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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. Electromagnetic. Cosmic Rays. Strong Scientific

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high energy rays

High Energy -rays

Roger Blandford

KIPAC

Stanford

slide2

The Electromagnetic Spectrum

ir

o

uv

x

g

mm

r

smm

100TeV

mec2

mpc2

100neV

1GeV

P5

High Energy -rays

slide3

Multi-Messenger Science

High Energy

-rays

Electromagnetic

Cosmic Rays

Strong

Scientific

Synergy

Neutrinos

Dark Matter

Gravitational Radiation

10-32eV

1028eV

Cosmology

Hubble

Planck

P5

gamma ray astrophysics
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 ->…

P5

glast
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

P5

glast1
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

P5

exploring the terascale
Exploring the Terascale

MAGIC x 2

VERITAS (NSF+DOE+Smithsonian)

H.E.S.S. (2)

~1-10 TeV

  • ~10 ns flash
  • ~1o @ 10 km->104 m2
  • Stereo imaging
  • ~ 0.1-100TeV
  • ~5o field of view
  • ~5’ PSF per photon
  • ~100 sources

Milagro

P5

hadrons vs leptons vs wimps pions vs compton vs annihilation
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 ?

UHECR?

If DM is cosmologically-generated,

weakly interacting 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!

P5

cosmic accelerators
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

P5

gamma ray bursts
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

P5

future tev options
~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

P5

cultural observations
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

P5

gamma ray physics
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

P5

summary
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

P5