Observed emission-line profiles with overlaid Gaussian models of a) O VII λ21.6 and O VII λ21.8 (MEG ± 1); b) O VIII λ18.97 (HEG ± 1); c) Ne IX λ13.45 and Ne IX λ13.55 (HEG ± 1); d) Ne X λ12.13 (HEG ± 1); e) Mg XI λ9.16 and Mg XI λ9.23 (HEG ± 1); f) Mg XII λ8.42 (HEG ± 1); g) Si XIII λ6.64, Si XIII λ6.68, and Si XIII λ6.74 (HEG ± 1); h) Si XIV λ6.18 (HEG± 1); i) S XV λ5.04, S XV λ5.06, and S XV λ5.10 (HEG ± 1); j) S XVI λ4.73 (HEG ± 1); k) Ar XVIII λ3.73, Ar XVII λ3.944 + Ar XVII λ3.961 + Ar XVII λ3.965, and Ar XVII λ3.994 + S XVI λ3.992 + S XVI λ3.991 (HEG ± 1); l) Ca XX λ3.02 and Ca XIX λ3.17 (HEG ± 1); and m) Fe XXVI λ1.78, Fe XXV λ1.85 and Fe XXV λ1.86 (HEG ± 1), where the HETG data and model profiles are shown with black and red histograms, respectively. Below each panel, we plot the fit residuals. Where overlapping, the HEG±1 and MEG±1 spectra were fit simultaneously; HEG±1 is shown for illustrative purposes. As discussed in Luna et al. (2010), the broad wings in the residuals to the fits of some of the emission lines – O VIII in particular – are due to emission by the photoionized preshock accretion flow.