  We reexamine the spectroscopic underpinnings of recent suggestions that [O I]
and [Fe II] lines from the Orion H II region are produced in gas where the
iron-carrying grains have been destroyed and the electron density is
surprisingly high. Our new observations show that previous detections of [O I]
5577 were dominated by telluric emission. Our limits are consistent with a
moderate density (10^4 cm^{-3}) photoionized gas. We show that a previously
proposed model of the Orion H II region reproduces the observed [O I] and [Fe
II] spectrum. These lines are fully consistent with formation in a dusty region
of moderate density.
