We present evidence for a broad , ionized Fe K \alpha line in the XMM-Newton spectrum of the broad-line radio galaxy ( BLRG ) 4C+74.26 .
This is the first indication that the innermost regions of the accretion flow in BLRGs contain thin , radiatively efficient disks .
Analysis of the 35 ks XMM-Newton observation finds a broad line with an inner radius close to the innermost stable circular orbit for a maximally spinning black hole .
The outer radius of the relativistic line is also found to be within 10 gravitational radii .
The Fe K \alpha line profile gives an inclination angle of \sim 40 ° , consistent with the radio limit .
There are two narrow components to the Fe K \alpha complex : one at 6.4 keV from neutral Fe , and one at 6.2 keV .
These may form the blue and red horns of a diskline from farther out on the disk , but a longer observation is required to confirm this hypothesis .
We discuss the implications of this observation for models of jet production , and suggest that BLRGs and radio-loud quasars will have larger than average black hole masses , thus resulting in thicker accretion flows close to the black hole .