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We present XMM and Suzaku observations of the Broad-Line Radio Galaxy (BLRG)3C390.3. The Fe Ka line has a width FWHM ~ 8,800 km/s, consistent within afactor two with the width of the double-peaked H_alpha line, suggesting anorigin from the Broad Line Region. The data show for the first time a weak,broad bump extending from 5 to 7 keV. When fitted with a Gaussian, its centroidenergy is 6.6 keV in the source's rest-frame with FWHM of 43,000 km/s and EW of50 eV; its most likely interpretation is emission from He-like Fe (Fe XXV),suggesting the presence of an ionized medium in the inner regions of 3C390.3.The broad-band 0.5-100 keV continuum is well described by a single power lawwith photon index Gamma=1.6 and cutoff energy 157 keV, plus cold reflectionwith strength R=0.5. In addition, ionized reflection is required to account forthe 6.6 keV bump in the broad-band continuum, yielding an ionization parameterxi ~ 2700 ergs cm s^-1; the inner radius of the ionized reflector isconstrained to be larger than 20 r_G, although this result depends on theassumed emissivity profile of the disk. If true, we argue that the lack ofbroad Fe K emission from within 20 r_G indicates that the innermost regions ofthe disk in 3C390.3 are obscured and/or poorly illuminated. While the SED of3C390.3 is generally dominated by accretion-related continuum, during accretionlow states the jet can significantly contribute in the optical to X-ray bandsvia synchrotron self-Compton emission. (Abridged)

Structure of the Accretion Flow in Broad-Line Radio Galaxies: The Case of 3C390.3