The Seyfert 2 galaxy NGC 5728 exhibits x-ray emission over a region ∼ ±1kpc in extent, including a broad (∼ 30,000 km/s) line at 6 keV as well as slower (∼ 1,000 km/s) outflow in [O III] and other low ionization state ions, and an even slower outflow in molecular gas. I will show that the ions producing the 6 keV line emission come from material that is not strongly coupled to the ambient (probably also outflowing) gas. I will argue that most of the emitting material is embedded in dust grains that are decoupled from the gas, and driven outward by radiation pressure from the big blue bump of the central AGN. The grains can be accelerated in a time shorter than the grain sputtering or shattering time, with a modest fraction of the Fe (and other) atoms being separated from the grains. The sputterd Fe atoms will produce the observed Fe Lyman alpha emission. The kinetic luminosity and momentum outflow rate are orders of magnitude lower than would be inferred using models of ultra-fast outflows of similar velocity. If this result holds for other UFOs, it will alter our current understanding of AGN feedback, removing one possible channel.
