also a brief ($\sim$ 30 s) and weak (few km s$^{-1}$) blue-ward “rebound” occurring around 17:31:30 UT once the red-shifted component has fully migrated back to the rest wavelength. This will be commented upon in Sect. \[sec:conclusion\].

Condensation: Spectral Fits {#sec:chrom_spectra}
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In the following we identify the Fe [i]{} 2814.11Å, Fe [ii]{} 2813.3 and 2814.45Å, Mg [ii]{} 2791.6Å, C [i]{} 1354.284Å and Si [ii]{} 1348.545Å lines as excellent diagnostics of flare chromospheric dynamics: while their intensity is much enhanced during the flare, these lines remain relatively narrow and unsaturated, and can be fairly well isolated from spectral blends and the general background.

Using the pixel at y=119.53 (marked in red diamonds on the bottom panel in Figure \[fig:ltspec\]) as a particularly clear example, we show in Figure \[fig:spectraA\] the spectra of multiple chromospheric lines in the Fe [ii]{} and Fe [ii]{} window, obtained at 5 consecutive time steps (black stepped lines). Fig. \[fig:spectraB\] shows the spectra of the Mg [ii]{}, C [i]{}, and Si [ii]{} lines in the same pixel, and times. The times in the panels of Figs. \[fig:spectraA\] and \[fig:spectraB\] correspond to the red diamonds of Figure \[fig:ltspec\], and the dotted black line indicates the nominal rest 