neutrino
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Transcript of neutrino
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neutrino
Particle Astrophysics (3) John Carr Centre de Physique des Particules de Marseille (IN2P3/CNRS)
CERN Summer Student Lectures, 24 July 2002
Cosmic Ray ObservationsGamma Rays AstronomyNeutrino Astronomy
High Energy Astronomy
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GeV: atmosphere
Gravity waves
Axions
Electromagneticradiation -> 100 TeV
Cosmic rayparticles -> 1020 eV
Neutrinos(MeV: sun, SNGeV: atmospherePeV: CR accelerators)
Dark matter
(W. Hoffmann)
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Thermal Radiation from Stars
103 105 107 109 1011 1013 1015
frequency(MHz)
Flux watts/m2
106
102
10-2
10-6
10-12
i.r. u.v. X ray gamma rays->
T=10000KT=6000K
Normal Stars surface temperature ~3000 to 30000K thermal radiation: radio ultra -violet non-thermal radiation: X-rays, gamma rays ( higher in energy more extreme is the source)
radio
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The Crab in Multi-Wavelengths Photons
Infrared Optical X-rayRadio
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Galactic Co-ordinate System
+180°180°
+90°
90°
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?
Multi-Wavelength Photons
Infra-rouge
Ondes radio
Lumière visible
Rayons X
Rayons gamma
Neutrinos
Satellite COBE
Radio télescope de Bonn
Télescope du Mont Palomar
Satellite INTEGRAL
Satellite CGRO
Télescope à neutrinos ANTARES
Radio
Gamma Ray
Infrared
X-ray
Visible light
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Hot plasma (surface of stars)
Bremsstrahlung / Synchrotron Radiation
Inverse Compton Scattering
ee
magnetic field
Annihilation of matter/antimatter
e-
e+
e
e
High energy showers p
interstellar matter
interstellar matter
+
0
Production Mechanisms of Photons
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Non-Photonic Astronomy
Antares (Toulon) Gravitational WavesVirgo (Pisa)
High Energy Cosmic Rays
Auger (Argentina)Neutrinos
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Simulations indicate can get~ 50% of energy of supernova explosion
Cosmic Rays by ~1000 yrs
Acceleration of High Energy Particles p accelerated in shock waves:non-relativistic supernova remnantsrelativistic quasars/microquasars
p/A + p/ e
e
p interact with interstellar matter and produce showers :
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Types of Cosmic Ray Detectors
Satellites
Array of particle detectors on ground
Whipple >1 TeV
Compton Gamma Ray Obs.
EGRET
BATSE 0.1-10GeV
KASCADEp,N 0.3-100PeV
KASCADEp,N 0.3-100PeVGround based telescopes
looking at light produced in atmosphere
Arrays of particle detectors
ground level
top of atmosphere
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Ground, Air Shower Arrays
CASA - KASCADE - AGASA - AUGER
Space observed Shower
EUSO
Satellite, ballons AMS
Whipple-CAT-HEGRA-CELESTE H.E.S.S.-MAGIC-VERITAS
satellite
telescopes
telescopes
CCGO, GLAST
AMANDA, ANTARES
Charged Cosmic Ray Energy Spectrum
‘knee’
‘ankle’
Why thesefeatures ?
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Features of Cosmic Ray SpectrumE
2 dN
/dE
[c m
-2 s
-1 s
r-1 e
V]
E [ eV/nucleus]
E2.7
E3.2
E2.8ankle
dN/dE E propagatio
n
source
= 2.0 to 2.2,..
= 0.3 to 0.6
‘Conventional Wisdom’: Galactic SNR
Extragalactic E > 3 1018 eV exotic E > 7 1019 eV
Source acceleration:
Source cut-off eV
GZK cut-off on CMB E 7 1019 eV
Diffusion models
Galactic lossesE < 3 1018 eVE > 4 1014 eV
Ingredients of models:
isotropicMass composition ?
BG E <1018 Z
Rkpcknee
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Cosmic Rays Spectrum: Knee and Ankle
Flux E2.7 Flux E3
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Explanations of knee (E~3.1015 eV)
• Galactic de-confinement• Single dominant source• Single SNR acceleration multiple SNR acceleration
• Absorption on massive neutrinos in galaxy
• New interaction effects in atmosphere
Various interactions invoked to give threshold at E = 3 1015 eV. eg. p + e n + e, with M(e) = 0.1 eV p + + ,, with M() = 100 eV
Particle Physics type explanations
Astronomy type explanations
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Mass composition from shower depth
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1015 1016 1017
1.5
2.5
0.5
3.5
<ln A>
Energy eV
CASA-BLANCA
Flux E2.5 Mean ln(A)
Mass composition at kneeAverage shower depth and ratio N / Ne sensitive to primary mass (NB. Mass composition extracted is very sensitive to Monte Carlo simulation)
KASCADEKASCADE
KASCADE series of knees at different energies: p,He,..,C,..,Fe. E(Knee) Z knee due to source confinement cut-off ?
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‘GZK cutoff ’ HE cosmic rays
HE gamma rays
Mrk 501 120Mpc
Mrk 421 120Mpc
Sources uniform in universe
100 Mpc
10 Mpc
e+ e
p N
Interaction with background ( infrared and 2.7K CMBR)
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• ‘Bottom-Up’ : acceleration - pulsars in galaxy, - radio lobes of AGN (proximity a problem due to GZK, also should see source)
• ‘Top-Down’ : decay of massive particles - GUT X particles with mass > 1020 eV and long lifetimes - Topological defects - Neutrinos as messenger particle
• New Physics
Explanations of Ankle/ E > 1020 eV events
Particle Physics type explanations
Astronomy type explanations
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M. Masetti
Cosmic rays cannot be used to image the Universe...
PeV proton
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But we try anyway….
308/242.5 in 20
E> 4 1019 eV
SunSNR
Galactic source ?
galactic plane
GC
anti GC See events from same place in < 2.5 3 doublets and 1 triplet
Are these sources?
Or random chance coincidences? Probability < 1% that is chance
8 1017 <E< 8 1018 eV
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Water Cherenkov
Tanks
(1600 each 10m2)
Fluorescence Telescopes (6 telescopes each 30 at 4 sites)
2 sites each 3000km2, E > 5.1018eV
Southern site, Mendoza Province, Argentina
3.5m mirrors
AUGER experiment
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AMS Experiment
Space Shuttle June 1998
Detailed measurements on Cosmic Ray composition: anti-matter ?
limit on anti-helium/helium ratio < 106
International Space Station 2004
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Gamma Ray AstronomyLow Energy Gamma Astronomy from satellites
GLAST XMM Integral
CELESTE
CATSTACEE
CELESTE
High Energy Gamma Astronomy from ground
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Gamma-Ray Burst StoryGamma Ray Burst were first detected by the Vela satellites that were developed in the sixties to monitor nuclear test ban treaties.
1st GRB
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Burst duration
Gamma Ray Bursts
Redshifts measured for about 20 extragalactic distances
1-2 per day observed by BATSE
Some evidencefor GRB onsites of previoussupernova
Isotropic sky distribution
Two types ?
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Imaging Gamma Ray Telescopes
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Future projects in high-energy gamma-ray astronomy
MAGIC
CANGAROO
VERITAS
H.E.S.S.
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Markarian 421: a Blazar
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Flares from Markarian 421
X-Ray
TeV
Correlation of flares at different wavelengths
Timescale of flares indicatesolar system dimensions of source
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Sgr A*
VLA 2cm VLBI 6 mm
Radio
Infrared1”
= 0
,04 p
c
Black Hole horizon ?
Black Hole mass
Black Hole at Galactic Centre
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(EGRET sources)
SUGAR “<0.5% fluctuation”
Cosmic Ray Source 7 from Galactic Centre
AGASA “4.5” effect
Cosmic Rays
RXJ 1713.7-3946
TeV Gamma rays
GeV Gamma raysGalactic centre
Galactic Centre in Multi-Messengers
Cosmic Rays E ~ 1018 eV
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Neutrino Telescope Projects
NESTOR : Pylos, Greece
ANTARES La-Seyne-sur-Mer, France ( NEMO Catania, Italy ) BAIKAL: Lake Baikal, Siberia
DUMAND, Hawaii (cancelled 1995)
AMANDA, South Pole, Antarctica
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Neutrinos weakly interacting in matter
103
106
109
1 103 106
E (TeV)
Equivalent Earth diameter
Neu
trin
o in
tera
ctio
n le
ngth
(km
wa t
e r e
quiv
ale n
t)
Low cross-section good : Astronomic sources and universe transparent to neutrinos Earth transparent up to 100 TeV bad : Need massive detector
Interaction length of neutrinos vs energy
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Why in deep sea / glacier ?
Need enormous mass detector : ~ 30 M tonnes ,Calorimeter in iron > 5000 Meuro for iron alone,H2O matter free, detector system ~ 20 Meuro
Need to have > 1000 m depthto absorb light and cosmics rays
Tank in a cavern eg SuperKamiokande 30 K tonnesMega projects discuss 1 M tonne for few 100 Meuro
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South Pole: glacial ice
1993 First strings AMANDA A1998 AMANDA B10 ~ 300 Optical Modules
2000 ~ 700 Optical Modules
ICECUBE 8000 Optical Modules
AMANDA
> 50GeV
AMANDA
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AMANDA: Drill Holes in ice with Hot Water
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AMANDA Search for Neutrino Point Sources
vertically up horizontally
~ 300 events
Events consistent with neutrinos produced in atmosphere,No evidence yet for astrophyisical sources of neutrinos
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Future in telescopes: ANTARES1996 Started 1996 - 2000 Site exploration and demonstrator line2001 - 2004 Construction of 10 line detector, area ~0.1km2 on Toulon site future 1 km3 in Mediterranean
Angular resolution <0.4° for E>10 TeV
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2500m2500m
300m300mactiveactive
Electro-opticElectro-opticsubmarine cablesubmarine cable ~40km~40km
Junction boxJunction box
Readout cablesReadout cables
Shore stationShore station
anchoranchor
floatfloat
Electronics containersElectronics containers
~60m~60mCompass,Compass,tilt metertilt meter
hydrophonehydrophone
Optical moduleOptical module
Acoustic beaconAcoustic beacon
ANTARES 0.1km2 Detector
~100m
13 strings12 m between storeys
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Demonstrator LineNov 1999- Jun 2000
42°59 N, 5°17 E Depth 1200 m
ANTARES 0.1km2 Site42°50 N, 6°10 E Depth 2400 m
Existing CableMarseille-Corsica
Marseille
ToulonLa Seyne sur Mer
New Cable (2001)La Seyne-ANTARES
ANTARES Deployment Sites
~ 40 deployments and recoveries of test lines for site exploration0.1 km2 detector with 900 Optical Modules, deployment 2002- 2004
ThetysThetys
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ReferencesBooks:Particle Astrophysics, H.V. Klapdor-Kleingrothaus and K. ZuberThe Big Bang, J.SilkThe Physics of Stars, A.C. Phillips
Preprints:Introduction to Cosmology, David H. Lyth, astro-ph/9312022Cosmological Parameters, Michael S. Turner, astro-ph/9904051Non-Baryonic Dark Matter, Lars Bergstrom, hep-ph/0002126
Transparencies of School/Workshop:Neutrino Particle Astrophysics , http://leshouches.in2p3.fr
For more details contact me at: [email protected]
Discussion Session, Council Chamber, 11:15