A complete view of the broad-line radio galaxy 4C+74.26 with XMM-Newton

This paper presents a timing study and broadband spectral analysis of the broad-line radio galaxy 4C+74.26 based on a 35 ks XMM-Newton observation. As found in previous datasets, the source exhibits no evidence for rapid variability, and its 0.2–10 keV lightcurve is well fit by a constant. An excellent fit to the pn 0.3–12 keV spectrum was found using a continuum that combines an ionized and a neutral reflector, augmented by both cold and warm absorption. There is no evidence for a soft excess. The column of cold absorption was greater than the Galactic value with an intrinsic column of∼ 1.9×10 cm. Evidence for the warm absorber was found from O VII and O VIII absorption edges with maximum optical depths of τ O VII = 0.3 and τ O VIII = 0.03, respectively. A joint pn-MOS fit increased the O VIII optical depth to τ O VIII = 0.1. A simple, one-zone warm absorber model yielded a column of ∼ 9 × 10 20 cm and an ionization parameter of ∼ 60. Partial covering models provide significantly worse fits than ones including a relativistically broadened Fe Kα line, strengthening the case for the existence of such a line. On the whole, the X-ray spectrum of 4C+74.26 exhibits many features typical of both a radio-loud quasar (excess absorption) and radio-quiet Seyfert 1 galaxies (Fe Kα emission and warm absorption). We also show that a spurious absorption line at ∼ 8 keV can be created by the subtraction of an instrumental Cu Kα emission line.