gamma-rays and uhe cosmic rays from clusters of galaxies susumu inoue (nat. astron. obs. japan) and...
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Gamma-Rays and UHE Cosmic Rays
from Clusters of GalaxiesSusumu Inoue
(Nat. Astron. Obs. Japan)and collaborators
GeV100keV
HESS Auger
GLASTSuzaku
ZeV
TeV
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outline
1. introduction
2. gamma-ray emission from clusters
3. UHE cosmic rays from clusters
- UHE proton - photon pair syn.+IC
- UHE cosmic ray nuclei (and photopairs)
I, Aharonian & Sugiyama
I, Sigl, Armengaud & Miniati
- cascading (pair “halo”) I, Coppi & Aharonian
“Multi-messenger-nisme”
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current evidence for nonthermal emission: Coma1. introduction
radio Giovannini et al. 93 hard X-rayFusco-Femianoet al. 04
Rossetti &Molendi 04
4.8 detection
no detection
gamma-ray no clear evidence yet!GeV Reimer et al. 03
EUV
Bowyeret al. 04
TeV Perkins et al. 06
Renaud et al. astro-ph/0606114
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large scale structure formation (SF) shocks
formation of galaxies, groups, clusters...= hierarchical, dark matter-driven mergers and accretion→ shock formation → gas heating + nonthermal particle acceleration → nonthermal radiation
cosmological hydro simulations by Ryu et al. 03
shock velocitiesthermal emission
clusters are forming this very moment!
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cluster accretion shocks
accretion(minor merger)
(major) merger
Ryu et al. 03
strong (high M) shock-> high injection, hard spectra
weak (low M) shock-> low injection, soft spectra
crucial for nonthermal high energy phenomena
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nonthermal high energy emission from clusters
Miniati ‘03
thermal >100 MeV>100 keV
• primary electron IC
• LE proton p+p->0
• UHE proton-induced pair syn.+ICc.f. Aharonian 02 Rordorf, Grasso & Dolag ‘04
traces shock
traces gas
e.g. Waxman & Loeb 00 Totani & Kitayama 00
e.g. Völk et al. 96 Berezinsky et al. 97
tIC<<tshock
tloss, tconf>>tH
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11
10
9
8
720.520.019.519.018.518.017.5
log E [eV]
UHE proton-induced pair emission from cluster accretion shocks
accel. vs CMB losses, lifetime
photopion
lifetimeescape accel.
Bs=0.1 G
photopair
accel.Bs=1 G
e.g. Coma-like clusterM=2x1015 M(T=8.3 keV)WMAP cosmo. parameters
Inoue, Aharonian & Sugiyama 2005 ApJ 628, L9proton Emax
c.f. Kang, Rachen & Biermann 97
Rs~3.2 MpcVs~2200 km/sBs,eq~ 6 G
Emax~1018-1019 eVphotopair important
tacc=(20/3) rgc/Vs2
shock radius, velocity, etc.
Bohm limit shock accel. time
SNR observations ~1e.g. Völk et al. 05
escape timetesc~R2/D(E=Emax)~R/V~2 Gyr shock lifetimetsl~R/V~2 Gyr < tadiab~6 Gyr
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proton injection luminosity in accretion shocks
accretion rate & luminosityM(M,z)=fgasfaccVs
3/GLacc(M,z)=fgasfaccGMM/Rs
~2.7x1046 (fgas/0.16) (facc/0.1) (M/ 2x1015 M)5/3 erg/s
proton luminosity & spectrumLp(M,z)=fpLacc(M,z) fp=0.1Fp(E,M,z) ∝ E-2 exp(-E/Emax)
facc=0.1 normalized from simulationKeshet et al. 03
secondary production and emission processes
p+CMB→ p+ e+e-
Ep~1018eV E+-~+-Ep~1015eV→ e+e-+B(~G)→ syn. E~keV-MeV e+e-+CMB→ IC E~TeV-PeV
Aharonian 02 solve proton & pair kinetic eq.
..
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emitted flux & detectability Coma-like cluster at D=100 Mpcsensitivities for 1 deg2 extended source
- large radiative efficiency from protons- hard (~-1.5) spectrum + rollover- sensitive to B c.f. primary IC, pp 0 (~-2)
> TeV “absorption” by IRB+CMB
Suzaku, NeXTHESS, MAGIC,CANG.3, etc.
5 100h
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cascade emission: pair “halo”
pre-“absorbed” fluxcascade down to GeV-TeV
cluster pair “halos”- isotropic (much stronger than beamed sources)- hard spectrum
also for p-p 0 from core
probe of IRB, TeV-PeV power
Aharonian, Coppi & Völk 94Coppi & Aharonian 97
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3. UHECRs from cluster accretion shocks?
Norman, Achterberg & Melrose ‘95Kang, Ryu & Jones 96Kang, Rachen & Biermann 97
GRB
AGN jet
clusters
energetic requirements
Lcluster~1046 erg/sncluster~10-6 Mpc-3
Pcluster~~1040 erg s-1Mpc-3
UHECR@1020 eVuCR ~10-20 erg cm-3
CR ~0.3(1) Gyr for p (Fe)PCR ~3x1037 erg s-1Mpc-3 massive clusters (~1015 M)
energetically plausiblebut proton Emax insufficient
oblique shocks do not helpOstrowski & Siemieniec-Ozieblo 00
“Hillas plot” adapted fromYoshida & Dai 98
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UHECRs: energy losses during propagation
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p+CMB→ p+ e+e- Ep>~5x1017eVp+CMB→ p+ Ep>~7x1019eV
Lp, 20eV <~100 Mpc
A+CMB→ A+ e+e-
A+FIRB→ A-iN +iNNagano & Watson 00
Fe
p
E
Lloss
LFe, 20eV <~300 Mpc
protons: photopair+photopion
nuclei: photopair+photodisint.
e.g. Stecker &Salamon 99
E>2x1019 eV no data at all (too low statistics)E<2x1019 eV light dominant but greater uncertainties than commonly believed?
current data on composition HiRes stereo Xmax
Watson astro-ph/0408110
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nuclei from cluster accretion shocks as UHECRs
107
108
109
1010
1011
1018
2 3 4 5 6
1019
2 3 4 5 6
1020
2 3 4 5 6
1021
log E [eV]
56Fe
photodisint
photopair
Bs=0.1 G
Bs=1 G
heavy nuclei Emax
for Bs~1 G, EFe, max>~1020 eV
Inoue, Sigl, Armengaud & Miniatiin prep.
UHE nuclei propagation calculations
56Fe
lifetimeescape
log E [eV]lo
g t ac
c, t lo
ss [y
r]
Bs~1 G Johnston-Hollitt & Ekers 05
- simulation-based structured IGB models (also no IGB case)- source density ns~10-6 Mpc-3 ∝ baryon density- source power LCR(M)~ 3x1045 erg/s (fCR/0.1)(M/2x1015 M)5/3
- spectral index p=2, Emax(Z) from tacc vs. tloss, tlife- Galactic CR-like source composition (nFe/np~10-3 at fixed E/A)- CMB+FIRB losses, IGB deflections inc. all secondary nuclei
Feretti & Neumann 06
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UHE nuclei from clusters: results
with IGB
no IGB
spectra composition
anisotropyspectra, anisotropy, composition• consistent with current HiRes but not AGASA? higher Bs?• predictions: - “GZK” cutoff >1020 eV - heavy dominant >1019 eV - large scale aniso. toward few nearby sources
Auger, TA, EUSO
1020 eV1019 eV 1019 eV 1020 eV
fCR~0.03
fCR~0.005
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source composition “Galactic CR-like” (solar metallicity)metallicity outside clusters (warm-hot IGM filaments)
hard spectra at high E p<~1.5
Drury, Meyer & Ellison 99
nonlinear acceleration effects?
Kang & Jones 05
rigidity selection (heavy enhancement)stronger effects for accretion shocks?
Nicastro et al 05~0.1 solar (X-ray absorption)~0.2 solar (simulations) Cen & Ostriker astro-ph/0601008
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UHE nuclei induced pairs and emission
107
108
109
1010
1011
1018
2 3 4 5 6
1019
2 3 4 5 6
1020
2 3 4 5 6
1021
log E [eV]
56Fe
photodisint
photopair
Bs=0.1 G
Bs=1 G
107
108
109
1010
1011
1018
2 3 4 5 6
1019
2 3 4 5 6
1020
2 3 4 5 6
1021
log E [eV]
16O
nuclei photopair+photodisint. loss importantadditional hard X-ray and -ray emission, broader spectra?
56Fe16O
lifetimeescape
direct proof of nuclei accelerationconstrain source compositionpotentially
Ee+e-,A ~ (me /Amp ) Z Ep Ee-,ndec ~ (mn-p /Amp ) Z Ep
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summary
expected high energy emission from clusters• primary inverse Compton outskirts, MeV-GeV• p-p 0 core, GeV-TeV p-p e+- core, MeV• UHE p photopair emission outskirts, MeV+TeV• cascade emission (pair halo) larger scales, GeV-TeV• UHECR nuclei EeV-ZeV
different components dominate at different energy, locationpotential probe of cluster evolution
new type of high energy sourcepotentially very rich informationfertile new field of high energy astrophysics (Renaixança)!
e.g. non-gravitational energy injection, I & Nagashima, in prep.
but very little neutrinos…