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UHECR (Ultra High Cosmic Rays) made by He-like lightest nuclei might solvethe AUGER extragalactic clustering along Cen A: He UHECR cannot arrive fromVirgo because the light nuclei fragility and opacity above few Mpc; UHECRsignals are clustering along Cen-A spreading as observed by horizontal galacticarms magnetic fields, along random vertical angles [18]. Cen A events byHe-like spread along a width angle as large as the observed clustered one.UHECR He, being fragile should partially fragment in secondaries at tens EeVmultiplet (D,He3,p) almost as it occurs in the very recent UHECR multiplet at20 EeV along Cen A UHECR clustering [23]. Their narrow crowding within a tiny(Cen A centric disk) observation area (below 10^{-2} of the whole AUGER sky)aligned with Cen A may occur by a very low probability, below 3 \dot 10^{-5},see Fig. 1, 2,3, [23]. Remaining UHECR spread group show correlations withother gamma (MeV-Al^26 radioactive) maps, mainly due to galactic SNR sources asVela pulsar, the brightest, nearest GeV source [20]. Other nearest galacticgamma sources (as partially Crab and Galactic Center core) show links withUHECR via TeV correlated maps, see Fig.7. We speculate here that UHECR are alsoheavy radioactive galactic nuclei as Ni^56, Ni^57 and Co^57,Co^60 widely bent(tens degree up to \geq 100{\deg}) by galactic fields. UHECR radioactivity (inbeta,gamma channels) decay in flight at hundreds keV is boosted (by hugeLorentz factor \simeq 10^9 - 10^8) leading to TeVs gamma correlated skyanisotropy, see Fig.7. Tau neutrinos secondaries and their tau airshowers athorizons may rise (from hundreds TeVs-PeVs) in future ICECUBE,ANTARES [28],double bang events [29], or in ARGO and ASHRA [1] horizons or in AUGER or TAairshowers at PeVs-EeV energies, showing the expected Neutrino astronomy linkto UHECR decay in flight.

TeV sky versus AUGER one: are UHECR also radioactive, heavy galactic nuclei?