  The Chandra HETGS spectra of the Seyfert 1 galaxy MCG--6-30-15 show numerous
narrow, unresolved (FWHM < 200 km/s) absorption lines from a wide range of
ionization states of N, O, Mg, Ne, Si, S, Ar, and Fe. The initial analysis of
these data, presented in Lee et al. (2001), shows that a dusty warm absorber
model adequately explains the spectral features > 0.48 keV (< 26 A). We
attribute previous reports of an apparently highly redshifted O VII edge to the
neutral Fe L absorption complex and the O VII resonance series (by transitions
higher than He $\gamma$; He $\alpha,\beta,\gamma$ are also seen at lower
energies). The implied dust column density needed to explain the FeI L edge
feature agrees with that obtained from earlier reddening studies, which had
already concluded that the dust should be associated with the ionized absorber
(given the relatively lower observed X-ray absorption by cold gas). Our
findings contradict the interpretation of Branduardi-Raymont et al. (2001),
based on XMM-Newton RGS spectra, that this spectral region is dominated by
highly relativistic soft X-ray line emission originating near the central black
hole. Here we review these issues pertaining to the soft X-ray spectral
features as addressed by Lee et al., (2001). (Details found in Lee et al.,
2001, ApJ., 554, L13)
