Variability of the radial velocity and Hα line profile during the Great Dimming. The main panel showcases the radial velocity variability, and the small numbered panels around it correspond to spectral line profiles on dates highlighted and numbered on the radial velocity curve of the main panel. Behind the highlighted line, all other five profiles are drawn in light grey, to provide a point of reference. Panel nr. 1 is from before the dimming minimum, but the emission is already visible. Panel nr. 2 showcases the profile when the star was faintest. The following panels, 3–6, were taken when the star was already brightening and the strength of the emission in Hα decreased. In the later period, the variability in radial velocity was caused mostly due to the variable profile of the absorption component rather than the strong emission influence (compare panels 4 and 5). Panels 2, 4, and 5 are FIES spectra; panel 1 is from DAO; and panels 3 and 6 are TO spectra. The lower resolution of panels 3 and 6 results in a smoother profile shape. We note that the systemic velocity of the star has not been subtracted from the velocity axis.