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Fairall 9 is one of several type 1 active galactic nuclei for which it hasbeen claimed that the angular momentum (or spin) of the supermassive black holecan be robustly measured, using the Fe K$\alpha$ emission line andCompton-reflection continuum in the X-ray spectrum. The method rests upon theinterpretation of the Fe K$\alpha$ line profile and associatedCompton-reflection continuum in terms of relativistic broadening in the stronggravity regime in the innermost regions of an accretion disc, within a fewgravitational radii of the black hole. Here, we re-examine a Suzaku X-rayspectrum of Fairall 9 and show that a face-on toroidal X-ray reprocessor modelinvolving only nonrelativistic and mundane physics provides an excellent fit tothe data. The Fe K$\alpha$ line emission and Compton reflection continuum arecalculated self-consistently, the iron abundance is solar, and an equatorialcolumn density of $\sim 10^{24} \ \rm cm^{-2}$ is inferred. In this scenario,neither the Fe K$\alpha$ line, nor the Compton-reflection continuum provide anyinformation on the black-hole spin. Whereas previous analyses have assumed aninfinite column density for the distant-matter reprocessor, the shape of thereflection spectrum from matter with a finite column density eliminates theneed for a relativistically broadened Fe K$\alpha$ line. We find a 90 per centconfidence range in the Fe K$\alpha$ line FWHM of $1895$-$6205 \ \rm km \s^{-1}$, corresponding to a distance of $\sim 3100$ to $33,380$ gravitationalradii from the black hole, or $0.015$-$0.49$ pc for a black-hole mass of $\sim1-3 \times 10^{8} \ M_{\odot}$.

No Signatures of Black-Hole Spin in the X-ray Spectrum of the Seyfert 1 Galaxy Fairall 9