Aspen Institute for Physics 02 Francis Halzen

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Aspen Institute for Physics 02Francis Halzen

• the sky gt 10 GeV photon energy
• lt 10-14 cm wavelength
• gt 108 TeV particles exist
• Flys Eye/Hires
• they should not
• more/better data
• arrays of air Cherenkov telescopes
• 104 km2 air shower arrays
• km3 neutrino detectors

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Energy (eV)
CMB
1 TeV
Radio
Visible
GeV g-rays
Flux
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With 103 TeV energy, photons do not reach us from
the edge of our galaxy because of their small
mean free path in the microwave background.

• ?g gCMB ?????e e-

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n
/ / / / / / / / / / / / / / / / /
TeV sources!
cosmic rays
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Acceleration to 1021eV? 102
Joules 0.01 MGUT

• dense regions with exceptional
• gravitational force creating relativistic
• flows of charged particles, e.g.
• annihilating black holes/neutron stars
• dense cores of exploding stars
• supermassive black holes

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Cosmic Accelerators
E GcBR
R GM/c2
magnetic field
energy
E GBM
mass
boost factor
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Supernova shocks expanding in interstellar medium
Crab nebula
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Active Galaxies Jets
20 TeV gamma rays Higher energies obscured by IR
light
VLA image of Cygnus A
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Gamma Ray Burst
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E G?B M
E gt 1019 eV ?

• quasars G _at_ 1 B _at_ 103G M _at_?109 Msun
• blasars 10
• neutron stars G _at_ 1 B _at_ 1012G M _at_ Msun
• black holes
• .
• .
• grb ?? 102

gt
gt
emit highest energy gs!
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Particles gt 1020 eV ?
new astrophysics?

• not protons
• cannot reach us from cosmic accelerators
• lint lt 50 Mpc
• no diffusion in magnetic fields
• doublets, triplet
• not photons
• g Bearth e e- not seen
• showers not muon-poor
• not neutrinos
• snp ? 10-5 spp ?????no air showers

trouble for top-down scenarios
snp ? spp with TeV - gravity unitarity?
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Particles gt 1020 eV ?
new astrophysics?

• not protons
• cannot reach us from cosmic accelerators
• lint lt 50 Mpc
• no diffusion in magnetic fields
• doublets, triplet
• not photons
• g Bearth e e- not seen
• showers not muon-poor
• not neutrinos
• snp ? 10-5 spp ?????no air showers

trouble for top-down scenarios
snp ? spp with TeV - gravity unitarity?
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TeV-Scale Gravity Modifies PeV Neutrino Cross
Sections!
103 TeV
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The Oldest Problem in Astronomy

• No accelerator
• No particle candidate (worse than dark matter!)
• Not photons (excludes extravagant particle
  physics ideas)

What Now?
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black hole
radiation enveloping black hole
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neutrinos associates with the source of the
cosmic rays?
even neutrons do not escape
neutrons escape
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Radiation field Ask astronomers
Produces cosmic ray beam
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neutrinos associates with the source of the
cosmic rays?
even neutrons do not escape
neutrons escape
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• Infrequently, a cosmic neutrino is captured in
  the ice, i.e. the neutrino interacts with an ice
  nucleus
• In the crash a muon (or electron,
• or tau) is produced

Cherenkov light cone
muon
interaction
Detector

• The muon radiates blue light in its wake
• Optical sensors capture (and map) the light

neutrino
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Optical Module
Photomultiplier 10 inch Hamamatsu
Active PMT base
Glass sphere Nautillus
Mu metal magnetic shield
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Amundsen-Scott South Pole Station
South Pole
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Optical sensor
The Counting House
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1.5 km
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Neutrino sky seen by AMANDA
events

• Monte Carlo methods verified on data
• 300 neutrinos from 130 days of B-10 operation
  (Nature 410, 441, 2001)

Cos(?)
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Atmospheric Muons and Neutrinos
Lifetime 135 days Lifetime 135 days Lifetime 135 days
Observed Data Predicted Neutrinos Predicted Neutrinos
Triggered Triggered 1,200,000,000 4574 4574
Reconstructed upgoing Reconstructed upgoing 5000 571 571
Pass Quality Cuts (Q 7) Pass Quality Cuts (Q 7) 204 273 273
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Search for a diffuse n-flux of astrophysical
sources

• Method
• Assume a diffuse neutrino flux (Hypothesis),
  e.g.
• dN/dE 10-5E-2/(cm2 sec GeV)
• The background is the atmospheric neutrino flux
  (after quality cuts) 200 events
• Apply energy cut.

Preliminary
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Compare to Mrk 501 gamma rays
Field of viewContinuous 2 p ster !
AMANDA limit B10 1year only
Sensitivity of 3 years of IceCube
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AMANDA II - the full detector
120m

horizontal neutrino detection possible
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...online 2001 analysis
2 recent events
October 1, 2001
October 10, 2001
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...online 2001 analysis
Zenith angle comparison with signal MC
? real-time filtering at Pole ? real-time
processing (Mainz) Left plot ? 20 days
(Sept/Oct 2001) ? 90 ??candidates above 100
atmospheric muons
atmospheric ?s
4.5 ??candidates / day
(data/MC normalized above 100)
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AMANDA II first look (16 days)
Zenith angle distribution
MC energy
? up to now 10 of 2000 data analysed ? after
cuts about 5 ?? per day ? cut efficiency
improved from AMANDA B10 by 3-5
Average energy 0.3 TeV
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AMANDA Proof of Concept

• since 1992 we have deployed 24 strings with more
  than 750 photon detectors (basically 8-inch
  photomultipliers).
• RD detector for proof of concept 375 times
  SuperK instrumented volume with 1.5 the total
  photocathode area.
• IceCube 45 times AMANDA II instrumented volume
  with 7 times the total photocathode area.

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AMANDA Proof of Concept

• 80 modules first nus, Astropart. Phys. 13, 1,
  2000
• 302 modules 97 atmospheric neutrino analysis
  published 98, 99 data analysis in progress (1-2
  neutrinos per day).
• 677 modules 01, 02 data analysis in progress (gt5
  neutrino events per day despite higher
  threshold)-- scaling of detector verified!
• Daily nus extract neutrinos from daily satellite
  transmissions.

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IceCube

• 80 Strings
• 4800 PMT
• Instrumented volume 1 km3 (1 Gt)
• IceCube is designed to detect neutrinos of all
  flavors at energies from 107 eV (SN) to 1020 eV

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South Pole
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South Pole
Dark sector
Skiway
AMANDA
Dome
IceCube
Planned Location 1 km east
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South Pole
Dark sector
Skiway
AMANDA
Dome
IceCube
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µ-event in IceCube300 atmospheric neutrinos per
day
AMANDA II
IceCube --gt Larger telescope --gt Superior
detector
1 km
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WIMPs from the Sun with IceCube
J. Edsjö, 2000

• Ice3 will significantly improve the sensitivity.
• Sensitivity
• comparable to
• GENIUS,

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Muon Events
Eµ 10 TeV
Eµ 6 PeV
Measure energy by counting the number of fired
PMT. (This is a very simple but robust
method)
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ne e W m? nm 6400 TeV
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Cascade event
Energy 375 TeV
ne N --gt e- X

• The length of the actual cascade, 10 m, is
  small compared to the spacing of sensors
• roughly spherical density distribution of light
• 1 PeV 500 m diameter
• Local energy deposition good energy resolution
  of neutrino energy

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Enhanced role of tau neutrinos because of SNO
discovery

• Cosmic beam ne nµ nt because of oscillations
• nt not absorbed by the Earth (regeneration)
• Pile-Up near 1 PeV where ideal sensitivity

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Neutrino ID (solid)Energy and angle (shaded)
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nt t
PeV t(300m)
t decays
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?? at EgtPeV Partially contained
Photoelectron density

• The incoming tau radiates little light.
• The energy of the second bang can be measured
  with high precision.
• Clear signature
• Muon Brem would be much brighter than the tau
  (compare to the PeV muon event shown before)

Timing, realistic spacing
Result high effective volume only second bang
seen in Ice3
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SUMMARY

• the sky gt 10 GeV photon energy
• lt 10-14 cm wavelength
• gt 108 TeV particles exist
• Flys Eye/Hires
• they should not
• more/better data
• arrays of air Cherenkov telescopes
• 104 km2 air shower arrays
• km3 neutrino detectors

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The End
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The IceCube Collaboration

• Institutions 11 US and 9 European institutions
• (most of them are also AMANDA member
  institutions)
• Bartol Research Institute, University of Delaware
• BUGH Wuppertal, Germany
• Universite Libre de Bruxelles, Brussels, Belgium
• CTSPS, Clark-Atlanta University, Atlanta USA
• DESY-Zeuthen, Zeuthen, Germany
• Institute for Advanced Study, Princeton, USA
• Dept. of Technology, Kalmar University, Kalmar,
  Sweden
• Lawrence Berkeley National Laboratory, Berkeley,
  USA
• Department of Physics, Southern University and
  A\M College, Baton Rouge, LA, USA
• Dept. of Physics, UC Berkeley, USA
• Institute of Physics, University of Mainz, Mainz,
  Germany
• Dept. of Physics, University of Maryland, USA
• University of Mons-Hainaut, Mons, Belgium
• Dept. of Physics and Astronomy, University of
  Pennsylvania, Philadelphia, USA
• Dept. of Astronomy, Dept. of Physics, SSEC, PSL,
  University of Wisconsin, Madison, USA
• Physics Department, University of Wisconsin,
  River Falls, USA

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Upper limits to the muon flux from point sources
10-13
Southern Sky
Northern Sky
m ? cm-2 s-1
10-14
10-15
-90
0
-45
90
45
declination (degrees)
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cosmic ray puzzle
neutrinos
protons
TeV g - rays
1 km3 high energy detectors
104 km2 air shower arrays

• atmospheric Cherenkov
• space-based

• AMANDA / Ice Cube
• Antares, Nestor,
• NEMO

• Veritas, Hess, Magic
• GLAST

• Hi Res, Auger,
• Airwatch,
• OWL, TA

e.g.

• particle physics
• and cosmology
• dark matter search
• discovery

• short-wavelength
• study of supernova
• remnants and galaxies

also
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AMANDA NEUTRINO SKY