pfrommer: non-thermal emission from galaxy clusters
TRANSCRIPT
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8/14/2019 Pfrommer: Non-thermal emission from galaxy clusters
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Cosmological structure formation shocks
Diffuse radio emission in clusters
High-energy -ray emission
Deciphering an enigma Non-thermalemission from galaxy clusters
Christoph Pfrommer1
in collaboration with
Torsten Enlin2, Volker Springel2, Anders Pinzke3,Nick Battaglia1, Jon Sievers1, Dick Bond1
1Canadian Institute for Theoretical Astrophysics, Canada2Max-Planck Institute for Astrophysics, Germany
3Stockholm University, Sweden
Nov 21, 2008 / Princeton University Cosmology Lunch
Christoph Pfrommer Non-thermal emission from galaxy clusters
http://find/http://goback/ -
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Cosmological structure formation shocks
Diffuse radio emission in clusters
High-energy -ray emission
Outline
1 Cosmological structure formation shocks
Cosmological galaxy cluster simulations
Mach numbers and shock acceleration
Cosmic ray transport and pressure distribution
2 Diffuse radio emission in clustersGeneral picture of non-thermal processes in clusters
Shock related emission
Hadronically induced emission
3 High-energy -ray emissionMorphology and spectra
Predictions for Fermi
Minimum -ray flux
Christoph Pfrommer Non-thermal emission from galaxy clusters
http://find/http://goback/ -
8/14/2019 Pfrommer: Non-thermal emission from galaxy clusters
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Cosmological structure formation shocks
Diffuse radio emission in clusters
High-energy -ray emission
Cosmological galaxy cluster simulations
Mach numbers and shock acceleration
Cosmic ray transport and pressure distribution
Outline
1 Cosmological structure formation shocks
Cosmological galaxy cluster simulations
Mach numbers and shock acceleration
Cosmic ray transport and pressure distribution
2 Diffuse radio emission in clustersGeneral picture of non-thermal processes in clusters
Shock related emission
Hadronically induced emission
3 High-energy -ray emissionMorphology and spectra
Predictions for Fermi
Minimum -ray flux
Christoph Pfrommer Non-thermal emission from galaxy clusters
http://find/http://goback/ -
8/14/2019 Pfrommer: Non-thermal emission from galaxy clusters
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Cosmological structure formation shocks
Diffuse radio emission in clusters
High-energy -ray emission
Cosmological galaxy cluster simulations
Mach numbers and shock acceleration
Cosmic ray transport and pressure distribution
Shocks in galaxy clusters
1E 0657-56 (Bullet cluster)
(X-ray: NASA/CXC/CfA/M.Markevitch et al.; Optical:
NASA/STScI; Magellan/U.Arizona/D.Clowe et al.; Lensing:
NASA/STScI; ESO WFI; Magellan/U.Arizona/D.Clowe et al.)
Abell 3667
(radio: Johnston-Hollitt. X-ray: ROSAT/PSPC.)
Christoph Pfrommer Non-thermal emission from galaxy clusters
http://find/http://goback/ -
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Cosmological structure formation shocks
Diffuse radio emission in clusters
High-energy -ray emission
Cosmological galaxy cluster simulations
Mach numbers and shock acceleration
Cosmic ray transport and pressure distribution
Topics of interest
consistent picture of non-thermal processes in galaxyclusters (radio, soft/hard X-ray, -ray emission) illuminating the process of structure formation
history of individual clusters: cluster archeology
understanding the non-thermal pressure distribution toaddress biases of thermal cluster observables
nature of dark matter: annihilation signal vs. cosmic ray
(CR) induced -rays
gold sample of clusters for precision cosmology: using
non-thermal observables to gauge hidden parameters
fundamental plasma physics:
diffusive shock acceleration in high-plasmasorigin and evolution of large scale magnetic fieldsnature of turbulent models
Christoph Pfrommer Non-thermal emission from galaxy clusters
C l i l f i h k C l i l l l i l i
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Cosmological structure formation shocks
Diffuse radio emission in clusters
High-energy -ray emission
Cosmological galaxy cluster simulations
Mach numbers and shock acceleration
Cosmic ray transport and pressure distribution
Radiative simulations flowchart
Christoph Pfrommer Non-thermal emission from galaxy clusters
C l i l t t f ti h k C l i l l l t i l ti
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Cosmological structure formation shocks
Diffuse radio emission in clusters
High-energy -ray emission
Cosmological galaxy cluster simulations
Mach numbers and shock acceleration
Cosmic ray transport and pressure distribution
Radiative simulations with cosmic ray (CR) physics
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocks Cosmological galaxy cluster simulations
http://find/http://goback/ -
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Cosmological structure formation shocks
Diffuse radio emission in clusters
High-energy -ray emission
Cosmological galaxy cluster simulations
Mach numbers and shock acceleration
Cosmic ray transport and pressure distribution
Radiative simulations with extended CR physics
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocks Cosmological galaxy cluster simulations
http://find/http://goback/ -
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Cosmological structure formation shocks
Diffuse radio emission in clusters
High-energy -ray emission
Cosmological galaxy cluster simulations
Mach numbers and shock acceleration
Cosmic ray transport and pressure distribution
Previous numerical work on cosmic rays in clusters
COSMOCR: A numerical code for cosmic ray studies in computational
cosmology (Miniati, 2001):
advantages: good resolution in momentum space
drawbacks: CR pressure not accounted for in EoM, insufficient spatial
resolution (grid code), non-radiative gas physics
Figure: Hard X-rays, thermal X-rays, -rays, adopted from Miniati (2003)
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocks Cosmological galaxy cluster simulations
http://find/http://goback/ -
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Cosmological structure formation shocks
Diffuse radio emission in clusters
High-energy -ray emission
Cosmological galaxy cluster simulations
Mach numbers and shock acceleration
Cosmic ray transport and pressure distribution
Our philosophy and description
An accurate description of CRs should follow the evolution ofthe spectral energy distribution of CRs as a function of time and
space, and keep track of their dynamical, non-linear coupling
with the hydrodynamics.
We seek a compromise between
capturing as many physical properties as possible
requiring as little computational resources as necessary
Assumptions:protons dominate the CR population
a momentum power-law is a typical spectrum
CR energy & particle number conservation
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocks Cosmological galaxy cluster simulations
http://find/http://goback/ -
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Cosmological structure formation shocks
Diffuse radio emission in clusters
High-energy -ray emission
Cosmological galaxy cluster simulations
Mach numbers and shock acceleration
Cosmic ray transport and pressure distribution
Our philosophy and description
An accurate description of CRs should follow the evolution ofthe spectral energy distribution of CRs as a function of time and
space, and keep track of their dynamical, non-linear coupling
with the hydrodynamics.
We seek a compromise between
capturing as many physical properties as possible
requiring as little computational resources as necessary
Assumptions:protons dominate the CR population
a momentum power-law is a typical spectrum
CR energy & particle number conservation
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocks Cosmological galaxy cluster simulations
http://find/http://goback/ -
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Cosmological structure formation shocks
Diffuse radio emission in clusters
High-energy -ray emission
Cosmological galaxy cluster simulations
Mach numbers and shock acceleration
Cosmic ray transport and pressure distribution
Our philosophy and description
An accurate description of CRs should follow the evolution ofthe spectral energy distribution of CRs as a function of time and
space, and keep track of their dynamical, non-linear coupling
with the hydrodynamics.
We seek a compromise between
capturing as many physical properties as possible
requiring as little computational resources as necessary
Assumptions:protons dominate the CR population
a momentum power-law is a typical spectrum
CR energy & particle number conservation
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocks Cosmological galaxy cluster simulations
http://find/http://goback/ -
8/14/2019 Pfrommer: Non-thermal emission from galaxy clusters
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g
Diffuse radio emission in clusters
High-energy -ray emission
g g y
Mach numbers and shock acceleration
Cosmic ray transport and pressure distribution
CR spectral description
p = Pp/mp c
f(p) =dN
dp dV = C p
(p
q)
q() =
0
13
q0
C() = 0+2
3C0
nCR =
0
dp f(p) = C q1
1
PCR =mpc
2
3
0 dp f(p)(p) p
=C mpc
2
6 B 11+q2
2
2 ,3
2
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocks Cosmological galaxy cluster simulations
http://find/http://goback/ -
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g
Diffuse radio emission in clusters
High-energy -ray emission
g g y
Mach numbers and shock acceleration
Cosmic ray transport and pressure distribution
Thermal & CR energy spectra
Kinetic energy per logarithmic momentum interval:
10-4
10-3
10-2
10-1
100
101
102
103
0.01
0.10
1.00
0.1MeV
p
dTCR
/dlog
p=
pTp
(p)
f(p)
in
mp
c2
= 2.25
= 2.50
= 2.75
10 eV 1 keV
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocks Cosmological galaxy cluster simulations
http://find/http://goback/ -
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Diffuse radio emission in clusters
High-energy -ray emission
Mach numbers and shock acceleration
Cosmic ray transport and pressure distribution
Cooling time scales of CR protons
Cooling of primordial gas:
104
105
106
107
108
109
T [ K ]
0.0001
0.0010
0.0100
0.1000
1.0000
10.0000
cool
[Gyr]
n = 0.01 cm-3
Cooling of cosmic rays:
0.01 0.10 1.00 10.00 100.00
q
0.01
0.10
1.00
10.00
cool
[Gyr]
n = 0.01 cm-3
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocks Cosmological galaxy cluster simulations
http://find/http://goback/ -
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Diffuse radio emission in clusters
High-energy -ray emission
Mach numbers and shock acceleration
Cosmic ray transport and pressure distribution
CR protons in clusters
relativistic proton populations can often be expected, since
acceleration mechanisms work for protons . . .
. . . as efficient as for electrons (adiabatic compression) or
. . . more efficient than for electrons (DSA, stochastic acc.)galactic CR protons are observed to have 100 times higherenergy density than electrons
CR protons are very inert against radiative losses and thereforelong-lived ( Hubble time in galaxy clusters, longer outside)
an energetic CR proton population should exist in clusters
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocks
Diff di i i i l
Cosmological galaxy cluster simulations
M h b d h k l i
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Diffuse radio emission in clusters
High-energy -ray emission
Mach numbers and shock acceleration
Cosmic ray transport and pressure distribution
Radiative cool core cluster simulation: gas density
10-1
100
101
102
-15 -10 -5 0 5 1 0 15-15
-10
-5
0
5
10
15
-15 -10 -5 0 5 10 15
x [ h-1 Mpc ]
-15
-10
-5
0
5
10
15
y
[h-1Mpc]
-15 -10 -5 0 5 1 0 15-15
-10
-5
0
5
10
15
1+
gas
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocks
Diff di i i i l t
Cosmological galaxy cluster simulations
M h b d h k l ti
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Diffuse radio emission in clusters
High-energy -ray emission
Mach numbers and shock acceleration
Cosmic ray transport and pressure distribution
Mass weighted temperature
105
106
107
108
-15 -10 -5 0 5 1 0 15-15
-10
-5
0
5
10
15
-15 -10 -5 0 5 10 15
x [ h-1 Mpc ]
-15
-10
-5
0
5
10
15
y[h-1Mpc]
-15 -10 -5 0 5 1 0 15-15
-10
-5
0
5
10
15
T
gas
/gas
[K]
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocks
Diffuse radio emission in clusters
Cosmological galaxy cluster simulations
Mach numbers and shock acceleration
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Diffuse radio emission in clusters
High-energy -ray emission
Mach numbers and shock acceleration
Cosmic ray transport and pressure distribution
Mach number distribution weighted by diss
1
10
-15 -10 -5 0 5 1 0 15-15
-10
-5
0
5
10
15
-15 -10 -5 0 5 10 15
x [ h-1 Mpc ]
-15
-10
-5
0
5
10
15
y
[h-1Mpc]
-15 -10 -5 0 5 1 0 15-15
-10
-5
0
5
10
15
M
diss/
dis
s
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocks
Diffuse radio emission in clusters
Cosmological galaxy cluster simulations
Mach numbers and shock acceleration
http://find/http://goback/ -
8/14/2019 Pfrommer: Non-thermal emission from galaxy clusters
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Diffuse radio emission in clusters
High-energy -ray emission
Mach numbers and shock acceleration
Cosmic ray transport and pressure distribution
Diffusive shock acceleration Fermi 1 mechanism (1)
conditions:
a collisionless shock wave
magnetic fields to confine energetic particles
plasma waves to scatter energetic particles particle diffusion
supra-thermal particles
mechanism:
supra-thermal particles diffuse upstream across shock wave
each shock crossing energizes particles through momentum transfer
from recoil-free scattering off macroscopic scattering agents
momentum increases exponentially with number of shock crossings
particle number decreases exponentially with number of crossings
power-law CR distribution
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocksDiffuse radio emission in clusters
Cosmological galaxy cluster simulationsMach numbers and shock acceleration
http://find/http://goback/ -
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Diffuse radio emission in clusters
High-energy -ray emission
Mach numbers and shock acceleration
Cosmic ray transport and pressure distribution
Diffusive shock acceleration Fermi 1 mechanism (1)
conditions:
a collisionless shock wave
magnetic fields to confine energetic particles
plasma waves to scatter energetic particles particle diffusion
supra-thermal particles
mechanism:
supra-thermal particles diffuse upstream across shock wave
each shock crossing energizes particles through momentum transfer
from recoil-free scattering off macroscopic scattering agents
momentum increases exponentially with number of shock crossings
particle number decreases exponentially with number of crossings
power-law CR distribution
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocksDiffuse radio emission in clusters
Cosmological galaxy cluster simulationsMach numbers and shock acceleration
http://find/http://goback/ -
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Diffuse radio emission in clusters
High-energy -ray emission
Mach numbers and shock acceleration
Cosmic ray transport and pressure distribution
Diffusive shock acceleration Fermi 1 mechanism (2)
Spectral index depends on the Mach number of the shock,M = shock/cs:
log p
strong shock
10 GeV
weak shock
keV
log f
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocksDiffuse radio emission in clusters
Cosmological galaxy cluster simulationsMach numbers and shock acceleration
http://find/http://goback/ -
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Diffuse radio emission in clusters
High-energy -ray emission
Mach numbers and shock acceleration
Cosmic ray transport and pressure distribution
Diffusive shock acceleration efficiency (3)
CR proton energy injection efficiency, inj
= CR
/diss
:
2.0 2.5 3.0 3.5 4.0
0.001
0.010
0.100
1.000
CR
energ
yinjectionefficien
cyinj
inj
Mach number M
kT2 = 10 keVkT2 = 0.3 keVkT2 = 0.01 keV
3 5 11/3 3
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocksDiffuse radio emission in clusters
Cosmological galaxy cluster simulationsMach numbers and shock acceleration
http://find/http://goback/ -
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High-energy -ray emission Cosmic ray transport and pressure distribution
Mach number distribution weighted by diss
1
10
-15 -10 -5 0 5 1 0 15-15
-10
-5
0
5
10
15
-15 -10 -5 0 5 10 15
x [ h-1 Mpc ]
-15
-10
-5
0
5
10
15
y
[h-1Mpc]
-15 -10 -5 0 5 1 0 15-15
-10
-5
0
5
10
15
M
diss/
diss
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocksDiffuse radio emission in clusters
Cosmological galaxy cluster simulationsMach numbers and shock acceleration
http://find/http://goback/ -
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High-energy -ray emission Cosmic ray transport and pressure distribution
Mach number distribution weighted by CR,inj
1
10
-15 -10 -5 0 5 1 0 15-15
-10
-5
0
5
10
15
-15 -10 -5 0 5 10 15
x [ h-1 Mpc ]
-15
-10
-5
0
5
10
15
y
[h-1Mpc]
-15 -10 -5 0 5 1 0 15-15
-10
-5
0
5
10
15
M
CR,
inj
/CR,
inj
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocksDiffuse radio emission in clusters
Cosmological galaxy cluster simulationsMach numbers and shock acceleration
http://find/http://goback/ -
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High-energy -ray emission Cosmic ray transport and pressure distribution
Mach number distribution weighted by CR,inj(q> 30)
1
10
-15 -10 -5 0 5 1 0 15-15
-10
-5
0
5
10
15
-15 -10 -5 0 5 10 15
x [ h-1 Mpc ]
-15
-10
-5
0
5
10
15
y
[h-1Mpc]
-15 -10 -5 0 5 1 0 15-15
-10
-5
0
5
10
15
M
CR,inj/CR,inj
(q>
30)
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocksDiffuse radio emission in clusters
Cosmological galaxy cluster simulationsMach numbers and shock acceleration
http://find/http://goback/ -
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High-energy -ray emission Cosmic ray transport and pressure distribution
CR pressure PCR
10-17
10-16
10-15
10-14
10-13
10-12
-15 -10 -5 0 5 1 0 15-15
-10
-5
0
5
10
15
-15 -10 -5 0 5 10 15
x [ h-1 Mpc ]
-15
-10
-5
0
5
10
15
y[h-1Mpc]
-15 -10 -5 0 5 1 0 15-15
-10
-5
0
5
10
15
PCRgas
/gas
[erg
cm3h2
]
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocksDiffuse radio emission in clusters
Hi h i i
Cosmological galaxy cluster simulationsMach numbers and shock acceleration
C i d di ib i
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High-energy -ray emission Cosmic ray transport and pressure distribution
Relative CR pressure PCR/Ptotal
10-2
10-1
100
-15 -10 -5 0 5 1 0 15-15
-10
-5
0
5
10
15
-15 -10 -5 0 5 10 15
x [ h-1 Mpc ]
-15
-10
-5
0
5
10
15
y[h-1Mpc]
-15 -10 -5 0 5 1 0 15-15
-10
-5
0
5
10
15
PCR
/Ptotgas
/
gas
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocksDiffuse radio emission in clusters
Hi h i i
Cosmological galaxy cluster simulationsMach numbers and shock acceleration
C i t t d di t ib ti
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High-energy -ray emission Cosmic ray transport and pressure distribution
Relative CR pressure PCR/Ptotal
10-2
10-1
100
-4 -2 0 2 4-4
-2
0
2
4
-4 -2 0 2 4
x [ h-1 Mpc ]
-4
-2
0
2
4
y[h-1Mpc]
-4 -2 0 2 4-4
-2
0
2
4
PCR
/Ptotgas
/
gas
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocksDiffuse radio emission in clusters
High energy ray emission
Cosmological galaxy cluster simulationsMach numbers and shock acceleration
Cosmic ray transport and pressure distribution
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High-energy -ray emission Cosmic ray transport and pressure distribution
CR phase-space diagram: final distribution @ z= 0
0
0
0
0
1
10-4
10
-3
10-2
10-1
100
phasespacedensity[arbitraryunits]
-2 0 2 4 6 8-4
-3
-2
-1
0
1
2
-2 0 2 4 6 8log[ 1 +
gas]
-4
-3
-2
-1
0
1
2
log[PCR/
Pth
]
-2 0 2 4 6 8-4
-3
-2
-1
0
1
2 -2 0 2 4 6 8
-4
-3
-2
-1
0
1
2
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocksDiffuse radio emission in clusters
High energy ray emission
Cosmological galaxy cluster simulationsMach numbers and shock acceleration
Cosmic ray transport and pressure distribution
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High-energy -ray emission Cosmic ray transport and pressure distribution
CR impact on SZ effect: Compton y parameter
10-6
10-5
C
omptony
-2 -1 0 1 2-2
-1
0
1
2
-2 -1 0 1 2x [ h-1Mpc ]
-2
-1
0
1
2
y
[h-1Mpc]
-2 -1 0 1 2-2
-1
0
1
2
large merging cluster, Mvir 1015M/h
10-7
10-6
Comptony
-1.0 -0.5 0.0 0.5 1.0-1.0
-0.5
0.0
0.5
1.0
-1.0 -0.5 0.0 0.5 1.0x [ h
-1Mpc ]
-1.0
-0.5
0.0
0.5
1.0
y[
h-1Mpc]
-1.0 -0.5 0.0 0.5 1.0-1.0
-0.5
0.0
0.5
1.0
small cool core cluster, Mvir 1014M/h
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocksDiffuse radio emission in clusters
High-energy -ray emission
Cosmological galaxy cluster simulationsMach numbers and shock acceleration
Cosmic ray transport and pressure distribution
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High-energy -ray emission Cosmic ray transport and pressure distribution
Compton y difference map: yCR yth
-10-4
-10-5
-10-6
-10-7
0
10-7
10-6
10-5
10-4
Compton-ydi
fferencemap:yCR-yth
Y / Y= - 1.6%
-1 0 1
-1
0
1
-1 0 1x [ h-1Mpc ]
-1
0
1
y
[h-1Mpc]
-1 0 1
-1
0
1
large merging cluster, Mvir 1015M/h
-10-5
-10-6
-10-7
-10-8
0
10-8
10-7
10-6
10-5
Compton-ydifferencemap:yCR-yth
Y / Y= - 0.8%
-0.5 0.0 0.5
-0.5
0.0
0.5
-0.5 0.0 0.5x [ h
-1Mpc ]
-0.5
0.0
0.5
y[
h-1Mpc]
-0.5 0.0 0.5
-0.5
0.0
0.5
small cool core cluster, Mvir 1014M/h
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocksDiffuse radio emission in clusters
High-energy -ray emission
Non-thermal processes in clustersShock related emission
Hadronically induced emission
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High energy ray emission Hadronically induced emission
Outline
1 Cosmological structure formation shocksCosmological galaxy cluster simulations
Mach numbers and shock acceleration
Cosmic ray transport and pressure distribution
2 Diffuse radio emission in clustersGeneral picture of non-thermal processes in clusters
Shock related emission
Hadronically induced emission
3 High-energy -ray emissionMorphology and spectraPredictions for Fermi
Minimum -ray flux
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocksDiffuse radio emission in clusters
High-energy -ray emission
Non-thermal processes in clustersShock related emission
Hadronically induced emission
http://find/http://goback/ -
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High energy ray emission Hadronically induced emission
Multi messenger approach for non-thermal processes
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocksDiffuse radio emission in clusters
High-energy -ray emission
Non-thermal processes in clustersShock related emission
Hadronically induced emission
http://find/http://goback/ -
8/14/2019 Pfrommer: Non-thermal emission from galaxy clusters
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g gy y y
Multi messenger approach for non-thermal processes
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocksDiffuse radio emission in clusters
High-energy -ray emission
Non-thermal processes in clustersShock related emission
Hadronically induced emission
http://find/http://goback/ -
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36/72
g gy y y
Multi messenger approach for non-thermal processes
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocksDiffuse radio emission in clusters
High-energy -ray emission
Non-thermal processes in clustersShock related emission
Hadronically induced emission
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37/72
Multi messenger approach for non-thermal processes
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocksDiffuse radio emission in clusters
High-energy -ray emission
Non-thermal processes in clustersShock related emission
Hadronically induced emission
http://find/http://goback/ -
8/14/2019 Pfrommer: Non-thermal emission from galaxy clusters
38/72
Cosmic web: Mach number
1
10
-15 -10 -5 0 5 1 0 15-15
-10
-5
0
5
10
15
-15 -10 -5 0 5 10 15
x [ h-1 Mpc ]
-15
-10
-5
0
5
10
15
y
[h-1Mpc]
-15 -10 -5 0 5 1 0 15-15
-10
-5
0
5
10
15
M
diss/
diss
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocksDiffuse radio emission in clusters
High-energy -ray emission
Non-thermal processes in clustersShock related emission
Hadronically induced emission
http://find/http://goback/ -
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39/72
Radio gischt (relics): primary CRe (1.4 GHz)
10-8
10-6
10-4
10-2
100
S,primary
[mJyarcm
in-2h70
2]
-15 -10 -5 0 5 10 15-15
-10
-5
0
5
10
15
-15 -10 -5 0 5 10 15
x [ h-1Mpc ]
-15
-10
-5
0
5
10
15
y
[h-1Mpc]
-15 -10 -5 0 5 10 15-15
-10
-5
0
5
10
15
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocksDiffuse radio emission in clusters
High-energy -ray emission
Non-thermal processes in clustersShock related emission
Hadronically induced emission
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40/72
Radio gischt: primary CRe (150 MHz)
10-8
10-6
10-4
10-2
100
S,primary
[mJyarcm
in-2h70
2]
-15 -10 -5 0 5 10 15-15
-10
-5
0
5
10
15
-15 -10 -5 0 5 10 15
x [ h-1Mpc ]
-15
-10
-5
0
5
10
15
y
[h-1Mpc]
-15 -10 -5 0 5 10 15-15
-10
-5
0
5
10
15
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocksDiffuse radio emission in clusters
High-energy -ray emission
Non-thermal processes in clustersShock related emission
Hadronically induced emission
http://find/http://goback/ -
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41/72
Radio gischt: primary CRe (15 MHz)
10-8
10-6
10-4
10-2
100
S,primary
[mJyarcm
in-2h70
2]
-15 -10 -5 0 5 10 15-15
-10
-5
0
5
10
15
-15 -10 -5 0 5 10 15
x [ h-1Mpc ]
-15
-10
-5
0
5
10
15
y
[h-1Mpc]
-15 -10 -5 0 5 10 15-15
-10
-5
0
5
10
15
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocksDiffuse radio emission in clusters
High-energy -ray emission
Non-thermal processes in clustersShock related emission
Hadronically induced emission
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42/72
Radio gischt: primary CRe (15 MHz), slower magnetic decline
10-8
10-6
10-4
10-2
100
S,primary
[mJyarcm
in-2h70
2]
-15 -10 -5 0 5 10 15-15
-10
-5
0
5
10
15
-15 -10 -5 0 5 10 15
x [ h-1Mpc ]
-15
-10
-5
0
5
10
15
y
[h-1Mpc]
-15 -10 -5 0 5 10 15-15
-10
-5
0
5
10
15
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocksDiffuse radio emission in clusters
High-energy -ray emission
Non-thermal processes in clustersShock related emission
Hadronically induced emission
http://find/http://goback/ -
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43/72
Radio gischt illuminates cosmic magnetic fields
1
3
2
-2 -1 0 1 2-2
-1
0
1
2
-2 -1 0 1 2
x [ h-1 Mpc ]
-2
-1
0
1
2
y[
h-1Mpc]
-2 -1 0 1 2-2
-1
0
1
2
Mdiss
/diss
Structure formation shocks triggered
by a recent merger of a large galaxy
cluster.
-2 -1 0 1 2-2
-1
0
1
2
-2 -1 0 1 2
x [ h-1Mpc ]
-2
-1
0
1
2
y[
h-1Mpc]
-2 -1 0 1 2-2
-1
0
1
2-2 -1 0 1 2
-2
-1
0
1
2
red/yellow: shock-dissipated energy,
blue/contours: 150 MHz radio gischt
emission from shock-accelerated CRe
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocksDiffuse radio emission in clusters
High-energy -ray emission
Non-thermal processes in clustersShock related emission
Hadronically induced emission
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Diffuse cluster radio emission an inverse problemExploring the magnetized cosmic web
Battaglia, Pfrommer, Sievers, Bond, Enlin (2008):
By suitably combining the observables associated with diffusepolarized radio emission at low frequencies ( 150 MHz,GMRT/LOFAR/MWA/LWA), we can probe
the strength and coherence scale of magnetic fields on scales ofgalaxy clusters,
the process of diffusive shock acceleration of electrons,
the existence and properties of the WHIM,
the exploration of observables beyond the thermal clusteremission which are sensitive to the dynamical state of thecluster.
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocksDiffuse radio emission in clusters
High-energy -ray emission
Non-thermal processes in clustersShock related emission
Hadronically induced emission
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45/72
Population of faint radio relics in merging clustersProbing the large scale magnetic fields
Finding radio relics in 3D cluster simulations using a friends-of-friends finderwith an emission threshold relic luminosity function
10-3
10-2
10-1
1
101
S[
mJyarcmin-2]
-2 -1 0 1 2-2
-1
0
1
2
-2 -1 0 1 2
x [ h-1Mpc ]
-2
-1
0
1
2
y
[h-1Mpc]
-2 -1 0 1 2-2
-1
0
1
2
radio map with GMRT emissivity threshold
10-3
10-2
10-1
1
101
S[
mJyarcmin-2]
-2 -1 0 1 2-2
-1
0
1
2
-2 -1 0 1 2
x [ h-1Mpc ]
-2
-1
0
1
2
y
[h-1Mpc]
-2 -1 0 1 2-2
-1
0
1
2
theoretical threshold (towards SKA)
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocksDiffuse radio emission in clusters
High-energy -ray emission
Non-thermal processes in clustersShock related emission
Hadronically induced emission
R li l i i f i h
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Relic luminosity function theory
Relic luminosity function is very sensitive to large scale behavior of the
magnetic field and dynamical state of cluster:
1
10
Numberofrelics
25 26 27 28 29 30 31 32
10-2 10-1 100 101 102 103 104F [mJy] for a cluster @ z ~ 0.05
B = 0.3
= 150MHz, B0 = 5 G
B = 0.5B = 0.7
B = 0.9
log(J/J0), J0 = 1 erg/Hz/s/ster
varying magnetic decline with radius
1
10
Numberofrelics
25 26 27 28 29 30 31 32
10-2 10-1 100 101 102 103 104F [mJy] for a cluster @ z ~ 0.05
B0 = 10 G
= 150MHz, B = 0.5
B0 = 5 GB0 = 2.5 G
log(J/J0), J0 = 1 erg/Hz/s/ster
varying overall normalization of the mag-
netic field
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocksDiffuse radio emission in clusters
High-energy -ray emission
Non-thermal processes in clustersShock related emission
Hadronically induced emission
R t ti (RM)
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Rotation measure (RM)
RM maps and power spectra have the potential to infer the magnetic
pressure support and discriminate the nature of MHD turbulence in clusters:
-150
-75
0
75
150
RM[radm-2]
-0.4 -0.2 0.0 0.2 0.4x [ Mpc]
-0.4
-0.2
0.0
0.2
0.4
y[Mpc]
-5 0 5arcmin
-5
0
5
arcmin
1
10
P
[RM](k)k2[
rad2m
-4]
10-7
10-6
P
[Bz]
(k)k2[
G2M
pc]
P[RM] (k)P[Bz]
(k)
1 10 100k[h Mpc-1]
1
10
P
[RM](k)k2[
rad2m
-4]
MFR1
MFR2
MFR3
Left: RM map of the largest relic, right: Magnetic and RM power spectrum comparing
Kolmogorow and Burgers turbulence models.
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocksDiffuse radio emission in clusters
High-energy -ray emission
Non-thermal processes in clustersShock related emission
Hadronically induced emission
H d i i t i t ti
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Hadronic cosmic ray proton interaction
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocksDiffuse radio emission in clusters
High-energy -ray emission
Non-thermal processes in clustersShock related emission
Hadronically induced emission
Cl t di i i b h d i ll d d CR
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Cluster radio emission by hadronically produced CRe
10-8
10-6
10-4
10-2
100
S,secondary
[mJyarc
min-2h70
3]
-15 -10 -5 0 5 10 15-15
-10
-5
0
5
10
15
-15 -10 -5 0 5 10 15
x [ h-1Mpc ]
-15
-10
-5
0
5
10
15
y
[h-1Mp
c]
-15 -10 -5 0 5 10 15-15
-10
-5
0
5
10
15
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocksDiffuse radio emission in clusters
High-energy -ray emission
Non-thermal processes in clustersShock related emission
Hadronically induced emission
Thermal X ray emission
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Thermal X-ray emission
10-9
10-8
10-7
10-6
10-5
10-4
SX
[ergcm-2s
-1h
3]
-15 -10 -5 0 5 10 15-15
-10
-5
0
5
10
15
-15 -10 -5 0 5 10 15x [ h-1Mpc ]
-15
-10
-5
0
5
10
15
y[h-1Mp
c]
-15 -10 -5 0 5 10 15-15
-10
-5
0
5
10
15
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocksDiffuse radio emission in clusters
High-energy -ray emission
Non-thermal processes in clustersShock related emission
Hadronically induced emission
Radio gischt: primary CRe (150 MHz)
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Radio gischt: primary CRe (150 MHz)
10-8
10-6
10-4
10-2
100
S,primary
[mJyarcmin-2h70
2]
-15 -10 -5 0 5 10 15-15
-10
-5
0
5
10
15
-15 -10 -5 0 5 10 15
x [ h-1Mpc ]
-15
-10
-5
0
5
10
15
y
[h-1Mp
c]
-15 -10 -5 0 5 10 15-15
-10
-5
0
5
10
15
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocksDiffuse radio emission in clusters
High-energy -ray emission
Non-thermal processes in clustersShock related emission
Hadronically induced emission
Radio gischt + central hadronic halo giant radio halo
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Radio gischt + central hadronic halo = giant radio halo
10-8
10-6
10-4
10-2
100
S,total
[mJyarcm
in-2h70
3]
-15 -10 -5 0 5 10 15-15
-10
-5
0
5
10
15
-15 -10 -5 0 5 10 15
x [ h-1Mpc ]
-15
-10
-5
0
5
10
15
y
[h-1Mp
c]
-15 -10 -5 0 5 10 15-15
-10
-5
0
5
10
15
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocksDiffuse radio emission in clusters
High-energy -ray emission
Non-thermal processes in clustersShock related emission
Hadronically induced emission
Which one is the simulation/observation of A2256?
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Which one is the simulation/observation of A2256?
red/yellow: thermal X-ray emission,
blue/contours: 1.4 GHz radio emission with giant radio halo and relic
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocks
Diffuse radio emission in clusters
High-energy -ray emission
Non-thermal processes in clusters
Shock related emission
Hadronically induced emission
Observation simulation of A2256
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Observation simulation of A2256
Clarke & Enlin (2006) Pfrommer et al. (2008 in prep.)
red/yellow: thermal X-ray emission,
blue/contours: 1.4 GHz radio emission with giant radio halo and relic
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocks
Diffuse radio emission in clusters
High-energy -ray emission
Non-thermal processes in clusters
Shock related emission
Hadronically induced emission
Unified model of radio halos and relics
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Unified model of radio halos and relics
Cluster radio emission varies with dynamical stage of a cluster:
Cluster relaxes and develops cool core: radio mini-halo develops due to
hadronically produced CR electrons, magnetic fields are adiabatically
compressed (cooling gas triggers radio mode feedback of AGN that
outshines mini-halo selection effect).
Cluster experiences major merger: two leading shock waves are
produced that become stronger as they break at the shallow peripheralcluster potential shock-acceleration of primary electrons and
development of radio relics.
Generation of morphologically complex network of virializing shock
waves. Lower sound speed in the cluster outskirts lead to strong shocks
irregular distribution of primary electrons, MHD turbulence amplifiesmagnetic fields.
Giant radio halo develops due to (1) boost of the hadronically generated
radio emission in the center (2) irregular radio gischt emission in the
cluster outskirts.
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocks
Diffuse radio emission in clusters
High-energy -ray emission
Non-thermal processes in clusters
Shock related emission
Hadronically induced emission
Non-thermal emission from clusters
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Non thermal emission from clustersExploring the memory of structure formation
primary, shock-accelerated CR electrons resemble currentaccretion and merging shock waves
CR protons/hadronically produced CR electrons trace the timeintegrated non-equilibrium activities of clusters that is modulatedby the recent dynamical activities
How can we read out this information about non-thermal populations? new era of multi-frequency experiments, e.g.:
GMRT, LOFAR, MWA, LWA, SKA: interferometric array of radio
telescopes at low frequencies (
(15
240) MHz)Simbol-X/NuSTAR: future hard X-ray satellites (E (1100) keV)
Fermi -ray space telescope (E (0.1 300) GeV)
Imaging air Cerenkov telescopes (E (0.1 100) TeV)
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocks
Diffuse radio emission in clusters
High-energy -ray emission
Non-thermal processes in clusters
Shock related emission
Hadronically induced emission
Non-thermal emission from clusters
http://find/http://goback/ -
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57/72
Non thermal emission from clustersExploring the memory of structure formation
primary, shock-accelerated CR electrons resemble currentaccretion and merging shock waves
CR protons/hadronically produced CR electrons trace the timeintegrated non-equilibrium activities of clusters that is modulatedby the recent dynamical activities
How can we read out this information about non-thermal populations? new era of multi-frequency experiments, e.g.:
GMRT, LOFAR, MWA, LWA, SKA: interferometric array of radio
telescopes at low frequencies (
(15
240) MHz)Simbol-X/NuSTAR: future hard X-ray satellites (E (1100) keV)
Fermi -ray space telescope (E (0.1 300) GeV)
Imaging air Cerenkov telescopes (E (0.1 100) TeV)
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocks
Diffuse radio emission in clusters
High-energy -ray emission
Morphology and spectra
Predictions for Fermi
Minimum -ray flux
Outline
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Outline
1 Cosmological structure formation shocksCosmological galaxy cluster simulations
Mach numbers and shock acceleration
Cosmic ray transport and pressure distribution
2
Diffuse radio emission in clustersGeneral picture of non-thermal processes in clusters
Shock related emission
Hadronically induced emission
3 High-energy -ray emissionMorphology and spectra
Predictions for Fermi
Minimum -ray flux
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocks
Diffuse radio emission in clusters
High-energy -ray emission
Morphology and spectra
Predictions for Fermi
Minimum -ray flux
The quest for high-energy -ray emission from clusters
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The quest for high energy ray emission from clustersMulti-messenger approach towards fundamental astrophysics
1 complements current non-thermal observations of galaxyclusters in radio and hard X-rays:
identifying the nature of emission processes
unveiling the contribution of cosmic ray protons2 elucidates the nature of dark matter:
disentangling annihilation signal vs. CR induced -raysspectral and morphological -ray signatures DMproperties
3 probes plasma astrophysics such as macroscopic parametersfor diffusive shock acceleration
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocks
Diffuse radio emission in clusters
High-energy -ray emission
Morphology and spectra
Predictions for Fermi
Minimum -ray flux
Hadronic -ray emission, E > 100 GeV
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Hadronic ray emission, E > 100 GeV
10-12
10-11
10
-10
10-9
10-8
S
(100GeV,
100TeV)[
cm-2s
-1h70
3]
-3 -2 -1 0 1 2 3-3
-2
-1
0
1
2
3
-3 -2 -1 0 1 2 3
x [ h-1Mpc ]
-3
-2
-1
0
1
2
3
y
[h-1Mpc]
-3 -2 -1 0 1 2 3-3
-2
-1
0
1
2
3
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocks
Diffuse radio emission in clusters
High-energy -ray emission
Morphology and spectra
Predictions for Fermi
Minimum -ray flux
Inverse Compton emission, EIC > 100 GeV
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e se Co pto e ss o , IC > 00 Ge
10-12
10-11
10-10
10-9
10-8
S
(100GeV,
100TeV)[
cm-2s
-1h70
3]
-3 -2 -1 0 1 2 3-3
-2
-1
0
1
2
3
-3 -2 -1 0 1 2 3
x [ h-1Mpc ]
-3
-2
-1
0
1
2
3
y
[h-1Mpc]
-3 -2 -1 0 1 2 3-3
-2
-1
0
1
2
3
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocks
Diffuse radio emission in clusters
High-energy -ray emission
Morphology and spectra
Predictions for Fermi
Minimum -ray flux
Total -ray emission, E > 100 GeV
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62/72
y ,
10-12
10-11
10-10
10-9
10-8
S
(100GeV,
100TeV
)[
cm-2s
-1h70
3]
-3 -2 -1 0 1 2 3-3
-2
-1
0
1
2
3
-3 -2 -1 0 1 2 3
x [ h-1Mpc ]
-3
-2
-1
0
1
2
3
y
[h-1Mpc]
-3 -2 -1 0 1 2 3-3
-2
-1
0
1
2
3
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocks
Diffuse radio emission in clusters
High-energy -ray emission
Morphology and spectra
Predictions for Fermi
Minimum -ray flux
Universal CR spectrum in clusters
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63/72
p
GLAST: ~ 2.4
IACT: ~ 2.2p
p
10-4
10-2
100
102
104
106
108
1010
p
0.001
0.01
0.1
1
10
Normalized CR spectrum shows universal concave shape governed
mainly by hierarchical structure formation and adiabatic CR transport
processes. (Pinzke & Pfrommer, in prep.)
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocks
Diffuse radio emission in clusters
High-energy -ray emission
Morphology and spectra
Predictions for Fermi
Minimum -ray flux
Gamma-ray scaling relations
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64/72
y g
1014
1015
1044
1045
1046
L
(E
>100Me
V)[
s-1h70
]
S1, B0 = 10G, B = 0.5
S2, B0 = 10G, B = 0.5
Scaling relation + complete sample of the brightest X-ray clusters (extended
HIFLUCGS) predictions for Fermi
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocks
Diffuse radio emission in clusters
High-energy -ray emission
Morphology and spectra
Predictions for Fermi
Minimum -ray flux
Predicted cluster sample for Fermi
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65/72
p
10-9
10-8
0
2
4
6
8
10
12
14model S3
Ophiu
chus,
Forna
x
Coma
A3627Pe
rseus,
Centau
rus,A1060
M49
AWM7
,3C129
NGC4
636
A075
4
Trian
gulum
Nclusters
F [cm2 s1]
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocks
Diffuse radio emission in clusters
High-energy -ray emission
Morphology and spectra
Predictions for Fermi
Minimum -ray flux
Minimum -ray flux in the hadronic model (1)
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0.1 1.0 10.0
10-3
10-2
10-1
100
101
B[G]
j,IC(B)/j
,IC(BCMB)
j(B)/j(BCMB)
jIC(B)/jIC(BCMB)
For j(B) :
= 1 = 1.15
= 1.30
= 1.45
Synchrotron emissivity of high-
energy, steady state electrondistribution is independent of the
magnetic field for B BCMB!
Synchrotron luminosity:
L = A
dV nCRngas
(+1)/2B
CMB + B
A
dV nCRngas (B CMB)
-ray luminosity:
L = A
dV nCRngas
minimum -ray flux:
F,min =AA
L4D2
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocks
Diffuse radio emission in clusters
High-energy -ray emission
Morphology and spectra
Predictions for Fermi
Minimum -ray flux
Minimum -ray flux in the hadronic model (1)
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0.1 1.0 10.0
10-3
10-2
10-1
100
101
B[G]
j,IC(B)/j
,IC(BCMB)
j(B)/j(BCMB)
jIC(B)/jIC(BCMB)
For j(B) :
= 1 = 1.15
= 1.30
= 1.45
Synchrotron emissivity of high-
energy, steady state electrondistribution is independent of the
magnetic field for B BCMB!
Synchrotron luminosity:
L = A
dV nCRngas
(+1)/2B
CMB + B
A
dV nCRngas (B CMB)
-ray luminosity:
L = A
dV nCRngas
minimum -ray flux:
F,min =AA
L4D2
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocks
Diffuse radio emission in clustersHigh-energy -ray emission
Morphology and spectra
Predictions for FermiMinimum -ray flux
Minimum -ray flux in the hadronic model (2)
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Minimum -ray flux (E > 100 MeV) for the Coma cluster:
CR spectral index 2.0 2.3 2.6 2.9
F [1010cm2s1] 0.8 1.6 3.4 7.1
These limits can be made even tighter when consideringenergy constraints, PB < Pgas/20 and B-fields derivedfrom Faraday rotation studies, B0 = 3 G:F,COMA 2 10
9cm2s1 = FFermi, 2yr
Non-detection by Fermiseriously challenges the hadronicmodel.
Potential of measuring the CR acceleration efficiency for
diffusive shock acceleration.
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocks
Diffuse radio emission in clustersHigh-energy -ray emission
Morphology and spectra
Predictions for FermiMinimum -ray flux
Conclusions
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In contrast to the thermal plasma, the non-equilibrium distributions ofCRs preserve the information about their injection and transportprocesses and provide thus a unique window of current and paststructure formation processes and fundamental plasma astrophysics!
1 Cosmological hydrodynamical simulations are indispensable for
understanding non-thermal processes in galaxy clusters illuminating the process of structure formation
2 Unified model for the generation of giant radio halos, radiomini-halos, and relics: interplay of primary and secondarysynchrotron emission.
3 We predict Fermito detect ten -ray clusters: test of thepresented scenario
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocks
Diffuse radio emission in clustersHigh-energy -ray emission
Morphology and spectra
Predictions for FermiMinimum -ray flux
Literature for the talk
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Battaglia, Pfrommer, Sievers, Bond, Enlin, 2008, MNRAS, in print,
arXiv:0806.3272, Exploring the magnetized cosmic web through low frequencyradio emission
Pfrommer, 2008, MNRAS, 385, 1242 Simulating cosmic rays in clusters ofgalaxies III. Non-thermal scaling relations and comparison to observations
Pfrommer, Enlin, Springel, 2008, MNRAS, 385, 1211, Simulating cosmic rays inclusters of galaxies II. A unified scheme for radio halos and relics with
predictions of the-ray emissionPfrommer, Enlin, Springel, Jubelgas, Dolag, 2007, MNRAS, 378, 385,Simulating cosmic rays in clusters of galaxies I. Effects on theSunyaev-Zeldovich effect and the X-ray emission
Pfrommer, Springel, Enlin, Jubelgas, 2006, MNRAS, 367, 113,Detecting shock waves in cosmological smoothed particle hydrodynamics
simulationsEnlin, Pfrommer, Springel, Jubelgas, 2007, A&A, 473, 41,Cosmic ray physics in calculations of cosmological structure formation
Jubelgas, Springel, Enlin, Pfrommer, A&A, , 481, 33,Cosmic ray feedback in hydrodynamical simulations of galaxy formation
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocks
Diffuse radio emission in clustersHigh-energy -ray emission
Morphology and spectra
Predictions for FermiMinimum -ray flux
Diffuse low-frequency radio emission in Abell 521
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Brunetti et al. 2008, Nature, 455, 944:
colors: thermal X-ray emission, contours: diffuse radio emission, presence of radio structure at 610 MHz and their absence at three
times higher/lower frequency is incompatible with synchrotron theory!
Christoph Pfrommer Non-thermal emission from galaxy clusters
Cosmological structure formation shocks
Diffuse radio emission in clustersHigh-energy -ray emission
Morphology and spectra
Predictions for FermiMinimum -ray flux
Radio spectrum of radio halo in Abell 521
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Brunetti et al. 2008, Nature, 455, 944:
asterisks denote spectrum ofthe radio relic with 1.5
filled circles that of radio
halo with 2.1
radio halo interpretation:
re-acceleration of relativisticelectrons (Brunetti et al.)
hadronic model inconsistent
with spectra and morphologyradio relic interpretations:
aged population ofshock-accelerated electrons
populations of severalshock-compressed radioghosts (aged radio lobes)
polarization is key to differentiate
Christoph Pfrommer Non-thermal emission from galaxy clusters
http://find/http://goback/