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cluster accretion shocks!"#$%&'()*+,-./012
34 5 (6789:)

UHE proton induced
hard X-rays & #-rays w. Felix Aharonian (MPIK), "#$ (6789:)
UHE cosmic ray nuclei w. Günter Sigl, Eric Armengaud (IAP)
Francesco Miniati (ETH)
GLASTSuzaku
GeV100keV

AugerHESSTeVZeVUHECRs from cluster accretion shocks?
Norman, Achterberg & Melrose ‘95
Kang, Ryu & Jones 96
Kang, Rachen & Biermann 97

crucial for nonthermal high energy phenomena

Ryu et al. 03

accretion(minor merger)
strong (high M) shock-> high injection,
hard spectra

GRB

AGN jetclusters(major) merger

weak (low M) shock-> low injection,
soft spectraenergetic requirements
UHECR@1020 eV
uCR ~10-20 erg cm-3!CR ~0.3(1) Gyr for p (Fe)PCR ~3x1037 erg s-1Mpc-3
massive clusters (~1015 M")
Lcluster~1046 erg/s
ncluster~10-6 Mpc-3
Pcluster~~1040 erg s-1Mpc-3
energetically plausible, but
proton Emax insufficientUHE proton-induced pair emission from cluster accretion shocks
Inoue, Aharonian & Sugiyama 2005 ApJ 628, L9emitted flux & detectability

Coma-like cluster at D=100 Mpc> TeV absorption by IRB, CMB

sensitivities for 1 deg2 extended sourcemax p energy accel. vs CMB losses, lifetime e.g. Coma-like cluster
M=2x1015 M"(T=8.3 keV)WMAP cosmo. parameters

photopairshock radius, velocity, etc.

lifetime
escapeaccel.
Bs=0.1 µG
accel.
Bs=1 µG

photopion

Rs~3.2 Mpc
Vs~2200 km/s
Bs,eq~ 6 µG
Bohm limit shock accel.
tacc=(20/3) & rgc/Vs2
SNR observations &~1e.g. Völk et al. 05
shock lifetimets~2 Gyr < tadiab~6 GyrEmax~1018-1019 eV
photopair importantInoue, Sigl, Armengaud & Miniati, in prep.

coming very soon!!!
• Inoue, Gabici, Aharonian & Rowell, HESS proposal, accepted• Inoue, Nakazawa, Fukazawa et al., Suzaku proposal, submittedX

photopair+photopion CMB
photodisint FIRB+CMB

Bs~1 µG
also expecting
contributions fromCANGAROO III

HESS#maximum E for heavy nuclei

if Bs~1 µG
EFe, max>~1020 eV
photopair important

Suzaku#<-> primary IC, pp %0($~-2)

nuclei from cluster accretion shocks as UHECRs

TeV #-ray and hard X-ray observations of clusters

X- large radiative efficiency from protons- hard ($~-1.5) spectrum + rollover- sensitive to B

photopair56Fe

Bs=0.1 µG

Johnston-Hollitt & Ekers ‘05

lifetime
escape

Bs=1 µG
photodisint

UHE nuclei propagation calculations- realistic IGB models based on cosmological simulations- source density ~10-6 Mpc-3 % baryon density- Emax(Z) from tacc vs. tloss, tlife- Galactic CR-like source composition (nFe/np~0.05)- interactions in CMB+FIRB, deflections in IGB
including all secondary nuclei

UHE nuclei from clusters: results
spectracomposition

UHE nuclei induced pairs
16O

photopair56Fe

Bs=0.1 µG
lifetime
escapewith IGB
no IGB

anisotropy

summaryspectra, anisotropy, composition• consistent withcurrent HiRes but not AGASA…
• predictions:- “GZK” cutoff >1020 eV- heavy dominant >1019 eV- one or few extended source(s)>4x1019eV

UHE processes in cluster accretion shocks

UHE p-induced emission• acceleration to E~1018-1019eV• efficient secondary pair emission-> hard X sync. Suzaku, NeXT (imaging), …
-> TeV IC HESS, CANG.III, other current IACTs• important probe of UHE p acceleration, B in cluster outskirts, …
stay tuned for upcoming HESS & Suzaku observations!
UHECR nuclei• Fe acceleration to E~1020eV plausible if B~1 µG• UHECR flux and spectra consistent if nFe/np~0.05 at source• predictions for Auger, TA, EUSO:- spectra: cutoff >~1020 eV- composition: p dominant ~<1019 eV, Fe dominant >~1020 eV- anisotropy: a few extended sources >~4x1019 eV• additional hard X/TeV from pairs HESS, Suzaku, …

Bs=1 µGphotodisint

photopair important
additional hard X-ray and #-ray emission, broader spectra
direct proof of nuclei acceleration in cluster accretion shocks