Download - Icefishing for… Icefishing for… Neutrinos Neutrinos Francis Halzen University of Wisconsin
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Icefishing Icefishing for…for…
NeutrinosNeutrinos
Francis HalzenFrancis Halzen
University of University of WisconsinWisconsin
http://http://icecube.wisc.eduicecube.wisc.edu
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seeingseeing
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SeeingSeeing::Cosmic MessengersCosmic Messengers
•light ( Alhassan 1000 )light ( Alhassan 1000 )•light of other light of other wavelengths:wavelengths:
blue, blue, redred, , infraredinfrared, , X-X-raysrays, , radiowavesradiowaves,….,….
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Supernova shocksexpanding in
interstellar medium
Crab nebulaCrab nebula
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X-ray pictureX-ray picture Infrared pictureInfrared picture
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Cosmic AcceleratorsCosmic AcceleratorsHigh EnergyHigh Energy
• large magnetic fieldlarge magnetic field• over large distancesover large distances
cfr cfr FermilabFermilab
requiresrequiresmany Teslamany Tesla(~10 Tesla)(~10 Tesla)
many kilometersmany kilometers(~4 km)(~4 km)
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Crab nebula
Supernova shocksexpanding in
interstellar medium
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Active Galaxies: JetsActive Galaxies: Jets
VLA image of Cygnus A
20 TeV gamma rays20 TeV gamma raysHigher energies obscured by IR lightHigher energies obscured by IR light
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GammaGammaRayRayBurstBurst
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1 pc ~ 3 ly ~ 101 pc ~ 3 ly ~ 101818 cm cm
1000 Mpc1000 Mpc
100 Mpc100 Mpc
10 Mpc10 Mpc
1 Mpc1 Mpc
100 kpc100 kpc
10 kpc10 kpc
1 kpc1 kpc
0.1 kpc0.1 kpc
gamma ray burstsgamma ray bursts
closest active galaxiesclosest active galaxieslocal supeclusterlocal supeclusterVirgoVirgo
halohalo
center of galaxycenter of galaxy
galaxy (scale height)galaxy (scale height)
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SeeingSeeing::Cosmic MessengersCosmic Messengers
•light ( Alhassan 1000 )light ( Alhassan 1000 )•light of other light of other wavelengths:wavelengths:
blue, red, blue, red, infraredinfrared, X-, X-rays, radiowaves…rays, radiowaves…
•NeutrinosNeutrinos instead of instead of photons (particles of photons (particles of light)light)
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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 3K cosmic
background
X-ray Giacconi … 1965 Sun, moon neutron stars
accreting binaries
Radio Hewish,
Bell 1967 Ionosphere Pulsars
-rays military 1960? Thermonuclear
explosions Gamma ray
bursts
New Window on Universe?New Window on Universe? Expect SurprisesExpect Surprises New Window on Universe?New Window on Universe? Expect SurprisesExpect Surprises
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the science: a samplerthe science: a sampler• Source(s) of cosmic raysSource(s) of cosmic rays:
gamma-ray bursts, active galaxies, cosmological remnants…?
• Dark matterDark matter
• MoreMore
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A particle that is almost A particle that is almost nothing may tell us everything nothing may tell us everything
about the Universe.about the Universe.
Christine Sutton,Christine Sutton,
in Spaceship Neutrinoin Spaceship Neutrino
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You can see a lot by looking.You can see a lot by looking.
Yogi BerraYogi Berra
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How large a neutrino telescope?How large a neutrino telescope?
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Kilometer-scaleKilometer-scaleneutrino detectors?neutrino detectors?
How?How?
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I have done a terrible thing, I I have done a terrible thing, I have invented a particle that have invented a particle that
cannot be detected.cannot be detected.
Wolfgang PauliWolfgang Pauli
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neutrino
muon or tau Cerenkov
light cone
Detector interaction
•Infrequently, a cosmic neutrino is captured in the ice, i.e. the neutrino interacts with an ice nucleus
•The muon radiates blue light in its wake
•In the crash a muon (or electron, or tau) is produced
•Optical sensors capture (and map) the light
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Optical ModuleOptical Module
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How to build a How to build a detector detector
Use the phenomenon of Cherenkov lightUse the phenomenon of Cherenkov light
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Copyright © 2001 Purdue University
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neutrino
muon or tau Cherenkov
light cone
Detector interaction
•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
•The muon radiates blue light in its wake
•Optical sensors capture (and map) the light
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South PoleSouth Pole
AMANDA– 1 mile deepAMANDA– 1 mile deep
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Size perspectiveSize perspective
50 m
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AMANDA AMANDA Event Event
Signatures:Signatures:MuonsMuons
AMANDA AMANDA Event Event
Signatures:Signatures:MuonsMuons
+ N + N + + XX
CC muon neutrinoCC muon neutrinoInteractionInteraction tracktrack
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A real event in A real event in AMANDAAMANDA
• Recorded on May Recorded on May 1, 2003 1, 2003 (demonstrating (demonstrating “daily nu” “daily nu” realtime filtering)realtime filtering)
tim
eti
me
time
time
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seeing with neutrinosseeing with neutrinos
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Neutrino sky seen by AMANDANeutrino sky seen by AMANDA
• Monte Carlo methods verified on dataMonte Carlo methods verified on data
• ~ 300 neutrinos from 130 days of B-10 operation~ 300 neutrinos from 130 days of B-10 operation ((Nature 410, 441, 2001)
cos()
Data
Atmospheric n MC
0
5
10
15
20
25
30
35
40
-1 -0.9 -0.8 -0.7 -0.6 -0.5 -0.4 -0.3 -0.2 -0.1 0
Cos
events
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AMANDA II 2000AMANDA II 2000
1555 events1555 events
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AMANDA II 2000AMANDA II 2000
1555 events1555 events
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The Challenge is TechnologicalThe Challenge is Technological
• Needle in a haystack: have to find each Needle in a haystack: have to find each neutrino in a background of more than neutrino in a background of more than one million background eventsone million background events
• Do this at a rate of 100 muons per secondDo this at a rate of 100 muons per second
• Deploy a particle physics detector in a Deploy a particle physics detector in a hostile environmenthostile environment
• Solutions demonstrated with AMANDASolutions demonstrated with AMANDA
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We were lucky!We were lucky!
• Light travels more than 100 meters Light travels more than 100 meters in the ultra-pure, sterile icein the ultra-pure, sterile ice
• Scattering of the light is manageableScattering of the light is manageable• We use the existing infrastructure of We use the existing infrastructure of
the National Science Foundation’s the National Science Foundation’s South Pole Research StationSouth Pole Research Station
• Makes the construction of the ultimate kilometerMakes the construction of the ultimate kilometer--
scale neutrino observatory possiblescale neutrino observatory possible
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Ignorance and luck represent a Ignorance and luck represent a powerful mix fostering original powerful mix fostering original
research.research.
Wisconsin Research Profiles in DiscoveryWisconsin Research Profiles in DiscoveryYes, it was me.Yes, it was me.
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Seven Wonders of Modern Astronomy
The Sharpest The Biggest The Farthest Flung
The Most Extensive The Swiftest The Deadliest
The Wierdest
www.sciam.com/1999/1299engineering/1299musser.html
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Science!Science!
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1 km
2 km
1 km
deep and shallow ice deep and shallow ice for future IceCubefor future IceCube
IceCubeIceCube
0.02 0.1 0.5
ScatteringScatteringcoefficientcoefficient(1/m)(1/m)vs. depthvs. depth
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Education and Outreach• Astronomy in the IceAstronomy in the Ice to
Science in the Ice
– Partner with NSF MSP SCALE project to bring Polar Science to nearly 1 million mostly underrepresented K-12 students
LA Denver
Madison Providence
• One time events to multi-media resourcesOne time events to multi-media resources
– Use Exploratorium “Origins” project, NSF’s eTeach & National Science Digital Library to produce & distribute interactive, engaging resources
• Math Science Partnership Collaborative ProposalMath Science Partnership Collaborative Proposal
– Build on Hands-on Universe model to provide student access to high energy cosmic ray and neutrino data
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Building Building AMANDAAMANDABuilding Building
AMANDAAMANDA
Drilling Holes with Hot WaterDrilling Holes with Hot Water
The Optical ModuleThe Optical Module
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Christchurch, New ZealandChristchurch, New ZealandInternational Antarctic CenterInternational Antarctic Center
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McMurdo, AntarcticaMcMurdo, Antarctica
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LC-130 HerculesLC-130 Hercules
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thethe domedome
the new stationthe new station
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Building AMANDABuilding AMANDA
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Is ice the solution, really…?
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Assessment:Assessment:The planned IceCube experiment can open a The planned IceCube experiment can open a new window on the Universe by detecting new window on the Universe by detecting very high energy neutrinos from objects very high energy neutrinos from objects across the Universe. The science is well across the Universe. The science is well motivated and exciting, the detection motivated and exciting, the detection technique is proven, and the experiment technique is proven, and the experiment appears ready for construction.appears ready for construction.
Neutrinos and Beyond: New Windows on NatureNeutrinos and Beyond: New Windows on Nature
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South PoleSouth PoleDark sectorDark sector
AMANDAAMANDA
IceCubeIceCubePlanned Location 1 km eastPlanned Location 1 km east
Dome
SkiwaySkiway
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South PoleSouth PoleDark sector
AMANDAAMANDA
IceCubeIceCube
Dome
Skiway
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Assembled DOM
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The IceCube CollaborationThe IceCube Collaboration(1) Bartol Research Institute, University of Delaware, Newark, DE 19716, USA(2) Fachbereich 8 Physik, BUGH Wuppertal, D-42097 Wuppertal, Germany(3) Universite Libre de Bruxelles, Science Faculty CP230, Boulevard du Triomphe, B-1050
Brussels, Belgium(4) CTSPS, Clark-Atlanta University, Atlanta, GA 30314, USA(5) Dept. of Physics, Chiba University, Chiba 263-8522 Japan(6) DESY-Zeuthen, D-15738 Zeuthen, Germany(7) Blackett Laboratory, Imperial College, London SW7 2BW, UK(8) Institute for Advanced Study, Princeton, NJ 08540, USA(9) Dept. of Physics and Astronomy, University of Kansas, Lawrence, KS 66045, USA(10) Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USA(11) Dept. of Astronomy and Astrophysics, Pennsylvania State University, University Park, PA
16802, USA(12) Dept. of Physics, Pennsylvania State University, University Park, PA 16802, USA(13) Dept. of Physics, Southern University, Baton Rouge, LA 70813, USA(14) Dept. of Physics, University of California, Berkeley, CA 94720, USA(15) Institute of Physics, University of Mainz, Staudinger Weg 7, D-55099 Mainz, Germany(16) Dept. of Physics, University of Maryland, College Park, MD 20742, USA(17) University of Mons-Hainaut, 7000 Mons, Belgium(18) Departamento de Fisica, Universidad Simon Bolvar, Caracas, 1080, Venezuela(19) Dept. of Astronomy, University of Wisconsin, Madison, WI 53706, USA(20) Dept. of Physics, University of Wisconsin, Madison, WI 53706, USA(21) SSEC and PSL, University of Wisconsin, Madison, WI 53706, USA(22) Physics Dept., University of Wisconsin, River Falls, WI 54022, USA(23) Division of High Energy Physics, Uppsala University, S-75121 Uppsala, Sweden(24) Faculty of Physics and Astronomy, Utrecht University, NL-3584 CC Utrecht, The Netherlands(25) Dept. of Physics, Stockholm University, SE-10691 Stockholm, Sweden(26) Vrije Universiteit Brussel, Dienst ELEM, B-1050 Brussels, Belgium
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The scientists are naïve and The scientists are naïve and arrogant. They can get tangled arrogant. They can get tangled
up in their own underwear up in their own underwear faster than anybody.faster than anybody.
Anthoni FragomeniAnthoni FragomeniCOBE observatory managerCOBE observatory manager
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AMANDAAMANDA
DrillingDrillingeducation
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IceCubeIceCube
• start 02start 02• first first
strings 04strings 04•
completed completed <09<09
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IceCube Funding, by Phase
$0
$10
$20
$30
$40
$50
$60
$70
2000 2001 2002 2003 2004 2005 2006 2007 2008 2009 2010 2011 2012 2013Fiscal Year
$M Concept/Development Implementation Operations & Maintenance
first 8 stringsfirst 8 strings
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The sole purpose of human The sole purpose of human existence is to kindle a light in existence is to kindle a light in
the darkness of mere being.the darkness of mere being.
Carl Gustav YoungCarl Gustav Young
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The EndThe End
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Aurora Australis
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IceCubeIceCube
1400 m1400 m
2400 m2400 m
AMANDAAMANDA
South PoleSouth Pole
IceTopIceTop
RunwayRunway• 80 Strings80 Strings
• 4800 PMT4800 PMT • Instrumented Instrumented
volume: 1 km3 volume: 1 km3 (1 Gton)(1 Gton)
• IceCube is designed IceCube is designed to detect neutrinos to detect neutrinos of all flavors at of all flavors at energies from 10energies from 1077 eV eV (SN) to 10(SN) to 102020 eV eV
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1 km
AMANDAAMANDA IIII
µ-event in µ-event in IceCubeIceCube
300 atmospheric 300 atmospheric neutrinos per dayneutrinos per day
IceCubeIceCube:: -> Larger telescope-> Larger telescope -> Superior detector-> Superior detector
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Eµ= 10 TeVEµ= 6 PeV
Muon EventsMuon Events
Measure energy by counting the number of fired PMT. (This is a very simple but robust method)
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The effort to understand the The effort to understand the Universe is one of the very few Universe is one of the very few
things that lifts human life things that lifts human life above the level of farce and above the level of farce and gives it some of the grace of gives it some of the grace of
tragedytragedy
Steve WeinbergSteve Weinberg
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The AMANDA detectorThe AMANDA detector
• Construction began in Construction began in 1995 (4 strings)1995 (4 strings)
• AMANDA-II completed in AMANDA-II completed in 2000 (19 strings total)2000 (19 strings total)
• 677 optical modules677 optical modules• 200 m across200 m across• ~500 m tall (most densely ~500 m tall (most densely
instrumented volume)instrumented volume)
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The effort to understand the The effort to understand the Universe is one of the very few Universe is one of the very few
things that lifts human life things that lifts human life above the level of farce and above the level of farce and gives it some of the grace of gives it some of the grace of
tragedytragedy
Steve Weinberg
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Blue glow of the particleBlue glow of the particle (produced by the neutrino at (produced by the neutrino at locations removed by up to locations removed by up to 10 kilometers) lights up the10 kilometers) lights up the
sensors in the icesensors in the ice
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DAQ, Online filter
• Raw: ~4 MB/s
• Reconstructed: 100 GB/day
Tape
• Filtered: 10GB/day
Satellite
Data Rates
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How large a neutrino telescope?How large a neutrino telescope?
• 1 neutrino per lifetime1 neutrino per lifetime (30,000 days) (30,000 days) in our in our bodybody (100 kg or 0.1 m(100 kg or 0.1 m33 ) means ) means
• 0.00003 per day in 0.1 m0.00003 per day in 0.1 m33 oror
• 3 per day in 100,000 m3 per day in 100,000 m33 ( roughly SuperK with( roughly SuperK with 40x40x40 m40x40x40 m33) or) or
• 300,000 per day in 300,000 per day in 101099 m m33 or or 1 km1 km33
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IceCubeIceCube
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Classroom visits – sharing the excitement, technology, and science
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IceCube is part of the HEPAPIceCube is part of the HEPAP “ “Roadmap to Particle Physics”.Roadmap to Particle Physics”.
It is the only university basedIt is the only university based project.project.
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AMANDA IIAMANDA II
•upgoing muonupgoing muon
• 61 modules61 modules
ttiimmee
size ~size ~ number of photonsnumber of photons
4~5 neutrinos/day4~5 neutrinos/day on-lineon-line
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AMANDA IIAMANDA II
•upgoing muonupgoing muon
• 61 modules61 modules
ttiimmee
size ~size ~ number of photonsnumber of photons
4~5 neutrinos/day4~5 neutrinos/day on-lineon-line
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Neutrino EventNeutrino Event
detecteddetected
October 26, 02October 26, 02
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Point source search 2000Point source search 2000
AMANDA-IIAMANDA-II• Cuts optimized for Cuts optimized for
each declination each declination band band
• Analysis developed Analysis developed with azimuth-with azimuth-scrambled data for scrambled data for blindnessblindness
• 25,000 m25,000 m22 area above area above 10 TeV10 TeV
2000 data2000 data::Contamination by cosmic Contamination by cosmic ray muons: <10% (above ray muons: <10% (above 110 degrees)110 degrees)
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AMANDA, South PoleAMANDA, South Pole
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ENGINEERING AND INSTRUMENTATION-UNIVERSITY OF WISCONSIN MADISON
Hose Winch for the Ice Cube ProjectHose Winch for the Ice Cube ProjectHose Winch for the Ice Cube ProjectHose Winch for the Ice Cube Project
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Receiving drum weldmentReceiving drum weldmentReceiving drum weldmentReceiving drum weldment
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How to build a neutrino How to build a neutrino detectordetector
• Look for the neutrino’s interaction product (e,Look for the neutrino’s interaction product (e,,,))• Use the earth as a filterUse the earth as a filter
• 1:10,000,000 1:10,000,000
background rejection!background rejection!
EarthEarth
DetectorDetector
cosmic raycosmic ray