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We investigate the interplay between jets from Active Galactic Nuclei (AGNs)and the surrounding InterStellar Medium (ISM) through full 3D, high resolution,Adaptive Mesh Refinement simulations performed with the FLASH code. We followthe jet- ISM system for several Myr in its transition from an early, compactsource to an extended one including a large cocoon. During the jet evolution,we identify three major evolutionary stages and we find that, contrary to theprediction of popular theoretical models, none of the simulations shows aself-similar behavior. We also follow the evolution of the energy budget, andfind that the fraction of input power deposited into the ISM (the AGN couplingconstant) is of order of a few percent during the first few Myr. This is inbroad agreement with galaxy formation models employing AGN feedback. However,we find that in these early stages, this energy is deposited only in a smallfraction (< 1%) of the total ISM volume. Finally we demonstrate the relevanceof backflows arising within the extended cocoon generated by a relativistic AGNjet within the ISM of its host galaxy, previously proposed as a mechanism forself-regulating the gas accretion onto the central object. These backflows tendlater to be destabilized by the 3D dynamics, rather than by hydrodynamic(Kelvin- Helmholtz) instabilities. Yet, in the first few hundred thousandyears, backflows may create a central accretion region of significant extent,and convey there as much as a few millions of solar masses.

3D simulations of the early stages of AGN jets: geometry, thermodynamics and backflow