  Chandra and XMM observations are showing that the Fe-K emission lines in type
1 AGN are composite, in general consisting of a narrow and a broad component.
We review the latest Chandra HETG results and compare the line profiles with
those measured by ASCA. The narrow Fe-K line components necessitate re-modeling
of the line profiles measured previously and revision of the parameters of the
relativistic broad components, as well re-interpretation of variability
studies. We also explicitly demonstrate the effect of changes in the ASCA
calibration on the measurements of the Fe-K lines in AGN. We find that the
differences in measured parameters are insignificant. Both the intrinsic width
and EW change by less than 8%. Fe-K line studies which claim much larger
differences do not adequately model the line emission. We point out that it is
incorrect to compare different calibrations, and indeed make astrophysical
inferences, using models which do not describe the data. We then present some
new results for the highest S/N broad Fe-K line profile in the entire ASCA
archive, from NGC 4151.
