James
Just to give you a flavour, a Sept AGN paper abstract is here, discussing the high density jets of re-ionized matter. And one thing I forgot the Milky Way certainly DOES 'still have' and AGN. (iro Sagattarius A) Not (back) up to any great speed yet, so the 14 hypervelocity stars it has spat out recently are still in one piece, but there's also plenty of ions and gas.
Some are certainly worth paying for. The 'bipolar structures' referred in this one is a bit complex but can include 'kinetically decoupled' haloes and cores (rotating the other axis) which the recycling model explains.:
Claude-Andr茅 Faucher-Gigu猫re, Eliot Quataert The physics of galactic winds driven by active galactic nuclei MNRAS Volume 425 Issue 1, pages 605-622, 1 September 2012 http://onlinelibrary.wiley.com/doi/10.1111/j.1365-2966.2012.21512.x/abstract
Active galactic nuclei (AGN) drive fast winds in the interstellar medium of their host galaxies. It is commonly assumed that the high ambient densities and intense radiation fields in galactic nuclei imply short cooling times, thus making the outflows momentum conserving. We show that cooling of high-velocity shocked winds in AGN is in fact inefficient in a wide range of circumstances, including conditions relevant to ultraluminous infrared galaxies (ULIRGs), resulting in energy-conserving outflows. We further show that fast energy-conserving outflows can tolerate a large amount of mixing with cooler gas before radiative losses become important. For winds with initial velocity聽vin聽≳ 10 000 km s−1, as observed in ultraviolet and X-ray absorption, the shocked wind develops a two-temperature structure. While most of the thermal pressure support is provided by the protons, the cooling processes operate directly only on the electrons. This significantly slows down inverse Compton cooling, while free-free cooling is negligible. Slower winds with聽vin聽∼ 1000 km s−1, such as may be driven by radiation pressure on dust, can also experience energy-conserving phases but under more restrictive conditions. During the energy-conserving phase, the momentum flux of an outflow is boosted by a factor ∼vin/2vs聽by work done by the hot post-shock gas, where聽vs聽is the velocity of the swept-up material. Energy-conserving outflows driven by fast AGN winds (vin聽∼ 0.1c) may therefore explain the momentum fluxes聽聽of galaxy-scale outflows recently measured in luminous quasars and ULIRGs. Shocked wind bubbles expanding normal to galactic discs may also explain the large-scale bipolar structures observed in some systems, including around the Galactic Centre, and can produce significant radio, X-ray and γ-ray emission. The analytic solutions presented here will inform implementations of AGN feedback in numerical simulations, which typically do not include all the important physics.
There are scores of recent ones more relevant to halo density and morphology.
Peter