a rest velocity within $30-60$ seconds. This confirms and expands our previous findings (cf. Fig. 5 in Paper I), that the “satellite” component of chromospheric lines provides a clear picture of the condensation occurring within each flaring pixel at the early stages of the flare. The overall decay curve is essentially identical in all lines, even if the spectra in the IRIS FUV and NUV ranges are acquired with different exposure times (8 s and 2.4 s, respectively). Thus, it seems that the 9.4 s cadence of the observations is rapid enough to preserve the basic properties of the condensation evolution [@1989ApJ...346.1019F; @2017ApJ...836...12K], although higher cadence data could provide further insight.

After $\sim$ 60 s from the peak velocity, the fits for the red-shifted component in most lines become ambiguous, and a large scatter is thus observed in the time-velocity plot. For the Mg [ii]{} line, a fit is instead possible for a longer period, and a fairly constant condensation velocity of few km s$^{-1}$ is observed for several minutes (not fully shown in Figure \[fig:condensation\]).

Finally, from Fig. \[fig:condensation\] we see that a “build up phase” of the flows is apparent in Mg [ii]{}, and possibly in other lines, 