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X-ray data for quasar 4C 74.26 have previously been modeled with a broad FeK$\alpha$ emission line and reflection continuum originating in the inner partof the accretion disk around the central supermassive black hole (SMBH), i.e.the strong gravity regime. We modeled broadband X-ray spectra from $Suzaku$ and$NuSTAR$ with MYTORUS, self-consistently accounting for Fe K$\alpha$ lineemission, as well as direct and reflected continuum emission, from finitecolumn density matter. A narrow Fe K$\alpha$ emission line originating in anX-ray reprocessor with solar Fe abundance far from the central SMBH issufficient to produce excellent fits for all spectra. For the first time, weare able to measure the global, out of the line-of-sight column density to bein the range $\sim$$1.5$ to $\sim$$2.9\times10^{24}$ cm$^{-2}$, i.e. in theCompton thick regime, while the line-of-sight column density is Compton thin inall observations. The Fe K$\alpha$ emission line is unresolved in all but oneobservations. The Compton scattered continuum from distant matter removes theneed for relativistic broadening of the Fe K$\alpha$ emission line, which isrequired for SMBH spin measurements. The resolved line observation canalternatively be modeled with a relativistic model but we do not find evidencefor a truncated accretion disk model. We conclude that the X-ray emission inthese 4C 74.26 data is unlikely to originate in the inner accretion disk regionand thus cannot be used to measure SMBH spin.

Broad Band X-ray Constraints on the Accreting Black Hole in Quasar 4C 74.26