Transcript Science_Expeditions_Slideshow - IceCube

“Ice Fishing for… Neutrinos”
AMANDA/ICECUBE
Department of Physics
Science Expeditions:
Wows & Whys!
April 5th, 2003
Seeing: Cosmic Messengers
• Visible light (Alhassan ~1000)
• Light of other wavelengths
(e.g. radiowaves, X-rays, etc.)
• Neutrinos!
Neutrinos, they are very small,
they have no charge and have no mass,
and do not interact at all.
John Updike
“I have done a terrible thing…
…I have invented a particle
that cannot be detected”
-Wolfgang Pauli
But Neutrino Astronomy Began with
Solar Neutrinos 30 Yrs Ago!
•Superkamiokande’s
portrait of the Sun
in neutrinos:
compilation of the
directions of all
neutrinos observed
• Discovery of
neutrino mass!
R. Svoboda, LSU
Sources of Neutrinos
• The Earth’s atmosphere: every second one
thousand neutrinos, made in the interactions of
cosmic rays with nitrogen and oxygen nuclei, pass
through your body-- one in a lifetime interacts
• The sun: 1014 stream through our body every
second (even at night)
• Supernovae: 20 neutrinos detected from a dying
star in 1987
• Beyond the sun? Requires kilometer-scale
neutrino detectors (i.e. Ice Cube).
Supernovae
We did see 20 neutrinos
from one supernova in 1987
SN1987A
• Measurements of
many neutrino
properties with
only ~20 events
(mass, ….)
• Several mysteries
remain awaiting a
new observation
Hubble, NASA
Supernova shocks
expanding in
interstellar medium
Crab nebula
Active Galaxies: Jets
20 TeV gamma rays
Higher energies obscured by IR light
VLA image of Cygnus A
Radiation field:
Produces cosmic ray beam
Merger of Neutron Star and
Black hole
Gamma Ray Bursts (GRBs)
•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
muon
light cone
Detector
•The muon radiates blue light in its wake
•Optical sensors capture (and map) the light
interaction
neutrino
This characteristic blue light, known as Cherenkov Radiation,
Copyright © 2001 Purdue University
is also seen in nuclear reactors.
Another example:
velocity muon > velocity light
Like a sonic boom... for light.
How large a neutrino telescope?
• 1 neutrino per lifetime (30,000 days) in our body
(100 kg or 0.1 m3 ) means
• 0.00003 per day in 0.1 m3 or
• 3 per day in 100,000 m3 ( roughly SuperK with
40x40x40 m3) 0r
• 300,000 per day in 109 m3 or 1 km3 (we actually
will detect 300 per day because we limit ourselves
to neutrinos above 100 GeV as opposed to 1 GeV
which means 100 1.7).
Neutrino Astronomy to the
Rescue…
• Energy balance of the Universe: roughly equal
amounts of light and neutrinos
• 1950’s: proposals to use neutrinos rather than
(the particles of) light as astronomical
messengers
• 1970’s: first attempts to construct neutrino
telescopes in deep ocean water
• 1987: ice proposed as a detector
• 1998: AMANDA detects first neutrinos
The Challenge is Technological
• Needle in a haystack: have to find each
neutrino in a background of more than
one million background events.
• Do this at a rate of 100 muons per second.
• Deploy a particle physics detector in a
hostile environment.
• Solutions demonstrated with AMANDA
We were lucky …
• Light travels more than 100 meters in the ultrapure, sterile ice.
• Scattering of the light is manageable.
• We use the existing infrastructure of the
National Science Foundation’s South Pole
Research Station.
• Makes the construction of the ultimate
kilometer-scale neutrino observatory possible.
Optical Cherenkov
Neutrino Telescope Projects
ANTARES
La-Seyne-sur-Mer, France
NEMO
Catania, Italy
BAIKAL
Russia
DUMAND
Hawaii
(cancelled 1995)
NESTOR
Pylos, Greece
AMANDA, South Pole, Antarctica
The AMANDA Collaboration
7 US, 9 European and 1 South American institutions, ~ 110 members:
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Bartol Research Institute, University of Delaware, Newark, USA
BUGH Wuppertal, Germany
Universite Libre de Bruxelles, Brussels, Belgium
Universidad Simon Bolivar, Caracas, Venezuela
DESY-Zeuthen, Zeuthen, Germany
Dept. of Technology, Kalmar University, Kalmar, Sweden
Lawrence Berkeley National Laboratory, Berkeley, USA
Dept. of Physics, UC Berkeley, USA
Institute of Physics, University of Mainz, Mainz, Germany
University of Mons-Hainaut, Mons, Belgium
University of California, Irvine, CA
Dept. of Physics, Pennsylvania State University, University Park, USA
Physics Department, University of Wisconsin, River Falls, USA
Physics Department, University of Wisconsin, Madison, USA
Division of High Energy Physics, Uppsala University, Uppsala, Sweden
Fysikum, Stockholm University, Stockholm, Sweden
Vrije Universiteit Brussel, Brussel, Belgium
Recently: Maryland, Chiba University, Imperial College London…
AMANDA
•Neutrino Astronomy
•AMANDA: The First
Neutrino Telescope
•Proof of Concept for
IceCube
The
AMANDA
Detector
Antarctic
Muon
And
Neutrino
Detector
Array
Depth
1.5 km
Christchurch, New Zealand
International Antarctic Center
McMurdo, Antarctica
Amundsen-Scott South Pole Station
South Pole
AMANDA, South Pole
Optical
sensor
The Counting House
Building
AMANDA
Drilling Holes with Hot Water
The Optical Module (OM)
Receiving drum weldment
Building AMANDA: The Optical
Module and the String
Optical Module (OM)
Photomultiplier: 10 inch Hamamatsu
Active PMT base
Glass sphere: Nautillus
Mu metal magnetic shield
South Pole Air Shower Experiment (SPASE)
South Pole
Dark sector
Skiway
AMANDA
Dome
IceCube
AMANDA-II: 200 x 500 cylinder + 3 1km strings, running since 2000
AMANDA
Event
Signatures:
Muons
CC muon neutrino
interaction
 track
nm + N  m + X
AMANDA
Event
Signatures:
Cascades
 CC electron and tau
neutrino interaction:
 n(e,,) + N  (e, ) + X
 NC neutrino interaction:
nx + N  nx + X
Cascades
The IceCube Collaboration
Institutions: 11 US and 9 European institutions
(most of them are also AMANDA member institutions)
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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
Division of High Energy Physics, Uppsala University, Uppsala, Sweden
Fysikum, Stockholm University, Stockholm, Sweden
University of Alabama, Tuscaloosa, USA
Vrije Universiteit Brussel, Brussel, Belgium
IceCube
IceTop
AMANDA
South Pole
Runway
• 80 Strings
• 4800 PMT
• Instrumented volume:
1 km3 (1 Gton)
1400 m
• IceCube is designed to
detect neutrinos of all
flavors at energies from
107 eV (SN) to 1020 eV
2400 m
South Pole
South Pole
Dark sector
Skiway
AMANDA
Dome
IceCube
Planned Location 1 km east
South Pole
Dark sector
Skiway
AMANDA
Dome
IceCube
µ-event in
IceCube
AMANDA II
IceCube:
--> Larger telescope
--> Superior detector
1 km
New Window on Universe?
Expect Surprises
Telescope
User
date
Intended Use
Actual use
Optical
Galileo
1608
Navigation
Moons of Jupiter
Optical
Hubble
1929
Nebulae
Expanding
Universe
Radio
Jansky
1932
Noise
Radio galaxies
Micro-wave
Penzias,
Wilson
1965
Radio-galaxies, noise
X-ray
Giacconi …
1965
Sun, moon
Radio
Hewish,
Bell
1967
Ionosphere
Pulsars
-rays
military
1960?
Thermonuclear
explosions
Gamma ray
bursts
3K cosmic
background
neutron stars
accreting binaries
The 21st Century will feature Neutrino-Astronomy with AMANDA/IceCube!
AMANDA & ICECUBE have tremendous
potential for new physics.
The End