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Gernot Maier
Teilchenteleskope in der Physik
Astronomie bei sehr hohen Energien - Gammastrahlungsastronomie
Gernot Maier | Teilchenteleskope in der Physik | October 2010 |
Inhalt
> Astronomie Einführung
Höchste Energien - Gammastrahlung
> Kosmische Teilchenbeschleuniger Explodierende Sterne (Supernovae)
Doppelsternsysteme
Supermassive schwarze Löcher
> Teleskope zur Messung hochenergetischer Gammastrahlung HESS, MAGIC, VERITAS
Fermi - LAT
CTA, AGIS
> Ausblick
Gernot Maier | Teilchenteleskope in der Physik | October 2010 |
Die Milchstrasse
500 Millionen Sterne
100 000 Lichtjahre = 900 000 000 000 000 000 km = 9x1017 km
Gernot Maier | Teilchenteleskope in der Physik | October 2010 |
Die Sonne
Gernot Maier | Teilchenteleskope in der Physik | October 2010 |
Die Sonne
Gernot Maier | Teilchenteleskope in der Physik | October 2010 |
Galaxien
Gernot Maier | Teilchenteleskope in der Physik | October 2010 |
Galaxien - Kollisionen
Gernot Maier | Teilchenteleskope in der Physik | October 2010 |
Nicht nur Sterne - Gas und Staub
Photons
1 m - 1 km 1 cm 1 μm - 1 mm 400-700 nm 10 - 400 nm 0.01 - 10 nm < 0.01 nm
Radio
MicrowavesInfrared
VisibleUltraviolet
X-raysGamma-rays
10,000 K 108 K 1010 K
eV keV MeV GeV TeV
1 K 100 K
Photons
1 m - 1 km 1 cm 1 μm - 1 mm 400-700 nm 10 - 400 nm 0.01 - 10 nm < 0.01 nm
Radio
MicrowavesInfrared
VisibleUltraviolet
X-raysGamma-rays
10,000 K 108 K 1010 K
eV keV MeV GeV TeV
1 K 100 K
Photons
1 m - 1 km 1 cm 1 μm - 1 mm 400-700 nm 10 - 400 nm 0.01 - 10 nm < 0.01 nm
Radio
MicrowavesInfrared
VisibleUltraviolet
X-raysGamma-rays
10,000 K 108 K 1010 K
eV keV MeV GeV TeV
1 K 100 K
Charged particles
e±,p
B→
synchrotron radiation
γ γγ’
e±inverse Compton scattering
e±’π0-decay from
hadronic interactions
π0 → γγ
Photons
1 m - 1 km 1 cm 1 μm - 1 mm 400-700 nm 10 - 400 nm 0.01 - 10 nm < 0.01 nm
Radio
MicrowavesInfrared
VisibleUltraviolet
X-raysGamma-rays
10,000 K 108 K 1010 K
eV keV MeV GeV TeV
1 K 100 K
Cosmic Rays (protons, ..., iron nuclei), electrons103 eV 1015 eV 1020 eV
Charged particles
e±,p
B→
synchrotron radiation
γ γγ’
e±inverse Compton scattering
e±’π0-decay from
hadronic interactions
π0 → γγ
Neutrinos
Gravitational waves
Photons
1 m - 1 km 1 cm 1 μm - 1 mm 400-700 nm 10 - 400 nm 0.01 - 10 nm < 0.01 nm
Radio
MicrowavesInfrared
VisibleUltraviolet
X-raysGamma-rays
10,000 K 108 K 1010 K
eV keV MeV GeV TeV
1 K 100 K
Cosmic Rays (protons, ..., iron nuclei), electrons103 eV 1015 eV 1020 eV
Charged particles
e±,p
B→
synchrotron radiation
γ γγ’
e±inverse Compton scattering
e±’π0-decay from
hadronic interactions
π0 → γγ
Gernot Maier | Teilchenteleskope in der Physik | October 2010 |
optical
Multi-wavelength Astronomy
Gernot Maier | Teilchenteleskope in der Physik | October 2010 |
optical
x-ray
Multi-wavelength Astronomy
Gernot Maier | Teilchenteleskope in der Physik | October 2010 |
infrared
optical
x-ray
Multi-wavelength Astronomy
Gernot Maier | Teilchenteleskope in der Physik | October 2010 |
Die Milchstrasse
Gernot Maier | Teilchenteleskope in der Physik | October 2010 |
Die Milchstrasse
The Milky Way
Optical 0.4-0.6 μm
NASA, mwmw.gsfc.nasa.gov
star light
The Milky Way
Optical 0.4-0.6 μm
NASA, mwmw.gsfc.nasa.gov
star light
thermal emission from interstellar dust
Infrared 12, 60, 100 μm
The Milky Way
Optical 0.4-0.6 μm
NASA, mwmw.gsfc.nasa.gov
very hot, shocked gas
X-ray 0.25, 0.75,1.5 keV
star light
thermal emission from interstellar dust
Infrared 12, 60, 100 μm
The Milky Way
Optical 0.4-0.6 μm
NASA, mwmw.gsfc.nasa.gov
very hot, shocked gas
X-ray 0.25, 0.75,1.5 keV
star light
Hydrogen 21 cm line, cold interstellar medium (gas)
Radio 21 cm
thermal emission from interstellar dust
Infrared 12, 60, 100 μm
The Milky Way
Optical 0.4-0.6 μm
NASA, mwmw.gsfc.nasa.gov
very hot, shocked gas
X-ray 0.25, 0.75,1.5 keV
star light
synchrotron emission from HE electrons moving through interstellar magnetic fields
Radio 480 MHz Hydrogen 21 cm line, cold interstellar medium (gas)
Radio 21 cm
thermal emission from interstellar dust
Infrared 12, 60, 100 μm
The Milky Way
Optical 0.4-0.6 μm
NASA, mwmw.gsfc.nasa.gov
π0 decay from interaction of Cosmic Rays with interstellar medium
γ-ray >300 MeV
very hot, shocked gas
X-ray 0.25, 0.75,1.5 keV
star light
synchrotron emission from HE electrons moving through interstellar magnetic fields
Radio 480 MHz Hydrogen 21 cm line, cold interstellar medium (gas)
Radio 21 cm
thermal emission from interstellar dust
Infrared 12, 60, 100 μm
The Milky Way
Optical 0.4-0.6 μm
NASA, mwmw.gsfc.nasa.gov
π0 decay from interaction of Cosmic Rays with interstellar medium
γ-ray >300 MeV
very hot, shocked gas
X-ray 0.25, 0.75,1.5 keV
emission from high-energy charged particles>300 GeVγ-ray
star light
synchrotron emission from HE electrons moving through interstellar magnetic fields
Radio 480 MHz Hydrogen 21 cm line, cold interstellar medium (gas)
Radio 21 cm
thermal emission from interstellar dust
Infrared 12, 60, 100 μm
The Milky Way
Optical 0.4-0.6 μm
NASA, mwmw.gsfc.nasa.gov
π0 decay from interaction of Cosmic Rays with interstellar medium
γ-ray >300 MeV
very hot, shocked gas
X-ray 0.25, 0.75,1.5 keV
emission from high-energy charged particles>300 GeVγ-ray
star light
synchrotron emission from HE electrons moving through interstellar magnetic fields
Radio 480 MHz Hydrogen 21 cm line, cold interstellar medium (gas)
Radio 21 cm
thermal emission from interstellar dust
Infrared 12, 60, 100 μm
InstrumentsArecibo (Radio) Spitzer (IR)Fermi (Gamma-rays)
VERITAS (Gamma-rays)VLT (Optical)
Suzaku (X-rays)
Auger (Cosmic Rays) LIGO (Gravitational waves)
IceCube(Neutrinos)
1 m - 1 km 1 cm 1 μm - 1 mm 400-700 nm 10 - 400 nm 0.01 - 10 nm < 0.01 nm
Radio Microwaves Infrared Visible Ultraviolet X-rays Gamma-rays
10,000 K 108 K 1010 K
eV keV MeV GeV
1 K 100 K
TeV
Gernot Maier | Physics with CTA | October, 2010 |
The non-thermal Universe
TeV
Fermi LAT all sky view > 100 MeV
Gernot Maier | Physics with CTA | October, 2010 |
The non-thermal Universe
TeV
sources > 100 GeV
Gernot Maier | Physics with CTA | October, 2010 |
The non-thermal Universe
TeV
sources > 100 GeV
Supe
rnova
Remn
ants
Pulsa
r Wind
Nebu
la
Binary
Syste
ms
Starbu
rst Ga
laxies
Activ
e Gala
ctic N
uclei
Gamm
a Ray
Burst
s
Dark
Matte
r
Gernot Maier | Physics with CTA | October, 2010 |
The non-thermal Universe
TeV
sources > 100 GeV
Supe
rnova
Remn
ants
Pulsa
r Wind
Nebu
la
Binary
Syste
ms
Starbu
rst Ga
laxies
Activ
e Gala
ctic N
uclei
Gamm
a Ray
Burst
s
Dark
Matte
r
500 Million stars known in the Milky Way 100 very high-energy gamma-ray sources known
Gernot Maier | Teilchenteleskope in der Physik | October 2010 |
Quellen von Gammastrahlung - Explodierende Sterne
Massive Sterne explodieren am Ende ihres ‘Lebens’
Wahrscheinlich die Quellen der kosmischen Strahlung
Tycho’s Supernova (1572)
Teilchenbeschleunigung
heißer Überrest (Millionen Grad Celsius)
• distant bright galaxies
• central core produces more radiation than rest of galaxy: Active Galactic Nucleus (AGN)
• supermassive black hole: 109 solar masses
• extremely powerful radio source: quasar
• ~10% of all AGNs produce beams of energetic particles and magnetic fields: jets
• powered by accretion of matter onto a supermassive black hole and/or black hole rotation
M87: HST opticalActive Galactic Nuclei
core and accretion disk
jet: relativistic, hot, magnetized plasma
thou
sand
s of l
ight
year
s
hot spots: shocked jet
plasma
blue light: synchrotron radiation from HE
electrons
• distant bright galaxies
• central core produces more radiation than rest of galaxy: Active Galactic Nucleus (AGN)
• supermassive black hole: 109 solar masses
• extremely powerful radio source: quasar
• ~10% of all AGNs produce beams of energetic particles and magnetic fields: jets
• powered by accretion of matter onto a supermassive black hole and/or black hole rotation
M87: HST opticalActive Galactic Nuclei
core and accretion disk
jet: relativistic, hot, magnetized plasma
thou
sand
s of l
ight
year
s
hot spots: shocked jet
plasma
blue light: synchrotron radiation from HE
electrons
M87: HST opticalActive Galactic Nuclei
Gernot Maier | Teilchenteleskope in der Physik | October 2010 |
Schwarze Löcher und Jets
HH30: 1995 - 2000
SS 433(2-10 keV)
Young Stars(Herbig-Haro Objects)
Microquasars(X-ray binaries)
Gamma Ray Bursts(hypernovae)
long GRBscollapse of massive, rapidly rotating stars
Gernot Maier | Teilchenteleskope in der Physik | October 2010 |
Quellen von Gammastrahlung - Doppelsternsysteme
Mikroquasar
Gernot Maier | Teilchenteleskope in der Physik | October 2010 |
Quellen von Gammastrahlung - Doppelsternsysteme
Mikroquasar
accretion disk
jet
core: black hole or neutron star
donor star
Charged Particle Acceleration - Shocks in the Universe
kitchen sink Kepler’s Supernova
Extragalactic background light:How many stars are in the sky?
γTeV+γstar → e+e-
Gernot Maier | Teilchenteleskope in der Physik | October 2010 |
Dark Matter
Atoms4%
Dark Matter26%
Dark Energy70%
Wir kennen nur 4% unseres Universums...
Gernot Maier | Teilchenteleskope in der Physik | October 2010 |
Dark Matter
Galactic center
Dwarf Galaxies
Milky Way Halo
Gernot Maier | Physics with CTA | October, 2010 |
The non-thermal Universe - the big questions
TeV
Supe
rnova
Remn
ants
Pulsa
r Wind
Nebu
la
Binary
Syste
ms
Starbu
rst Ga
laxies
Activ
e Gala
ctic N
uclei
Gamm
a Ray
Burst
s
Dark
Matte
r
Gernot Maier | Physics with CTA | October, 2010 |
The non-thermal Universe - the big questions
TeV
Supe
rnova
Remn
ants
Pulsa
r Wind
Nebu
la
Binary
Syste
ms
Starbu
rst Ga
laxies
Activ
e Gala
ctic N
uclei
Gamm
a Ray
Burst
s
Dark
Matte
r
Understanding the origin of cosmic rays and how they interact with their environment.
Gernot Maier | Physics with CTA | October, 2010 |
The non-thermal Universe - the big questions
TeV
Supe
rnova
Remn
ants
Pulsa
r Wind
Nebu
la
Binary
Syste
ms
Starbu
rst Ga
laxies
Activ
e Gala
ctic N
uclei
Gamm
a Ray
Burst
s
Dark
Matte
r
Understanding the nature and variety of black hole particle accelerators.
Understanding the origin of cosmic rays and how they interact with their environment.
Gernot Maier | Physics with CTA | October, 2010 |
The non-thermal Universe - the big questions
TeV
Supe
rnova
Remn
ants
Pulsa
r Wind
Nebu
la
Binary
Syste
ms
Starbu
rst Ga
laxies
Activ
e Gala
ctic N
uclei
Gamm
a Ray
Burst
s
Dark
Matte
r
What is the nature of dark-matter particles?
Understanding the nature and variety of black hole particle accelerators.
Understanding the origin of cosmic rays and how they interact with their environment.
VHE Cherenkov telescopes
VERITAS
MAGIC
H.E.S.S.
Cangoroo
Fermi LAT
Whipple
MAGIC
VERITAS
H.E.S.S.
Gernot Maier | Teilchenteleskope in der Physik | October 2010 |
October 1968
First detection:1989
Gernot Maier | Physics with CTA | October, 2010 |
A CTA telescope
Gernot Maier | Teilchenteleskope in der Physik | October 2010 |
Atmospheric Opacity
e+
e–
e–
e–
e+ e+
e
p
e–
v~
ca. 100-200m
Extensive Air Showers
prim
ary
part
icle
primaryparticle
show
er a
xis
lead
ing
hadr
on
e/ detector arrayhadroncalorimeter
fluorescence,cherenkov light
! detectors
~1 m thick
composition of part.at ground level(after 25 X0, 11 int)
! 80 % photons! 18 % electrons! 1.7 % muons! 0.3 % hadrons! 106 secondary part. from 1015 eV proton
~ 20km height
c
Gernot Maier | Teilchenteleskope in der Physik | October 2010 |
Cherenkov light
Pavel Alekseyevich Cherenkov(Nobel 1958)
emitted when velocity of charged particle exceeds local speed of light
Gernot Maier | Physics with CTA | October, 2010 |
Detection of high-energy γ-rays
γ-ray
particle shower
~10 km
‘flat’ light pool with radius of ~120 m:
detection areas of 105 to 106 m2
Cherenkov photon densities on ground level:
1-105 γ/m2
duration of Cherenkov flash: ~ns
Gernot Maier | Teilchenteleskope in der Physik | October 2010 |
Fluxes
> flux of strongest γ-ray source (Crab Nebula): ~10-7 γ’s/m2/s
>satellite with detection area of 1-5 m2: ~15 γ’s / year
> imaging atmospheric Cherenkov telescopes: detection area >105 m2: 50 γ’s/h
Power law E-2.4
Background
γ-ray proton
Cosmic Ray flux typically 103-104 larger than γ-ray flux
Background
γ-ray protonCherenkov photons on ground
γ-ray
proton
Cosmic Ray flux typically 103-104 larger than γ-ray flux
shower
maximum at8-10 km altitude
alti
tude
Cherenkov flash is a few nanoseconds long
shower
maximum at8-10 km altitude
alti
tude
mirror
Cherenkov flash is a few nanoseconds long
shower
maximum at8-10 km altitude
alti
tude
focal plane
mirror
Cherenkov flash is a few nanoseconds long
shower
maximum at8-10 km altitude
alti
tude
focal plane
mirror
Cherenkov flash is a few nanoseconds long
shower
maximum at8-10 km altitude
alti
tude
focal plane
mirror
Cherenkov flash is a few nanoseconds long
shower
maximum at8-10 km altitude
alti
tude
focal plane
mirror
Cherenkov flash is a few nanoseconds long
shower
maximum at8-10 km altitude
alti
tude
Image in the focalplane
focal plane
mirror
Cherenkov flash is a few nanoseconds long
(observation of the Crab Nebula)gamma-rays measured by VERITAS
(each frame 2 ns long)
Monte Carlo Simulation
gamma-rays ‘measured’ by VERITAS
(each frame 2 ns long)
Gernot Maier | Teilchenteleskope in der Physik | October 2010 |
VERITAS - Technical Details
Telescope (x 4)12 m diameter Davies-Cottonf 1.0, 110 m2 mirror area
Mirror Facets (x 350)Reflectivity ~88%(recoated every 2 y) Light concentrators
3.5°
Camera (x 4)499 PMTs3.5o Field of View
PMT (x 499)
FADC SAMPLES
Electronics500 MSPS FADCCFD trigger,3 adjacent pixel and 2/4 telescope coincidence~10% dead time; ~300 Hz
Pointing Monitor
Gernot Maier | Physics with CTA | October, 2010 |
The Cherenkov Telescope Array
CTA Consortium: >22 countries (big: D, F, US) >600 scientists€180 M (invest)first science data 2014
north and south array - full sky coverage
Gernot Maier | Physics with CTA | October, 2010 |
The Cherenkov Telescope ArrayCrab
10% Crab
1% Crab
FERMI LAT
MAGIC
H.E.S.S./VERITAS
CTA
CTA Consortium: >22 countries (big: D, F, US) >600 scientists€180 M (invest)first science data 2014
north and south array - full sky coverage