  The X-ray emission of many active galactic nuclei (AGNs) is absorbed between
15 and 17 Angstrom by means of unresolved (inner-shell) transition arrays
(UTAs) of Fe M-shell ions. The outflow velocities implied by the Doppler shifts
of the individual UTAs in the spectrum have never before been measured. Thus,
the Fe-M absorber has been commonly assumed to be part of the ionized AGN
outflow, whose velocities are readily obtained from more easily measured
spectral lines. The best spectrum of Fe-M absorption is available from the
integrated 900 ks Chandra HETGS observations of NGC 3783, in which some Fe-M
ions are clearly resolved. We measure the velocities of the individual Fe-M
ions in NGC 3783 for the first time. Surprisingly, we find that the Fe-M
absorber, most noticeably Fe$^{+8}$, Fe$^{+9}$, and Fe$^{+10}$, is not
outflowing at the same velocity as the previously known wind. In fact, it
appears to be stationary and therefore not part of the outflow at all. It
could, alternatively, be ascribed to the skin of the dusty torus. This reduces
appreciably the mass loss rate estimated for the NGC 3783 outflow and perhaps
for other similar sources as well, in which the various Fe-M ions are not
resolved.
