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High Energy  -rays

High Energy  -rays. Roger Blandford KIPAC Stanford. The Electromagnetic Spectrum. ir. o. uv. x. g. mm. r. smm. 100TeV. m e c 2. m p c 2. 100neV. 1GeV. High Energy  -rays. Multi-Messenger Science. High Energy  -rays. Signals!. Electromagnetic. Cosmic Rays. Strong

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High Energy  -rays

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  1. High Energy -rays Roger Blandford KIPAC Stanford

  2. The Electromagnetic Spectrum ir o uv x g mm r smm 100TeV mec2 mpc2 100neV 1GeV CFAR High Energy -rays

  3. Multi-Messenger Science High Energy -rays Signals! Electromagnetic Cosmic Rays Strong Scientific Synergy Neutrinos Dark Matter Gravitational Radiation 10-32eV 1028eV Cosmology Hubble Planck CFAR

  4. Gamma Ray Astrophysics • GeV observations from space • Direct detection • SAS-2 -> CosB -> EGRET -> GLAST • TeV observations from ground • Atmospheric Cerenkov • Whipple -> HESS/MAGIC/VERITAS ->… • Water Cerenkov • Milagro ->… CFAR

  5. GLAST • Joint NASA-DOE-Italy- France-Japan-Sweden, Germany… mission • Launch May 16 2008 • Cape Canaveral • Success of GLAST is top priority • 50-100 x EGRET; high energy extension • Future program likely ground-based for a while CFAR

  6. LAT 0.02 - 300 GeV 2.5 sr, 0.3 - 0.9m2 5o - 5’resolution ln E ~ 0.1 3 x 10-9 cm-2 s-1 (>0.1 GeV, point source) 109 photons (3Hz) All sky every 3hr Sources after a decade? 10,000 Active Galactic Nuclei 1000 Gamma Ray Bursts 100 Pulsars 100 Supernova Remnants 10 Galaxies 10 Clusters of Galaxies 10 X-Ray Binaries ? Unidentified Sources GBM 0.01-30 MeV 9sr, 100 cm2. 1o resolution ln E ~ 0.1 Combine with Swift GLAST CFAR

  7. Exploring the Terascale MAGIC x 2 VERITAS (NSF+DOE+Smithsonian) H.E.S.S. (2) • ~10 ns flash • ~1o @ 10 km->104 m2 • Stereo imaging • ~ 0.1-100TeV • ~5o field of view • ~5’ PSF per photon • ~100 sources Milagro ~1-10 TeV CFAR

  8. Hadrons vs Leptons vs WIMPS(Pions vs Compton vs Annihilation) WIMPs? Leptons? Hadrons? X-ray vs TeV Fermi acceleration at shocks Magnetic field amplification Origin of cosmic rays? Many puzzles remain GLAST will interpolate Relativistic jets created by massive black hole in galactic nuclei Gamma ray emission at small radii Inverse Compton radiation 2 min variability? EM -> L -> H ? RFF? UHECR? If DM is cosmologically-generated, weakly interacting massive particle, there may be detectable annihilation from Galactic center and dwarf galaxies. Constraints will be combined with results from LHC and underground direct searches. Must understand diffuse background! CFAR

  9. Stochastic acceleration Unipolar induction u u / r u u / r  L B B Cosmic Accelerators UHECR?  Neutron stars Black holes V ~ TeV - ZeV I ~ 10 GA - 10 EA Shocks transmit power law distribution f(p) ~ p-3r/(r-1) Also second order processes V ~  I ~ V / Z0 P ~ V I CFAR

  10. SN energy in seconds Birth cry of stellar black hole? Special supernovae Binary NS merger?? LIGO! NS magnetosphere flare (1015G) Environmental impact Ultrarelativistic outflow “AGN on speed” opacity used to understanding sources Across the universe Cosmological probes Gamma Ray Bursts Expect Unscripted Discoveries CFAR

  11. ~0.04 - 200 TeV ~ 50 telescopes Large FOV ~1’ PSF per photon ~10 x VERITAS sensitivity ~ $100M class Exploring cheaper detectors ~1-100 TeV ~15 x Milagro Improved rejection Wide field Large duty cycle $10M class HAWC Tank Array in GEANT 4 DAQ trailer Road 150 m (30 tanks) Future TeV Options AGIS/CTA 10-100 x sources DM, LI studies Unexpected Technology and scientific trade studies underway-> decadal survey HESS/VERITAS Simulation AGIS/CTA Simulation CFAR

  12. EBL absorption Already interesting Hard sources Variable c??? Violation of LI Testable! Shower models probe physics @300TeV CM HAWC IACT GLAST Propagation Effects CFAR

  13. Auger N?? CFAR

  14. Summary • Golden age of Cosmic HE -rays • Support GLAST, VERITAS as they solve classic astrophysical problems and explore fundamental physics • Next phase will be just as exciting and is (relatively) inexpensive and quick • Invest in the future now CFAR

  15. Cultural Observations • Particle physicists, astrophysicists collaborating very well. • Organized more like HEP • Interagency collaboration “debugged” • Common detector technology • GLAST: Si tracking technology… • AGIS/CTA: photodetectors, fast electronics, triggers, computing… • Proven signals • cf DM, GW, VHEaxion… searches • Excellent, hands on training for students and postdocs • Fabrication and data analysis CFAR

  16. discover the nature of cosmic accelerators and monitor galaxy growth and development seek annihilation signature of supersymmetry particles in combination with LHC, underground check validity of Lorentz invariance over cosmic distances attract and train students who will be needed to work on future detectors and their data …understand how our universe works at its most fundamental level …discovering the most elementary constituents of matter and energy …exploring the basic nature of space and time itself …development of key technologies and trained manpower HAWC IACT GLAST Gamma-ray Physics DoE/HEP Mission High Energy -rays CFAR

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