The AMANDA and IceCube ??????????:??????

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The AMANDA and IceCube ????????????????

• Physics Motivation
• AMANDA detector
• Recent Experimental Results
• IceCube Project overview and Status
• EHE Physics Example Detection of GZK neutrinos

?? ? (?????)
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You cannot expect too many n!
p g (p,n) p
2g
m n
e n n
You cannot expect too high energies
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Theoretical bounds
Suppressed by Synchrotron Cooling
opaque for neutrons
MPR
neutrons can escape
atmospheric ??
WB
Mannheim, Protheroe and Rachen (2000) Waxman,
Bahcall (1999) ? derived from known limits on
extragalactic protons ?-ray flux
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EHE(Extremely HE) n
Synchrotron cooling of m Production sites
with low B
Intergalactic space!!

• GZK Production
• Z-burst
• Topological Defects/Super heavy Massive particles

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Shall we Dance?
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Where are we ?
South Pole
Dome
road to work
AMANDA
Summer camp
1500 m
Amundsen-Scott South Pole Station
2000 m
not to scale
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AMANDA-B10 (inner core of AMANDA-II) 10
strings 302 OMs Data years 1997-99
AMANDA-II 19 strings 677 OMs Trigger rate 80
Hz Data years gt2000


Optical Module
PMT looking downward
PMT noise 1 kHz
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Event detection in the ice
O(km) long m tracks
South Pole ice the most transparent natural
medium ?
event reconstruction by Cherenkov light timing
15 m
AMANDA-II m tracks pointing error 1.5º -
2.5º slog10(E/TeV) 0.3 - 0.4 coverage
2p Cascades (particle
showers) pointing error 30º -
40º slog10(E/TeV) 0.1 - 0.2 coverage
4p cosmic rays
(SPASE) combined pointing err lt
0.5º slog10(E/TeV) 0.06 - 0.1 Nucl.
Inst. Meth. A 524, 169 (2004)
cascades
a neutrino telescope Qmn?0.65o?(En/TeV)-0.48 (3Te
VltEnlt100TeV)
Longer absorption length ? larger effective volume
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Atmospheric n's in AMANDA-II
? neural network energy reconstruction ?
regularized unfolding
PRELIMINARY
measured atmospheric neutrino spectrum
1 sigma energy error
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Oscillation in AMANDAs range
SuperK values Dm² 2,4 10-3 eV² sin²(2QMix)
1,0
1 TeV
100 GeV
50 GeV
30 GeV
Problem lower energy threshold 100 GeV - 1 TeV
P( nm ? nm )
10 GeV
positive identification not possible
flight length / km
110
180
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Oscillation in AMANDAs range
Variation of Dm² (En 100GeV)
10-3 eV²

• significant
• oscillation
• in
• AMANDAs
• range
• exclusion
• regions in
• sin²(2Q)-Dm²
• -plane

2,4 10-3 eV²
10-2 eV²
P( nm ? nm )
2,8 10-2 eV²
flight length / km
110
180
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Excess of cosmic neutrinos? Not yet ...
talk HE 2.3-4
.. for now use number of hit channels as energy
variable ...
muon neutrinos (1997 B10-data) accepted by PRL
AGN with 10-5 E-2 GeV-1 cm-2 s-1 sr-1
cuts determined by MC blind analyses !
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The highest energy event (200 TeV)
300 m
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Theoretical bounds and future
opaque for neutrons
MPR
neutrons can escape
atmospheric ??
WB
Mannheim, Protheroe and Rachen (2000) Waxman,
Bahcall (1999) ? derived from known limits on
extragalactic protons ?-ray flux
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n telescope point source search
Preliminary

• Search for clustering in northern hemisphere
• compare significance of local fluctuation to
• atmospheric n expectations
• un-binned statistical analysis
• no significant excess

2000-2003 3369 n from northern hemisphere 3438 n
expected from atmosphere
? also search for neutrinos from unresolved
sources
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Extend this information to the AMANDA exposure
time, caveat g-rays observation are generally
very short and for limited periods Tibet data
quite cover the (HEGRA) High period
Second Assumption use X-ray data to define
relative High/Low time for the whole time
2000/2003
AMANDA observational time High state/total
time 210/807 or also 1 year/4 years of AMANDA
exposure
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Low state can be compared to our best upper
limit (sensitivity shown here)
about factor 2
Correction for extra-galactic g absorption TeV
g-ray spectra are modified by red-shift dependent
absorption by intergalactic IR-UV background
O.C.De Jager F.W.Stecker, Astrophy.J. 566
(2002), 738-743
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High state can be compared to the AMANDA
sensitivity for 200 days of live time (1 year
exposure) Sensitivity n/g1 BUT without
accounting for oscillations
(a factor 2 in the n flux should be added!!)
Current best estimate
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Search for ?? correlated with GRBs
-1 hour
1 hour
10 min
Blinded Window
Background determined on-source/off-time
Background determined on-source/off-time
Time of GRB (Start of T90 )
Low background analysis due to space and
time coincidence!
PRELIMINARY
Year Detector NBursts NBG, Pred NObs Event U.L.
1997 B-10 78 (BT) 0.06 0 2.41
1998 B-10 94 (BT) 0.20 0 2.24
1999 B-10 96 (BT) 0.20 0 2.24
2000 A-II (2 analyses) 44 (BT) 0.83/0.40 0/0 1.72/2.05
97-00 B-10/A-II 312 (BT) 1.29 0 1.45
2000 A-II 24 (BNT) 0.24 0 2.19
2000 A-II 46 (New) 0.60 0 1.88
2000 A-II 114 (All) 1.24 0 1.47

• GRB catalogs
• BATSE, IPN3 GUSBAD
• Analysis is blind
• finalized off-source ( 5 min) with MC
  simulated signal
• BG stability required within 1 hour
• Muon effective area (averaged over zenith angle)
  ? 50,000 m2 _at_ PeV

(BT BATSE Triggered BNT BATSE
Non-Triggered New IPN GUSBAD)
97-00 Flux Limit at Earth E2F? 410-8 GeV
cm-2 s-1 sr-1 For 312 bursts w/ WB Broken
Power-Law Spectrum (Ebreak 100 TeV, GBulk 300)
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WIMP annihilations in the center of Earth
Sensitivity to muon flux from neutralino
annihilations in the center of the Earth
PRELIMINARY
Muon flux limits
Look for vertically upgoing tracks
Eµ gt 1 GeV
NN optimized (on 20 data) to - remove
misreconstructed atm. µ - suppress atmospheric
? - maximize sensitivity to WIMP signal Combine
3 years 1997-99 Total livetime (80) 422 days
Disfavored by direct search (CDMS II)
No WIMP signal found
Limit for hardest channel
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WIMP annihilations in the Sun
Increased capture rate due to addition of
spin-dependent processes Sun is maximally 23
below horizon Search with AMANDA-II possible
thanks to improved reconstruction capabilities
for horizontal tracks Exclusion sensitivity
from analyzing off-source bins 2001
data 0.39 years livetime
PRELIMINARY
Muon flux limits
Eµ gt 1 GeV
No WIMP signal found
Best sensitivity (considering livetime) of
existing indirect searches using muons from the
Sun/Earth
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AMANDA as supernova monitor
MeV

• Bursts of low-energy (MeV) ?e from SN
• ? simultaneous increase of all
• PMT count rates (10s)
• Since 2003
• SNDAQ includes all AMANDA-II channels
• Recent online analysis software upgrades
• can detect 90 of SN within 9.4 kpc
• less than 15 fakes/year
• ? can contribute to
• SuperNova Early Warning System
• (with Super-K, SNO, Kamland, LVD, BooNE)

coverage
B10 70 of Galaxy A-II 95 of
Galaxy IceCube up to LMC
Analysis of 200X data in progress
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The IceCube Neutrino Telescope

• Project overview and Status
• EHE Physics Example Detection of GZK neutrinos

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Who are we ?
Bartol Research Inst, Univ of Delaware,
USA Pennsylvania State University, USA University
of Wisconsin-Madison, USA University of
Wisconsin-River Falls, USA LBNL, Berkeley, USA UC
Berkeley, USA UC Irvine, USA
Univ. of Alabama, USA Clark-Atlanta University,
USA Univ. of Maryland, USA IAS, Princeton,
USA University of Kansas, USA Southern Univ. and
AM College, Baton Rouge
Chiba University, Japan
University of Canterbury, Christchurch, New
Zealand
Universidad Simon Bolivar, Caracas,Venezuela
Université Libre de Bruxelles, Belgium Vrije
Universiteit Brussel, Belgium Université de
Mons-Hainaut, Belgium Universität Mainz,
Germany DESY-Zeuthen, Germany Universität
Wuppertal, Germany
Uppsala Universitet, Sweden Stockholm
universitet, Sweden Kalmar Universitet,
Sweden Imperial College, London, UK University of
Oxford, UK Utrecht University, Utrecht, NL
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First year deployment (Jan 2005) 4 IceCube
strings (240 OMs) 8 IceTop Tanks (16 OMs)
IceTop 160 tanks frozen-water tanks 2 OMs / tank
1200 m

IceTop
IceCube
AMANDA
IceCube 80 strings 60 OMs/string 17 m vertical
spacing 125 m between strings

IceTop Tank deployed in 2004
10 Hamamatsu R-7081
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Road to South Pole
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How EHE events look like
The typical light cylinder generated by a muon of
100 GeV is 20 m, 1PeV 400 m, 1EeV it is about
600 to 700 m.
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Digital Optical Module (DOM)
HV Base
Flasher Board
Main Board (DOM-MB)
10 PMT
13 Glass (hemi)sphere
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Capture Waveform information (MC)
nt
E10 PeV
String 5
String 4
String 3
String 1
String 2

• ATWD 300MHz 14 bits.
• 3 different gains (x15 x3 x0.5)
• Capture inter. 426nsec
• 10 bits FADC for long duration pulse.

Events / 10 nsec
0 - 4 µsec
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World-wide DOM collaboration
Stockholm
Wisconsin
LBL
DESY
Chiba
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Photomultiplier Hamamatsu R7081-02 (10,
10-stage, 1E08 gain)

• Selection criteria (_at_ -40 C)
• Noise lt 300 Hz (SN, bandwidth)
• Gain gt 5E7 at 2kV (nom. 1E7 margin)
• P/V gt 2.0 (Charge res. in-situ gain calibration)
• Notes
• Only Hamamatsu PMT meets excellent low noise
  rates!
• Tested three flavors of R7081.

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SPE Charge Spectrum
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Setup photo
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Expected Data Rates

• PMT noise rate of 1 kHz is expected
• "Scintillation" of glass introduces correlations!
• Two DOMs/twisted pair ( , kg, flights,...)
• Rates/pair (bits/s) for coincidence mode
• (with zero suppression and compression)
• None 18 kbytes/s x 2 x 10 400 kbits/s
• Soft 6-8 kbytes x 2 x 10 160 kbits/s
• Hard lt1 kbyte/s x 2 x 10 20 kbits/s
• Demonstrated in the lab 1 Mbit/s

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IceCube Software
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ROMEO Optical detector simulator

• ROOT Ttask base
• Full detector simulation

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JULIeT Particle Propagator
Monte-Carlo Simulation
Numerical Calculation
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Angular resolution as a function of zenith angle
Waveform information not used. Will
improve resolution for high energies !
0.8 0.6

• above 1 TeV, resolution 0.6 - 0.8 degrees for
  most zenith angles

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Energy Spectrum Diffuse Search
Blue after downgoing muon rejection Red after
cut on Nhit to get ultimate sensitivity
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Project status
HEAPA 2004

• Startup phase has been approved by the U.S. NSB
  and funds have been allocated.
• 100 DOMs are produced and being tested this
  year.
• Assembling of the drill/IceTop prototypes is
  carried out at the pole last season.
• Full Construction start in 04/05 (this year!!)
  takes 6 years to complete.
• Then 16 strings per season, increased rate may be
  possible.

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Right now at the pole
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GZK EHEn detection
HEAPA 2004

• What is the GZK mechanism?
• EHE n/m/t Propagation in the Earth
• Expected intensities at the IceCube depth
• Atmospheric m background
• Event rate

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UHE (EeV or even higher) Neutrino Events
Arriving Extremely Horizontally

• Needs Detailed Estimation
• Limited Solid Angle Window

(srNA)-1 600 (s/10-32cm2) -1(r/2.6g cm-3) -1
km
Involving the interactions generating
electromagnetic/hadron cascades
mN
mX ee-
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Products
ne
nm
nt
m
t
p
e/g
ne
Weak
Weak
nm
Weak
Weak
nt
Weak
Weak
Incoming
e/g
Cascades
Decay
Decay Weak
Pair/decay Bremss
m
Pair
Pair
PhotoNucl.
DecayPair
Pair Bremss Decay
Decay
Decay Weak
Decay
Decay
t
PhotoNucl.
Pair
p
Cascades
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Upward-going
Downward going!!
HEAPA 2004
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Down-going events dominate
Atmospheric m is strongly attenuated
Up
Down
HEAPA 2004
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Flux as a function of energy deposit in km3

• dE/dXbE DEDXbE

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Uncertainty in Prompt Lepton Cross
Sections

• The uncertainty 3 orders
• Need for accelerator data extrapolation
• Crossover between 40TeV and 3 PeV

ZhVd
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Constraining Charm Neutrino models by
analysis of downgoing Muon Data

• Very preliminary sensitivity on ZHV-D model
• Systematics to be well understood
• Potential to set a more restrictive limit than
  neutrino diffuse analyses

ZHVd
AMANDA II (muons)
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IceCube EHE n Sensitivity
90 C.L. for 10 year observation

• Published in Phys. Rev. D
• S.Yoshida, R.Ishibashi, H,Miyamoto, PRD 69
  103004 (2004)

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IceTop EeV detection
Potential to reject this background for EeV
neutrinos by detecting the fringe of coincident
horizontal air shower in an array of water
Cherenkov detectors (cf. Ave et al., PRL 85
(2000) 2244, analysis of Haverah Park)
back
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Grand Summary
RICE
Flys Eye
Macro
AGASA
Frejus
Baikal
Amanda-B
NT-214
AMANDA-II ANTARES
AUGER nt
IceCube km3 in sea
OWL, EUSO
Courtesy Learned Mannheim Spiering