Is there a relativistic Fe K line in qusarar 4C 74.26?

X-ray data for quasar 4C 74.26 have previously been modeled with a broad Fe Kα line emission consistent with an origin in the strong gravity regime in the inner part of the accretion disk, thus allowing estimates of supermassive black hole spin. We extracted broadband X-ray spectra from Suzaku and NuSTAR data and for the first time modeled them self-consistently with both direct and reflected continuum, as well as Fe K, emission using MYTORUS. We found that all spectra can be modeled well only with narrow Fe Kα line emission from a distant X-ray reprocessor, precluding the need for broad, relativistic components, so that supermassive black hole spin measurements cannot be carried out. We further obtained results for the equivalent neutral hydrogen column density both in and out of the line of sight, finding that all spectra are consistent with at least moderate Compton thick column density values.