8/14/2019 Pfrommer: Particle Acceleration and Radiation from Galaxy Clusters
1/54
Cosmological simulations with cosmic rays
Gamma-ray emission from clusters
Diffuse radio emission in clusters
Particle Acceleration and Radiationfrom Galaxy Clusters
Christoph Pfrommer1,2
in collaboration with
Anders Pinzke3, Torsten Enlin4, Volker Springel4,Nick Battaglia1, Jon Sievers1, Dick Bond1
1
Canadian Institute for Theoretical Astrophysics, Canada2Kavli Institute for Theoretical Physics, Santa Barbara
3Stockholm University, Sweden4Max-Planck Institute for Astrophysics, Germany
2 Oct 2009 / KITP Conference on Astrophysical Plasmas
Christoph Pfrommer Particle Acceleration and Radiation from Galaxy Clusters
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Cosmological simulations with cosmic rays
Gamma-ray emission from clusters
Diffuse radio emission in clusters
Outline
1 Cosmological simulations with cosmic rays
Motivation and observations
Cosmological galaxy cluster simulations
Non-thermal processes in clusters
2 Gamma-ray emission from clusters
Spectra and morphology
Predictions for Fermi and IACTs
MAGIC observations of Perseus
3 Diffuse radio emission in clustersThe cosmic magnetized web
Properties of cluster magnetic fields
Cluster turbulence
Christoph Pfrommer Particle Acceleration and Radiation from Galaxy Clusters
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3/54
Cosmological simulations with cosmic rays
Gamma-ray emission from clusters
Diffuse radio emission in clusters
Motivation and observations
Cosmological galaxy cluster simulations
Non-thermal processes in clusters
Outline
1 Cosmological simulations with cosmic rays
Motivation and observations
Cosmological galaxy cluster simulations
Non-thermal processes in clusters
2 Gamma-ray emission from clustersSpectra and morphology
Predictions for Fermi and IACTs
MAGIC observations of Perseus
3 Diffuse radio emission in clustersThe cosmic magnetized web
Properties of cluster magnetic fields
Cluster turbulence
Christoph Pfrommer Particle Acceleration and Radiation from Galaxy Clusters
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Cosmological simulations with cosmic rays
Gamma-ray emission from clusters
Diffuse radio emission in clusters
Motivation and observations
Cosmological galaxy cluster simulations
Non-thermal processes in clusters
How universal is diffusive shock acceleration (DSA)?What can galaxy clusters teach us about the process of shock acceleration?
Cosmological structure formation shock physics complementary tointerplanetary and SNR shocks:
probing unique regions of DSA parameter space: Mach numbers M 2 . . .10 with infinitely extended (Mpc)and lasting (Gyr) shocks (observationally accessible @ z = 0) plasma- factors of 102 . . .105
origin and evolution of large scale magnetic fields and nature ofturbulent models in a cleaner environment (1-phase medium)
consistent picture of non-thermal processes in galaxy clusters(radio, soft/hard X-ray, -ray emission) illuminating the process of structure formation history of individual clusters: cluster archeology
Christoph Pfrommer Particle Acceleration and Radiation from Galaxy Clusters
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Cosmological simulations with cosmic rays
Gamma-ray emission from clusters
Diffuse radio emission in clusters
Motivation and observations
Cosmological galaxy cluster simulations
Non-thermal processes in clusters
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 Particle Acceleration and Radiation from Galaxy Clusters
C l i l i l i i h i M i i d b i
http://find/http://goback/8/14/2019 Pfrommer: Particle Acceleration and Radiation from Galaxy Clusters
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Cosmological simulations with cosmic rays
Gamma-ray emission from clusters
Diffuse radio emission in clusters
Motivation and observations
Cosmological galaxy cluster simulations
Non-thermal processes in clusters
Radiative simulations with GADGET flowchart
CP, Enlin, Springel (2008)
Christoph Pfrommer Particle Acceleration and Radiation from Galaxy Clusters
C l i l i l ti ith i M ti ti d b ti
http://find/http://goback/8/14/2019 Pfrommer: Particle Acceleration and Radiation from Galaxy Clusters
7/54
Cosmological simulations with cosmic rays
Gamma-ray emission from clusters
Diffuse radio emission in clusters
Motivation and observations
Cosmological galaxy cluster simulations
Non-thermal processes in clusters
Radiative simulations with cosmic ray (CR) physics
CP, Enlin, Springel (2008)
Christoph Pfrommer Particle Acceleration and Radiation from Galaxy Clusters
Cosmological simulations with cosmic rays Motivation and observations
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Cosmological simulations with cosmic rays
Gamma-ray emission from clusters
Diffuse radio emission in clusters
Motivation and observations
Cosmological galaxy cluster simulations
Non-thermal processes in clusters
Diffusive shock acceleration Fermi 1 mechanism (1)
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 Particle Acceleration and Radiation from Galaxy Clusters
Cosmological simulations with cosmic rays Motivation and observations
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Cosmological simulations with cosmic rays
Gamma-ray emission from clusters
Diffuse radio emission in clusters
Motivation and observations
Cosmological galaxy cluster simulations
Non-thermal processes in clusters
Diffusive shock acceleration efficiency (2)
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
yinjectionefficiencyinj
inj
Mach number M
kT2 = 10 keVkT2 = 0.3 keVkT2 = 0.01 keV
3 5 11/3 3
Christoph Pfrommer Particle Acceleration and Radiation from Galaxy Clusters
Cosmological simulations with cosmic rays Motivation and observations
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Cosmological simulations with cosmic rays
Gamma-ray emission from clusters
Diffuse radio emission in clusters
Motivation and observations
Cosmological galaxy cluster simulations
Non-thermal processes in clusters
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 Particle Acceleration and Radiation from Galaxy Clusters
Cosmological simulations with cosmic rays Motivation and observations
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Cosmological simulations with cosmic rays
Gamma-ray emission from clusters
Diffuse radio emission in clusters
Motivation and observations
Cosmological galaxy cluster simulations
Non-thermal processes in clusters
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 Particle Acceleration and Radiation from Galaxy Clusters
Cosmological simulations with cosmic rays Motivation and observations
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Cosmological simulations with cosmic rays
Gamma-ray emission from clusters
Diffuse radio emission in clusters
Motivation and observations
Cosmological galaxy cluster simulations
Non-thermal processes in clusters
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 Particle Acceleration and Radiation from Galaxy Clusters
Cosmological simulations with cosmic rays Motivation and observations
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g y
Gamma-ray emission from clusters
Diffuse radio emission in clusters
Cosmological galaxy cluster simulations
Non-thermal processes in clusters
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 Particle Acceleration and Radiation from Galaxy Clusters
Cosmological simulations with cosmic rays Motivation and observations
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14/54
g y
Gamma-ray emission from clusters
Diffuse radio emission in clusters
Cosmological galaxy cluster simulations
Non-thermal processes in clusters
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 Particle Acceleration and Radiation from Galaxy Clusters
Cosmological simulations with cosmic rays Motivation and observations
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15/54
Gamma-ray emission from clusters
Diffuse radio emission in clusters
Cosmological galaxy cluster simulations
Non-thermal processes in clusters
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 Particle Acceleration and Radiation from Galaxy Clusters
Cosmological simulations with cosmic rays Motivation and observations
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16/54
Gamma-ray emission from clusters
Diffuse radio emission in clusters
Cosmological galaxy cluster simulations
Non-thermal processes in clusters
Multi messenger approach for non-thermal processes
Christoph Pfrommer Particle Acceleration and Radiation from Galaxy Clusters
Cosmological simulations with cosmic rays
G i i f l
Motivation and observations
C l i l l l i l i
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Gamma-ray emission from clusters
Diffuse radio emission in clusters
Cosmological galaxy cluster simulations
Non-thermal processes in clusters
Multi messenger approach for non-thermal processes
Christoph Pfrommer Particle Acceleration and Radiation from Galaxy Clusters
Cosmological simulations with cosmic rays
G i i f l t
Motivation and observations
C l i l l l t i l ti
http://find/http://goback/8/14/2019 Pfrommer: Particle Acceleration and Radiation from Galaxy Clusters
18/54
Gamma-ray emission from clusters
Diffuse radio emission in clusters
Cosmological galaxy cluster simulations
Non-thermal processes in clusters
Multi messenger approach for non-thermal processes
Christoph Pfrommer Particle Acceleration and Radiation from Galaxy Clusters
Cosmological simulations with cosmic rays
Gamma ray emission from clusters
Motivation and observations
Cosmological galaxy cluster simulations
http://find/http://goback/8/14/2019 Pfrommer: Particle Acceleration and Radiation from Galaxy Clusters
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Gamma-ray emission from clusters
Diffuse radio emission in clusters
Cosmological galaxy cluster simulations
Non-thermal processes in clusters
Multi messenger approach for non-thermal processes
Christoph Pfrommer Particle Acceleration and Radiation from Galaxy Clusters
Cosmological simulations with cosmic rays
Gamma ray emission from clusters
Motivation and observations
Cosmological galaxy cluster simulations
http://find/http://goback/8/14/2019 Pfrommer: Particle Acceleration and Radiation from Galaxy Clusters
20/54
Gamma-ray emission from clusters
Diffuse radio emission in clusters
Cosmological galaxy cluster simulations
Non-thermal processes in clusters
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 modulated
by 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 Particle Acceleration and Radiation from Galaxy Clusters
Cosmological simulations with cosmic raysGamma-ray emission from clusters
Motivation and observationsCosmological galaxy cluster simulations
http://find/http://goback/8/14/2019 Pfrommer: Particle Acceleration and Radiation from Galaxy Clusters
21/54
Gamma-ray emission from clusters
Diffuse radio emission in clusters
Cosmological galaxy cluster simulations
Non-thermal processes in clusters
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 modulated
by 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 Particle Acceleration and Radiation from Galaxy Clusters
Cosmological simulations with cosmic raysGamma-ray emission from clusters
Spectra and morphologyPredictions for Fermi and IACTs
http://find/http://goback/8/14/2019 Pfrommer: Particle Acceleration and Radiation from Galaxy Clusters
22/54
Gamma ray emission from clusters
Diffuse radio emission in clusters
Predictions for Fermi and IACT s
MAGIC observations of Perseus
Outline
1 Cosmological simulations with cosmic raysMotivation and observations
Cosmological galaxy cluster simulations
Non-thermal processes in clusters
2 Gamma-ray emission from clustersSpectra and morphology
Predictions for Fermi and IACTs
MAGIC observations of Perseus
3 Diffuse radio emission in clustersThe cosmic magnetized web
Properties of cluster magnetic fields
Cluster turbulence
Christoph Pfrommer Particle Acceleration and Radiation from Galaxy Clusters
Cosmological simulations with cosmic raysGamma-ray emission from clusters
Spectra and morphologyPredictions for Fermi and IACTs
http://find/http://goback/8/14/2019 Pfrommer: Particle Acceleration and Radiation from Galaxy Clusters
23/54
Gamma ray emission from clusters
Diffuse radio emission in clusters
Predictions for Fermi and IACT s
MAGIC observations of Perseus
CR proton and -ray spectrum (Pinzke & CP 2009)
10-2 100 102 104 106 108
p = Pp / (mp c)
10-3
10-2
10-1
1.0
f(p)p
2
10-2
100
102
104
106
108
1010
E[ GeV ]
10-12
10-11
10-10
10-9
F
(>E
)E
[GeVcm
2s
1]
sIC
pIC
Pion decay
Christoph Pfrommer Particle Acceleration and Radiation from Galaxy Clusters
Cosmological simulations with cosmic raysGamma-ray emission from clusters
Spectra and morphologyPredictions for Fermi and IACTs
http://find/http://goback/8/14/2019 Pfrommer: Particle Acceleration and Radiation from Galaxy Clusters
24/54
y
Diffuse radio emission in clusters MAGIC observations of Perseus
Hadronic -ray emission, E > 100 GeV
10-12
10-11
10-10
10-9
10-8
S
(E
>100GeV)[ph
cm-2s
-1]
-5 0 5
-5
0
5
-8 -6 -4 -2 0 2 4 6 8
x[Mpc ]
-8
-6
-4
-2
0
2
4
6
8
y[Mpc]
-8 -6 -4 -2 0 2 4 6 8-8
-6
-4
-2
0
2
4
6
8
Christoph Pfrommer Particle Acceleration and Radiation from Galaxy Clusters
Cosmological simulations with cosmic raysGamma-ray emission from clusters
Spectra and morphologyPredictions for Fermi and IACTs
http://find/http://goback/8/14/2019 Pfrommer: Particle Acceleration and Radiation from Galaxy Clusters
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y
Diffuse radio emission in clusters MAGIC observations of Perseus
Inverse Compton emission, EIC > 100 GeV
10-12
10-11
10-10
10-9
10-8
SIC,total
(E
>100GeV)[phcm-2s
-1]
-5 0 5
-5
0
5
-8 -6 -4 -2 0 2 4 6 8
x[Mpc ]
-8
-6
-4
-2
0
2
4
6
8
y[Mpc]
-8 -6 -4 -2 0 2 4 6 8-8
-6
-4
-2
0
2
4
6
8
Christoph Pfrommer Particle Acceleration and Radiation from Galaxy Clusters
Cosmological simulations with cosmic raysGamma-ray emission from clusters
Spectra and morphologyPredictions for Fermi and IACTs
http://find/http://goback/8/14/2019 Pfrommer: Particle Acceleration and Radiation from Galaxy Clusters
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Diffuse radio emission in clusters MAGIC observations of Perseus
Total -ray emission, E > 100 GeV
10-12
10-11
10-10
10-9
10-8
Stotal
(E
>100GeV)[phcm-2s
-1]
-5 0 5
-5
0
5
-8 -6 -4 -2 0 2 4 6 8
x[Mpc ]
-8
-6
-4
-2
0
2
4
6
8
y[Mpc]
-8 -6 -4 -2 0 2 4 6 8-8
-6
-4
-2
0
2
4
6
8
Christoph Pfrommer Particle Acceleration and Radiation from Galaxy Clusters
Cosmological simulations with cosmic raysGamma-ray emission from clusters
Spectra and morphologyPredictions for Fermi and IACTs
http://find/http://goback/8/14/2019 Pfrommer: Particle Acceleration and Radiation from Galaxy Clusters
27/54
Diffuse radio emission in clusters MAGIC observations of Perseus
Correlation between thermal X-ray and -ray emission
10-3
10-2
10-1
100
correlationspace
density[arbitraryunits]
10-10 10-9 10-8 10-7 10-6 10-5 10-4 10-310-10
10-9
10-8
10-7
10-6
10-5
10-4
10-10 10-9 10-8 10-7 10-6 10-5 10-4 10-3
SX
[ ergcm-2 s-1h703]
10-10
10-9
10-8
10-7
10-6
10-5
10-4
S
(>100Me
V)[
cm-s-h70]
10-10 10-9 10-8 10-7 10-6 10-5 10-4 10-310-10
10-9
10-8
10-7
10-6
10-5
10-4
merger, 10
15
h
-1
MO
:
Correlation with pion decay/sec. IC emission,
X-ray and secondary emission n2
(CP, Enlin, Springel 2008)
10-3
10-2
10-1
100
correlationspace
density[arbitraryunits]
10-10 10-9 10-8 10-7 10-6 10-5 10-4 10-310-10
10-9
10-8
10-7
10-6
10-5
10-4
10-10 10-9 10-8 10-7 10-6 10-5 10-4 10-3
SX [ ergcm-2 s-1h70
3]
10-10
10-9
10-8
10-7
10-6
10-5
10-4
S
(>100MeV)[
cm-2s
-1h70
2]
10-10 10-9 10-8 10-7 10-6 10-5 10-4 10-310-10
10-9
10-8
10-7
10-6
10-5
10-4
merger, 1015
h-1
MO :
Correlation with primary IC emission,
correlation space substructure
oblique curved shocks; B-generation!
Christoph Pfrommer Particle Acceleration and Radiation from Galaxy Clusters
Cosmological simulations with cosmic raysGamma-ray emission from clusters
Diff di i i i l
Spectra and morphologyPredictions for Fermi and IACTs
MAGIC b i f P
http://find/http://goback/8/14/2019 Pfrommer: Particle Acceleration and Radiation from Galaxy Clusters
28/54
Diffuse radio emission in clusters MAGIC observations of Perseus
Photon index - variations on large scales
0.80
0.87
0.93
1.00
1.07
1.13
1.20
(100M
eV,1GeV)
-5 0 5
-5
0
5
-8 -6 -4 -2 0 2 4 6 800000000
x [Mpc ]
-8
-6
-4
-2
0
2
4
6
8
00000000
y[
Mpc]
-8 -7 -6 -5 -4 -3 -2 -1 0 1 2 3 4 5 6 7 8-8
-7
-6
-5
-4
-3
-2
-1
0
1
2
3
4
5
6
7
8-8 -7 -6 -5 -4 -3 -2 -1 0 1 2 3 4 5 6 7 8
-8
-7
-6
-5
-4
-3
-2
-1
0
1
2
3
4
5
6
7
8
1 GeV100 MeV
(Fermi): pion bump (center)
transition to pIC (strong accretion shocks)
1.00
1.10
1.20
1.30
1.40
1.50
1.60
(100G
eV,
1TeV)
-5 0 5
-5
0
5
-8 -6 -4 -2 0 2 4 6 800000000
x [Mpc ]
-8
-6
-4
-2
0
2
4
6
8
00000000
y[Mpc]
-8 -7 -6 -5 -4 -3 -2 -1 0 1 2 3 4 5 6 7 8-8
-7
-6
-5
-4
-3
-2
-1
0
1
2
3
4
5
6
7
8-8 -7 -6 -5 -4 -3 -2 -1 0 1 2 3 4 5 6 7 8
-8
-7
-6
-5
-4
-3
-2
-1
0
1
2
3
4
5
6
7
8
1 TeV100 GeV
(IACTs): pion-decay (center)
pIC (accretion shocks, cutoff Emax)
Christoph Pfrommer Particle Acceleration and Radiation from Galaxy Clusters
Cosmological simulations with cosmic raysGamma-ray emission from clusters
Diff di i i i l t
Spectra and morphologyPredictions for Fermi and IACTs
MAGIC b ti f P
http://find/http://goback/8/14/2019 Pfrommer: Particle Acceleration and Radiation from Galaxy Clusters
29/54
Diffuse radio emission in clusters MAGIC observations of Perseus
Universal CR spectrum in clusters
Fermi: ~ 2.5
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 by
hierarchical structure formation and the implied distribution of Mach numbers
that a fluid element had to pass through in cosmic history (Pinzke & CP 2009).
Christoph Pfrommer Particle Acceleration and Radiation from Galaxy Clusters
Cosmological simulations with cosmic raysGamma-ray emission from clusters
Diffuse radio emission in clusters
Spectra and morphologyPredictions for Fermi and IACTs
MAGIC observations of Perseus
http://find/http://goback/8/14/2019 Pfrommer: Particle Acceleration and Radiation from Galaxy Clusters
30/54
Diffuse radio emission in clusters MAGIC observations of Perseus
An analytic model for the cluster -ray emissionComparison: simulation vs. analytic model, Mvir (10
14, 1015)M
10-32
10-31
10-30
10-29
10-28
10-27
(r,
E
=100M
eV)[phcm-3s
-1]
g72a
g914
pion decay profile:
simulation
analytic model
0.01 0.10 1.00R / Rvir
-0.4-0.20.00.20.4
/
Spatial -ray emission profile
10-13
10-12
10-11
10-10
10-9
g72a
g914
pion decay spectrum:
simulation
analytic model
10-2 100 102 104 106 108 1010
E[ GeV ]
-0.4-0.20.00.20.4
F
(>E
)E
[GeVcm
2s
1]
F
/F
Pion decay spectrum
Christoph Pfrommer Particle Acceleration and Radiation from Galaxy Clusters
Cosmological simulations with cosmic raysGamma-ray emission from clusters
Diffuse radio emission in clusters
Spectra and morphologyPredictions for Fermi and IACTs
MAGIC observations of Perseus
http://find/http://goback/8/14/2019 Pfrommer: Particle Acceleration and Radiation from Galaxy Clusters
31/54
Diffuse radio emission in clusters MAGIC observations of Perseus
Gamma-ray scaling relations
1014 1015
Mvir [ MO ]
1041
1042
1043
1044
1045
1046
L
(E
>100MeV)[phs-
1]
total -ray emission, excl. galaxies, R
8/14/2019 Pfrommer: Particle Acceleration and Radiation from Galaxy Clusters
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Diffuse radio emission in clusters MAGIC observations of Perseus
Predicted cluster sample for Fermiand IACTs
0 20 40 60 80 100
10-10
10-9
10-8
0 20 40 60 80 100
10-13
10-12
10-10
10-9
10-8
OPHIU
CHU
COMA
FORN
AX
A3627
PERS
EUS
A352
6
A1060
3C129
AWM7
M49
A075
4
CRs with galaxiesCRs witout galaxies
F
(E
>100GeV)
F
(E
>100MeV)
extended HIFLUGCS cluster ID
black: optimistic model, including galactic point sources that bias -ray flux
high; red: realistic model, excluding galactic point sources
Christoph Pfrommer Particle Acceleration and Radiation from Galaxy Clusters
Cosmological simulations with cosmic raysGamma-ray emission from clusters
Diffuse radio emission in clusters
Spectra and morphologyPredictions for Fermi and IACTs
MAGIC observations of Perseus
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Diffuse radio emission in clusters MAGIC observations of Perseus
Predicted cluster sample for Fermi brightest objects
10-10
10-9
10-8
0
2
4
6
8
10
12
14
excl. galaxies
Ophiuch
us
Com
aA36
27,Perseus
Fo
rnax
A36
26,A10
60
3C
129
Nclusters
F [phcm2 s1]
Christoph Pfrommer Particle Acceleration and Radiation from Galaxy Clusters
Cosmological simulations with cosmic raysGamma-ray emission from clusters
Diffuse radio emission in clusters
Spectra and morphologyPredictions for Fermi and IACTs
MAGIC observations of Perseus
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Diffuse radio emission in clusters MAGIC observations of Perseus
MAGIC observations of Perseus
Christoph Pfrommer Particle Acceleration and Radiation from Galaxy Clusters
Cosmological simulations with cosmic raysGamma-ray emission from clusters
Diffuse radio emission in clusters
Spectra and morphologyPredictions for Fermi and IACTs
MAGIC observations of Perseus
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Upper limit on the TeV -ray emission from Perseus
100 1000
E[GeV]
10-14
10-13
10-12
10-11
10-10
F
(>E
)[phs-1c
m-2]
radiative physics w/ gal. x 3.5radiative physics w/ gal.
radiative physics w/o gal.
F, min (B0 = 10 G, B < th / 3)
The MAGIC Collaboration: Aleksic et al. & CP et al. 2009
Christoph Pfrommer Particle Acceleration and Radiation from Galaxy Clusters
Cosmological simulations with cosmic raysGamma-ray emission from clusters
Diffuse radio emission in clusters
Spectra and morphologyPredictions for Fermi and IACTs
MAGIC observations of Perseus
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Results from the Perseus observation by MAGIC
assuming f p with = 2.1, PCR Pth:ECR < 0.017Eth most stringent constraint on CR pressure!
upper limits consistent with cosmological simulations:Fupper limits(100GeV) = 3.5 Fsim (optimistic model)
simulation modeling of pressure constraint yieldsPCR/Pth < 0.07 (0.14) for the core (entire cluster)
3 physical effects that resolve the apparent discrepancy:
concave curvature hides CR pressure at GeV energies
galactic point sources bias -ray flux high and pressurelimits low (partly physical)relative CR pressure increases towards the outer parts(adiabatic compression and softer equation of state of CRs)
Christoph Pfrommer Particle Acceleration and Radiation from Galaxy Clusters
Cosmological simulations with cosmic raysGamma-ray emission from clusters
Diffuse radio emission in clusters
Spectra and morphologyPredictions for Fermi and IACTs
MAGIC observations of Perseus
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Minimum -ray flux in the hadronic model
0.1 1.0 10.0
10-3
10-2
10-1
100
10
1
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 electron
distribution 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 Particle Acceleration and Radiation from Galaxy Clusters
Cosmological simulations with cosmic raysGamma-ray emission from clusters
Diffuse radio emission in clusters
Spectra and morphologyPredictions for Fermi and IACTs
MAGIC observations of Perseus
http://find/http://goback/8/14/2019 Pfrommer: Particle Acceleration and Radiation from Galaxy Clusters
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Minimum -ray flux in the hadronic model
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 electron
distribution 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 Particle Acceleration and Radiation from Galaxy Clusters
Cosmological simulations with cosmic raysGamma-ray emission from clusters
Diffuse radio emission in clusters
Spectra and morphologyPredictions for Fermi and IACTs
MAGIC observations of Perseus
http://find/http://goback/8/14/2019 Pfrommer: Particle Acceleration and Radiation from Galaxy Clusters
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Minimum -ray flux in the hadronic model: Fermi
Minimum -ray flux (E > 100 MeV) for the Coma cluster:
CR spectral index 2.0 2.3 2.6 2.9
F [1010 phcm2s1] 0.8 1.6 3.4 7.1
These limits can be made even tighter when considering energyconstraints, PB < Pgas/30 and B-fields derived from Faradayrotation studies, B0 = 3 G:F,COMA (1.1 . . .1.5) 10
9cm2s1 FFermi, 2yr
Non-detection by Fermi seriously challenges the hadronicmodel.
Potential of measuring the CR acceleration efficiency fordiffusive shock acceleration.
Christoph Pfrommer Particle Acceleration and Radiation from Galaxy Clusters
Cosmological simulations with cosmic raysGamma-ray emission from clusters
Diffuse radio emission in clusters
Spectra and morphologyPredictions for Fermi and IACTs
MAGIC observations of Perseus
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Minimum -ray flux in the hadronic model: IACTs
Minimum -ray flux (E > 100 GeV) for the Coma cluster:
CR spectral index 2.0 2.3 2.6 2.9
F [1014 phcm2s1] 20.2 7.6 2.9 1.1
These limits can be made even tighter when considering energyconstraints, PB < Pgas/30, FRM B-fields with B0 = 3 G, andp < 2.3 (caution: this assumes a power-law scaling):F,COMA (5.3 . . .7.6) 10
13cm2s1
Potential of measuring the CR spectrum, the effectiveacceleration efficiency for diffusive shock acceleration, andrelate this to the history of structure formation shock waves(Mach number distribution).
Christoph Pfrommer Particle Acceleration and Radiation from Galaxy Clusters
Cosmological simulations with cosmic raysGamma-ray emission from clusters
Diffuse radio emission in clusters
The cosmic magnetized webProperties of cluster magnetic fields
Cluster turbulence
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Outline
1 Cosmological simulations with cosmic raysMotivation and observations
Cosmological galaxy cluster simulations
Non-thermal processes in clusters
2 Gamma-ray emission from clustersSpectra and morphology
Predictions for Fermi and IACTs
MAGIC observations of Perseus
3 Diffuse radio emission in clustersThe cosmic magnetized web
Properties of cluster magnetic fields
Cluster turbulence
Christoph Pfrommer Particle Acceleration and Radiation from Galaxy Clusters
Cosmological simulations with cosmic raysGamma-ray emission from clusters
Diffuse radio emission in clusters
The cosmic magnetized webProperties of cluster magnetic fields
Cluster turbulence
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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 Particle Acceleration and Radiation from Galaxy Clusters
Cosmological simulations with cosmic raysGamma-ray emission from clusters
Diffuse radio emission in clusters
The cosmic magnetized webProperties of cluster magnetic fields
Cluster turbulence
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43/54
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 Particle Acceleration and Radiation from Galaxy Clusters
Cosmological simulations with cosmic raysGamma-ray emission from clusters
Diffuse radio emission in clusters
The cosmic magnetized webProperties of cluster magnetic fields
Cluster turbulence
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44/54
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 Particle Acceleration and Radiation from Galaxy Clusters
Cosmological simulations with cosmic raysGamma-ray emission from clusters
Diffuse radio emission in clusters
The cosmic magnetized webProperties of cluster magnetic fields
Cluster turbulence
http://find/http://goback/8/14/2019 Pfrommer: Particle Acceleration and Radiation from Galaxy Clusters
45/54
Radio gischt: primary CRe (15 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 Particle Acceleration and Radiation from Galaxy Clusters
Cosmological simulations with cosmic raysGamma-ray emission from clusters
Diffuse radio emission in clusters
The cosmic magnetized webProperties of cluster magnetic fields
Cluster turbulence
R di i h i CR (15 MH )
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Radio gischt: primary CRe (15 MHz), slower magnetic decline
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 Particle Acceleration and Radiation from Galaxy Clusters
Cosmological simulations with cosmic raysGamma-ray emission from clusters
Diffuse radio emission in clusters
The cosmic magnetized webProperties of cluster magnetic fields
Cluster turbulence
R di i ht ill i t i ti fi ld
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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 Particle Acceleration and Radiation from Galaxy Clusters
Cosmological simulations with cosmic raysGamma-ray emission from clusters
Diffuse radio emission in clusters
The cosmic magnetized webProperties of cluster magnetic fields
Cluster turbulence
Diff l t di i i i bl
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Diffuse cluster radio emission an inverse problemExploring the magnetized cosmic web
Battaglia, CP, 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 Particle Acceleration and Radiation from Galaxy Clusters
Cosmological simulations with cosmic raysGamma-ray emission from clusters
Diffuse radio emission in clusters
The cosmic magnetized webProperties of cluster magnetic fields
Cluster turbulence
P l ti f f i t di li i i l t
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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 Particle Acceleration and Radiation from Galaxy Clusters
Cosmological simulations with cosmic raysGamma-ray emission from clusters
Diffuse radio emission in clusters
The cosmic magnetized webProperties of cluster magnetic fields
Cluster turbulence
Relic luminosity function theory
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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 Particle Acceleration and Radiation from Galaxy Clusters
Cosmological simulations with cosmic raysGamma-ray emission from clusters
Diffuse radio emission in clusters
The cosmic magnetized webProperties of cluster magnetic fields
Cluster turbulence
Rotation measure (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 Particle Acceleration and Radiation from Galaxy Clusters
Cosmological simulations with cosmic raysGamma-ray emission from clusters
Diffuse radio emission in clusters
The cosmic magnetized webProperties of cluster magnetic fields
Cluster turbulence
Conclusions
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Conclusions
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 diffusive shock acceleration!
1 Universal distribution of CR protons determined by maximum
shock acceleration efficiency max and adiabatic transport:mapping between the hadronic -ray emission and max cosmological simulations are indispensable for exploring this(non-linear) map spectral shape illuminates the process of structure formation
2 Primary radio (gischt) emission traces the magnetized cosmicweb; sensitive to electron acceleration efficiency Faraday rotation on polarized Mpc-sized relics allowsdetermining the nature of the intra-cluster turbulence
Christoph Pfrommer Particle Acceleration and Radiation from Galaxy Clusters
Cosmological simulations with cosmic raysGamma-ray emission from clusters
Diffuse radio emission in clusters
The cosmic magnetized webProperties of cluster magnetic fields
Cluster turbulence
Conclusions
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53/54
Conclusions
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 diffusive shock acceleration!
1 Universal distribution of CR protons determined by maximum
shock acceleration efficiency max and adiabatic transport:mapping between the hadronic -ray emission and max cosmological simulations are indispensable for exploring this(non-linear) map spectral shape illuminates the process of structure formation
2 Primary radio (gischt) emission traces the magnetized cosmicweb; sensitive to electron acceleration efficiency Faraday rotation on polarized Mpc-sized relics allowsdetermining the nature of the intra-cluster turbulence
Christoph Pfrommer Particle Acceleration and Radiation from Galaxy Clusters
Cosmological simulations with cosmic rays
Gamma-ray emission from clusters
Diffuse radio emission in clusters
The cosmic magnetized web
Properties of cluster magnetic fields
Cluster turbulence
Conclusions
http://find/http://goback/8/14/2019 Pfrommer: Particle Acceleration and Radiation from Galaxy Clusters
54/54
Conclusions
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 diffusive shock acceleration!
1 Universal distribution of CR protons determined by maximum
shock acceleration efficiency max and adiabatic transport:mapping between the hadronic -ray emission and max cosmological simulations are indispensable for exploring this(non-linear) map spectral shape illuminates the process of structure formation
2 Primary radio (gischt) emission traces the magnetized cosmicweb; sensitive to electron acceleration efficiency Faraday rotation on polarized Mpc-sized relics allowsdetermining the nature of the intra-cluster turbulence
Christoph Pfrommer Particle Acceleration and Radiation from Galaxy Clusters
http://find/http://goback/