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As energetic particles diffuse out of radio and star-forming galaxies (SFGs),their intracluster density builds up to a level that could account for asubstantial part or all the emission from a radio halo. We calculate theparticle time-dependent, spectro-spatial distributions from a solution of adiffusion equation with radio galaxies as sources of electrons, and SFGs assources of both electrons and protons. Whereas strong radio galaxies aretypically found in the cluster (e.g., Coma) core, the fraction of SFGsincreases with distance from the cluster center. Scaling particle escape ratesfrom their sources to the reasonably well determined Galactic rates, and forrealistic gas density and magnetic field spatial profiles, we find thatpredicted spectra and spatial profiles of radio emission from primary andsecondary electrons are roughly consistent with those deduced from currentmeasurements of the Coma halo (after subtraction of emission from the relicComa A). Nonthermal X-ray emission is predicted to be mostly by Comptonscattering of electrons from radio galaxies off the CMB, whereas $\gamma$-rayemission is primarily from the decay of neutral pions produced in interactionsof protons from SFGs with protons in intracluster gas.

Galactic Energetic Particles and Their Radiative Yields in Clusters