remains low in the red wing of the Si [ii]{} line, so we constrain the maximum intensity and position to avoid double fitting the shifted, satellite Si [ii]{} line [cf. e.g. the list of adjacent spectral lines in @1986ApJS...61..801S]. The stationary component of Si [ii]{} also has a tendency to peak just blue-ward of the rest wavelength during the rise phase. The profile is itself slightly asymmetric, perhaps indicating an unidentified blend not listed in the [@1986ApJS...61..801S] atlas or a difference in the formation height of the ion compared to the other lines shown. Aside from these small uncertainties, the general behavior remains very clear in all lines.

Lastly, we notice that the width of the red-shifted components appears to be very large with respect to that of the stationary component, and to the pre-flare situation in general. While some broadening could be expected due to the long exposure times coupled with the rapid motion of the component (particularly in the FUV), it is plausible that most of the excess width could be created by flare-induced turbulent motions in the chromosphere [@2011ApJ...740...70M; @2015ApJ...804...56R]; the fact that the width of the red-shifted component seem to decrease with time (cf. the top 