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Particle Astrophysics (3). John Carr Centre de Physique des Particules de Marseille (IN2P3/CNRS). CERN Summer Student Lectures, 24 July 2002. High Energy Astronomy. Cosmic Ray Observations Gamma Rays Astronomy Neutrino Astronomy.
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Particle Astrophysics (3) John Carr Centre de Physique des Particules de Marseille (IN2P3/CNRS) CERN Summer Student Lectures, 24 July 2002 High Energy Astronomy Cosmic Ray Observations Gamma Rays Astronomy Neutrino Astronomy neutrino
GeV: atmosphere Dark matter Neutrinos (MeV: sun, SN GeV: atmosphere PeV: CR accelerators) Axions Cosmic ray particles -> 1020 eV Gravity waves Electromagnetic radiation -> 100 TeV (W. Hoffmann)
Thermal Radiation from Stars Flux watts/m2 106 102 10-2 10-6 10-12 T=10000K T=6000K radio i.r. u.v. X ray gamma rays-> 103 105 107 109 1011 1013 1015 frequency(MHz) 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)
The Crab in Multi-Wavelengths Photons Radio Infrared Optical X-ray
Galactic Co-ordinate System +90° +180° 180° 90°
Multi-Wavelength Photons Radio Infrared Visible light X-ray Gamma Ray ?
Production Mechanisms of Photons e- e e e+ magnetic field e e Hot plasma (surface of stars) Annihilation of matter/antimatter interstellar matter Bremsstrahlung / Synchrotron Radiation Inverse Compton Scattering + High energy showers p 0 interstellar matter
Non-Photonic Astronomy Antares (Toulon) Gravitational Waves Virgo (Pisa) Neutrinos Auger (Argentina) High Energy Cosmic Rays
Acceleration of High Energy Particles p accelerated in shock waves: non-relativistic supernova remnants relativistic quasars/microquasars p interact with interstellar matter and produce showers : p/A + p/g p0 + p + ... g gnmm nm nee Simulations indicate can get ~ 50% of energy of supernova explosion Cosmic Rays by ~1000 yrs
Types of Cosmic Ray Detectors KASCADE KASCADE p,N 0.3-100PeV p,N 0.3-100PeV Compton Gamma Ray Obs. 0.1-10GeV BATSE EGRET Satellites top of atmosphere Ground based telescopes looking at light produced in atmosphere ground level Whipple >1 TeV Array of particle detectors on ground Arrays of particle detectors
Charged Cosmic Ray Energy Spectrum Satellite, ballons AMS satellite Ground, Air Shower Arrays CCGO, GLAST CASA - KASCADE - AGASA - AUGER telescopes Whipple-CAT-HEGRA-CELESTE H.E.S.S.-MAGIC-VERITAS Space observed Shower telescopes EUSO AMANDA, ANTARES Why these features ? ‘knee’ ‘ankle’
Features of Cosmic Ray Spectrum R B E <1018 Z G kpc Ingredients of models: propagation source dN/dE E = 2.0 to 2.2,.. Source acceleration: E2.7 eV Source cut-off E2 dN/dE [cm-2 s-1 sr-1 eV] knee Diffusion models = 0.3 to 0.6 E3.2 E 7 1019 eV GZK cut-off on CMB ankle ‘Conventional Wisdom’: Galactic SNR E2.8 isotropic E < 3 1018 eV Mass composition ? Galactic losses E > 4 1014 eV Extragalactic E > 3 1018 eV exotic E > 7 1019 eV E [eV/nucleus]
Cosmic Rays Spectrum: Knee and Ankle Flux E3 Flux E2.7
Explanations of knee (E~3.1015 eV) Astronomy type explanations • Galactic de-confinement • Single dominant source • Single SNR acceleration multiple SNR acceleration • Absorption on massive neutrinos in galaxy • New interaction effects in atmosphere Particle Physics type explanations 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
Mass composition at knee Average shower depth and ratio N / Ne sensitive to primary mass (NB. Mass composition extracted is very sensitive to Monte Carlo simulation) Flux E2.5 Mean ln(A) KASCADE <ln A> KASCADE 3.5 2.5 1.5 CASA-BLANCA 0.5 1015 1016 1017 Energy eV KASCADE series of knees at different energies: p,He,..,C,..,Fe. E(Knee) Z knee due to source confinement cut-off ?
‘GZK cutoff ’ HE cosmic rays Interaction with background ( infrared and 2.7K CMBR) p N Sources uniform in universe 100 Mpc HE gamma rays 10 Mpc Mrk 501 120Mpc e+ e Mrk 421 120Mpc
Explanations of Ankle/ E > 1020 eV events Astronomy type explanations • ‘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 Particle Physics type explanations
Cosmic rays cannot be used to image the Universe... PeV proton M. Masetti
But we try anyway…. 308/242.5 in 20 E> 4 1019 eV 8 1017 <E<8 1018 eV galactic plane 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 anti GC Galactic source ? GC Sun SNR
AUGER experiment 2 sites each 3000km2, E > 5.1018eV Southern site, Mendoza Province, Argentina Water Cherenkov Tanks (1600 each 10m2) Fluorescence Telescopes (6 telescopes each 30 at 4 sites) 3.5m mirrors
AMS Experiment Detailed measurements on Cosmic Ray composition: anti-matter ? International Space Station 2004 Space Shuttle June 1998 limit on anti-helium/helium ratio < 106
Gamma Ray Astronomy XMM Integral GLAST Low Energy Gamma Astronomy from satellites High Energy Gamma Astronomy from ground STACEE CAT CELESTE CELESTE
Gamma-Ray Burst Story Gamma Ray Burst were first detected by the Vela satellites that were developed in the sixties to monitor nuclear test ban treaties. 1st GRB
Gamma Ray Bursts 1-2 per day observed by BATSE Isotropic sky distribution Burst duration Two types ? Some evidence for GRB on sites of previous supernova Redshifts measured for about 20 extragalactic distances
Imaging Gamma Ray Telescopes
Future projects in high-energy gamma-ray astronomy MAGIC VERITAS H.E.S.S. CANGAROO
Flares from Markarian 421 TeV X-Ray Correlation of flares at different wavelengths Timescale of flares indicate solar system dimensions of source
Black Hole at Galactic Centre Sgr A* Radio Black Hole horizon ? VLBI 6 mm VLA 2cm Black Hole mass Infrared 1” = 0,04 pc
Galactic Centre in Multi-Messengers Cosmic Rays E ~ 1018 eV Cosmic Rays AGASA “4.5” effect SUGAR “<0.5% fluctuation” Cosmic Ray Source 7 from Galactic Centre GeV Gamma rays Galactic centre (EGRET sources) RXJ 1713.7-3946 TeV Gamma rays
Neutrino Telescope Projects ANTARES La-Seyne-sur-Mer, France ( NEMO Catania, Italy ) BAIKAL: Lake Baikal, Siberia DUMAND, Hawaii (cancelled 1995) NESTOR : Pylos, Greece AMANDA, South Pole, Antarctica
Neutrinos weakly interacting in matter 109 Neutrino interaction length (km water equivalent) 106 Equivalent Earth diameter 103 106 1 103 E (TeV) Interaction length of neutrinos vs energy Low cross-section good : Astronomic sources and universe transparent to neutrinos Earth transparent up to 100 TeV bad : Need massive detector
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 Tank in a cavern eg SuperKamiokande 30 K tonnes Mega projects discuss 1 M tonne for few 100 Meuro Need to have > 1000 m depth to absorb light and cosmics rays
AMANDA AMANDA > 50GeV South Pole: glacial ice 1993 First strings AMANDA A 1998 AMANDA B10 ~ 300 Optical Modules 2000 ~ 700 Optical Modules ICECUBE 8000 Optical Modules
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
Future in telescopes: ANTARES 1996 Started 1996 - 2000 Site exploration and demonstrator line 2001 - 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
ANTARES 0.1km2 Detector Shore station Optical module 13 strings 12 m between storeys hydrophone Compass, tilt meter 2500m float ~60m Electro-optic submarine cable ~40km 300m active Electronics containers Readout cables ~100m Junction box anchor Acoustic beacon
ANTARES Deployment Sites Thetys Marseille La Seyne sur Mer Toulon Existing Cable Marseille-Corsica Demonstrator Line Nov 1999- Jun 2000 42°59 N, 5°17 E Depth 1200 m New Cable (2001) La Seyne-ANTARES ANTARES 0.1km2 Site 42°50 N, 6°10 E Depth 2400 m ~ 40 deployments and recoveries of test lines for site exploration 0.1 km2 detector with 900 Optical Modules, deployment 2002- 2004
References Books: Particle Astrophysics, H.V. Klapdor-Kleingrothaus and K. Zuber The Big Bang, J.Silk The Physics of Stars, A.C. Phillips Preprints: Introduction to Cosmology, David H. Lyth, astro-ph/9312022 Cosmological Parameters, Michael S. Turner, astro-ph/9904051 Non-Baryonic Dark Matter, Lars Bergstrom, hep-ph/0002126 Transparencies of School/Workshop: Neutrino Particle Astrophysics , http://leshouches.in2p3.fr Discussion Session, Council Chamber, 11:15 For more details contact me at: carr@cppm.in2p3.fr