amplitude of downflows. Similarly to earlier observations and modelling [e.g. @1989ApJ...346.1019F], condensation velocities of up to $30-40~{\rm 
km~s^{-1}}$ were found, rapidly decaying to zero within $30-60$ s. While the evolution of the condensation velocity was extremely clear (see Figure 5, Paper I) we did not delve further into details of the line profiles themselves. It was, however, apparent that at several positions and times the Mg [ii]{} subordinate line profiles were strongly asymmetric, or even had distinct red-shifted components. Such a property was also noted by @2015ApJ...811..139T for several Si [ii]{} lines adjacent to the coronal Fe [xxi]{} line, but not analyzed further.

![Temporal evolution of Fe [i]{} 2814.1Å and Fe [ii]{} 2813.33 & 2814.45Å spectral profiles (top panel) and Mg [ii]{} 2791.6Å subordinate (middle panel), for flaring pixel y = 119.53. The intensity scale is reversed for clarity. The presence of a separate, rapidly evolving strongly redshifted component is obvious for all lines (horizontal dashed lines mark the rest wavelengths). The red diamonds (all panels) indicate the time of the spectra sampled in Fig. \[fig:spectraA\] and \[fig:spectraB\]. Bottom panel: space-time plot from a subset of 81 pixels along the IRIS slit (see Figure \[fig:irisaia\] or Paper I for context). 