Iron K line emission in AGN: observations

Abstract

Iron K-alpha lines are key diagnostics of the central regions of AGN. Their profiles indicate that they are formed deep in the potential well of the central black hole, where extreme broadening and red shift occur. The profiles are most easily reproducible in an accretion disk: the lack of significant emission blue-ward of the rest energy is difficult produce in other geometries. In one source an apparent (and perhaps variable) absorption feature in the red wing of the line may represent rare evidence for inflow onto the black hole. Sample analysis has defined the mean properties, showing a strong concentration of the emission in the central regions and face-on accretion disks, at least in Seyfert 1 galaxies. Surprising results have been obtained from examination of the line variability. Strong profile changes may be accounted for by changes in the illumination pattern of the central, relativistic part of the disk. In at least the case of MCG-6-30-15, there is evidence for emission from within 6 R_g, possibly indicating a spinning black hole. Developing an understanding of these complex changes has the potential to reveal the geometry and kinematics of the inner few gravitational radii around extragalactic black holes.