  We present preliminary results from a 900 ks exposure of NGC 3783 with the
Chandra/HETGS. This is the best combination of signal-to-noise and resolution
ever obtained for an Active Galactic Nucleus (AGN). We resolve the narrow Fe
K\alpha line to have FWHM of 1720+/-360 km/s which, under the simple assumption
of virialized system, suggest that this narrow line is emitted between the
broad line region and the narrow line region. We do not detect any broad
component for the Fe K\alpha line though such component was observed in
previous ASCA observations of this object. Our results suggest an evolution in
the broad Fe K\alpha line that took place from the observations in 1996 to the
observations in 2000/2001.
  The high resolution X-ray spectrum of NGC 3783 shows more than a hundred
absorption lines and several dozen emission lines from the H-like and He-like
ions of N, O, Ne, Mg, Al, Si, and S as well as from Fe_XVII to Fe_XXIV L-shell
transitions. All these features can be modeled by a multi-component,
outflowing, photoionized absorber. There is no evidence (or need in the model)
for soft X-ray emission lines from a relativistic accretion disk as have been
proposed to be seen in a few other AGNs.
