeepCore?

74. North and South
At high energies: much less  BG from above  look above horizon !
At low energies: contained events in large detectors  look above horizon !
IceCube, after 106 BG reduction
up galactic down
center

75. Another Option: „Outer Ring“
Reconfiguration of last 8-10 strings at km radius
1.5-2 more sensitivity at 1 PeV
Logistic challenge (drilling) 21 30 29 40 50 39 38 49 59 46 47 48 58 57 66 67 74 65 73 78 56 72 77 71 64 55 75 76 70 69 68 63 62 61 60 53 54 52 45 44
Marked positions:
deployed, or fixed by drill plans 07/08

76. Options for EeV energies
Need huge array due to feeble fluxes
Economical affordable only for large sensor spacing
Need signal with km attenuation length (light ~ 100 m)
In water: acoustic signals
In ice: acoustic and radio signals

77. Installed in last season and under evaluation:
3 test strings
acoustics
SPATS
test:
- noise
- attenuation
length
- refraction
3 test strings radio AURA
(Askaryan Underice Radio Array)
South Pole Acoustic Test Setup

78. Acoustic attenuation length: still open
Answer will hopefully come from
4th acoustic test string (this season)

79. First IceCube-9 Results
- atmospheric neutrinos
- point source search
- UHE events
- IceTop
- Presently everybody is preparing IC22 analysis

80. Neutrinos in IC9 9-string data (2006)
Cosmic ray background seen with weak cuts
Atmospheric neutrinos seen with strong cuts
Agreement in event rate over 6 decades
downward muons
Final Cuts
atmos.neutrinos
Achterberg et al. astro-ph/

81. Point Source: Discovery Potential
Simulate a neutrino source at a given declination
90% of sources with the given E-2 flux are detected
at the stated significance

82. Significance Map IC9, 250 events

83. IceTop – spectrum with 2006 data

84. Supernova in IceCube Detection by enhanced noise rates Dark noise in
5 signal for SN of 1987A strength
Dark noise in
IceCube
Optical Modules
is only ~ 320 Hz !

85. Significance of observation vs distance:
signal expected at LMC:
52 kpc
Integrated over 10s
IceCube
AMANDA
Visibility up to Large Magellanic Cloud (~ 5  signal)

86. Conclusions
„AMANDA only“ analysis is basically finished, with record upper limits
New order of sensitivity with IC22 (expect results in Summer 2008)
By today, 3 of strings of this season deployed: may reach ½ IceCube
1 km³year in 2009
Enter a region with fair discovery potential
Most exciting 5 years just ahead of us !

87. END

88. Indirect Dark Matter Search

89. Capture by Sun and Earth
Capture in Sun
Mostly on Hydrogen
Both spin-independent and spin- dependent scattering
Capture in Earth
Mostly on Iron
Essentially only spin- independent scattering
Resonant scattering when mass matches element in Earth
Figure from Jungman, Kamionkowski and Griest

90. Amanda Analysis: Earth WIMPs 1999 as example
Background rejection
optimization = f (mass, decay mode)
Angular distribution
Start with
events at trigger
level in 99 data
LIMIT
Aeff

91. Muon flux limits compared to MSSM predictions
Situation 2004
but … 

92. Halo WIMPs diffuse in the solar system by action of the other planets.
Lundberg & Edsjö, 2004:
When the halo WIMPs have reached the Earth, they have gained speed by the Sun’s attraction. Hence, capture is very inefficient.
Halo WIMPs diffuse in the solar system by action of the other planets.
2005
But:

93. Neutrino-induced muon fluxes from the Earth center
Usual Gaussian approximation
New estimate including solar capture
Maxwell-Boltzmann velocity distribution assumed.

94. Neutrino-induced muon fluxes from the Sun
Compared to the Earth, much better complementarity due to spin-dependent capture in the Sun.

95. Comparing direct vs. indirect searches: a word of caution
~ density
actual density
High-velocity region
~ density squared
Density integrated over cosmological times
Low-velocity region
Branching ratios !

96. Neutrino-induced fluxes and future direct detection limits
Sun
Earth
Future direct detection sensitivity is assumed to be 10-9 pb.