  Examination of emission lines in high-velocity resolution optical spectra of
the Orion Nebula confirms that the velocity component on the red wing of the
main ionization front emission line is due to backscattering in the Photon
Dominated Region. This scattered light component has a weak wavelength
dependence that is consistent with either general interstellar medium particles
or particles in the foreground of the Orion Nebula Cluster. An anomalous
line-broadening component that has been known for 60+ years is characterized in
unprecedented detail. Although this extra broadening may be due to turbulence
along the line-of-sight of our spectra, we explore the possibility that it is
due to \alf\ waves in conditions where the ratio of magnetic and thermal
energies are about equal and constant throughout the ionized gas.
