T. Jane Turner (UMBC)
Chandra and XMM data have revealed narrow and highly redshifted Fe K emission lines in a handful of AGN. Rapid flux variability and energy shifts of the lines have lead to speculations for their origin ranging from hotspots on the accretion disk to emission from decelerating ejected blobs of gas traveling close to the escape velocity. Whichever scenario proves correct, these lines are invaluable in tracing gas close to the black hole, and arguably less subject to the ambiguities which have plagued interpretation of broad `disk lines'. I review observations of such lines to date and discuss progress possible with current and future instrumentation.